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1. Towards a Real-Time Bayesian Imitation System for a Humanoid Robot.

Author: Aaron P. Shon, Joshua J. Storz, and Rajesh P. N. Rao
Published: 2007
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2. MAGIC upper limits on the GRB 090102 afterglow

Author: M. Gaug, Elisa Bernardini, Gianluca Giavitto, A. González Muñoz, C. Delgado Mendez, Victor Stamatescu, T. Schweizer, A. De Angelis, Mosè Mariotti, A.-K. Overkemping, D. Dominis Prester, Robert Wagner, L. A. Antonelli, Julian Sitarek, Saverio Lombardi, M. L. Knoetig, P. Antoranz, J. Hose, Natalia Lewandowska, T. Toyama, A. Sillanpää, Nikola Godinovic, Takashi Saito, P. Temnikov, Benito Marcote, Abelardo Moralejo, A. La Barbera, Fabrizio Tavecchio, M. V. Fonseca, A. Bouvier, J. Moldón, D. Garrido Terrats, Konstancja Satalecka, Ll. Font, Reiko Orito, Francisco Prada, W. Idec, Julia Thaele, Michele Doro, M. Palatiello, Dario Hrupec, Jelena Aleksić, M. A. Lopez, E. Colombo, P. Da Vela, V. Scalzotto, Dominik Elsaesser, U. Barres de Almeida, A. Niedzwiecki, M. Doert, Damir Lelas, Fabio Zandanel, Ralph Bock, L. O. Takalo, K. Frantzen, Q. Weitzel, Tihomir Surić, M. Uellenbeck, David Paneque, Francesco Dazzi, Patrick Vogler, Hiroyasu Tajima, I. Snidaric, D. Carreto Fidalgo, Ana Babić, Dorota Sobczyńska, G. De Caneva, U. Menzel, M. Salvati, Stefano Ansoldi, S. Rügamer, Juan Abel Barrio, Riccardo Paoletti, Nina Nowak, Diego F. Torres, A. Herrero, Christian Fruck, S. Partini, M. Hayashida, Francesco Longo, E. Lorenz, S. Paiano, Kari Nilsson, Karl Mannheim, Nijil Mankuzhiyil, K. Berger, P. Munar-Adrover, I. Lozano, D. Hadasch, Giacomo Bonnoli, E. Prandini, J. M. Paredes, M. Garczarczyk, Antonio Stamerra, Silvia Preziuso, Marc Ribó, P. G. Prada Moroni, J. Kushida, Aldo Treves, Jose Luis Contreras, J. Krause, B. De Lotto, Masahiro Teshima, O. Tibolla, Juan Cortina, Martin Makariev, Oscar Blanch, Tomislav Terzić, A. Hadamek, J. Storz, Ivica Puljak, Alicia López-Oramas, Pierre Colin, J. Becerra González, Emanuele Paolo Farina, S. Bonnefoy, Aaron Dominguez, Mario Meucci, R. Mirzoyan, D. Eisenacher, E. Carmona, Daniel Ferenc, Thomas Bretz, S. N. Shore, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, Felix Spanier, D. Nakajima, C. Schultz, V. Scapin, Jose Miguel Miranda, F. Borracci, Wolfgang Rhode, Ignasi Reichardt, G. Maneva, R. Zanin, A. Saggion, Adrian Biland, J. Rico, R. Reinthal, L. Maraschi, Elina Lindfors, Daniel Mazin, K. Mallot, R. J. García López, Stefano Covino, S. Sun, Massimo Persic, A. Boller, L. Cossio, D. Tescaro, T. Krähenbühl, K. Saito, J. Masbou, M. I. Martínez, V. Kadenius, S. R. Gozzini, J. Rodriguez Garcia, Daniela Dorner, J., Aleksic, S., Ansoldi, L. A., Antonelli, P., Antoranz, A., Babic, U. B., de Almeida, J. A., Barrio, J. B., Gonzalez, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, F., Borracci, T., Bretz, E., Carmona, A., Carosi, D. C., Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C. D., Mendez, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, E., Farina, D., Ferenc, M. V., Fonseca, L., Font, K., Frantzen, C., Fruck, R. J. G., Lopez, M., Garczarczyk, D. G., Terrat, M., Gaug, G., Giavitto, N., Godinovic, A. G., Munoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, W., Idec, V., Kadeniu, M. L., Knoetig, T., Krahenbuhl, J., Krause, J., Kushida, A. L., Barbera, D., Lela, N., Lewandowska, E., Lindfor, S., Lombardi, R., Lopez Coto, M., Lopez, A., Lopez Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martinez, J., Masbou, D., Mazin, U., Menzel, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldon, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, K., Nilsson, N., Nowak, R., Orito, A., Overkemping, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, F., Prada, P. G. P., Moroni, E., Prandini, S., Preziuso, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, J. R., Garcia, S., Rugamer, A., Saggion, K., Saito, T., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpaa, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, V., Stamatescu, A., Stamerra, J., Storz, S., Sun, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, J., Thaele, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, A., Bouvier, M., Hayashida, H., Tajima, and Longo, Francesco
Subjects: Photon, General, Non-thermal - gamma-ray burst, Radiation mechanisms, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Hadron, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, general [gamma-ray burst], 7. Clean energy, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, MAGIC (telescope), 010306 general physics, 010303 astronomy & astrophysics, Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, ta115, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], Afterglow, gamma-rays bursts: general, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: Indications of a GeV component in the emission from GRBs are known since the EGRET observations during the 1990's and they have been confirmed by the data of the Fermi satellite. These results have, however, shown that our understanding of GRB physics is still unsatisfactory. The new generation of Cherenkov observatories and in particular the MAGIC telescope, allow for the first time the possibility to extend the measurement of GRBs from several tens up to hundreds of GeV energy range. Both leptonic and hadronic processes have been suggested to explain the possible GeV/TeV counterpart of GRBs. Observations with ground-based telescopes of very high energy photons (E>30 GeV) from these sources are going to play a key role in discriminating among the different proposed emission mechanisms, which are barely distinguishable at lower energies. MAGIC telescope observations of the GRB 090102 (z=1.547) field and Fermi Large Area Telescope (LAT) data in the same time interval are analysed to derive upper limits of the GeV/TeV emission. We compare these results to the expected emissions evaluated for different processes in the framework of a relativistic blast wave model for the afterglow. Simultaneous upper limits with Fermi and a Cherenkov telescope have been derived for this GRB observation. The results we obtained are compatible with the expected emission although the difficulties in predicting the HE and VHE emission for the afterglow of this event makes it difficult to draw firmer conclusions. Nonetheless, MAGIC sensitivity in the energy range of overlap with space-based instruments (above about 40 GeV) is about one order of magnitude better with respect to Fermi. This makes evident the constraining power of ground-based observations and shows that the MAGIC telescope has reached the required performance to make possible GRB multiwavelength studies in the very high energy range., 8 pages, 5 figures, 2 tables. Submitted to MNRAS
Published: 2014

3. The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system

Author: R. Zanin, Adrian Biland, I. Lozano, J. Rico, Masahiro Teshima, W. Idec, Takashi Saito, J. Krause, B. De Lotto, Nikola Godinovic, Benito Marcote, Stefano Ansoldi, I. Snidaric, David Fink, K. Mallot, R. J. García López, D. Corti, Alessandro Carosi, Mosè Mariotti, A.-K. Overkemping, J. M. Illa, Riccardo Paoletti, Massimo Persic, Gianluca Giavitto, A. González Muñoz, Reiko Orito, P. Temnikov, M. Palatiello, J. Becerra González, Marcel Strzys, Dario Hrupec, M. Bitossi, Ruben Lopez-Coto, Jose Luis Lemus, D. Nakajima, Elina Lindfors, E. Lorenz, Abelardo Moralejo, Saverio Lombardi, A. Treves, Vitaly Neustroev, M. Makariev, Thomas Bretz, Daniel Mazin, Jose Miguel Miranda, M. A. Lopez, S. Rügamer, Juan Abel Barrio, S. Schmidl, T. Steinbring, Francesco Dazzi, J. M. Paredes, Antonio Stamerra, C. Delgado Mendez, G. Maneva, Stefano Covino, B. Biasuzzi, A. Dettlaff, M. Hayashida, D. Hildebrand, Francesco Longo, G. De Caneva, D. Fidalgo, Daniela Dorner, Jose Luis Contreras, Wolfgang Rhode, M. I. Martínez, Marc Ribó, S. Bonnefoy, K. Saito, Natalia Lewandowska, Patrick Vogler, E. Colombo, M. Gaug, Juan Cortina, D. Tescaro, Roberto Cecchi, P. Bangale, H. Wetteskind, A. La Barbera, A. Deangelis, J. Herrera, Hidetoshi Kubo, Sabrina Einecke, S. R. Gozzini, Luis Ángel Tejedor, M. V. Fonseca, Hanna Kellermann, Koji Noda, Louis Antonelli, G. Bonnoli, J. Rodriguez Garcia, Elisa Bernardini, X. Paredes-Fortuny, J. Hose, U. Menzel, K. Kodani, J. Storz, Yusuke Konno, Christian Fruck, A. Sillanpää, D. Elsaesser, L. O. Takalo, F. Borracci, W. Haberer, H. Takami, Oscar Blanch, K. Frantzen, P. G. Prada Moroni, Diego F. Torres, W. Bednarek, Fabrizio Tavecchio, V. Kadenius, S. Paiano, Ll. Font, D. Garrido Terrats, A. Lorca, Karl Mannheim, O. Tibolla, Alicia López-Oramas, T. Schweizer, Felix Spanier, R. Mirzoyan, P. Munar-Adrover, D. Eisenacher, V. Scalzotto, Markus Garczarczyk, N. Mankuzhiyil, Juri Poutanen, Kyoshi Nishijima, D. Dominis Prester, Y. Hanabata, C. Schultz, V. Scapin, P. Antoranz, M. L. Knoetig, Ana Babić, Julia Thaele, E. Carmona, Kari Nilsson, M. Will, L. Maraschi, E. Prandini, Tomislav Terzić, R. Reinthal, M. Negrello, Damir Lelas, Dorota Sobczyńska, Ivica Puljak, Pierre Colin, E. de Oña Wilhelmi, Jelena Aleksić, A. Niedzwiecki, David Paneque, M. Barcelo, D. Galindo, Konstancja Satalecka, Michele Doro, Julian Sitarek, Daniela Hadasch, T. Toyama, Junko Kushida, P. Da Vela, J. Schlammer, Universitat de Barcelona, Aleksić, J, Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barceló, M., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Bitossi, M., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Cecchi, R., Colin, P., Colombo, E., Contreras, J. L., Corti, D., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., Deangelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Dettlaff, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Fidalgo, D., Fink, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Haberer, W., Hadasch, D., Hanabata, Y., Hayashida, M., Herrera, J., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Illa, J. M., Kadenius, V., Kellermann, H., Knoetig, M. L., Kodani, K., Konno, Y., Krause, J., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lemus, J. L., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorca, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Negrello, M., Neustroev, V., Niedzwiecki, A., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Rügamer, S., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schlammer, J., Schmidl, S., Schweizer, T., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamerra, A., Steinbring, T., Storz, J., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Tejedor, L. A., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Vogler, P., Wetteskind, H., Will, M., and Zanin, R.
Subjects: Astrofísica, Physics::Instrumentation and Detectors, MAGIC, Imaging Atmospheric Cherenkov Telescopes, Instruments, TeV astrophysics, Very High Energy Gamma Rays, Stereoscopy, Astrophysics, 01 natural sciences, law.invention, Raigs gamma, law, Overall performance, MAGIC (telescope), TeV, astrophysics, CRAB-NEBULA, PERFORMANCE, STEREO, 010303 astronomy & astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Instrument, Upgrade, ddc:540, Electrónica, Física nuclear, Astrophysics::Earth and Planetary Astrophysics, Electricidad, Astrophysics - Instrumentation and Methods for Astrophysics, TeV astrophysic, Noise (radio), Computer hardware, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Telescope, 0103 physical sciences, Very High Energy Gamma Ray, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, ta115, Telescopis, 010308 nuclear & particles physics, business.industry, Gamma rays, Cherenkov Telescope Array, Imaging Atmospheric Cherenkov Telescope, business, astro-ph.IM, Telescopes
Abstract: The MAGIC telescopes are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma. The telescopes are designed to measure Cherenkov light from air showers initiated by gamma rays in the energy regime from around 50 GeV to more than 50 TeV. The two telescopes were built in 2004 and 2009, respectively, with different cameras, triggers and readout systems. In the years 2011-2012 the MAGIC collaboration undertook a major upgrade to make the stereoscopic system uniform, improving its overall performance and easing its maintenance. In particular, the camera, the receivers and the trigger of the first telescope were replaced and the readout of the two telescopes was upgraded. This paper (Part I) describes the details of the upgrade as well as the basic performance parameters of MAGIC such as raw data treatment, dead time of the system, linearity in the electronic chain and sources of noise. In Part II, we describe the physics performance of the upgraded system., 19 pages, 18 figures, accepted by Astroparticle Physics
Published: 2016

4. Etiological Studies on Epizootic Bovine Abortion

Author: D. G. McKercher and J. Storz
Subjects: Gynecology, medicine.medical_specialty, Miyagawanella, General Veterinary, First pregnancy, Fetal tissue, Antigenic analysis, Biology, medicine.disease, Bovine abortion, medicine, Subcutaneous edema, Intrauterine infection, Epizootic
Abstract: ummary For many years, epizootic bovine abortion in California has been recognized as the cause of extensive calf losses, particularly among heifers in their first pregnancy. Fetal pathology revealed subcutaneous edema, ascites, generalized hemorrhage, and hepatopathy. Earlier workers excluded all known bacterial causes of abortion. Five viral isolates were recovered from various tissues of aborted fetuses originating from herds in widely separated areas. Cultures of bovine embryonic kidney cells and embryonated chicken eggs were employed as the means for isolation. Four isolates were studied comparatively. The behavior in chicken embryos, mice, and guinea pigs identified these isolates as members of the Psittacosis-Lymphogranuloma-Venereum group. Smears showed typical elementary bodies after staining by the Macchiavello, Castaneda, Giemsa and the Stamp technique. Electronmicroscopic observations and serological investigations confirmed these findings. A disease similar to epizootic bovine abortion was reproduced experimentally by inoculating cows in various stages of pregnancy by the intrafetal, intravenous, intramuscular, and subcutaneous exposure. After aerosal exposure of a pregnant cow the EBA-agent was recovered from the fetus at slaughter 18 days later. Oral administration of the agent and contact with infected animals were without effect. The inoculated cows aborted or gave birth to weak calves 11 to 126 days after inoculation. The virus was reisolated from uterine contents, and from the internal organs of the fetuses. Intrauterine infection of the fetuses was thus demonstrated. Cows were bred and conceived after experimentally produced abortion. The immunity of two of these cows was challenged. Virus was not recovered either from uterine contents or fetal tissues subsequently, although these animals, as well as others that recovered from experimental abortion, responded with fever to the challenge exposure. Comparative studies in one cow with Miyagawanella bovis were carried out. They revealed certain differences in the response of the cow to the agent. Intrauterine infection of the calf could be demonstrated 84 days after inoculation. It is recommended that the agent isolated from epizootic bovine abortion be considered a separate entity until exact antigenic analysis reveals its relation to other agents of this group associated with cattle infections. Zusammenfassung Atiologische Studien am epizootischen Abort der Rinder Seit vielen Jahren auftretendes Verkalben bei Rindern mit betrachtlichen Verlusten an Kalbern, besonders bei Erstlingsfarsen, wurde in Kalifornien als epizootischer Abort der Rinder bezeichnet. Fotale pathologische Veranderungen waren subkutanes Odem, Aszites, generalisierte petechiale Blutungen und Hepatopathie. Andere Bearbeiter hatten fruher die bekannten bakteriellen Ursachen von Aborten bei Rindern ausgeschlossen. Funf Virusstamme wurden von Organen abortierter Kalber, die aus geographisch weit getrennten Herden stammten, mittels embryonaler Rindernierenzellen und Huhnerembryonen isoliert. Vier Stamme wurden vergleichend untersucht. Das Verhalten im embryonierten Huhnerei, in Mausen und in Meerschweinchen sowie elektronenmikroskopische und serologische Befunde charakterisierten diese Stamme als zur Psittakose-Lymphogranuloma-Venereum-Gruppe gehorend. Eine dem epizootischen Rinderabort ahnliche Krankheit wurde experimentell erzeugt durch intrafotale, intravenose, intramuskulare und subkutane Inokulation von Kuhen in verschiedenen Trachtigkeitsstadien. Aerosolinfektion einer Kuh fuhrte zur Infektion ihres Fotus, wahrend orale Verabreichung des Virus und Kontakt mit infizierten Tieren ohne klinische Folgen blieben. Die inokulierten Tiere verkalbten oder hatten lebensschwache Kalber 11 bis 126 Tage nach der Injektion. Intrauterine Infektion wurde durch Virusisolierung vom Uterusinhalt und von den inneren Organen der Kalber nachgewiesen. Kuhe, die nach experimenteller Infektion verkalbten, wurden wieder tragend. Die Immunitat zweier dieser Tiere wurde gepruft. Virus wurde weder vom Uterusinhalt noch von fotalen Geweben isoliert, obwohl diese Tiere wie auch andere, die sich vom experimentellen Abort erholt hatten und nicht tragend waren, mit Fieber auf die Testinfektion reagierten. Vergleichende Studien an einer tragenden Kuh mit Miyagawanella bovis zeigten eine mildere Erkrankung dieser Kuh nach der Inokulation, doch konnte 84 Tage spater intrauterine Infektion ihres Kalbes nachgewiesen werden. Resume Etudes sur l'etiologie d'un avortement epizootique des bovides Un avortement observe depuis plusieurs annees chez des bovins et provoquant une perte considerable en veaux, surtout chez les primipares est appele en Californie “avortement epizootique bovin”. A l'autopsie du foetus on trouve un oedeme sous-cutane, une ascite, des hemorragies petechiales generalisees et une hepatopathie. D'autres auteurs ont exclu dans de precedents travaux les causes bacteriennes connues de l'avortement chez les bovins. Cinq souches de virus furent isolees des organes des veaux nes avant terme provenant de troupeaux geographiquement eloignes les uns des autres, au moyen de cellules renales bovines embryonales et sur des embryons de poulet. Quatre souches furent l'objet d'une etude comparee. Leur comportement dans l'oeuf embryonne de poulet, chez la souris et le cobaye ainsi que les resultats obtenus au microscope electronique et l'etude serologique caracteriserent ces souches comme appartenant au groupe psittacose-lymphogranuloma-venereum. Une maladie analogue a “l'avortement epizootique bovin” put etre reproduite experimentalement par inoculation intrafoetale, intraveineuse, intramusculaire et sous-cutanee chez des vaches a differents stades de gestation. Une infection par aerosol chez une vache provoqua l'infection du foetus tandis que l'administration orale du virus et le contact avec des animaux infectes resta sans consequences cliniques. Les animaux inocules avorterent ou donnerent naissance a des veaux debiles 11–126 jours apres l'injection. Des infections intrauterines furent mises en evidence par l'isolement du virus dans le contenu uterin et dans les visceres. Des vaches ayant avorte apres l'infection experimentale devinrent a nouveau portantes. L'immunite de deux de ces animaux fut verifiee. On ne put isoler le virus ni dans le contenu uterin ni dans les tissus du foetus, bien que ces animaux comme ceux qui avaient surmonte un avortement experimental et ne portaient pas reagirent par une poussee de fievre a l'infection test. Des etudes comparees effectuees sur une vache portante avec Miyagawanella bovis montrerent une maladie plus benigne chez cette vache apres l'inoculation, mais on put mettre en evidence 84 jours plus tard une infection intrauterine chez le veau qu'elle portait. Resumen Estudios etiologicos sobre el aborto epizootico del ganado vacuno En California se denomina aborto epizootico del ganado vacuno a un tipo de aborto en vacas que desde hace muchos anos viene ocasionado grandes perdidas entre las terneras, sobre todo en novillas. Las alteraciones patologicas fetales eran edema subcutaneo, ascitis, hemorragicas petequiales generalizadas y hepatopatia. Otros autores ya habian excluido con anterioridad las conocidas causas bacterianas de abortos en vacas. Se aislaron 5 cepas de virus de organos de terneras abortadas, procedentes de vacadas geograficamente bastante distantes entre si, mediante cultivos en celulas embrionarias de rinones vacunos y embriones de pollo. 4 cepas se estudiaron comparativamente. El comportamiento en el huevo embrionado de gallina, en ratones y en cobayas, asi como los hallazgos electonicomicroscopicos y serologicos caracterizaban a estas cepas como pertenecientes al grupo de la psitacosis-linfogranuloma venereo. Una enfermedad semejante al aborto epizootico vacuno se produjo experimentalmente por medio de inoculacion intrafetal, intravenosa, intramuscular y subcutanea de vacas en diversos estadios de gestacion. La infeccion aerosolica de una vaca condujo a la infeccion de su feto, mientras que la administracion oral del virus y el contacto con animales infectados quedaron sin consecuencias clinicas. Los animales inoculados abortaron o tenian terneras con escasa vitalidad a los 11–126 dias despues de la inyeccion. La infeccion intrauterina se comprobo mediante aislamiento del virus del contenido uterino y de ios organos internos de las terneras. Las vacas que abortaron tras la infeccion experimental, volvieron a concebir. Se comprobo la inmunidad en dos de estos animales. Del contenido uterino y de los tejidos fetales no se aislo virus alguno, aunque estos animales, al igual que otros que se habian recuperado del aborto experimental y no estaban gestantes, reaccionaban con fiebre frente a la infeccion patron. Estudios comparativos en una vaca gestante con Miyagawanella bovis presentaban una enfermedad benigna de esta vaca tras la inoculacion, pero al cabo de 84 dias se pudo identificar la infeccion intrauterina de su ternera.
Published: 2010

5. Serologische und aetiologische Studien über die intestinale Psittakose-Lymphogranuloma-Infektion der Schafe*)

Author: W. R. Thornley and J. Storz
Subjects: Gynecology, medicine.medical_specialty, Specific antibody, medicine, Antibody level, Ileal lymph node, Lymph, Enzootic abortion, Biology, Chick embryos, Surgery, Serology
Abstract: Zusammenfassung Intestinale Psittakose-Lymphogranuloma-Infektion bei Schafen, durch Isolierung von Erregern in Dottersackkulturen sich entwickelnder Huhnerembryonen diagnostiziert, wurde mit den komplementbindenden, spezifischen Antikorpern der betreffenden Tiere in Zusammenhang gebracht. Dabei hatten 20 von 29 Schafen, die Psittakoseerreger im Kot ausschieden, einen Antikorpertiter von weniger als 1:8. Der Titer der restlichen 9 Schafe schwankte zwischen 1:8 und 1:32. Andererseits vermochten in 4 Schafen nach enzootischem Abort hohe Antikorpertiter die intestinale Infektion weder zu unterdrucken noch die enterale Ausscheidung der Psittakose-Lymphogranuloma-Erreger zu verhindern. Die Psittakose-Lymphogranuloma-Erreger wurden bei 7 eingehend untersuchten, klinisch normalen Schafen aus Duodenum und den Darmabschnitten abwarts isoliert. Eines dieser Schafe beherbergte diese Erreger im Leberlymphknoten und dem Lymphknoten des Ileum, ein weiteres nur im letztgenannten Lymphknoten. Ein drittes Tier hatte neben der intestinalen Infektion auch infizierte Nieren. Die Schafe mit parenteraler Infektion hatten Antikorperstimulation. Die intestinale Psittakose-Lymphogranuloma-Infektion wurde in allen 4 untersuchten Schafherden festgestellt. Schafe im Alter von 2 Monaten bis zu 6 Jahren wurden als Ausscheider aetiologisch diagnostiziert. Einzelne Schafe schieden diese Erreger mit moglichen Unterbrechungen uber Zeitspannen von mehreren Jahren enteral aus. Summary Serological and aetiological studies on sheep with intestinal infection with psittacosis-lymphogranuloma agents Intestinal psittacosis-lymphogranuloma infection in sheep was demonstrated by isolation of the agents from faecal samples by means of developing chick embryos and was correlated with the complement-fixing, specific antibodies of these animals at the time of sampling. The antibody level was below 1:8 in 20 of 29 animals which were shedding psittacosis-lymphogranuloma agents in the faeces. The titre of the remaining 9 sheep ranged from 1:8 to 1:32. A high antibody titre, on the other hand, did not inhibit intestinal infection and faecal shedding of these agents in 4 ewes following natural cases of enzootic abortion. Among 7 clinically normal sheep which were studied aetiologically in detail, the psittacosis-lymphogranuloma agents were isolated from composite samples of digestive contents and the mucosa of the duodenum and all lower parts of the intestine. One of these sheep harboured the agent also in the hepatic and ileal lymph nodes, a second one only in the ileal lymph node, and a third sheep had infected kidneys. The sheep with parenteral infection had evidence of antibody stimulation. The intestinal psittacosis-lymphogranuloma infection was identified in all 4 herds of sheep examined. Sheep aged 2 months to 6 years were identified aetiologically as intestinal shedders. Selected sheep were found to shed those agents in the faeces during a period of 4 years with possible negative intervals. Resume Etudes serologiques et etiologiques d'une infection intestinale du Mouton par un virus du groupe psittacose-lymphogranulomatose L'infection intestinale du mouton par un virus du groupe psittacoselymphogranulomatose fut mise en parallele avec la presence d'anticorps specifiques deviant le complement chez les memes animaux. Le diagnostic de l'infection avait ete etabli par l'isolement des germes dans des cultures sur sac vitellin d'embryons de poulet en developpement. On constata a ce sujet que 20 sur 29 moutons qui eliminaient le virus dans les feces avaient un titre inferieur a 1:8. Le titre des 9 autres moutons variait entre 1:8 et 1:32. D'autre part des titres d'anticorps eleves trouves chez 4 moutons apres un avortement enzootique ne suffisaient pas a empecher l'infection intestinale ni l'elimination enterale des germes du groupe psittacose-lymphogranulomatose. Les germes du groupe psittacose-lymphogranulomatose ont ete isoles a partir du duodenum et d'autres portions du tractus intestinal de 7 moutons examines tres completement et cliniquement sains. Un de ces moutons hebergeait le virus dans les ganglions lymphatiques du foie et de l'ileum, un autre seulement dans les ganglions de l'ileum. Un troisieme animal presentait outre l'infection intestinale une infection renale. Chez les moutons atteints d'une infection parenterale on constatait une stimulation d'anticorps. L'infection intestinale par le virus du groupe psittacose-lymphogranulomatose fut constatee dans les 4 troupeaux de moutons examines. On diagnostiqua une elimination specifique de virus chez des moutons âges de 2 mois a 6 ans. Quelques moutons eliminerent ces germes par voie enterale, avec des interruptions possibles, pendant une periode s'etendant sur plusieurs annees. Resumen Estudios serologicos y etiologicos sobre la infeccion de psitacosis-linfogranuloma intestinal en las ovejas La infeccion de psitacosis-linfogranuloma intestinal en ovejas, diagnosticada mediante aislamiento de germenes en cultivos de sacos vitelinos de embriones de pollo en desarrollo, se relaciono con los anticuerpos especificos fijadores del complemento de los animales correspondientes. Con ello, 20 de 29 ovejas, las cuales eliminaron agentes de la psitacosis con el estiercol, tenia un titulo de anticuerpos menor que 1:8. El titulo de las 9 ovejas restantes oscilaba entre 1:8 y 1:32. Por otro lado, en 4 ovejas tras aborto enzootico titulos elevados de anticuerpos no lograron contener la infeccion intestinal ni impedir la difusion enterica del agente etiologico de la psitacosis-linfogranuloma. Los agentes de la psitacosis-linfogranuloma se aislaron en 7 ovejas normales, exploradas con detenimiento, a partir del duodeno y los tramos intestinales descendientes. Una de estas ovejas albergaba estos agentes etiologicos en los ganglios hepaticos y en los iliacos, mientras que otra solo en los ganglios citados en ultimo lugar. Un tercer animal tambien tenia al lado de la infeccion intestinal infectados los rinones. Las ovejas con infeccion parenteral tenian estimulacion de anticuerpos. La infeccion intestinal de psitacosis-linfogranuloma se comprobo en todos los 4 rebanos examinados. Ovejas de edades comprendidas entre 2 meses y 6 anos se diagnosticaron etiologicamente como difusores. Ciertas ovejas eliminaron estos agentes por via enteral con posibles interrupciones a lo largo de varios anos.
Published: 2010

6. Tissue Culture Adaptation and Pathogenic Properties of an Ovine Chlamydial Abortion Strain*

Author: J. Storz and V. M. Becerra
Subjects: Infectivity, Sheep, Virus Cultivation, Strain (chemistry), Adaptation, Biological, Sheep Diseases, Abortion, Veterinary, Biology, Molecular biology, Cell Line, Mice, Titer, Tissue culture, Pregnancy, Serial passage, Culture Techniques, Animals, Female, Chlamydia, Chlamydial infection, Fetal infection
Abstract: Summary The ovine chlamydial abortion strain B-577 was adapted and maintained for 101 serial passages in cell cultures. Rates of chlamydial infection of cells ranged between 8.2 and 100%, and the infectivity in developing chicken embryos of the tissue culture-adapted strain varied from 103.5 to 107.833 CELD50/0.5 ml. at different passage levels. Unexpected reductions of chlamydial infectivity occurred at the 55th, 56th and 93rd passages. The tissue culture-adapted chlamydial strain B-577 remained consistently pathogenic for chicken embryos, and caused placental and fetal infection after inoculation of pregnant ewes with material of the 54th passage in L cells. Furthermore, this strain caused an accidental laboratory infection of man after the 94th passage in tissue culture. These facts indicate that this chlamydial strain did not become attenuated during serial passage in culture cells. Zusammenfassung Pathogenitat eines Chlamydienstammes vom Schafabort nach Adaption an Gewebekulturen Der Chlamydienstamm B 577 vom Schafabort wurde an L-Zellen adaptiert und in 101 Passagen darin weitergezuchtet. Wahrend dieser Passagen schwankte die Rate infizierter Zellen zwischen 8,2 und 100%. Der Infektionstiter in Huhnerembryonen lag zwischen 10−3,5 und 10−7,833 LD50. In der 55., 56. und 93. Gewebekulturpassage waren die Titer am niedrigsten. Die Pathogenitat des Stammes fur die Huhnerembryonen blieb unverandert. Nach der 54. L-Zellen-Passage infizierte dieser Stamm Plazenta und Fotus in tragenden Schafen. Auserdem verursachte der Stamm B 577 wahrend der 94. Passage eine Augeninfektion beim Menschen. Diese Befunde weisen darauf hin, das der Chlamydienstamm B 577 durch Passagen in L-Zellen nicht attenuiert wurde. Resume Pathogenite d'une souche de Chlamydia, isolee lors d'une avortement chez le mouton, apres une adaptation aux cultures de tissue On a adapte aux cellules-L la souche Chlamydia B 577 d'un avortement de mouton et on l'a reproduite lors de 101 passages. Le taux de cellules infectees alla de 8,2 a 100% durant ces passages. Le titre infectieux se situa chez l'embryon de poulet entre 10−3,5 et 10−7,833 LD50. Les titres furent les plus bas lors du 55e, 56e et 93e passage en culture de tissu. La pathogenite de la souche pour l'embryon de poulet resta inchangee. Cette souche infecta le placenta et le foetus de brebis gravides apres le 54e passage sur cellules-L. La souche B 577 provoqua en outre une infection oculaire chez l'homme pendant le 94e passage. Ces resultats montrent que la souche Chlamydia B 577 n'a pas ete attenuee par des passages sur cellules-L. Resumen Patogeneidad de una estirpe de clamidios del aborto ovino tras adaptacion a cultivos histicos Se adapto la estirpe de clamidios B 577 del aborto ovino a celulas L y se siguio cultivando en ellas durante 101 pases. A lo largo de estos pases oscilaba la tasa de celulas infectadas entre 8,2 y 100%. El titulo de infeccion en los embriones de pollo se hallaba entre 10−3,5 y 10−7,833 DL50. Los titulos eran minimos en los pases 55°, 56° y 93° por cultivo histico. La patogeneidad de la estirpe permanecio inalterada para los embriones de pollo. Tras el pase 54° por celulas infectaba esta estirpe la placenta y feto en ovejas gestantes. Ademas ocasiono la estirpe B 577 durante el pase 94° una infeccion ocular en una persona. Estos hallazgos indican que la estirpe de clamidios B 577 no fue atenuada mediante los pases por celulas L.
Published: 2010

7. Early Events inVibrio fetusInfection of Ewes*

Author: Marriott Me, Miner Ml, and J. Storz
Subjects: Gynecology, medicine.medical_specialty, medicine, Biology, Surgery
Abstract: Summary The dynamics of the bacteremic phase of vibrio infection of non-pregnant and pregnant ewes was investigated using vibrio organisms which differed distinctly in catalase activity, hydrogen sulfide production and cellular morphology. The following facts emerged: 1 The rate of clearance of vibrio organisms from the blood is the same in pregnant and non-pregnant ewes. The rate is determined by the morphologic characteristics of the vibrio cells. Coccoid Vibrio fetus are cleared relatively slowly from the blood while typical comma-shaped cells are eliminated at a significantly faster rate. The catalase activity of an organism and its ability to produce hydrogen sulfide do not influence the rates of clearance. 2 The coccoid Vibrio fetus strain, which remained for a long period in the blood stream, was lethal to ewes 5½ to 12 hours after inoculation. The animals developed a shock-like syndrome and died. Generalized thrombosis was observed in these ewes. 3 A duration of detectable bacteremia of as little as 15 minutes was sufficient to establish uterine infection in pregnant ewes. Catalase activity seemed to be a determining factor in the establishment of uterine infection. 4 Gall bladder infection with Vibrio fetus was observed after bacteremia. Vibrio fetus was also present in the intestinal tract in cases where gall bladder infection had been established. Zusammenfassung Uber Ereignisse im Fruhstadium der Vibrio fetus-Infektion bei Mutterschafen Die Dynamik der bakteriamischen Phase der Vibrioinfektion tragender und nichttragender Schafe wurde untersucht. Verwendet wurden Vibrionen, die sich eindeutig voneinander in ihrer Katalase-Aktivitat, ihrer Schwefelwasserstoffproduktion und ihrer Zellmorphologie unterschieden. Folgende Befunde wurden erhoben: 1 Die Geschwindigkeit, mit der Vibrionen aus dem Blut eliminiert werden, ist bei tragenden und nichttragenden Schafen die gleiche und hangt anscheinend von morphologischen Eigenschaften der Vibrionen ab. Coccoide Vibrio fetus-Organismen werden langsam aus dem Blut eliminiert, wahrend typisch kommaformige Vibrionen signifikant schneller aus dem Blut beseitigt werden. Die Katalase-Aktivitat der Erreger und Befahigung zur Schwefelwasserstoffbildung beeinflussen die Ausscheidungsrate nicht. 2 Der hier verwendete coccoide Vibrio fetus-Stamm verursacht 5½ bis 12 Stunden nach intravenoser Inokulation ein todlich verlaufendes, schockartiges Syndrom. Bei diesen Schafen wird eine generalisierte Thrombose fest-gestellt. 3 Eine fur nur 15 Minuten nachweisbare Bakteriamie fuhrt bei tragenden Schafen zur uterinen Infektion. Hierfur erscheint die Katalaseaktivitat bestimmend zu sein. 4 Nach der bakteriamischen Phase ist eine Infektion der Gallenblase mit Vibrio fetus feststellbar. In diesen Fallen last sich Vibrio fetus auch im Intestinaltrakt nachweisen. Resume Phenomenes accompagnant le stade precoce de l'infection par «vibrio fetus» chez les moutons femelles L'examen a porte sur la dynamique de la phase bacteriemique de l'infection par vibrions chez les moutons gravides et ceux qui ne le sont pas. Les vibrions utilises se distinguaient nettement les uns des autres par leur activite catalasique, leur production d'hydrogene sulfure et leur morphologie cellulaire. Les constats suivants ont ete enregistres: 1 La rapidite avec laquelle les vibrions sont elimines du sang est la meme chez les moutons gravides et ceux qui ne le sont pas et semble dependre des proprietes morphologiques des vibrions. Les vibrions de forme coccoide sont elimines lentement du sang tandis que ceux qui sont de forme nettement en virgule disparaissent beaucoup plus rapidement du sang. L'activite catalasique des microorganismes et leur faculte de produire de l'hydrogene sulfure n'influence en rien leur taux d'elimination. 2 La souche de vibrions coccoides utilises ici provoque 5½ a 12 heures apres l'inoculation intraveineuse, un syndrome de choc avec issue mortelle. Chez ces moutons on constate une trombose generalisee. 3 Une bacteriemie decelable pendant 15 minutes seulement entraine chez les moutons gravides une infection uterine. A cet egard, l'activite catalasique semble etre determinante. 4 Apres la phase bacteriemique, on peut constater une infection de la vesicule biliaire par «vibrio fetus». Dans ces cas-la, le microorganisme peut egalement etre identifie dans le tractus intestinal. Resumen Sobre sucesos en el estadio precoz de la infeccion por Vibrio fetus en ovejas madres Se estudio la dinamica de la fase bacteriemica de la vibrioinfeccion en ovejas prenadas y vacias. Utilizaronse vibriones que se diferenciaban con evidencia entre si en su actividad catalasica, su produccion de acido sulfhidrico y su morfologia celular. Se evidenciaron los hallazgos siguientes: 1 La velocidad, con la que se eliminan los vibriones de la sangre, es la misma en ovejas gravidas que vacias, dependiendo al parecer de las propiedades morfologicas de los vibriones. Los organismos Vibrio fetus cocoides se eliminan con lentitud de la sangre, mientras que los vibriones en forma tipica de coma se eliminan del torrente sanguineo con una velocidad significativa mucho mayor. La actividad catalasica de los agentes etiologicos y la capacidad de formacion de acido sulfhidrico no influencian la cuota de eliminacion. 2 La cepa cocoide de Vibrio fetus aqui empleada ocasiona entre las 5½ y 12 horas a contar de la inoculacion intravenosa un sindrome en forma de choque, de curso mortal. En estas ovejas se comprobo la existencia de una trombosis generalizada. 3 La bacteriemia solo identificable durante 15 minutos conduce en ovejas prenadas a la infeccion uterina. A este respecto parece ser decisiva la actividad catalasica. 4 Tras la fase bacteriemica se puede comprobar una infeccion de la vesicula biliar con Vibrio fetus. En estos casos tambien se puede identificar Vibrio fetus en el tracto intestinal.
Published: 2010

8. Enterovirusinfektion und Immunität vor und nach der Geburt bei Kühen und Kälbern*

Author: G. S. Warren, J. Storz, and A. K. Eugster
Subjects: Gynecology, Titer, medicine.medical_specialty, business.industry, Immunity, Immunology, Medicine, Colostrum, Enterovirus, Antibody level, business, medicine.disease_cause, Antibody formation
Abstract: Zusammenfassung Der Verlauf einer naturlich auftretenden Enterovirusinfektion in einer Gruppe von tragenden Kuhen wurde untersucht. Die Kuhe waren zu Beginn der Untersuchung 2 bis 4 Monate tragend und schieden Enteroviren im Kot aus. Enteroviren wurden wahrend der Trachtigkeit fur eine Zeitspanne von mindestens 86 Tagen ausgeschieden. Nach der Geburt schieden 2 Kuhe erneut Enteroviren aus. Die Trachtigkeit verlief normal, und die Kalber hatten bei der Geburt keine Enterovirusinfektion. Funf der 8 Versuchskuhe bildeten Antikorper gegen die intestinale Enterovirusinfektion, doch fielen die Neutralisationstiter im letzten Trimester der Trachtigkeit. Die restlichen 3 Kuhe bildeten keine neutralisierenden Antikorper als Folge der Infektion. Nach der Geburt wurde bei allen Tieren ein Anstieg des Neutralisationstiters festgestellt. Die Antikorpertiter im Kolostrum entsprachen den Serumtitern am Tage der Geburt. Die Kalber hatten vor der Kolostrumfutterung keine Antikorper. Die Menge des verabreichten Kolostrums bestimmte den Serumantikorperspiegel der Kalber. Summary Enterovirus infection and immunity before and after birth in cows and calves The dynamics of the enterovirus infection were studied in 8 pregnant cows. At the beginning of the investigations the cows were 2 to 4 months pregnant and all were shedding enteroviruses in the feces as a result of a natural infection. During gestation this infection persisted for at least 86 days. Two cows excreted enteroviruses again after parturition in their feces. Gestation was normal and the calves were free of enteroviruses at birth. Five of the cows formed neutralizing antibodies against the enteroviruses. Their antibody titers decreased markedly during the last trimester of gestation. The remaining 3 cows did not form neutralizing antibodies to the enterovirus infection. A rise in neutralizing antibodies occurred in all cows following parturition. The antibody titers in the colostrum corresponded with the serum titers at the time of birth. No neutralizing antibodies were detected in the sera of calves before the feeding of colostrum. The amount of the colostrum given determined the subsequent antibody levels in the serum of the calves. Resume Infection a enterovirus et immunite avant et apres la naissance chez les vaches et les veaux On etudie le developpement d'une infection naturelle a enterovirus sur un groupe de vaches portantes. Au debut des examens, les vaches se trouvaient vers 2 a 4 mois de gestation et excretaient des enterovirus par les matieres fecales. L'elimination des enterovirus se poursuivait pendant une duree d'au moins 86 jours en cours de gestation. Apres la naissance, deux vaches recommencerent a eliminer des enterovirus. La gestation s'est deroulee normalement naissance. Cinq des huit vaches d'experience formerent des anticorps contre une infection intestinale a enterovirus, mais les titres de neutralisation diminuerent au cours du dernier trimestre de la gestation. Les trois autres vaches ne formerent pas d'anticorps neutralisants a la suite de l'infection. Apres la naissance, on observe chez tous les animaux une augmentation du titre de neutralisation. Les titres des anticorps du colostrum correspondent au titre serique du jour de la naissance. Les veaux ne possedent pas d'anticorps avant l'ingestion de colostrum. La quantite de colostrum administree determine le niveau des anticorps seriques du veau. Resumen Infeccion enterovirosica e inmunidad antes y despues del parto en vacas y en los terneros Se estudio el curso de una infeccion enterovirosica natural en un grupo de vacas gestantes. Las vacas llevaban, en el comienzo del examen, de 2 a 4 meses de prenez y eliminaban enterovirus con el estiercol. Durante la gestacion fueron eliminados enterovirus por un periodo minimo de tiempo de 86 dias. Tras el parto, 2 vacas eliminaron de nuevo enterovirus. Cada gestacion transmomento del parto. Cinco de las 8 vacas de ensayo formaron anticuerpos frente a la infeccion enterovirosica intestinal, aunque los titulos de neutralizacion disminuyesen de forma apreciable en el trimestre ultimo de gestacion. Las tres vacas restantes no formaron anticuerpos neutralizantes como consecuencia de la infeccion. Despues de acontecido el parto, en todas las hembras se constato el aumento del titulo de neutralizacion. Los titulos de anticuerpos en el calostro correspondian a los titulos sericos en el dia del parto. Los terneros no tenian anticuerpos antes de administrarseles el calostro. La cantidad administrada de calostro determianba el nivel de seroanticuerpos en los terneros.
Published: 2010

9. Light and Ultrastructural Pathologic Changes in Intestinal Coronavirus Infection of Newborn Calves*

Author: J. Storz and A. M. Doughri
Subjects: Lamina propria, Coronaviridae Infections, Small intestinal wall, Cattle Diseases, Virus multiplication, Biology, medicine.disease_cause, Molecular biology, Decreased height, Intestinal Diseases, Microscopy, Electron, medicine.anatomical_structure, Animals, Newborn, Recien nacido, Cytology, medicine, Ultrastructure, Animals, Original Article, Cattle, Coronavirus
Abstract: Summary Seven conventional newborn calves were inoculated orally with the coronavirus strain LY-138, originally recovered from naturally-infected diarrheic calves. All calves developed diarrhea during the first 24 h after inoculation. The presence and excretion of virus was monitored by electron microscopy. Grossly, the changes were subtle and not striking. The intestinal tract was distended and contained a yellow clear fluid. The small intestinal wall was thin and transparent. Histologic changes were characterized by atrophy and fusion of the villi, decreased height and vacuolation of the intestinal epithelial cells, by a reduced number of goblet cells, crypt hypertrophy and dilatation, and by edema and increased cellularity of the lamina propria mucosae. Ultrastructurally the viral agent infected the intestinal absorptive epithelial cells, undifferentiated epithelial cells and goblet cells of the villi, and occasionally fibroblasts and endothelial cells of the lamina propria mucosae. Morphologic evidence indicated that virus multiplication occurred only in the cytoplasm of infected cells. The rough and smooth endoplasmic reticulum became dilated, and electron-dense, granulo-fibrillar material filled their cysternae to form smooth membrane-bounded viral factories in the supranuclear cytoplasm of infected intestinal epithelial cells. Ultrastructural cytologic changes in this viral infection consisted of dilation of the endoplasmic reticulum network, cellular ribosome depletion, extensive endoplasmic vacuolation and vesiculation of Golgi elements of intestinal epithelial cells, swelling and degeneration of mitochondria, loss of normal nuclear polarity with pyknosis and karyolysis of the nuclei, loss of cytoplasmic matrix, and a broad spectrum of pathologic changes involving the microvilli and terminal web. Zusammenfassung Lichtmikroskopische und Ultrastrukturelle pathologische Veranderungen bei intestinaler Coronavirusinfektion neugeborener Kalber Sieben konventionelle neugeborene Kalber wurden oral mit dem Coronavirus-Stamm LY-138, der ursprunglich von naturlich infizierten Kalbern mit Diarrhoe stammt, infiziert. Alle Kalber entwickelten Durchfall wahrend der ersten 24 Stunden nach Inokulation. Vorhandensein und die Ausscheidung des Virus wurden elektronenoptisch verfolgt. Sichtbare Veranderungen waren gering und wenig auffallend. Der Darmtrakt war erweitert und enthielt eine gelbe, klare Flussigkeit. Die Dunndarmwand war dunn und durchscheinend. Histologische Veranderungen waren charakterisiert durch Atrophie und Verschmelzung der Zotten, verminderte Hohe und Vakuolisierung der intestinalen Epithelzellen, durch eine reduzierte Anzahl von Gobletzellen, Kryptenhypertrophie und -erweiterung, sowie Odematisierung und erhohte Zellularitat der lamina propria mucusae. Ultrastrukturell infizierte das Virus die intestinalen absorptiven Epithelzellen, nichtdifferenzierte Epithelzellen und Gobletzellen der Zotten, und gelegentlich Fibroblasten sowie Endothelzellen der Lamina propria mucosae. Die morphologischen Veranderungen weisen darauf hin, das die Virusvermehrung nur im Zytoplasma infizierter Zellen stattfand. Das rauhe und glatte endoplasmatische Retikulum war erweitert, und elektronendichtes, granulo-fibrillares Material fullte die Zisternen aus, die feine Membran-gebundene Virusvermehrungsfabriken in dem supranuklearen Zytoplasmabereich infizierter intestinaler Epithelzellen bildeten. Ultrastrukturelle zytologische Veranderungen bestanden bei dieser Virusinfektion aus Erweiterung des endoplasmatischen Retikulumnetzwerks, zellularem Ribosomenverlust, extensiver endoplasmatischer Vakuolisierung der Golgielemente der intestinalen Epithelzellen, Schwellung und Degeneration von Mitochondrien, Verlust der normalen nuklearen Polaritat mit Pyknose und Karyolyse der Zellkerne, Verlust der Zytoplasmamatrix, und aus einem breiten Spektrum pathologischer Veranderungen an den Mikrozotten und der terminalen Netzstruktur. Resume Lesions pathologiques ultrastructurelles et au microscope optique lors d'infection intestinale a Coronavirus chez des veaux nouveau-nes Sept veaux nouveau-nes conventionnels ont ete infectes oralement par la souche LY-138 de Coronavirus, isolee precedement chez des veaux naturellement infectes presentant une diarrhee. Tous les veaux developperent une diarrhee durant les premieres 24 heures suivant l'inovulation. La presence et la secretion du virus ont ete suivies au microscope electronique. Les lesions apparentes furent faibles et peu apparentes. Le tractus digestif fut elargi et contenait un liquide jaune et clair. La paroi de l'intestin grele etait mince et transparente. Les lesions histologiques furent caracterisees par une atrophie et une fusion des villi, une hauteur diminuee et une vacuolisation des cellules epitheliales de l'intestin, par un nombre reduit des cellules caliciformes, une hypertrophie et un elargissement des cryptes ainsi qu'un oedeme et un nombre de cellules augmente de Lamina propria mucosae. Le virus a infecte ultrastructurellement les cellules epitheliales absorbantes de l'intestin, des cellules epitheliales non differenciees et des cellules caliciformes des villi, de temps en temps des fibroblastes et des cellules endotheliales de Lamina propria mucosae. Les lesions morphologiques ont montre que la multiplication du virus n'avait lieu que dans le cytoplasme des cellules infectees. Le Reticulum endoplasmique grossier et fin fut elargi et un materiel granuleux et fibrillaire remplissait les citernes qui formaient de fines regions de replication virale liees a la membrane dans le voisinage cytoplasmique supranucleaire des cellules epitheliales infectees de l'intestin. Les lesions cytologiques ultrastructurelles lors de cette infection virale consisterent en un elargissement du reseau endoplasmique, une perte des ribosomes cellulaires, une vacuolisation endoplasmique extensive des elements de Golgi dans les cellules epitheliales de l'intestin, une enflure et une degenerescence des mitochondries, une perte de la polarite nucleaire normale avec une picnose et une carylolyse des noyaux cellulaires, une perte de la matrice cytoplasmique et un large eventail de lesions pathologiques des microvilli et des tissus terminaux. Resumen Modificaciones patologicas fotomicroscopicas y ultraestructurales en la infeccion intestinal de terneros recien nacidos por virus Corona Se infectaron por via oral siete terneros convencionales con la estirpe de virus Corona LY-138, la cual es originaria de terneros, infectados naturalmente, con diarrea. Todos los terneros manifestaban diarrea durante las 24 horas primeras despues de la inoculacion. Se seguia electronicoopticamente la presencia y eliminacion de virus. Las modificaciones visibles eran escasas y se destacaban poco. El tracto intestinal se hallaba dilatado, conteniendo un liquido amarillo claro. La pared del intestino delgado era tenue y translucida. Las modificaciones histopatologicas se caracterizaban por atrofia y soldadura de las villosidades, altura reducida y vacuolizacion de las celulas epiteliales intestinales, por una cantidad reducida de celulas caliciformes, hipertrofia y ensanchamiento de las criptas, y por edematizacion y celularidad aumentada de la lamina propia mucosa. El virus infectaba ultraestructuralmente las celulas epiteliales intestinales absortivas, celulas epiteliales no diferenciadas y celulas caliciformes de las villosidades, y, en ocasiones fibroblastos y celulas endoteliales de la lamina propia mucosa. Las modificaciones morfologicas senalan que la multiplicacion de virus solo tuvo lugar en el citoplasma de las celulas infectadas. El reticulo endoplasmatico basto y fino se hallaba dilatado y material granulosofibrilar, opaco a los electrones, ocupaba las cisternas, las cuales formaban lugares finos de replicacion antiviral, ligados a las membranas en el ambito citoplasmatico supranuclear de celulas epiteliales intestinales infectadas. Las modificaciones citologicas ultraestructurales consistian en esta infeccion a virus en dilatacion del reticulo endoplasmatico, perdida celular de ribosomas, vacuolizacion endoplasmatica extensiva de los elementos de Golgi de las celulas epiteliales intestinales, tumefaccion y degeneracion de mitocondrias, perdida de la polaridad nuclear normal con picnosis y cariolisis de los nucleos celulares, perdida de la matriz citoplasmatica, y en un espectro amplio de modificaciones patologicas en las microvillosidades y tejidos terminales.
Published: 2010

10. A COGNITIVE MODEL OF IMITATIVE DEVELOPMENT IN HUMANS AND MACHINES

Author: Joshua J. Storz, Aaron P. Shon, Andrew N. Meltzoff, and Rajesh P. N. Rao
Subjects: Cognitive model, ComputingMethodologies_SIMULATIONANDMODELING, business.industry, Computer science, Mechanical Engineering, media_common.quotation_subject, ComputingMilieux_PERSONALCOMPUTING, Robotics, Bayesian inference, ComputingMethodologies_ARTIFICIALINTELLIGENCE, Action (philosophy), Artificial Intelligence, Robot, Artificial intelligence, Cognitive imitation, Imitation, business, Humanoid robot, media_common
Abstract: Several algorithms and models have recently been proposed for imitation learning in humans and robots. However, few proposals offer a framework for imitation learning in noisy stochastic environments where the imitator must learn and act under real-time performance constraints. We present a novel probabilistic framework for imitation learning in stochastic environments with unreliable sensors. Bayesian algorithms, based on Meltzoff and Moore's AIM hypothesis for action imitation, implement the core of an imitation learning framework. Our algorithms are computationally efficient, allowing real-time learning and imitation in an active stereo vision robotic head and on a humanoid robot. We present simulated and real-world robotics results demonstrating the viability of our approach. We conclude by advocating a research agenda that promotes interaction between cognitive and robotic studies of imitation.
Published: 2007

11. Detection of VHE γ-rays from HESS J0632+057 during the 2011 February X-ray outburst with the MAGIC Telescopes

Author: The MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. A. Alvarez(Universidad Complutense, E-28040 Madrid, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Asensio(Universidad Complutense, E-28040 Madrid, Spain), M. Backes(Technische Universität Dortmund, D-44221 Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), D. Bastieri(Università di Padova and INFN, I-35131 Padova, Italy), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Łódź, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Boller(ETH Zurich, CH-8093 Zurich, Switzerland), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, D-80805 München, Germany), V. Bosch-Ramon(Universitat de Barcelona), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), A. Cañellas(Universitat de Barcelona), E. Carmona(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), L. Cossio(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), E. De Cea del Pozo(Institut de Ciències de l'Espai), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), A. Diago Ortega(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(ETH Zurich, CH-8093 Zurich, Switzerland), M. Doro(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), D. Hadasch(Institut de Ciències de l'Espai), D. Häfner(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), B. Huber(ETH Zurich, CH-8093 Zurich, Switzerland), F. Jankowski(Deutsches Elektronen-Synchrotron), T. Jogler(Max-Planck-Institut für Physik, D-80805 München, Germany), V. Kadenius(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Klepser(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), T. Krähenbühl(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), S. Lombardi(Università di Padova and INFN, I-35131 Padova, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), A. Niedzwiecki(University of Łódź, PL-90236 Lodz, Poland), D. Nieto(Universidad Complutense, E-28040 Madrid, Spain), K. Nilsson(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), D. Paneque(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), S. Pardo(Universidad Complutense, E-28040 Madrid, Spain), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. A. Perez-Torres(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), M. Pilia(Università dell'Insubria, Como, I-22100 Como, Italy), J. Pochon(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), I. Puerto Gimenez(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. Reinthal(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, E-08010 Barcelona, Spain)), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Y. Saito(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Łódź, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, I-00136 Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), B. Steinke(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), N. Strah(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland), H. Takami(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(ICREA, E-08010 Barcelona, Spain)), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), Q. Weitzel(ETH Zurich, CH-8093 Zurich, Switzerland), V. Zabalza(Universitat de Barcelona), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), now at(EPFL), (EPFL), Ecole polytechnique fédérale de Lausanne(EPFL), Lausanne(EPFL), Switzerland(CIEMAT), supported by INFN Padova(CIEMAT), now at(CIEMAT), (CIEMAT), Centro de Investigaciones Energéticas(CIEMAT), Medioambientales y Tecnológicas(CIEMAT), Madrid(FINCA), Spain(FINCA), now at(FINCA), (FINCA), KIPAC(FINCA), SLAC National Accelerator Laboratory(FINCA), USA(FINCA), Finnish Centre for Astronomy with ESO(FINCA), University of Turku(), and Finland)()
Subjects: High energy, Be star, Astrophysics::High Energy Astrophysical Phenomena, binaries: general, gamma rays: general, stars: individual (MWC 148), X-rays: binaries, X-rays: individual (HESS J0632+057), Astrophysics, Compact star, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, Raigs gamma, 0103 physical sciences, 010303 astronomy & astrophysics, Estels binaris de raigs X, Physics, astro-ph.HE, COUNTERPART, 010308 nuclear & particles physics, Gamma rays, X-ray, Gamma ray, Astronomy and Astrophysics, TEV BINARY, EMISSION, DISCOVERY, VARIABILITY, X-ray binaries, 13. Climate action, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The very high energy (VHE) \gamma-ray source HESS J0632+057 has recently been confirmed to be a \gamma-ray binary. The optical counterpart is the Be star MWC 148, and a compact object of unknown nature orbits it every ~321 d with a high eccentricity of ~0.8. We monitored HESS J0632+057 with the stereoscopic MAGIC telescopes from 2010 October to 2011 March and detected significant VHE \gamma-ray emission during 2011 February, when the system exhibited an X-ray outburst. We find no \gamma-ray signal in the other observation periods when the system did not show increased X-ray flux. Thus HESS J0632+057 exhibits \gamma-ray variability on timescales of the order of one to two months possibly linked to the X-ray outburst that takes place about 100 days after the periastron passage. Furthermore our measurements provide for the first time the \gamma-ray spectrum down to about 140 GeV and indicate no turnover of the spectrum at low energies. We compare the properties of HESS J0632+057 with the similar \gamma-ray binary LS I +61 303, and discuss on the possible origin of the multi-wavelength emission of the source, Comment: 6 pages and 3 figures, submitted, corresponding authors T. Jogler and P. Munar-Adrover
Published: 2015

12. Very high energy gamma-ray observation of the peculiar transient event Swift J1644+57 with the MAGIC telescopes and AGILE

Author: Abelardo Moralejo, Ivica Puljak, Pierre Colin, T. Krähenbühl, L. A. Antonelli, K. Berger, E. Colombo, S. Bonnefoy, Giacomo Bonnoli, R. Mirzoyan, D. Eisenacher, E. Carmona, Markus Garczarczyk, Fabio Zandanel, Ralph Bock, L. O. Takalo, Nina Nowak, Natalia Lewandowska, Mosè Mariotti, M. Doert, Michael Backes, M. Asensio, Takashi Saito, Juan Abel Barrio, K. Mallot, Fabrizio Tavecchio, R. J. García López, Saverio Lombardi, D. Borla Tridon, Ll. Font, F. Jankowski, C. Schultz, V. Scapin, Reiko Orito, S. Partini, Francesco Longo, Julian Sitarek, Kari Nilsson, M. Salvati, R. Reinthal, J. Hose, Dominik Elsaesser, A. Sillanpää, Steven N. Shore, A. La Barbera, Emanuele Paolo Farina, U. Barres de Almeida, Dario Hrupec, Nikola Godinovic, Benito Marcote, Daniela Hadasch, Felix Spanier, P. G. Prada Moroni, J. Moldón, Christian Fruck, T. Toyama, Nijil Mankuzhiyil, W. Idec, Damir Lelas, Patrick Vogler, P. Munar-Adrover, D. Garrido Terrats, Ignasi Reichardt, O. Tibolla, V. Scalzotto, C. Pittori, M. L. Knoetig, Tomislav Terzić, M. Palatiello, Massimo Persic, J. Krause, Dorota Sobczyńska, B. De Lotto, M. A. Lopez, Hajime Takami, Martin Makariev, Oscar Blanch, Riccardo Paoletti, I. Snidaric, Marc Ribó, D. Dominis Prester, Aaron Dominguez, M. V. Fonseca, G. Maneva, Fabrizio Lucarelli, Francesco Dazzi, R. Zanin, A. Saggion, Adrian Biland, J. Kushida, G. De Caneva, S. Klepser, E. Prandini, Jose Luis Contreras, Francisco Prada, Juan Cortina, J. M. Paredes, Antonio Stamerra, S. Spiro, E. Lorenz, A. De Angelis, Victor Stamatescu, Aldo Treves, J. Rico, Thomas Bretz, B. Steinke, J. Masbou, A. Hadamek, J. Storz, Diego F. Torres, M. I. Martínez, Wolfgang Rhode, J. Becerra González, P. Da Vela, A. Boller, L. Cossio, Daniel Ferenc, Mario Meucci, Artemio Herrero, K. Saito, F. Verrecchia, Q. Weitzel, Tihomir Surić, D. Carreto Fidalgo, V. Kadenius, S. Paiano, Karl Mannheim, C. Delgado Mendez, S. R. Gozzini, Gianluca Giavitto, A. González Muñoz, Daniela Dorner, M. Gaug, Elisa Bernardini, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Nakajima, Jose Miguel Miranda, L. Maraschi, Elina Lindfors, Daniel Mazin, Konstancja Satalecka, P. Temnikov, Michele Doro, Shan Sun, Jelena Aleksić, A. Niedzwiecki, David Paneque, Stefano Covino, T. Schweizer, I. Lozano, D. Tescaro, Masahiro Teshima, Robert Wagner, M. Uellenbeck, P. Antoranz, UAM. Departamento de Física Teórica, J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, J., Becerra González, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, E., Farina, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, W., Idec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, and F., Verrecchia
Subjects: Swift Gamma-Ray Burst Mission, active [Galaxies], Radiation mechanisms: non-thermal, TIDAL DISRUPTION, Astrophysics::High Energy Astrophysical Phenomena, radiation mechanisms: non-thermal, galaxies: active, Gamma rays: general, general [Gamma rays], Astrophysics, 01 natural sciences, Tidal disruption event, NEARBY, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Zenith, Physics, gamma rays: general, non-thermal [Radiation mechanisms], STAR, 010308 nuclear & particles physics, Gamma ray, Astronomy, Física, MASSIVE BLACK-HOLE, GALAXIES, BLAZARS, Astronomy and Astrophysics, Galaxies: active, Galaxy, 13. Climate action, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: Astronomy and astrophysics 552(A112 ), 1-6 (2013). doi:10.1051/0004-6361/201321197, Context. On March 28, 2011, the BAT instrument on board the Swift satellite detected a new transient event that in the very beginning was classified as a gamma ray burst (GRB). However, the unusual X-ray flaring activity observed from a few hours up to days after the onset of the event made a different nature seem to be more likely. The long-lasting activity in the X-ray band, followed by a delayed brightening of the source in infrared and radio activity, suggested that it is better interpreted as a tidal disruption event that triggered a dormant black hole in the nucleus of the host galaxy and generated an outflowing jet of relativistic matter. Aims. Detecting a very high energy emission component from such a peculiar object would be enable us to constrain the dynamic of the emission processes and the jet model by providing information on the Doppler factor of the relativistic ejecta. Methods. The MAGIC telescopes observed the peculiar source Swift J1644+57 during the flaring phase, searching for gamma-ray emission at very-high energy (VHE, E > 100 GeV), starting observations nearly 2.5 days after the trigger time. MAGIC collected a total of 28 h of dataduring 12 nights. The source was observed in wobble mode during dark time at a mean zenith angle of 35◦. Data were reduced using a new image-cleaning algorithm, the so-called sum-cleaning, which guarantees a better noise suppression and a lower energy threshold than the standard analysis procedure. Results. No clear evidence for emission above the energy threshold of 100 GeV was found. MAGIC observations permit one to constrain theemission from the source down to 100 GeV, which favors models that explain the observed lower energy variable emission. Data analysis of simultaneous observations from AGILE, Fermi and VERITAS also provide negative detection, which additionally constrain the self-Compton emission component., Published by EDP Sciences, Les Ulis
Published: 2013

13. The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, Italy), M. Asensio(Universidad Complutense, Spain), M. Backes(Technische Universität Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, München, Germany), J. A. Barrio(Universidad Complutense, Spain), W. Bednarek(University of Łódź, Poland), K. Berger(Inst. de Astrofísica de Canarias, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, Spain), R. K. Bock(Max-Planck-Institut für Physik, München, Germany), A. Boller(ETH Zurich, Switzerland), S. Bonnefoy(Universidad Complutense, Spain), G. Bonnoli(INAF National Institute for Astrophysics, Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, München, Germany), T. Bretz(Universität Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), A. Carosi(INAF National Institute for Astrophysics, Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. L. Contreras(Universidad Complutense, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, Spain), L. Cossio(Università di Udine, and INFN Trieste, Italy), S. Covino(INAF National Institute for Astrophysics, Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, Italy), F. Dazzi(Università di Udine, and INFN Trieste, Italy), A. De Angelis(Università di Udine, and INFN Trieste, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), M. Doert(Technische Universität Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Dorner(Universität Würzburg, Germany), M. Doro(Universitat Autònoma de Barcelona, Spain), D. Eisenacher(Universität Würzburg, Germany), D. Elsaesser(Universität Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), M. V. Fonseca(Universidad Complutense, Spain), L. Font(Universitat Autònoma de Barcelona, Spain), C. Fruck(Max-Planck-Institut für Physik, München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, Spain), M. Gaug(Universitat Autònoma de Barcelona, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. Hose(Max-Planck-Institut für Physik, München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), F. Jankowski(Deutsches Elektronen-Synchrotron), V. Kadenius(Tuorla Observatory, University of Turku, Finland), S. Klepser(IFAE, Edifici Cn., Campus UAB, Spain), M. L. Knoetig(Max-Planck-Institut für Physik, München, Germany), T. Krähenbühl(ETH Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, Italy), N. Lewandowska(Universität Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, Finland), S. Lombardi(INAF National Institute for Astrophysics, Rome, Italy), M. López(Universidad Complutense, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, Spain), E. Lorenz(Max-Planck-Institut für Physik, München, Germany), I. Lozano(Universidad Complutense, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, Italy), K. Mannheim(Universität Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, Spain), J. Masbou(Università di Padova and INFN Padova, Italy), D. Mazin(Max-Planck-Institut für Physik, München, Germany), M. Meucci(Università di Siena, and INFN Pisa, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Max-Planck-Institut für Physik, München, Germany), A. Niedzwiecki(University of Łódź, Poland), D. Nieto(Universidad Complutense, Spain), K. Nilsson(Tuorla Observatory, University of Turku, Finland), N. Nowak(Max-Planck-Institut für Physik, München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, Italy), D. Paneque(Max-Planck-Institut für Physik, München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, Italy), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, Italy), M. Persic(Università di Udine, and INFN Trieste, Italy), M. Pilia(Università dell'Insubria, Como, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, Italy), E. Prandini(Università di Padova and INFN Padova, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, Spain), R. Reinthal(Tuorla Observatory, University of Turku, Finland), W. Rhode(Technische Universität Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, Barcelona, Spain), S. Rügamer(Universität Würzburg, Germany), A. Saggion(Università di Padova and INFN Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), T. Y. Saito(Max-Planck-Institut für Physik, München, Germany), M. Salvati(INAF National Institute for Astrophysics, Rome, Italy), K. Satalecka(Universidad Complutense, Spain), V. Scalzotto(Università di Padova and INFN Padova, Italy), V. Scapin(Universidad Complutense, Spain), C. Schultz(Università di Padova and INFN Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Sobczynska(University of Łódź, Poland), F. Spanier(Universität Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, Spain), A. Stamerra(Università di Siena, and INFN Pisa, Italy), B. Steinke(Max-Planck-Institut für Physik, München, Germany), J. Storz(Universität Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), L. Takalo(Tuorla Observatory, University of Turku, Finland), H. Takami(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), F. Tavecchio(INAF National Institute for Astrophysics, Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, München, Germany), O. Tibolla(Universität Würzburg, Germany), D. F. Torres(ICREA, Barcelona, Spain), T. Toyama(Max-Planck-Institut für Physik, München, Germany), A. Treves(Università dell'Insubria, Como, Italy), M. Uellenbeck(Technische Universität Dortmund, Germany), P. Vogler(ETH Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, München, Germany), Q. Weitzel(ETH Zurich, Switzerland), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), The MAGIC Collaboration(Università di Trieste, and INFN Trieste, Italy), F. Longo(Università di Trieste, and INFN Trieste, Italy), F. Lucarelli(Agenzia Spaziale Italiana), C. Pittori(Agenzia Spaziale Italiana), S. Vercellone(INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy), for the AGILE team(Università di Padova and INFN Padova, Italy), D. Bastieri(Università di Padova and INFN Padova, Italy), C. Sbarra(INFN Padova, Italy), for the Fermi-LAT Collaboration(Max-Planck-Institut für Radioastronomie, Germany), E. Angelakis(Max-Planck-Institut für Radioastronomie, Germany), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Germany), I. Nestoras(Max-Planck-Institut für Radioastronomie, Germany), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Germany), A. Sievers(Instituto de Radio Astronoma Milimétrica, Spain), J. A. Zensus(Max-Planck-Institut für Radioastronomie, Germany), for the F-GAMMA program(Crimean Astrophysical Observatory, Ukraine), K. A. Antonyuk(Crimean Astrophysical Observatory, Ukraine), W. Baumgartner(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), A. Berduygin(Tuorla Observatory, University of Turku, Finland), M. Carini(Department of Physics and Astronomy, Western Kentucky University, USA), K. Cook(Department of Physics and Astronomy, Western Kentucky University, USA), N. Gehrels(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Kadler(Universität Würzburg, Germany), Yu. A. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), Y. Y. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), F. Krauss(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), H. A. Krimm(Universities Space Research Association, Columbia, MD 21044, USA), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory, Finland), M. L. Lister(Department of Physics, Purdue University, USA), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), M. Pasanen(Tuorla Observatory, University of Turku, Finland), A. B. Pushkarev(Pulkovo Observatory, St. Petersburg, Russia), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), J. L. Richards(Department of Physics, Purdue University, USA), J. Sainio(Tuorla Observatory, University of Turku, Finland), D. N. Shakhovskoy(Crimean Astrophysical Observatory, Ukraine), K. V. Sokolovsky(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), M. Tornikoski(Aalto University Metsähovi Radio Observatory, Finland), J. Tueller(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Weidinger(Theoretische Physik IV, Ruhr-Universität Bochum, Germany), J. Wilms(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Università degli Studi di Udine - University of Udine [Italie], Universita degli studi di Napoli 'Parthenope' [Napoli], Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Vecteurs - Infections tropicales et méditerranéennes (VITROME), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées (IRBA), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), DAAA, ONERA, Université Paris Saclay (COmUE) [Meudon], ONERA-Université Paris-Saclay, University of Bath [Bath], Waves and Solitons LLC, 918 W. Windsong Dr., Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, E., Leonardo, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, D., Nieto, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, M., Pilia, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, S., Rügamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, S., Vercellone, D., Bastieri, C., Sbarra, E., Angelaki, L., Fuhrmann, I., Nestora, T. P., Krichbaum, A., Siever, J. A., Zensu, K. A., Antonyuk, W., Baumgartner, A., Berduygin, M., Carini, K., Cook, N., Gehrel, M., Kadler, Kovalev, Y. u. A., Y. Y., Kovalev, F., Krau, H. A., Krimm, A., Lähteenmäki, M. L., Lister, W., Max Moerbeck, M., Pasanen, A. B., Pushkarev, A. C. S., Readhead, J. L., Richard, J., Sainio, D. N., Shakhovskoy, K. V., Sokolovsky, M., Tornikoski, J., Tueller, M., Weidinger, J., Wilms, UAM. Departamento de Física Teórica, Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées [Brétigny-sur-Orge] (IRBA), Universitat Autònoma de Barcelona [Barcelona] (UAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Helmholtz-Gemeinschaft, National Institute for Nuclear Physics (INFN), National Academy of Sciences of Armenia, The Netherlands Institute for Radio Astronomy (ASTRON), 7990-AA Dwingeloo, Netherlands, Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), INAF-OAB, and DAAA, ONERA, Université Paris Saclay [Meudon]
Subjects: galaxies [Gamma rays], Radiation mechanisms: non-thermal, Flux, Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], BL Lacertae objects: individual: 1ES 2344+514, MAGIC (telescope), 010303 astronomy & astrophysics, galaxies: active, BL Lacerae objects: individual: 1ES 2344+514, gamma rays: galaxies, X-rays: individuals: 1ES 2344+514, radiation mechanisms: non-thermal, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, ACTIVE GALACTIC NUCLEI, BL-LACERTAE OBJECTS, GAMMA-RAY EMISSION, SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS, SELF-COMPTON MODEL, X-RAY, LAC OBJECTS, RELATIVISTIC JETS, MARKARIAN 501, Gamma ray, non-thermal [radiation mechanisms], active [galaxies], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxie [gamma rays], 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Light curve, individual: 1ES 2344+514 [BL Lacertae objects], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies [gamma-rays], Space and Planetary Science, ddc:520, individuals: 1ES 2344+514 [X-rays], Fermi Gamma-ray Space Telescope
Abstract: Astronomy and Astrophysics 556 (2013): A67 reproduced with permission from Astronomy and Astrophysics, Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims.We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods.The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign, The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A.Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged
Published: 2013

14. Multiwavelength observations of Mrk 501 in 2008

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(2,*), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), T. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(7,*), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS Collaboration(Deutsches Elektronen-Synchrotron), (Deutsches Elektronen-Synchrotron), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), A. Bouvier(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), C. Duke(Department of Physics, Grinnell College, Grinnell, IA 50112-1690, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(now at GRAPPA Institute, University of Amsterdam, 1098XH), Q. Feng(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), N. Galante(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Gillanders(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), A. S Madhavan(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), G. Maier(Deutsches Elektronen-Synchrotron), P. Majumdar(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), D. Nieto(Physics Department, Columbia University, New York, NY 10027, USA), A. O'Faoláin de Bhróithe(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), G. Ratliff(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), L. C. Reyes(Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Sembroski(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), F. Sheidaei(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), A. W. Smith(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), S. Vincent(Deutsches Elektronen-Synchrotron), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Welsing(Deutsches Elektronen-Synchrotron), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), A. Zajczyk(Department of Physics, Washington University, St. Louis, MO 63130, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External Collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. M. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Ajello(Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA), M. Perri(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), V. M. Larionov(Astron. Inst., St.-Petersburg State Univ., Russia), N. V. Efimova(Astron. Inst., St.-Petersburg State Univ., Russia), T. S. Konstantinova(Astron. Inst., St.-Petersburg State Univ., Russia), E. N. Kopatskaya(Astron. Inst., St.-Petersburg State Univ., Russia), W. P. Chen(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), E. Koptelova(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), H. Y. Hsiao(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), G. N. Kimeridze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), B. Jordan(School of Cosmic Physics, Dublin Institute For Advanced Studies, Ireland), P. Leto(INAF - Osservatorio Astrofisico di Catania, Italy), C. S. Buemi(INAF - Osservatorio Astrofisico di Catania, Italy), C. Trigilio(INAF - Osservatorio Astrofisico di Catania, Italy), G. Umana(INAF - Osservatorio Astrofisico di Catania, Italy), A. Lahtenmaki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), E. Nieppola(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), J. Sainio(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), A. Cesarini(University of Trento, Department of Physics, I38050 Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Yu. A. Kovalev(Astro Space Center of the Lebedev Physical Institute, 117997), Y. Y. Kovalev(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, School services, ELEC, and ~
Subjects: extragalactic background light, Ciencias Físicas, Flux, Electron, Astrophysics, 7. Clean energy, law.invention, purl.org/becyt/ford/1 [https], Raigs gamma, bl lacertae objects, law, individual: Mrk 501 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, Astroparticle physics, BL Lacertae objects: individual: Mrk 501, Gamma rays: general, Astronomy and Astrophysics, Space and Planetary Science, Synchrotron, individual: Mrk 50 [BL Lacertae objects], Homogeneous, astroparticle physics, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, 1171 Geosciences, Astrophysics::High Energy Astrophysical Phenomena, emitting electrons, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, bl lacertae objects: individual: mrk 501, crab-nebula, Blazar, Astrophysics::Galaxy Astrophysics, tev blazars, variability, 221 Nanotechnology, Gamma rays, Individual: Mrk 501, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], gamma rays: general, Galaxies, gamma-ray emission, telescope system, Galàxies, Active Galaxies, blazars, gamma-rays, Mrk 501, Astronomía, Crab Nebula, x-ray, 115 Astronomy and space science, Low emission, 216 Materials engineering, Galàxies actives, active galactic nuclei, Active galaxies, ddc:520, general [gamma rays]
Abstract: Mrk 501 is one of the brightest blazars at TeV energies and has been extensively studied since its first VHE detection in 1996. Our goal is to characterize in detail the source gamma-ray emission, together with the radio-to-X-ray emission, during the non-flaring (low) activity, which is less often studied than the occasional flaring (high) activity. We organized a multiwavelength (MW) campaign on Mrk 501 between March and May 2008. This multi-instrument effort included the most sensitive VHE gamma-ray instruments in the northern hemisphere, namely the imaging atmospheric Cherenkov telescopes MAGIC and VERITAS, as well as Swift, RXTE, the F-GAMMA, GASP-WEBT, and other collaborations and instruments. Mrk 501 was found to be in a low state of activity during the campaign, with a VHE flux in the range of 10%-20% of the Crab nebula flux. Nevertheless, significant flux variations were detected with various instruments, with a trend of increasing variability with energy. The broadband spectral energy distribution during the two different emission states of the campaign can be adequately described within the homogeneous one-zone synchrotron self-Compton model, with the (slightly) higher state described by an increase in the electron number density. This agrees with previous studies of the broadband emission of this source during flaring and non-flaring states. We report for the first time a tentative X-ray-to-VHE correlation during a low VHE activity. Although marginally significant, this positive correlation between X-ray and VHE, which has been reported many times during flaring activity, suggests that the mechanisms that dominate the X-ray/VHE emission during non-flaring-activity are not substantially different from those that are responsible for the emission during flaring activity., Comment: Accepted for publication in A&A
Published: 2015

15. The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies

Author: MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Mu\ noz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Longo(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(6,32,*), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS collaboration(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), (Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. Archambault(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. H. Buckley(Department of Physics, Washington University, St. Louis, MO 63130, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), J. D. Eisch(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(DESY, Platanenallee 6, 15738 Zeuthen, Germany), Q. Feng(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), H. Fleischhack(Deutsches Elektronen-Synchrotron), P. Fortin(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), G. Hughes(Deutsches Elektronen-Synchrotron), T. B. Humensky(Physics Department, Columbia University, New York, NY 10027, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), Y. Khassen(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), F. Krennrich(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), S. Kumar(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), G. Maier(Deutsches Elektronen-Synchrotron), S. McArthur(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), N. Park(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), K. Ragan(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. C. Rovero(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), G. H. Sembroski(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. V. Tucci(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. Weinstein(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), R. Welsing(Deutsches Elektronen-Synchrotron), A. Wilhelm(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), W. P. Chen(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), B. Jordan(School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, 2, Ireland), E. Koptelova(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), B. McBreen(University College Dublin, Belfield, Dublin 4, Ireland), V. M. Larionov(Isaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, Russia), C. S. Lin(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), E. Angelakis(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Capalbi(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), A. Carrami\ nana(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), L. Carrasco(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), P. Cassaro(INAF Istituto di Radioastronomia, Sezione di Noto, Contrada Renna Bassa, 96017 Noto), A. Cesarini(Department of Physics, University of Trento, I38050, Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), T. Hovatta(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), H. A. Krimm(Astro Space Center of the Lebedev Physical Institute, 117997 Moscow, Russia), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. W. Moody(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), G. Maccaferri(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), Y. Mori(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), I. Nestoras(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), A. Orlati(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), C. Pace(Indiana University, Department of Astronomy, Swain Hall West 319, Bloomington, IN 47405-7105, USA), R. Pearson(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), M. Perri(INAF National Institute for Astrophysics, I-00136 Rome, Italy), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. L. Richards(Department of Physics, Purdue University, 525 Northwestern Ave, West Lafayette, IN 47907), A. C. Sadun(Department of Physics, University of Colorado, Denver, CO 80220, USA), T. Sakamoto(Department of Physics and Mathematics, College of Science and 952 Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuoku, Sagamihara-shi Kanagawa 252-5258, Japan), J. Tammi(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), Y. Yatsu(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), A. Zook(Department of Physics and Astronomy, Pomona College, Claremont CA 91711-6312, USA), Aleksić, J, Ansoldi, Stefano, Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Carreto Fidalgo, D., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadamek, A., Hadasch, D., Herrero, A., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Krause, J., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Longo, Francesco, Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Meucci, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nowak, N., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Partini, S., Persic, M., Prada, F., Prada Moroni, P. G., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguezgarcia, J., Rügamer, S., Saggion, A., Saito, K., Salvati, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Wagner, R. M., Zandanel, F., Zanin, R., Archambault, S., Behera, B., Beilicke, M., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Collins Hughes, E., Cui, W., Dumm, J., Eisch, J. D., Falcone, A., Federici, S., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Hanna, D., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krawczynski, H., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Mukherjee, R., Ong, R. A., Otte, A. N., Park, N., Pichel, A., Pohl, M., Popkow, A., Prokoph, H., Quinn, J., Ragan, K., Rajotte, J., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Theiling, M., Tucci, J. V., Tyler, J., Varlotta, A., Wakely, S. P., Weekes, T. C., Weinstein, A., Welsing, R., Wilhelm, A., Williams, D. A., Zitzer, B., Villata, M., Raiteri, C., Aller, H. D., Aller, M. F., Chen, W. P., Jordan, B., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Mcbreen, B., Larionov, V. M., Lin, C. S., Nikolashvili, M. G., Angelakis, E., Capalbi, M., Carramiñana, A., Carrasco, L., Cassaro, P., Cesarini, A., Fuhrmann, L., Giroletti, M., Hovatta, T., Krichbaum, T. P., Krimm, H. A., Max Moerbeck, W., Moody, J. W., Maccaferri, G., Mori, Y., Nestoras, I., Orlati, A., Pace, C., Pearson, R., Perri, M., Readhead, A. C. S., Richards, J. L., Sadun, A. C., Sakamoto, T., Tammi, J., Tornikoski, M., Yatsu, Y., Zook, A., Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Universitat de Barcelona
Subjects: Astrofísica, Brightness, Ciencias Físicas, blazars, Astrophysics, telescope, x-ray variability, 01 natural sciences, Spectral line, BL Lacertae objects, individual, Mrk 421, purl.org/becyt/ford/1 [https], Raigs gamma, emission, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), individual: Mrk 421 [BL Lacertae objects], Galaxies: BL Lacertae objects: individual: Markarian 421, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectra, BL Lacertae object, tev photons, 0103 physical sciences, Nucli galàctic actiu, bl lacertae objects: individual: mrk 421, Blazar, Astronomy and Astrophysics, Space and Planetary Science, Active galactic nuclei, 010308 nuclear & particles physics, light curves, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Light curve, Galaxies, Galàxies, Astronomía, Crab Nebula, optical variability, active galactic nuclei, Galàxies actives, Active galaxies, markarian-421, ddc:520
Abstract: We performed a 4.5-month multi-instrument campaign (from radio to VHE gamma rays) on Mrk421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies., Comment: Accepted for publication in A&A, 18 pages, 14 figures (v2 has a small modification in the acknowledgments, and also corrects a typo in the field "author" in the metadata)
Published: 2015
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16. Black hole lightning due to particle acceleration at subhorizon scales

Author: J. Kushida, Jose Luis Contreras, Juan Cortina, J. Hose, R. Reinthal, D. Elsaesser, Michele Palatiello, P. Munar-Adrover, Elina Lindfors, Damir Lelas, Dario Hrupec, R. Zanin, Daniel Mazin, D. Nakajima, Victor Stamatescu, M. A. Lopez, Dorota Sobczyńska, Adrian Biland, K. Nishijima, M. Uellenbeck, D. Garrido Terrats, D. Dominis Prester, J. Rico, V. Scalzotto, Christian Fruck, E. Prandini, Stefano Covino, P. G. Prada Moroni, Francesco Longo, F. Borracci, P. Da Vela, Nikola Godinovic, Benito Marcote, Patrick Vogler, Ana Babić, D. Galindo, Yusuke Konno, O. Tibolla, I. Snidaric, M. Makariev, D. Tescaro, P. Temnikov, Ivica Puljak, M. V. Fonseca, A. Sillanpää, Jörn Wilms, G. Bonnoli, L. Maraschi, Pierre Colin, C. Delgado Mendez, S. R. Gozzini, E. de Oña Wilhelmi, Konstancja Satalecka, Julian Sitarek, Michele Doro, A. Treves, Kari Nilsson, Tomislav Terzić, N. Mankuzhiyil, Daniela Hadasch, Jelena Aleksić, Oscar Blanch, Alessandro Carosi, E. Lorenz, Ruben Lopez-Coto, T. Toyama, A. Niedzwiecki, I. Lozano, G. De Caneva, M. Hayashida, David Paneque, S. Bonnefoy, A. González Muñoz, T. Schweizer, Jose Miguel Miranda, E. Colombo, Francesco Dazzi, Masahiro Teshima, G. Maneva, Felix Spanier, Y. Hanabata, Daniela Dorner, C. Schultz, V. Scapin, Miriam Lucio Martinez, S. Rügamer, Juan Abel Barrio, M. Gaug, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Juri Poutanen, Stefano Ansoldi, J. Herrera, Koji Noda, B. Biasuzzi, U. Bach, Marc Ribó, Riccardo Paoletti, P. Antoranz, Elisa Bernardini, Hajime Takami, P. Bangale, J. M. Paredes, Felicia Krauß, Hidetoshi Kubo, Antonio Stamerra, Julia Thaele, K. Kodani, E. Carmona, L. O. Takalo, Louis Antonelli, J. Storz, A. De Angelis, D. Hildebrand, Mosè Mariotti, A.-K. Overkemping, Sabrina Einecke, Saverio Lombardi, J. Rodriguez Garcia, K. Saito, W. Idec, K. Frantzen, V. Kadenius, S. Paiano, Karl Mannheim, Alicia López-Oramas, Natalia Lewandowska, R. Mirzoyan, A. La Barbera, D. Eisenacher, Markus Garczarczyk, X. Paredes-Fortuny, J. Becerra González, Abelardo Moralejo, T. Steinbring, Hanna Kellermann, U. Menzel, Diego F. Torres, J. Krause, B. De Lotto, Takashi Saito, Reiko Orito, Eduardo Ros, Marcel Strzys, Matthias Kadler, K. Mallot, R. J. García López, Massimo Persic, R. Schulz, Thomas Bretz, S. N. Shore, Wolfgang Rhode, Aleksić, J, Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Biasuzzi, B., Bil, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Mendez, C. Delgado, Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Godinoviæ, N., Muñoz, A. González, Gozzini, S. R., Hadasch, D., Hanabata, Y., Hayashida, M., Herrera, J., Hildebr, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Kodani, K., Konno, Y., Krause, J., Kubo, H., Kushida, J., Barbera, A. La, Lelas, D., Lewowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Mira, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Rügamer, S., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Zanin, R., Kadler, M., Schulz, R., Ros, E., Bach, U., Krauß, F., and Wilms, J.
Subjects: Black Holes, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Very High Energy Gamma Astronomy, Black Holes, Very High Energy Gamma Astronomy, Active Galactic Nuclei, X-shaped radio galaxy, supermassive black hole, jet formation, IC 310, MAGIC telescopes, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Supermassive black hole, ta115, Multidisciplinary, Active Galactic Nuclei, Astronomy and Astrophysics, Galaxy, Intermediate-mass black hole, Stellar black hole, Electrónica, Física nuclear, ddc:500, Spin-flip, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius
Abstract: Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry, but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here, we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC telescopes revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20\% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet., 19 pages, 10 figures, includes Supplementary Materials
Published: 2014

17. Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010

Author: E. Pueschel, J. Hose, Svetlana G. Jorstad, M. F. Aller, David A. Williams, G. H. Sembroski, D. Nakajima, M. Strzys, R. Welsing, A. Archer, E. Colombo, B. Biasuzzi, F. Borracci, Stefano Ansoldi, Riccardo Paoletti, I. Telezhinsky, Jamie Holder, D. Elsaesser, D. Staszak, Dario Hrupec, L. Ciupik, L. C. Reyes, G. Bonnoli, K. Ragan, M. A. Lopez, N. Galante, Hajime Takami, J. M. Paredes, P. T. Reynolds, Natalia Lewandowska, Hugh D. Aller, L. O. Takalo, G. H. Gillanders, T. Schweizer, Mosè Mariotti, Wystan Benbow, A.-K. Overkemping, D. Hadasch, Victor Stamatescu, J. Biteau, Paul S. Smith, Gordon T. Richards, Wei Cui, A. La Barbera, Sinéad M. Griffin, E. Roache, A. López-Oramas, S. Rügamer, Juan Abel Barrio, J. A. Ros, O. M. Kurtanidze, Alessandro Carosi, Ruben Lopez-Coto, X. Paredes-Fortuny, Mark Gurwell, U. Menzel, Saverio Lombardi, Calvin A. Johnson, P. Kar, M. Villata, K. Mallot, R. J. García López, Felix Spanier, M. Kertzman, A. C. S. Readhead, E. Prandini, D. Galindo, Merja Tornikoski, Yusuke Konno, Diego F. Torres, M. G. Nikolashvili, D. Eisenacher, Antonio Stamerra, K. Kodani, Givi N. Kimeridze, Julian Sitarek, Lorand A. Sigua, K. Nishijima, J. V. Tucci, A. Cesarini, M. Perri, P. Kaaret, J. Storz, D. Dominis Prester, Martin Pohl, C. M. Raiteri, Markus Garczarczyk, C. Fruck, A. Sillanpää, N. Håkansson, M. Makariev, T. Toyama, L. Maraschi, A. Pichel, Jose Miguel Miranda, Matteo Cerruti, Konstancja Satalecka, J. Becerra González, P. Antoranz, Amy Furniss, S. P. Wakely, B. Jordan, Elena G. Larionova, Xuhui Chen, H. C. Lin, Geza Gyuk, Louis Antonelli, Michele Doro, Abelardo Moralejo, Jelena Aleksić, S. McArthur, M. L. Knoetig, P. G. Prada Moroni, P. Munar-Adrover, Ivica Puljak, E. Collins-Hughes, K. Meagher, Nikola Godinovic, Benito Marcote, T. Steinbring, W. Idec, M. V. Fonseca, Pierre Colin, P. Temnikov, M. Hayashida, Patrick Vogler, J. Tyler, A. Niedzwiecki, C. Schultz, V. Scapin, J. H. Buckley, P. Moriarty, Tomislav Terzić, K. Berger, T. Sakamoto, C. Delgado Mendez, S. R. Gozzini, B. McBreen, O. Tibolla, Shan Sun, E. de Oña Wilhelmi, Ivan S. Troitsky, David Paneque, I. Snidaric, Marc Ribó, P. Da Vela, D. Hildebrand, B. Steinke, Steven N. Shore, Q. Feng, K. Frantzen, Massimo Persic, Hidetoshi Kubo, A. Boller, D. A. Morozova, A. Wilhelm, R. Reinthal, Thomas Bretz, Sofia O. Kurtanidze, Kari Nilsson, Elina Lindfors, Justin D. Finke, J. Krause, B. De Lotto, Walter Max-Moerbeck, K. Saito, Razmik Mirzoyan, U. Barres de Almeida, A. González Muñoz, V. Kadenius, Damir Lelas, N. Mankuzhiyil, J. P. Finley, J. S. Perkins, Wen Ping Chen, S. Paiano, E. Lorenz, Karl Mannheim, H. Prokoph, Hanna Kellermann, Daniel Mazin, I. Lozano, Dorota Sobczyńska, J. D. Eisch, Wolfgang Rhode, Daniela Dorner, M. Palatiello, Joseph Moody, Lucy Fortson, M. I. Martínez, M. Gaug, P. Bangale, G. De Caneva, J. Herrera, Matthias Beilicke, Koji Noda, J. Millis, Abraham D. Falcone, Francesco Dazzi, Karlen Shahinyan, Elisa Bernardini, S. Bonnefoy, Sabrina Einecke, J. Rodriguez Garcia, W. Bednarek, Fabrizio Tavecchio, Ll. Font, A. C. Sadun, Anne Lähteenmäki, Stefano Covino, M. J. Lang, A. Varlotta, Masahiro Teshima, A. McCann, Ekaterina Koptelova, A. C. Rovero, J. Kushida, D. Tescaro, Jose Luis Contreras, G. Hughes, M. Uellenbeck, Takashi Saito, Y. Hanabata, A. Popkow, Juan Cortina, V. Bugaev, David Kieda, Reiko Orito, S. Buson, J. L. Richards, Ann E. Wehrle, D. Garrido Terrats, P. Fortin, Oscar Blanch, Ralph Bird, S. Archambault, Valeri M. Larionov, V. Scalzotto, Ana Babić, Julia Thaele, E. Carmona, A. De Angelis, A. Treves, R. A. Ong, G. Maneva, R. Zanin, A. N. Otte, Adrian Biland, J. Rico, Alan P. Marscher, Universitat de Barcelona, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and ~
Subjects: extragalactic background light, Ciencias Físicas, spectral energy-distribution, Flux, Non-thermal / galaxies, Astrophysics, law.invention, Relativistic particle, purl.org/becyt/ford/1 [https], atmospheric cherenkov telescopes, Raigs gamma, bl lacertae objects, law, MAGIC (telescope), Active / BL Lacertae objects, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual: Mrk 421 [BL Lacertae objects], education.field_of_study, gamma-ray outburst, non-thermal [radiation mechanisms], BL Lacertae objects: individual: Mrk 421, Galaxies: active, Gamma rays: galaxies, Radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, Particle acceleration, NON THERMAL RADIATION, large-area telescope, active [galaxies], galaxies [gamma rays], BL LACERTAE OBJECTS, Electrónica, self-compton model, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Flare, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, radiation mechanisms: non-thermal, gamma rays: galaxies, Radiation mechanisms, BL Lacertae objects: individual, simultaneous multiwavelength observations, AGN, education, Blazar, Individual: Mrk 421 / gamma rays, tev blazars, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Galaxies, Astronomía, x-ray, Galàxies actives, Active galaxies, ddc:520
Abstract: A flare from the TeV blazar Mrk 421, occurring in March 2010, was observed for 13 consecutive days from radio to very high energy (VHE, E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, FermiLAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We model the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigate the physical parameters, and evaluate whether the observed broadband SED variability can be associated to variations in the relativistic particle population. Flux variability was remarkable in the X-ray and VHE bands while it was minor or not significant in the other bands. The one-zone SSC model can describe reasonably well the SED of each day for the 13 consecutive days. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission while the other smaller zone, which is spatially separated from the first one, contributes to the daily-variable emission occurring in X-rays and VHE gamma-rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly to the underlying particle population. This shows that the particle acceleration and cooling mechanism producing the radiating particles could be the main one responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by the variation of the parameters related to the emitting region itself ($\delta$, $B$ and $R$), in addition to the parameters related to the particle population., Comment: Published in A&A, 30 pages, 15 figures, 6 tables. Online-data: multi-wavelength light curves (data in Fig. 1) and broadband spectral energy distributions (the data in Figs. 6, and B1-B4) are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A22. Corresponding authors: David Paneque (dpaneque@mpp.mpg.de), Shangyu Sun (sysun@mpp.mpg.de), Hajime Takami (takami@post.kek.jp)
Published: 2014

18. First broadband characterization and redshift determination of the VHE blazar MAGIC J2001+439

Author: Robert Wagner, Konstancja Satalecka, Michele Doro, K. Nishijima, K. Mallot, R. J. García López, A. Herrero, D. Dominis Prester, M. Uellenbeck, Nina Nowak, J. M. Paredes, A. López-Oramas, J. Kushida, Antonio Stamerra, Jelena Aleksić, Nikola Godinovic, Benito Marcote, Jose Luis Contreras, A. Niedzwiecki, David Paneque, Wlodek Bednarek, Alessandro Carosi, Francisco Prada, J. L. Richards, Juan Cortina, K. Kodani, Ruben Lopez-Coto, Massimo Persic, D. Nakajima, J. Storz, D. Garrido Terrats, Talvikki Hovatta, Patrick Vogler, P. G. Prada Moroni, Valeri M. Larionov, Jose Miguel Miranda, V. Scalzotto, C. Schultz, V. Scapin, Tomislav Terzić, Yusuke Konno, Anthony C. S. Readhead, J. Krause, O. Tibolla, M. Hayashida, B. De Lotto, P. Da Vela, Ana Babić, Hanna Kellermann, L. Maraschi, Elina Lindfors, Kari Nilsson, Daniel Mazin, Marc Ribó, M. V. Fonseca, P. Bangale, Julia Thaele, Hidetoshi Kubo, Stefano Covino, U. Menzel, Emanuele Paolo Farina, A. De Angelis, D. Tescaro, M. Perri, I. Snidaric, Natalia Lewandowska, M. Palatiello, Diego F. Torres, S. Rügamer, Stefano Ansoldi, Juan Abel Barrio, M. I. Martínez, Riccardo Paoletti, Felix Spanier, T. Sakamoto, M. Garczarczyk, E. Lorenz, Hajime Takami, A. La Barbera, L. A. Antonelli, Francesco Dazzi, Sabrina Einecke, P. Antoranz, R. Reinthal, J. Rodriguez Garcia, Dominik Elsaesser, Giacomo Bonnoli, X. Paredes-Fortuny, U. Barres de Almeida, I. Lozano, Fabrizio Tavecchio, Damir Lelas, Ll. Font, Masahiro Teshima, Victor Stamatescu, S. Bonnefoy, R. D. Schwartz, Filippo D'Ammando, Dorota Sobczyńska, R. Mirzoyan, D. Eisenacher, Abelardo Moralejo, P. Temnikov, Fabio Zandanel, Shan Sun, E. Carmona, T. Steinbring, Julian Sitarek, J. Hose, Aaron Dominguez, E. Prandini, Daniela Hadasch, T. Toyama, Aldo Treves, W. Idec, Thomas Bretz, S. N. Shore, Walter Max-Moerbeck, Wolfgang Rhode, K. Frantzen, Ivica Puljak, Tihomir Surić, Pierre Colin, D. Carreto Fidalgo, T. Schweizer, C. Delgado Mendez, S. R. Gozzini, F. Borracci, V. Kadenius, S. Paiano, Karl Mannheim, J. Becerra González, Mario Meucci, F. Verrecchia, E. Colombo, Nijil Mankuzhiyil, P. Munar-Adrover, G. Maneva, Silvia Preziuso, L. O. Takalo, R. Zanin, A. Saggion, Adrian Biland, A. González Muñoz, Mosè Mariotti, A.-K. Overkemping, J. Rico, A. Sillanpää, Daniela Dorner, Takashi Saito, Saverio Lombardi, M. Gaug, Reiko Orito, J. Herrera, Koji Noda, Elisa Bernardini, Christian Fruck, K. Saito, D. Hildebrand, Daniel Ferenc, G. De Caneva, S. Partini, Marcel Strzys, L. C. Reyes, Martin Makariev, Oscar Blanch, M. Doert, Dario Hrupec, M. A. Lopez, Aleksic J, Ansoldi S, Antonelli LA, Antoranz P, Babic A, Bangale P, de Almeida UB, Barrio JA, Gonzalez JB, Bednarek W, Bernardini E, Biland A, Blanch O, Bonnefoy S, Bonnoli G, Borracci F, Bretz T, Carmona E, Carosi A, Fidalgo DC, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi F, De Angelis A, De Caneva G, De Lotto B, Mendez CD, Doert M, Dominguez A, Prester DD, Dorner D, Doro M, Einecke S, Eisenacher D, Elsaesser D, Farina E, Ferenc D, Fonseca MV, Font L, Frantzen K, Fruck C, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Godinovic N, Munoz AG, Gozzini SR, Hadasch D, Hayashida M, Herrera J, Herrero A, Hildebrand D, Hose J, Hrupec D, Idec W, Kadenius V, Kellermann H, Kodani K, Konno Y, Krause J, Kubo H, Kushida J, La Barbera A, Lelas D, Lewandowska N, Lindfors E, Lombardi S, Lopez M, Lopez-Coto R, Lopez-Oramas A, Lorenz E, Lozano I, Makariev M, Mallot K, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Meucci M, Miranda JM, Mirzoyan R, Moralejo A, Munar-Adrover P, Nakajima D, Niedzwiecki A, Nilsson K, Nishijima K, Noda K, Nowak N, Orito R, Overkemping A, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Partini S, Persic M, Prada F, Moroni PGP, Prandini E, Preziuso S, Puljak I, Reinthal R, Rhode W, Riboo M, Rico J, Garcia JR, Rugamer S, Saggion A, Saito T, Saito K, Satalecka K, Scalzotto V, Scapin V, Schultz C, Schweizer T, Shore SN, Sillanpaa A, Sitarek J, Snidaric I, Sobczynska D, Spanier F, Stamatescu V, Stamerra A, Steinbring T, Storz J, Strzys M, Sun S, Suric T, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Thaele J, Tibolla O, Torres DF, Toyama T, Treves A, Uellenbeck M, Vogler P, Wagner RM, Zandanel F, Zanin R, DAmmando F, Hovatta T, Larionov VM, Max-Moerbeck W, Perri M, Readhead ACS, Richards JL, Sakamoto T, Schwartz RD, Verrecchia F, and Reyes LC
Subjects: ACTIVE GALACTIC NUCLEI, BL Lacertae objects: individual: MAGIC J2001+439, Galaxies: active, BL Lac objects: individual (MAGIC J2001+435), gamma rays: observations, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, Nordic Optical Telescope, Spectral line, BL Lacertae objects: individual: MAGIC J2001+435, Gamma rays: galaxies, 0103 physical sciences, GAMMA-RAY SPECTRUM, MAGIC (telescope), 010306 general physics, Blazar, 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), galaxies: active – BL Lacertae objects: individual: MAGIC J2001+435 – BL Lacertae objects: individual: MAGIC J2001+439 – gamma rays: galaxies, FERMI ERA, Astronomy and Astrophysics, PKS 1424+240, BL-LACERTAE OBJECTS, Galaxy, Redshift, EXTRAGALACTIC BACKGROUND LIGHT, LAC OBJECTS, SKY SURVEY, RADIATION, Amplitude, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract: We aim to characterize the broadband emission from 2FGL J2001.1+4352, which has been associated with the unknown-redshift blazar MG4 J200112+4352. Based on its gamma-ray spectral properties, it was identified as a potential very high energy (VHE; E > 100 GeV) gamma-ray emitter. The source was observed with MAGIC first in 2009 and later in 2010 within a multi-instrument observation campaign. The MAGIC observations yielded 14.8 hours of good quality stereoscopic data. The object was monitored at radio, optical and gamma-ray energies during the years 2010 and 2011. The source, named MAGIC J2001+439, is detected for the first time at VHE with MAGIC at a statistical significance of 6.3 {\sigma} (E > 70 GeV) during a 1.3-hour long observation on 2010 July 16. The multi-instrument observations show variability in all energy bands with the highest amplitude of variability in the X-ray and VHE bands. We also organized deep imaging optical observations with the Nordic Optical Telescope in 2013 to determine the source redshift. We determine for the first time the redshift of this BL Lac object through the measurement of its host galaxy during low blazar activity. Using the observational evidence that the luminosities of BL Lac host galaxies are confined to a relatively narrow range, we obtain z = 0.18 +/- 0.04. Additionally, we use the Fermi-LAT and MAGIC gamma-ray spectra to provide an independent redshift estimation, z = 0.17 +/- 0.10. Using the former (more accurate) redshift value, we adequately describe the broadband emission with a one-zone SSC model for different activity states and interpret the few-day timescale variability as produced by changes in the high-energy component of the electron energy distribution., Comment: 17 pages, 15 figures, Accepted for publication in A&A
Published: 2014

19. Observations of the Blazar 3C 66A with the MAGIC Telescopes in Stereoscopic Mode

Author: Denis Bastieri, A. Saggion, Q. Weitzel, Tihomir Surić, Ignasi Reichardt, Adrian Biland, G. Maneva, Francesco Dazzi, Thomas Bretz, S. N. Shore, Miguel A. Sánchez-Conde, D. Elsaesser, E. Leonardo, S. Rügamer, Silvia Pardo, Elina Lindfors, Antonio Stamerra, Juan Abel Barrio, Karl Mannheim, Ivica Puljak, T. Jogler, D. Borla Tridon, J. Rico, Daniel Mazin, V. Scalzotto, D. Dominis Prester, Pierre Colin, B. Huber, J. Krause, Wolfgang Rhode, R. G. Pegna, Manel Errando, R. J. García López, M. Salvati, B. De Lotto, Andrei Berdyugin, P. G. Prada Moroni, Agnieszka Sierpowska-Bartosik, J. Storz, Dario Hrupec, Francisco Prada, D. Hildebrand, L. Peruzzo, M. Camara, A. Boller, M. A. Lopez, L. Cossio, Fabio Zandanel, M. Thom, M. Shayduk, F. De Sabata, S. Klepser, Takashi Saito, C. Schultz, Massimo Persic, A. Sillanpää, Pol Bordas, Stefano Covino, Artemio Herrero, Tomislav Terzić, Jose Luis Contreras, Aaron Dominguez, Nijil Mankuzhiyil, M. V. Fonseca, D. Bose, T. Krähenbühl, K. Berger, Felicitas Pauss, Daniel Ferenc, N. Puchades, Juan Cortina, Wlodek Bednarek, Alessandro Carosi, H. Vankov, A. La Barbera, N. Strah, Victor Zabalza, Reiko Orito, Riccardo Paoletti, Ilana M. Braun, B. Steinke, E. De Cea del Pozo, D. Tescaro, D. Garrido, Diego F. Torres, Jose Miguel Miranda, Felix Spanier, M. Pasanen, E. Prandini, L. A. Antonelli, Laura Maraschi, M. I. Martínez, M. Doert, Abelardo Moralejo, Michael Backes, Igor Oya, Fabrizio Tavecchio, Daniel Kranich, Ll. Font, K. Saito, J. Becerra González, Kari Nilsson, R. Reinthal, D. Hadasch, Damir Lelas, Masahiro Teshima, Patrick Vogler, Dorota Sobczyńska, A. Diago Ortega, Robert Wagner, Hiroko Miyamoto, Mario Meucci, S. Partini, Francesco Longo, D. Höhne-Mönch, Jelena Aleksić, Parthasarathi Majumdar, Josep M. Paredes, Javier Moldon, S. Spiro, E. Lorenz, Konstancja Satalecka, Michele Doro, Martin Makariev, Oscar Blanch, T. Schweizer, Valentí Bosch-Ramon, V. Scapin, Gianluca Giavitto, A. Cañellas, Julian Sitarek, J. Hose, Mosè Mariotti, Daniela Dorner, Saverio Lombardi, J. Pochon, E. Colombo, Ralph Bock, L. O. Takalo, Petar Temnikov, Elisa Bernardini, P. Antoranz, C. Delgado Mendez, J. C. Struebig, Roberta Zanin, Miguel A. Pérez-Torres, Marc Ribó, Nikola Godinovic, M. De Maria, A. De Angelis, Giacomo Bonnoli, Daniel Nieto, R. Mirzoyan, E. Carmona, Markus Garczarczyk, Universitat de Barcelona, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, J. A., Barrio, D., Bastieri, Gonzalez, J., W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, Tridon, D., V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, M., Camara, A., Ca\~nella, E., Carmona, A., Carosi, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, F., Dazzi, Angelis, A., Cea, E., Lotto, B., Maria, M., Sabata, F., Mendez, C., Ortega, A., M., Doert, A., Dom\inguez, Prester, D., D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J., Garc\ia, M., Garczarczyk, G., Giavitto, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., H\ohne M\onch, J., Hose, D., Hrupec, T., Jogler, S., Klepser, T., Kr\ahenb\uhl, D., Kranich, J., Krause, Barbera, A., E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, M., Makariev, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Mart\inez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, A., Moralejo, D., Nieto, K., Nilsson, R., Orito, I., Oya, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, J., Pochon, F., Prada, P. G., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, S., R\ugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanp\a\a, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J., Storz, N., Strah, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, M., Thom, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, and R., Zanin
Subjects: galaxies [Gamma rays], individual: 3C 66A [BL Lacertae objects], Radio galaxy, CHERENKOV TELESCOPE, Astrophysics, BL Lacertae objects: individual (3C 66A), 01 natural sciences, Raigs gamma, MAGIC (telescope), Absorption (logic), 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), TEV BLAZARS, Extragalactic background light, BL LACERTAE OBJECTS, EXTRAGALACTIC BACKGROUND LIGHT, HIGH-ENERGY EMISSION, GAMMA-RAY EMISSION, PROTON BLAZAR, LAC OBJECTS, X-RAY, SPECTRA, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lacertae objects: individual: 3C 66A, BL Lac object, individual (3C 66A) [BL Lacertae objects], active [Galaxies], BL Lacertae objects: individual (3C 66A) — galaxies: active — gamma rays: galaxies, galaxies: active, FOS: Physical sciences, 0103 physical sciences, gamma rays: galaxies, Blazar, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Redshift, Crab Nebula, Space and Planetary Science, Galàxies actives, Active galaxies
Abstract: 5 páginas, 3 figuras, 1 tabla.-- El Pdf del artículo es la versión pre-print: arXiv:1010.0550.-- et al., We report new observations of the intermediate-frequency peaked BL Lacertae object 3C 66A with the MAGIC telescopes. The data sample we use were taken in 2009 December and 2010 January, and comprises 2.3 hr of good quality data in stereoscopic mode. In this period, we find a significant signal from the direction of the blazar 3C 66A. The new MAGIC stereoscopic system is shown to play an essential role for the separation between 3C 66A and the nearby radio galaxy 3C 66B, which is at a distance of only 6'. The derived integral flux above 100 GeV is 8.3% of the Crab Nebula flux and the energy spectrum is reproduced by a power law of photon index 3.64 ± 0.39stat ± 0.25sys. Within errors, this is compatible with the one derived by VERITAS in 2009. From the spectra corrected for absorption by the extragalactic background light, we only find small differences between the four models that we applied, and constrain the redshift of the blazar to z < 0.68., This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence “Origin and Structure of the Universe,” and by the Polish MNiSzW Grant N N203 390834.
Published: 2010
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20. MAGIC upper limits for two milagro-detected bright Fermi sources in the region of SNR G65.1+0.6

Author: M. Camara, R. Reinthal, Mosè Mariotti, Pratik Majumdar, M. V. Fonseca, Dominik Elsaesser, Thomas Bretz, M. Rissi, Saverio Lombardi, J. Pochon, Denis Bastieri, Tihomir Surić, S. N. Shore, Stefano Covino, L. O. Takalo, B. Steinke, J. Krause, B. De Lotto, M. Salvati, Aaron Dominguez, Felicitas Pauss, T. Krähenbühl, M. Lopez, Dorota Sobczyńska, S. Partini, D. Höhne-Mönch, D. Tescaro, R. Mirzoyan, Wolfgang Rhode, N. Strah, S. Klepser, Victor Zabalza, Karl Mannheim, K. Nilsson, D. Dominis Prester, S. Rügamer, E. Carmona, Juan Abel Barrio, S. Spiro, E. Lorenz, E. Lindfors, M. I. Martínez, Giacomo Bonnoli, E. De Cea del Pozo, Julian Sitarek, D. Borla Tridon, R. J. García López, Francisco Prada, Jose Luis Contreras, P. G. Prada Moroni, D. Bose, E. Prandini, J. Hose, C. DelgadoMendez, Juan Cortina, Agnieszka Sierpowska-Bartosik, Nikola Godinovic, M. De Maria, A. La Barbera, K. Berger, Daniela Hadasch, L. Maraschi, Massimo Persic, P. Bordas, C. Schultz, Igor Oya, Fabrizio Tavecchio, Felix Spanier, Oscar Blanch, J. C. Struebig, J. Moldón, J. Becerra González, Ll. Font, J. M. Paredes, Diego F. Torres, F. Longo, M. Pasanen, V. Scalzotto, Andrei Berdyugin, Antonio Stamerra, Roberta Zanin, D. Hildebrand, L. Peruzzo, Mario Meucci, Masahiro Teshima, R. G. Pegna, A. Boller, K. Saito, M. Doert, Michael Backes, A. Carosi, R. K. Bock, M. Garczarczyk, V. Scapin, J. Storz, Manel Errando, Abelardo Moralejo, Francesco Dazzi, F. De Sabata, N. Puchades, R. Paoletti, Fabio Zandanel, Miguel A. Sánchez-Conde, Miguel A. Pérez-Torres, E. Leonardo, T. Saito, Daniel Ferenc, H. Vankov, Ilana M. Braun, Marc Ribó, Tomislav Terzić, Reiko Orito, A. Saggion, Adrian Biland, I. Puljak, N. Mankuzhiyil, J. Rico, A. De Angelis, L. A. Antonelli, T. Jogler, D. Kranich, Ignasi Reichardt, Wlodek Bednarek, M. Shayduk, A. Herrero, Quirin Weitzel, Daniel Nieto, Jose Miguel Miranda, G. Maneva, Dario Hrupec, Valentí Bosch-Ramon, Gianluca Giavitto, P. Colin, D. Mazin, A. Sillanpää, Daniela Dorner, M. Gaug, Petar Temnikov, Elisa Bernardini, P. Antoranz, Konstancja Satalecka, Michele Doro, Hiroko Miyamoto, T. Schweizer, Jelena Aleksić, A. Diago Ortega, Robert Wagner, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, J. A., Barrio, D., Bastieri, Gonzalez, J., W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, Tridon, D., V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, M., Camara, E., Carmona, A., Carosi, P., Colin, J. L., Contrera, J., Cortina, S., Covino, F., Dazzi, Angelis, A., Cea, E., Lotto, B., Maria, M., Sabata, F., Mendez, C., Ortega, A., M., Doert, A., Dom\inguez, Prester, D., D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J., Garc\ia, M., Garczarczyk, M., Gaug, G., Giavitto, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., H\ohne M\onch, J., Hose, D., Hrupec, T., Jogler, S., Klepser, T., Kr\ahenb\uhl, D., Kranich, J., Krause, Barbera, A., E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Mart\inez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, A., Moralejo, D., Nieto, K., Nilsson, R., Orito, I., Oya, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, J., Pochon, F., Prada, P. G., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., R\ugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, A., Sierpowska Bartosik, A., Sillanp\a\a, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J., Storz, N., Strah, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, and R., Zanin
Subjects: Photon, GAMMA-RAY PULSARS, TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, SOURCE LIST, CATALOG, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Telescope, Pulsar, law, Observatory, ISM: supernova remnants, pulsars: individual: PSR J1957+2831 LAT PSR J1954+2836 LAT PSR J1958+2846, pulsars: individual(PSR J1957+2831, LAT PSR J1954+2836, LAT PSR J1958+2846), 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Pulsars, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Supernoves, Astronomy and Astrophysics, individual: PSR J1957+2831 LAT PSR J1954+2836 LAT PSR J1958+2846 [pulsars], Púlsars, Crab Nebula, Supernovae, 13. Climate action, Space and Planetary Science, Milagro, supernova remnant [ISM], Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We report on the observation of the region around supernova remnant G65.1+0.6 with the stand-alone MAGIC-I telescope. This region hosts the two bright GeV gamma-ray sources 1FGL J1954.3+2836 and 1FGL J1958.6+2845. They are identified as GeV pulsars and both have a possible counterpart detected at about 35 TeV by the Milagro observatory. MAGIC collected 25.5 hours of good quality data, and found no significant emission in the range around 1 TeV. We therefore report differential flux upper limits, assuming the emission to be point-like (, 8 pages, 3 figures, 1 table
Published: 2010

21. Detection of very high energy γ-ray emission from the Perseus cluster Head-Tail Galaxy IC 310 by the MAGIC telescopes

Author: D. Bose, T. Krähenbühl, J. Becerra González, Diego F. Torres, M. Pasanen, Mario Meucci, M. Doert, Michael Backes, Abelardo Moralejo, E. De Cea del Pozo, N. Strah, M. Shayduk, Stefano Covino, Marc Ribó, Riccardo Paoletti, A. Pinzke, Aaron Dominguez, Nijil Mankuzhiyil, K. Berger, Felicitas Pauss, Victor Zabalza, Manel Errando, D. Tescaro, J. M. Paredes, Antonio Stamerra, Fabio Zandanel, K. Saito, A. La Barbera, T. Schweizer, S. Rügamer, R. J. García López, Agnieszka Sierpowska-Bartosik, Juan Abel Barrio, D. Borla Tridon, Jose Luis Contreras, J. Krause, B. De Lotto, Massimo Persic, Juan Cortina, A. De Angelis, S. Partini, Felix Spanier, Giacomo Bonnoli, J. Storz, Takashi Saito, A. Cañellas, Francesco Longo, D. Höhne-Mönch, Christoph Pfrommer, Reiko Orito, L. Maraschi, Elina Lindfors, Ignasi Reichardt, A. Boller, S. Klepser, D.V. Semikoz, M. Camara, Pierre Colin, L. Cossio, N. Puchades, Masahiro Teshima, Andrei Berdyugin, L. A. Antonelli, A. Diago Ortega, Robert Wagner, Daniel Mazin, T. Jogler, Pratik Majumdar, M. V. Fonseca, M. Salvati, Hiroko Miyamoto, Jelena Aleksić, R. G. Pegna, C. Schultz, Thomas Bretz, S. N. Shore, F. De Sabata, Mosè Mariotti, G. Maneva, A. Sillanpää, Artemio Herrero, Nikola Godinovic, Igor Oya, Fabrizio Tavecchio, Daniel Kranich, Ll. Font, D. Dominis Prester, A. Saggion, Denis Bastieri, Q. Weitzel, Adrian Biland, Tihomir Surić, Daniel Nieto, M. De Maria, B. Steinke, Kari Nilsson, Saverio Lombardi, Pol Bordas, Wolfgang Rhode, Tomislav Terzić, Javier Moldon, Francisco Prada, J. Pochon, Julian Sitarek, S. Spiro, E. Lorenz, Daniel Ferenc, Andrii Neronov, Martin Makariev, Oscar Blanch, Karl Mannheim, J. Hose, Daniela Hadasch, H. Vankov, Ilana M. Braun, V. Scalzotto, E. Colombo, Wlodek Bednarek, Alessandro Carosi, Konstancja Satalecka, Michele Doro, Jose Miguel Miranda, Ralph Bock, P. Antoranz, L. O. Takalo, Dario Hrupec, M. A. Lopez, E. Prandini, R. Reinthal, Dominik Elsaesser, Dorota Sobczyńska, R. Mirzoyan, E. Carmona, Markus Garczarczyk, Valentí Bosch-Ramon, V. Scapin, Gianluca Giavitto, Daniela Dorner, J. C. Struebig, Petar Temnikov, Roberta Zanin, Elisa Bernardini, Miguel A. Pérez-Torres, C. Delgado Mendez, Francesco Dazzi, J. Rico, Miguel A. Sánchez-Conde, E. Leonardo, D. Hildebrand, L. Peruzzo, M. I. Martínez, P. G. Prada Moroni, I. Puljak, J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, J. A., Barrio, D., Bastieri, J. B., Gonzalez, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, M., Camara, A., Canella, E., Carmona, A., Carosi, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, F., Dazzi, A. D., Angeli, E. D., del Pozo, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A. D., Ortega, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J. G., Lopez, M., Garczarczyk, G., Giavitto, N., Godinovic, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, T., Jogler, S., Klepser, T., Krahenbuhl, D., Kranich, J., Krause, A. L., Barbera, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, M., Makariev, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, A., Moralejo, D., Nieto, K., Nilsson, R., Orito, I., Oya, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, J., Pochon, F., Prada, P. G. P., Moroni, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribo, J., Rico, S., Rugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J., Storz, N., Strah, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, R., Zanin, A., Neronov, C., Pfrommer, A., Pinzke, D. V., Semikoz, APC - THEORIE, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), MAGIC, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, gamma rays: galaxies, galaxies: individual: IC310, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Raigs gamma, Very High Energy Gamma-ray Astronomy, MAGIC telescope, Active Galactic Nuclei, Galaxies, galaxies: individual: IC 310, 0103 physical sciences, MAGIC (telescope), Cosmic rays, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Spectral index, 010308 nuclear & particles physics, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma rays, Astronomy and Astrophysics, gamma rays: galaxies — galaxies: active — galaxies: individual (IC 310), Galaxy, Galàxies, Crab Nebula, Space and Planetary Science, ddc:520, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We report on the detection with the MAGIC telescopes of very high energy gamma-rays from IC 310, a head-tail radio galaxy in the Perseus galaxy cluster, observed during the interval November 2008 to February 2010. The Fermi satellite has also detected this galaxy. The source is detected by MAGIC at a high statistical significance of 7.6sigma in 20.6 hr of stereo data. The observed spectral energy distribution is flat with a differential spectral index of -2.00 \pm 0.14. The mean flux above 300 GeV, between October 2009 and February 2010, (3.1 \pm 0.5)x10^{-12} cm^{-2} s^{-1}, corresponds to (2.5 \pm 0.4)% of Crab Nebula units. Only an upper limit, of 1.9% of Crab Nebula units above 300 GeV, was obtained with the 2008 data. This, together with strong hints (>3sigma) of flares in the middle of October and November 2009, implies that the emission is variable. The MAGIC results favour a scenario with the very high energy emission originating from the inner jet close to the central engine. More complicated models than a simple one-zone SSC scenario, e.g. multi-zone SSC, external Compton or hadronic, may be required to explain the very flat spectrum and its extension over more than three orders of magnitude in energy., 6 pages, 5 figures, submitted to ApJL
Published: 2010

22. Antibody Responses of Cattle with Respiratory Coronavirus Infections during Pathogenesis of Shipping Fever Pneumonia Are Lower with Antigens of Enteric Strains than with Those of a Respiratory Strain

Author: Kathy L. O'Reilly, J. Storz, and Xiaoqing Lin
Subjects: Microbiology (medical), Serotype, Clinical Biochemistry, Immunology, Biology, Antibodies, Viral, medicine.disease_cause, Veterinary Immunology, Microbiology, Immune system, Antigen, Neutralization Tests, medicine, Animals, Immunology and Allergy, Coronaviridae, Pasteurellosis, Pneumonic, Serotyping, Antigens, Viral, Lung, Bovine coronavirus, Coronavirus, Coronavirus, Bovine, Hemagglutinin esterase, virus diseases, biology.organism_classification, Virology, Intestines, biology.protein, Cattle, Antibody, Coronavirus Infections
Abstract: The serum antibody responses of cattle with respiratory coronavirus infections during the pathogenesis of shipping fever pneumonia were analyzed with different bovine coronavirus antigens, including those from a wild-type respiratory bovine coronavirus (RBCV) strain (97TXSF-Lu 15-2) directly isolated from lung tissue from a fatally infected bovine, a wild-type enteropathogenic bovine coronavirus (EBCV) strain (Ly 138-3), and the highly cell culture-adapted, enteric prototype strain (EBCV L9-81). Infectivity-neutralizing (IN) and hemagglutinin-inhibiting (HAI) activities were tested. Sequential serum samples, collected during the onset of the respiratory coronavirus infection and at weekly intervals for 5 weeks thereafter, had significantly higher IN and HAI titers for antigens of RBCV strain 97TXSF-Lu15-2 than for the wild-type and the highly cell culture-adapted EBCV strains, with P values ranging from
Published: 2002
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23. Black hole physics. Black hole lightning due to particle acceleration at subhorizon scales

Author: J, Aleksić, S, Ansoldi, L A, Antonelli, P, Antoranz, A, Babic, P, Bangale, J A, Barrio, J, Becerra González, W, Bednarek, E, Bernardini, B, Biasuzzi, A, Biland, O, Blanch, S, Bonnefoy, G, Bonnoli, F, Borracci, T, Bretz, E, Carmona, A, Carosi, P, Colin, E, Colombo, J L, Contreras, J, Cortina, S, Covino, P, Da Vela, F, Dazzi, A, De Angelis, G, De Caneva, B, De Lotto, E, de Oña Wilhelmi, C, Delgado Mendez, D, Dominis Prester, D, Dorner, M, Doro, S, Einecke, D, Eisenacher, D, Elsaesser, M V, Fonseca, L, Font, K, Frantzen, C, Fruck, D, Galindo, R J, García López, M, Garczarczyk, D, Garrido Terrats, M, Gaug, N, Godinović, A, González Muñoz, S R, Gozzini, D, Hadasch, Y, Hanabata, M, Hayashida, J, Herrera, D, Hildebrand, J, Hose, D, Hrupec, W, Idec, V, Kadenius, H, Kellermann, K, Kodani, Y, Konno, J, Krause, H, Kubo, J, Kushida, A, La Barbera, D, Lelas, N, Lewandowska, E, Lindfors, S, Lombardi, F, Longo, M, López, R, López-Coto, A, López-Oramas, E, Lorenz, I, Lozano, M, Makariev, K, Mallot, G, Maneva, N, Mankuzhiyil, K, Mannheim, L, Maraschi, B, Marcote, M, Mariotti, M, Martínez, D, Mazin, U, Menzel, J M, Miranda, R, Mirzoyan, A, Moralejo, P, Munar-Adrover, D, Nakajima, A, Niedzwiecki, K, Nilsson, K, Nishijima, K, Noda, R, Orito, A, Overkemping, S, Paiano, M, Palatiello, D, Paneque, R, Paoletti, J M, Paredes, X, Paredes-Fortuny, M, Persic, J, Poutanen, P G, Prada Moroni, E, Prandini, I, Puljak, R, Reinthal, W, Rhode, M, Ribó, J, Rico, J, Rodriguez Garcia, S, Rügamer, T, Saito, K, Saito, K, Satalecka, V, Scalzotto, V, Scapin, C, Schultz, T, Schweizer, S N, Shore, A, Sillanpää, J, Sitarek, I, Snidaric, D, Sobczynska, F, Spanier, V, Stamatescu, A, Stamerra, T, Steinbring, J, Storz, M, Strzys, L, Takalo, H, Takami, F, Tavecchio, P, Temnikov, T, Terzić, D, Tescaro, M, Teshima, J, Thaele, O, Tibolla, D F, Torres, T, Toyama, A, Treves, M, Uellenbeck, P, Vogler, R, Zanin, M, Kadler, R, Schulz, E, Ros, U, Bach, F, Krauß, and J, Wilms
Abstract: Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.
Published: 2014

24. Discovery of very high energy gamma-ray emission from the blazar 1ES 0033+595 by the MAGIC telescopes

Author: T. Steinbring, A. González Muñoz, Natalia Lewandowska, D. Hildebrand, A. La Barbera, Daniela Dorner, X. Paredes-Fortuny, A. De Angelis, F. Borracci, M. Uellenbeck, Konstancja Satalecka, Michele Doro, S. Partini, S. Buson, Aaron Dominguez, Dario Hrupec, M. A. Lopez, K. Saito, U. Menzel, M. Gaug, J. Becerra González, Mario Meucci, Jelena Aleksić, R. López-Coto, Julian Sitarek, J. Hose, Daniela Hadasch, K. Nishijima, Takashi Saito, A. Niedzwiecki, J. Herrera, T. Toyama, Koji Noda, Giacomo Bonnoli, D. Dominis Prester, Reiko Orito, Diego F. Torres, Thomas Bretz, K. Frantzen, David Paneque, Elisa Bernardini, S. N. Shore, D. Nakajima, G. Maneva, Nikola Godinovic, Benito Marcote, R. Zanin, A. Saggion, P. G. Prada Moroni, M. Garczarczyk, Tihomir Surić, D. Carreto Fidalgo, Martin Makariev, M. I. Martínez, A. Borghese, E. Prandini, Oscar Blanch, O. Tibolla, V. Kadenius, P. Temnikov, Adrian Biland, Francisco Prada, S. Paiano, Lluis Font, Karl Mannheim, M. Hayashida, Victor Stamatescu, J. Krause, A. Herrero, B. De Lotto, J. Rico, Alicia López-Oramas, Stefano Covino, A. Sillanpää, K. Berger, M. Doert, C. Delgado Mendez, V. Tronconi, Hajime Takami, I. Lozano, Nijil Mankuzhiyil, G. De Caneva, S. Bonnefoy, Wolfgang Rhode, Aldo Treves, Sabrina Einecke, S. R. Gozzini, Robert Wagner, J. Rodriguez Garcia, Felix Spanier, W. Idec, P. Munar-Adrover, M. Palatiello, Francesco Dazzi, Masahiro Teshima, S. Sun, Christian Fruck, Daniel Ferenc, D. Tescaro, Yusuke Konno, Silvia Preziuso, Mosè Mariotti, A.-K. Overkemping, P. Da Vela, C. Schultz, V. Scapin, Ivica Puljak, Pierre Colin, Saverio Lombardi, Wlodek Bednarek, Alessandro Carosi, L. Maraschi, Elina Lindfors, E. Colombo, Julia Thaele, Daniel Mazin, Fabio Zandanel, Marc Ribó, L. O. Takalo, P. Bangale, Jose Miguel Miranda, R. Reinthal, Dominik Elsaesser, Hidetoshi Kubo, U. Barres de Almeida, Damir Lelas, R. Mirzoyan, M. V. Fonseca, P. Antoranz, Dorota Sobczyńska, D. Eisenacher, L. A. Antonelli, J. A. Barrio, E. Carmona, Fabrizio Tavecchio, Emanuele Paolo Farina, Nina Nowak, T. Schweizer, S. Rügamer, Tomislav Terzić, Patrick Vogler, I. Snidaric, Hanna Kellermann, K. Mallot, R. J. García López, E. Lorenz, Massimo Persic, J. M. Paredes, Antonio Stamerra, K. Kodani, J. Storz, Stefano Ansoldi, Riccardo Paoletti, J. Kushida, Jose Luis Contreras, Juan Cortina, D. Garrido Terrats, V. Scalzotto, Ana Babić, Kari Nilsson, and Abelardo Moralejo
Subjects: BL Lacertae objects: individual: (1ES 0033+595), Gamma-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.HE, astro-ph.CO, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, individual: (1ES 0033 595), gamma-rays: galaxies [BL Lacertae objects], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, BL Lacertae objects: individual: (1ES 0033 595), 01 natural sciences, Luminosity, 0103 physical sciences, MAGIC (telescope), education, Blazar, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, ta115, 010308 nuclear & particles physics, galaxies: BL Lacertae objects: individual (1ES 0033+595), gamma rays: galaxies, Compton scattering, Astronomy, Astrophysics - Astrophysics of Galaxies, Extragalactic background light, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Monthly Notices of the Royal Astronomical Society, 446 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
Published: 2014

25. MAGIC search for vhe γ-ray emission from ae aquarii in a multiwavelength context

Author: D. Nakajima, P. G. Prada Moroni, Laura Maraschi, Yusuke Konno, A. López-Oramas, Alessandro Carosi, Ruben Lopez-Coto, Victor Stamatescu, B. Biasuzzi, Konstancja Satalecka, Michele Doro, D. Dorner, I. Snidaric, Jose Miguel Miranda, M. Bogosavljevic, E. Lorenz, Fabrizio Tavecchio, Hajime Takami, Z. Ioannou, Tomislav Terzić, Ll. Font, A.-K. Overkemping, Elina Lindfors, M. López, Julia Thaele, E. Carmona, Daniel Mazin, A. Treves, K. Nishijima, M. V. Fonseca, Abelardo Moralejo, Patrick Vogler, M. Mariotti, Thomas Bretz, S. Rügamer, Julian Sitarek, Saverio Lombardi, T. Steinbring, Louis Antonelli, Morihiro Hayashida, P. Da Vela, Pierre Colin, K. Nilsson, J. Kushida, D. Hadasch, Dorothee Hildebrand, P. Antoranz, Robert Wagner, G. De Caneva, J. Becerra González, S. Bonnefoy, C. Schultz, X. Paredes-Fortuny, T. Toyama, Dario Hrupec, R. Paoletti, P. Munar-Adrover, Razmik Mirzoyan, M. Palatiello, I. Lozano, M. Strzys, Jose Luis Contreras, Jelena Aleksić, Silvia Preziuso, Damir Lelas, D. Galindo, D. Dominis Prester, R. Zanin, A. Niedzwiecki, A. Saggion, A. De Angelis, A. Sillanpää, Stefano Covino, Dorota Sobczyńska, V. Scapin, Juan Cortina, K. Frantzen, David Paneque, A. Biland, Diego F. Torres, Masahiro Teshima, Christopher W. Mauche, Takashi Saito, E. de Ona Wilhelmi, Y. Hanabata, D. Tescaro, W. Idec, J. M. Paredes, Nikola Godinovic, Benito Marcote, D. Garrido Terrats, R. Reinthal, M. Uellenbeck, Natalia Lewandowska, Reiko Orito, Francesco Dazzi, V. Scalzotto, A. La Barbera, T. Schweizer, Ana Babić, E. V. Palaiologou, Leo O. Takalo, R. J. García López, Antonio Stamerra, Oscar Blanch, Petar Temnikov, Koji Noda, J. Herrera, Elisa Bernardini, H. Kellermann, G. Bonnoli, N. Mankuzhiyil, W. Rhode, Felix Spanier, K. Kodani, C. Delgado Mendez, O. Tibolla, G. Maneva, A. González Muñoz, Christian Fruck, J. Storz, Juan Abel Barrio, I. Puljak, Stefano Ansoldi, D. Eisenacher, Markus Gaug, Markus Garczarczyk, Nina Nowak, D. Elsaesser, J. Hose, B. De Lotto, Elisa Prandini, M. Makariev, W. Bednarek, J. Rico, S. Paiano, U. Menzel, Miguel A. Pérez-Torres, M. I. Martínez, E. Colombo, P. Bangale, V. Kadenius, M. Doert, Sabrina Einecke, S. R. Gozzini, J. Rodriguez Garcia, K. Saito, Marc Ribó, Hidetoshi Kubo, F. Borracci, K. Mallot, T. Tuominen, Massimo Persic, K. Mannheim, J. Krause, and Universitat de Barcelona
Subjects: accretion: accretion disks, Radiation mechanisms: non-thermal, Novae: cataclysmic variables, Gamma rays: stars, Astrofísica, Accretion, Photon, Astrophysics::High Energy Astrophysical Phenomena, Signal region, Cataclysmic variable star, Astrophysics, Noves (Estels), Raigs gamma, Coincident, Accretion, accretion disks, Novae, cataclysmic variables, Astronomy and Astrophysics, Space and Planetary Science, New stars, Novae, Astrophysics::Galaxy Astrophysics, Physics, astro-ph.HE, cataclysmic variables, Spectral index, accretion disks, Gamma rays, Gamma ray, Stars, Estels, Wavelength, 13. Climate action, ddc:520, Electrónica, Física nuclear, Rayleigh test, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: It has been claimed that the nova-like cataclysmic variable (CV) AE Aquarii (AE Aqr) is a very-high-energy (VHE, $E>$100 GeV) source both on observational and theoretical grounds. We aim to search for VHE gamma-ray emission from AE Aqr during different states of the source at several wavelengths to confirm or rule out previous claims of detection of gamma-ray emission from this object. We report on observations of AE Aqr performed by MAGIC. The source was observed during 12 hours as part of a multiwavelength campaign carried out between May and June 2012 covering the optical, X-ray, and gamma-ray ranges. Besides MAGIC, the other facilities involved were the KVA, Skinakas, and Vidojevica telescopes in the optical and Swift in X-rays. We calculated integral upper limits coincident with different states of the source in the optical. We computed upper limits to the pulsed emission limiting the signal region to 30% of the phaseogram and we also searched for pulsed emission at different frequencies applying the Rayleigh test. AE Aqr was not detected at VHE energies during the multiwavelength campaign. We establish integral upper limits at the 95\% confidence level for the steady emission assuming the differential flux proportional to a power-law function d\phi/dE \propto E^{-Gamma}, with a Crab-like photon spectral index of Gamma=2.6. The upper limit above 200 GeV is 6.4\times10^{-12} cm^{-2}s^{-1} and above 1 TeV is 7.4\times10^{-13} cm^{-2}s^{-1}. We obtained an upper limit for the pulsed emission of 2.6\times10^{-12} cm^{-2}s^{-1} for energies above 200 GeV. Applying the Rayleigh test for pulsed emission at different frequencies we did not find any significant signal. Our results indicate that AE Aqr is not a VHE gamma-ray emitter at the level of emission previously claimed. We have established the most constraining upper limits for the VHE gamma-ray emission of AE Aqr., Comment: 9 pages, 5 figures. Accepted for publication in A&A
Published: 2014

26. Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes

Author: Nina Nowak, Abelardo Moralejo, D. Häfner, L. A. Antonelli, W. Idec, J. Masbou, M. I. Martínez, J. M. Paredes, Antonio Stamerra, M. Salvati, Dario Hrupec, Thomas Bretz, V. Kadenius, S. Rügamer, Mosè Mariotti, Marc Ribó, M. A. Lopez, Fabrizio Tavecchio, S. N. Shore, Juan Abel Barrio, D. Borla Tridon, Dominik Elsaesser, U. Barres de Almeida, S. Bonnefoy, K. Berger, Ll. Font, A. Hadamek, M. Doert, Emanuele Paolo Farina, Aaron Dominguez, J. Storz, G. De Caneva, Damir Lelas, R. Mirzoyan, Michael Backes, A. De Angelis, Christian Fruck, D. Eisenacher, J. Becerra González, Saverio Lombardi, T. Krähenbühl, M. L. Knoetig, Ignasi Reichardt, P. G. Prada Moroni, E. Carmona, I. Snidaric, Markus Garczarczyk, Nijil Mankuzhiyil, P. Munar-Adrover, Wolfgang Rhode, O. Tibolla, Dorota Sobczyńska, Kari Nilsson, M. V. Fonseca, Mario Meucci, Felix Spanier, M. Palatiello, E. Colombo, G. Maneva, Daniel Ferenc, A. Boller, L. Cossio, R. Zanin, A. Saggion, Ralph Bock, Nikola Godinovic, Benito Marcote, K. Mallot, R. J. García López, S. Spiro, E. Lorenz, Adrian Biland, Francesco Dazzi, L. O. Takalo, B. Steinke, Riccardo Paoletti, S. Partini, D. Dominis Prester, Artemio Herrero, J. Rico, K. Saito, J. Kushida, Jose Luis Contreras, Tomislav Terzić, J. Moldón, Francisco Prada, Juan Cortina, Hajime Takami, Ivica Puljak, Massimo Persic, Pierre Colin, R. Reinthal, Giacomo Bonnoli, Patrick Vogler, J. Krause, B. De Lotto, Martin Makariev, M. Asensio, Oscar Blanch, D. Garrido Terrats, A. Sillanpää, V. Scalzotto, Takashi Saito, Q. Weitzel, Tihomir Surić, Reiko Orito, C. Schultz, V. Scapin, D. Carreto Fidalgo, E. Prandini, Aldo Treves, S. Klepser, S. Paiano, C. Delgado Mendez, S. R. Gozzini, Karl Mannheim, Gianluca Giavitto, A. González Muñoz, Daniela Dorner, M. Gaug, Diego F. Torres, Elisa Bernardini, Natalia Lewandowska, F. Jankowski, F. Borracci, A. La Barbera, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Nakajima, Jose Miguel Miranda, P. Antoranz, L. Maraschi, M. Uellenbeck, Elina Lindfors, Konstancja Satalecka, Daniel Mazin, Michele Doro, P. Temnikov, Fabio Zandanel, Shan Sun, Jelena Aleksić, I. Lozano, D. Hadasch, Masahiro Teshima, A. Niedzwiecki, T. Schweizer, Stefano Covino, David Paneque, D. Tescaro, Robert Wagner, Victor Stamatescu, Julian Sitarek, J. Hose, T. Toyama, P. Da Vela, and Universitat de Barcelona
Subjects: Astrofísica, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Telescope, Raigs gamma, law, 0103 physical sciences, MAGIC (telescope), Nucli galàctic actiu, Blazar, 010303 astronomy & astrophysics, BL Lac objects: individual(1ES 1727+502), galaxies: active, gamma rays, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Active galactic nuclei, Telescopis, 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Galaxies: active, Space and Planetary Science, Galaxies, Galàxies, Crab Nebula, 13. Climate action, ddc:520, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Telescopes
Abstract: Motivated by the Costamante & Ghisellini (2002) predictions we investigated if the blazar 1ES 1727+502 (z=0.055) is emitting very high energy (VHE, E>100 GeV) gamma rays. We observed the BL Lac object 1ES 1727+502 in stereoscopic mode with the two MAGIC telescopes during 14 nights between May 6th and June 10th 2011, for a total effective observing time of 12.6 hours. For the study of the multiwavelength spectral energy distribution (SED) we use simultaneous optical R-band data from the KVA telescope, archival UV/optical and X-ray observations by instruments UVOT and XRT on board of the Swift satellite and high energy (HE, 0.1 GeV - 100 GeV) gamma-ray data from the Fermi-LAT instrument. We detect, for the first time, VHE gamma-ray emission from 1ES 1727+502 at a statistical significance of 5.5 sigma. The integral flux above 150 GeV is estimated to be (2.1\pm0.4)% of the Crab Nebula flux and the de-absorbed VHE spectrum has a photon index of (2.7\pm0.5). No significant short-term variability was found in any of the wavebands presented here. We model the SED using a one-zone synchrotron self-Compton model obtaining parameters typical for this class of sources., 7 pages, 5 figures, 2 tables, submitted to A&A
Published: 2014

27. Optimized dark matter searches in deep observations of Segue 1 with MAGIC

Author: M. V. Fonseca, L. Maraschi, M. Palatiello, Daniel Ferenc, Antonio Stamerra, Christian Fruck, Juan Abel Barrio, I. Puljak, J. Kushida, K. Kodani, Mosè Mariotti, Abelardo Moralejo, A.-K. Overkemping, Stefano Covino, Jose Luis Contreras, Oscar Blanch, Tomislav Terzić, Francesco Dazzi, Daniela Dorner, Juan Cortina, T. Steinbring, J. Storz, R. J. García López, Fabio Zandanel, G. Bonnoli, Shan Sun, Nikola Godinovic, Benito Marcote, R. Zanin, P. Da Vela, Robert Wagner, D. Hadasch, A. Saggion, Tihomir Surić, D. Carreto Fidalgo, Jelena Aleksić, D. Tescaro, A. Niedzwiecki, Adrian Biland, David Paneque, B. De Lotto, Saverio Lombardi, D. Garrido Terrats, K. Frantzen, Nijil Mankuzhiyil, X. Paredes-Fortuny, D. Dominis Prester, Damir Lelas, D. Nakajima, Louis Antonelli, Elina Lindfors, Karl Mannheim, P. Munar-Adrover, P. G. Prada Moroni, Daniel Mazin, A. De Angelis, V. Scalzotto, Stefano Ansoldi, Konstancja Satalecka, Silvia Preziuso, Riccardo Paoletti, Markus Gaug, S. Rügamer, Michele Doro, C. Schultz, V. Scapin, Dario Hrupec, Aaron Dominguez, Marc Ribó, A. López-Oramas, M. Uellenbeck, Dorothee Hildebrand, Ana Babić, G. De Caneva, R. Reinthal, Alessandro Carosi, P. Antoranz, Hidetoshi Kubo, S. Bonnefoy, Ruben Lopez-Coto, J. Becerra González, Petar Temnikov, J. M. Paredes, J. Hose, Diego F. Torres, Jose Miguel Miranda, Kari Nilsson, M. López, Dorota Sobczyńska, Elisa Bernardini, D. Elsaesser, T. Schweizer, H. Kellermann, Yusuke Konno, O. Tibolla, U. Barres de Almeida, Mario Meucci, K. Berger, I. Lozano, M. Salvati, F. Borracci, W. Idec, R. K. Bock, Emanuele Paolo Farina, A. Sillanpää, M. Doert, Takashi Saito, Masahiro Teshima, Alejandro Ibarra, E. Colombo, Hajime Takami, Reiko Orito, G. Maneva, C. Delgado Mendez, Felix Spanier, Natalia Lewandowska, K. Saito, Julian Sitarek, Pierre Colin, Julia Thaele, Aldo Treves, L. O. Takalo, A. La Barbera, E. Carmona, M. I. Martínez, Kazuyoshi Nishijima, M. Hayashida, P. Bangale, Gianluca Giavitto, A. González Muñoz, V. Kadenius, Sabrina Einecke, S. R. Gozzini, Francisco Prada, J. Rodriguez Garcia, M. Makariev, J. Rico, Victor Stamatescu, U. Menzel, Simona Paiano, Thomas Bretz, R. Mirzoyan, Wolfgang Rhode, J. Krause, K. Mallot, Massimo Persic, Takeshi Toyama, I. Snidaric, D. Eisenacher, Markus Garczarczyk, Nina Nowak, E. Lorenz, W. Bednarek, Fabrizio Tavecchio, Ll. Font, Elisa Prandini, Patrick Vogler, A. Herrero, S. Partini, Universitat de Barcelona, and SCOAP
Subjects: Astrofísica, Particle physics, Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, dark matter, indirect searches, gamma-ray experiments, Imaging Air Cherenkov Telescopes, dwarf spheroidal galaxies, Segue 1, Gamma ray experiments, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Gamma ray astronomy, Satellite galaxy, Astronomia de raigs gamma, ddc:530, 010306 general physics, Dwarf galaxies, Dwarf galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, Telescopis, 010308 nuclear & particles physics, Bremsstrahlung, Astronomy and Astrophysics, Segue, Galaxies, dwarfs galaxies, Galàxies, High Energy Physics - Phenomenology, Dark matter experiments, Dark matter (Astronomy), dark matter experiments, gamma ray experiments, Monochromatic color, Matèria fosca (Astronomia), Astrophysics - High Energy Astrophysical Phenomena, Telescopes
Abstract: Aleksic, J. et al., We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ~ 500 GeV dark matter particle annihilating into τ+τ−, and is of order langleσannvrangle simeq 1.2 × 10−24 cm3 s−1 — a factor ~ 40 above the langleσannvrangle simeq thermal value., The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider- Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the Croatian Science Foundation Project 09/176, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.
Published: 2014

28. MAGIC long-term study of the distant TeV blazar PKS 1424+240 in a multiwavelength context

Author: Aaron Dominguez, Mosè Mariotti, A.-K. Overkemping, P. G. Prada Moroni, C. Schultz, V. Scapin, Anthony C. S. Readhead, A. González Muñoz, Hajime Takami, O. Tibolla, A. De Angelis, A. Treves, Saverio Lombardi, Daniela Dorner, Daniel Ferenc, S. Rügamer, Juan Abel Barrio, M. Gaug, J. Herrera, Koji Noda, Hanna Kellermann, Elisa Bernardini, G. Maneva, R. Zanin, A. Saggion, S. Partini, Antonio Stamerra, S. N. Shore, K. Kodani, Adrian Biland, Victor Stamatescu, C. Delgado Mendez, J. Rico, P. Temnikov, Stefano Covino, J. Storz, Nina Nowak, Fabio Zandanel, Nikola Godinovic, Benito Marcote, S. Sun, Jari Kotilainen, Julian Sitarek, S. Bonnefoy, D. Tescaro, C. Fruck, T. Toyama, M. Palatiello, Dario Gasparrini, D. Eisenacher, T. Schweizer, Stefano Ansoldi, M. Uellenbeck, Francesco Dazzi, Riccardo Paoletti, E. Carmona, Markus Garczarczyk, A. K. Furniss, Oscar Blanch, J. L. Richards, Elina Lindfors, K. Mallot, Daniel Mazin, R. J. García López, Matthew L. Lister, Konstancja Satalecka, E. Prandini, Michele Doro, Talvikki Hovatta, G. De Caneva, G. Bonnoli, M. Doert, Massimo Persic, P. Da Vela, Ivica Puljak, Pierre Colin, M. Makariev, D. Nakajima, Robert Wagner, R. Reinthal, Razmik Mirzoyan, U. Barres de Almeida, U. Menzel, Jelena Aleksić, Damir Lelas, I. Lozano, D. Hildebrand, W. Idec, M. V. Fonseca, A. Niedzwiecki, Vasiliki Pavlidou, Dorota Sobczyńska, David Paneque, Anne Lähteenmäki, A. Sillanpää, Masahiro Teshima, K. Nishijima, K. Saito, Tuomas Kangas, Takashi Saito, Dario Hrupec, D. Dominis Prester, D. Hadasch, M. I. Martínez, P. Bangale, Francisco Prada, Reiko Orito, Sabrina Einecke, S. R. Gozzini, J. Rodriguez Garcia, E. Colombo, Louis Antonelli, Felix Spanier, L. O. Takalo, Nijil Mankuzhiyil, X. Paredes-Fortuny, P. Munar-Adrover, Silvia Preziuso, M. A. Lopez, P. Antoranz, Natalia Lewandowska, A. La Barbera, Yusuke Konno, Julia Thaele, J. Becerra González, Mario Meucci, K. Frantzen, Tihomir Surić, D. Carreto Fidalgo, J. M. Paredes, V. Kadenius, S. Paiano, Karl Mannheim, M. Hayashida, Alicia López-Oramas, J. Krause, B. De Lotto, Marc Ribó, Diego F. Torres, Hidetoshi Kubo, Abelardo Moralejo, J. Hose, T. Steinbring, D. Elsaesser, A. Herrero, Emanuele Paolo Farina, S. Cutini, Kari Nilsson, Thomas Bretz, J. Kushida, Jose Luis Contreras, Juan Cortina, F. Borracci, D. Garrido Terrats, V. Scalzotto, Ana Babić, Walter Max-Moerbeck, Wolfgang Rhode, Alessandro Carosi, Ruben Lopez-Coto, Jose Miguel Miranda, W. Bednarek, Fabrizio Tavecchio, Ll. Font, I. Snidaric, E. Lorenz, Patrick Vogler, Erkki Kankare, L. Maraschi, Tomislav Terzić, Universitat de Barcelona, Metsähovi Radio Observatory, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Anne Lähteenmäki Group
Subjects: Astrofísica, PARTICLE-ACCELERATION, Astrophysics, 7. Clean energy, LARGE-AREA TELESCOPE, Spectral line, Raigs gamma, Gamma rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, MAGIC (telescope), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, BL-LACERTAE OBJECTS, EXTRAGALACTIC BACKGROUND LIGHT, GAMMA-RAY EMISSION, SPECTRAL ENERGY-DISTRIBUTION, ACTIVE GALACTIC NUCLEI, LAC OBJECTS, X-RAY, FERMI OBSERVATIONS, Gamma ray, Extragalactic background light, galaxies [gamma rays], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, 1171 Geosciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma rays: observations, blazar, BL Lac: AGNs: individual (PKS 1424+240), 114 Physical sciences, Nucli galàctic actiu, Blazar, Active galactic nuclei, Telescopis, 221 Nanotechnology, Gamma rays, Light curve, Redshift, individual: PKS 1424+240 [BL Lacertae objects], 115 Astronomy and space science, 216 Materials engineering, ddc:520, Telescopes
Abstract: We present a study of the very high energy (VHE; E > 100 GeV) gamma-ray emission of the blazar PKS 1424+240 observed with the MAGIC telescopes. The primary aim of this paper is the multiwavelength spectral characterization and modeling of this blazar, which is made particularly interesting by the recent discovery of a lower limit of its redshift of z > 0.6 and makes it a promising candidate to be the most distant VHE source. The source has been observed with the MAGIC telescopes in VHE gamma rays for a total observation time of ~33.6 h from 2009 to 2011. The source was marginally detected in VHE gamma rays during 2009 and 2010, and later, the detection was confirmed during an optical outburst in 2011. The combined significance of the stacked sample is ~7.2 sigma. The differential spectra measured during the different campaigns can be described by steep power laws with the indices ranging from 3.5 +/- 1.2 to 5.0 +/- 1.7. The MAGIC spectra corrected for the absorption due to the extragalactic background light connect smoothly, within systematic errors, with the mean spectrum in 2009-2011 observed at lower energies by the Fermi-LAT. The absorption-corrected MAGIC spectrum is flat with no apparent turn down up to 400 GeV. The multiwavelength light curve shows increasing flux in radio and optical bands that could point to a common origin from the same region of the jet. The large separation between the two peaks of the constructed non-simultaneous spectral energy distribution also requires an extremely high Doppler factor if an one zone synchrotron self-Compton model is applied. We find that a two-component synchrotron self-Compton model describes the spectral energy distribution of the source well, if the source is located at z~0.6., 15 pages, 8 figures. A&A accepted for publication
Published: 2014

29. Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

Author: P. G. Prada Moroni, W. Bednarek, Pierre Colin, Diego F. Torres, D. Nakajima, Fabrizio Tavecchio, Stefano Covino, Ll. Font, Konstancja Satalecka, Michele Doro, Kouichi Hirotani, Nijil Mankuzhiyil, X. Paredes-Fortuny, Dario Hrupec, R. Zanin, A. Saggion, Adrian Biland, Kazuo Saito, P. Munar-Adrover, A. Treves, R. Reinthal, Shan Sun, A. Sillanpää, Antonio Stamerra, Silvia Preziuso, M. A. Lopez, Marc Ribó, Thomas Bretz, S. N. Shore, G. Maneva, Jelena Aleksić, Takashi Saito, A. Niedzwiecki, Abelardo Moralejo, J. Kushida, Jose Luis Contreras, J. M. Paredes, Hidetoshi Kubo, Reiko Orito, Natalia Lewandowska, U. Barres de Almeida, T. Steinbring, M. Makariev, A. Herrero, I. Puljak, M. V. Fonseca, E. Lorenz, M. Uellenbeck, D. Hadasch, J. Storz, Juan Cortina, D. Paneque, G. De Caneva, A. La Barbera, J. Rico, Christian Fruck, Elina Lindfors, S. Partini, Yusuke Konno, Emanuele Paolo Farina, U. Menzel, S. Bonnefoy, M. Doert, Daniel Mazin, Simona Paiano, B. Biasuzzi, Patrick Vogler, Daniel Ferenc, Elisa Prandini, P. Da Vela, T. Schweizer, Razmik Mirzoyan, S. Rügamer, B. De Lotto, L. Maraschi, Robert Wagner, J. Krause, I. Lozano, J. Becerra González, S. Ansoldi, Damir Lelas, M. I. Martínez, P. Bangale, V. Kadenius, Tomislav Terzić, D. Tescaro, G. Bonnoli, Hajime Takami, C. Delgado Mendez, Dorota Sobczyńska, Sabrina Einecke, Oscar Blanch, M. Hayashida, S. R. Gozzini, R. J. García López, N. Nowak, Kari Nilsson, Masahiro Teshima, Juan Abel Barrio, J. Rodriguez Garcia, Riccardo Paoletti, Markus Gaug, Nikola Godinovic, Benito Marcote, J. Hose, D. Garrido Terrats, Daniela Dorner, Takeshi Toyama, K. Mallot, W. Rhode, V. Scalzotto, D. Eisenacher, I. Šnidarić, K. Frantzen, M. Palatiello, Markus Garczarczyk, D. Elsaesser, Massimo Persic, Ana Babić, Petar Temnikov, Koji Noda, Elisa Bernardini, H. Kellermann, A. González Muñoz, C. Schultz, V. Scapin, Jose Carlos Herrera, Francesco Dazzi, A. López-Oramas, Karl Mannheim, Alessandro Carosi, Ruben Lopez-Coto, Jose Miguel Miranda, F. Borracci, T. Surić, Julia Thaele, E. Carmona, D. Fidalgo, Dorothee Hildebrand, P. Antoranz, M. Strzys, Julian Sitarek, Victor Stamatescu, Felix Spanier, K. Nishijima, D. Dominis Prester, Omar Tibolla, Louis Antonelli, A. De Angelis, K. Kodani, W. Idec, Mosè Mariotti, A.-K. Overkemping, Saverio Lombardi, E. Colombo, L. O. Takalo, and Universitat de Barcelona
Subjects: Astrofísica, Spectral shape analysis, Astrophysics::High Energy Astrophysical Phenomena, Theoretical models, FOS: Physical sciences, Gamma rays: stars, Pulsars: individual: Crab pulsar, Stars: neutron, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Spectral line, Raigs gamma, MAGIC (telescope), Connection (algebraic framework), pulsars: individual: Crab pulsar, gamma rays: stars, Pulsars, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Telescopis, Crab Pulsar, Gamma rays, Light curve, Stars, Púlsars, Estels, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Telescopes, Fermi Gamma-ray Space Telescope
Abstract: The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E>100GeV) gamma-rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. In order to test the new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. We analyzed 135 hours of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 4.6 years of {\it Fermi}-LAT data were also analyzed. The known two pulses per period were detected with a significance of $8.0 \sigma$ and $12.6 \sigma$. In addition, significant emission was found between the two pulses with $6.2 \sigma$. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models., Comment: 5 pages, 4 figures
Published: 2014

30. Contemporaneous observations of the radio galaxy NGC 1275 from radio to very high energy gamma-rays

Author: M. Palatiello, A. La Barbera, R. Zanin, X. Paredes-Fortuny, A. Saggion, Adrian Biland, Francesco Dazzi, Abelardo Moralejo, K. Berger, M. Uellenbeck, D. Garrido Terrats, T. Schweizer, M. Salvati, A. Herrero, T. Steinbring, V. Scalzotto, J. Rico, C. Delgado Mendez, S. R. Gozzini, S. Rügamer, S. Bonnefoy, K. Frantzen, F. Borracci, Felix Spanier, Tihomir Surić, D. Carreto Fidalgo, P. Temnikov, P. Da Vela, D. Dominis Prester, D. Hildebrand, Nijil Mankuzhiyil, Dominik Elsaesser, R. Mirzoyan, Fabio Zandanel, U. Barres de Almeida, Shan Sun, P. Munar-Adrover, R. Reinthal, L. A. Antonelli, Silvia Preziuso, D. Eisenacher, W. Idec, Ana Babić, Daniela Dorner, Damir Lelas, S. Paiano, Francisco Prada, Karl Mannheim, E. Carmona, J. Kushida, K. Mallot, R. J. García López, Jose Luis Contreras, Julian Sitarek, M. Gaug, Stefano Covino, I. Lozano, E. Colombo, K. Saito, J. Hose, Dorota Sobczyńska, Juan Cortina, Daniela Hadasch, J. Krause, B. De Lotto, M. Doert, J. A. Barrio, A. De Angelis, A. López-Oramas, Thomas Bretz, Alessandro Carosi, Ralph Bock, Daniel Ferenc, Barbara Balmaverde, M. V. Fonseca, S. N. Shore, L. O. Takalo, D. Nakajima, T. Toyama, Masahiro Teshima, J. Becerra González, L. Font, Massimo Persic, Mosè Mariotti, A.-K. Overkemping, Ruben Lopez-Coto, Nikola Godinovic, A. Sillanpää, Benito Marcote, Elisa Bernardini, Fabrizio Tavecchio, Mario Meucci, Wolfgang Rhode, D. Tescaro, P. G. Prada Moroni, M. I. Martínez, G. Maneva, Hanna Kellermann, Giacomo Bonnoli, U. Menzel, Jose Miguel Miranda, I. Snidaric, Saverio Lombardi, Ivica Puljak, Pierre Colin, Diego F. Torres, V. Kadenius, O. Tibolla, R. Rekola, L. Maraschi, Sabrina Einecke, Kari Nilsson, Tomislav Terzić, Gianluca Giavitto, Reiko Orito, A. González Muñoz, M. Garczarczyk, Elina Lindfors, Daniel Mazin, J. Rodriguez Garcia, S. Partini, Nina Nowak, E. Lorenz, G. De Caneva, Martin Makariev, Oscar Blanch, Patrick Vogler, Aaron Dominguez, Christian Fruck, Dario Hrupec, W. Bednarek, M. A. Lopez, E. Prandini, Aldo Treves, C. Schultz, V. Scapin, P. Antoranz, M. L. Knoetig, Julia Thaele, Stefano Ansoldi, Riccardo Paoletti, J. M. Paredes, Jun Kataoka, Antonio Stamerra, A. Hadamek, Emanuele Paolo Farina, J. Storz, Robert Wagner, Y. Takahashi, Konstancja Satalecka, Michele Doro, Marc Ribó, Jelena Aleksić, P. Bangale, A. Niedzwiecki, David Paneque, Victor Stamatescu, Natalia Lewandowska, and Universitat de Barcelona
Subjects: Astrofísica, PARTICLE-ACCELERATION, Radio galaxy, Flux, Astrophysics, 01 natural sciences, Spectral line, LARGE-AREA TELESCOPE, MAGIC TELESCOPES, Raigs gamma, Jets (Astrofísica), Galaxies: active, Galaxies: individual: NGC 1275, Galaxies: jets, Gamma rays: galaxies, MAGIC (telescope), 010303 astronomy & astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, COSMIC-RAYS, galaxies: active, galaxies: jets, galaxies: individual (NGC1275/3C 84), gamma rays: galaxies, ACTIVE GALACTIC NUCLEI, PERSEUS CLUSTER, TEV EMISSION, 3C 84, CHANDRA VIEW, LAC OBJECTS, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, 010308 nuclear & particles physics, Gamma rays, Física atmosférica, Light curve, Galaxies, Galaxy, Galàxies, Astrophysical jets, Galàxies actives, Active galaxies, ddc:520
Abstract: The radio galaxy NGC 1275, recently identified as a very high energy (VHE, >100 GeV) gamma-ray emitter by MAGIC, is one of the few non-blazar AGN detected in the VHE regime. In order to better understand the origin of the gamma-ray emission and locate it within the galaxy, we studied contemporaneous multi-frequency observations of NGC 1275 and modeled the overall spectral energy distribution (SED). We analyzed unpublished MAGIC observations carried out between Oct. 2009 and Feb. 2010, and the previously published ones taken between Aug. 2010 and Feb. 2011. We studied the multi-band variability and correlations by analyzing data of Fermi-LAT (0.1-100 GeV), as well as Chandra (X-ray), KVA (optical) and MOJAVE (radio) data taken during the same period. Using customized Monte Carlo simulations corresponding to early MAGIC stereo data, we detect NGC 1275 also in the earlier campaign. The flux level and energy spectra are similar to the results of the second campaign. The monthly light curve >100 GeV shows a hint of variability at the 3.6 sigma level. In the Fermi-LAT band, both flux and spectral shape variabilities are reported. The optical light curve is variable and shows a clear correlation with the gamma-ray flux >100 MeV. In radio, 3 compact components are resolved in the innermost part of the jet. One of them shows a similar trend as the LAT and KVA light curves. The 0.1-650 GeV spectra measured simultaneously with MAGIC and Fermi-LAT can be well fitted either by a log-parabola or by a power-law with a sub-exponential cutoff for both campaigns. A single-zone synchrotron-self-Compton model, with an electron spectrum following a power-law with an exponential cutoff, can explain the broadband SED and the multi-band behavior of the source. However, this model suggests an untypical low bulk-Lorentz factor or a velocity alignment closer to the line of sight than the pc-scale radio jet., 14 pages, 11 figures, accepted for publication in A&A
Published: 2014

31. Infectivity-Neutralizing and Hemagglutinin-Inhibiting Antibody Responses to Respiratory Coronavirus Infections of Cattle in Pathogenesis of Shipping Fever Pneumonia

Author: Mamie L. Burrell, Kathy L. O'Reilly, J. Storz, and Xiaoqing Lin
Subjects: Microbiology (medical), Clinical Biochemistry, Immunology, Pneumonia, Viral, Biology, medicine.disease_cause, Antibodies, Viral, Immunoglobulin G, Veterinary Immunology, Microbiology, Neutralization Tests, medicine, Immunology and Allergy, Animals, Viral shedding, Epizootic, Coronavirus, Coronavirus, Bovine, Hemagglutination Tests, medicine.disease, Virology, Pneumonia, medicine.anatomical_structure, Immunoglobulin M, biology.protein, Cattle, Antibody, Coronavirus Infections, Respiratory tract
Abstract: Respiratory bovine coronaviruses (RBCV) emerged as an infectious agent most frequently isolated from respiratory tract samples of cattle with acute respiratory tract diseases. Infectivity-neutralizing (IN) and hemagglutinin-inhibiting (HAI) antibodies induced by RBCV infections were monitored in sequential serum samples collected from cattle during a naturally evolving and experimentally monitored epizootic of shipping fever pneumonia (SFP). Cattle nasally shedding RBCV at the beginning of the epizootic started with low levels of serum IN and HAI antibodies. An increase in serum IN antibody after day 7 led to reduction of virus shedding in nasal secretions by the majority of the cattle between days 7 and 14. A substantial rise in the serum HAI antibody was observed during the initial phase among the sick but not the clinically normal cattle which were infected with RBCV. The RBCV isolation-positive cattle that developed fatal SFP had minimal serum IN and HAI antibodies during the course of disease development. Cattle that remained negative in RBCV isolation tests entered this epizootic with high levels of serum IN and HAI antibodies, which dramatically increased during the next two weeks. Protection against SFP was apparently associated with significantly higher levels of serum IN antibodies at the beginning of the epizootic. The RBCV-neutralizing activity is associated with serum immunoglobulin G (IgG), particularly the IgG2 subclass, while RBCV-specific HAI antibody is related to both serum IgG and IgM fractions.
Published: 2001
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32. Antibody responses to respiratory coronavirus infections of cattle during shipping fever pathogenesis

Author: J. Storz, Xiaoqing Lin, Purdy Cw, Raymond W. Loan, and K. L. O’Reilly
Subjects: Cattle Diseases, Antibodies, Viral, medicine.disease_cause, Article, Immune system, Virology, medicine, Animals, Coronaviridae, Pasteurellosis, Pneumonic, Viral shedding, Respiratory Tract Infections, Epizootic, Bovine coronavirus, Coronavirus, Coronavirus, Bovine, Viral Structural Proteins, biology, General Medicine, medicine.disease, biology.organism_classification, Virus Shedding, Nasal Mucosa, Pneumonia, Immunology, biology.protein, Cattle, Antibody, Coronavirus Infections
Abstract: Summary. Antibody responses against respiratory bovine coronavirus (RBCV) infections were monitored in cattle from the onset of a naturally occurring severe shipping fever (SF) epizootic to complete recovery of affected cattle or fatal outcomes. The infection with RBCV was detected in nasal secretions of 86 cattle, and 81 of them developed acute respiratory tract disease, including fatal pneumonia. Cattle nasally shedding RBCV at the beginning of the epizootic experienced characteristic primary immune responses with specific antibodies for hemagglutinin-esterase (HE) and spike (S) glycoproteins. Virus shedding in nasal secretions of the majority of the cattle ceased between days 7 and 14 with the appearance of HE- and S-specific antibodies. Nasal samples and lung tissues from 9 of the 10 fatal cases had high titers of RBCV, but these cattle had only IgM responses to RBCV infections. Cattle remaining negative in RBCV isolation tests entered this epizootic with antibodies against HE and S. Protection against respiratory tract disease was apparently associated with high level of opsonic and virus-neutralizing IgG2. The HE and S glycoproteins were recognized earliest by the bovine immune system while the N protein induced antibody responses during the later stage of initial infection and the early stage of reinfection. The membrane (M) glycoprotein was the least immunogenic of the major viral structural proteins.
Published: 2000

33. Isolation of respiratory bovine coronavirus, other cytocidal viruses, and Pasteurella spp from cattle involved in two natural outbreaks of shipping fever

Author: Xiaoqing Lin, Mamie L. Burrell, Glynn H. Frank, Robert E. Briggs, Charles W. Purdy, J. Storz, Robert E. Truax, and Raymond W. Loan
Subjects: Male, Pasteurella multocida, animal diseases, Biology, Antibodies, Viral, medicine.disease_cause, Disease Outbreaks, Neutralization Tests, medicine, Animals, Pasteurella, Pasteurellosis, Pneumonic, Respiratory system, Mannheimia haemolytica, Herpesvirus 1, Bovine, Coronavirus, Bovine coronavirus, Coronavirus, Bovine, General Veterinary, Outbreak, Hemagglutination Inhibition Tests, biology.organism_classification, medicine.disease, Isolation (microbiology), Virology, biology.protein, Cattle, Female, Nasal Cavity, Antibody, Coronavirus Infections, Pasteurellosis
Abstract: Objective—To identify cytocidal viruses and Pasteurella spp that could be isolated from cattle involved in 2 natural outbreaks of shipping fever. Design—105 and 120 castrated male 4- to 8-monthold feedlot cattle involved in 1997 and 1998 outbreaks, respectively. Animals—Nasal swab specimens and blood samples were collected, and cattle were vaccinated on arrival at an order-buyer barn from 4 local auction houses. Four days later, they were transported to a feedlot, and additional nasal swab specimens and blood samples were collected. Nasal swab specimens were submitted for virus isolation and bacterial culture; blood samples were submitted for measurement of respiratory bovine coronavirus (RBCV) hemagglutinin inhibition titers. Results—93 of 105 cattle and 106 of 120 cattle developed signs of respiratory tract disease during 1997 and 1998, respectively, and RBCV was isolated from 81 and 89 sick cattle, respectively, while at the orderbuyer's barn or the day after arrival at the feedlot. During the 1997 outbreak, bovine herpesvirus 1 was isolated from 2 cattle at the order-buyer's barn and from 5 cattle 7 and 14 days after arrival at the feedlot, and parainfluenza virus 3 was isolated from 4 cattle 14 days after arrival at the feedlot. During the 1998 outbreak, bovine herpesvirus 1 was isolated from 2 cattle at the order-buyer's barn and on arrival at the feedlot and from 5 cattle 7 and 14 days after arrival at the feedlot, and parainfluenza virus 3 was isolated from 1 animal the day of, and from 18 cattle 7 and 14 days after, arrival at the feedlot. Pasteurella spp was cultured from 4 and 6 cattle at the order-buyer's barn and from 92 and 72 cattle on arrival at the feedlot during the 1997 and 1998 outbreaks, respectively. Conclusion and Clinical Relevance—Results suggest that RBCV may play a causative role in outbreaks of shipping fever in cattle. More than 80% of the sick cattle shed RBCV at the beginning of 2 outbreaks when the Pasteurella spp infection rate was low. (J Am Vet Med Assoc 2000;216:1599–1604)
Published: 2000

34. جداسازی ویروسهای parapox از انسان و دامها: کشت و تغییرات سلولی در سلولیهای جنینی طحال گاو

Author: م. حسامی, D.A. Keney, L. D. Pearson, and J. Storz
Subjects: Veterinary medicine, SF600-1100
Published: 1978
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35. [Untitled]

Author: Vladimir N. Chouljenko, J. Storz, Konstantin G. Kousoulas, and Xiaoqing Lin
Subjects: Genetics, chemistry.chemical_classification, General Medicine, Biology, medicine.disease_cause, Molecular biology, Genome, Amino acid, Open reading frame, chemistry, Virology, Complementary DNA, medicine, Nucleotide, Molecular Biology, Gene, Bovine coronavirus, Coronavirus
Abstract: The 3′-ends of the genomes (9538 bp) of two wild-type respiratory bovine coronavirus (RBCV) isolates LSU and OK were obtained by cDNA sequencing. In addition, the 3′-end of the genome (9545) of the wild-type enteric bovine coronavirus (EBCV) strain LY-138 was assembled from available sequences and by cDNA sequencing of unknown genomic regions. Comparative analyses of RBCV and EBCV nucleotide and deduced amino acid sequences revealed that RBCV-specific nucleotide and amino acid differences were disproportionally concentrated within the S gene and the genomic region between the S and E genes. Comparisons among virulent and avirulent BCV strains revealed that virulence-specific nucleotide and amino acid changes were located within the S and E genes, and the 32 kDa open reading frame.
Published: 1998

36. Rapid and multi-band variability of the TeV-bright active nucleus of the galaxy IC 310

Author: Dario Hrupec, M. A. Lopez, I. Lozano, D. Dominis Prester, Takashi Saito, S. Rügamer, Juan Abel Barrio, R. Zanin, D. Borla Tridon, A. Saggion, Adrian Biland, J. Becerra González, Francisco Prada, Reiko Orito, M. Salvati, A. Sillanpää, J. Rico, I. Snidaric, Mario Meucci, Masahiro Teshima, Daniela Dorner, Stefano Covino, Christian Fruck, M. L. Knoetig, T. Krähenbühl, Nikola Godinovic, Benito Marcote, S. Wilbert, Kari Nilsson, Daniel Ferenc, Abelardo Moralejo, M. V. Fonseca, Tomislav Terzić, A. De Angelis, K. Berger, S. Spiro, E. Lorenz, D. Tescaro, Mosè Mariotti, A.-K. Overkemping, Nijil Mankuzhiyil, E. Prandini, P. Munar-Adrover, Silvia Preziuso, J. Moldón, A. Boller, L. Cossio, M. Gaug, Ignasi Reichardt, Giacomo Bonnoli, M. Palatiello, J. Kushida, Q. Weitzel, Tihomir Surić, Aldo Treves, Artemio Herrero, M. Doert, Jose Luis Contreras, D. Carreto Fidalgo, Juan Cortina, P. Temnikov, Marc Ribó, Patrick Vogler, K. Saito, B. Steinke, G. Maneva, Elisa Bernardini, Riccardo Paoletti, L. Font, V. Kadenius, Fabio Zandanel, Shan Sun, S. Paiano, L. Maraschi, Karl Mannheim, Felix Spanier, G. De Caneva, Ivica Puljak, Gianluca Giavitto, L. A. Antonelli, Elina Lindfors, Daniel Mazin, D. Garrido Terrats, Natalia Lewandowska, J. Masbou, Pierre Colin, Jörn Wilms, P. Fortin, Thomas Bretz, S. N. Shore, M. I. Martínez, Francesco Dazzi, A. González Muñoz, Saverio Lombardi, S. Bonnefoy, A. La Barbera, Konstancja Satalecka, J. M. Paredes, Antonio Stamerra, Hajime Takami, V. Scalzotto, Michele Doro, Diego F. Torres, Julia Thaele, M. Uellenbeck, Fabrizio Tavecchio, D. Häfner, R. Mirzoyan, R. Reinthal, Dominik Elsaesser, S. Partini, Wolfgang Rhode, D. Eisenacher, U. Barres de Almeida, Damir Lelas, J. Krause, Ana Babić, Emanuele Paolo Farina, B. De Lotto, Aaron Dominguez, C. Delgado Mendez, S. R. Gozzini, Dorota Sobczyńska, T. Dauser, A. Hadamek, Matthias Kadler, W. Idec, J. Storz, E. Carmona, Markus Garczarczyk, Martin Makariev, Nina Nowak, F. Krauß, E. Colombo, P. Antoranz, Oscar Blanch, P. G. Prada Moroni, Ralph Bock, L. O. Takalo, O. Tibolla, Robert Wagner, C. Schultz, V. Scapin, T. Schweizer, Jelena Aleksić, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Nakajima, A. Niedzwiecki, Jose Miguel Miranda, F. Borracci, David Paneque, K. Mallot, R. J. García López, Massimo Persic, Julian Sitarek, J. Hose, Daniela Hadasch, T. Toyama, P. Da Vela, Victor Stamatescu, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Universität Erlangen-Nürnberg - Erlangen, German Aerospace Center (DLR), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), and Universitat de Barcelona
Subjects: Astrofísica, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Photon, Spectral shape analysis, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Radio galaxy, Raigs còsmics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], X-ray astronomy, Galaxies: individual: IC 310, galaxies active, galaxies individual, IC 310, gamma rays galaxies, X-rays galaxies, Gamma ray astronomy, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Galaxies: active, Gamma rays: galaxies, X-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Astronomia de raigs gamma, Blazar, Cosmic rays, ComputingMilieux_MISCELLANEOUS, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Light curve, Galaxy, Astronomia de raigs X, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galàxies actives, Active galaxies, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius, Order of magnitude
Abstract: Context. The radio galaxy IC 310 has recently been identified as a gamma-ray emitter based on observations at GeV energies with Fermi-LAT and at very high energies (VHE, E>100GeV) with the MAGIC telescopes. Originally classified as a head-tail radio galaxy, the nature of this object is subject of controversy since its nucleus shows blazar-like behavior. Aims. In order to understand the nature of IC 310 and the origin of the VHE emission we studied the spectral and flux variability of IC 310 from the X-ray band to the VHE gamma-ray regime. Methods. The light curve of IC 310 above 300GeV has been measured with the MAGIC telescopes from Oct. 2009 to Feb. 2010. Fermi-LAT data (2008-2011) in the 10-500GeV energy range were also analyzed. In X-ray, archival observations from 2003 to 2007 with XMM, Chandra, and Swift-XRT in the 0.5-10keV band were studied. Results. The VHE light curve reveals several high-amplitude and short-duration flares. Day-to-day flux variability is clearly present. The photon index between 120GeV and 8TeV remains at the value $\Gamma\sim2.0$ during both low and high flux states. The VHE spectral shape does not show significant variability, whereas the flux at 1TeV changes by a factor of $\sim7$. Fermi-LAT detected only eight gamma-ray events in the energy range 10GeV-500GeV in three years of observation. The measured photon index of $\Gamma=1.3\pm0.5$ in the Fermi-LAT range is very hard. The X-ray measurements show strong variability in flux and photon index. The latter varied from $1.76\pm0.07$ to $2.55\pm0.07$. Conclusion. The rapid variability measured confirms the blazar-like behavior of IC 310. The TeV emission seems to originate from scales of less than 80 Schwarzschild radii within the compact core of its FRI radio jet with orientation angle 10deg-38deg. The SED resembles that of an extreme blazar, albeit the luminosity is more than two orders of magnitude lower., Comment: 9 pages, 5 figures, 4 tables. Accepted for publication in A&A
Published: 2013
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37. Observations of the magnetars 4U 0142+61 and 1E 2259+586 with the MAGIC telescopes

Author: K. Berger, E. Prandini, Aldo Treves, Felix Spanier, J. Moldón, Daniel Ferenc, R. Zanin, A. Saggion, Adrian Biland, D. Dominis Prester, A. Boller, S. Partini, E. Colombo, Ivica Puljak, Francisco Prada, L. Cossio, Pierre Colin, Dario Hrupec, M. A. Lopez, Ralph Bock, L. O. Takalo, Mario Meucci, V. Scapin, S. Bonnefoy, R. Reinthal, Dominik Elsaesser, Daniela Dorner, Nijil Mankuzhiyil, J. M. Paredes, P. Munar-Adrover, P. G. Prada Moroni, U. Barres de Almeida, Damir Lelas, Nikola Godinovic, Benito Marcote, Konstancja Satalecka, P. Temnikov, Michele Doro, Antonio Stamerra, Artemio Herrero, Dorota Sobczyńska, Q. Weitzel, Tihomir Surić, D. Carreto Fidalgo, Thomas Bretz, S. N. Shore, Fabio Zandanel, M. Pilia, Aaron Dominguez, Shan Sun, Takashi Saito, Ignasi Reichardt, M. Gaug, Jelena Aleksić, Stefano Covino, Giacomo Bonnoli, Marc Ribó, Martin Makariev, Oscar Blanch, Reiko Orito, T. Schweizer, O. Tibolla, R. Mirzoyan, V. Kadenius, S. Paiano, Karl Mannheim, Julian Sitarek, Nanda Rea, S. Rügamer, A. López-Oramas, K. Saito, D. Eisenacher, A. Niedzwiecki, Wlodek Bednarek, Alessandro Carosi, Natalia Lewandowska, Juan Abel Barrio, M. Asensio, J. Hose, M. Doert, Elisa Bernardini, D. Borla Tridon, F. Jankowski, A. La Barbera, Ruben Lopez-Coto, M. Uellenbeck, A. Hadamek, G. Maneva, D. Tescaro, D. Nakajima, Daniel Nieto, T. Toyama, J. Storz, Mosè Mariotti, G. De Caneva, E. Carmona, Markus Garczarczyk, David Paneque, M. Palatiello, Jose Miguel Miranda, Nina Nowak, M. L. Knoetig, D. Garrido Terrats, P. Antoranz, C. Delgado Mendez, S. R. Gozzini, K. Mallot, Wolfgang Rhode, A. De Angelis, J. Rico, L. Maraschi, M. V. Fonseca, Francesco Dazzi, Tomislav Terzić, Saverio Lombardi, R. J. García López, V. Scalzotto, Elina Lindfors, Christian Fruck, M. Salvati, E. Leonardo, Daniel Mazin, A. Sillanpää, Gianluca Giavitto, P. Da Vela, B. Steinke, A. González Muñoz, Riccardo Paoletti, Victor Stamatescu, J. Masbou, I. Lozano, D. Hadasch, M. I. Martínez, Robert Wagner, Massimo Persic, T. Krähenbühl, C. Schultz, Masahiro Teshima, J. Kushida, Jose Luis Contreras, L. Font, Hajime Takami, Juan Cortina, Kari Nilsson, Patrick Vogler, L. A. Antonelli, Fabrizio Tavecchio, I. Snidaric, S. Spiro, E. Lorenz, Diego F. Torres, Abelardo Moralejo, J. Krause, B. De Lotto, S. Klepser, Universitat de Barcelona, Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Friedrich-Alexander-Universität, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], High energy, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], astro-ph.GA, Astronomy, FOS: Physical sciences, Astrophysics, Magnetar, 01 natural sciences, Neutron stars, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Telescope, law, Gamma ray astronomy, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Astronomia de raigs gamma, Analysis software, 010306 general physics, 010303 astronomy & astrophysics, Cherenkov radiation, Estels de neutrons, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Telescopis, Magic (programming), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, radiation mechanisms: non-thermal, stars: magnetars, gamma rays: stars, stars: individual: 4U 0142+61, 1E 2259+586, Neutron star, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astronomia, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, High magnetic field, Telescopes
Abstract: Astronomy and astrophysics 549(A23), 1-4 (2013). doi:10.1051/0004-6361/201220275, Magnetars are an extreme, highly magnetized class of isolated neutron stars whose large X-ray luminosity is believed to be driven by their high magnetic field. In this work we study for the first time the possible very high energy gamma-ray emission above 100 GeV from magnetars, observing the sources 4U 0142+61 and 1E 2259+586. We observed the two sources with atmospheric Cherenkov telescopes in the very high energy range (E > 100 GeV). 4U 0142+61 was observed with the MAGIC I telescope in 2008 for ~25 h and 1E 2259+586 was observed with the MAGIC stereoscopic system in 2010 for ~14 h. The data were analyzed with the standard MAGIC analysis software. Neither magnetar was detected. Upper limits to the differential and integral flux above 200 GeV were computed using the Rolke algorithm. We obtain integral upper limits to the flux of 1.52*10^-12cm^-2 s^-1 and 2.7*10^-12cm^-2 s^-1 with a confidence level of 95% for 4U 0142+61 and 1E 2259+586, respectively. The resulting differential upper limits are presented together with X-ray data and upper limits in the GeV energy range., Published by EDP Sciences, Les Ulis
Published: 2012

38. High zenith angle observations of PKS 2155-304 with the MAGIC-I telescope

Author: J. Aleksić, E. A. Alvarez, L. A. Antonelli, P. Antoranz, M. Asensio, M. Backes, U. Barres de Almeida, J. A. Barrio, D. Bastieri, J. Becerra González, W. Bednarek, A. Berdyugin, K. Berger, E. Bernardini, A. Biland, O. Blanch, R. K. Bock, A. Boller, G. Bonnoli, D. Borla Tridon, I. Braun, T. Bretz, A. Cañellas, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, L. Cossio, S. Covino, F. Dazzi, A. De Angelis, G. De Caneva, E. De Cea del Pozo, B. De Lotto, C. Delgado Mendez, A. Diago Ortega, M. Doert, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, D. Eisenacher, D. Elsaesser, D. Ferenc, M. V. Fonseca, L. Font, C. Fruck, R. J. García López, M. Garczarczyk, D. Garrido, G. Giavitto, N. Godinović, S. R. Gozzini, D. Hadasch, D. Häfner, A. Herrero, D. Hildebrand, D. Höhne-Mönch, J. Hose, D. Hrupec, T. Jogler, H. Kellermann, S. Klepser, T. Krähenbühl, J. Krause, J. Kushida, A. La Barbera, D. Lelas, E. Leonardo, N. Lewandowska, E. Lindfors, S. Lombardi, M. López, R. López, A. López-Oramas, E. Lorenz, M. Makariev, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, J. M. Miranda, R. Mirzoyan, J. Moldón, A. Moralejo, P. Munar-Adrover, A. Niedzwiecki, D. Nieto, K. Nilsson, N. Nowak, R. Orito, S. Paiano, D. Paneque, R. Paoletti, S. Pardo, J. M. Paredes, S. Partini, M. A. Perez-Torres, M. Persic, L. Peruzzo, M. Pilia, J. Pochon, F. Prada, P. G. Prada Moroni, E. Prandini, I. Puerto Gimenez, I. Puljak, I. Reichardt, R. Reinthal, W. Rhode, M. Ribó, J. Rico, S. Rügamer, A. Saggion, K. Saito, T. Y. Saito, M. Salvati, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, M. Shayduk, S. N. Shore, A. Sillanpää, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, S. Spiro, V. Stamatescu, A. Stamerra, B. Steinke, J. Storz, N. Strah, S. Sun, T. Surić, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzić, D. Tescaro, M. Teshima, O. Tibolla, D. F. Torres, A. Treves, M. Uellenbeck, H. Vankov, P. Vogler, R. M. Wagner, Q. Weitzel, V. Zabalza, F. Zandanel, and R. Zanin
Subjects: Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, law.invention, law, 0103 physical sciences, MAGIC (telescope), 010303 astronomy & astrophysics, Zenith, PKS 2155-304, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, BL Lacertae objects: individual: PKS 2155-304, astroparticle physics, methods: data analysis, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Light curve, Crab Nebula, 13. Climate action, Space and Planetary Science, Galàxies actives, astro-ph.CO, Active galaxies, Spectral energy distribution, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The high frequency peaked BL Lac PKS 2155-304 with a redshift of z=0.116 was discovered in 1997 in the very high energy (VHE, E >100GeV) gamma-ray range by the University of Durham Mark VI gamma-ray Cherenkov telescope in Australia with a flux corresponding to 20% of the Crab Nebula flux. It was later observed and detected with high significance by the Southern Cherenkov observatory H.E.S.S. Detection from the Northern hemisphere is difficult due to challenging observation conditions under large zenith angles. In July 2006, the H.E.S.S. collaboration reported an extraordinary outburst of VHE gamma-emission. During the outburst, the VHE gamma-ray emission was found to be variable on the time scales of minutes and with a mean flux of ~7 times the flux observed from the Crab Nebula. Follow-up observations with the MAGIC-I standalone Cherenkov telescope were triggered by this extraordinary outburst and PKS 2155-304 was observed between 28 July to 2 August 2006 for 15 hours at large zenith angles. Here we present our studies on the behavior of the source after its extraordinary flare and an enhanced analysis method for data taken at high zenith angles. We developed improved methods for event selection that led to a better background suppression. The averaged energy spectrum we derived has a spectral index of -3.5 +/- 0.2 above 400GeV, which is in good agreement with the spectral shape measured by H.E.S.S. during the major flare on MJD 53944. Furthermore, we present the spectral energy distribution modeling of PKS 2155-304. With our observations we increased the duty cycle of the source extending the light curve derived by H.E.S.S. after the outburst. Finally, we find night-by-night variability with a maximal amplitude of a factor three to four and an intranight variability in one of the nights (MJD 53945) with a similar amplitude., 10 pages, 9 figures; Accepted for publication in A&A
Published: 2012

39. Mrk 421 active state in 2008: the MAGIC view, simultaneous multi-wavelength observations and SSC model constrained

Author: Jose Luis Contreras, Juan Cortina, J. Moldón, D. Hildebrand, L. Peruzzo, E. Lindfors, Diego F. Torres, R. Reinthal, M. Pasanen, J. Becerra González, M. Garczarczyk, L. Maraschi, Dominik Elsaesser, G. De Caneva, M. Doert, Michael Backes, Damir Lelas, Marc Ribó, Mario Meucci, Dorota Sobczyńska, Christian Fruck, A. Boller, L. Cossio, A. Carosi, C. Schultz, Kazuo Saito, Giacomo Bonnoli, P. G. Prada Moroni, V. Scalzotto, R. K. Bock, O. Tibolla, J. M. Paredes, Hiroko Miyamoto, T. Jogler, M. Shayduk, J. Krause, B. De Lotto, Jelena Aleksić, K. Nilsson, A. Herrero, M. Pilia, E. A. Alvarez, C. Delgado Mendez, D. Mazin, B. Huber, S. Partini, D. Höhne-Mönch, S. Klepser, E. De Cea del Pozo, Stefano Covino, J. Storz, P. Munar-Adrover, Daniel Ferenc, Denis Bastieri, P. Temnikov, E. Prandini, Andrei Berdyugin, Tihomir Surić, Patrick Vogler, David Paneque, H. Vankov, Nikola Godinovic, K. Berger, Aldo Treves, Abelardo Moralejo, E. Colombo, A. Saggion, P. Antoranz, Adrian Biland, H. Takami, Fabio Zandanel, Ilana M. Braun, R. Paoletti, Silvia Pardo, D. Tescaro, Daniela Dorner, M. Lopez, Karl Mannheim, J. Rico, V. Scapin, M. Asensio, Julian Sitarek, Ivica Puljak, J. Hose, Daniela Hadasch, L. O. Takalo, Miguel A. Pérez-Torres, Felix Spanier, Dario Hrupec, Reiko Orito, Wlodek Bednarek, T. Saito, Martin Makariev, Oscar Blanch, A. Lopez, Mosè Mariotti, M. Salvati, Roberta Zanin, D. Häfner, A. La Barbera, S. Spiro, E. Lorenz, A. Stamerra, D. Dominis Prester, A. Diago Ortega, Robert Wagner, T. Schweizer, R. J. García López, Elisa Bernardini, L. A. Antonelli, D. Garrido, A. Cañellas, Jose Miguel Miranda, Tomislav Terzić, Aaron Dominguez, Miriam Lucio Martinez, Francisco Prada, Felicitas Pauss, A. Sillanpää, A. De Angelis, Saverio Lombardi, Quirin Weitzel, Ignasi Reichardt, R. Mirzoyan, Victor Zabalza, Massimo Persic, Igor Oya, Fabrizio Tavecchio, Ll. Font, Daniel Nieto, J. Pochon, T. Krahenbuh, Thomas Bretz, Masahiro Teshima, Gianluca Giavitto, P. Colin, G. Maneva, Konstancja Satalecka, M. Uellenbeck, Michele Doro, N. Strah, E. Carmona, Wolfgang Rhode, Hanna Kellermann, Francesco Dazzi, E. Leonardo, N. Mankuzhiyil, M. V. Fonseca, S. N. Shore, B. Steinke, S. Rügamer, Juan Abel Barrio, and D. Borla Tridon
Subjects: Radiation mechanisms: non-thermal, ELECTRON ACCELERATION, BACKGROUND-RADIATION, Astrophysics, radiation mechanisms: non-thermal / BL Lacertae objects: individual: Mrk 421, 01 natural sciences, law.invention, Raigs gamma, law, Observacions astronòmiques, MAGIC (telescope), 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, FAST TEV VARIABILITY, CORRELATED VARIABILITY, BL Lacertae objects: individual: Mrk 421, Astronomy and Astrophysics, Space and Planetary Science, SELF-COMPTON MODEL, symbols, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Doppler effect, Astronomical observations, GALACTIC NUCLEI, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, Telescope, symbols.namesake, 0103 physical sciences, Blazar, Cherenkov radiation, BL-LACERTAE OBJECTS, GAMMA-RAY EMISSION, X-RAY, LAC OBJECTS, 010308 nuclear & particles physics, Gamma rays, Galaxies, Galàxies, Crab Nebula, 13. Climate action, Sky, ddc:520
Abstract: Context: The blazar Markarian 421 is one of the brightest TeV gamma-ray sources of the northern sky. From December 2007 until June 2008 it was intensively observed in the very high energy (VHE, E > 100 GeV) band by the single-dish Major Atmospheric Gamma-ray Imaging Cherenkov telescope (MAGIC-I). Aims: We aimed to measure the physical parameters of the emitting region of the blazar jet during active states. Methods: We performed a dense monitoring of the source in VHE with MAGIC-I, and also collected complementary data in soft X-rays and optical-UV bands; then, we modeled the spectral energy distributions (SED) derived from simultaneous multi-wavelength data within the synchrotron self--compton (SSC) framework. Results: The source showed intense and prolonged gamma-ray activity during the whole period, with integral fluxes (E > 200 GeV) seldom below the level of the Crab Nebula, and up to 3.6 times this value. Eight datasets of simultaneous optical-UV (KVA, Swift/UVOT), soft X-ray (Swift/XRT) and MAGIC-I VHE data were obtained during different outburst phases. The data constrain the physical parameters of the jet, once the spectral energy distributions obtained are interpreted within the framework of a single-zone SSC leptonic model. Conclusions: The main outcome of the study is that within the homogeneous model high Doppler factors (40, 12 pages, 7 figures. Accepted for publication in A&A 7 January 2012
Published: 2012

40. PG 1553+113: five years of observations with MAGIC

Author: R. Reinthal, Dominik Elsaesser, Damir Lelas, S. Spiro, E. Lorenz, Dorota Sobczyńska, F. D'Ammando, M. I. Martínez, Michael Backes, T. Krähenbühl, S. Klepser, Kari Nilsson, D. Tescaro, N. Strah, P. G. Prada Moroni, Denis Bastieri, Q. Weitzel, Tihomir Surić, J. Moldón, M. Pilia, Andrei Berdyugin, M. Salvati, Gianluca Giavitto, D. Dominis Prester, Karl Mannheim, A. Boller, L. Cossio, E. Colombo, O. Tibolla, E. Prandini, Jose Luis Contreras, Francisco Prada, Artemio Herrero, Juan Cortina, Aldo Treves, Daniel Ferenc, K. Saito, Hiroko Miyamoto, A. La Barbera, Daniela Dorner, C. Schultz, V. Scapin, Silvia Pardo, P. Temnikov, H. Vankov, Ilana M. Braun, Fabio Zandanel, K. Berger, J. Krause, A. Cañellas, Ivica Puljak, Pierre Colin, B. De Lotto, Victor Stamatescu, S. Partini, D. Höhne-Mönch, Jelena Aleksić, M. Shayduk, Aaron Dominguez, Tomislav Terzić, A. López-Oramas, Abelardo Moralejo, Dario Hrupec, Stefano Covino, Wlodek Bednarek, Alessandro Carosi, Patrick Vogler, J. Becerra González, Elisa Bernardini, Nijil Mankuzhiyil, D. Horan, H. Kellermann, P. Munar-Adrover, M. A. Lopez, V. Scalzotto, Felix Spanier, Riccardo Paoletti, Masahiro Teshima, Mario Meucci, Felicitas Pauss, Victor Zabalza, D. Garrido, Thomas Bretz, Julian Sitarek, D. Hildebrand, L. Peruzzo, Ralph Bock, S. N. Shore, J. Hose, Marc Ribó, M. Uellenbeck, Jose Miguel Miranda, J. M. Paredes, Martin Makariev, G. De Caneva, Daniela Hadasch, Antonio Stamerra, S. Buson, Oscar Blanch, T. Jogler, E. A. Alvarez, L. O. Takalo, J. Storz, Wolfgang Rhode, Nikola Godinovic, B. Huber, E. Carmona, Giacomo Bonnoli, E. De Cea del Pozo, Francesco Dazzi, Diego F. Torres, M. Pasanen, Hajime Takami, R. J. García López, Ignasi Reichardt, David Paneque, E. Leonardo, T. Schweizer, L. Maraschi, Elina Lindfors, Daniel Mazin, P. Antoranz, M. Doert, S. Larsson, Massimo Persic, M. Asensio, Daniel Nieto, G. Maneva, Konstancja Satalecka, Michele Doro, A. Saggion, A. Diago Ortega, Robert Wagner, Adrian Biland, Mosè Mariotti, J. Rico, A. De Angelis, Saverio Lombardi, J. Pochon, D. Häfner, R. Mirzoyan, Markus Garczarczyk, Takashi Saito, L. A. Antonelli, R. Zanin, Igor Oya, Fabrizio Tavecchio, Ll. Font, Reiko Orito, M. A. Perez-Torres, A. Sillanpää, M. V. Fonseca, Christian Fruck, B. Steinke, S. Rügamer, Juan Abel Barrio, D. Borla Tridon, C. Delgado Mendez, Aleksic J, Alvarez EA, Antonelli LA, Antoranz P, Asensio M, Backes M, Barrio JA, Bastieri D, Gonzalez JB, Bednarek W, Berdyugin A, Berger K, Bernardini E, Biland A, Blanch O, Bock RK, Boller A, Bonnoli G, Tridon DB, Braun I, Bretz T, Canellas A, Carmona E, Carosi A, Colin P, Colombo E, Contreras JL, Cortina J, Cossio L, Covino S, Dazzi F, De Angelis A, De Caneva G, del Pozo ED, De Lotto B, Mendez CD, Ortega AD, Doert M, Dominguez A, Prester DD, Dorner D, Doro M, Elsaesser D, Ferenc D, Fonseca MV, Font L, Fruck C, Lopez RJG, Garczarczyk M, Garrido D, Giavitto G, Godinovic N, Hadasch D, Hafner D, Herrero A, Hildebrand D, Ohne-Monch DH, Hose J, Hrupec D, Huber B, Jogler T, Kellermann H, Klepser S, Krahenbuhl T, Krause J, La Barbera A, Lelas D, Leonardo E, Lindfors E, Lombardi S, Lopez M, Lopez-Oramas A, Lorenz E, Makariev M, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Mariotti M, Martinez M, Mazin D, Meucci M, Miranda JM, Mirzoyan R, Miyamoto H, Moldon J, Moralejo A, Munar-Adrover P, Nieto D, Nilsson K, Orito R, Oya I, Paneque D, Paoletti R, Pardo S, Paredes JM, Partini S, Pasanen M, Pauss F, Perez-Torres MA, Persic M, Peruzzo L, Pilia M, Pochon J, Prada F, Moroni PGP, Prandini E, Puljak I, Reichardt I, Reinthal R, Rhode W, Ribo M, Rico J, Rugamer S, Saggion A, Saito K, Saito TY, Salvati M, Satalecka K, Scalzotto V, Scapin V, Schultz C, Schweizer T, Shayduk M, Shore SN, Sillanpaa A, Sitarek J, Sobczynska D, Spanier F, Spiro S, Stamatescu V, Stamerra A, Steinke B, Storz J, Strah N, Suric T, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Tibolla O, Torres DF, Treves A, Uellenbeck M, Vankov H, Vogler P, Wagner RM, Weitzel Q, Zabalza V, Zandanel F, Zanin R, Buson S, Horan D, Larsson S, and DAmmando F
Subjects: Flux, Astrophysics, 01 natural sciences, Raigs gamma, MAGIC (telescope), 010303 astronomy & astrophysics, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), TEV BLAZARS, Gamma ray, radiation mechanisms: non-thermal, gamma-rays: observations, BL Lacertae objects: individual (PG 1553+113), astro-ph.CO, BL LACERTAE OBJECTS, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Astrophysics - Cosmology and Nongalactic Astrophysics, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, FERMI, 0103 physical sciences, Blazar, MULTIWAVELENGTH OBSERVATIONS, BL Lacertae objects: individual (PG 1553+113) – gamma rays: galaxies – radiation mechanisms: non-thermal, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Galaxies, Galàxies, EXTRAGALACTIC BACKGROUND LIGHT, Crab Nebula, Space and Planetary Science, LAC OBJECTS, ddc:520, SKY SURVEY, GAMMA-RAY EMISSION, Fermi Gamma-ray Space Telescope
Abstract: We present the results of five years (2005-2009) of MAGIC observations of the BL Lac object PG 1553+113 at very high energies (VHEs, E > 100 GeV). Power law fits of the individual years are compatible with a steady mean photon index ��= 4.27 $\pm$ 0.14. In the last three years of data, the flux level above 150 GeV shows a clear variability (probability of constant flux < 0.001%). The flux variations are modest, lying in the range from 4% to 11% of the Crab Nebula flux. Simultaneous optical data also show only modest variability that seems to be correlated with VHE gamma ray variability. We also performed a temporal analysis of (all available) simultaneous Fermi/LAT data of PG 1553+113 above 1 GeV, which reveals hints of variability in the 2008-2009 sample. Finally, we present a combination of the mean spectrum measured at very high energies with archival data available for other wavelengths. The mean spectral energy distribution can be modeled with a one-zone Synchrotron Self Compton (SSC) model, which gives the main physical parameters governing the VHE emission in the blazar jet., 11 pages, 6 figures, accepted for publication in ApJ
Published: 2012

41. Discovery of VHE gamma-rays from the blazar 1ES 1215+303 with the MAGIC Telescopes and simultaneous multi-wavelength observations

Author: I. Snidaric, Aaron Dominguez, M. Makariev, Victor Zabalza, S. Spiro, E. Lorenz, Daniela Dorner, R. J. García López, I. Puerto Gimenez, Natalia Lewandowska, S. Larsson, Massimo Persic, Elisa Bernardini, D. Hildebrand, F. Jankowski, A. La Barbera, Abelardo Moralejo, W. Bednarek, Fabrizio Tavecchio, K. Berger, M. I. Martínez, Gianluca Giavitto, E. A. Alvarez, A. González Muñoz, K. Saito, Patrick Vogler, Silvia Pardo, Dario Hrupec, Joni Tammi, B. Huber, P. G. Prada Moroni, S. Partini, A. De Angelis, J. Becerra González, M. A. Lopez, S. Rügamer, E. De Cea del Pozo, A. Boller, Ignasi Reichardt, Juan Abel Barrio, L. Cossio, A. Diago Ortega, Robert Wagner, T. Krähenbühl, D. Eisenacher, O. Tibolla, Mario Meucci, V. Scapin, Artemio Herrero, L. Maraschi, D. Borla Tridon, G. Maneva, Stefano Ansoldi, E. Carmona, Jelena Aleksić, N. Strah, Nikola Godinovic, Markus Garczarczyk, Riccardo Paoletti, Andrei Berdyugin, Tomislav Terzić, T. Jogler, R. Zanin, A. Saggion, A. Niedzwiecki, Adrian Biland, Emilia Järvelä, Nina Nowak, Daniel Ferenc, M. Asensio, Denis Bastieri, Q. Weitzel, J. M. Paredes, C. Schultz, J. Rico, Diego F. Torres, David Paneque, Tihomir Surić, Antonio Stamerra, Oscar Blanch, Marc Ribó, Louis Antonelli, M. Salvati, V. Kadenius, S. Paiano, C. Delgado Mendez, S. R. Gozzini, M. Doert, Michael Backes, J. Hose, A. Sillanpää, M. A. Perez-Torres, Karl Mannheim, Felix Spanier, L. Font, Francesco Dazzi, M. V. Fonseca, E. Colombo, J. Krause, D. Elsaesser, J. Storz, G. Bonnoli, E. Leonardo, P. Antoranz, B. De Lotto, Nijil Mankuzhiyil, Christian Fruck, Hajime Takami, P. Munar-Adrover, Kari Nilsson, Daniel Nieto, Thomas Bretz, Konstancja Satalecka, Michele Doro, S. N. Shore, D. Dominis Prester, S. Klepser, B. Steinke, G. De Caneva, Hanna Kellermann, M. Pilia, Francisco Prada, A. López-Oramas, Alessandro Carosi, D. Garrido Terrats, A. Cañellas, Ruben Lopez-Coto, Ralph Bock, V. Scalzotto, L. O. Takalo, Wolfgang Rhode, Jose Miguel Miranda, J. Moldón, D. Häfner, S. Buson, T. Schweizer, Jose Luis Contreras, Juan Cortina, Mosè Mariotti, Ivica Puljak, Pierre Colin, Saverio Lombardi, J. Pochon, R. Reinthal, Razmik Mirzoyan, U. Barres de Almeida, Damir Lelas, Elina Lindfors, Daniel Mazin, Dorota Sobczyńska, Stefano Covino, D. Tescaro, E. Prandini, Takashi Saito, Aldo Treves, Reiko Orito, P. Da Vela, Julian Sitarek, Victor Stamatescu, P. Temnikov, Fabio Zandanel, Shan Sun, D. Hadasch, Anne Lähteenmäki, Masahiro Teshima, M. Uellenbeck, Department of Radio Science and Engineering, School services, ELEC, Aalto-yliopisto, Aalto University, and Anne Lähteenmäki Group
Subjects: gamma-rays: galaxies, Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, law.invention, Telescope, Radio telescope, law, BL Lacertae objects: individual: 1ES 1215+303, Target of opportunity, 0103 physical sciences, Gamma ray astronomy, Astronomia de raigs gamma, Blazar, 010303 astronomy & astrophysics, individual: 1ES 1215+303 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 010308 nuclear & particles physics, 213 Electronic, automation and communications engineering, electronics, Optical polarization, Astronomy and Astrophysics, Galaxies, Galàxies, galaxies [gamma-rays], Space and Planetary Science, 115 Astronomy and space science, Spectral energy distribution, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, BL Lac object
Abstract: Context. We present the discovery of very high energy (VHE, E > 100GeV) gamma-ray emission from the BL Lac object 1ES 1215+303 by the MAGIC telescopes and simultaneous multi-wavelength data in a broad energy range from radio to gamma-rays. Aims. We study the VHE gamma-ray emission from 1ES 1215+303 and its relation to the emissions in other wavelengths. Methods. Triggered by an optical outburst, MAGIC observed the source in January-February 2011 for 20.3 hrs. The target was monitored in the optical R-band by the KVA telescope that also performed optical polarization measurements. We triggered target of opportunity observations with the Swift satellite and obtained simultaneous and quasi-simultaneous data from the Fermi Large Area Telescope and from the Mets��hovi radio telescope. We also present the analysis of older MAGIC data taken in 2010. Results. The MAGIC observations of 1ES 1215+303 carried out in January-February 2011 resulted in the first detection of the source at VHE with a statistical significance of 9.4 sigma. Simultaneously, the source was observed in a high optical and X-ray state. In 2010 the source was observed in a lower state in optical, X-ray, and VHE, while the GeV gamma-ray flux and the radio flux were comparable in 2010 and 2011. The spectral energy distribution obtained with the 2011 data can be modeled with a simple one zone SSC model, but it requires extreme values for the Doppler factor or the electron energy distribution., 10 pages, 8 figures, accepted to A&A
Published: 2012

42. Performance of the MAGIC stereo system obtained with Crab Nebula data

Author: J. M. Paredes, Antonio Stamerra, Aldo Treves, Daniel Nieto, V. Scalzotto, Daniela Dorner, Abelardo Moralejo, J. Storz, Thomas Bretz, S. N. Shore, Riccardo Paoletti, D. Häfner, R. Mirzoyan, S. Partini, Hanna Kellermann, D. Höhne-Mönch, Ignasi Reichardt, Masahiro Teshima, Petar Temnikov, W. Bednarek, Igor Oya, Fabrizio Tavecchio, Elisa Bernardini, Silvia Pardo, Pierre Colin, Ll. Font, M. Martı´nez, P. Antoranz, E. A. Alvarez, Konstancja Satalecka, A. Boller, Wolfgang Rhode, Elina Lindfors, K. Saito, L. Cossio, J. Moldón, M. Uellenbeck, Gianluca Giavitto, E. Colombo, Michele Doro, Kari Nilsson, Hiroko Miyamoto, Jelena Aleksić, D. Dominis Prester, Daniel Mazin, G. Maneva, Julian Sitarek, Fabio Zandanel, A. Saggion, Patrick Vogler, Dario Hrupec, Nikola Godinovic, M. Asensio, M. Salvati, Adrian Biland, Oscar Blanch, Ralph Bock, L. O. Takalo, Elisa Prandini, M. A. Perez-Torres, Daniela Hadasch, T. Schweizer, M. Shayduk, Artemio Herrero, David Paneque, R. Reinthal, Louis Antonelli, Jose Luis Contreras, Francisco Prada, Stefano Covino, Mosè Mariotti, Juan Cortina, A. De Angelis, Nijil Mankuzhiyil, I. Snidaric, Damir Lelas, Diego F. Torres, P. Munar-Adrover, A. Cañellas, C. Delgado Mendez, M. Pasanen, Dorota Sobczyńska, Michael Backes, J. Krause, R. J. García López, B. De Lotto, Francesco Dazzi, K. Berger, Victor Zabalza, G. De Caneva, S. Spiro, E. Lorenz, E. Carmona, A. Diago Ortega, Robert Wagner, Markus Garczarczyk, Saverio Lombardi, E. Leonardo, D. Tescaro, M. Makariev, M. Pilia, J. Pochon, A. Sillanpää, Victor Stamatescu, Felix Spanier, J. Rico, D. Hildebrand, L. Peruzzo, Takashi Saito, P. G. Prada Moroni, R. Zanin, B. Huber, O. Tibolla, Reiko Orito, Daniel Ferenc, H. Vankov, Ilana M. Braun, Massimo Persic, T. Krähenbühl, S. Klepser, G. Bonnoli, M. V. Fonseca, N. Strah, Christian Fruck, T. Jogler, B. Steinke, M. López, S. Rügamer, Juan Abel Barrio, D. Borla Tridon, I. Puljak, A. La Barbera, J. Becerra González, Mario Meucci, M. Doert, Denis Bastieri, Q. Weitzel, Tihomir Surić, Karl Mannheim, Marc Ribó, Andrei Berdyugin, J. Hose, A. López-Oramas, D. Elsaesser, Alessandro Carosi, D. Garrido, Jose Miguel Miranda, C. Schultz, V. Scapin, Felicitas Pauss, L. Maraschi, Hajime Takami, Tomislav Terzić, E. De Cea del Pozo, and A. Domi´nguez
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Stereoscopy, Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, Neutron stars, law.invention, law, Gamma ray astronomy, 0103 physical sciences, Astronomia de raigs gamma, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, MAGIC (telescope), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Zenith, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Estels de neutrons, Physics, 010308 nuclear & particles physics, ATMOSPHERIC CHERENKOV TELESCOPES, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Gamma-ray astronomy, PULSAR, gamma-ray astronomy, Cherenkov telescopes, Crab Nebula, ARRAYS, ddc:540, FLARES, TEV, Electrónica, Física nuclear, Astrophysics::Earth and Planetary Astrophysics, Electricidad, Astrophysics - Instrumentation and Methods for Astrophysics, GAMMA-RAY EMISSION, astro-ph.IM
Abstract: MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located in the Canary island of La Palma. Since autumn 2009 both telescopes have been working together in stereoscopic mode, providing a significant improvement with respect to the previous single-telescope observations. We use observations of the Crab Nebula taken at low zenith angles to assess the performance of the MAGIC stereo system. The trigger threshold of the MAGIC telescopes is 50-60 GeV. Advanced stereo analysis techniques allow MAGIC to achieve a sensitivity as good as (0.76 +/- 0.03)% of the Crab Nebula flux in 50 h of observations above 290 GeV. The angular resolution at those energies is better than ~0.07 degree. We also perform a detailed study of possible systematic effects which may influence the analysis of the data taken with the MAGIC telescopes., Comment: 15 pages, 19 figures, 4 tables, added run-by-run systematics study, and the study of angular resolution as the function of the distance to the camera centre, accepted for publication in Astroparticle Physics
Published: 2012

43. Phase-resolved energy spectra of the Crab pulsar in the range of 50-400 GeV measured with the MAGIC telescopes

Author: Adrian Biland, Aaron Dominguez, K. Berger, L. Maraschi, Elina Lindfors, Daniel Mazin, Fabio Zandanel, E. Colombo, S. Partini, D. Höhne-Mönch, Felix Spanier, Abelardo Moralejo, K. Saito, J. M. Paredes, Ralph Bock, L. O. Takalo, Victor Stamatescu, Stefano Covino, Antonio Stamerra, M. V. Fonseca, M. Uellenbeck, M. Shayduk, R. Reinthal, D. Eisenacher, V. Scalzotto, P. Antoranz, Oscar Blanch, Victor Zabalza, Christian Fruck, Patrick Vogler, Dominik Elsaesser, J. Moldón, Ignasi Reichardt, D. Dominis Prester, P. G. Prada Moroni, E. Carmona, Markus Garczarczyk, Silvia Pardo, T. Schweizer, Damir Lelas, J. Storz, D. Häfner, M. Doert, Michael Backes, T. Jogler, J. Krause, B. De Lotto, O. Tibolla, B. Steinke, C. Delgado Mendez, Nina Nowak, L. A. Antonelli, Nijil Mankuzhiyil, P. Munar-Adrover, Francisco Prada, Dorota Sobczyńska, G. Maneva, Konstancja Satalecka, Michele Doro, S. Klepser, Mosè Mariotti, Daniel Ferenc, Jelena Aleksić, Francesco Dazzi, Daniela Dorner, Elisa Prandini, M. A. Perez-Torres, H. Vankov, A. Niedzwiecki, W. Bednarek, S. Rügamer, Diego F. Torres, Ilana M. Braun, M. Pilia, E. Leonardo, Juan Abel Barrio, Kari Nilsson, David Paneque, Fabrizio Tavecchio, M. Asensio, Aldo Treves, D. Borla Tridon, A. Sillanpää, I. Puljak, Masahiro Teshima, Petar Temnikov, Julian Sitarek, Ll. Font, Elisa Bernardini, H. Kellermann, A. Cañellas, E. De Cea del Pozo, Saverio Lombardi, Takashi Saito, Gianluca Giavitto, G. Bonnoli, Pierre Colin, R. J. García López, J. Pochon, Jose Luis Contreras, A. Diago Ortega, Robert Wagner, Riccardo Paoletti, Dario Hrupec, Reiko Orito, J. Hose, Daniela Hadasch, Juan Cortina, M. A. Lopez, I. Snidaric, A. De Angelis, M. Salvati, Tomislav Terzić, J. Kushida, Thomas Bretz, S. N. Shore, R. Mirzoyan, S. Spiro, E. Lorenz, Wolfgang Rhode, Daniel Nieto, Marc Ribó, A. Boller, L. Cossio, Artemio Herrero, M. Makariev, J. Rico, I. Puerto Gimenez, Roberta Zanin, D. Hildebrand, L. Peruzzo, M. I. Martínez, D. Tescaro, T. Krähenbühl, N. Strah, A. López-Oramas, Alessandro Carosi, D. Garrido, Jose Miguel Miranda, Kouichi Hirotani, Hajime Takami, Andrei Berdyugin, G. De Caneva, C. Schultz, Massimo Persic, V. Scapin, E. A. Alvarez, Nikola Godinovic, Denis Bastieri, Q. Weitzel, Tihomir Surić, Karl Mannheim, Natalia Lewandowska, A. La Barbera, J. Becerra González, Mario Meucci, and A. Saggion
Subjects: Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, ACCELERATION, 01 natural sciences, Spectral line, gamma rays: stars, pulsars: individual: Crab Pulsar, Raigs gamma, SLOT GAPS, Pulsar, NEBULA, OUTER MAGNETOSPHERE, 0103 physical sciences, MAGIC (telescope), 010306 general physics, 010303 astronomy & astrophysics, Cosmic rays, Pulsars, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Crab Pulsar, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, Gamma rays, Compton scattering, Astronomy and Astrophysics, GAMMA-RAY EMISSION, RADIATION, WIND, Stars, Estels, Púlsars, Crab Nebula, Space and Planetary Science, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We use 73 h of stereoscopic data taken with the MAGIC telescopes to investigate the very high-energy (VHE) gamma-ray emission of the Crab pulsar. Our data show a highly significant pulsed signal in the energy range from 50 to 400 GeV in both the main pulse (P1) and the interpulse (P2) phase regions. We provide the widest spectra to date of the VHE components of both peaks, and these spectra extend to the energy range of satellite-borne observatories. The good resolution and background rejection of the stereoscopic MAGIC system allows us to cross-check the correctness of each spectral point of the pulsar by comparison with the corresponding (strong and well-known) Crab nebula flux. The spectra of both P1 and P2 are compatible with power laws with photon indices of 4.0 \pm 0.8 (P1) and 3.42 \pm 0.26 (P2), respectively, and the ratio P1/P2 between the photon counts of the two pulses is 0.54 \pm 0.12. The VHE emission can be understood as an additional component produced by the inverse Compton scattering of secondary and tertiary e\pm pairs on IR-UV photons., 6 pages, 4 figures. Accepted for publication in A&A on 16 February 2012
Published: 2012

44. Morphological and spectral properties of the W51 region measured with the MAGIC telescopes

Author: R. Zanin, A. Saggion, Nikola Godinovic, Daniel Nieto, Adrian Biland, Gianluca Giavitto, A. González Muñoz, Hanna Kellermann, Takashi Saito, J. M. Paredes, Antonio Stamerra, D. Dominis Prester, P. G. Prada Moroni, D. Häfner, O. Tibolla, T. Jogler, R. Reinthal, Nina Nowak, L. Maraschi, Elina Lindfors, R. J. García López, J. Rico, Dominik Elsaesser, Francesco Dazzi, M. V. Fonseca, Reiko Orito, U. Barres de Almeida, Aaron Dominguez, Daniel Mazin, E. Leonardo, Silvia Pardo, J. Storz, Nijil Mankuzhiyil, Giacomo Bonnoli, Christian Fruck, Damir Lelas, P. Munar-Adrover, M. A. Perez-Torres, Victor Stamatescu, Francisco Prada, M. I. Martínez, M. Asensio, A. Cañellas, J. Krause, A. Diago Ortega, Robert Wagner, Massimo Persic, B. De Lotto, Dorota Sobczyńska, G. De Caneva, Louis Antonelli, B. Steinke, Victor Zabalza, Denis Bastieri, Q. Weitzel, C. Delgado Mendez, S. R. Gozzini, Stefano Covino, T. Krähenbühl, Tihomir Surić, Tomislav Terzić, R. Mirzoyan, Riccardo Paoletti, D. Eisenacher, Daniela Dorner, S. Rügamer, N. Strah, E. Colombo, Ralph Bock, E. Carmona, Markus Garczarczyk, Konstancja Satalecka, Michele Doro, E. Prandini, K. Berger, S. Klepser, Juan Abel Barrio, Dario Hrupec, M. A. Lopez, L. O. Takalo, Jelena Aleksić, D. Tescaro, Masahiro Teshima, A. Boller, L. Cossio, A. Niedzwiecki, D. Borla Tridon, Aldo Treves, M. Salvati, Mosè Mariotti, Julian Sitarek, Marc Ribó, Elisa Bernardini, David Paneque, M. Uellenbeck, A. Sillanpää, Diego F. Torres, J. Hose, Daniela Hadasch, B. Huber, Artemio Herrero, V. Kadenius, Felix Spanier, A. De Angelis, Abelardo Moralejo, S. Paiano, Ignasi Reichardt, Saverio Lombardi, Ivica Puljak, Pierre Colin, P. Temnikov, Hajime Takami, Daniel Ferenc, Karl Mannheim, Fabio Zandanel, P. Da Vela, Shan Sun, J. Pochon, G. Maneva, Natalia Lewandowska, F. Jankowski, I. Puerto Gimenez, A. La Barbera, T. Schweizer, C. Schultz, V. Scapin, D. Hildebrand, J. Becerra González, Mario Meucci, P. Antoranz, S. Partini, Martin Makariev, Oscar Blanch, M. Doert, Michael Backes, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, Thomas Bretz, D. Garrido, S. N. Shore, M. Pilia, Jose Miguel Miranda, Wolfgang Rhode, E. De Cea del Pozo, V. Scalzotto, J. Moldón, Fabrizio Tavecchio, Kari Nilsson, Ll. Font, I. Snidaric, S. Spiro, E. Lorenz, Jose Luis Contreras, K. Saito, Juan Cortina, Patrick Vogler, and E. A. Alvarez
Subjects: Hadron, Astrophysics, MOLECULAR CLOUD, 01 natural sciences, Pulsar wind nebula, SUPERNOVA REMNANT W51C, Raigs gamma, MHZ, Supernova remnant, 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Supernoves, Acceleradors de partícules, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, Cosmic rays, Gamma ray, NONTHERMAL EMISSION, GAMMA-RAY EMISSION, GALACTIC COSMIC-RAYS, ACCELERATION, DISCOVERY, RADIATION, Supernovae, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, acceleration of particles, gamma rays: general, ISM: supernova remnants, ISM: clouds, gamma rays: ISM, 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, Molecular cloud, Gamma rays, Astronomy and Astrophysics, Particle accelerators, 13. Climate action, Space and Planetary Science, ddc:520, Fermi Gamma-ray Space Telescope
Abstract: The W51 complex hosts the supernova remnant W51C which is known to interact with the molecular clouds in the star forming region W51B. In addition, a possible pulsar wind nebula CXO J192318.5+140305 was found likely associated with the supernova remnant. Gamma-ray emission from this region was discovered by Fermi/LAT (between 0.2 and 50 GeV) and H.E.S.S. (>1 TeV). The spatial distribution of the events could not be used to pinpoint the location of the emission among the pulsar wind nebula, the supernova remnant shell and/or the molecular cloud. However, the modeling of the spectral energy distribution presented by the Fermi/LAT collaboration suggests a hadronic emission mechanism. We performed observations of the W51 complex with the MAGIC telescopes for more than 50 hours. The good angular resolution in the medium (few hundred GeV) to high (above 1 TeV) energies allow us to perform morphological studies. We detect an extended emission of very-high-energy gamma rays, with a significance of 11 standard deviations. We extend the spectrum from the highest Fermi/LAT energies to \sim 5 TeV and find that it follows a single power law with an index of 2.58 \pm 0.07stat \pm 0.22syst . The main part of the emission coincides with the shocked cloud region, while we find a feature extending towards the pulsar wind nebula. The possible contribution of the pulsar wind nebula, assuming a point-like source, shows no dependence on energy and it is about 20% of the overall emission. The broad band spectral energy distribution can be explained with a hadronic model that implies proton acceleration above 100 TeV. This result, together with the morphology of the source, tentatively suggests that we observe ongoing acceleration of ions in the interaction zone between supernova remnant and cloud. These results shed light on the long-standing problem of the origin of galactic cosmic rays., 11 pages, 7 figures, accepted by A&A, corresponding authors: J. Krause, I Reichardt, E. Carmona
Published: 2012
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45. MAGIC observations of the giant radio galaxy M 87 in a low-emission state between 2005 and 2007

Author: Jose Luis Contreras, T. Schweizer, M. A. Perez-Torres, Juan Cortina, L. Maraschi, Elina Lindfors, P. Antoranz, Daniel Nieto, K. Saito, Daniel Mazin, D. Dominis Prester, Hanna Kellermann, A. Cañellas, D. Hadasch, Daniela Dorner, Stefano Covino, Abelardo Moralejo, Thomas Bretz, S. N. Shore, M. Pilia, Patrick Vogler, Francisco Prada, E. A. Alvarez, A. López-Oramas, Takashi Saito, Masahiro Teshima, M. Doert, Michael Backes, R. Mirzoyan, Giacomo Bonnoli, Wlodek Bednarek, Alessandro Carosi, L. A. Antonelli, K. Berger, Tomislav Terzić, M. Gaug, Reiko Orito, A. La Barbera, Mosè Mariotti, A. Sillanpää, M. V. Fonseca, E. Carmona, Markus Garczarczyk, M. Asensio, P. Temnikov, D. Hildebrand, L. Peruzzo, Aaron Dominguez, A. Boller, L. Cossio, Felicitas Pauss, Wolfgang Rhode, Elisa Bernardini, Dario Hrupec, Felix Spanier, Igor Oya, Fabrizio Tavecchio, Christian Fruck, Artemio Herrero, D. Garrido, Ll. Font, Julian Sitarek, Nikola Godinovic, J. Moldón, Jose Miguel Miranda, Victor Zabalza, B. Huber, Ivica Puljak, M. Uellenbeck, Pierre Colin, Denis Bastieri, Q. Weitzel, Tihomir Surić, I. Snidaric, Saverio Lombardi, J. Pochon, B. Steinke, M. A. Lopez, J. Hose, M. I. Martínez, R. J. García López, S. Partini, D. Höhne-Mönch, C. Delgado Mendez, J. Krause, B. De Lotto, Riccardo Paoletti, E. Colombo, S. Spiro, E. Lorenz, E. De Cea del Pozo, Karl Mannheim, S. Rügamer, D. Tescaro, Juan Abel Barrio, Fabio Zandanel, Ralph Bock, J. M. Paredes, M. Salvati, S. Klepser, Antonio Stamerra, Andrei Berdyugin, L. O. Takalo, A. Diago Ortega, Robert Wagner, D. Borla Tridon, Victor Stamatescu, Gianluca Giavitto, M. Shayduk, Diego F. Torres, C. Schultz, D. Häfner, M. Pasanen, Martin Makariev, A. De Angelis, J. Becerra González, J. Storz, Nijil Mankuzhiyil, Oscar Blanch, P. Munar-Adrover, T. Jogler, Mario Meucci, Ignasi Reichardt, V. Scapin, Hajime Takami, Gabriele Ghisellini, Daniel Ferenc, H. Vankov, Francesco Dazzi, Ilana M. Braun, Silvia Pardo, Marc Ribó, Konstancja Satalecka, E. Leonardo, Michele Doro, Hiroko Miyamoto, Jelena Aleksić, G. Maneva, A. Saggion, David Paneque, Adrian Biland, Roberta Zanin, J. Rico, Kari Nilsson, V. Scalzotto, P. G. Prada Moroni, Massimo Persic, T. Krähenbühl, O. Tibolla, N. Strah, G. De Caneva, E. Prandini, Aldo Treves, R. Reinthal, Dominik Elsaesser, Damir Lelas, and Dorota Sobczyńska
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, law.invention, galaxies: individual: M 87, Telescope, law, Observacions astronòmiques, Gamma ray astronomy, 0103 physical sciences, gamma rays: galaxies, Astronomia de raigs gamma, MAGIC (telescope), 010303 astronomy & astrophysics, Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Spectral index, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Gamma-ray astronomy, Space and Planetary Science, astro-ph.CO, ddc:520, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astronomical observations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the results of a long M87 monitoring campaign in very high energy $\gamma$-rays with the MAGIC-I Cherenkov telescope. We aim to model the persistent non-thermal jet emission by monitoring and characterizing the very high energy $\gamma$-ray emission of M87 during a low state. A total of 150\,h of data were taken between 2005 and 2007 with the single MAGIC-I telescope, out of which 128.6\,h survived the data quality selection. We also collected data in the X-ray and \textit{Fermi}--LAT bands from the literature (partially contemporaneous). No flaring activity was found during the campaign. The source was found to be in a persistent low-emission state, which was at a confidence level of $7\sigma$. We present the spectrum between 100\,GeV and 2\,TeV, which is consistent with a simple power law with a photon index $\Gamma=2.21\pm0.21$ and a flux normalization at 300\,GeV of $(7.7\pm1.3) \times 10^{-8}$ TeV$^{-1}$ s$^{-1}$ m$^{-2}$. The extrapolation of the MAGIC spectrum into the GeV energy range matches the previously published \textit{Fermi}--LAT spectrum well, covering a combined energy range of four orders of magnitude with the same spectral index. We model the broad band energy spectrum with a spine layer model, which can satisfactorily describe our data., Comment: 8 pages, 5 figures, 2 tables; A&A Journal version, fixed typo in the author list
Published: 2012

46. Detection of very-high energy gamma-ray emission from NGC 1275 by the MAGIC telescopes

Author: H. Vankov, Ilana M. Braun, E. De Cea del Pozo, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, Ruben Lopez-Coto, D. Garrido, Jose Miguel Miranda, Thomas Bretz, S. N. Shore, T. Jogler, Abelardo Moralejo, Wolfgang Rhode, A. Diago Ortega, Robert Wagner, Dario Hrupec, M. A. Lopez, J. Moldón, K. Saito, M. V. Fonseca, A. De Angelis, Nijil Mankuzhiyil, D. Dominis Prester, T. Krähenbühl, P. Munar-Adrover, Patrick Vogler, Francesco Dazzi, R. Reinthal, A. Cañellas, Ignasi Reichardt, Stefano Covino, L. A. Antonelli, M. Doert, Michael Backes, Victor Stamatescu, E. Leonardo, B. Steinke, Konstancja Satalecka, Dominik Elsaesser, N. Strah, Michele Doro, U. Barres de Almeida, G. Maneva, R. Zanin, Jelena Aleksić, Francisco Prada, C. Delgado Mendez, S. R. Gozzini, A. Saggion, A. Niedzwiecki, Damir Lelas, Fabrizio Tavecchio, P. Temnikov, Adrian Biland, David Paneque, Fabio Zandanel, Shan Sun, I. Snidaric, Silvia Pardo, J. Rico, S. Rügamer, Daniel Nieto, Kari Nilsson, R. J. García López, Juan Abel Barrio, Dorota Sobczyńska, S. Spiro, E. Lorenz, D. Borla Tridon, Riccardo Paoletti, Daniela Dorner, K. Berger, M. Uellenbeck, L. Maraschi, Elina Lindfors, G. De Caneva, J. M. Paredes, Antonio Stamerra, Daniel Mazin, Massimo Persic, Diego F. Torres, E. A. Alvarez, M. Pilia, P. G. Prada Moroni, T. Schweizer, E. Prandini, V. Scalzotto, S. Partini, D. Höhne-Mönch, O. Tibolla, Felix Spanier, Christoph Pfrommer, M. Shayduk, J. Storz, Elisa Bernardini, Nikola Godinovic, Aldo Treves, H. Kellermann, J. Krause, B. De Lotto, P. Antoranz, Masahiro Teshima, Takashi Saito, Marc Ribó, Gianluca Giavitto, Jose Luis Contreras, Ivica Puljak, Pierre Colin, M. Salvati, S. Klepser, Reiko Orito, Juan Cortina, Martin Makariev, A. Sillanpää, Julian Sitarek, Oscar Blanch, J. Hose, Daniela Hadasch, C. Fruck, J. Kushida, Anders Pinzke, Andrei Berdyugin, C. Schultz, V. Scapin, Tomislav Terzić, Aaron Dominguez, Victor Zabalza, Giacomo Bonnoli, M. Asensio, L. Font, Hajime Takami, I. Puerto Gimenez, E. Colombo, D. Hildebrand, L. Peruzzo, Ralph Bock, A. Boller, L. Cossio, L. O. Takalo, Mosè Mariotti, Artemio Herrero, Saverio Lombardi, J. Pochon, D. Häfner, M. I. Martínez, D. Tescaro, R. Mirzoyan, D. Eisenacher, Natalia Lewandowska, E. Carmona, Markus Garczarczyk, Nina Nowak, A. La Barbera, M. A. Perez-Torres, J. Becerra González, Mario Meucci, Denis Bastieri, Q. Weitzel, Tihomir Surić, S. Paiano, Karl Mannheim, and Daniel Ferenc
Subjects: POLARIZATION, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, NGC-1275, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, Power law, Raigs gamma, 0103 physical sciences, MAGIC (telescope), galaxies: active, galaxies: jets, galaxies: individual (NGC 1275), galaxies: individual (IC 310), gamma rays: galaxies, Nuclear Experiment, 010303 astronomy & astrophysics, CRAB-NEBULA, GALAXY M87, IC 310, PERFORMANCE, DISCOVERY, EVOLUTION, VERITAS, astro-ph.HE, Physics, Spectral index, 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Galaxies, Light curve, Galaxy, Galàxies, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the detection of very-high energy (VHE, E>100 GeV) gamma-ray emission from NGC 1275, the central radio galaxy of the Perseus cluster of galaxies. The source has been detected by the MAGIC telescopes with a statistical significance of 6.6 sigma above 100 GeV in 46 hr of stereo observations carried out between August 2010 and February 2011. The measured differential energy spectrum between 70 GeV and 500 GeV can be described by a power law with a steep spectral index of \Gamma=-4.1+/-0.7stat+/-0.3syst, and the average flux above 100 GeV is F_{gamma}=(1.3+/-0.2stat+/-0.3syst) x 10^-11 cm^-2 s^-1. These results, combined with the power-law spectrum measured in the first two years of observations by the Fermi-LAT above 100 MeV, with a spectral index of Gamma ~ -2.1, strongly suggest the presence of a break or cut-off around tens of GeV in the NGC 1275 spectrum. The light curve of the source above 100 GeV does not show hints of variability on a month time scale. Finally, we report on the nondetection in the present data of the radio galaxy IC 310, previously discovered by the Fermi-LAT and MAGIC. The derived flux upper limit F^{U.L.}_{gamma} (>300 GeV)=1.2 x 10^-12 cm^-2 s^-1 is a factor ~ 3 lower than the mean flux measured by MAGIC between October 2009 and February 2010, thus confirming the year time-scale variability of the source at VHE., Comment: Corresponding authors are S. Lombardi, P. Colin, D. Hildebrand, and F. Zandanel. Published in A&A; 4 pages, 4 figures
Published: 2012

47. Constraining cosmic rays and magnetic fields in the Perseus galaxy cluster with TeV observations by the MAGIC telescopes

Author: S. Partini, D. Höhne-Mönch, V. Scalzotto, Silvia Pardo, G. De Caneva, Ivica Puljak, Pierre Colin, D. Dominis Prester, Martin Makariev, Oscar Blanch, Francisco Prada, Thomas Bretz, S. N. Shore, Marc Ribó, J. Krause, J. M. Paredes, Antonio Stamerra, A. Sillanpää, M. V. Fonseca, J. Storz, Kari Nilsson, B. De Lotto, Riccardo Paoletti, M. Doert, Michael Backes, P. Temnikov, Fabio Zandanel, Shan Sun, J. Kushida, E. Prandini, Aldo Treves, Christian Fruck, E. A. Alvarez, L. A. Antonelli, K. Berger, Nijil Mankuzhiyil, P. Munar-Adrover, P. Antoranz, B. Steinke, Jose Luis Contreras, Stefano Covino, Julian Sitarek, J. Hose, T. Jogler, Daniela Hadasch, Anders Pinzke, S. Klepser, Juan Cortina, R. Reinthal, Nikola Godinovic, M. Pilia, Wolfgang Rhode, Dominik Elsaesser, Abelardo Moralejo, E. Colombo, U. Barres de Almeida, Damir Lelas, Felix Spanier, Daniel Ferenc, Daniel Nieto, Konstancja Satalecka, Michele Doro, Masahiro Teshima, Dorota Sobczyńska, J. Moldón, S. Rügamer, Juan Abel Barrio, H. Vankov, Ralph Bock, Christoph Pfrommer, L. O. Takalo, M. Uellenbeck, D. Borla Tridon, R. Mirzoyan, Ilana M. Braun, T. Schweizer, Tomislav Terzić, D. Eisenacher, Fabrizio Tavecchio, Ll. Font, A. Cañellas, D. Häfner, M. Salvati, I. Snidaric, A. Diago Ortega, Robert Wagner, Giacomo Bonnoli, Mosè Mariotti, E. De Cea del Pozo, E. Carmona, Markus Garczarczyk, M. Asensio, Victor Stamatescu, Dario Hrupec, Saverio Lombardi, L. Maraschi, Elina Lindfors, Jelena Aleksić, S. Spiro, E. Lorenz, J. Pochon, M. A. Lopez, K. Saito, Daniel Mazin, A. Niedzwiecki, Patrick Vogler, Diego F. Torres, David Paneque, Nina Nowak, Takashi Saito, M. A. Perez-Torres, Reiko Orito, I. Puerto Gimenez, D. Hildebrand, L. Peruzzo, M. I. Martínez, D. Tescaro, A. Boller, L. Cossio, Artemio Herrero, Natalia Lewandowska, Daniela Dorner, A. La Barbera, J. Becerra González, Mario Meucci, Elisa Bernardini, Denis Bastieri, Q. Weitzel, Tihomir Surić, H. Kellermann, S. Paiano, Karl Mannheim, C. Delgado Mendez, S. R. Gozzini, Gianluca Giavitto, A. De Angelis, P. G. Prada Moroni, Ignasi Reichardt, O. Tibolla, M. Shayduk, Francesco Dazzi, G. Maneva, R. J. García López, E. Leonardo, R. Zanin, A. Saggion, Massimo Persic, Adrian Biland, T. Krähenbühl, N. Strah, J. Rico, Andrei Berdyugin, A. López-Oramas, Wlodek Bednarek, Alessandro Carosi, C. Schultz, Ruben Lopez-Coto, V. Scapin, D. Garrido, Aaron Dominguez, Jose Miguel Miranda, Victor Zabalza, and Hajime Takami
Subjects: Radio galaxy, gamma rays: galaxies: clusters, acceleration of particles, galaxies: clusters: individual: Perseus, Astrophysics, SCALING RELATIONS, 01 natural sciences, 7. Clean energy, Raigs gamma, DIFFUSE RADIO-EMISSION, HADRONIC MODELS, 010303 astronomy & astrophysics, PARTICLE HYDRODYNAMICS SIMULATIONS, GAMMA-RAY, X-RAY, COMA CLUSTER, DARK-MATTER, INTRACLUSTER MEDIUM, HESS OBSERVATIONS, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Clusters of galaxies, Cosmic rays, gamma ray astronomy, IMAGING CHERENKOV DETECTOR, 16. Peace & justice, Magnetic field, astro-ph.CO, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Cúmuls de galàxies, Structure formation, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, Cluster (physics), Cherenkov radiation, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Galaxies, Galàxies, 13. Climate action, Space and Planetary Science, ddc:520
Abstract: Galaxy clusters are being assembled today in the most energetic phase of hierarchical structure formation which manifests itself in powerful shocks that contribute to a substantial energy density of cosmic rays (CRs). Hence, clusters are expected to be luminous gamma-ray emitters since they also act as energy reservoirs for additional CR sources, such as active galactic nuclei and supernova-driven galactic winds. To detect the gamma-ray emission from CR interactions with the ambient cluster gas, we conducted the deepest to date observational campaign targeting a galaxy cluster at very high-energy gamma-rays and observed the Perseus cluster with the MAGIC Cherenkov telescopes for a total of ~85 hr of effective observing time. This campaign resulted in the detection of the central radio galaxy NGC 1275 at energies E > 100 GeV with a very steep energy spectrum. Here, we restrict our analysis to energies E > 630 GeV and detect no significant gamma-ray excess. This constrains the average CR-to-thermal pressure ratio to be 4-9 microG, depending on the rate of decline of the magnetic field strength toward larger radii., Corresponding authors are F. Zandanel, C. Pfrommer, P. Colin, A. Pinzke and S. Lombardi. Accepted for publication in A&A on 06/03/2012
Published: 2012

48. Discovery of VHEγ-ray emission from the BL Lacertae object B3 2247+381 with the MAGIC telescopes

Author: Silvia Pardo, Ivica Puljak, Pierre Colin, M. I. Martínez, M. Uellenbeck, Riccardo Paoletti, J. M. Paredes, Antonio Stamerra, J. Storz, D. Dominis Prester, S. Buson, Denis Bastieri, Q. Weitzel, Tihomir Surić, Francisco Prada, Andrei Berdyugin, T. Krähenbühl, A. Diago Ortega, Robert Wagner, M. V. Fonseca, M. Salvati, M. A. Perez-Torres, D. Tescaro, R. Reinthal, C. Schultz, G. De Caneva, Dominik Elsaesser, Daniela Dorner, A. Sillanpää, N. Strah, Hiroko Miyamoto, Jelena Aleksić, J. Rico, V. Scapin, J. Krause, B. De Lotto, V. Kadenius, S. Klepser, A. De Angelis, Karl Mannheim, E. A. Alvarez, Christian Fruck, Damir Lelas, K. Berger, M. Shayduk, Ignasi Reichardt, P. Temnikov, Fabio Zandanel, D. Hildebrand, L. Peruzzo, L. Maraschi, Elina Lindfors, B. Steinke, Nijil Mankuzhiyil, G. Maneva, Dorota Sobczyńska, A. Boller, David Paneque, L. Cossio, L. Font, T. Schweizer, J. Becerra González, Tomislav Terzić, P. Munar-Adrover, Daniel Mazin, A. Saggion, Nikola Godinovic, Diego F. Torres, Felix Spanier, M. Pasanen, Adrian Biland, S. Rügamer, A. Cañellas, Juan Abel Barrio, Mario Meucci, A. López-Oramas, Artemio Herrero, Hajime Takami, Wlodek Bednarek, Alessandro Carosi, Roberta Zanin, D. Borla Tridon, Abelardo Moralejo, E. Prandini, Aaron Dominguez, Felicitas Pauss, Elisa Bernardini, R. Mirzoyan, D. Garrido, Masahiro Teshima, B. Huber, Jose Miguel Miranda, H. Kellermann, Julian Sitarek, Marc Ribó, Aldo Treves, Stefano Covino, J. Hose, Matthias Weidinger, Victor Zabalza, Konstancja Satalecka, E. Carmona, Markus Garczarczyk, Michele Doro, R. J. García López, Daniela Hadasch, C. Delgado Mendez, Daniel Nieto, P. Antoranz, A. La Barbera, Massimo Persic, Victor Stamatescu, Gianluca Giavitto, Giacomo Bonnoli, M. Asensio, Thomas Bretz, S. N. Shore, Wolfgang Rhode, E. De Cea del Pozo, J. Moldón, Dario Hrupec, M. A. Lopez, L. A. Antonelli, Igor Oya, Fabrizio Tavecchio, I. Snidaric, P. G. Prada Moroni, O. Tibolla, S. Spiro, E. Lorenz, T. Jogler, Francesco Dazzi, E. Leonardo, K. Saito, Daniel Ferenc, E. Colombo, H. Vankov, Ilana M. Braun, Ralph Bock, L. O. Takalo, Mosè Mariotti, Patrick Vogler, V. Scalzotto, Saverio Lombardi, S. Partini, J. Pochon, D. Höhne-Mönch, D. Häfner, Kari Nilsson, Jose Luis Contreras, Juan Cortina, Martin Makariev, Takashi Saito, Oscar Blanch, Reiko Orito, M. Doert, Michael Backes, and M. Pilia
Subjects: Photon, Swift Gamma-Ray Burst Mission, SAMPLE, Astrophysics::High Energy Astrophysical Phenomena, EXTRAGALACTIC BACKGROUND LIGHT, LARGE-AREA TELESCOPE, MISSION, BEPPOSAX, SPECTRA, CATALOG, BLAZARS, NUCLEI, QUASAR, Flux, Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, 01 natural sciences, 0103 physical sciences, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, Space and Planetary Science, Galàxies actives, Active galaxies, Spectral energy distribution, Electrónica, Electricidad, BL Lac object, Fermi Gamma-ray Space Telescope
Abstract: We study the non-thermal jet emission of the BL Lac object B3 2247+381 during a high optical state. The MAGIC telescopes observed the source during 13 nights between September 30th and October 30th 2010, collecting a total of 14.2 hours of good quality very high energy (VHE) $\gamma$-ray data. Simultaneous multiwavelength data was obtained with X-ray observations by the Swift satellite and optical R-band observations at the KVA-telescope. We also use high energy $\gamma$-ray (HE, 0.1 GeV-100 GeV) data from the Fermi satellite. The BL Lac object B3 2247+381 (z=0.119) was detected, for the first time, at VHE $\gamma$-rays at a statistical significance of 5.6 $\sigma$. A soft VHE spectrum with a photon index of -3.2 $\pm$ 0.6 was determined. No significant short term flux variations were found. We model the spectral energy distribution using a one-zone SSC-model, which can successfully describe our data.
Published: 2012

49. Searches for Dark Matter annihilation signatures in the Segue 1 satellite galaxy with the MAGIC-I telescope

Author: E. Prandini, Aldo Treves, P. Antoranz, Jose Luis Contreras, Juan Cortina, Ignasi Reichardt, Ivica Puljak, S. Partini, D. Höhne-Mönch, J. Krause, B. De Lotto, V. Scalzotto, Pierre Colin, D. Dominis Prester, Silvia Pardo, Takashi Saito, G. Maneva, Masahiro Teshima, Kari Nilsson, L. Maraschi, Elina Lindfors, Dario Hrupec, R. Zanin, R. Essig, A. De Angelis, A. Saggion, Adrian Biland, T. Jogler, E. Colombo, Daniel Mazin, J. Moldón, Reiko Orito, M. A. Lopez, Francisco Prada, Ralph Bock, E. A. Alvarez, K. Saito, M. Doert, Riccardo Paoletti, Fabio Zandanel, M. Salvati, L. O. Takalo, Martin Makariev, Oscar Blanch, R. Reinthal, R. Mirzoyan, Stefano Covino, A. Sillanpää, M. Thom, M. Shayduk, Dominik Elsaesser, Diego F. Torres, Daniel Nieto, Nikola Godinovic, M. Pasanen, T. Schweizer, Julian Sitarek, Damir Lelas, A. Diago Ortega, Robert Wagner, K. Berger, J. Hose, Thomas Bretz, S. N. Shore, J. M. Paredes, Nijil Mankuzhiyil, Abelardo Moralejo, P. G. Prada Moroni, Dorota Sobczyńska, Neelima Sehgal, Michael Backes, Daniela Hadasch, C. Fruck, Antonio Stamerra, Patrick Vogler, P. Munar-Adrover, Markus Garczarczyk, A. Cañellas, D. Häfner, O. Tibolla, L. A. Antonelli, Daniel Ferenc, Louis E. Strigari, Wolfgang Rhode, J. Storz, Konstancja Satalecka, Francesco Dazzi, E. De Cea del Pozo, H. Vankov, M. Asensio, M. Pilia, E. Leonardo, Mosè Mariotti, Ilana M. Braun, Igor Oya, Fabrizio Tavecchio, Felix Spanier, Ll. Font, G. Bonnoli, Marc Ribó, E. Carmona, J. Rico, Mattia Fornasa, Saverio Lombardi, M. A. Perez-Torres, S. Spiro, E. Lorenz, J. Pochon, Hajime Takami, Tomislav Terzić, Wlodek Bednarek, Alessandro Carosi, Aaron Dominguez, Felicitas Pauss, D. Hildebrand, Victor Zabalza, L. Peruzzo, M. I. Martínez, D. Garrido, M. V. Fonseca, Jose Miguel Miranda, B. Steinke, D. Tescaro, A. Boller, L. Cossio, S. Rügamer, Juan Abel Barrio, D. Borla Tridon, Artemio Herrero, Andrei Berdyugin, C. Schultz, V. Scapin, Michele Doro, Hiroko Miyamoto, Jelena Aleksić, David Paneque, Gianluca Giavitto, Daniela Dorner, Petar Temnikov, Elisa Bernardini, C. Delgado Mendez, J. Becerra González, Mario Meucci, A. La Barbera, Denis Bastieri, Q. Weitzel, Tihomir Surić, B. Huber, S. Paiano, Karl Mannheim, T. Krähenbühl, S. Klepser, N. Strah, R. J. García López, and Massimo Persic
Subjects: SPECTROSCOPIC SURVEY, DWARF SPHEROIDAL GALAXIES, ENERGIES, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, gamma ray experiments, Astrophysics, Parameter space, 01 natural sciences, Spectral line, LARGE-AREA TELESCOPE, FERMI, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Positron, ddc:670, 0103 physical sciences, Satellite galaxy, Emission spectrum, GALACTIC SATELLITES, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Annihilation, 010308 nuclear & particles physics, hep-ex, dark matter experiments, CONSTRAINTS, Astronomy and Astrophysics, Segue, Estels nans, dwarfs galaxies, dwarf galaxies, Dark matter (Astronomy), Dwarf stars, MILKY-WAY HALO, Electrónica, Física nuclear, Matèria fosca (Astronomia), GAMMA-RAY EMISSION, PARTICLE, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the results of the observation of the nearby satellite galaxy Segue 1 performed by the MAGIC-I ground-based gamma-ray telescope between November 2008 and March 2009 for a total of 43.2 hours. No significant gamma-ray emission was found above the background. Differential upper limits on the gamma-ray flux are derived assuming various power-law slopes for the possible emission spectrum. Integral upper limits are also calculated for several power-law spectra and for different energy thresholds. The values are of the order of 10^{-11} ph cm^{-2}$ s^{-1} above 100 GeV and 10^{-12} ph cm^{-2} s^{-1} above 200 GeV. Segue 1 is currently considered one of the most interesting targets for indirect dark matter searches. In these terms, the upper limits have been also interpreted in the context of annihilating dark matter particles. For such purpose, we performed a grid scan over a reasonable portion of the parameter space for the minimal SuperGravity model and computed the flux upper limit for each point separately, taking fully into account the peculiar spectral features of each model. We found that in order to match the experimental upper limits with the model predictions, a minimum flux boost of 10^{3} is required, and that the upper limits are quite dependent on the shape of the gamma-ray energy spectrum predicted by each specific model. Finally we compared the upper limits with the predictions of some dark matter models able to explain the PAMELA rise in the positron ratio, finding that Segue 1 data are in tension with the dark matter explanation of the PAMELA spectrum in the case of a dark matter candidate annihilating into tau+tau-. A complete exclusion however is not possible due to the uncertainties in the Segue 1 astrophysical factor., Comment: 26 pages, 10 figures. Matched to published version
Published: 2011
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50. A search for Very High Energy gamma-ray emission from Sco X-1 with the MAGIC telescopes

Author: Daniel Ferenc, Abelardo Moralejo, H. Vankov, L. Maraschi, Elina Lindfors, Ilana M. Braun, Daniel Mazin, L. A. Antonelli, E. Prandini, Aldo Treves, Michael Backes, Hiroko Miyamoto, Wlodek Bednarek, Alessandro Carosi, Aaron Dominguez, D. Garrido, Jose Miguel Miranda, Felicitas Pauss, A. Saggion, J. Moldón, Adrian Biland, T. Jogler, Dario Hrupec, M. A. Lopez, Tomislav Terzić, Igor Oya, Jelena Aleksić, Stefano Covino, Ivica Puljak, Fabrizio Tavecchio, Silvia Pardo, Victor Zabalza, Pierre Colin, Ll. Font, Takashi Saito, Giacomo Bonnoli, M. Shayduk, Julian Sitarek, E. A. Alvarez, J. Hose, Diego F. Torres, M. Pasanen, E. Colombo, M. Pilia, Daniela Hadasch, R. Zanin, Reiko Orito, M. Asensio, S. Partini, David Paneque, J. Becerra González, R. Reinthal, Ralph Bock, D. Höhne-Mönch, T. Schweizer, Dominik Elsaesser, L. O. Takalo, Daniel Nieto, Damir Lelas, Jose Luis Contreras, A. Cañellas, Nijil Mankuzhiyil, K. Berger, Nikola Godinovic, J. Krause, B. De Lotto, Dorota Sobczyńska, Hajime Takami, P. Munar-Adrover, Mario Meucci, E. De Cea del Pozo, Fabio Zandanel, Konstancja Satalecka, Michele Doro, Juan Cortina, D. Häfner, E. Carmona, A. De Angelis, Martin Makariev, Andrei Berdyugin, Oscar Blanch, Ignasi Reichardt, Valentí Bosch-Ramon, Masahiro Teshima, Felix Spanier, C. Schultz, A. Diago Ortega, Robert Wagner, V. Scapin, Gianluca Giavitto, P. Antoranz, G. Maneva, Thomas Bretz, S. N. Shore, Mosè Mariotti, D. Dominis Prester, Kari Nilsson, M. Salvati, Saverio Lombardi, A. Sillanpää, M. V. Fonseca, M. Thom, J. Pochon, Denis Bastieri, Q. Weitzel, Wolfgang Rhode, Tihomir Surić, Francesco Dazzi, Daniela Dorner, V. Scalzotto, Francisco Prada, Christian Fruck, Pol Bordas, E. Leonardo, Karl Mannheim, Petar Temnikov, B. Steinke, Elisa Bernardini, P. G. Prada Moroni, A. La Barbera, S. Rügamer, Juan Abel Barrio, J. M. Paredes, C. Delgado Mendez, O. Tibolla, R. Mirzoyan, Antonio Stamerra, D. Borla Tridon, K. Saito, Patrick Vogler, Markus Garczarczyk, S. Spiro, E. Lorenz, J. Storz, M. A. Perez-Torres, Riccardo Paoletti, J. Rico, M. Doert, D. Hildebrand, L. Peruzzo, M. I. Martínez, D. Tescaro, A. Boller, L. Cossio, Artemio Herrero, Marc Ribó, B. Huber, T. Krähenbühl, S. Klepser, N. Strah, R. J. García López, Massimo Persic, and Universitat de Barcelona
Subjects: High energy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, gamma rays: stars, 01 natural sciences, MICROQUASAR, X-rays: binaries, HESS, 0103 physical sciences, X-rays, FIELD, 010306 general physics, 010303 astronomy & astrophysics, acceleration of particles, Estels binaris de raigs X, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, acceleration of particles — X-rays: binaries — Stars: individual (Sco X-1) — Gamma rays: stars, RADIO, Acceleradors de partícules, Gamma ray, Astronomy and Astrophysics, BINARY, PULSAR, Horizontal branch, EVOLUTION, Particle accelerators, X-ray binaries, stars: individual: Sco X-1, 13. Climate action, Space and Planetary Science, DISCOVERY, Power ratio, X-RAY, RADIATION, Electrónica, Física nuclear, High Energy Physics::Experiment, Raigs X, Electricidad, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The acceleration of particles up to GeV or higher energies in microquasars has been the subject of considerable theoretical and observational efforts in the past few years. Sco X-1 is a microquasar from which evidence of highly energetic particles in the jet has been found when it is in the so-called Horizontal Branch (HB), a state when the radio and hard X-ray fluxes are higher and a powerful relativistic jet is present. Here we present the first very high energy gamma-ray observations of Sco X-1 obtained with the MAGIC telescopes. An analysis of the whole dataset does not yield a significant signal, with 95% CL flux upper limits above 300 GeV at the level of 2.4x10^{-12} ph/cm^2/s. Simultaneous RXTE observations were conducted to search for TeV emission during particular X-ray states of the source. A selection of the gamma-ray data obtained during the HB based on the X-ray colors did not yield a signal either, with an upper limit of 3.4x10^{-12} ph/cm^2/s. These upper limits place a constraint on the maximum TeV luminosity to non-thermal X-ray luminosity of L_{VHE}/L_{ntX}, 5 pages, 2 figures, 2 tables. Version as published in ApJL
Published: 2011

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