FERMI-LAT OBSERVATIONS OF HIGH-ENERGY γ-RAY EMISSION TOWARD THE GALACTIC CENTER

被引:281
作者
Ajello, M. [1 ]
Albert, A. [2 ,3 ]
Atwood, W. B. [4 ,5 ]
Barbiellini, G. [6 ,7 ]
Bastieri, D. [8 ,9 ]
Bechtol, K. [10 ,11 ]
Bellazzini, R. [12 ]
Bissaldi, E. [13 ]
Blandford, R. D. [2 ,3 ]
Bloom, E. D. [2 ,3 ]
Bonino, R. [14 ,15 ]
Bottacini, E. [2 ,3 ]
Brandt, T. J. [16 ]
Bregeon, J. [17 ]
Bruel, P. [18 ]
Buehler, R. [19 ]
Buson, S. [8 ,9 ]
Caliandro, G. A. [2 ,3 ,20 ]
Cameron, R. A. [2 ,3 ]
Caputo, R. [4 ,5 ]
Caragiulo, M. [13 ]
Carave, P. A. [21 ]
Cecchi, C. [22 ,23 ]
Chekhtman, A. [24 ]
Chiang, J. [2 ,3 ]
Chiaro, G. [9 ]
Ciprini, S. [22 ,25 ,26 ]
Cohen-Tanugi, J. [17 ]
Cominsky, L. R. [27 ]
Conrad, J. [28 ,29 ,30 ]
Cutini, S. [22 ,25 ,26 ]
D'Ammando, F. [31 ,32 ]
de Angelis, A. [33 ,34 ]
de Palma, F. [13 ,35 ]
Desiante, R. [14 ,36 ]
Di Venere, L. [37 ]
Drell, P. S. [2 ,3 ]
Favuzzi, C. [13 ,37 ]
Ferrara, E. C. [16 ]
Fusco, P. [13 ,37 ]
Gargano, F. [13 ]
Gasparrini, D. [22 ,25 ,26 ]
Giglietto, N. [13 ,37 ]
Giommi, P. [25 ]
Giordano, F. [13 ,37 ]
Giroletti, M. [31 ]
Glanzman, T. [2 ,3 ]
Godfrey, G. [2 ,3 ]
Gomez-Vargas, G. A. [38 ,39 ]
Grenier, I. A. [40 ]
机构
[1] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA
[2] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA
[3] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA
[4] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[6] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy
[7] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy
[8] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy
[9] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[10] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA
[11] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA
[12] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy
[13] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy
[14] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy
[15] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy
[16] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[17] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34059 Montpellier, France
[18] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[19] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany
[20] CIFS, I-10133 Turin, Italy
[21] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy
[22] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy
[23] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy
[24] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA
[25] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy
[26] INAF Osservatorio Astron Roma, I-00040 Rome, Italy
[27] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA
[28] Stockholm Univ, Dept Phys, Alballova, SE-10691 Stockholm, Sweden
[29] Oskar Klein Ctr Cosmoparticle Phys, Alballova, SE-10691 Stockholm, Sweden
[30] Royal Swedish Acad Sci, Box 50005, SE-10405 Stockholm, Sweden
[31] INAF Ist Radioastron, I-40129 Bologna, Italy
[32] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy
[33] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy
[34] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy
[35] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy
[36] Univ Udine, I-33100 Udine, Italy
[37] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy
[38] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy
[39] Pontificia Univ Catolica Chile, Dept Fis, Ave Vicuna Mackenna 4860, Santiago, Chile
[40] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France
[41] Univ Gottingen, Inst Theoret Phys, Fac Phys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany
[42] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA
[43] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
[44] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland
[45] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[46] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA
[47] CNRS, IRAP, F-31028 Toulouse 4, France
[48] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France
[49] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden
[50] CSIC, Inst Space Sci IEEC, Campus UAB, E-08193 Barcelona, Spain
基金
美国国家航空航天局; 瑞典研究理事会;
关键词
cosmic rays; Galaxy: center; gamma-rays: general; gamma-rays: ISM; radiation mechanisms: non-thermal; LARGE-AREA TELESCOPE; RADIAL-DISTRIBUTION; DARK-MATTER; COSMIC-RAYS; SOURCE CATALOG; SUPERNOVA-REMNANTS; EGRET OBSERVATIONS; OUTER GALAXY; CONSTRAINTS; GRADIENT;
D O I
10.3847/0004-637X/819/1/44
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The Fermi Large Area Telescope (LAT) has provided the most detailed view to date of the emission toward the Galactic center (GC) in high-energy gamma-rays. This paper describes the analysis of data taken during the first 62 months of the mission in the energy range 1-100 GeV from a 15 degrees x 15 degrees region about the direction of the GC. Specialized interstellar emission models (IEMs) are constructed to enable the separation of the.-ray emissions produced by cosmic ray particles interacting with the interstellar gas and radiation fields in the Milky Way into that from the inner similar to 1 kpc surrounding the GC, and that from the rest of the Galaxy. A catalog of point sources for the 15 degrees x 15 degrees region is self-consistently constructed using these IEMs: the First Fermi-LAT Inner Galaxy Point Source Catalog (1FIG). The spatial locations, fluxes, and spectral properties of the 1FIG sources are presented, and compared with gamma-ray point sources over the same region taken from existing catalogs. After subtracting the interstellar emission and point-source contributions a residual is found. If templates that peak toward the GC are used to model the positive residual the agreement with the data improves, but none of the additional templates tried account for all of its spatial structure. The spectrum of the positive residual modeled with these templates has a strong dependence on the choice of IEM.
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页数:30
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