Fermi Large Area Telescope observations of Local Group galaxies: detection of M31 and search for M33

被引：138

作者：

Abdo, A. A. ^{[1
,2
]}

Ackermann, M. ^{[3
,4
]}

Ajello, M. ^{[3
,4
]}

Allafort, A. ^{[3
,4
]}

Atwood, W. B. ^{[5
,6
]}

Baldini, L. ^{[7
]}

Ballet, J. ^{[8
]}

Barbiellini, G. ^{[9
,10
]}

Bastieri, D. ^{[11
,12
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[7
]}

Berenji, B. ^{[3
,4
]}

Blandford, R. D. ^{[3
,4
]}

Bloom, E. D. ^{[3
,4
]}

Bonamente, E. ^{[13
,14
]}

Borgland, A. W. ^{[3
,4
]}

Bouvier, A. ^{[3
,4
]}

Brandt, T. J. ^{[15
,16
]}

Bregeon, J. ^{[7
]}

Brigida, M. ^{[17
,18
,19
]}

Bruel, P. ^{[20
]}

Buehler, R. ^{[3
,4
]}

Burnett, T. H. ^{[21
]}

Buson, S. ^{[11
,12
]}

Caliandro, G. A. ^{[22
]}

Cameron, R. A. ^{[3
,4
]}

Cannon, A. ^{[23
,24
]}

Caraveo, P. A. ^{[25
]}

Casandjian, J. M. ^{[8
]}

Cecchi, C. ^{[13
,14
]}

Celik, Oe. ^{[23
,26
,27
,28
]}

Charles, E. ^{[3
,4
]}

Chekhtman, A. ^{[1
,29
]}

Chiang, J. ^{[3
,4
]}

Ciprini, S. ^{[14
]}

Claus, R. ^{[3
,4
]}

Cohen-Tanugi, J. ^{[30
]}

Conrad, J. ^{[31
,32
]}

Dermer, C. D. ^{[1
]}

de Angelis, A. ^{[33
,34
]}

de Palma, F. ^{[17
,18
,19
]}

Digel, S. W. ^{[3
,4
]}

do Couto e Silva, E. ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Drlica-Wagner, A. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Favuzzi, C. ^{[17
,18
,19
]}

Fegan, S. J. ^{[20
]}

Fortin, P. ^{[20
]}

Frailis, M. ^{[33
,34
,35
]}

机构：

[1] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA

[2] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA

[3] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[5] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[7] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[8] Univ Paris Diderot, CEA Saclay, CNRS, CEA IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France

[9] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[10] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[11] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[12] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[13] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[14] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[15] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

[16] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA

[17] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[18] Politecn Bari, I-70126 Bari, Italy

[19] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[20] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[21] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[22] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain

[23] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[24] Univ Coll Dublin, Dublin 4, Ireland

[25] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy

[26] CRESST, Greenbelt, MD 20771 USA

[27] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

[28] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

[29] George Mason Univ, Fairfax, VA 22030 USA

[30] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France

[31] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden

[32] Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden

[33] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[34] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[35] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy

[36] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[37] INAF, Ist Radioastron, I-40129 Bologna, Italy

[38] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

[39] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

[40] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[41] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[42] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[43] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[44] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[45] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[46] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

[47] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

[48] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[49] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[50] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 523卷

关键词：

Local Group; cosmic rays; gamma rays: galaxies; LARGE-MAGELLANIC-CLOUD; GAMMA-RAY EMISSION; STAR-FORMATION; NGC; 253; NEUTRAL HYDROGEN; NEARBY GALAXIES; SPACE-TELESCOPE; ATOMIC GAS; STARBURST; DISTANCE;

D O I：

10.1051/0004-6361/201015759

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Cosmic rays (CRs) can be studied through the galaxy-wide gamma-ray emission that they generate when propagating in the interstellar medium. The comparison of the diffuse signals from different systems may inform us about the key parameters in CR acceleration and transport. Aims. We aim to determine and compare the properties of the cosmic-ray-induced gamma-ray emission of several Local Group galaxies. Methods. We use 2 years of nearly continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope to search for gamma-ray emission from M31 and M33. We compare the results with those for the Large Magellanic Cloud, the Small Magellanic Cloud, the Milky Way, and the starburst galaxies M82 and NGC 253. Results. We detect a gamma-ray signal at 5 sigma significance in the energy range 200 MeV-20 GeV that is consistent with originating from M31. The integral photon flux above 100 MeV amounts to (9.1 +/- 1.9(stat) +/- 1.0(sys)) x 10(-9) ph cm(-2) s(-1). We find no evidence for emission from M33 and derive an upper limit on the photon flux > 100 MeV of 5.1 x 10(-9) ph cm(-2) s(-1) (2 sigma). Comparing these results to the properties of other Local Group galaxies, we find indications of a correlation between star formation rate and gamma-ray luminosity that also holds for the starburst galaxies. Conclusions. The gamma-ray luminosity of M31 is about half that of the Milky Way, which implies that the ratio between the average CR densities in M31 and the Milky Way amounts to xi = 0.35 +/- 0.25. The observed correlation between gamma-ray luminosity and star formation rate suggests that the flux of M33 is not far below the current upper limit from the LAT observations.

引用

页数：7

共 47 条

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