已知红移Fermi/LAT暴的谱能关系

Fermi卫星的GBM可以更精确地测量Epeak,以及LAT在GeV能段的定位和观测,提供了一个独特的研究伽玛暴谱能关系之一Eiso-Epeak关系的机会.根据9个具有红移的Fermi/LAT暴的谱能关系,发现长暴的这个关系满足一定的关系,而短暴却不满足.     

伽玛射线暴的高能辐射

伽玛暴是宇宙中最剧烈的恒星级高能爆发现象,一般被认为产生于大质量恒星死亡(一些爆发时标长于2 s的伽玛暴在观测上被证实与一类特殊的超新星成协)或者双致密星(比如双中子星系统)并合(这类并合时标很短,可产生时标短于2 s的伽玛暴).工作在8 ke V–300 Ge V能段的Fermi伽玛射线空间望远镜自2008年升空工作之后,伽玛暴瞬时辐射和高能辐射研究取得了重要进展.本综述将介绍Fermi卫星在过去几年内关于伽玛暴领域的一些重要观测结果,并着重介绍这些观测对探索伽玛暴物理(伽玛暴外流体的光球辐射、磁化、Ge V高能辐射起源),特别是Fermi卫星大面积望远镜(LAT)的高能(100 Me V)辐射观测对限制伽玛暴初始速度/洛伦兹因子,限制宇宙河外背景光模型以及检验光速不变原理等方面的主要研究进展.     

Fermi伽马射线暴的光谱能量关系

基于Fermi卫星对伽马射线暴峰值能量探测灵敏度的提高,本文收集了Fermi卫星近8年的已知红移和E_(peak)的84个数据样本,再次分析Amati和Yonetoku关系。研究结果表明:Amati和Yonetoku关系可以分别用两条很好的直线拟合,对能量和光度关系进行了更新。大多数伽马射线暴的均质能量满足2.02×10~(54)erg量级,均质光度满足2.32×10~(52)erg量级。     

Fermi/GBM伽马暴的谱能关系

选取10个已知红移的单峰Fermi/GBM长暴,采用交叉相关函数计算第1与第3能道之间的相对能谱延迟(R_(SL)).研究发现,伽马暴的R_(SL)s分别与峰值光度和红移相关,所得结果与已报道文献中利用BATSE暴得到的结果相符合.这意味着R_(SL)与峰值光度和红移的相关关系不受探测仪器选择效应的影响.这表明R_(SL)可以作为一个可能的宇宙红移探测指示器用于宇宙学参数的测量.利用这些Fermi/GBM伽马暴样本,通过重新分析发现峰值能量与峰值光度、各向同性能存在较强相关.这些关系与从BATSE暴中得到的结果不一致,而与从Swift暴得到的结果符合.     

Fermi γ暴在ARGO-YBJ和AS γ实验中的流强研究

分析2008—2015年Fermi卫星观测到的所有γ射线暴,并将这些Fermiγ暴的能谱延伸到ARGO-YBJ与ASγ实验的工作能区,计算其到达羊八井地面实验中的流强.结果表明:对于在羊八井视场范围内且光子能量在Ge V能区的Fermiγ暴,若不考虑河外背景光子的吸收效应,ARGO-YBJ实验运行期间内,在其灵敏度范围内的有3个;新升级的ASγ实验运行期间内,在其灵敏度范围内的有4个.最后讨论有机会被ARGO-YBJ实验探测到的3个γ暴未得到正结果的原因.此研究为羊八井地面实验与卫星γ射线暴的符合寻找提供重要信息.     

Fermi/GBM单峰长暴的FWHM相关关系研究

本文选取26个已知红移的单峰Fermi/GBM长暴,采用KRL模型拟合光变曲线计算出半峰全宽FWHM,探讨了FWHM相关的关系。发现伽马暴的FWHM与峰值能量Ep相关性不强,未明显发现之前利用BeppoSAX、Swift暴得到的结果。这意味着FWHM与峰值能量Ep的相关关系可能受探测仪器选择效应的影响。同时利用这些Fermi/GBM伽马暴样本,通过重新对FWHM与持续时间T做相关分析,结果发现,FWHM与T90、T50都存在较强的幂律关系,其相关系数分别为R=0.85、R=0.72。这表明FWHM与T90、T50存在这密切关系,同利用BeppoSAX、Swift暴得到的结果一致。     

研究GBM和BAT同时触发的暴

结合Swift和Fermi两个卫星的各自优点,选择Fermi/GBM和Swift/BAT同时触发的伽玛暴观测数据,发现GBM暴持续时间的平均值比BAT暴要小,但是它们的持续时间分布、伽玛暴本身的流量分布以及光子峰值能量分布(log N-log P分布)之间不存在系统性差异.所以,不同仪器的观测差异可能是由于仪器本身的灵敏度引起的,与暴的性质无关.     

Fermi blazar的射电谱指数性质

以Fermi/LAT 4FGL-DR3中blazar为样本,绘制了其射电能谱图(logf_ν-logν).根据散点的分布趋势,分别用一次、二次或三次曲线对能谱进行了拟合,最后得到2347个blazar的能谱及其拟合曲线的参数.根据拟合结果给出了0.05, 0.1, 0.5, 1.4, 5, 8, 15, 50和150 GHz等9个频率处的射电谱指数.讨论了平均谱指数随频率的变化,以及同步辐射谱曲率与射电谱指数的关系.结果表明:平均射电谱指数在-0.1–1的范围内变化,在1–50 GHz频率范围内,谱指数变化幅度最小(0–0.2);在同一频率处,不同子类blazar的平均谱指数不同,且有■;随着射电辐射频率的增加,平均谱指数先减小后增加,呈开口向上的抛物线形状;按照散点的分布趋势,射电能谱图可分成3种类型(Λ, V和S型), 3种类型源的射电谱均应是小尺度和大尺度喷流辐射成分的合成,但Λ与V型源中的2种成分可能不同;各子类blazar的同步辐射谱曲率与射电谱指数有较好的正相关关系,射电辐射对低同步峰频BL Lac (LBL)、平谱射电源(FSRQ)、高同步峰频BL L...     

SWIFT伽玛暴的谱延迟距离指示器

早期研究发现,BASTE长暴的相对谱延迟RSL是一个有用的宇宙距离指示器。本文从SWIFT卫星数据中,挑选10个单脉冲长伽玛暴(T90>2.6)作为样本,对样本进行降噪和去除背景,用交叉相关函数分析1,3能道的谱延迟,通过拟合研究各脉冲参数Asymmetry,Fm,Fp,tm,FWHM,τ31和相对谱延迟的关系,发现相对谱延迟和红移具有很好的相关性,这充分表明SWIFT长暴的相对谱延迟仍然是一个很好的红移指示器。     

从谱演化方面的信息探讨 GRB 061007 的暴周环境

GRB 061007是一个明亮的、长时标的伽玛射线暴（简称伽玛暴）,其红移为1．261．一方面,Swift／XRT观测到的数据显示,此暴X射线波段的光变曲线呈现出单一幂率形态,且幂率指数αXRt=1．68±0．01．另一方面,经由Faulkes Telescope South（简写为FTS）提供的BVRi’多波段光学余辉数据,作者分析发现其各波段光变曲线的幂率指数αOptical均在1．6左右．拟合得到的2个波段幂率指数如此相近,也就意味着此暴的X射线波段和光学波段具有同一起源．作者通过分析X射线波段和光学波段的谱演化情况,探究GRB061007的暴周环境．分析的结果显示,X射线波段的谱指数JB没有演化,而光学波段的谱有向蓝端演化的趋势．根据其光学波段谱的演化趋势,推测此暴的暴周环境不是均匀介质,而应是星风环境．     

γ暴能谱硬度系数的分布及其分类特征

采用非参量化线性相关性分析方法分析康顿空间天文台（CGRO）上的BATSE仪器观测到的γ暴不同能道流量间的相关性，提出新的γ暴能谱硬度系数的定义，并分析其分布特征，进一步证实了γ蛤谱硬度系数与持续时间之间的反相关性，并对这个反相关性提出新的解释，软谱长暴，短暴硬谱，同时，从定量上给出按谱硬度系数对γ暴进行分类的依据，提出了γ暴新的分类方法。     

An origin in the local Universe for some short gamma-ray bursts

Gamma-ray bursts (GRBs) divide into two classes: 'long', which typically have initial durations of T90 > 2 s, and 'short', with durations of T90 < 2 s (where T90 is the time to detect 90% of the observed fluence). Long bursts, which on average have softer gamma-ray spectra, are known to be associated with stellar core-collapse events-in some cases simultaneously producing powerful type Ic supernovae. In contrast, the origin of short bursts has remained mysterious until recently. A subsecond intense 'spike' of gamma-rays during a giant flare from the Galactic soft gamma-ray repeater, SGR 1806-20, reopened an old debate over whether some short GRBs could be similar events seen in galaxies out to approximately 70 Mpc (refs 6-10; redshift z approximately 0.016). Shortly after that, localizations of a few short GRBs (with optical afterglows detected in two cases) have shown an apparent association with a variety of host galaxies at moderate redshifts. Here we report a correlation between the locations of previously observed short bursts and the positions of galaxies in the local Universe, indicating that between 10 and 25 per cent of short GRBs originate at low redshifts (z < 0.025).     

An enigmatic long-lasting gamma-ray burst not accompanied by a bright supernova

Gamma-ray bursts (GRBs) are short, intense flashes of soft gamma-rays coming from the distant Universe. Long-duration GRBs (those lasting more than approximately 2 s) are believed to originate from the deaths of massive stars, mainly on the basis of a handful of solid associations between GRBs and supernovae. GRB 060614, one of the closest GRBs discovered, consisted of a 5-s hard spike followed by softer, brighter emission that lasted for approximately 100 s (refs 8, 9). Here we report deep optical observations of GRB 060614 showing no emerging supernova with absolute visual magnitude brighter than M(V) = -13.7. Any supernova associated with GRB 060614 was therefore at least 100 times fainter, at optical wavelengths, than the other supernovae associated with GRBs. This demonstrates that some long-lasting GRBs can either be associated with a very faint supernova or produced by different phenomena.     

The optical afterglow of the short gamma-ray burst GRB 050709

It has long been known that there are two classes of gamma-ray bursts (GRBs), mainly distinguished by their durations. The breakthrough in our understanding of long-duration GRBs (those lasting more than approximately 2 s), which ultimately linked them with energetic type Ic supernovae, came from the discovery of their long-lived X-ray and optical 'afterglows', when precise and rapid localizations of the sources could finally be obtained. X-ray localizations have recently become available for short (duration <2 s) GRBs, which have evaded optical detection for more than 30 years. Here we report the first discovery of transient optical emission (R-band magnitude approximately 23) associated with a short burst: GRB 050709. The optical afterglow was localized with subarcsecond accuracy, and lies in the outskirts of a blue dwarf galaxy. The optical and X-ray afterglow properties 34 h after the GRB are reminiscent of the afterglows of long GRBs, which are attributable to synchrotron emission from ultrarelativistic ejecta. We did not, however, detect a supernova, as found in most nearby long GRB afterglows, which suggests a different origin for the short GRBs.     

The afterglow and elliptical host galaxy of the short gamma-ray burst GRB 050724

Despite a rich phenomenology, gamma-ray bursts (GRBs) are divided into two classes based on their duration and spectral hardness--the long-soft and the short-hard bursts. The discovery of afterglow emission from long GRBs was a watershed event, pinpointing their origin to star-forming galaxies, and hence the death of massive stars, and indicating an energy release of about 10(51) erg. While theoretical arguments suggest that short GRBs are produced in the coalescence of binary compact objects (neutron stars or black holes), the progenitors, energetics and environments of these events remain elusive despite recent localizations. Here we report the discovery of the first radio afterglow from the short burst GRB 050724, which unambiguously associates it with an elliptical galaxy at a redshift z = 0.257. We show that the burst is powered by the same relativistic fireball mechanism as long GRBs, with the ejecta possibly collimated in jets, but that the total energy release is 10-1,000 times smaller. More importantly, the nature of the host galaxy demonstrates that short GRBs arise from an old (> 1 Gyr) stellar population, strengthening earlier suggestions and providing support for coalescing compact object binaries as the progenitors.     

Gamma暴光变曲线主峰特征参量的相关性分析

γ暴被认为由一系列脉冲所组成，其光变曲线中的峰对应看不同时刻网个相对论火球党层相互作用过程．光变曲线中的主峰对应着最强烈的作用过程，所受背景噪音的污染相对来说最小．因此光变曲线的主峰最适合于用以研究脉冲特性．本文对美国康普顿γ射线天文台观测卫星上BATSE仪器观测到的γ暴的光变曲线主峰数据进行统计分析，研究脉冲特征参量间的相关性．光变曲线的主峰按其形状分类，分为单峰结构峰和多峰结构峰．通过分析、比较两类峰特征的相关性发现：单峰结构的主峰其各种特征量的分布比多峰结构更为集中，这分明是由于多峰结构中存在着多个脉冲基元的随机叠加．因此，对于研究脉冲形态，采用单峰结构的主峰比采用多峰结构更为合理。     

A very energetic supernova associated with the gamma-ray burst of 29 March 2003

Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model.     

An optical supernova associated with the X-ray flash XRF 060218

Long-duration gamma-ray bursts (GRBs) are associated with type Ic supernovae that are more luminous than average and that eject material at very high velocities. Less-luminous supernovae were not hitherto known to be associated with GRBs, and therefore GRB-supernovae were thought to be rare events. Whether X-ray flashes--analogues of GRBs, but with lower luminosities and fewer gamma-rays--can also be associated with supernovae, and whether they are intrinsically 'weak' events or typical GRBs viewed off the axis of the burst, is unclear. Here we report the optical discovery and follow-up observations of the type Ic supernova SN 2006aj associated with X-ray flash XRF 060218. Supernova 2006aj is intrinsically less luminous than the GRB-supernovae, but more luminous than many supernovae not accompanied by a GRB. The ejecta velocities derived from our spectra are intermediate between these two groups, which is consistent with the weakness of both the GRB output and the supernova radio flux. Our data, combined with radio and X-ray observations, suggest that XRF 060218 is an intrinsically weak and soft event, rather than a classical GRB observed off-axis. This extends the GRB-supernova connection to X-ray flashes and fainter supernovae, implying a common origin. Events such as XRF 060218 are probably more numerous than GRB-supernovae.     

A new gamma-ray burst classification scheme from GRB 060614

Gamma-ray bursts (GRBs) are known to come in two duration classes, separated at approximately 2 s. Long-duration bursts originate from star-forming regions in galaxies, have accompanying supernovae when these are near enough to observe and are probably caused by massive-star collapsars. Recent observations show that short-duration bursts originate in regions within their host galaxies that have lower star-formation rates, consistent with binary neutron star or neutron star-black hole mergers. Moreover, although their hosts are predominantly nearby galaxies, no supernovae have been so far associated with short-duration GRBs. Here we report that the bright, nearby GRB 060614 does not fit into either class. Its approximately 102-s duration groups it with long-duration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short-duration GRBs. This combination of a long-duration event without an accompanying supernova poses a challenge to both the collapsar and the merging-neutron-star interpretations and opens the door to a new GRB classification scheme that straddles both long- and short-duration bursts.     

The bright optical afterglow of the nearby gamma-ray burst of 29 March 2003

Past studies of cosmological gamma-ray bursts (GRBs) have been hampered by their extreme distances, resulting in faint afterglows. A nearby GRB could potentially shed much light on the origin of these events, but GRBs with a redshift z 相似文献