Deep view of the Large Magellanic Cloud with six years of Fermi-LAT observations

被引:62
作者
Ackermann, M. [1 ]
Albert, A. [2 ,3 ]
Atwood, W. B. [4 ,5 ]
Baldini, L. [2 ,3 ,6 ,7 ]
Ballet, J. [8 ]
Barbiellini, G. [9 ,10 ]
Bastieri, D. [11 ,12 ]
Bellazzini, R. [13 ]
Bissaldi, E. [14 ]
Bloom, E. D. [2 ,3 ]
Bonino, R. [15 ,16 ]
Brandt, T. J. [17 ]
Bregeon, J. [18 ]
Bruel, P. [19 ]
Buehler, R. [1 ]
Caliandro, G. A. [2 ,3 ,20 ]
Cameron, R. A. [2 ,3 ]
Caragiulo, M. [14 ]
Caraveo, P. A. [21 ]
Cavazzuti, E. [22 ]
Cecchi, C. [23 ,24 ]
Charles, E. [2 ,3 ]
Chekhtman, A. [25 ,26 ]
Chiang, J. [2 ,3 ]
Chiaro, G. [12 ]
Ciprini, S. [22 ,23 ,27 ]
Cohen-Tanugi, J. [18 ]
Cutini, S. [22 ,23 ,27 ]
D'Ammando, F. [28 ,29 ]
de Angelis, A. [30 ,31 ]
de Palma, F. [14 ,32 ]
Desiante, R. [15 ,33 ]
Digel, S. W. [2 ,3 ]
Drell, P. S. [2 ,3 ]
Favuzzi, C. [14 ,34 ,35 ]
Ferrara, E. C. [17 ]
Focke, W. B. [2 ,3 ]
Franckowiak, A. [2 ,3 ]
Fusco, P. [14 ,34 ,35 ]
Gargano, F. [14 ]
Gasparrini, D. [22 ,23 ,27 ]
Giglietto, N. [14 ,34 ,35 ]
Giordano, F. [14 ,34 ,35 ]
Godfrey, G. [2 ,3 ]
Grenier, I. A. [8 ]
Grondin, M. -H. [36 ]
Guillemot, L. [37 ,38 ]
Guiriec, S. [17 ,39 ]
Harding, A. K. [17 ]
Hill, A. B. [2 ,3 ,40 ]
机构
[1] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany
[2] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA
[3] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA
[4] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA
[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[6] Univ Pisa, I-56127 Pisa, Italy
[7] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy
[8] Univ Paris Diderot, CEA IRFU, Lab AIM, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France
[9] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy
[10] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy
[11] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy
[12] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[13] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy
[14] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy
[15] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy
[16] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy
[17] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[18] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, F-34059 Montpellier, France
[19] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[20] CIFS, I-10133 Turin, Italy
[21] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy
[22] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy
[23] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy
[24] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy
[25] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA
[26] Naval Res Lab, Washington, DC 20375 USA
[27] INAF Osservatorio Astron Roma, I-00040 Rome, Italy
[28] INAF Ist Radioastron, I-40129 Bologna, Italy
[29] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy
[30] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy
[31] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy
[32] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy
[33] Univ Udine, I-33100 Udine, Italy
[34] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy
[35] Politecn Bari, I-70126 Bari, Italy
[36] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, BP120, F-33175 Gradignan, France
[37] Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France
[38] CNRS INSU, Stn Radioastron Nancay, Observ Paris, F-18330 Nancay, France
[39] NASA, Moffett Field, CA USA
[40] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
[41] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland
[42] IRAP, CNRS, F-31028 Toulouse 4, France
[43] Univ Toulouse, UPS OMP, IRAP, Toulouse, France
[44] AlbaNova, Dept Phys, KTH Royal Inst Technol, S-10691 Stockholm, Sweden
[45] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden
[46] Inst Space Sci IEEC CSIC, Campus UAB, Barcelona 08193, Spain
[47] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan
[48] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy
[49] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA
[50] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA
关键词
gamma rays: galaxies; Magellanic Clouds; cosmic rays; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; STAR-FORMING GALAXIES; SUPERNOVA REMNANT; INTERSTELLAR-MEDIUM; MAGNETIC-FIELD; SOURCE CATALOG; COSMIC-RAYS; NGC; 253; PULSAR;
D O I
10.1051/0004-6361/201526920
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The nearby Large Magellanic Cloud (LMC) provides a rare opportunity of a spatially resolved view of an external star-forming galaxy in gamma-rays. The LMC was detected at 0.1-100 GeV as an extended source with CGRO/EGRET and using early observations with the Fermi-LAT. The emission was found to correlate with massive star-forming regions and to be particularly bright towards 30 Doradus. Aims. Studies of the origin and transport of cosmic rays (CRs) in the Milky Way are frequently hampered by line-of-sight confusion and poor distance determination. The LMC offers a complementary way to address these questions by revealing whether and how the gamma-ray emission is connected to specific objects, populations of objects, and structures in the galaxy. Methods. We revisited the gamma-ray emission from the LMC using about 73 months of Fermi-LAT P7REP data in the 0.2-100 GeV range. We developed a complete spatial and spectral model of the LMC emission, for which we tested several approaches: a simple geometrical description, template-fitting, and a physically driven model for CR-induced interstellar emission. Results. In addition to identifying PSR J0540-6919 through its pulsations, we find two hard sources positionally coincident with plerion N 157B and supernova remnant N 132D, which were also detected at TeV energies with H.E.S.S. We detect an additional soft source that is currently unidentified. Extended emission dominates the total flux from the LMC. It consists of an extended component of about the size of the galaxy and additional emission from three to four regions with degree-scale sizes. If it is interpreted as CRs interacting with interstellar gas, the large-scale emission implies a large-scale population of similar to 1-100 GeV CRs with a density of similar to 30% of the local Galactic value. On top of that, the three to four small-scale emission regions would correspond to enhancements of the CR density by factors 2 to 6 or higher, possibly more energetic and younger populations of CRs compared to the large-scale population. An alternative explanation is that this is emission from an unresolved population of at least two dozen objects, such as pulsars and their nebulae or supernova remnants. This small-scale extended emission has a spatial distribution that does not clearly correlate with known components of the LMC, except for a possible relation to cavities and supergiant shells. Conclusions. The Fermi-LAT GeV observations allowed us to detect individual sources in the LMC. Three of the newly discovered sources are associated with rare and extreme objects. The 30 Doradus region is prominent in GeV gamma-rays because PSR J0540-6919 and N 157B are strong emitters. The extended emission from the galaxy has an unexpected spatial distribution, and observations at higher energies and in radio may help to clarify its origin.
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页数:17
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