SEARCH FOR GAMMA-RAY EMISSION FROM THE COMA CLUSTER WITH SIX YEARS OF FERMI-LAT DATA

被引：80

作者：

Ackermann, M. ^{[1
]}

Ajello, M. ^{[2
]}

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

Atwood, W. B. ^{[1
,5
,6
]}

Baldini, L. ^{[3
,4
,7
,8
]}

Ballet, J. ^{[9
]}

Barbiellini, G. ^{[10
,11
]}

Bastieri, D. ^{[12
,13
]}

Bechtol, K. ^{[14
,15
]}

Bellazzini, R. ^{[16
]}

Bissaldi, E. ^{[17
]}

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

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

Bonino, R. ^{[18
,19
]}

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

Bregeon, J. ^{[20
]}

Bruel, P. ^{[21
]}

Buehler, R. ^{[1
]}

Caliandro, G. A. ^{[3
,4
,22
]}

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

Caragiulo, M. ^{[17
,23
,24
]}

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

Casandjian, J. M. ^{[9
]}

Cavazzuti, E. ^{[26
]}

Cecchi, C. ^{[27
,28
]}

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

Chekhtman, A. ^{[29
,30
]}

Chiaro, G. ^{[13
]}

Ciprini, S. ^{[26
,27
]}

Cohen-Tanugi, J. ^{[20
]}

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

Cutini, S. ^{[26
,27
,33
]}

D'Ammando, F. ^{[34
,35
]}

de Angelis, A. ^{[36
,37
]}

de Palma, F. ^{[17
,38
]}

Desiante, R. ^{[18
,39
]}

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

Di Venere, L. ^{[17
,23
,24
]}

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

Favuzzi, C. ^{[17
,23
,24
]}

Fegan, S. J. ^{[21
]}

Fukazawa, Y. ^{[40
]}

Funk, S. ^{[41
]}

Fusco, P. ^{[17
,23
,24
]}

Gargano, F. ^{[17
]}

Gasparrini, D. ^{[26
,27
]}

Giglietto, N. ^{[17
,23
,24
]}

Giordano, F. ^{[17
,23
,24
]}

Giroletti, M. ^{[34
]}

Godfrey, G. ^{[3
,4
]}

机构：

[1] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[2] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA

[3] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 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, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

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

[7] Univ Pisa, I-56127 Pisa, Italy

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

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

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

[11] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

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

[13] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[14] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA

[15] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA

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

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

[18] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[19] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy

[20] Univ Montpellier, CNRS, IN2P3, Lab Universe & Particules Montpellier, F-34059 Montpellier, France

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

[22] CIFS, I-10133 Turin, Italy

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

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

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

[26] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy

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

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

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

[30] Naval Res Lab, Washington, DC 20375 USA

[31] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden

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

[33] Osserv Astron Roma, INAF, I-00040 Rome, Italy

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

[35] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

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

[37] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy

[38] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy

[39] Univ Udine, I-33100 Udine, Italy

[40] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan

[41] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

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

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

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

[45] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA

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

[47] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden

[48] CSIC, Inst Space Sci IEEC, Campus UAB, E-08193 Barcelona, Spain

[49] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA

[50] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 819卷 / 02期

基金：

美国国家航空航天局;

关键词：

galaxies: clusters: individual (Coma); gamma rays: galaxies: clusters; LARGE-AREA TELESCOPE; DIFFUSE RADIO-EMISSION; GALAXY CLUSTERS; NONTHERMAL EMISSION; UPPER LIMITS; CONSTRAINTS; ACCELERATION; ENERGIES; HALOES;

D O I：

10.3847/0004-637X/819/2/149

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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

引用

页数：10

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