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25 results on '"Olaf Reimer"'

1. Erratum: First Fermi-LAT Solar Flare Catalog (2021, ApJS, 252, 13)

Author

E. Hays, G. Jóhannesson, M. Orienti, G. Zaharijas, G. Martí-Devesa, S. Larsson, Massimo Persic, Carmelo Sgrò, Luca Latronico, M. N. Lovellette, E. Troja, E. Orlando, David Paneque, S. Rainò, M. Kuss, Vahé Petrosian, R. Desiante, F. D'Ammando, Giacomo Principe, M. Negro, Miloš Kovačević, D. Green, Sara Buson, J. W. Hewitt, Yasushi Fukazawa, P. Spinelli, Seb. Funk, F. de Palma, J. Li, D. Bastieri, Marcello Giroletti, T. A. Porter, Regina Caputo, A. Morselli, S. Maldera, Luca Baldini, R. A. Cameron, E. Cavazzuti, Nicola Omodei, M. E. Monzani, D. Serini, T. Mizuno, P. Bruel, Gloria Spandre, Marco Ajello, R. Bonino, D. Tak, P. Fusco, Z. Pei, S. Cutini, Sylvain Guiriec, Igor V. Moskalenko, N. Di Lalla, Olaf Reimer, D. Horan, R. Bellazzini, F. Piron, R. Rando, Mn Mazziotta, P. F. Michelson, L. Di Venere, G. Chiaro, D. Gasparrini, C. C. Cheung, P. Lubrano, S. J. Fegan, J. L. Racusin, Ferdinando Giordano, D. Costantin, Soebur Razzaque, J. Valverde, Elisabetta Bissaldi, I. Mereu, Roger Blandford, A. Berretta, A. Reimer, F. Longo, Alberto Manfreda, M. Razzano, F. Gargano, Melissa Pesce-Rollins, E. J. Siskind, F. Fana Dirirsa, Bindu Rani, and K. S. Wood

Subjects
Physics, Solar flare, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics, Fermi Gamma-ray Space Telescope
Published
2021

2. GALAXY CLUSTERS IN THESWIFT/BAT ERA. II. 10 MORE CLUSTERS DETECTED ABOVE 15 keV

Author

Paola Rebusco, Hans Boehringer, Olaf Reimer, Marco Ajello, Nico Cappelluti, G. Cusumano, and V. La Parola

Subjects
Swift, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Space and Planetary Science, Cluster (physics), Spectral analysis, Thermal model, computer, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics, computer.programming_language
Abstract

We report on the discovery of 10 additional galaxy clusters detected in the ongoing Swift/BAT all-sky survey. Among the newly BAT-discovered clusters there are: Bullet, Abell 85, Norma, and PKS 0745-19. Norma is the only cluster, among those presented here, which is resolved by BAT. For all the clusters we perform a detailed spectral analysis using XMM-Newton and Swift/BAT data to investigate the presence of a hard (non-thermal) X-ray excess. We find that in most cases the clusters' emission in the 0.3-200keV band can be explained by a multi-temperature thermal model confirming our previous results. For two clusters (Bullet and Abell 3667) we find evidence for the presence of a hard X-ray excess. In the case of the Bullet cluster, our analysis confirms the presence of a non-thermal, power-law like, component with a 20-100 keV flux of 3.4 \times 10-12 erg cm-2 s-1 as detected in previous studies. For Abell 3667 the excess emission can be successfully modeled as a hot component (kT=~13keV). We thus conclude that the hard X-ray emission from galaxy clusters (except the Bullet) has most likely thermal origin., Accepted for publication by ApJ

Published
2010

3. EIGHT γ-RAY PULSARS DISCOVERED IN BLIND FREQUENCY SEARCHES OFFERMILAT DATA

Author

M. Dormody, Andrea Belfiore, Jean Ballet, P. M. Saz Parkinson, Paul S. Ray, Olaf Reimer, Fernando Camilo, Patrick Weltevrede, Martino Marelli, Scott M. Ransom, Elizabeth C. Ferrara, K. S. Wood, A. Makeev, D. J. Thompson, Paulo C. C. Freire, A. A. Abdo, Simon Johnston, Tyrel J. Johnson, Roger W. Romani, David A. Smith, A. De Luca, Alice K. Harding, P. A. Caraveo, Peter F. Michelson, Matthew Kerr, Michael T. Wolff, Jürgen Knödlseder, G. A. Caliandro, Michael Keith, M. Ziegler, Matthew G. Baring, C. Gwon, Karen Watters, T. H. Burnett, D. Parent, R. P. Johnson, J. E. Grove, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, open clusters and associations: individual (Westerlund 2), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, pulsars: individual (PSR J1023-5746, PSR J1413-6205, 98.70.Rz &ggr;-ray sources, 1+mm%29%22">&ggr;-ray bursts 98.20.Di Open clusters in the Milky Way 97.60.Gb Pulsars 95.85.Bh Radio, microwave (>1 mm), PSR J1954+2836, Spitzer Space Telescope, Pulsar, pulsars: general, 0103 physical sciences, X-rays: individual (CXOU J102302.8-574606, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, PSR J2055+25), PSR J1957+5033, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy and Astrophysics, gamma rays: general, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Light curve, Astrophysics - Astrophysics of Galaxies, PSR J1429-5911, PSR J1846+0919, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Milagro, XMMU J205549.4+253959), Astrophysics - High Energy Astrophysical Phenomena, PSR J1044-5737, Fermi Gamma-ray Space Telescope
Abstract

We report the discovery of eight gamma-ray pulsars in blind frequency searches using the LAT, onboard the Fermi Gamma-ray Space Telescope. Five of the eight pulsars are young (tau_c10^36 erg/s), and located within the Galactic plane (|b, Submitted to ApJ

Published
2010

4. Erratum: 'Search for Gamma-Ray Emission from the Coma Cluster with Six Years of Fermi-LAT Data' (2016, ApJ, 819, 149)

Author

Luca Latronico, I. A. Grenier, E. Cavazzuti, David H. Green, Igor V. Moskalenko, Hiroyasu Tajima, Johann Cohen-Tanugi, Francesco Longo, L. Di Venere, S. Murgia, G. A. Caliandro, Gloria Spandre, Jan Conrad, Olaf Reimer, Liang Li, Guido Barbiellini, T. Ohsugi, Johan Bregeon, S. Rainò, Tsunefumi Mizuno, Ronaldo Bellazzini, M. Orienti, G. Chiaro, S. Cutini, C. Favuzzi, Diego F. Torres, Yasushi Fukazawa, G. Jóhannesson, Eric Charles, A. De Angelis, G. Tosti, E. J. Siskind, S. Maldera, Carmelo Sgrò, Riccardo Rando, P. Fusco, Giacomo Vianello, S. J. Fegan, G. Godfrey, Jean Ballet, W. B. Atwood, M. Caragiulo, E. Nuss, F. Loparco, J. W. Hewitt, D. Horan, L. Tibaldo, Markus Ackermann, Nicola Giglietto, David Paneque, M. Kuss, Vahé Petrosian, Stefano Ciprini, E. Troja, M. Mayer, Elliott D. Bloom, R. Buehler, M. N. Lovellette, F. de Palma, P. A. Caraveo, Seb. Funk, R. Bonino, Persis S. Drell, Peter F. Michelson, Marcello Giroletti, Marco Ajello, J. B. Thayer, F. Piron, G. M. Madejski, Hiromitsu Takahashi, Andrea Albert, F. Gargano, E. Orlando, P. Lubrano, Jingcheng Li, J. F. Ormes, Roger Blandford, A. Reimer, J. M. Casandjian, K. S. Wood, Stephan Zimmer, Luca Baldini, M. E. Monzani, Sylvain Guiriec, Mn Mazziotta, Yoel Rephaeli, Melissa Pesce-Rollins, T. A. Porter, Denis Bastieri, Seth Digel, Elisabetta Bissaldi, G. Pivato, E. Hays, Eugenio Bottacini, Alberto Manfreda, Dario Gasparrini, Miguel A. Sánchez-Conde, F. Spada, Stefan Larsson, M. Razzano, Filippo D'Ammando, Keith Bechtol, A. Chekhtman, Warit Mitthumsiri, P. Spinelli, Francesco Giordano, R. A. Cameron, P. Bruel, R. Desiante, A. Morselli, Claudia Cecchi, ITA, USA, FRA, and DEU

Subjects
Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Coma Cluster, ddc:520, 010306 general physics, Fermi Gamma-ray Space Telescope
Abstract

We present results from $\gamma$-ray observations of the Coma cluster incorporating six years of Fermi-LAT data and the newly released "Pass 8" event-level analysis. Our analysis of the region reveals low-significance residual structures within the virial radius of the cluster that are too faint for a detailed investigation with the current data. Using a likelihood approach that is free of assumptions on the spectral shape we derive upper limits on the $\gamma$-ray flux that is expected from energetic particle interactions in the cluster. We also consider a benchmark spatial and spectral template motivated by models in which the observed radio halo is mostly emission by secondary electrons. In this case, the median expected and observed upper limits for the flux above 100 $\mathrm{MeV}$ are 1.7 × $10^{−9} ph$ $cm^{−2} s^{−1}$ and 5.2 × $10^{−9} ph$ $cm^{−2} s^{−1}$ respectively (the latter corresponds to residual emission at the level of 1.8$\sigma$). These bounds are comparable to or higher than predicted levels of hadronic gamma-ray emission in cosmic-ray (CR) models with or without reacceleration of secondary electrons, although direct comparisons are sensitive to assumptions regarding the origin and propagation mode of CRs and magnetic field properties. The minimal expected $\gamma$-ray flux from radio and star-forming galaxies within the Coma cluster is roughly an order of magnitude below the median sensitivity of our analysis.

Published
2018

5. GALAXY CLUSTERS IN THESWIFT/BURST ALERT TELESCOPE ERA: HARD X-RAYS IN THE INTRACLUSTER MEDIUM

Author

Nico Cappelluti, A. Moretti, Hans Boehringer, Olaf Reimer, Paola Rebusco, Jochen Greiner, N. Gehrels, J. Tueller, and Marco Ajello

Subjects
Swift, Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Thermal emission, Astrophysics, Coupling (probability), Galaxy, Space and Planetary Science, Hard X-rays, computer, Astrophysics::Galaxy Astrophysics, Galaxy cluster, computer.programming_language, Luminosity function (astronomy)
Abstract

We report about the detection of 10 clusters of galaxies in the ongoing Swift/BAT all-sky survey. This sample, which comprises mostly merging clusters, was serendipitously detected in the 15--55 keV band. We use the BAT sample to investigate the presence of excess hard X-rays above the thermal emission. The BAT clusters do not show significant (e.g. >2 $\sigma$) non-thermal hard X-ray emission. The only exception is represented by Perseus whose high-energy emission is likely due to NGC 1275. Using XMM-Newton, Swift/XRT, Chandra and BAT data, we are able to produce upper limits on the Inverse Compton (IC) emission mechanism which are in disagreement with most of the previously claimed hard X-ray excesses. The coupling of the X-ray upper limits on the IC mechanism to radio data shows that in some clusters the magnetic field might be larger than 0.5 $\mu$G. We also derive the first logN-logS and luminosity function distribution of galaxy clusters above 15 keV.

Published
2008

6. A Hard X‐Ray View of Two Distant VHE Blazars: 1ES 1101−232 and 1ES 1553+113

Author

A. Reimer, Olaf Reimer, Daniela Dorner, L. Costamante, and Greg Madejski

Subjects
Physics, Photon, Spectral shape analysis, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Context (language use), Astrophysics, law.invention, Telescope, Extragalactic background light, Space and Planetary Science, law, Blazar, Absorption (electromagnetic radiation)
Abstract

TeV blazars are known as prominent nonthermal emitters across the entire electromagnetic spectrum with their photon power peaking in the X-ray and TeV bands. If distant, absorption of gamma-ray photons by the extragalactic background light (EBL) alters the intrinsic TeV spectral shape, thereby affecting the overall interpretation. Suzaku observations for two of the more distant TeV blazars known to date, 1ES 1101-232 and 1ES 1553+113, were carried out in 2006 May and July, respectively, including a quasi-simultaneous coverage with the state-of-the-art Cerenkov telescope facilities. We report on the resulting data sets with emphasis on the X-ray band and set in context to their historical behavior. During our campaign, we did not detect any significant X-ray or gamma-ray variability. 1ES 1101-232 was found in a quiescent state with the lowest X-ray flux ever measured. The combined XIS and HXD PIN data for 1ES 1101-232 and 1ES 1553+113 clearly indicate spectral curvature up to the highest hard X-ray data point (~30 keV), manifesting as softening with increasing energy. We describe this spectral shape by either a broken power law or a log-parabolic fit with equal statistical goodness of fits. The combined 1ES 1553+113 very high energy spectrum (90-500 GeV) did not show any significant changes with respect to earlier observations. The resulting contemporaneous broadband spectral energy distributions of both TeV blazars are discussed in view of implications for intrinsic blazar parameter values, taking into account the gamma-ray absorption in the EBL., 9 pages, 10 figures

Published
2008

7. The GeV‐TeV Connection in Galactic γ‐Ray Sources

Author

Jim Hinton, Diego F. Torres, Stefan Funk, and Olaf Reimer

Subjects
Physics, education.field_of_study, biology, Astrophysics::High Energy Astrophysical Phenomena, Population, Gamma ray, Astronomy and Astrophysics, Astrophysics, Galactic plane, biology.organism_classification, Spectral line, law.invention, Telescope, Space and Planetary Science, law, Egret, MAGIC (telescope), education, Cherenkov radiation
Abstract

Recent observations with atmospheric Cherenkov telescope systems such as H.E.S.S. and MAGIC have revealed a large number of new sources of very-high-energy (VHE) gamma-rays from 100 GeV - 100 TeV, mostly concentrated along the Galactic plane. At lower energies (100 MeV - 10 GeV) the satellite-based instrument EGRET revealed a population of sources clustering along the Galactic Plane. Given their adjacent energy bands a systematic correlation study between the two source catalogues seems appropriate. Here, the populations of Galactic sources in both energy domains are characterised on observational as well as on phenomenological grounds. Surprisingly few common sources are found in terms of positional coincidence and spectral consistency. These common sources and their potential counterparts and emission mechanisms will be discussed in detail. In cases of detection only in one energy band, for the first time consistent upper limits in the other energy band have been derived. The EGRET upper limits are rather unconstraining due to the sensitivity mismatch to current VHE instruments. The VHE upper limits put strong constraints on simple power-law extrapolation of several of the EGRET spectra and thus strongly suggest cutoffs in the unexplored energy range from 10 GeV - 100 GeV. Physical reasons for the existence of cutoffs and for differences in the source population at GeV and TeV energies will be discussed. Finally, predictions will be derived for common GeV - TeV sources for the upcoming GLAST mission bridging for the first time the energy gap between current GeV and TeV instruments.

Published
2008

8. A Systematic and Quantitative Approach to the Identification of High-Energy γ-Ray Source Populations

Author

Diego F. Torres and Olaf Reimer

Subjects
Protocol (science), Physics, High energy, business.industry, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Sample (statistics), Astrophysics, Machine learning, computer.software_genre, Identification (information), Space and Planetary Science, Key (cryptography), A priori and a posteriori, Fraction (mathematics), Artificial intelligence, business, Lying, computer
Abstract

A large fraction of the detections to be made by the Gamma-ray Large Area Space Telescope (GLAST) will initially be unidentified. We argue that traditional methodological approaches to identify individuals and/or populations of $\gamma$-ray sources will encounter procedural limitations. These limitations will hamper our ability to classify source populations lying in the anticipated dataset with the required degree of confidence, particularly those for which no member has yet been convincingly detected in the predecessor experiment EGRET. Here we suggest a new paradigm for achieving the classification of $\gamma$-ray source populations based on the implementation of an a priori protocol to search for theoretically-motivated candidate sources. In order to protect the discovery potential of the sample, it is essential that such paradigm will be defined before the data is unblinded. Key to the new procedure is a statistical assessment by which the discovery of a new population can be claimed. Although we explicitly refer here to the case of GLAST, the scheme we present may be adapted to other experiments confronted with a similar problematic., Comment: In press in The Astrophysical Journal Letters. Accepted on July 12, 2005

Published
2005

9. A Multiwavelength Search for a Counterpart of the Brightest Unidentified Gamma‐Ray Source 3EG J2020+4017 (2CG 078+2)

Author

Olaf Reimer, Allyn F. Tennant, Duncan R. Lorimer, Stephen L. O'Dell, Martin C. Weisskopf, Fernando Camilo, Ronald F. Elsner, Gottfried Kanbach, Zaven Arzoumanian, Douglas A. Swartz, and Werner Becker

Subjects
Physics, Line-of-sight, Pulsar, Space and Planetary Science, Observatory, Infrared, ROSAT, Gamma ray, Green Bank Telescope, Flux, Astronomy and Astrophysics, Astrophysics
Abstract

In search of the counterpart to the brightest unidentified gamma-ray source 3EG J2020+4017 we report on new X-ray and radio observations of the gamma-Cygni field with the Chandra X-ray Observatory and with the Green Bank Telescope. We also report on reanalysis of archival ROSAT data. With Chandra it became possible for the first time to measure the position of the putative gamma-ray counterpart RX J2020.2+4026 with sub-arcsec accuracy and to deduce its X-ray spectral characteristics. These observations demonstrate that RX J2020.2+4026 is associated with a K field star and therefore is unlikely to be the counterpart of the bright gamma-ray source 2CG078+2 in the SNR G78.2+2.1 as had been previously suggested. The Chandra observation detected 37 additional X-ray sources which were correlated with catalogs of optical and infrared data. Subsequent GBT radio observations covered the complete 99% EGRET likelihood contour of 3EG J2020+4017 with a sensitivity limit of L_820 ~ 0.1 mJy kpc^2 which is lower than most of the recent deep radio search limits. If there is a pulsar operating in 3EG J2020+4017 this sensitivity limit suggests that the pulsar either does not produce significant amounts of radio emission or that its geometry is such that the radio beam does not intersect with the line of sight. Finally, reanalysis of archival ROSAT data leads to a flux upper limit of f_x = 160 (d/1.5 kpc)^-1 ms, P_dot >= 5 x 10^-13 (d/1.5 kpc)^-1 s s^-1 and B_perp >= 9 x 10^12 (d/1.5 kpc)^-1 G.

Published
2004

10. A New Determination of the Extragalactic Diffuse Gamma‐Ray Background from EGRET Data

Author

Igor V. Moskalenko, Olaf Reimer, and Andrew W. Strong

Subjects
Physics, education.field_of_study, biology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Population, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Curvature, biology.organism_classification, High Energy Physics - Phenomenology, Background spectrum, High Energy Physics - Phenomenology (hep-ph), Space and Planetary Science, Egret, education, Blazar, Astrophysics::Galaxy Astrophysics
Abstract

We use the GALPROP model for cosmic-ray propagation to obtain a new estimate of the Galactic component of gamma rays, and show that away from the Galactic plane it gives an accurate prediction of the observed EGRET intensities in the energy range 30 MeV - 50 GeV. On this basis we re-evaluate the extragalactic gamma-ray background. We find that for some energies previous work underestimated the Galactic contribution at high latitudes and hence overestimated the background. Our new background spectrum shows a positive curvature similar to that expected for models of the extragalactic emission based on the blazar population., Comment: Accepted for publication in The Astrophysical Journal; 6 pages, 14 ps-figures, 4 tables emulateapj.sty, natbib.sty, aastex.cls. More details can be found at http://www.gamma.mpe-garching.mpg.de/~aws/aws.html

Published
2004

11. Luminous Infrared Galaxies as Plausible Gamma-Ray Sources for the Gamma-Ray Large Area Space Telescope and the Imaging Atmospheric Cerenkov Telescopes

Author

Olaf Reimer, Diego F. Torres, Seth Digel, and E. Domingo-Santamaría

Subjects
Physics, Luminous infrared galaxy, education.field_of_study, biology, Astrophysics::High Energy Astrophysical Phenomena, Population, Gamma ray, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, biology.organism_classification, law.invention, Telescope, Spitzer Space Telescope, Space and Planetary Science, law, Egret, education, Astrophysics::Galaxy Astrophysics
Abstract

We argue that luminous infrared galaxies may constitute a newly detectable population of γ-ray sources for the next generation of ground- and space-based high-energy telescopes. In addition, we report for the first time upper limits on their fluxes using data obtained with the EGRET telescope.

Published
2004

12. A Quantitative Evaluation of Potential Radio Identifications for 3EG EGRET Sources

Author

R. C. Hartman, J. R. Mattox, and Olaf Reimer

Subjects
Physics, biology, Space and Planetary Science, Astronomy, Egret, Astronomy and Astrophysics, Astrophysics, biology.organism_classification, Blazar
Abstract

The method of Mattox et al. for identifying EGRET sources with 5 GHz radio sources has been applied to the 3EG EGRET catalog of Hartman et al. Complete results are tabulated. We tabulate separately 46 EGRET sources with radio identifications which we expect to have a high probability of being correct. We suggest that these sources are appropriate for most studies of the properties of γ-ray blazars as a class. All but one of these 46 sources were classified by Hartman et al. as high-confidence identifications; and the additional source was classified by Hartman et al. as a plausible identification. We also tabulate separately 37 additional "plausible identifications of EGRET sources with radio sources." These less secure possibilities include the remaining 21 "high-confidence identifications" of Hartman et al., three of the 27 "lower confidence potential blazar identifications" of Hartman et al., and an additional 15 plausible identifications which have not been suggested previously. Many of these sources require new radio and optical observations to establish them as blazars. We suggest that the 23 "lower-confidence potential blazar identifications" of Hartman et al. which we do not find plausible should not be used in studies of the properties of the EGRET blazars. For this analysis, we have made elliptical fits to the 95% confidence contours of the position uncertainty regions of the 3EG sources which are tabulated in an Appendix.

Published
2001

13. COLLIDING-WIND BINARIES WITH STRONG MAGNETIC FIELDS

Author

K. Reitberger, Anita Reimer, Ralf Kissmann, Emanuele Grimaldo, and Olaf Reimer

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Electron, 01 natural sciences, 7. Clean energy, Magnetic field, Computational physics, Particle acceleration, Acceleration, Stars, Pion, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Magnetohydrodynamics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

The dynamics of colliding wind binary systems and conditions for efficient particle acceleration therein have attracted multiple numerical studies in the recent years. These numerical models seek an explanation of the thermal and non-thermal emission of these systems as seen by observations. In the non-thermal regime, radio and X-ray emission is observed for several of these colliding-wind binaries, while gamma-ray emission has so far only been found in $\eta$ Carinae and possibly in WR 11. Energetic electrons are deemed responsible for a large fraction of the observed high-energy photons in these systems. Only in the gamma-ray regime there might be, depending on the properties of the stars, a significant contribution of emission from neutral pion decay. Thus, studying the emission from colliding-wind binaries requires detailed models of the acceleration and propagation of energetic electrons. This in turn requires a detailed understanding of the magnetic field, which will not only affect the energy losses of the electrons but in case of synchrotron emission also the directional dependence of the emissivity. In this study we investigate magnetohydrodynamic simulations of different colliding wind binary systems with magnetic fields that are strong enough to have a significant effect on the winds. Such strong fields require a detailed treatment of the near-star wind acceleration zone. We show the implementation of such simulations and discuss results that demonstrate the effect of the magnetic field on the structure of the wind collision region., Comment: 24 pages, 7 figures, accepted for publication in The Astrophysical Journal

Published
2016

14. Multiwavelength Observations of PKS 2255−282

Author

Steven Tingay, Valerie Connaughton, Anastasios Tzioumis, A. W. Chen, A. Mucke, E. A. King, Fredrik T. Rantakyrö, D. P. Rayner, Melanie Johnston-Hollitt, Merja Tornikoski, P. McGee, J. Kemp, Olaf Reimer, and David L. Jauncey

Subjects
Physics, Active galactic nucleus, biology, Galactic astronomy, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, biology.organism_classification, Space and Planetary Science, Observatory, Extremely high frequency, Very-long-baseline interferometry, Astrophysics::Solar and Stellar Astrophysics, Egret, Radio frequency, Astrophysics::Galaxy Astrophysics
Abstract

During high radio frequency active galactic nucleus monitoring, we observed a major millimeter wave outburst from PKS 2255-282 in 1997 and initiated a campaign for multifrequency radio monitoring and VLBI imaging of the source. In 1998 January the EGRET instrument on board the Compton Gamma Ray Observatory detected a bright high-energy γ-ray outburst from its direction. Thus, we had the unique opportunity to monitor the source in detail at various radio frequencies already before the detection of the γ-ray outburst. We also initiated multiwavelength follow-up observations. In this paper we present multiwavelength data for PKS 2255-282 before and after the γ-ray outburst. Further, based on the observations, we estimate some physical parameters for this source and discuss the various emission mechanisms possibly involved during this outburst.

Published
1999

15. In‐Flight Calibration of EGRET on the Compton Gamma‐Ray Observatory

Author

H. A. Mayer-Hasselwander, Peter F. Michelson, P. L. Nolan, D. L. Bertsch, Olaf Reimer, W. F. Tompkins, C. E. Fichtel, A. W. Chen, R. C. Hartman, D. J. Thompson, T. D. Willis, D. A. Kniffen, Gottfried Kanbach, L. M. McDonald, J. A. Esposito, Brenda Dingus, Reshmi Mukherjee, C. von Montigny, Yiing Lin, Stanley D. Hunter, P. Sreekumar, and E. J. Schneid

Subjects
Physics, biology, Gamma ray, Astronomy, Astronomy and Astrophysics, biology.organism_classification, Methods observational, law.invention, Telescope, Space and Planetary Science, Observatory, law, Calibration, Egret, Analysis software, Spark chamber
Abstract

The Energetic Gamma-Ray Experiment Telescope (EGRET) on the Compton Gamma-Ray Observatory has been operating for over 7 yr since its launch in 1991 April. This span of time far exceeds the design lifetime of 2 yr. As the instrument has aged, several changes have occurred owing to spark chamber gas exchanges as well as some hardware degradation and failures, all of which have an influence on the instrument sensitivity. This paper describes postlaunch measurements and analysis that are done to calibrate the instrument response functions. The updated instrument characteristics are incorporated into the analysis software.

Published
1999

16. The Cosmic‐Ray3He/4He Ratio from 200 MeV per Nucleon−1to 3.7 GeV per Nucleon−1

Author

E. R. Christian, A. W. Labrador, R. L. Golden, I. L. Rasmussen, W. R. Webber, S. M. Schindler, K. E. Krombel, M. Hof, Jonathan F. Ormes, L. M. Barbier, W. Menn, Andrew Davis, M. Simon, R. E. Streitmatter, Olaf Reimer, R. A. Mewaldt, John Mitchell, and S. J. Stochaj

Subjects
Physics, Nuclear reaction, Wire chamber, Spectrometer, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Nuclear physics, Space and Planetary Science, Nucleosynthesis, Antimatter, Nuclear Experiment, Nucleon, Isotopes of helium
Abstract

The abundances of cosmic-ray helium isotopes between 0.2 and 3.7 GeV nucleon^(-1) were measured by the Isotope Matter Antimatter Experiment (IMAX) during a flight from Lynn Lake, Manitoba, Canada on 1992 July 16-17. The IMAX balloon-borne magnetic spectrometer realized a direct measurement of the charge, the velocity, and the rigidity of cosmic rays using plastic scintillators, a high-resolution time-of-flight system, and two silica-aerogel Cerenkov counters in conjunction with a drift chamber/multiwire proportional chamber tracking system. About 75,000 helium isotopes are identified by their mass using the velocity versus magnetic rigidity technique. The measured ^3He/^4He ratios are corrected to the top of the atmosphere, and a comparison with previous data is given. The observed isotopic composition is found to be generally consistent with the predictions of a standard leaky box model of cosmic-ray transport in the Galaxy.

Published
1998

17. FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE SUPERNOVA REMNANT G8.7-0.1

Author

Hartmut Sadrozinski, R. A. Cameron, Stefano Ciprini, Marco Ajello, J. B. Thayer, Sho Nishino, Jay P. Norris, Akira Okumura, T. A. Porter, Pascal Bruel, T. Ohsugi, Eleonora Troja, Gloria Spandre, Gudlaugur Johannesson, Elliott D. Bloom, Alex Drlica-Wagner, K. Hayashi, D. Parent, S. Buson, E. Hays, R. Buehler, Luca Latronico, T. Glanzman, Johann Cohen-Tanugi, S. Murgia, Stephan Zimmer, Roger Blandford, F. Piron, Peter F. Michelson, Marcello Giroletti, Justin Vandenbroucke, M. Roth, Guido Barbiellini, Nicola Omodei, G. Godfrey, Zhenwei Yang, Carmelo Sgrò, Riccardo Rando, Yasuo Fukui, A. De Angelis, G. Tosti, R. Dubois, W. B. Focke, V. Pelassa, E. Nuss, David Paneque, M. Ohno, M. E. Monzani, M. Kuss, Alice K. Harding, P. Spinelli, Francesco Giordano, Hideaki Katagiri, F. de Palma, Melissa Pesce-Rollins, A. Van Etten, Igor V. Moskalenko, M. Frailis, Elizabeth C. Ferrara, G. A. Caliandro, Jonathan F. Ormes, Olaf Reimer, E. Do Couto E Silva, B. Berenji, Ryo Yamazaki, Giacomo Vianello, A. Morselli, Hiromitsu Takahashi, V. Vitale, D. Hadasch, Keith Bechtol, S. Rainò, M. Brigida, Tsunefumi Mizuno, Hajimu Yasuda, Francesco Longo, C. Favuzzi, Jürgen Knödlseder, E. Orlando, Takeshi Nakamori, J. M. Casandjian, A. Tramacere, R. Claus, Hiroaki Yamamoto, Hiroyasu Tajima, J. Bregeon, Ryosuke Itoh, Nicola Giglietto, P. L. Nolan, J. E. Grove, Yasushi Fukazawa, Takaaki Tanaka, A. P. Waite, S. Germani, Brian L Winer, Shiu-Hang Lee, Ronaldo Bellazzini, Andrea Lionetto, M. N. Lovellette, Dario Gasparrini, Diego F. Torres, Hidetoshi Kubo, P. A. Caraveo, Alice Allafort, P. Fusco, Persis S. Drell, Paolo Giommi, C. Monte, T. Kamae, V. Vasileiou, J. G. Thayer, T. L. Usher, A. A. Moiseev, Yasunobu Uchiyama, Jun Kataoka, S. J. Fegan, J. Mehault, Luca Baldini, A. Reimer, M. Naumann-Godo, Charles D. Dermer, E. J. Siskind, M. Pierbattista, A. S. Johnson, S. Cutini, Claudia Cecchi, F. Loparco, P. Wang, Denis Bastieri, Emanuele Bonamente, J. Lande, Sylvain Guiriec, K. S. Wood, L. Tibaldo, O. Tibolla, N. Vilchez, Y. Hanabata, F. Gargano, P. D. Smith, T. Reposeur, A. W. Borgland, T. Uehara, M. Ziegler, M. N. Mazziotta, A. Chekhtman, P. Lubrano, Eric Charles, D. J. Suson, Jean Ballet, Ajello, M., Allafort, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Charles, E., Chekhtman, A., Ciprini, S., Claus, R., Cohen Tanugi, J., Cutini, S., Angelis, A., Palma, F., Dermer, C. D., E. d. C., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Frailis, M., Fukazawa, Y., Fukui, Y., Fusco, P., Gargano, F., Gasparrini, D., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grove, J. E., Guiriec, S., Hadasch, D., Hanabata, Y., Harding, A. K., Hayashi, K., Hays, E., Itoh, R., Johannesson, G., Johnson, A. S., Kamae, T., Katagiri, H., Kataoka, J., Kn\odlseder, J., Kubo, H., Kuss, M., Lande, J., Latronico, L., Lee, S., Lionetto, A. M., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mehault, J., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann Godo, M., Nishino, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Parent, D., Pelassa, V., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Rain\`o, S., Rando, R., Reimer, A., Reimer, O., Reposeur, T., Roth, M., Sadrozinski, H. F., Sgr\`o, C., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Troja, E., Uchiyama, Y., Uehara, T., Usher, T. L., Vandenbroucke, J., Etten, A., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yamamoto, H., Yamazaki, R., Yang, Z., Yasuda, H., Ziegler, M., Zimmer, S., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), GLAST, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, acceleration of particles, cosmic rays, gamma rays, ISM, ISM: individual objects (G8.7–0.1, HESS J1804–216), ISM: supernova remnants, Spectral line, Particle decay, individual objects: G8.7{\ndash}0.1 HESS J1804{\ndash}216 [ISM], gamma rays: ISM, ISM: individual objects (G8.7?0.1, ISM [gamma rays], ISM: individual objects (G8.7?0.1, HESS J1804?216), Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, 14. Life underwater, Supernova remnant, ISM: individual objects (G8.7-0.1, 010303 astronomy & astrophysics, acceleration of particle, cosmic ray, Astrophysics::Galaxy Astrophysics, Acceleration of particles, ISM: individual objects (G8.7-0.1, HESS J1804-216), Physics, Spectral index, HESS J1804-216), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], supernova remnants [ISM], Astronomy, Gamma-ray astronomy, ISM: individual objects: G8.7{\ndash}0.1 HESS J1804{\ndash}216, Interstellar medium, HESS J1804?216), High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

We present a detailed analysis of the GeV gamma-ray emission toward the supernova remnant (SNR) G8.7-0.1 with the Large Area Telescope (LAT) onboard the \emph{Fermi} Gamma-ray Space Telescope. An investigation of the relationship among G8.7-0.1 and the TeV unidentified source HESS J1804-216 provides us with an important clue on diffusion process of cosmic rays if particle acceleration operates in the SNR. The GeV gamma-ray emission is extended with most of the emission in positional coincidence with the SNR G8.7-0.1 and a lesser part located outside the western boundary of G8.7-0.1. The region of the gamma-ray emission overlaps spatially-connected molecular clouds, implying a physical connection for the gamma-ray structure. The total gamma-ray spectrum measured with LAT from 200 MeV--100 GeV can be described by a broken power-law function with a break of 2.4 $\pm$ 0.6 (stat) $\pm$ 1.2 (sys) GeV, and photon indices of 2.10 $\pm$ 0.06 (stat) $\pm$ 0.10 (sys) below the break and 2.70 $\pm$ 0.12 (stat) $\pm$ 0.14 (sys) above the break. Given the spatial association among the gamma rays, the radio emission of G8.7$-$0.1, and the molecular clouds, the decay of $\pi^{0}$s produced by particles accelerated in the SNR and hitting the molecular clouds naturally explains the GeV gamma-ray spectrum. We also find that the GeV morphology is not well represented by the TeV emission from HESS J1804$-$216 and that the spectrum in the GeV band is not consistent with the extrapolation of the TeV gamma-ray spectrum. The spectral index of the TeV emission is consistent with the particle spectral index predicted by a theory that assumes energy-dependent diffusion of particles accelerated in an SNR. We discuss the possibility that the TeV spectrum originates from the interaction of particles accelerated in G8.7$-$0.1 with molecular clouds, and we constrain the diffusion coefficient of the particles., Comment: 42 pages, 5 figures. Accepted for publication in the Astrophysical Journal. Corresponding authors: Y. Hanabata, H. Katagiri

Published
2012

18. VERY HIGH ENERGY γ -RAYS FROM THE UNIVERSE’S MIDDLE AGE: DETECTION OF THE z = 0.940 BLAZAR PKS 1441+25 WITH MAGIC

Author

M. Pesce Rollins, Lluis Font, Francesco Longo, Abelardo Moralejo, I. Snidaric, Thomas Bretz, M. Feige, E. Moretti, Mosè Mariotti, A.-K. Overkemping, M. Makariev, D. Wolfert, E. Lorenz, Max Ludwig Ahnen, S. Haarto, P. Giammaria, T. Steinbring, S. Maldera, F. de Palma, D. Dominis Prester, Nicola Omodei, Marcel Strzys, P. Haeusner, R. Clavero, W. Bednarek, Fabrizio Tavecchio, R. Reinthal, R. Zanin, Elina Lindfors, D. Nakajima, Daniela Dorner, Adrian Biland, P. G. Prada Moroni, R. A. Cameron, M. Gaug, M. Caragiulo, Johan Bregeon, Saverio Lombardi, Kyoshi Nishijima, Arka Chatterjee, D. Fidalgo, U. Barres de Almeida, Damir Lelas, J. Kushida, Daniel Mazin, Igor V. Moskalenko, Olaf Reimer, Julie McEnery, Anne Lähteenmäki, Hiromitsu Takahashi, Julian Sitarek, A. López Oramas, J. Herrera, Wolfgang Rhode, J. Rico, J. Klamt, Dorota Sobczyńska, Jose Luis Contreras, Hiroyasu Tajima, X. Paredes Fortuny, Koji Noda, J. Li, A. Niedzwiecki, Masahiro Teshima, P. Bruel, E. Orlando, Yusuke Konno, T. Toyama, E. Recillas, V. Fallah Ramazani, Elisa Bernardini, K. S. Wood, Carmelo Sgrò, Riccardo Rando, Nikola Godinovic, T. Ohsugi, Eleonora Troja, Juan Cortina, D. J. Thompson, F. Di Pierro, Benito Marcote, P. Fusco, E. Colombo, Stefano Ansoldi, Ievgen Vovk, Oscar Blanch, N. Zottmann, E. Hays, Talvikki Hovatta, Riccardo Paoletti, M. Razzano, Ivica Puljak, E. Nuss, David Paneque, C. Delgado Mendez, Filippo D'Ammando, F. Piron, Pierre Colin, B. De Lotto, Stefano Covino, A. De Angelis, Luigi Pacciani, A. Treves, Vitaly Neustroev, T. Schweizer, M. Kuss, R. Bonino, J. Palacio, R. Mirzoyan, I. A. Grenier, P. Temnikov, Stefano Ciprini, E. de Oña Wilhelmi, Nestor Mirabal, P. Da Vela, L. Carrasco, Marcello Giroletti, L. O. Takalo, D. Guberman, M. I. Martínez, J. M. Paredes, E. Cavazzuti, M. Mayer, Juri Poutanen, S. Rainò, Antonio Stamerra, F. Borracci, Tsunefumi Mizuno, Y. Hanabata, A. González Muñoz, G. Maneva, Marina Manganaro, P. Spinelli, S. Bonnefoy, Kari Nilsson, T. A. Porter, Gloria Spandre, J. Hose, P. Antoranz, Tomoki Saito, D. Tescaro, D. Galindo, U. Menzel, E. Prandini, M. Will, G. Chiaro, Marco Ajello, J. B. Thayer, Merja Tornikoski, F. Loparco, Markus Garczarczyk, Francesco Giordano, B. Banerjee, Sabrina Einecke, D. Elsaesser, J. W. Hewitt, R. Desiante, D. Garrido Terrats, A. Fernández Barral, Diego F. Torres, James Chiang, H. Takami, M. Palatiello, S. Buson, Alessandro Carosi, J. Rodriguez Garcia, P. Lubrano, Mislav Baloković, A. Carraminana, Konstancja Satalecka, A. Sillanpää, L. Di Venere, Dario Gasparrini, Michele Doro, Roger Blandford, Vassil Verguilov, Roopesh Ojha, L. Maraschi, Francesco Dazzi, Ana Babić, Gareth Hughes, F. Spada, Julia Thaele, Tomislav Terzić, A. Porras, M. E. Monzani, A. Morselli, Jose Miguel Miranda, G. A. Caliandro, A. Reimer, W. Idec, A. Hahn, E. Carmona, Stefan Larsson, J. Kania, M. Hayashida, Wu M. H., Steven N. Shore, C. Lorey, Marc Ribó, P. Bangale, E. J. Siskind, Hidetoshi Kubo, Dario Hrupec, M. A. Lopez, G. Bonnoli, F. Gargano, K. Mallot, R. J. García López, R. Lopez Coto, Massimo Persic, V. H. Chavushyan, Liang Li, Guido Barbiellini, J. León Tavares, Pratik Majumdar, M. V. Fonseca, K. Kodani, Reiko Orito, Aaron Dominguez, Juan Abel Barrio, Luca Baldini, J. E. Ward, Sylvain Guiriec, Mn Mazziotta, Christian Fruck, J. S. Perkins, Nicola Giglietto, B. Biasuzzi, M. N. Lovellette, P. A. Caraveo, J. Becerra González, Elisabetta Bissaldi, G. Pivato, Andrei Berdyugin, T. Jogler, Ronaldo Bellazzini, C. Schultz, Louis Antonelli, K. Frantzen, Denis Bastieri, S. Paiano, Karl Mannheim, A. La Barbera, D. Eisenacher Glawion, M. Nievas Rosillo, Universitat de Barcelona, 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), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), ITA, USA, GBR, FRA, DEU, ESP, AFG, ALB, DZA, AND, AGO, BGR, BFA, BDI, KHM, CMR, CAN, CPV, CS, TCD, CYM, COD, CHL, TWN, CYP, VAT, COL, COM, COG, PRK, KOR, CIV, DOM, CCK, CRI, HRV, CUB, DNK, DMA, ECU, EGY, SLV, ARE, CHN, ERI, AIA, EST, ETH, FJI, PHL, FIN, GAB, GMB, GAZA, ZAF, GEO, COK, GHA, JAM, JPN, GIB, DJI, JOR, GRC, REU, GRD, GRL, GLP, FRO, GUM, GTM, GIN, GNB, GNQ, GUI, ROU, GUY, GUF, HTI, HND, FLK, HKG, IND, IDN, IRN, MNP, RWA, MHL, MUS, UMI, SLB, TCA, VIR, ATA, VGB, ISR, KAZ, RUS, KGZ, KIR, SCG, KWT, LAO, LSO, LVA, ATG, LBN, LBR, ESH, LBY, LIE, LTU, LUX, MAC, MKD, MDG, MWI, ANT, MDV, AUS, MYS, MLI, MLT, MAR, MTQ, MRT, MYT, MEX, MDA, SAU, IRQ, MCO, MNG, MSR, MOZ, MMR, NAM, NRU, NPL, NIC, NER, KNA, ARG, NGA, NIU, NOR, NCL, NZL, OMN, NLD, PAK, PLW, SPM, PAN, ARM, PNG, PRY, PER, PCN, PYF, POL, PRI, PRT, VCT, QAT, CZE, ABW, CAF, ASM, WSM, SMR, LCA, SHN, STP, SEN, IRL, AUT, SYC, SLE, SGP, SYR, SVK, SVN, SOM, LKA, ISL, FSM, AZE, SGS, SDN, SUR, SJM, SWE, CHE, SWZ, TJK, BVT, TZA, IOT, BHS, ATF, PSE, THA, TLS, TGO, TKL, TON, MAN, TTO, TUN, TUR, BHR, TKM, TUV, UKR, UGA, HUN, URY, CXR, UZB, VUT, VEN, VNM, BGD, WLF, YEM, ZMB, ZWE, BRB, HMD, BEL, BLZ, BEN, BMU, BTN, BLR, BOL, BIH, BWA, BRA, NFK, BRN, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., De Almeida, U. Barre, Barrio, J. A., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Oña Wilhelmi, E., Mendez, C. Delgado, Di Pierro, F., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Glawion, D. Eisenacher, Elsaesser, D., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Giammaria, P., Godinović, N., Muñoz, A. González, Guberman, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Saito, T., Satalecka, K., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Ajello, M., Baldini, L., Barbiellini, G., Bastieri, D., González, J. Becerra, Bellazzini, R., Bissaldi, E., Blandford, R. D., Bonino, R., Bregeon, J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Chiang, J., Chiaro, G., Ciprini, S., D'Ammando, F., De Palma, F., Desiante, R., Di Venere, L., Domínguez, A., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Grenier, I. A., Guiriec, S., Hays, E., Hewitt, J. W., Jogler, T., Kuss, M., Larsson, S., Li, J., Li, L., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Mirabal, N., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Nuss, E., Ojha, R., Ohsugi, T., Omodei, N., Orlando, E., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Porter, T. A., Raino, S., Rando, R., Razzano, M., Reimer, A., Reimer, O., Sgro, C., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Tajima, H., Takahashi, H., Thayer, J. B., Thompson, D. J., Troja, E., Wood, K. S., Balokovic, M., Berdyugin, A., Carraminana, A., Carrasco, L., Chavushyan, V., Ramazani, V. Fallah, Feige, M., Haarto, S., Haeusner, P., Hovatta, T., Kania, J., Klamt, J., Lähteenmäki, A., Leon Tavares, J., Lorey, C., Pacciani, L., Porras, A., Recillas, E., Reinthal, R., Tornikoski, M., Wolfert, D., Zottmann, N., Ahnen ML, Ansoldi S, Antonelli LA, Antoranz P, Babic A, Banerjee B, Bangale P, De Almeida UB, Barrio JA, Bednarek W, Bernardini E, Biasuzzi B, Biland A, Blanch O, Bonnefoy S, Bonnoli G, Borracci F, Bretz T, Carmona E, Carosi A, Chatterjee A, Clavero R, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi F, De Angelis A, De Lotto B, Wilhelmi ED, Mendez CD, Di Pierro F, Prester DD, Dorner D, Doro M, Einecke S, Glawion DE, Elsaesser D, Fernandez-Barral A, Fidalgo D, Fonseca MV, Font L, Frantzen K, Fruck C, Galindo D, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Giammaria P, Godinovic N, Munoz AG, Guberman D, Hahn A, Hanabata Y, Hayashida M, Herrera J, Hose J, Hrupec D, Hughes G, Idec W, Kodani K, Konno Y, Kubo H, Kushida J, La Barbera A, Lelas D, Lindfors E, Lombardi S, Lopez M, Lopez-Coto R, Lopez-Oramas A, Lorenz E, Majumdar P, Makariev M, Mallot K, Maneva G, Manganaro M, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Miranda JM, Mirzoyan R, Moralejo A, Moretti E, Nakajima D, Neustroev V, Niedzwiecki A, Rosillo M, Nilsson K, Nishijima K, Noda K, Orito R, Overkemping A, Paiano S, Palacio J, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Persic M, Poutanen J, Moroni PGP, Prandini E, Puljak I, Rhode W, Ribo M, Rico J, Garcia JR, Saito T, Satalecka K, Schultz C, Schweizer T, Shore SN, Sillanpaa A, Sitarek J, Snidaric I, Sobczynska D, Stamerra A, Steinbring T, Strzys M, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Thaele J, Torres DF, Toyama T, Treves A, Verguilov V, Vovk I, Ward JE, Will M, Wu MH, Zanin R, Ajello M, Baldini L, Barbiellini G, Bastieri D, Gonzalez JB, Bellazzini R, Bissaldi E, Blandford RD, Bonino R, Bregeon J, Bruel P, Buson S, Caliandro GA, Cameron RA, Caragiulo M, Caraveo PA, Cavazzuti E, Chiang J, Chiaro G, Ciprini S, DAmmando F, de Palma F, Desiante R, Di Venere L, Dominguez A, Fusco P, Gargano F, Gasparrini D, Giglietto N, Giordano F, Giroletti M, Grenier IA, Guiriec S, Hays E, Hewitt JW, Jogler T, Kuss M, Larsson S, Li J, Li L, Longo F, Loparco F, Lovellette MN, Lubrano P, Maldera S, Mayer M, Mazziotta MN, McEnery JE, Mirabal N, Mizuno T, Monzani ME, Morselli A, Moskalenko IV, Nuss E, Ojha R, Ohsugi T, Omodei N, Orlando E, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Porter TA, Raino S, Rando R, Razzano M, Reimer A, Reimer O, Sgro C, Siskind EJ, Spada F, Spandre G, Spinelli P, Tajima H, Takahashi H, Thayer JB, Thompson DJ, Troja E, Wood KS, Balokovic M, Berdyugin A, Carraminana A, Carrasco L, Chavushyan V, Ramazani VF, Feige M, Haarto S, Haeusner P, Hovatta T, Kania J, Klamt J, Lahteenmaki A, Leon-Tavares J, Lorey C, Pacciani L, Porras A, Recillas E, Reinthal R, Tornikoski M, Wolfert D, and Zottmann N

Subjects
individual (PKS 1441+25) [quasars], cosmic background radiation, Astrophysics, 7. Clean energy, Raigs gamma, Jets (Astrofísica), galaxies: active, galaxies: jets, gamma rays: galaxies, quasars: individual (PKS 1441+25), MAGIC (telescope), Space and Planetary Science, Astronomy and Astrophysics, ComputingMilieux_MISCELLANEOUS, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Extragalactic background light, active [galaxies], Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], cosmic background radiation – galaxies: active – galaxies: jets – gamma rays: galaxies – quasars: individual (PKS 1441+25), galaxie [gamma rays], Blazar, Quasars, Quàsars, Gamma rays, Quasar, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Astrophysical jets, jet [galaxies], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Galàxies actives, Active galaxies, ddc:520, Fermi Gamma-ray Space Telescope
Abstract

The flat-spectrum radio quasar PKS 1441+25 at a redshift of z = 0.940 is detected between 40 and 250 GeV with a significance of 25.5 {\sigma} using the MAGIC telescopes. Together with the gravitationally lensed blazar QSO B0218+357 (z = 0.944), PKS 1441+25 is the most distant very high energy (VHE) blazar detected to date. The observations were triggered by an outburst in 2015 April seen at GeV energies with the Large Area Telescope on board Fermi. Multi-wavelength observations suggest a subdivision of the high state into two distinct flux states. In the band covered by MAGIC, the variability time scale is estimated to be 6.4 +/- 1.9 days. Modeling the broadband spectral energy distribution with an external Compton model, the location of the emitting region is understood as originating in the jet outside the broad line region (BLR) during the period of high activity, while being partially within the BLR during the period of low (typical) activity. The observed VHE spectrum during the highest activity is used to probe the extragalactic background light at an unprecedented distance scale for ground-based gamma-ray astronomy., Comment: Corresponding Authors: J. Becerra (josefa.becerra@nasa.gov), M. Nievas Rosillo (mnievas@ucm.es), M. Manganaro (manganaro@iac.es), F. Tavecchio (fabrizio.tavecchio@brera.inaf.it) Published in The Astrophysical Journal Letters (ApJL), 2015ApJ...815L..23A, DOI: 10.1088/2041-8205/815/2/L23

Published
2015

20. FERMI-LAT OBSERVATIONS OF HIGH- AND INTERMEDIATE-VELOCITY CLOUDS: TRACING COSMIC RAYS IN THE HALO OF THE MILKY WAY

Author

L. Tibaldo, Gudlaugur Johannesson, M. Negro, A. Franckowiak, I. A. Grenier, D. J. Marshall, Seth Digel, J. M. Casandjian, T. A. Porter, Elena Orlando, Igor V. Moskalenko, Olaf Reimer, and Andrew W. Strong

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Article, Galaxy, Interstellar medium, Galactic halo, Space and Planetary Science, Halo, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of gamma-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for gamma-ray emission produced by CR interactions in several high- and intermediate-velocity clouds located at up to ~ 7 kpc above the Galactic plane. We achieve the first detection of intermediate-velocity clouds in gamma rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the gamma-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models., Comment: Accepted for publication in the Astrophysical Journal

Published
2015

21. HIGH-ENERGY PARTICLE TRANSPORT IN THREE-DIMENSIONAL HYDRODYNAMIC MODELS OF COLLIDING-WIND BINARIES

Author

Ralf Kissmann, Olaf Reimer, Guillaume Dubus, K. Reitberger, and Anita Reimer

Subjects
Physics, High energy particle, Radiative cooling, Astrophysics::High Energy Astrophysical Phenomena, Bremsstrahlung, Astronomy and Astrophysics, 7. Clean energy, Charged particle, Computational physics, Relativistic particle, Acceleration, Stars, 13. Climate action, Space and Planetary Science, Orbital motion
Abstract

Massive stars in binary systems (such as WR 140, WR 147, or η Carinae) have long been regarded as potential sources of high-energy γ-rays. The emission is thought to arise in the region where the stellar winds collide and produce relativistic particles that subsequently might be able to emit γ-rays. Detailed numerical hydrodynamic simulations have already offered insight into the complex dynamics of the wind collision region (WCR), while independent analytical studies, albeit with simplified descriptions of the WCR, have shed light on the spectra of charged particles. In this paper, we describe a combination of these two approaches. We present a three-dimensional hydrodynamical model for colliding stellar winds and compute spectral energy distributions of relativistic particles for the resulting structure of the WCR. The hydrodynamic part of our model incorporates the line-driven acceleration of the winds, gravity, orbital motion, and the radiative cooling of the shocked plasma. In our treatment of charged particles, we consider diffusive shock acceleration in the WCR and the subsequent cooling via inverse Compton losses (including Klein-Nishina effects), bremsstrahlung, collisions, and other energy loss mechanisms.

Published
2014

22. The Absolute Flux of Protons and Helium at the Top of the Atmosphere Using IMAX

Author

W. R. Webber, A.E. Labrador, Jonathan F. Ormes, R. L. Golden, K. E. Krombel, I. L. Rasmussen, John Mitchell, R. A. Mewaldt, M. Hof, L. M. Barbier, W. Menn, S. M. Schindler, E. R. Christian, Steven Stochaj, Andrew Davis, Olaf Reimer, Robert E. Streitmatter, M. Simon, and John Krizmanic

Subjects
Physics, Spectrometer, Proton, chemistry.chemical_element, Astronomy and Astrophysics, Cosmic ray, Scintillator, Spectral line, Nuclear physics, chemistry, Space and Planetary Science, Antiproton, Nuclear Experiment, Helium, Cherenkov radiation
Abstract

The cosmic-ray proton and helium spectra from 0.2 GeV nucleon^(-1) to about 200 GeV nucleon^(-1) have been measured with the balloon-borne experiment Isotope Matter-Antimatter Experiment (IMAX) launched from Lynn Lake, Manitoba, Canada, in 1992. IMAX was designed to search for antiprotons and light isotopes using a superconducting magnet spectrometer together with scintillators, a time-of-flight system, and Cherenkov detectors. Using redundant detectors, an extensive examination of the instrument efficiency was carried out. We present here the absolute spectra of protons and helium corrected to the top of the atmosphere and to interstellar space. If demodulated with a solar modulation parameter of Φ = 750 MV, the measured interstellar spectra between 20 and 200 GV can be represented by a power law in rigidity, with (1.42 ± 0.21) × 10^4R^(-2.71±0.04) (m^2 GV s sr)^(-1) for protons and (3.15 ± 1.03) × 10^3R^(-2.79±0.08) (m^2 GV s sr)^(-1) for helium.

Published
2000

23. ERRATUM: 'CONSTRAINTS ON THE COSMIC-RAY DENSITY GRADIENT BEYOND THE SOLAR CIRCLE FROM FERMI γ-RAY OBSERVATIONS OF THE THIRD GALACTIC QUADRANT' (2011, ApJ, 726, 81)

Author

Francesco Longo, A. Chekhtman, J. Mehault, R. Dubois, A. W. Borgland, W. B. Focke, Eric Charles, P. L. Nolan, D. Parent, P. Spinelli, T. Uehara, D. J. Suson, Francesco Giordano, Nicola Omodei, M. Ziegler, Pierrick Martin, Joachim Ripken, R. A. Cameron, Hiromitsu Takahashi, S. Murgia, Jean Ballet, Andrey Vladimirov, P. Wang, P. Bruel, F. Piron, P. Lubrano, Julie McEnery, Yasunobu Uchiyama, E. Orlando, Stefano Ciprini, R. Buehler, P. Fusco, Emanuele Bonamente, Hartmut Sadrozinski, Melissa Pesce-Rollins, R. Claus, Alice K. Harding, J. M. Casandjian, Peter F. Michelson, Tadayuki Takahashi, Marcello Giroletti, Ryosuke Itoh, Marco Ajello, Sho Nishino, J. B. Thayer, Elliott D. Bloom, Luca Baldini, A. Tramacere, G. Godfrey, Ronaldo Bellazzini, Hideaki Katagiri, A. Makeev, Takaaki Tanaka, T. J. Brandt, K. Hayashi, Igor V. Moskalenko, M. E. Monzani, S. Rainò, Zhenwei Yang, Tsunefumi Mizuno, Mn Mazziotta, Carmelo Sgrò, Riccardo Rando, T. Ohsugi, F. de Palma, F. Loparco, Olaf Reimer, S. Buson, Yasushi Fukazawa, Jan Conrad, T. A. Porter, R. E. Hughes, Shiu-Hang Lee, V. Pelassa, E. Nuss, Seth Digel, Charles D. Dermer, Claudia Cecchi, L. Tibaldo, M. Kuss, Diego F. Torres, Daniela Hadasch, M. Ozaki, D. J. Thompson, J. F. Ormes, A. P. Waite, C. Favuzzi, J. P. Norris, A. Morselli, V. Vitale, J. Bregeon, M. Razzano, T. Sada, Stefan Funk, S. Germani, K. S. Wood, T. Kamae, W. N. Johnson, B. Berenji, Keith Bechtol, A. Reimer, Gudlaugur Johannesson, Justin Vandenbroucke, Guido Barbiellini, M. Brigida, E. J. Siskind, M. Hayashida, C. Monte, N. Vilchez, Jun Kataoka, Markus Ackermann, M. Llena-Garde, Andrew W. Strong, A. S. Johnson, M. Pepe, T. Glanzman, Jürgen Knödlseder, Y. Hanabata, V. Vasileiou, F. Gargano, Luca Latronico, Nicola Giglietto, Denis Bastieri, M. N. Lovellette, P. A. Caraveo, James Chiang, Elizabeth C. Ferrara, Alessandro Brez, Persis S. Drell, I. A. Grenier, T. L. Usher, Atsushi Okumura, Gloria Spandre, J. Lande, Sylvain Guiriec, Johann Cohen-Tanugi, M. Naumann-Godo, M. S. Strickman, and G. A. Caliandro

Subjects
Physics, Density gradient, Space and Planetary Science, Galactic quadrant, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Fermi Gamma-ray Space Telescope
Published
2013

24. ERRATUM: 'THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS' (2010, ApJS, 187, 460)

Author

Na Wang, James Chiang, Roger Blandford, B. Lott, Cristobal M. Espinoza, Jun Kataoka, Ö. Çelik, V. M. Kaspi, A. S. Johnson, S. Cutini, F. Piron, Jean Ballet, Gudlaugur Johannesson, Sinéad McGlynn, I. A. Grenier, M. Hayashida, M. Roth, A. De Luca, C. Favuzzi, Stefano Ciprini, Felix Ryde, Lucas Guillemot, B. Giebels, A. Tramacere, A. Noutsos, Stefan Funk, Guido Barbiellini, H. Tajima, Nicola Omodei, S. Murgia, V. Vasileiou, Richard Dubois, Luca Baldini, T. Mizuno, M. Marelli, M. Frailis, P. Spinelli, Scott M. Ransom, Seth Digel, M. S. Jackson, F. de Palma, Matthew G. Baring, Alice K. Harding, Fernando Camilo, Benjamin Stappers, C. Farnier, Elliott D. Bloom, B. M. Baughman, L. Tibaldo, L. R. Cominsky, Igor V. Moskalenko, T. A. Porter, Jürgen Knödlseder, Brian L Winer, Sylvain Guiriec, Gloria Spandre, S. Rainò, Eric V. Gotthelf, S. Germani, Mn Mazziotta, Olaf Reimer, A. A. Moiseev, Christo Venter, A. van Etten, Francesco Longo, P. Fusco, W. B. Atwood, Diego F. Torres, Omar Tibolla, Paul J. Wang, Andrew W. Strong, Denise A. Smith, A. Sellerholm, Roger W. Romani, Grzegorz Madejski, Nicola Giglietto, Hartmut Sadrozinski, Robert R. Rando, M. Kramer, David Sánchez, Dario Gasparrini, F. Gargano, Ronaldo Bellazzini, Gilles Theureau, Hideaki Katagiri, Luca Latronico, A. Sander, C. Meurer, T. J. Johnson, Y. Hanabata, M. N. Lovellette, F. Loparco, Paolo Giommi, Carmelo Sgrò, Denis Bastieri, P. D. Smith, Persis S. Drell, Alessandro Brez, E. Do Couto E Silva, Aous A. Abdo, T. L. Schalk, E. Nuss, W. N. Johnson, G. A. Caliandro, Paul S. Ray, C. Gwon, Elizabeth C. Ferrara, Gottfried Kanbach, David Paneque, M. Kuss, A. Y. Rodriguez, Randall P. Johnson, P. Weltevrede, Robin H. D. Corbet, D. Parent, J. E. Grove, Yasushi Fukazawa, P. Caraveo, Karen Watters, E. Hays, Jan Conrad, Pascal Bruel, Ismaël Cognard, Y. Uchiyama, Johann Cohen-Tanugi, P. M. Saz Parkinson, M. Dormody, Nanda Rea, Melissa Pesce-Rollins, M. S. Strickman, Andrew Lyne, A. P. Waite, T. Kamae, Peter F. Michelson, Richard N. Manchester, M. Lemoine-Goumard, G.L. Godfrey, Charles D. Dermer, A. Makeev, K. S. Wood, J. G. Thayer, Matthew Kerr, Tadayuki Takahashi, W. Mitthumsiri, R. Claus, S. J. Fegan, M. E. Monzani, J. B. Thayer, P. R. den Hartog, Jean-Luc Starck, J. P. Norris, W. B. Focke, A. Morselli, V. Vitale, A. Chekhtman, J. Bregeon, A. Reimer, Keith Bechtol, Marco Ajello, S. Buson, J. Lande, M. Razzano, A. De Angelis, M. Brigida, T. L. Usher, M.-H. Grondin, R. E. Hughes, Stephen E. Thorsett, E. Charles, M. Ozaki, J. F. Ormes, Emanuele Bonamente, D. J. Thompson, Francesco Giordano, Hiromitsu Takahashi, D. Dumora, P. L. Nolan, N. Gehrels, Takaaki Tanaka, T. Mineo, Claudia Cecchi, T. Glanzman, E. Orlando, V. Pelassa, T. Ylinen, R. A. Cameron, Julie McEnery, Steven Ritz, D. J. Suson, T. H. Burnett, B. Berenji, Gianluca Giavitto, M. Ziegler, Takeshi Nakamori, J. M. Casandjian, E. J. Siskind, T. Ohsugi, C. C. Cheung, Magnus Axelsson, Paulo C. C. Freire, W. Mcconville, N. Vilchez, E. Striani, P. Fortin, G. Tosti, Markus Ackermann, P. Lubrano, Simon Johnston, M. Pepe, Margaret A. Livingstone, Jeffrey D. Scargle, N. Kawai, M. L. Kocian, C. Monte, T. Reposeur, A. W. Borgland, and J. H. Panetta

Subjects
Physics, 010308 nuclear & particles physics, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, law.invention, Telescope, Pulsar, Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Published
2011

25. Erratum

Author

Andrew W. Strong, Igor V. Moskalenko, and Olaf Reimer

Subjects
Physics, Space and Planetary Science, Continuum (design consultancy), Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Galaxy
Published
2000

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