SEARCH FOR GAMMA-RAY EMISSION FROM THE COMA CLUSTER WITH SIX YEARS OF FERMI-LAT DATA
SEARCH FOR GAMMA-RAY EMISSION FROM THE COMA CLUSTER WITH SIX YEARS OF FERMI-LAT DATA
复制标题
用六年的费米拉特数据搜索彗发星团的伽马射线发射
DOI：
10.3847/0004-637x/819/2/149
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发表时间：
2015
期刊：
影响因子：
--
通讯作者：
Y. Rephaeli
中科院分区：
文献类型：
--
作者：
M. Ackermann;M. Ajello;A. Albert;W. Atwood;L. Baldini;L. Baldini;J. Ballet;G. Barbiellini;G. Barbiellini;D. Bastieri;D. Bastieri;K. Bechtol;R. Bellazzini;E. Bissaldi;R. Blandford;E. Bloom;R. Bonino;E. Bottacini;J. Bregeon;P. Bruel;R. Buehler;G. Caliandro;R. Cameron;M. Caragiulo;M. Caragiulo;P. Caraveo;J. Casandjian;E. Cavazzuti;C. Cecchi;C. Cecchi;E. Charles;A. Chekhtman;G. Chiaro;S. Ciprini;S. Ciprini;J. Cohen;J. Conrad;S. Cutini;S. Cutini;S. Cutini;F. D’Ammando;F. D’Ammando;A. Angelis;F. Palma;R. Desiante;R. Desiante;S. Digel;L. Venere;L. Venere;P. Drell;C. Favuzzi;C. Favuzzi;S. Fegan;Y. Fukazawa;S. Funk;P. Fusco;P. Fusco;F. Gargano;D. Gasparrini;D. Gasparrini;N. Giglietto;N. Giglietto;F. Giordano;F. Giordano;M. Giroletti;G. Godfrey;D. Green;D. Green;I. Grenier;S. Guiriec;E. Hays;J. Hewitt;D. Horan;G. Jóhannesson;M. Kuss;S. Larsson;L. Latronico;J. Li;Liang Li;F. Longo;F. Longo;F. Loparco;F. Loparco;M. Lovellette;P. Lubrano;P. Lubrano;G. Madejski;S. Maldera;A. Manfreda;M. Mayer;M. Mazziotta;P. Michelson;W. Mitthumsiri;T. Mizuno;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;E. Nuss;T. Ohsugi;M. Orienti;E. Orlando;J. Ormes;D. Paneque;D. Paneque;M. Pesce;M. Pesce;V. Petrosian;F. Piron;G. Pivato;T. Porter;S. Rainò;S. Rainò;R. Rando;R. Rando;M. Razzano;A. Reimer;O. Reimer;M. Sánchez;C. Sgro’;E. Siskind;F. Spada;G. Spandre;P. Spinelli;P. Spinelli;H. Tajima;H. Tajima;H. Takahashi;J. Thayer;L. Tibaldo;D. Torres;G. Tosti;G. Tosti;E. Troja;E. Troja;G. Vianello;K. Wood;S. Zimmer;Y. Rephaeli;Y. Rephaeli
我们介绍了γ对彗星团的观测结果，其中包括六年的费米-LAT数据和最新发布的“PASS 8”事件能级分析。我们对该区域的分析揭示了星系团维里半径内的低重要性残余结构，这些结构太微弱，无法用目前的数据进行详细的研究。使用一种不需要假设光谱形状的似然方法，我们得到了星系团中高能粒子相互作用所期望的γ射线通量的上限。我们还考虑了一个基准空间和频谱模板，该模板由模型驱动，在该模型中，观测到的射电晕主要是由次级电子发射的。在这种情况下，超过100MeV？>；的通量的预期上限和观测上限的中位数分别为1.7x10−9ph cm−2 S−1和5.2×10−9ph cm−2 S−1(后者相当于1.8σ水平的剩余排放)。这些界限相当于或高于在有或没有二次电子再加速的宇宙线(CR)模型中预测的强子伽马射线发射水平，尽管直接比较对CRS的起源和传播模式以及磁场性质的假设很敏感。来自彗星团内射电星系和恒星形成星系的最小预期γ射线通量大约比我们分析的灵敏度中值低一个数量级。
We present results from γ-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 γ-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 100 MeV ?> are 1.7 × 10−9 ph cm−2 s−1 and 5.2 × 10−9 ph cm−2 s−1 respectively (the latter corresponds to residual emission at the level of 1.8σ). 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 γ-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.
用费米大面积望远镜观测到的最亮星团星系的叠加分析
影响因子：
4.8
作者：
Dutson K
通讯作者：
Dutson K