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102 results on '"Caraveo, A."'

1. Periodic Gamma-Ray Modulation of the Blazar PG 1553+113 Confirmed by Fermi-LAT and Multiwavelength Observations

Author

S. Abdollahi, L. Baldini, G. Barbiellini, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, E. Cavazzuti, C. C. Cheung, G. Chiaro, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, S. Cutini, F. D’Ammando, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Garrappa, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, E. Hays, D. Horan, M. Kuss, S. Larsson, M. Laurenti, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, L. Marcotulli, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, M. Perri, M. Persic, M. Pesce-Rollins, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, P. M. Saz Parkinson, L. Scotton, D. Serini, A. Sesana, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, J. Valverde, F. Verrecchia, and G. Zaharijas

Subjects
Active galactic nuclei, Blazars, Gamma-rays, Gamma-ray sources, Gamma-ray telescopes, Gamma-ray astronomy, Astrophysics, QB460-466
Abstract

A 2.1 yr periodic oscillation of the gamma-ray flux from the blazar PG 1553+113 has previously been tentatively identified in ∼7 yr of data from the Fermi Large Area Telescope. After 15 yr of Fermi sky-survey observations, doubling the total time range, we report >7 cycle gamma-ray modulation with an estimated significance of 4 σ against stochastic red noise. Independent determinations of oscillation period and phase in the earlier and the new data are in close agreement (chance probability

Published
2024
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3. AGILE Gamma-Ray Detection of the Exceptional GRB 221009A

Author

Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, and Fabio D’Amico

Subjects
Gamma-ray bursts, Gamma-ray astronomy, Gamma-ray observatories, Astrophysics, QB460-466
Abstract

Gamma-ray emission in the MeV–GeV range from explosive cosmic events is of invaluable relevance to understanding physical processes related to the formation of neutron stars and black holes. Here we report on the detection by the AGILE satellite in the MeV–GeV energy range of the remarkable long-duration gamma-ray burst GRB 221009A. The AGILE onboard detectors have good exposure to GRB 221009A during its initial crucial phases. Hard X-ray/MeV emission in the prompt phase lasted hundreds of seconds, with the brightest radiation being emitted between 200 and 300 s after the initial trigger. Very intense GeV gamma-ray emission is detected by AGILE in the prompt and early afterglow phase up to 10,000 s. Time-resolved spectral analysis shows time-variable MeV-peaked emission simultaneous with intense power-law GeV radiation that persists in the afterglow phase. The coexistence during the prompt phase of very intense MeV emission together with highly nonthermal and hardening GeV radiation is a remarkable feature of GRB 221009A. During the prompt phase, the event shows spectrally different MeV and GeV emissions that are most likely generated by physical mechanisms occurring in different locations. AGILE observations provide crucial flux and spectral gamma-ray information regarding the early phases of GRB 221009A during which emission in the TeV range was reported.

Published
2023
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4. Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Author

S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D’Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, and G. Zaharijas

Subjects
Gamma-ray bursts, Astrophysics, QB460-466
Abstract

We report the discovery of GRB 221009A, the highest flux gamma-ray burst (GRB) ever observed by the Fermi Gamma-ray Burst Monitor (Fermi-GBM). This GRB has continuous prompt emission lasting more than 600 s, which smoothly transitions to afterglow emission visible in the Fermi-GBM energy range (8 keV–40 MeV), and total energetics higher than any other burst in the Fermi-GBM sample. By using a variety of new and existing analysis techniques we probe the spectral and temporal evolution of GRB 221009A. We find no emission prior to the Fermi-GBM trigger time ( t _0 ; 2022 October 9 at 13:16:59.99 UTC), indicating that this is the time of prompt emission onset. The triggering pulse exhibits distinct spectral and temporal properties suggestive of the thermal, photospheric emission of shock breakout, with significant emission up to ∼15 MeV. We characterize the onset of external shock at t _0 + 600 s and find evidence of a plateau region in the early-afterglow phase, which transitions to a slope consistent with Swift-XRT afterglow measurements. We place the total energetics of GRB 221009A in context with the rest of the Fermi-GBM sample and find that this GRB has the highest total isotropic-equivalent energy ( E _γ _,iso = 1.0 × 10 ^55 erg) and second highest isotropic-equivalent luminosity ( L _γ _,iso = 9.9 × 10 ^53 erg s ^–1 ) based on its redshift of z = 0.151. These extreme energetics are what allowed us to observe the continuously emitting central engine of Fermi-GBM from the beginning of the prompt emission phase through the onset of early afterglow.

Published
2023
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6. The Third Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars

Author

D. A. Smith, S. Abdollahi, M. Ajello, M. Bailes, L. Baldini, J. Ballet, M. G. Baring, C. Bassa, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, B. Bhattacharyya, E. Bissaldi, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, M. Burgay, T. H. Burnett, R. A. Cameron, F. Camilo, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, S. Ciprini, C. J. Clark, I. Cognard, A. Corongiu, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D’Ammando, A. de Angelis, M. E. DeCesar, S. De Gaetano, R. de Menezes, J. Deneva, F. de Palma, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, D. Dumora, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, C. Flynn, A. Franckowiak, P. C. C. Freire, Y. Fukazawa, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, D. Gasparrini, F. Giacchino, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, L. Guillemot, S. Guiriec, M. Gustafsson, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, X. Hou, F. Jankowski, R. P. Johnson, T. J. Johnson, S. Johnston, J. Kataoka, M. J. Keith, M. Kerr, M. Kramer, M. Kuss, L. Latronico, S.-H. Lee, D. Li, J. Li, B. Limyansky, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, M. Lower, P. Lubrano, A. G. Lyne, Y. Maan, S. Maldera, R. N. Manchester, A. Manfreda, M. Marelli, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, P. F. Michelson, M. Mickaliger, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. E. Monzani, A. Morselli, M. Negro, R. Nemmen, L. Nieder, E. Nuss, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, M. Palatiello, D. Paneque, G. Panzarini, A. Parthasarathy, M. Persic, M. Pesce-Rollins, R. Pillera, H. Poon, T. A. Porter, A. Possenti, G. Principe, S. Rainò, R. Rando, S. M. Ransom, P. S. Ray, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, N. Renault-Tinacci, R. W. Romani, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, R. Shannon, V. Sharma, Z. Shen, E. J. Siskind, G. Spandre, P. Spinelli, B. W. Stappers, T. E. Stephens, D. J. Suson, S. Tabassum, H. Tajima, D. Tak, G. Theureau, D. J. Thompson, O. Tibolla, D. F. Torres, J. Valverde, C. Venter, Z. Wadiasingh, N. Wang, P. Wang, P. Weltevrede, K. Wood, J. Yan, G. Zaharijas, C. Zhang, and W. Zhu

Subjects
Binary pulsars, Millisecond pulsars, Pulsar timing method, Rotation powered pulsars, Pulsars, Gamma-rays, Astrophysics, QB460-466
Abstract

We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phase-connected rotation ephemerides are achieved. A further dozen optical and/or X-ray binary systems colocated with LAT sources also likely harbor gamma-ray MSPs. This catalog thus reports roughly 340 gamma-ray pulsars and candidates, 10% of all known pulsars, compared to ≤11 known before Fermi. Half of the gamma-ray pulsars are young. Of these, the half that are undetected in radio have a broader Galactic latitude distribution than the young radio-loud pulsars. The others are MSPs, with six undetected in radio. Overall, ≥236 are bright enough above 50 MeV to fit the pulse profile, the energy spectrum, or both. For the common two-peaked profiles, the gamma-ray peak closest to the magnetic pole crossing generally has a softer spectrum. The spectral energy distributions tend to narrow as the spindown power $\dot{E}$ decreases to its observed minimum near 10 ^33 erg s ^−1 , approaching the shape for synchrotron radiation from monoenergetic electrons. We calculate gamma-ray luminosities when distances are available. Our all-sky gamma-ray sensitivity map is useful for population syntheses. The electronic catalog version provides gamma-ray pulsar ephemerides, properties, and fit results to guide and be compared with modeling results.

Published
2023
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7. The Fermi-LAT Lightcurve Repository

Author

S. Abdollahi, M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, E. Burns, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, S. Cutini, F. D’Ammando, S. De Gaetano, S. W. Digel, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, A. Franckowiak, Y. Fukazawa, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, C. Gasbarra, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, D. Horan, X. Hou, G. Jóhannesson, M. Kerr, D. Kocevski, M. Kuss, L. Latronico, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, J. S. Perkins, M. Persic, M. Pesce-Rollins, R. Pillera, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, M. Sánchez-Conde, P. M. Saz Parkinson, Jeff Scargle, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. J. Thompson, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, S. Wagner, and K. Wood

Subjects
Gamma-ray astronomy, Active galactic nuclei, Light curves, Astrophysics, QB460-466
Abstract

The Fermi Large Area Telescope (LAT) lightcurve repository (LCR) is a publicly available, continually updated library of gamma-ray lightcurves of variable Fermi-LAT sources generated over multiple timescales. The Fermi-LAT LCR aims to provide publication-quality lightcurves binned on timescales of 3, 7, and 30 days for 1525 sources deemed variable in the source catalog of the first 10 yr of Fermi-LAT observations. The repository consists of lightcurves generated through full likelihood analyses that model the sources and the surrounding region, providing fluxes and photon indices for each time bin. The LCR is intended as a resource for the time-domain and multimessenger communities by allowing users to search LAT data quickly to identify correlated variability and flaring emission episodes from gamma-ray sources. We describe the sample selection and analysis employed by the LCR and provide an overview of the associated data access portal.

Published
2023
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8. The Fermi-LAT Lightcurve Repository.

Author

Abdollahi, S., Ajello, M., Baldini, L., Ballet, J., Bastieri, D., Becerra Gonzalez, J., Bellazzini, R., Berretta, A., Bissaldi, E., Bonino, R., Brill, A., Bruel, P., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cibrario, N., Ciprini, S., and Cristarella Orestano, P.

Published
2023
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10. Search for New Cosmic-Ray Acceleration Sites within the 4FGL Catalog Galactic Plane Sources.

Author

Abdollahi, S., Acero, F., Ackermann, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Berenji, B., Berretta, A., Bissaldi, E., Blandford, R. D., Bonino, R., Bruel, P., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Castro, D., and Chiaro, G.

Subjects
COSMIC rays, PROTON-proton interactions, SUPERNOVA remnants, SUPERNOVAE spectra, CATALOGS, CATALOGING
Abstract

Cosmic rays are mostly composed of protons accelerated to relativistic speeds. When those protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma-rays. This offers a compelling way to identify the acceleration sites of protons. A characteristic hadronic spectrum, with a low-energy break around 200 MeV, was detected in the gamma-ray spectra of four supernova remnants (SNRs), IC 443, W44, W49B, and W51C, with the Fermi Large Area Telescope. This detection provided direct evidence that cosmic-ray protons are (re-)accelerated in SNRs. Here, we present a comprehensive search for low-energy spectral breaks among 311 4FGL catalog sources located within 5° from the Galactic plane. Using 8 yr of data from the Fermi Large Area Telescope between 50 MeV and 1 GeV, we find and present the spectral characteristics of 56 sources with a spectral break confirmed by a thorough study of systematic uncertainty. Our population of sources includes 13 SNRs for which the protonâ€"proton interaction is enhanced by the dense target material; the high-mass gamma-ray binary LS I+61 303; the colliding wind binary η Carinae; and the Cygnus star-forming region. This analysis better constrains the origin of the gamma-ray emission and enlarges our view to potential new cosmic-ray acceleration sites. [ABSTRACT FROM AUTHOR]

Published
2022
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11. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation

Author

Abdalla, H., primary, Abe, H., additional, Acero, F., additional, Acharyya, A., additional, Adam, R., additional, Agudo, I., additional, Aguirre-Santaella, A., additional, Alfaro, R., additional, Alfaro, J., additional, Alispach, C., additional, Aloisio, R., additional, Batista, R. Alves, additional, Amati, L., additional, Amato, E., additional, Ambrosi, G., additional, Angüner, E.O., additional, Araudo, A., additional, Armstrong, T., additional, Arqueros, F., additional, Arrabito, L., additional, Asano, K., additional, Ascasíbar, Y., additional, Ashley, M., additional, Backes, M., additional, Balazs, C., additional, Balbo, M., additional, Balmaverde, B., additional, Larriva, A. Baquero, additional, Martins, V. Barbosa, additional, Barkov, M., additional, Baroncelli, L., additional, de Almeida, U. Barres, additional, Barrio, J.A., additional, Batista, P.-I., additional, González, J. Becerra, additional, Becherini, Y., additional, Beck, G., additional, Tjus, J. Becker, additional, Belmont, R., additional, Benbow, W., additional, Bernardini, E., additional, Berti, A., additional, Berton, M., additional, Bertucci, B., additional, Beshley, V., additional, Bi, B., additional, Biasuzzi, B., additional, Biland, A., additional, Bissaldi, E., additional, Biteau, J., additional, Blanch, O., additional, Bocchino, F., additional, Boisson, C., additional, Bolmont, J., additional, Bonanno, G., additional, Arbeletche, L. Bonneau, additional, Bonnoli, G., additional, Bordas, P., additional, Bottacini, E., additional, Böttcher, M., additional, Bozhilov, V., additional, Bregeon, J., additional, Brill, A., additional, Brown, A.M., additional, Bruno, P., additional, Bruno, A., additional, Bulgarelli, A., additional, Burton, M., additional, Buscemi, M., additional, Caccianiga, A., additional, Cameron, R., additional, Capasso, M., additional, Caprai, M., additional, Caproni, A., additional, Capuzzo-Dolcetta, R., additional, Caraveo, P., additional, Carosi, R., additional, Carosi, A., additional, Casanova, S., additional, Cascone, E., additional, Cauz, D., additional, Cerny, K., additional, Cerruti, M., additional, Chadwick, P., additional, Chaty, S., additional, Chen, A., additional, Chernyakova, M., additional, Chiaro, G., additional, Chiavassa, A., additional, Chytka, L., additional, Conforti, V., additional, Conte, F., additional, Contreras, J.L., additional, Coronado-Blazquez, J., additional, Cortina, J., additional, Costa, A., additional, Costantini, H., additional, Covino, S., additional, Cristofari, P., additional, Cuevas, O., additional, D'Ammando, F., additional, Daniel, M.K., additional, Davies, J., additional, Dazzi, F., additional, Angelis, A. De, additional, de Lavergne, M. de Bony, additional, Caprio, V. De, additional, Anjos, R. de Cássia dos, additional, Pino, E.M. de Gouveia Dal, additional, Lotto, B. De, additional, Martino, D. De, additional, de Naurois, M., additional, Wilhelmi, E. de Oña, additional, Palma, F. De, additional, de Souza, V., additional, Delgado, C., additional, Ceca, R. Della, additional, Volpe, D. della, additional, Depaoli, D., additional, Girolamo, T. Di, additional, Pierro, F. Di, additional, Díaz, C., additional, Díaz-Bahamondes, C., additional, Diebold, S., additional, Djannati-Ataï, A., additional, Dmytriiev, A., additional, Domínguez, A., additional, Donini, A., additional, Dorner, D., additional, Doro, M., additional, Dournaux, J., additional, Dwarkadas, V.V., additional, Ebr, J., additional, Eckner, C., additional, Einecke, S., additional, Ekoume, T.R.N., additional, Elsässer, D., additional, Emery, G., additional, Evoli, C., additional, Fairbairn, M., additional, Falceta-Goncalves, D., additional, Fegan, S., additional, Feng, Q., additional, Ferrand, G., additional, Fiandrini, E., additional, Fiasson, A., additional, Fioretti, V., additional, Foffano, L., additional, Fonseca, M.V., additional, Font, L., additional, Fontaine, G., additional, Franco, F.J., additional, Coromina, L. Freixas, additional, Fukami, S., additional, Fukazawa, Y., additional, Fukui, Y., additional, Gaggero, D., additional, Galanti, G., additional, Gammaldi, V., additional, Garcia, E., additional, Garczarczyk, M., additional, Gascon, D., additional, Gaug, M., additional, Gent, A., additional, Ghalumyan, A., additional, Ghirlanda, G., additional, Gianotti, F., additional, Giarrusso, M., additional, Giavitto, G., additional, Giglietto, N., additional, Giordano, F., additional, Glicenstein, J., additional, Goldoni, P., additional, González, J.M., additional, Gourgouliatos, K., additional, Grabarczyk, T., additional, Grandi, P., additional, Granot, J., additional, Grasso, D., additional, Green, J., additional, Grube, J., additional, Gueta, O., additional, Gunji, S., additional, Halim, A., additional, Harvey, M., additional, Collado, T. Hassan, additional, Hayashi, K., additional, Heller, M., additional, Cadena, S. Hernández, additional, Hervet, O., additional, Hinton, J., additional, Hiroshima, N., additional, Hnatyk, B., additional, Hnatyk, R., additional, Hoffmann, D., additional, Hofmann, W., additional, Holder, J., additional, Horan, D., additional, Hörandel, J., additional, Horvath, P., additional, Hovatta, T., additional, Hrabovsky, M., additional, Hrupec, D., additional, Hughes, G., additional, Hütten, M., additional, Iarlori, M., additional, Inada, T., additional, Inoue, S., additional, Insolia, A., additional, Ionica, M., additional, Iori, M., additional, Jacquemont, M., additional, Jamrozy, M., additional, Janecek, P., additional, Martínez, I. Jiménez, additional, Jin, W., additional, Jung-Richardt, I., additional, Jurysek, J., additional, Kaaret, P., additional, Karas, V., additional, Karkar, S., additional, Kawanaka, N., additional, Kerszberg, D., additional, Khélifi, B., additional, Kissmann, R., additional, Knödlseder, J., additional, Kobayashi, Y., additional, Kohri, K., additional, Komin, N., additional, Kong, A., additional, Kosack, K., additional, Kubo, H., additional, Palombara, N. La, additional, Lamanna, G., additional, Lang, R.G., additional, Lapington, J., additional, Laporte, P., additional, Lefaucheur, J., additional, Lemoine-Goumard, M., additional, Lenain, J., additional, Leone, F., additional, Leto, G., additional, Leuschner, F., additional, Lindfors, E., additional, Lloyd, S., additional, Lohse, T., additional, Lombardi, S., additional, Longo, F., additional, Lopez, A., additional, López, M., additional, López-Coto, R., additional, Loporchio, S., additional, Lucarelli, F., additional, Luque-Escamilla, P.L., additional, Lyard, E., additional, Maggio, C., additional, Majczyna, A., additional, Makariev, M., additional, Mallamaci, M., additional, Mandat, D., additional, Maneva, G., additional, Manganaro, M., additional, Manicò, G., additional, Marcowith, A., additional, Marculewicz, M., additional, Markoff, S., additional, Marquez, P., additional, Martí, J., additional, Martinez, O., additional, Martínez, M., additional, Martínez, G., additional, Martínez-Huerta, H., additional, Maurin, G., additional, Mazin, D., additional, Mbarubucyeye, J.D., additional, Miranda, D. Medina, additional, Meyer, M., additional, Micanovic, S., additional, Miener, T., additional, Minev, M., additional, Miranda, J.M., additional, Mitchell, A., additional, Mizuno, T., additional, Mode, B., additional, Moderski, R., additional, Mohrmann, L., additional, Molina, E., additional, Montaruli, T., additional, Moralejo, A., additional, Merino, J. Morales, additional, Morcuende-Parrilla, D., additional, Morselli, A., additional, Mukherjee, R., additional, Mundell, C., additional, Murach, T., additional, Muraishi, H., additional, Nagai, A., additional, Nakamori, T., additional, Nemmen, R., additional, Niemiec, J., additional, Nieto, D., additional, Nievas, M., additional, Nikolajuk, M., additional, Nishijima, K., additional, Noda, K., additional, Nosek, D., additional, Nozaki, S., additional, O'Brien, P., additional, Ohira, Y., additional, Ohishi, M., additional, Oka, T., additional, Ong, R.A., additional, Orienti, M., additional, Orito, R., additional, Orlandini, M., additional, Orlando, E., additional, Osborne, J.P., additional, Ostrowski, M., additional, Oya, I., additional, Pagliaro, A., additional, Palatka, M., additional, Paneque, D., additional, Pantaleo, F.R., additional, Paredes, J.M., additional, Parmiggiani, N., additional, Patricelli, B., additional, Pavletić, L., additional, Pe'er, A., additional, Pech, M., additional, Pecimotika, M., additional, Peresano, M., additional, Persic, M., additional, Petruk, O., additional, Pfrang, K., additional, Piatteli, P., additional, Pietropaolo, E., additional, Pillera, R., additional, Pilszyk, B., additional, Pimentel, D., additional, Pintore, F., additional, Pita, S., additional, Pohl, M., additional, Poireau, V., additional, Polo, M., additional, Prado, R.R., additional, Prast, J., additional, Principe, G., additional, Produit, N., additional, Prokoph, H., additional, Prouza, M., additional, Przybilski, H., additional, Pueschel, E., additional, Pühlhofer, G., additional, Pumo, M.L., additional, Punch, M., additional, Queiroz, F., additional, Quirrenbach, A., additional, Rando, R., additional, Razzaque, S., additional, Rebert, E., additional, Recchia, S., additional, Reichherzer, P., additional, Reimer, O., additional, Reimer, A., additional, Renier, Y., additional, Reposeur, T., additional, Rhode, W., additional, Ribeiro, D., additional, Ribó, M., additional, Richtler, T., additional, Rico, J., additional, Rieger, F., additional, Rizi, V., additional, Rodriguez, J., additional, Fernandez, G. Rodriguez, additional, Ramirez, J.C. Rodriguez, additional, Vázquez, J.J. Rodríguez, additional, Romano, P., additional, Romeo, G., additional, Roncadelli, M., additional, Rosado, J., additional, de Leon, A. Rosales, additional, Rowell, G., additional, Rudak, B., additional, Rujopakarn, W., additional, Russo, F., additional, Sadeh, I., additional, Saha, L., additional, Saito, T., additional, Greus, F. Salesa, additional, Sanchez, D., additional, Sánchez-Conde, M., additional, Sangiorgi, P., additional, Sano, H., additional, Santander, M., additional, Santos, E.M., additional, Sanuy, A., additional, Sarkar, S., additional, Saturni, F.G., additional, Sawangwit, U., additional, Scherer, A., additional, Schleicher, B., additional, Schovanek, P., additional, Schussler, F., additional, Schwanke, U., additional, Sciacca, E., additional, Scuderi, S., additional, Arroyo, M. Seglar, additional, Sergijenko, O., additional, Servillat, M., additional, Seweryn, K., additional, Shalchi, A., additional, Sharma, P., additional, Shellard, R.C., additional, Siejkowski, H., additional, Sinha, A., additional, Sliusar, V., additional, Slowikowska, A., additional, Sokolenko, A., additional, Sol, H., additional, Specovius, A., additional, Spencer, S., additional, Spiga, D., additional, Stamerra, A., additional, Stanič, S., additional, Starling, R., additional, Stolarczyk, T., additional, Straumann, U., additional, Strišković, J., additional, Suda, Y., additional, Świerk, P., additional, Tagliaferri, G., additional, Takahashi, H., additional, Takahashi, M., additional, Tavecchio, F., additional, Taylor, L., additional, Tejedor, L.A., additional, Temnikov, P., additional, Terrier, R., additional, Terzic, T., additional, Testa, V., additional, Tian, W., additional, Tibaldo, L., additional, Tonev, D., additional, Torres, D.F., additional, Torresi, E., additional, Tosti, L., additional, Tothill, N., additional, Tovmassian, G., additional, Travnicek, P., additional, Truzzi, S., additional, Tuossenel, F., additional, Umana, G., additional, Vacula, M., additional, Vagelli, V., additional, Valentino, M., additional, Vallage, B., additional, Vallania, P., additional, Eldik, C. van, additional, Varner, G.S., additional, Vassiliev, V., additional, Acosta, M. Vázquez, additional, Vecchi, M., additional, Veh, J., additional, Vercellone, S., additional, Vergani, S., additional, Verguilov, V., additional, Vettolani, G.P., additional, Viana, A., additional, Vigorito, C.F., additional, Vitale, V., additional, Vorobiov, S., additional, Vovk, I., additional, Vuillaume, T., additional, Wagner, S.J., additional, Walter, R., additional, Watson, J., additional, White, M., additional, White, R., additional, Wiemann, R., additional, Wierzcholska, A., additional, Will, M., additional, Williams, D.A., additional, Wischnewski, R., additional, Wolter, A., additional, Yamazaki, R., additional, Yanagita, S., additional, Yang, L., additional, Yoshikoshi, T., additional, Zacharias, M., additional, Zaharijas, G., additional, Zaric, D., additional, Zavrtanik, M., additional, Zavrtanik, D., additional, Zdziarski, A.A., additional, Zech, A., additional, Zechlin, H., additional, Zhdanov, V.I., additional, and Živec, M., additional

Published
2021
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12. Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre

Author

Acharyya, A., primary, Adam, R., additional, Adams, C., additional, Agudo, I., additional, Aguirre-Santaella, A., additional, Alfaro, R., additional, Alfaro, J., additional, Alispach, C., additional, Aloisio, R., additional, Batista, R. Alves, additional, Amati, L., additional, Ambrosi, G., additional, Angüner, E.O., additional, Antonelli, L.A., additional, Aramo, C., additional, Araudo, A., additional, Armstrong, T., additional, Arqueros, F., additional, Asano, K., additional, Ascasíbar, Y., additional, Ashley, M., additional, Balazs, C., additional, Ballester, O., additional, Larriva, A. Baquero, additional, Martins, V. Barbosa, additional, Barkov, M., additional, de Almeida, U. Barres, additional, Barrio, J.A., additional, Bastieri, D., additional, Becerra, J., additional, Beck, G., additional, Tjus, J. Becker, additional, Benbow, W., additional, Benito, M., additional, Berge, D., additional, Bernardini, E., additional, Bernlöhr, K., additional, Berti, A., additional, Bertucci, B., additional, Beshley, V., additional, Biasuzzi, B., additional, Biland, A., additional, Bissaldi, E., additional, Biteau, J., additional, Blanch, O., additional, Blazek, J., additional, Bocchino, F., additional, Boisson, C., additional, Arbeletche, L. Bonneau, additional, Bordas, P., additional, Bosnjak, Z., additional, Bottacini, E., additional, Bozhilov, V., additional, Bregeon, J., additional, Brill, A., additional, Bringmann, T., additional, Brown, A.M., additional, Brun, P., additional, Brun, F., additional, Bruno, P., additional, Bulgarelli, A., additional, Burton, M., additional, Burtovoi, A., additional, Buscemi, M., additional, Cameron, R., additional, Capasso, M., additional, Caproni, A., additional, Capuzzo-Dolcetta, R., additional, Caraveo, P., additional, Carosi, R., additional, Carosi, A., additional, Casanova, S., additional, Cascone, E., additional, Cassol, F., additional, Catalani, F., additional, Cauz, D., additional, Cerruti, M., additional, Chadwick, P., additional, Chaty, S., additional, Chen, A., additional, Chernyakova, M., additional, Chiaro, G., additional, Chiavassa, A., additional, Chikawa, M., additional, Chudoba, J., additional, Çolak, M., additional, Conforti, V., additional, Coniglione, R., additional, Conte, F., additional, Contreras, J.L., additional, Coronado-Blazquez, J., additional, Costa, A., additional, Costantini, H., additional, Cotter, G., additional, Cristofari, P., additional, D'A𝚤, A., additional, D'Ammando, F., additional, Damone, L.A., additional, Daniel, M.K., additional, Dazzi, F., additional, Angelis, A. De, additional, Caprio, V. De, additional, Anjos, R. de Cássia dos, additional, Pino, E.M. de Gouveia Dal, additional, Lotto, B. De, additional, Martino, D. De, additional, Wilhelmi, E. de Oña, additional, Palma, F. De, additional, de Souza, V., additional, Delgado, C., additional, Giler, A.G. Delgado, additional, Volpe, D. della, additional, Depaoli, D., additional, Girolamo, T. Di, additional, Pierro, F. Di, additional, Venere, L. Di, additional, Diebold, S., additional, Dmytriiev, A., additional, Domínguez, A., additional, Donini, A., additional, Doro, M., additional, Ebr, J., additional, Eckner, C., additional, Edwards, T. D. P., additional, Ekoume, T.R.N., additional, Elsässer, D., additional, Evoli, C., additional, Falceta-Goncalves, D., additional, Fedorova, E., additional, Fegan, S., additional, Feng, Q., additional, Ferrand, G., additional, Ferrara, G., additional, Fiandrini, E., additional, Fiasson, A., additional, Filipovic, M., additional, Fioretti, V., additional, Fiori, M., additional, Foffano, L., additional, Fontaine, G., additional, Fornieri, O., additional, Franco, F.J., additional, Fukami, S., additional, Fukui, Y., additional, Gaggero, D., additional, Galaz, G., additional, Gammaldi, V., additional, Garcia, E., additional, Garczarczyk, M., additional, Gascon, D., additional, Gent, A., additional, Ghalumyan, A., additional, Gianotti, F., additional, Giarrusso, M., additional, Giavitto, G., additional, Giglietto, N., additional, Giordano, F., additional, Giuliani, A., additional, Glicenstein, J., additional, Gnatyk, R., additional, Goldoni, P., additional, González, M.M., additional, Gourgouliatos, K., additional, Granot, J., additional, Grasso, D., additional, Green, J., additional, Grillo, A., additional, Gueta, O., additional, Gunji, S., additional, Halim, A., additional, Hassan, T., additional, Heller, M., additional, Cadena, S. Hernández, additional, Hiroshima, N., additional, Hnatyk, B., additional, Hofmann, W., additional, Holder, J., additional, Horan, D., additional, Hörandel, J., additional, Horvath, P., additional, Hovatta, T., additional, Hrabovsky, M., additional, Hrupec, D., additional, Hughes, G., additional, Humensky, T.B., additional, Hütten, M., additional, Iarlori, M., additional, Inada, T., additional, Inoue, S., additional, Iocco, F., additional, Iori, M., additional, Jamrozy, M., additional, Janecek, P., additional, Jin, W., additional, Jouvin, L., additional, Jurysek, J., additional, Karukes, E., additional, Katarzyński, K., additional, Kazanas, D., additional, Kerszberg, D., additional, Kherlakian, M.C., additional, Kissmann, R., additional, Knödlseder, J., additional, Kobayashi, Y., additional, Kohri, K., additional, Komin, N., additional, Kubo, H., additional, Kushida, J., additional, Lamanna, G., additional, Lapington, J., additional, Laporte, P., additional, de Oliveira, M.A. Leigui, additional, Lenain, J., additional, Leone, F., additional, Leto, G., additional, Lindfors, E., additional, Lohse, T., additional, Lombardi, S., additional, Longo, F., additional, Lopez, A., additional, López, M., additional, López-Coto, R., additional, Loporchio, S., additional, Luque-Escamilla, P.L., additional, Mach, E., additional, Maggio, C., additional, Maier, G., additional, Mallamaci, M., additional, de Almeida, R. Malta Nunes, additional, Mandat, D., additional, Manganaro, M., additional, Mangano, S., additional, Manicò, G., additional, Marculewicz, M., additional, Mariotti, M., additional, Markoff, S., additional, Marquez, P., additional, Martí, J., additional, Martinez, O., additional, Martínez, M., additional, Martínez, G., additional, Martínez-Huerta, H., additional, Maurin, G., additional, Mazin, D., additional, Mbarubucyeye, J.D., additional, Miranda, D. Medina, additional, Meyer, M., additional, Miceli, M., additional, Miener, T., additional, Minev, M., additional, Miranda, J.M., additional, Mirzoyan, R., additional, Mizuno, T., additional, Mode, B., additional, Moderski, R., additional, Mohrmann, L., additional, Molina, E., additional, Montaruli, T., additional, Moralejo, A., additional, Morcuende-Parrilla, D., additional, Morselli, A., additional, Mukherjee, R., additional, Mundell, C., additional, Nagai, A., additional, Nakamori, T., additional, Nemmen, R., additional, Niemiec, J., additional, Nieto, D., additional, Nikołajuk, M., additional, Ninci, D., additional, Noda, K., additional, Nosek, D., additional, Nozaki, S., additional, Ohira, Y., additional, Ohishi, M., additional, Ohtani, Y., additional, Oka, T., additional, Okumura, A., additional, Ong, R.A., additional, Orienti, M., additional, Orito, R., additional, Orlandini, M., additional, Orlando, S., additional, Orlando, E., additional, Ostrowski, M., additional, Oya, I., additional, Pagano, I., additional, Pagliaro, A., additional, Palatiello, M., additional, Pantaleo, F.R., additional, Paredes, J.M., additional, Pareschi, G., additional, Parmiggiani, N., additional, Patricelli, B., additional, Pavletić, L., additional, Pe'er, A., additional, Pecimotika, M., additional, Pérez-Romero, J., additional, Persic, M., additional, Petruk, O., additional, Pfrang, K., additional, Piano, G., additional, Piatteli, P., additional, Pietropaolo, E., additional, Pillera, R., additional, Pilszyk, B., additional, Pintore, F., additional, Pohl, M., additional, Poireau, V., additional, Prado, R.R., additional, Prandini, E., additional, Prast, J., additional, Principe, G., additional, Prokoph, H., additional, Prouza, M., additional, Przybilski, H., additional, Pühlhofer, G., additional, Pumo, M.L., additional, Queiroz, F., additional, Quirrenbach, A., additional, Rainò, S., additional, Rando, R., additional, Razzaque, S., additional, Recchia, S., additional, Reimer, O., additional, Reisenegger, A., additional, Renier, Y., additional, Rhode, W., additional, Ribeiro, D., additional, Ribó, M., additional, Richtler, T., additional, Rico, J., additional, Rieger, F., additional, Rinchiuso, L., additional, Rizi, V., additional, Rodriguez, J., additional, Fernandez, G. Rodriguez, additional, Ramirez, J.C. Rodriguez, additional, Rojas, G., additional, Romano, P., additional, Romeo, G., additional, Rosado, J., additional, Rowell, G., additional, Rudak, B., additional, Russo, F., additional, Sadeh, I., additional, Sæther Hatlen, E., additional, Safi-Harb, S., additional, Greus, F. Salesa, additional, Salina, G., additional, Sanchez, D., additional, Sánchez-Conde, M., additional, Sangiorgi, P., additional, Sano, H., additional, Santander, M., additional, Santos, E.M., additional, Santos-Lima, R., additional, Sanuy, A., additional, Sarkar, S., additional, Saturni, F.G., additional, Sawangwit, U., additional, Schussler, F., additional, Schwanke, U., additional, Sciacca, E., additional, Scuderi, S., additional, Seglar-Arroyo, M., additional, Sergijenko, O., additional, Servillat, M., additional, Seweryn, K., additional, Shalchi, A., additional, Sharma, P., additional, Shellard, R.C., additional, Siejkowski, H., additional, Silk, J., additional, Siqueira, C., additional, Sliusar, V., additional, Słowikowska, A., additional, Sokolenko, A., additional, Sol, H., additional, Spencer, S., additional, Stamerra, A., additional, Stanič, S., additional, Starling, R., additional, Stolarczyk, T., additional, Straumann, U., additional, Strišković, J., additional, Suda, Y., additional, Suomijarvi, T., additional, Świerk, P., additional, Tavecchio, F., additional, Taylor, L., additional, Tejedor, L.A., additional, Teshima, M., additional, Testa, V., additional, Tibaldo, L., additional, Peixoto, C.J. Todero, additional, Tokanai, F., additional, Tonev, D., additional, Tosti, G., additional, Tosti, L., additional, Tothill, N., additional, Truzzi, S., additional, Travnicek, P., additional, Vagelli, V., additional, Vallage, B., additional, Vallania, P., additional, Eldik, C. van, additional, Vandenbroucke, J., additional, Varner, G.S., additional, Vassiliev, V., additional, Acosta, M. Vázquez, additional, Vecchi, M., additional, Ventura, S., additional, Vercellone, S., additional, Vergani, S., additional, Verna, G., additional, Viana, A., additional, Vigorito, C.F., additional, Vink, J., additional, Vitale, V., additional, Vorobiov, S., additional, Vovk, I., additional, Vuillaume, T., additional, Wagner, S.J., additional, Walter, R., additional, Watson, J., additional, Weniger, C., additional, White, R., additional, White, M., additional, Wiemann, R., additional, Wierzcholska, A., additional, Will, M., additional, Williams, D.A., additional, Wischnewski, R., additional, Yanagita, S., additional, Yang, L., additional, Yoshikoshi, T., additional, Zacharias, M., additional, Zaharijas, G., additional, Zakaria, A.A., additional, Zampieri, L., additional, Zanin, R., additional, Zaric, D., additional, Zavrtanik, M., additional, Zavrtanik, D., additional, Zdziarski, A.A., additional, Zech, A., additional, Zechlin, H., additional, Zhdanov, V.I., additional, and Živec, M., additional

Published
2021
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15. AGILE and Konus-Wind Observations of GRB 190114C: The Remarkable Prompt and Early Afterglow Phases.

Author

Ursi, A., Tavani, M., Frederiks, D. D., Romani, M., Verrecchia, F., Marisaldi, M., Aptekar, R. L., Antonelli, L. A., Argan, A., Bulgarelli, A., Barbiellini, G., Caraveo, P., Cardillo, M., Casentini, C., Cattaneo, P. W., Chen, A., Costa, E., Donnarumma, I., Evangelista, Y., and Feroci, M.

Subjects
INVERSE Compton scattering, GAMMA ray bursts, HARD X-rays, RADIATION, PHYSICS, FLUX (Energy)
Abstract

GRB 190114C represents a breakthrough for the physics of gamma-ray bursts (GRBs), being the first GRB with delayed emission above 300 GeV, as reported by MAGIC. We present in this paper the sub-MeV/MeV data of the prompt and early afterglow emissions of GRB 190114C, as detected by AGILE and Konus-Wind, in the 20 keV–100 MeV energy range. The first stages of the burst exhibit multiple emission components, associated with an interesting spectral evolution. The first 2 s of the prompt emission can be described by a single "Band-like" spectral component. The successive 4 s show the presence of an additional high-energy spectral component, which quickly evolves into a "hard-flat" component of the νFν spectrum, extending up to 10–100 MeV and likely produced by inverse Compton radiation, whose onset and evolution are clearly shown in our data. After this phase, the νFν spectrum evolves into a "V shape," showing the persistence and spectral hardening of the additional high-energy component in substantial agreement with Fermi and Swift results. We also analyze the first ∼200 s of the early afterglow that show a reflaring episode near T0 + 15 s. We identify a new, so-far-unnoticed flux temporal break near T0 + 100 s, which is detected in hard X-rays by both Konus-Wind and INTEGRAL/SPI-ACS. We find this break incompatible with the commonly assumed adiabatic evolution of a fireball in a constant-density medium. We interpret this break as a consequence of radiative evolution of the early afterglow from a fireball expanding in a wind-like circumburst medium. [ABSTRACT FROM AUTHOR]

Published
2020
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17. Erratum: 'multi-wavelength observations of the flaring gamma-ray blazar 3c 66a in 2008 october' (2011, apj, 726, 43)

Author

Luca Baldini, Reshmi Mukherjee, Carla Buemi, I. de la Calle Perez, A. Varlotta, Wystan Benbow, Mn Mazziotta, Jamie Holder, J. P. Norris, A. Morselli, A. D. Falcone, V. Vitale, Henric Krawczynski, T. A. Porter, Takaaki Tanaka, J. Bregeon, P. Kaaret, Stefano Ciprini, David Sanchez, A. Bouvier, Keith Bechtol, J. M. Lopez, Stephen Fegan, P. D. Smith, J. Grube, A. Cannon, R. Turchetti, Manel Errando, Sang Hun Lee, Igor V. Moskalenko, D. Dumora, J. Mehault, T. Aune, J. Lande, J. E. Ward, F. Gargano, D. Pandel, T. Glanzman, P. Calcidese, S. M. Bradbury, A. Berduygin, Marco Ajello, Jun Kataoka, Olaf Reimer, Paul J. Wang, Mauro Dolci, T. Ylinen, D. Capezzali, Vladimir A. Hagen-Thorn, Seth Digel, H. Y. Hsiao, S. Buson, H. F.W. Sadrozinski, V. Bugaev, R. Bellazzini, V. A. Acciari, S. P. Swordy, J. Saino, G. Tešić, Steven Ritz, F. Piron, D. Parent, Vladimir Vassiliev, Luca Latronico, Julie McEnery, Benoit Lott, Anne Lähteenmäki, A. S. Johnson, S. Cutini, A. Konopelko, Joachim Ripken, Ekaterina Koptelova, Brian L Winer, Martin Pohl, Kari Nilsson, G. Tosti, P. L. Nolan, N. Gehrels, Uwe Bach, Corrado Trigilio, Wen Ping Chen, J. M. Casandjian, Geza Gyuk, S. Rainò, K. Ragan, A. McCann, Roger W. Romani, P. Moriarty, Gernot Maier, Karen Byrum, A. Chekhtman, Michele Fumagalli, D. Boltuch, Talvikki Hovatta, A. N. Otte, D. J. Suson, G. H. Sembroski, A. A. Moiseev, M. Pepe, M. G. Nikolashvili, A. Sievers, Ivan Agudo, D. Carosati, Deborah Dultzin, R. Dickherber, C. M. Raiteri, S. P. Wakely, D. Riquelme, Daniel Gall, Cullen H. Blake, M. Schroedter, R. A. Ong, B. Berenji, S. McArthur, Raúl Mújica, M. Razzano, T. L. Usher, Ryosuke Itoh, M. J. Lang, C. C. Cheung, M. Sorcia, D. da Rio, David S. Davis, G.L. Godfrey, J. F. Ormes, E. Do Couto E Silva, Lars Fuhrmann, E. Cavazzuti, Mark Gurwell, G. Umana, P. Spinelli, L. O. Takalo, Francesco Longo, Mar Roca-Sogorb, Claudia Cecchi, Hugh D. Aller, Atsushi Okumura, S. Thibadeau, Richard Dubois, L. A. Sigua, Elina Lindfors, J. S. Perkins, Melissa Pesce-Rollins, Markus Böttcher, A. C. Sadun, N. Karlsson, G. H. Gillanders, S. Godambe, David Hiriart, L. Ciupik, J. H. Panetta, C. Diltz, Merja Tornikoski, Tyrel J. Johnson, Tsunefumi Mizuno, Jason X. Prochaska, R. A. Cameron, Omer Celik, C. M. Hui, F. Loparco, W. N. Johnson, Charles D. Dermer, N. Galante, Diego F. Torres, E. Forné, S. LeBohec, Lucy Fortson, C. Monte, Rumen Bachev, Matthew Wood, M. Pasanen, M. McCutcheon, E. Charles, Jochen Heidt, S. Carrigan, Amy Furniss, P. Bruel, A. Tramacere, G. Demet Senturk, F. de Palma, H. Ungerechts, Stephan Wagner, G. Finnegan, A. W. Smith, Stefan Funk, O. M. Kurtanidze, M. Ziegler, José L. Gómez, Gloria Spandre, J. G. Thayer, A. Halkola, D. Hadasch, James Chiang, A. Sander, M. F. Aller, J. E. Grove, P. Roustazadeh, D. Horan, Roger Blandford, Zhenwei Yang, P. T. Reynolds, Hideaki Katagiri, E. Roache, Carmelo Sgrò, Riccardo Rando, Gianpiero Tagliaferri, E. Hays, David Kieda, Yasushi Fukazawa, David A. Williams, Amanda Weinstein, N. Vilchez, R. Guenette, Hiromitsu Takahashi, J. H. Buckley, M. Kertzman, R. Ligustri, Markus Ackermann, E. Nuss, M. S. Shaw, David Paneque, E. Aliu, P. Fortin, H. J. Rose, T. Kamae, M. Roth, M. Kuss, Erika Benítez, Emmanouil Angelakis, Jürgen Knödlseder, A. W. Borgland, Nicola Omodei, P. Fusco, F. Krennrich, Valeri M. Larionov, P. Lubrano, M. Hayashida, A. A. Abdo, E. Orlando, N. Palma, J. Ballet, A. Cesarini, D. Starr, Tatiana S. Konstantinova, G. N. Kimeridze, M. Theiling, I. Nestoras, S. Vincent, J. Dashti, Josh Bloom, Jan Conrad, S. Germani, R. Buehler, R. E. Hughes, F. Giordano, Alan P. Marscher, J. P. Finley, John L. Quinn, Luis C. Reyes, Peter F. Michelson, Marcello Giroletti, Emanuele Bonamente, A. Reimer, A. Pichel, P. Giommi, J. A. Ros, D. Steele, M. Ozaki, T. C. Weekes, D. J. Thompson, M. Hauser, Johann Cohen-Tanugi, R. Claus, A. Sillanää, M. S. Strickman, P. Beltrame, Tomaso Belloni, G. A. Caliandro, L. Guillemot, A. A. Arkharov, M. Naumann-Godo, A. P. Waite, Jeffrey D. Scargle, Marco Frailis, K. S. Wood, V. Vasileiou, D. Gasparrini, T. Ohsugi, Paolo Leto, M. Brigida, A. Brez, A. Di Paola, V. Pelassa, Nicola Giglietto, I. A. Grenier, D. S. Hanna, S. G. Jorstad, T. C. Arlen, A. Imran, L. Costamante, M. N. Lovellette, Stephanie Wissel, P. A. Caraveo, Persis S. Drell, Gudlaugur Johannesson, M. Villata, Michael Mommert, Justin Vandenbroucke, T. Weisgarber, Guido Barbiellini, Takeshi Nakamori, Thomas Brian Humensky, E. N. Kopatskaya, Matthias Beilicke, L. Tibaldo, Wei Cui, A. Makeev, M. E. Monzani, C. Favuzzi, Jodi Christiansen, J. B. Thayer, J. A. Zensus, S. Murgia, Denis Bastieri, and Sylvain Guiriec

Subjects
Physics, Space and Planetary Science, Gamma ray, Astronomy, Astronomy and Astrophysics, Multi wavelength, Astrophysics, Blazar
Published
2011

18. Constraints on cosmological dark matter annihilation from the Fermi-LAT isotropic diffuse gamma-ray measurement

Author

Abdo, A. A., Ackermann, M., Ajello, M., 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., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, Oe., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., de Angelis, A., de Palma, F., Digel, S. W., do Couto e Silva, E., Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grove, J. E., Guillemot, L., Guiriec, S., Gustafsson, M., Hadasch, D., Harding, A. K., Horan, D., Hughes, R. E., Johnson, A. S., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knoedlseder, J., Kuss, M., Lande, J., Latronico, L., Garde, M. Llena, Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Makeev, A., Mazziotta, M. N., McEnery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Raino, S., Rando, R., Reimer, A., Reimer, O., Reposeur, T., Rodriguez, A. Y., Roth, M., Sadrozinski, H. F. -W, Sander, A., Parkinson, P. M. Saz, Scargle, J. D., Sellerholm, A., Sgro, C., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. -L, Strickman, M. S., Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Torres, D. F., Uchiyama, Y., Usher, T. L., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Ylinen, Tomi, Zaharijas, G., Ziegler, M., Abdo, A. A., Ackermann, M., Ajello, M., 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., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, Oe., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., de Angelis, A., de Palma, F., Digel, S. W., do Couto e Silva, E., Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grove, J. E., Guillemot, L., Guiriec, S., Gustafsson, M., Hadasch, D., Harding, A. K., Horan, D., Hughes, R. E., Johnson, A. S., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knoedlseder, J., Kuss, M., Lande, J., Latronico, L., Garde, M. Llena, Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Makeev, A., Mazziotta, M. N., McEnery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Raino, S., Rando, R., Reimer, A., Reimer, O., Reposeur, T., Rodriguez, A. Y., Roth, M., Sadrozinski, H. F. -W, Sander, A., Parkinson, P. M. Saz, Scargle, J. D., Sellerholm, A., Sgro, C., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. -L, Strickman, M. S., Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Torres, D. F., Uchiyama, Y., Usher, T. L., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Ylinen, Tomi, Zaharijas, G., and Ziegler, M.

Abstract

The first published Fermi large area telescope (Fermi-LAT) measurement of the isotropic diffuse gamma-ray emission is in good agreement with a single power law, and is not showing any signature of a dominant contribution from dark matter sources in the energy range from 20 to 100 GeV. We use the absolute size and spectral shape of this measured flux to derive cross section limits on three types of generic dark matter candidates: annihilating into quarks, charged leptons and monochromatic photons. Predicted gamma-ray fluxes from annihilating dark matter are strongly affected by the underlying distribution of dark matter, and by using different available results of matter structure formation we assess these uncertainties. We also quantify how the dark matter constraints depend on the assumed conventional backgrounds and on the Universe's transparency to high-energy gamma-rays. In reasonable background and dark matter structure scenarios (but not in all scenarios we consider) it is possible to exclude models proposed to explain the excess of electrons and positrons measured by the Fermi-LAT and PAMELA experiments. Derived limits also start to probe cross sections expected from thermally produced relics (e. g. in minimal supersymmetry models) annihilating predominantly into quarks. For the monochromatic gamma-ray signature, the current measurement constrains only dark matter scenarios with very strong signals., QC 20110112. QC 20211018.

Published
2010
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19. Limits on large extra dimensions based on observations of neutron stars with the Fermi-LAT

Author

collaboration, Fermi-LAT, primary, Ajello, M, additional, Baldini, L, additional, Barbiellini, G, additional, Bastieri, D, additional, Bechtol, K, additional, Bellazzini, R, additional, Berenji, B, additional, Bloom, E.D, additional, Bonamente, E, additional, Borgland, A.W, additional, Bregeon, J, additional, Brigida, M, additional, Bruel, P, additional, Buehler, R, additional, Buson, S, additional, Caliandro, G.A, additional, Cameron, R.A, additional, Caraveo, P.A, additional, Casandjian, J.M, additional, Cecchi, C, additional, Charles, E, additional, Chekhtman, A, additional, Chiang, J, additional, Ciprini, S, additional, Claus, R, additional, Cohen-Tanugi, J, additional, Conrad, J, additional, Cutini, S, additional, Angelis, A. de, additional, Palma, F. de, additional, Dermer, C.D, additional, Silva, E. do Couto e, additional, Drell, P.S, additional, Drlica-Wagner, A, additional, Enoto, T, additional, Favuzzi, C, additional, Fegan, S.J, additional, Ferrara, E.C, additional, Fukazawa, Y, additional, Fusco, P, additional, Gargano, F, additional, Gasparrini, D, additional, Germani, S, additional, Giglietto, N, additional, Giordano, F, additional, Giroletti, M, additional, Glanzman, T, additional, Godfrey, G, additional, Graham, P, additional, Grenier, I.A, additional, Guiriec, S, additional, Gustafsson, M, additional, Hadasch, D, additional, Hayashida, M, additional, Hughes, R.E, additional, Johnson, A.S, additional, Kamae, T, additional, Katagiri, H, additional, Kataoka, J, additional, Knödlseder, J, additional, Kuss, M, additional, Lande, J, additional, Latronico, L, additional, Lionetto, A.M, additional, Longo, F, additional, Loparco, F, additional, Lovellette, M.N, additional, Lubrano, P, additional, Mazziotta, M.N, additional, Michelson, P.F, additional, Mitthumsiri, W, additional, Mizuno, T, additional, Monte, C, additional, Monzani, M.E, additional, Morselli, A, additional, Moskalenko, I.V, additional, Murgia, S, additional, Norris, J.P, additional, Nuss, E, additional, Ohsugi, T, additional, Okumura, A, additional, Orlando, E, additional, Ormes, J.F, additional, Ozaki, M, additional, Paneque, D, additional, Pesce-Rollins, M, additional, Pierbattista, M, additional, Piron, F, additional, Pivato, G, additional, Rainò, S, additional, Razzano, M, additional, Ritz, S, additional, Roth, M, additional, Parkinson, P.M. Saz, additional, Scargle, J.D, additional, Schalk, T.L, additional, Sgrò, C, additional, Siskind, E.J, additional, Spandre, G, additional, Spinelli, P, additional, Suson, D.J, additional, Tajima, H, additional, Takahashi, H, additional, Tanaka, T, additional, Thayer, J.G, additional, Thayer, J.B, additional, Tibaldo, L, additional, Tinivella, M, additional, Torres, D.F, additional, Troja, E, additional, Uchiyama, Y, additional, Usher, T.L, additional, Vandenbroucke, J, additional, Vasileiou, V, additional, Vianello, G, additional, Vitale, V, additional, Waite, A.P, additional, Winer, B.L, additional, Wood, K.S, additional, Wood, M, additional, Yang, Z, additional, and Zimmer, S, additional

Published
2012
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20. Constraints on dark matter annihilation in clusters of galaxies with the Fermi large area telescope

Author

Ackermann, M, primary, Ajello, M, additional, Allafort, A, additional, Baldini, L, additional, Ballet, J, additional, Barbiellini, G, additional, Bastieri, D, additional, Bechtol, K, additional, Bellazzini, R, additional, Blandford, R.D, additional, Bloom, E.D, additional, Bonamente, E, additional, Borgland, A.W, additional, Bouvier, A, additional, Brandt, T.J, additional, Bregeon, J, additional, Brigida, M, additional, Bruel, P, additional, Buehler, R, additional, Buson, S, additional, Caliandro, G.A, additional, Cameron, R.A, additional, Caraveo, P.A, additional, Carrigan, S, additional, Casandjian, J.M, additional, Cecchi, C, additional, Charles, E, additional, Chekhtman, A, additional, Cheung, C.C, additional, Chiang, J, additional, Ciprini, S, additional, Claus, R, additional, Cohen-Tanugi, J, additional, Cominsky, L.R, additional, Conrad, J, additional, Angelis, A. de, additional, Palma, F. de, additional, Silva, E. do Couto e, additional, Drell, P.S, additional, Drlica-Wagner, A, additional, Dubois, R, additional, Dumora, D, additional, Edmonds, Y, additional, Farnier, C, additional, Favuzzi, C, additional, Fegan, S.J, additional, Frailis, M, additional, Fukazawa, Y, additional, Fusco, P, additional, Gargano, F, additional, Gasparrini, D, additional, Gehrels, N, additional, Germani, S, additional, Giglietto, N, additional, Giordano, F, additional, Glanzman, T, additional, Godfrey, G, additional, Grenier, I.A, additional, Guiriec, S, additional, Gustafsson, M, additional, Harding, A.K, additional, Hayashida, M, additional, Horan, D, additional, Hughes, R.E, additional, Jeltema, T.E, additional, Jóhannesson, G, additional, Johnson, A S, additional, Johnson, W.N, additional, Kamae, T, additional, Katagiri, H, additional, Kataoka, J, additional, Knödlseder, J, additional, Kuss, M, additional, Lande, J, additional, Latronico, L, additional, Lee, S.-H, additional, Garde, M. Llena, additional, Longo, F, additional, Loparco, F, additional, Lovellette, M.N, additional, Lubrano, P, additional, Madejski, G.M, additional, Makeev, A, additional, Mazziotta, M.N, additional, Michelson, P.F, additional, Mitthumsiri, W, additional, Mizuno, T, additional, Moiseev, A.A, additional, Monte, C, additional, Monzani, M.E, additional, Morselli, A, additional, Moskalenko, I.V, additional, Murgia, S, additional, Nolan, P.L, additional, Norris, J.P, additional, Nuss, E, additional, Ohno, M, additional, Ohsugi, T, additional, Omodei, N, additional, Orlando, E, additional, Ormes, J.F, additional, Panetta, J.H, additional, Pepe, M, additional, Pesce-Rollins, M, additional, Piron, F, additional, Porter, T.A, additional, Profumo, S, additional, Rainò, S, additional, Razzano, M, additional, Reposeur, T, additional, Ritz, S, additional, Rodriguez, A.Y, additional, Roth, M, additional, Sadrozinski, H.F.-W, additional, Sander, A, additional, Scargle, J.D, additional, Sgrò, C, additional, Siskind, E.J, additional, Smith, P.D, additional, Spandre, G, additional, Spinelli, P, additional, Starck, J.-L, additional, Strickman, M.S, additional, Suson, D.J, additional, Takahashi, H, additional, Tanaka, T, additional, Thayer, J.B, additional, Thayer, J.G, additional, Tibaldo, L, additional, Torres, D.F, additional, Tosti, G, additional, Usher, T.L, additional, Vasileiou, V, additional, Vitale, V, additional, Waite, A.P, additional, Wang, P, additional, Winer, B.L, additional, Wood, K.S, additional, Yang, Z, additional, Ylinen, T, additional, and Ziegler, M, additional

Published
2010
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21. Constraints on cosmological dark matter annihilation from the Fermi-LAT isotropic diffuse gamma-ray measurement

Author

Abdo, A.A, primary, Ackermann, M, additional, Ajello, M, additional, Baldini, L, additional, Ballet, J, additional, Barbiellini, G, additional, Bastieri, D, additional, Bechtol, K, additional, Bellazzini, R, additional, Berenji, B, additional, Blandford, R.D, additional, Bloom, E.D, additional, Bonamente, E, additional, Borgland, A.W, additional, Bouvier, A, additional, Bregeon, J, additional, Brez, A, additional, Brigida, M, additional, Bruel, P, additional, Burnett, T.H, additional, Buson, S, additional, Caliandro, G.A, additional, Cameron, R.A, additional, Caraveo, P.A, additional, Carrigan, S, additional, Casandjian, J.M, additional, Cecchi, C, additional, Çelik, Ö, additional, Chekhtman, A, additional, Cheung, C.C, additional, Chiang, J, additional, Ciprini, S, additional, Claus, R, additional, Cohen-Tanugi, J, additional, Conrad, J, additional, Cutini, S, additional, Dermer, C.D, additional, Angelis, A. de, additional, Palma, F. de, additional, Digel, S.W, additional, Silva, E. do Couto e, additional, Drell, P.S, additional, Dubois, R, additional, Dumora, D, additional, Edmonds, Y, additional, Farnier, C, additional, Favuzzi, C, additional, Fegan, S.J, additional, Focke, W.B, additional, Fortin, P, additional, Frailis, M, additional, Fukazawa, Y, additional, Fusco, P, additional, Gargano, F, additional, Gasparrini, D, additional, Gehrels, N, additional, Germani, S, additional, Giglietto, N, additional, Giordano, F, additional, Glanzman, T, additional, Godfrey, G, additional, Grove, J.E, additional, Guillemot, L, additional, Guiriec, S, additional, Gustafsson, M, additional, Hadasch, D, additional, Harding, A.K, additional, Horan, D, additional, Hughes, R.E, additional, Johnson, A.S, additional, Johnson, W.N, additional, Kamae, T, additional, Katagiri, H, additional, Kataoka, J, additional, Kawai, N, additional, Kerr, M, additional, Knödlseder, J, additional, Kuss, M, additional, Lande, J, additional, Latronico, L, additional, Garde, M. Llena, additional, Longo, F, additional, Loparco, F, additional, Lott, B, additional, Lovellette, M.N, additional, Lubrano, P, additional, Makeev, A, additional, Mazziotta, M.N, additional, McEnery, J.E, additional, Meurer, C, additional, Michelson, P.F, additional, Mitthumsiri, W, additional, Mizuno, T, additional, Monte, C, additional, Monzani, M.E, additional, Morselli, A, additional, Moskalenko, I.V, additional, Murgia, S, additional, Nolan, P.L, additional, Norris, J.P, additional, Nuss, E, additional, Ohsugi, T, additional, Omodei, N, additional, Orlando, E, additional, Ormes, J.F, additional, Paneque, D, additional, Panetta, J.H, additional, Parent, D, additional, Pelassa, V, additional, Pepe, M, additional, Pesce-Rollins, M, additional, Piron, F, additional, Rainò, S, additional, Rando, R, additional, Reimer, A, additional, Reimer, O, additional, Reposeur, T, additional, Rodriguez, A.Y, additional, Roth, M, additional, Sadrozinski, H.F.-W, additional, Sander, A, additional, Parkinson, P.M. Saz, additional, Scargle, J.D, additional, Sellerholm, A, additional, Sgrò, C, additional, Siskind, E.J, additional, Smith, P.D, additional, Spandre, G, additional, Spinelli, P, additional, Starck, J.-L, additional, Strickman, M.S, additional, Suson, D.J, additional, Takahashi, H, additional, Tanaka, T, additional, Thayer, J.B, additional, Thayer, J.G, additional, Torres, D.F, additional, Uchiyama, Y, additional, Usher, T.L, additional, Vasileiou, V, additional, Vilchez, N, additional, Vitale, V, additional, Waite, A.P, additional, Wang, P, additional, Winer, B.L, additional, Wood, K.S, additional, Ylinen, T, additional, Zaharijas, G, additional, and Ziegler, M, additional

Published
2010
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22. MULTIFREQUENCY STUDIES OF THE PECULIAR QUASAR 4C +21.35 DURING THE 2010 FLARING ACTIVITY.

Author

Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Bonamente, E., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cavazzuti, E., Cecchi, C., and Chaves, R. C. G.

Subjects
QUASARS, X-ray astronomy, GAMMA ray astronomy, SPECTRAL energy distribution, KERR black holes
Abstract

The discovery of rapidly variable Very High Energy (VHE; E > 100 GeV) γ-ray emission from 4C +21.35 (PKS 1222+216) by MAGIC on 2010 June 17, triggered by the high activity detected by the Fermi Large Area Telescope (LAT) in high energy (HE; E > 100 MeV) γ-rays, poses intriguing questions on the location of the γ-ray emitting region in this flat spectrum radio quasar. We present multifrequency data of 4C +21.35 collected from centimeter to VHE during 2010 to investigate the properties of this source and discuss a possible emission model. The first hint of detection at VHE was observed by MAGIC on 2010 May 3, soon after a γ-ray flare detected by Fermi-LAT that peaked on April 29. The same emission mechanism may therefore be responsible for both the HE and VHE emission during the 2010 flaring episodes. Two optical peaks were detected on 2010 April 20 and June 30, close in time but not simultaneous with the two γ-ray peaks, while no clear connection was observed between the X-ray and γ-ray emission. An increasing flux density was observed in radio and mm bands from the beginning of 2009, in accordance with the increasing γ-ray activity observed by Fermi-LAT, and peaking on 2011 January 27 in the mm regime (230 GHz). We model the spectral energy distributions (SEDs) of 4C +21.35 for the two periods of the VHE detection and a quiescent state, using a one-zone model with the emission coming from a very compact region outside the broad line region. The three SEDs can be fit with a combination of synchrotron self-Compton and external Compton emission of seed photons from a dust torus, changing only the electron distribution parameters between the epochs. The fit of the optical/UV part of the spectrum for 2010 April 29 seems to favor an inner disk radius of

Published
2014
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23. Fermi LARGE AREA TELESCOPE OBSERVATIONS OF BLAZAR 3C 279 OCCULTATIONS BY THE SUN.

Author

Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Blandford, R. D., Borgland, A. W., Bregeon, J., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Chaves, R. C. G., Chekhtman, A., Cheung, C. C., Chiang, J., and Ciprini, S.

Subjects
OCCULTATIONS (Astronomy), HALOS (Meteorology), GALACTIC halos, DARK matter, FERMI Gamma-ray Space Telescope (Spacecraft)
Abstract

Observations of occultations of bright γ-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles—axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of ≈3σ, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar γ-ray emission at a 3σ confidence level. [ABSTRACT FROM AUTHOR]

Published
2014
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24. The SPI Spectrometer for the Integral Mission

Author

Vedrenne, G, primary, Jean, P, additional, Kandel, B, additional, Albernhe, F, additional, Borrel, V, additional, Mandrou, P, additional, Roques, J P, additional, Ballmoos, P von, additional, Durouchoux, Ph, additional, Cordier, B, additional, Diallo, N, additional, Schönfelder, V, additional, Lichti, G G, additional, Diehl, R, additional, Varendorff, M, additional, Strong, A W, additional, Georgii, R, additional, Teegarden, B J, additional, Naya, J, additional, Seifert, H, additional, Sturner, S, additional, Matteson, J, additional, Lin, R, additional, Slassi, S, additional, Sanchez, F, additional, Caraveo, P, additional, Leleux, P, additional, Skinner, G K, additional, and Connell, P, additional

Published
1998
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27. DISCOVERY OF NINE GAMMA-RAY PULSARS IN FERMI LARGE AREA TELESCOPE DATA USING A NEW BLIND SEARCH METHOD.

Author

Pletsch, H. J., Guillemot, L., Allen, B., Kramer, M., Aulbert, C., Fehrmann, H., Ray, P. S., Barr, E. D., Belfiore, A., Camilo, F., Caraveo, P. A., Çelik, Ö., Champion, D. J., Dormody, M., Eatough, R. P., Ferrara, E. C., Freire, P. C. C., Hessels, J. W. T., Keith, M., and Kerr, M.

Subjects
PULSARS, TELESCOPES, GAMMA rays, GRAVITATIONAL waves, COSMIC magnetic fields, GRAVITY waves
Abstract

We report the discovery of nine previously unknown gamma-ray pulsars in a blind search of data from the Fermi Large Area Telescope (LAT). The pulsars were found with a novel hierarchical search method originally developed for detecting continuous gravitational waves from rapidly rotating neutron stars. Designed to find isolated pulsars spinning at up to kHz frequencies, the new method is computationally efficient and incorporates several advances, including a metric-based gridding of the search parameter space (frequency, frequency derivative, and sky location) and the use of photon probability weights. The nine pulsars have spin frequencies between 3 and 12 Hz, and characteristic ages ranging from 17 kyr to 3 Myr. Two of them, PSRs J1803-2149 and J2111+ 4606, are young and energetic Galactic-plane pulsars (spin-down power above 6 x 1035 erg s-1 and ages below 100 kyr). The seven remaining pulsars, PSRs J0106+4855, J0622+3749, J1620-4927, J1746-3239, J2028+3332, J2030+4415, and J2139+4716, are older and less energetic; two of them are located at higher Galactic latitudes (|b| > 10°). PSR J0106+4855 has the largest characteristic age (3 Myr) and the smallest surface magnetic field (2 x 1011 G) of all LAT blind-search pulsars. PSR J2139+4716 has the lowest spin-down power (3 x 1033 erg s-1) among all non-recycled gamma-ray pulsars ever found. Despite extensive multi-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars. [ABSTRACT FROM AUTHOR]

Published
2012
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28. DISCOVERY OF A FAINT X-RAY COUNTERPART AND A PARSEC-LONG X-RAY TAIL FOR THE MIDDLE-AGED, γ-RAY-ONLY PULSAR PSR J0357+3205.

Author

DE LUCA, A., MARELLI, M., MIGNANI, R. P., CARAVEO, P. A., HUMMEL, W., COLLINS, S., SHEARER, A., SAZ PARKINSON, P. M., BELFIORE, A., and BIGNAMI, U. F.

Subjects
X-rays, LARGE astronomical telescopes, WAVELENGTHS, NEBULAE, PULSARS, SOLAR energetic particles
Abstract

The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope opened a new era for pulsar astronomy, detecting y-ray pulsations from more than 60 pulsars, ~40% of which are not seen at radio wavelengths. One of the most interesting sources discovered by LAT is PSR J0357+3205, a radio-quiet, middle- aged (Τc ~ 0.5 Myr) pulsar standing out for its very low spin-down luminosity (Erot ~ 6 x 1033 erg s-1), indeed the lowest among non-recycled y-ray pulsars. A deep X-ray observation with Chandra (0.5-10 keV), coupled with sensitive optical/infrared ground-based images of the field, allowed us to identify PSR J0357+3205 as a faint source with a soft spectrum, consistent with a purely non-thermal emission (photon index F' = 2.53 ± 0.25). The absorbing column (NH = 8 ± 4 x 1020 cm-2) is consistent with a distance of a few hundred parsecs. Moreover, the Chandra data unveiled a huge (9 arcmin long) extended feature apparently protruding from the pulsar. Its non-thermal X-ray spectrum points to synchrotron emission from energetic particles from the pulsar wind, possibly similar to other elongated X-ray tails associated with rotation-powered pulsars and explained as bow-shock pulsar wind nebulae (PWNe). However, energetic arguments as well as the peculiar morphology of the diffuse feature associated with PSR J0357+3205 make the bow-shock PWN interpretation rather challenging. [ABSTRACT FROM AUTHOR]

Published
2011
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29. A MULTIWAVELENGTH STUDY ON THE HIGH-ENERGY BEHAVIOR OF THE FERMI/LAT PULSARS.

Author

MARELLI, MARTINO, DE LUCA, ANDREA, and CARAVEO, PATRIZIA A.

Subjects
PULSARS, X-ray astronomy, NEUTRON stars, GAMMA rays, X-ray spectroscopy
Abstract

Using archival as well as freshly acquired data, we assess the X-ray behavior of the Fermi/Large Area Telescope γ-ray pulsars listed in the First Fermi source catalog. After revisiting the relationships between the pulsars' rotational energy losses and their X-ray and γ-ray luminosities, we focus on the distance-independent γ-to-X-ray flux ratios. When plotting our Fγ/Fx values as a function of the pulsars' rotational energy losses, one immediately sees that pulsars with similar energetics have Fγ/Fx spanning three decades. Such spread, most probably stemming from vastly different geometrical configurations of the X-ray and γ-ray emitting regions, defies any straightforward interpretation of the plot. Indeed, while energetic pulsars do have low Fγ/Fx values, little can be said for the bulk of the Fermi neutron stars. Dividing our pulsar sample into radio-loud and radio-quiet subsamples, we find that, on average, radio-quiet pulsars do have higher values of Fγ /Fx, implying an intrinsic faintness of their X-ray emission and/or a different geometrical configuration. Moreover, despite the large spread mentioned above, statistical tests show a lower scatter in the radio-quiet data set with respect to the radio-loud one, pointing to a somewhat more constrained geometry for the radio-quiet objects with respect to the radio-loud ones. [ABSTRACT FROM AUTHOR]

Published
2011
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32. The Swift Gamma-Ray Burst Mission.

Author

Gehrels, N., Chincarini, G., Giommi, P., Mason, K. O., Nousek, J. A., Wells, A. A., White, N. E., Barthelmy, S. D., Burrows, D. N., Cominsky, L. R., Hurley, K. C., Marshall, F. E., Mészáros, P., Roming, P. W. A., Angelini, L., Barbier, L. M., Belloni, T., Campana, S., Caraveo, P. A., and Chester, M. M.

Published
2004
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37. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-energy Emission from Prompt to Afterglow.

Author

M. Ajello, M. Arimoto, M. Axelsson, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, A. Berretta, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, E. Burns, S. Buson, R. A. Cameron, R. Caputo, and P. A. Caraveo

Subjects
GAMMA ray bursts, SYNCHROTRON radiation, FERMI energy, OPTICAL telescopes, X-ray telescopes, SPACE telescopes, LIGHT curves
Abstract

We report on the observations of gamma-ray burst (GRB) 190114C by the Fermi Gamma-ray Space Telescope and the Neil Gehrels Swift Observatory. The prompt gamma-ray emission was detected by the Fermi GRB Monitor (GBM), the Fermi Large Area Telescope (LAT), and the Swift Burst Alert Telescope (BAT) and the long-lived afterglow emission was subsequently observed by the GBM, LAT, Swift X-ray Telescope (XRT), and Swift UV Optical Telescope. The early-time observations reveal multiple emission components that evolve independently, with a delayed power-law component that exhibits significant spectral attenuation above 40 MeV in the first few seconds of the burst. This power-law component transitions to a harder spectrum that is consistent with the afterglow emission observed by the XRT at later times. This afterglow component is clearly identifiable in the GBM and BAT light curves as a slowly fading emission component on which the rest of the prompt emission is superimposed. As a result, we are able to observe the transition from internal-shock- to external-shock-dominated emission. We find that the temporal and spectral evolution of the broadband afterglow emission can be well modeled as synchrotron emission from a forward shock propagating into a wind-like circumstellar environment. We estimate the initial bulk Lorentz factor using the observed high-energy spectral cutoff. Considering the onset of the afterglow component, we constrain the deceleration radius at which this forward shock begins to radiate in order to estimate the maximum synchrotron energy as a function of time. We find that even in the LAT energy range, there exist high-energy photons that are in tension with the theoretical maximum energy that can be achieved through synchrotron emission from a shock. These violations of the maximum synchrotron energy are further compounded by the detection of very high-energy (VHE) emission above 300 GeV by MAGIC concurrent with our observations. We conclude that the observations of VHE photons from GRB 190114C necessitates either an additional emission mechanism at very high energies that is hidden in the synchrotron component in the LAT energy range, an acceleration mechanism that imparts energy to the particles at a rate that is faster than the electron synchrotron energy-loss rate, or revisions of the fundamental assumptions used in estimating the maximum photon energy attainable through the synchrotron process. [ABSTRACT FROM AUTHOR]

Published
2020
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38. Bright Gamma-Ray Flares Observed in GRB 131108A.

Author

M. Ajello, M. Arimoto, K. Asano, M. Axelsson, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, A. Berretta, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, S. Buson, R. A. Cameron, R. Caputo, and P. A. Caraveo

Published
2019
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39. A Decade of Gamma-Ray Bursts Observed by Fermi-LAT: The Second GRB Catalog.

Author

M. Ajello, M. Arimoto, M. Axelsson, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, P. N. Bhat, E. Bissaldi, R. D. Blandford, R. Bonino, J. Bonnell, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, R. A. Cameron, R. Caputo, P. A. Caraveo, and E. Cavazzuti

Subjects
GAMMA ray bursts, CATALOGS, GLIOBLASTOMA multiforme
Abstract

The Large Area Telescope (LAT) aboard the Fermi spacecraft routinely observes high-energy emission from gamma-ray bursts (GRBs). Here we present the second catalog of LAT-detected GRBs, covering the first 10 yr of operations, from 2008 to 2018 August 4. A total of 186 GRBs are found; of these, 91 show emission in the range 30–100 MeV (17 of which are seen only in this band) and 169 are detected above 100 MeV. Most of these sources were discovered by other instruments (Fermi/GBM, Swift/BAT, AGILE, INTEGRAL) or reported by the Interplanetary Network (IPN); the LAT has independently triggered on four GRBs. This catalog presents the results for all 186 GRBs. We study onset, duration, and temporal properties of each GRB, as well as spectral characteristics in the 100 MeV–100 GeV energy range. Particular attention is given to the photons with the highest energy. Compared with the first LAT GRB catalog, our rate of detection is significantly improved. The results generally confirm the main findings of the first catalog: the LAT primarily detects the brightest GBM bursts, and the high-energy emission shows delayed onset as well as longer duration. However, in this work we find delays exceeding 1 ks and several GRBs with durations over 10 ks. Furthermore, the larger number of LAT detections shows that these GRBs not only cover the high-fluence range of GBM-detected GRBs but also sample lower fluences. In addition, the greater number of detected GRBs with redshift estimates allows us to study their properties in both the observer and rest frames. Comparison of the observational results with theoretical predictions reveals that no model is currently able to explain all results, highlighting the role of LAT observations in driving theoretical models. [ABSTRACT FROM AUTHOR]

Published
2019
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40. AGILE Detection of Gamma-Ray Sources Coincident with Cosmic Neutrino Events.

Author

F. Lucarelli, M. Tavani, G. Piano, A. Bulgarelli, I. Donnarumma, F. Verrecchia, C. Pittori, L. A. Antonelli, A. Argan, G. Barbiellini, P. Caraveo, M. Cardillo, P. W. Cattaneo, A. Chen, S. Colafrancesco, E. Costa, E. Del Monte, G. Di Cocco, A. Ferrari, and V. Fioretti

Subjects
NEUTRINOS, COSMIC neutrino background, GAMMA ray sources, EXTRAGALACTIC distances, ARTIFICIAL satellites in astronomy
Abstract

The origin of cosmic neutrinos is still largely unknown. Using data obtained by the gamma-ray imager on board the Astro-rivelatore Gamma a Immagini Leggero (AGILE) satellite, we systematically searched for transient gamma-ray sources above 100 MeV that are temporally and spatially coincident with 10 recent high-energy neutrino IceCube events. We found three AGILE candidate sources that can be considered possible counterparts to neutrino events. Detecting three gamma-ray/neutrino associations out of 10 IceCube events is shown to be unlikely due to a chance coincidence. One of the sources is related to the BL Lac source TXS 0506+056. For the other two AGILE gamma-ray sources there are no obvious known counterparts, and both Galactic and extragalactic origin should be considered. [ABSTRACT FROM AUTHOR]

Published
2019
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41. Investigating the Nature of Late-time High-energy GRB Emission through Joint Fermi/Swift Observations.

Author

M. Ajello, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, R. A. Cameron, R. Caputo, P. A. Caraveo, G. Chiaro, S. Ciprini, J. Cohen-Tanugi, D. Costantin, and F. D’Ammando

Subjects
GAMMA ray astronomy, ELECTRON synchrotrons, AFTERGLOW (Physics), ASTRONOMICAL observations, TELESCOPES
Abstract

We use joint observations by the Swift X-ray Telescope (XRT) and the Fermi Large Area Telescope (LAT) of gamma-ray burst (GRB) afterglows to investigate the nature of the long-lived high-energy emission observed by Fermi LAT. Joint broadband spectral modeling of XRT and LAT data reveals that LAT nondetections of bright X-ray afterglows are consistent with a cooling break in the inferred electron synchrotron spectrum below the LAT and/or XRT energy ranges. Such a break is sufficient to suppress the high-energy emission so as to be below the LAT detection threshold. By contrast, LAT-detected bursts are best fit by a synchrotron spectrum with a cooling break that lies either between or above the XRT and LAT energy ranges. We speculate that the primary difference between GRBs with LAT afterglow detections and the nondetected population may be in the type of circumstellar environment in which these bursts occur, with late-time LAT detections preferentially selecting GRBs that occur in low wind-like circumburst density profiles. Furthermore, we find no evidence of high-energy emission in the LAT-detected population significantly in excess of the flux expected from the electron synchrotron spectrum fit to the observed X-ray emission. The lack of excess emission at high energies could be due to a shocked external medium in which the energy density in the magnetic field is stronger than or comparable to that of the relativistic electrons behind the shock, precluding the production of a dominant synchrotron self-Compton (SSC) component in the LAT energy range. Alternatively, the peak of the SSC emission could be beyond the 0.1–100 GeV energy range considered for this analysis. [ABSTRACT FROM AUTHOR]

Published
2018
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43. 3FHL: The Third Catalog of Hard Fermi-LAT Sources.

Author

M. Ajello, W. B. Atwood, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, R. Bellazzini, E. Bissaldi, R. D. Blandford, E. D. Bloom, R. Bonino, J. Bregeon, R. J. Britto, P. Bruel, R. Buehler, S. Buson, R. A. Cameron, R. Caputo, M. Caragiulo, and P. A. Caraveo

Published
2017
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44. AGILE Detection of a Candidate Gamma-Ray Precursor to the ICECUBE-160731 Neutrino Event.

Author

F. Lucarelli, C. Pittori, F. Verrecchia, I. Donnarumma, M. Tavani, A. Bulgarelli, A. Giuliani, L. A. Antonelli, P. Caraveo, P. W. Cattaneo, S. Colafrancesco, F. Longo, S. Mereghetti, A. Morselli, L. Pacciani, G. Piano, A. Pellizzoni, M. Pilia, A. Rappoldi, and A. Trois

Subjects
GALAXIES, GAMMA rays, NATURAL satellites, NEUTRINO astrophysics, GAMMA ray astronomy
Abstract

On 2016 July 31 the ICECUBE collaboration reported the detection of a high-energy starting event induced by an astrophysical neutrino. Here, we report on a search for a gamma-ray counterpart to the ICECUBE-160731 event, made with the AGILE satellite. No detection was found spanning the time interval of ±1 ks around the neutrino event time T0 using the AGILE “burst search” system. Looking for a possible gamma-ray precursor in the results of the AGILE-GRID automatic Quick Look procedure over predefined 48-hr time bins, we found an excess above 100 MeV between 1 and 2 days before T0, which is positionally consistent with the ICECUBE error circle, that has a post-trial significance of about . A refined data analysis of this excess confirms, a posteriori, the automatic detection. The new AGILE transient source, named AGL J1418+0008, thus stands as a possible ICECUBE-160731 gamma-ray precursor. No other space missions nor ground observatories have reported any detection of transient emission consistent with the ICECUBE event. We show that Fermi-LAT had a low exposure for the ICECUBE region during the AGILE gamma-ray transient. Based on an extensive search for cataloged sources within the error regions of ICECUBE-160731 and AGL J1418+0008, we find a possible common counterpart showing some of the key features associated with the high-energy peaked BL Lac (HBL) class of blazars. Further investigations on the nature of this source using dedicated SWIFT ToO data are presented. [ABSTRACT FROM AUTHOR]

Published
2017
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45. Gamma-Ray Blazars within the First 2 Billion Years.

Author

M. Ackermann, M. Ajello, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, E. D. Bloom, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, S. Buson, R. A. Cameron, M. Caragiulo, and P. A. Caraveo

Published
2017
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46. Fermi-LAT Observations of High-energy Behind-the-limb Solar Flares.

Author

M. Ackermann, R. Buehler, L. Latronico, S. Maldera, R. Bonino, M. Negro, R. Desiante, J. Bregeon, E. Nuss, F. Piron, P. Bruel, P. A. Caraveo, E. Cavazzuti, S. Ciprini, S. Cutini, P. Lubrano, C. Cecchi, M. Giroletti, F. D'Ammando, and A. Allafort

Subjects
SOLAR flares, GAMMA rays, SOLAR x-rays, SUN observations, CORONAL mass ejections
Abstract

We report on the Fermi-LAT detection of high-energy emission from the behind-the-limb (BTL) solar flares that occurred on 2013 October 11, and 2014 January 6 and September 1. The Fermi-LAT observations are associated with flares from active regions originating behind both the eastern and western limbs, as determined by STEREO. All three flares are associated with very fast coronal mass ejections (CMEs) and strong solar energetic particle events. We present updated localizations of the >100 MeV photon emission, hard X-ray (HXR) and EUV images, and broadband spectra from 10 keV to 10 GeV, as well as microwave spectra. We also provide a comparison of the BTL flares detected by Fermi-LAT with three on-disk flares and present a study of some of the significant quantities of these flares as an attempt to better understand the acceleration mechanisms at work during these occulted flares. We interpret the HXR emission to be due to electron bremsstrahlung from a coronal thin-target loop top with the accelerated electron spectra steepening at semirelativistic energies. The >100 MeV gamma-rays are best described by a pion-decay model resulting from the interaction of protons (and other ions) in a thick-target photospheric source. The protons are believed to have been accelerated (to energies >10 GeV) in the CME environment and precipitate down to the photosphere from the downstream side of the CME shock and landed on the front side of the Sun, away from the original flare site and the HXR emission. [ABSTRACT FROM AUTHOR]

Published
2017
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47. FERMI LARGE AREA TELESCOPE DETECTION OF EXTENDED GAMMA-RAY EMISSION FROM THE RADIO GALAXY FORNAX A.

Author

M. Ackermann, M. Ajello, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, R. Bellazzini, E. Bissaldi, R. D. Blandford, E. D. Bloom, R. Bonino, T. J. Brandt, J. Bregeon, P. Bruel, R. Buehler, S. Buson, G. A. Caliandro, R. A. Cameron, M. Caragiulo, and P. A. Caraveo

Subjects
COSMIC background radiation, EXTRAGALACTIC distances, GAMMA rays, GALAXIES, JETS (Nuclear physics)
Abstract

We report the Fermi Large Area Telescope detection of extended γ-ray emission from the lobes of the radio galaxy Fornax A using 6.1 years of Pass 8 data. After Centaurus A, this is now the second example of an extended γ-ray source attributed to a radio galaxy. Both an extended flat disk morphology and a morphology following the extended radio lobes were preferred over a point-source description, and the core contribution was constrained to be % of the total γ-ray flux. A preferred alignment of the γ-ray elongation with the radio lobes was demonstrated by rotating the radio lobes template. We found no significant evidence for variability on ∼0.5 year timescales. Taken together, these results strongly suggest a lobe origin for the γ-rays. With the extended nature of the γ-ray emission established, we model the source broadband emission considering currently available total lobe radio and millimeter flux measurements, as well as X-ray detections attributed to inverse Compton (IC) emission off the cosmic microwave background (CMB). Unlike the Centaurus A case, we find that a leptonic model involving IC scattering of CMB and extragalactic background light (EBL) photons underpredicts the γ-ray fluxes by factors of about ∼2–3, depending on the EBL model adopted. An additional γ-ray spectral component is thus required, and could be due to hadronic emission arising from proton–proton collisions of cosmic rays with thermal plasma within the radio lobes. [ABSTRACT FROM AUTHOR]

Published
2016
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48. AGILE OBSERVATIONS OF THE GRAVITATIONAL-WAVE EVENT GW150914.

Author

M. Tavani, C. Pittori, F. Verrecchia, A. Bulgarelli, A. Giuliani, I. Donnarumma, A. Argan, A. Trois, F. Lucarelli, M. Marisaldi, E. Del Monte, Y. Evangelista, V. Fioretti, A. Zoli, G. Piano, P. Munar-Adrover, L. A. Antonelli, G. Barbiellini, P. Caraveo, and P. W. Cattaneo

Published
2016
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50. CONTEMPORANEOUS BROADBAND OBSERVATIONS OF THREE HIGH-REDSHIFT BL LAC OBJECTS.

Author

M. Ackermann, M. Ajello, H. An, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, J. Bregeon, R. J. Britto, P. Bruel, R. Buehler, G. A. Caliandro, R. A. Cameron, M. Caragiulo, P. A. Caraveo, E. Cavazzuti, and C. Cecchi

Subjects
SPECTRAL energy distribution, COMPTON effect, ABSORPTION, SYNCHROTRONS, LUMINOSITY
Abstract

We have collected broadband spectral energy distributions (SEDs) of three BL Lac objects 3FGL J0022.1−1855 (z = 0.689), 3FGL J0630.9−2406 ( 1.239), and 3FGL J0811.2−7529 (z = 0.774), detected by Fermi with relatively flat gigaelectronvolt spectra. By observing simultaneously in the near-infrared to hard X-ray band, we can well characterize the high end of the synchrotron component of the SED. Thus, fitting the SEDs to synchro-Compton models of the dominant emission from the relativistic jet, we can constrain the underlying particle properties and predict the shape of the gigaelectronvolt Compton component. Standard extragalactic background light (EBL) models explain the high-energy absorption well, with poorer fits for high-ultraviolet models. The fits show clear evidence for EBL absorption in the Fermi spectrum of our highest-redshift source 3FGL J0630.9−2406. While synchrotron self-Compton models adequately describe the SEDs, the situation may be complicated by possible external Compton components. For 3FGL J0811.2−7529, we also discover a nearby serendipitous source in the X-ray data, which is almost certainly another lower synchrotron peak frequency () BL Lac, that may contribute flux in the Fermi band. Since our sources are unusual high-luminosity, moderate BL Lacs, we compare these quantities and the Compton dominance, the ratio of peak inverse Compton to peak synchrotron luminosities (), with those of the full Fermi BL Lac population. [ABSTRACT FROM AUTHOR]

Published
2016
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