Racusin 2011 Fermi和Swift暴的余辉统计

主要内容:
把这些暴拿过来一起统计，有多个量。

精彩摘抄:

统计的暴的来源数

上面是长暴，下面是短暴。 左边是X射线的，右边是u波段的光变曲线。

不同来源的暴的几率分布，可见BAT短暴明显分布于红移低的地方。

1天的时候x射线的光变指数和谱指数的分布

1天的时候光学波段的光变指数和谱指数的分布

不同时间不同来源的长暴的光度分布

对短暴（太少）

长暴和短暴各向同性能量的分布

各个量之间的关联的KS检验，值越小表明两个数据之间的差别越明显

（应该最大值是1，表明量数据完全相同）

暴的张角分布（不确定度很大），以及从而到处的实际光子能量

利用 11小时的时候X射线的光度所导出的动能（依赖于很多参数的方法）

和各向同性能量之间的统计关系

各参数值的范围

初始Lorentz因子的范围，采用了：gamma-gamma,t_peak,

ZP10, 2 zone-gamma gamma这四种方法

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· arXiv e-print (arXiv:1106.2469)

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Title:		Fermi and Swift Gamma-Ray Burst Afterglow Population Studies
Authors:		Racusin, J. L.; Oates, S. R.; Schady, P.; Burrows, D. N.; de Pasquale, M.; Donato, D.; Gehrels, N.;Koch, S.; McEnery, J.; Piran, T.; Roming, P.; Sakamoto, T.; Swenson, C.; Troja, E.; Vasileiou, V.;Virgili, F.; Wanderman, D.; Zhang, B.
Publication:		eprint arXiv:1106.2469
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		13 pages, 11 figures, Accepted for publication in ApJ
Bibliographic Code:		2011arXiv1106.2469R

Abstract

The new and extreme population of GRBs detected by Fermi-LAT shows several new features in high energy gamma-rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 6 years, it has been Swift that has provided the robust dataset of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT detected GRBs and the well studied, fainter, less energetic GRBs detected by Swift-BAT is only beginning to be explored by multi-wavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and Fermi-GBM, and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties, in order to better understand the nature of the special characteristics of the LAT bursts.

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Nakar 2011 shock breakout的动力学和辐射

主要内容:
计算光深tau=1的这层辐射作为breakout的辐射。
一个比较简单易懂的计算shock breakout的文章

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Title:		Relativistic shock breakouts - a variety of gamma-ray flares: from low luminosity gamma-ray bursts to type Ia supernovae
Authors:		Nakar, Ehud; Sari, Re'em
Publication:		eprint arXiv:1106.2556
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Bibliographic Code:		2011arXiv1106.2556N

Abstract

A large variety of explosions result in mildly or ultra relativistic shock breakouts. Here we calculate the luminosity and spectrum that these breakouts produce. In order to do so we improve an analytic description of relativistic radiation mediated shocks and follow the system from the breakout itself, through the planar phase and into the spherical phase. We limit our calculation to cases where the post breakout acceleration of the gas ends during the planar phase. (i.e., the final gas Lorentz factor <~30). We find that spherical relativistic breakouts produce a flash of gamma-rays with energy, temperature, and duration that always satisfy a specific relation between them as well as providing the breakout radius and Lorentz factor. The breakout flare is typically followed, on longer time scales, by X-rays that carry a comparable energy. We apply our model to a variety of explosions, including Ia and .Ia supernovae (SNe), AIC, energetic SNe and gamma-ray bursts (GRBs). We find that all these events produce detectable gamma-ray signals, some of which may have already been seen. Some particular examples are: (i) Relativistic shock breakouts provide a natural explanation to the energy, temperature and time scales, as well as many other observed features, of all low luminosity GRBs. (ii) Nearby broad-line Ib/c (like SN 2002ap) may produce a detectable gamma-ray signal. (iii) Galactic Ia SNe produce detectable gamma-ray flares, if their progenitors are single degenerate. We conclude that relativistic shock breakout is a generic process for the production of gamma-ray flares, which opens a new window for the study and detection of a variety of stellar explosions.

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Berger 2011 和SN 2009nz成协的GRB091127的观测

主要内容:
有一个比较确凿的成协的事例。现在主要有：

GRB 030329/SN 2003dh (z = 0.169; Hjorth et al.2003; Stanek et al. 2003), GRB 031203/SN 2003lw (z = 0.105; Malesani et al. 2004), XRF 060218/SN 2006aj(z = 0.033; Modjaz et al. 2006; Pian et al. 2006), and GRB 100316D/SN 2010bh (z = 0.059; Chornock et al. 2010).


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Title:		The Spectroscopic Classification and Explosion Properties of SN2009nz Associated with GRB091127 at z=0.490
Authors:		Berger, E.; Chornock, R.; Holmes, T. R.; Foley, R. J.; Cucchiara, A.; Wolf, C.; Podsiadlowski, Ph.;Fox, D. B.; Roth, K. C.
Publication:		eprint arXiv:1106.3073
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		Submitted to ApJ; 11 pages; 2 tables; 4 figures; emulateapj style
Bibliographic Code:		2011arXiv1106.3073B

Abstract

We present spectroscopic observations of GRB091127 (z=0.490) at the peak of the putative associated supernova, SN2009nz. Subtracting a late-time spectrum of the host galaxy, we isolate the contribution of SN2009nz and uncover broad features typical of nearby GRB-SNe. This establishes unambiguously that GRB091127 was accompanied by a broad-lined Type Ic SN, and links a cosmological long burst with a standard energy release (E_gamma,iso ~ 1.1e52 erg) to a massive star progenitor. The spectrum of SN2009nz closely resembles that of SN2006aj, with SN2003dh also providing an acceptable match, but has significantly narrower features than SNe 1998bw and 2010bh, indicative of a lower expansion velocity. The photospheric velocity inferred from the SiII 6355 absorption feature, v_ph ~ 17,000 km/s, is indeed closer to that of SNe 2006aj and 2003dh than to the other GRB-SNe. Combining the measured velocity with the light curve peak brightness and width, we estimate the following explosion parameters: M_Ni ~ 0.35 M_sun, E_K ~ 2.3e51 erg, and M_ej ~ 1.4 M_sun, similar to those of SN2006aj. These properties indicate that SN2009nz follows a trend of lower M_Ni for GRB-SNe with lower E_K and M_ej. Equally important, since GRB091127 is a typical cosmological burst, the similarity of SN2009nz to SN2006aj either casts doubt on the claim that XRF060218/SN2006aj was powered by a neutron star, or indicates that the nature of the central engine is encoded in the SN properties but not in the prompt emission. Future spectra of GRB-SNe at z > 0.3, including proper subtraction of the host galaxy contribution, will shed light on the full dispersion of SN properties for standard long GRBs, on the relation between SNe associated with sub-energetic and standard GRBs, and on a potential dispersion in the associated SN types.

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Dhillon 2011 首次看到了SGR 0501+4516的5.7秒的光学脉冲

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Title:		The first observation of optical pulsations from a soft gamma repeater: SGR 0501+4516
Authors:		Dhillon, V. S.; Marsh, T. R.; Littlefair, S. P.; Copperwheat, C. M.; Hickman, R. D. G.; Kerry, P.; Levan, A. J.; Rea, N.;Savoury, C. D. J.; Tanvir, N. R.; Turolla, R.; Wiersema, K.
Publication:		eprint arXiv:1106.1355
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - Solar and Stellar Astrophysics
Comment:		5 pages, 3 figures, accepted for publication in MNRAS Letters
Bibliographic Code:		2011arXiv1106.1355D

Abstract

We present high-speed optical photometry of the soft gamma repeater SGR 0501+4516, obtained with ULTRACAM on two consecutive nights approximately 4 months after the source was discovered via its gamma-ray bursts. We detect SGR 0501+4516 at a magnitude of i' = 24.4+/-0.1. We present the first measurement of optical pulsations from an SGR, deriving a period of 5.7622+/-0.0003 s, in excellent agreement with the X-ray spin period of the neutron star. We compare the morphologies of the optical pulse profile with the X-ray and infrared pulse profiles; we find that the optical, infrared and harder X-rays share similar double-peaked morphologies, but the softer X-rays exhibit only a single-peaked morphology, indicative of a different origin. The optical pulsations appear to be in phase with the X-ray pulsations and exhibit a root-mean-square pulsed fraction of 52+/-7%, approximately a factor of two greater than in the X-rays. Our results find a natural explanation within the context of the magnetar model for SGRs.

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