Rest-frame properties of 32 gamma-ray bursts observed by the Fermi Gamma-Ray Burst Monitor
D. Gruber, J. Greiner, A. von Kienlin, A. Rau, M. S. Briggs, V. Connaughton, A. Goldstein, A. J. van der Horst, M. Nardini, P. N. Bhat, E. Bissaldi, J. M. Burge… 展开作者
D. Gruber, J. Greiner, A. von Kienlin, A. Rau, M. S. Briggs, V. Connaughton, A. Goldstein, A. J. van der Horst, M. Nardini, P. N. Bhat, E. Bissaldi, J. M. Burgess, V. L. Chaplin, R. Diehl, G. J. Fishman, G. Fitzpatrick, S. Foley, M. H. Gibby, M. M. Giles, S. Guiriec, R. M. Kippen, C. Kouveliotou, L. Lin, S. McBreen, C. A. Meegan, F. Olivares E., W. S. Paciesas, R. D. Preece, D. Tierney, C. Wilson-Hodge
Aims: In this paper we study the main spectral and temporal properties of gamma-ray bursts (GRBs) observed by Fermi/GBM. We investigate these key properties of GRBs in the rest-frame of the progenitor and test for possible intra-parameter correlations to better understand the intrinsic nature of these events. Methods: Our sample comprises 32 GRBs with measured redshift that were observed by GBM until August 2010. 28 of them belong to the long-duration population and 4 events were classified as short/hard bursts. For all of these events we derive, where possible, the intrinsic peak energy in the $νF_ν$ spectrum (\eprest), the duration in the rest-frame, defined as the time in which 90% of the burst fluence was observed (\tninetyrest) and the isotropic equivalent bolometric energy (\eiso). Results: The distribution of \eprest has mean and median values of 1.1 MeV and 750 keV, respectively. A log-normal fit to the sample of long bursts peaks at ~800 keV. No high-\ep population is found but the distribution is biased against low \ep values. We find the lowest possible \ep that GBM can recover to be ~ 15 keV. The \tninetyrest distribution of long GRBs peaks at ~10 s. The distribution of \eiso has mean and median values of $8.9\times 10^{52}$ erg and $8.2 \times 10^{52}$ erg, respectively. We confirm the tight correlation between \eprest and \eiso (Amati relation) and the one between \eprest and the 1-s peak luminosity ($L_p$) (Yonetoku relation). Additionally, we observe a parameter reconstruction effect, i.e. the low-energy power law index $α$ gets softer when \ep is located at the lower end of the detector energy range. Moreover, we do not find any significant cosmic evolution of neither \eprest nor \tninetyrest.
17 Yr of Magnetar Bursts Observed with the Fermi Gamma-ray Burst Monitor
University of Alabama in Huntsville（亨茨维尔阿拉巴马大学）；Sabancı University, Faculty of Engineering and Natural Sciences（萨班哲大学工程与自然科学学院）；Beijing Normal University（北京师范大学）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与前沿科学研究院）；Universities Space and Research Association（大学空间研究协会）；University of Galway（高威大学）；Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville（亨茨维尔阿拉巴马大学空间等离子体与高空大气研究中心）；Rice University（莱斯大学）
Eight Gamma-Ray Bursts Observed with the Fermi Gamma-ray Burst Monitor: Significant Quasi-Thermal Components and Conditional Jet Constraints
College of Physics and Electronics information, Yunnan Normal University（云南师范大学物理与电子科学学院）；Department of Astronomy, School of Physics and Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University（云南大学物理与天文学院天文学系）；Liupanshui Normal College（六盘水师范学院）；State-owned Assets and Laboratory Management Office, Yunnan Normal University（云南师范大学国有资产管理处）
From Rare Events to a Population: Discovering Overlooked Extragalactic Magnetar Giant Flare Candidates in Archival Fermi Gamma-ray Burst Monitor Data
NASA Marshall Space Flight Center（美国国家航空航天局马歇尔太空飞行中心）；Louisiana State University（路易斯安那州立大学）；Universities Space Research Association（大学空间研究协会）；University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；Ioffe Institute（约费研究所）
Long term monitoring of FRB~20121102 with the Nançay Radio Telescope and multi-wavelength campaigns including INTEGRAL
Université Paris-Saclay（巴黎萨克雷大学）；Université Paris-Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理学与宇宙学研究所）；Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E)（环境与空间物理化学实验室）；Université d'Orléans（奥尔良大学）；Observatoire Radioastronomique de Nançay（南希射电天文台）；Observatoire de Paris（巴黎天文台）；Université PSL（巴黎文理研究大学）；Institut d'Astrophysique de Paris (IAP)（巴黎天体物理学研究所）；Sorbonne Université（索邦大学）；University of Galway（高威大学）；University of Sheffield（谢菲尔德大学）；Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究所）；Massachusetts Institute of Technology（麻省理工学院）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；LESIA（地球与空间环境演化观测与研究实验室）
Implications of Joint Spectral Analysis of Gamma-Ray Bursts detected by Fermi Large Area Telescope and Gamma-ray Burst Monitor on Phenomenological Correlations
University of Johannesburg（约翰内斯堡大学）；Omdurman Islamic University（恩图曼伊斯兰大学）；The George Washington University（乔治华盛顿大学）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；University of Trieste（的里雅斯特大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Istituto Nazionale di Fisica Nucleare, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Stanford University（斯坦福大学）；Istituto Nazionale di Fisica Nucleare, Sezione di Bari（意大利国家核物理研究所巴里分部）；Università degli studi di Trento（特伦托大学）
费米伽马射线太空望远镜（英语：Fermi Gamma-ray Space Telescope）的大面积望远镜（英语：Large Area Telescope）是一个对转换望远镜，对超过40个能量十年的伽马射线敏感，介于20 MeV和300 GeV之间。LAT与伽马射线暴监测器（GBM）-任务上的另一种仪器-协同作用，在研究伽马射线暴（GRB）方面，在光谱覆盖范围、有效面积和仪器死时间方面具有前所未有的灵敏度。我们将回顾GRB的Fermi-LAT观测的主要结果，介绍GeV能区GRB的主要性质。
Wideband Monitoring of FRB 20180916B Across a Half-Decade Bandwidth Using the Upgraded GMRT
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究所国家射电天文中心）；International Centre for Radio Astronomy Research (ICRAR), Curtin University（科廷大学国际射电天文研究中心）
Compton scattering in terrestrial gamma-ray flashes detected with the Fermi gamma-ray burst monitor
地面伽玛射线闪光（英语：Terrestrial gamma ray flashes，缩写为TGFs）是一种与雷暴中的闪电活动相关的短时间强烈伽玛射线闪光。使用蒙特卡罗模拟的相对论逃逸电子雪崩（RREA）的过程中，理论预测的时间和光谱演化的TGFs进行了比较与观测的伽马射线暴监视器（GBM）上的费米伽玛射线太空望远镜。假设一个单一的源高度为15公里，模拟数据的比较进行了一系列的经验选择的源电子变化的时间尺度。数据表现出明显的软化源距离的增加，在定性与理论预测一致。模拟光谱在数据中遵循这一趋势，但往往低估了观察到的硬度。这种差异可能意味着基本的RREA模型是不够的。或者，相对于天顶倾斜的TGF光束可以产生与数据兼容的源距离的演变。基于这些结果，我们提出，通过GBM观察到的TGFs的源电子分布在至少几十微秒的时间尺度上变化，上限约为。100微秒
Insights on the Gamma-Ray Bursts variability in their cosmological rest frame
Istituto Nazionale di Astrofisica（意大利国家天体物理研究所）；Agenzia Spaziale Italiana（意大利航天局）；Università degli Studi di Udine（乌迪内大学）；Istituto Nazionale di Fisica Nucleare（意大利国家核物理研究所）
