Burlon, D. 2009 BATSE前兆的谱

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与正常阶段的比较, 发现类似.

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Title:		Time resolved spectral behavior of bright BATSE precursors
Authors:		Burlon, D.; Ghirlanda, G.; Ghisellini, G.; Greiner, J.; Celotti, A.
Publication:		eprint arXiv:0907.5203
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		16 pages, 41 figures. Accepted in Astronomy and Astrophysics
Bibliographic Code:		2009arXiv0907.5203B

Abstract

Aims: Gamma Ray Bursts (GRBs) are sometimes preceded by dimmer emission episodes, called "precursors", whose nature is still a puzzle: they could either have the same origin as the main emission episode or they could be due to another mechanism. We investigate if precursors have some spectral distinctive feature with respect to the main GRB episodes. Methods: To this aim we compare the spectral evolution of the precursor with that of the main GRB event. We also study if and how the spectral parameters, and in particular the peak of the vFv spectrum of time resolved spectra, correlates with the flux. This allows us to test if the spectra of the precursor and of the main event belong to the same correlation (if any). We searched GRBs with precursor activity in the complete sample of 2704 bursts detected by BATSE finding that 12% of GRBs have one or more precursors. Among these we considered the bursts with time resolved spectral analysis performed by Kaneko et al. 2006, selecting those having at least two time resolved spectra for the precursor. Results: We find that precursors and main events have very similar spectral properties. The spectral evolution within precursors has similar trends as the spectral evolution observed in the subsequent peaks. Also the typical spectral parameters of the precursors are similar to those of the main GRB events. Moreover, in several cases we find that within the precursors the peak energy of the spectrum is correlated with the flux similarly to what happens in the main GRB event. This strongly favors models in which the precursor is due to the same fireball physics of the main emission episodes.

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Levesque, Emily M. 2009 几个z<1的伽玛暴的宿主星系的ISM

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Title:		The Host Galaxies of Gamma-Ray Bursts I: ISM Properties of Ten Nearby Long-Duration GRB Hosts
Authors:		Levesque, Emily M.; Berger, Edo; Kewley, Lisa J.; Bagley, Megan M.
Publication:		eprint arXiv:0907.4988
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - Galaxy Astrophysics
Comment:		27 pages, 19 figures, 5 tables, submitted to AJ
Bibliographic Code:		2009arXiv0907.4988L

Abstract

We present the first observations from a large-scale survey of nearby (z <> Bibtex entry for this abstract Preferred format for this abstract (see Preferences)

Galante, Nicola 2009 VERITAS的伽玛暴高能(>100GeV)的观测

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当然只有上限

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Title:		VERITAS Observation of Gamma-Ray Bursts
Authors:		Galante, Nicola; for the VERITAS Collaboration
Publication:		eprint arXiv:0907.4997
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		2 pages, 1 table, conference proceeding at the 31st ICRC, Lodz, Poland, 2009
Bibliographic Code:		2009arXiv0907.4997G

Abstract

During its first cycle of observations, VERITAS observed several GRBs in response to broadcast alerts from the Gamma-ray bursts Coordinates Network (GCN). The GRBs were followed up and observed thereafter with typical delays of 2 to 4 minutes from the beginning of the burst and of 92 s in the best case, searching for a very high energy (VHE) component above 100 GeV. The aim of the search for VHE emission from GRBs is to understand the behavior, composition and dynamics of the most accelerated particles in the bursts, as well as to get a better overall understanding of the model of GRBs. We report on the results from two years of observations by VERITAS.

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Page, K. L. 2009 GRB 080810的多波段观测

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详细

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Title:		Multi-wavelength observations of the energetic GRB 080810: detailed mapping of the broadband spectral evolution
Authors:		Page, K. L.; Willingale, R.; Bissaldi, E.; de Ugarte Postigo, A.; Holland, S. T.; McBreen, S.; O'Brien, P. T.; Osborne, J. P.; Prochaska, J. X.; Rol, E.; Rykoff, E. S.; Starling, R. L. C.; Tanvir, N. R.; van der Horst, A. J.; Wiersema, K.; Zhang, B.; Aceituno, F. J.; Akerlof, C.; Beardmore, A. P.; Briggs, M. S.; Burrows, D. N.; Castro-Tirado, A. J.; Connaughton, V.; Evans, P. A.; Fynbo, J. P. U.; Gehrels, N.; Guidorzi, C.; Howard, A. W.; Kennea, J. A.; Kouveliotou, C.; Pagani, C.; Preece, R.; Perley, D.; Yuan, F.
Publication:		eprint arXiv:0907.4578
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		15 pages, 9 figures, 4 in colour. Accepted for publication in MNRAS
Bibliographic Code:		2009arXiv0907.4578P

Abstract

GRB 080810 was one of the first bursts to trigger both Swift and the Fermi Gamma-ray Space Telescope. It was subsequently monitored over the X-ray and UV/optical bands by Swift, in the optical by ROTSE and a host of other telescopes and was detected in the radio by the VLA. The redshift of z= 3.355 +/- 0.005 was determined by Keck/HIRES and confirmed by RTT150 and NOT. The prompt gamma/X-ray emission, detected over 0.3-10^3 keV, systematically softens over time, with E_peak moving from ~600 keV at the start to ~40 keV around 100 s after the trigger; alternatively, this spectral evolution could be identified with the blackbody temperature of a quasithermal model shifting from ~60 keV to ~3 keV over the same time interval. The first optical detection was made at 38 s, but the smooth, featureless profile of the full optical coverage implies that this originated from the afterglow component, not the pulsed/flaring prompt emission. Broadband optical and X-ray coverage of the afterglow at the start of the final X-ray decay (~8 ks) reveals a spectral break between the optical and X-ray bands in the range 10^15 - 2x10^16 Hz. The decay profiles of the X-ray and optical bands show that this break initially migrates blueward to this frequency and then subsequently drifts redward to below the optical band by ~3x10^5 s. GRB 080810 was very energetic, with an isotropic energy output for the prompt component of 3x10^53 erg and 1.6x10^52 erg for the afterglow; there is no evidence for a jet break in the afterglow up to six days following the burst.

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Cardone, Vincenzo F. 2009 SN Ia+GRB限制引力模型

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实际上和限制宇宙学参数应该是一回事.

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Title:		Constraining f(R) theories with Type Ia Supernovae and Gamma Ray Bursts
Authors:		Cardone, Vincenzo F.; Diaferio, Antonaldo; Camera, Stefano
Publication:		eprint arXiv:0907.4689
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		14 pages, 5 figures, 2 tables, submitted to Physical Review D
Bibliographic Code:		2009arXiv0907.4689C

Abstract

Fourth - order gravity theories have received much interest in recent years thanks to their ability to provide an accelerated cosmic expansion in a matter only universe. In these theories, the Lagrangian density of the gravitational field has the form R + f(R), and the explicit choice of the arbitrary function f(R) must meet the local tests of gravity and the constraints from the primordial abundance of the light elements. Two popular classes of f(R) models, which are expected to fulfill all the above requirements, have recently been proposed. However, neither of these models has ever been quantitatively tested against the available astrophysical data. Here, by combining Type Ia Supernovae and Gamma Ray Bursts, we investigate the ability of these models to reproduce the observed Hubble diagram over the redshift range (0, 7). We find that both models fit very well this dataset with the present day values of the matter density and deceleration parameters which agree with previous estimates. However, the strong degeneracy among the f(R) parameters prevents us from putting strong constraints on the values of these parameters; nevertheless, we can identify the regions of the parameter space that should, in principle, be carefully explored with future data and dynamical probes in order to discriminate among f(R) theories and standard dark energy models.

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Perel'man, Mark E. 2009 暗暴可能是由于光学光子被bump到高能去了.

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(不过我不相信.)

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Title:		Dark gamma-ray bursts: possible role of multiphoton processes
Authors:		Perel'man, Mark E.
Publication:		eprint arXiv:0907.4613
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Quantum Physics
Comment:		4 pages
Bibliographic Code:		2009arXiv0907.4613P

Abstract

The absence of optical afterglow at some gamma-ray bursts (so called dark bursts) requires analyses of physical features of this phenomenon. It is shown that such singularity can be connected with multiphoton processes of frequencies summation in the Rayleigh- Jeans part of spectra, their pumping into higher frequencies. It can be registered most probably on young objects with still thin plasma coating, without further thermalization, i.e. soon after a prompt beginning of the explosive activity.

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Nardini, M. 2009 检查早期余辉中光学和X射线之间是否单一幂律

主要内容:
这需要先把X射线的低能段的谱指数找出来(比较难,因为有吸收). 然后和光学的观测比较, 看是否在这个谱指数的延伸上. 结果发现有些不是单一谱, 暗示光学和X射线可能来自不同的起源. 从而也是二者光变不一致的原因.

分析了好几个暴的谱.

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示意图

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Title:		Testing a new view of Gamma Ray Burst Afterglows
Authors:		Nardini, M.; Ghisellini, G.; Ghirlanda, G.; Celotti, A.
Publication:		eprint arXiv:0907.4157
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		12 pages, 11 figures, submitted to MNRAS
Bibliographic Code:		2009arXiv0907.4157N

Abstract

The optical and X-ray light-curves of long Gamma Ray Bursts (GRBs) often show a complex evolution and in most cases do not track each other. This behaviour can not be easily explained by the simplest standard afterglow models. A possible interpretation is to consider the observed optical and X-ray light-curves as the sum of two separate components. This scenario requires the presence of a spectral break between these bands. One of the aims of this work is to test whether such a break is present within the observed Swift XRT energy range. We analyse the X-ray afterglow spectra of a sample of 33 long GRBs with known redshift, good optical photometry and published estimate of the host galaxy dust absorption A_V(host). We find that indeed in 7 bright events a broken power-law provides a fit to the data that is better than a single power-law model. For 8 events, instead, the X-ray spectrum is better fitted by a single power-law. We discuss the role of these breaks in connection to the relation between the host hydrogen column density N_H(host) and A_V(host) and check the consistency of the X-ray spectral breaks with the optical bands photometry. We analyse the optical to X-ray spectral energy distributions at different times and find again consistency with two components interpretation.

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Xue, R. R. 2009 近处伽玛暴的超高能射线

主要内容:
远的由于和红外背景光子散射不能到达地球, 估算了近的, 大多也在Cherenkov探测器的阈值以下.

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Title:		Very High Energy Gamma-ray Afterglow Emission of Nearby Gamma-ray Bursts
Authors:		Xue, R. R.; Tam, P. H.; Wagner, S. J.; Behera, B.; Fan, Y. Z.; Wei, D. M.
Publication:		eprint arXiv:0907.4014
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		9 pages,5 figure,2 tables,accepted for publication in ApJ
Bibliographic Code:		2009arXiv0907.4014X

Abstract

The synchrotron self-Compton (SSC) emission from Gamma-ray Burst (GRB) forward shock can extend to the very-high-energy (VHE; $E_\gamma > $100 GeV) range. Such high energy photons are rare and are attenuated by the cosmic infrared background before reaching us. In this work, we discuss the prospect to detect these VHE photons using the current ground-based Cherenkov detectors. Our calculated results are consistent with the upper limits obtained with several Cherenkov detectors for GRB 030329, GRB 050509B, and GRB 060505 during the afterglow phase. For 5 bursts in our nearby GRB sample (except for GRB 030329), current ground-based Cherenkov detectors would not be expected to detect the modeled VHE signal. Only for those very bright and nearby bursts like GRB 030329, detection of VHE photons is possible under favorable observing conditions and a delayed observation time of $\la$10 hours.

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Fynbo, J. P. U. 2009 77个余辉的谱

主要内容:
列出了77个Swift的有谱观测暴的谱, 包括谱线的图.数据量大(共170页).

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Title:		Low-Resolution Spectroscopy of Gamma-ray Burst Optical Afterglows: Biases in the Swift Sample and Characterization of the Absorbers
Authors:		Fynbo, J. P. U.; Jakobsson, P.; Prochaska, J. X.; Malesani, D.; Ledoux, C.; de Ugarte Postigo, A.; Nardini, M.; Vreeswijk, P. M.; Hjorth, J.; Sollerman, J.; Chen, H. -W.; Thoene, C. C.; Bjoernsson, G.; Bloom, J. S.; Castro-Tirado, A.; Christensen, L.; De Cia, A.; Gorosabel, J. U.; Jaunsen, A.; Jensen, B. L.; Levan, A.; Maund, J.; Masetti, N.; Milvang-Jensen, B.; Palazzi, E.; Perley, D. A.; Pian, E.; Rol, E.; Schady, P.; Starling, R.; Tanvir, N.; Watson, D. J.; Wiersema, K.; Xu, D.; Augusteijn, T.; Grundahl, F.; Telting, J.; Quirion, P. -O.
Publication:		eprint arXiv:0907.3449
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		170 pages, 15 figures. Submitted to ApJS. A full resolution version of the paper can be found here: http://www.astro.ku.dk/~jfynbo/grb_lowres.pdf. Comments very welcome
Bibliographic Code:		2009arXiv0907.3449F

Abstract

(Abridged). We present a sample of 77 optical afterglows (OAs) of Swift detected GRBs for which spectroscopic follow-up observations have been secured. We provide linelists and equivalent widths for all detected lines redward of Ly-alpha. We discuss to what extent the current sample of Swift bursts with OA spectroscopy is a biased subsample of all Swift detected GRBs. For that purpose we define an X-ray selected sample of Swift bursts with optimal conditions for ground-based follow up from the period March 2005 to September 2008; 146 bursts fulfill our sample criteria. We derive the redshift distribution for this sample and conclude that less than 19% of Swift bursts are at z>7. We compare the high energy properties for three sub-samples of bursts in the sample: i) bursts with redshifts measured from OA spectroscopy, ii) bursts with detected OA, but no OA-based redshift, and iii) bursts with no detection of the OA. The bursts in group i) have significantly less excess X-ray absorption than bursts in the other two groups. In addition, the fraction of dark bursts is 14% in group i), 38% in group ii) and > 39% in group iii). From this we conclude that the sample of GRBs with OA spectroscopy is not representative for all Swift bursts, most likely due to a bias against the most dusty sight-lines. Finally, we characterize GRB absorption systems as a class and compare them to QSO absorption systems, in particular DLAs. On average GRB absorbers are characterized by significantly stronger EWs for HI as well as for both low and high ionization metal lines than what is seen in intervening QSO absorbers. Based on the z>2 bursts in the sample we place a 95% confidence upper limit of 7.5% on the mean escape fraction of ionizing photons from star-forming galaxies.

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Stamatikos, Michael 2009 Swift-BAT and Fermi-GBM的联合谱分析

主要内容:
并分析了两个暴 : GRBs 080804 and 080810

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Title:		The Cross-Calibration of Swift-BAT and Fermi-GBM via Correlative Spectral Analysis of GRBs
Authors:		Stamatikos, Michael
Publication:		eprint arXiv:0907.3190
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Comment:		4 pages, 6 figures. Contributed to the Proceedings of Frontiers of Space Astrophysics, Neutron Stars and Gamma Ray Bursts: Recent Developments and Future Directions
Bibliographic Code:		2009arXiv0907.3190S

Abstract

We report on recent inter-calibration studies featuring Swift's Burst Alert Telescope (BAT) and Fermi's Gamma-ray Burst Monitor (GBM) based upon correlated observations of GRBs 080804 and 080810, via their resultant joint spectral analysis. Swift's intrinsic multi-wavelength instrumentation and dynamical response complement Fermi's superior energy range. The addition of BAT's spectral response will (i) facilitate in-orbit GBM detector response calibration, (ii) augment Fermi's low energy sensitivity, (iii) enable ground-based follow-up efforts of Fermi GRBs, and (iv) help identify a subset of GRBs discovered via off-line GBM data analysis, for an annual estimate of ~30 GRBs. The synergy of BAT and GBM augments previous successful joint spectral fit efforts by enabling the study of peak photon energies (Epeak), while leveraging the over eleven energy decades afforded by Fermi's Large Area Telescope (LAT), in conjunction with Swift's X-Ray (XRT) and Ultraviolet-Optical (UVOT) Telescopes, for an unprecedented probe of broad-band spectral and temporal evolution, throughout their contemporaneous orbital tenure over the next decade.

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Xiong 2009 Monte Carlo模拟 POLAR的观测

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Title:		Expected performance of a hard X-ray polarimeter (POLAR) by Monte Carlo simulation
Authors:		Xiong, Shaolin; Produit, Nicolas; Wu, Bobing
Affiliation:		AA(Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, China), AB(ISDC, Université de Genève, Switzerland), AC(Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, China)
Publication:		Nuclear Instruments and Methods in Physics Research Section A, Volume 606, Issue 3, p. 552-559.
Publication Date:		07/2009
Origin:		ELSEVIER
Abstract Copyright:		Elsevier B.V.
DOI:		10.1016/j.nima.2009.04.033
Bibliographic Code:		2009NIMPA.606..552X

Abstract

Polarization measurements of the prompt emission in gamma-ray bursts (GRBs) can provide diagnostic information for understanding the nature of the central engine. POLAR is a compact polarimeter dedicated to the polarization measurement of GRBs between 50 and 300 keV and is scheduled to be launched aboard the Chinese Space Laboratory around the year 2012. A preliminary Monte Carlo simulation has been accomplished to model the expected performance of POLAR while a prototype of POLAR is being constructed. The modulation factor, efficiency and effective area, background rates and minimum detectable polarization (MDP) were calculated for different detector configurations and trigger strategies. With the optimized detector configuration and trigger strategy and the total weight constraint of less than 30 kg, the primary science goal to determine whether most GRBs are strongly polarized can be achieved, and about 9 GRBs/yr can be detected with an MDP<10%> Bibtex entry for this abstract Preferred format for this abstract (see Preferences)

Dong, Yongwei 2009 POLAR的聚光能力

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Title:		Light collection of POLAR detector
Authors:		Dong, Yongwei; Li, Yanguo; Wu, Bobing; Zhang, Yongjie; Zhang, Shuangnan
Publication:		eprint arXiv:0907.2771
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - Instrumentation and Methods for Astrophysics
Comment:		5 pages, accepted by Sci China Ser G-Phys Mech Astron. 2009
Bibliographic Code:		2009arXiv0907.2771D

Abstract

POLAR is a compact polarimeter dedicated to measure the polarization of GRBs between 50-300 keV. The light collection of 200*6*6mm3 plastic bars has been simulated and optimized in order to get uniform response to x-rays at different points of one single bar. According to the Monte Carlo results, the amplitude uniformity strongly depends on the polishing level of scintillator surface and the covering. A uniformity of 89% is achieved with a prototype constructed by a non position-sensitive PMT and an array of 4X4 bars.

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Esposito, P. 2009 SGR 1627-41的spin-down rate和磁场强度

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Title:		Spin-down rate and inferred dipole magnetic field of the soft gamma-ray repeater SGR 1627-41
Authors:		Esposito, P.; Burgay, M.; Possenti, A.; Turolla, R.; Zane, S.; De Luca, A.; Tiengo, A.; Israel, G. L.; Mattana, F.; Mereghetti, S.; Bailes, M.; Romano, P.; Götz, D.; Rea, N.
Publication:		eprint arXiv:0907.2873
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		5 pages, 2 figures; accepted for publication in MNRAS Letters
Bibliographic Code:		2009arXiv0907.2873E

Abstract

Using Chandra data taken on 2008 June, we detected pulsations at 2.59439(4) s in the soft gamma-ray repeater SGR 1627-41. This is the second measurement of the source spin period and allows us to derive for the first time a long-term spin-down rate of (1.9 +/- 0.4)E-11 s/s. From this value we infer for SGR 1627-41 a characteristic age of 2.2 kyr, a spin-down luminosity of 4E+34 erg/s (one of the highest among sources of the same class), and a surface dipole magnetic field strength of 2E+14 G. These properties confirm the magnetar nature of SGR 1627-41; however, they should be considered with caution since they were derived on the basis of a period derivative measurement made using two epochs only and magnetar spin-down rates are generally highly variable. The pulse profile, double-peaked and with a pulsed fraction of (13 +/- 2)% in the 2-10 keV range, closely resembles that observed by XMM-Newton in 2008 September. Having for the first time a timing model for this SGR, we also searched for a pulsed signal in archival radio data collected with the Parkes radio telescope nine months after the previous X-ray outburst. No evidence for radio pulsations was found, down to a luminosity level 10-20 times fainter (for a 10% duty cycle and a distance of 11 kpc) than the peak luminosity shown by the known radio magnetars.

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Hurley, K. 2009 IPN对伽玛暴的定位catalog

主要内容:
2000-2006年间的154个暴.

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Title:		The Interplanetary Network Supplement to the HETE-2 Gamma-Ray Burst Catalog
Authors:		Hurley, K.; Atteia, J. -L.; Barraud, C.; Pelangeon, A.; Boer, M.; Vanderspek, R.; Ricker, G.; Mazets, E.; Golenetskii, S.; Frederiks, D. D.; Pal'shin, V. D.; Aptekar, R. L.; Smith, D. M.; Wigger, C.; Hajdas, W.; Rau, A.; von Kienlin, A.; Mitrofanov, I. G.; Golovin, D. V.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.; Boynton, W.; Fellows, C.; Barthelmy, K. Harshman S.; Cline, T.; Cummings, J.; Gehrels, N.; Krimm, H.; Yamaoka, K.; Ohno, M.; Fukazawa, Y.; Hanabata, Y.; Takahashi, T.; Tashiro, M.; Terada, Y.; Murakami, T.; Makishima, K.; Guidorzi, C.; Frontera, F.; Montanari, C. E.; Rossi, F.; Trombka, J.; McClanahan, T.; Goldsten, R. Starr J.; Gold, R.
Publication:		eprint arXiv:0907.2709
Publication Date:		07/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		37 pages, 3 figures. To be submitted to ApJSS. Table 5 was truncated in the original version, and has been replaced
Bibliographic Code:		2009arXiv0907.2709H

Abstract

Between 2000 November and 2006 May, one or more spacecraft of the interplanetary network (IPN) detected 226 cosmic gamma-ray bursts that were also detected by the FREGATE experiment aboard the HETE-II spacecraft. During this period, the IPN consisted of up to nine spacecraft, and using triangulation, the localizations of 154 bursts were obtained. We present the IPN localization data on these events.

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