Chen et al UFFO望远镜系列文章

主要内容:
UFFO (Ultra Fast Flash Observatory)是俄罗斯的望远镜，放在Lomonosov卫星上，2011年11月上天。主要包含两个仪器：UBAT发现暴的，SMT观测UV和光学余辉的。主要目的就是观测早期的光学余辉，因为SMT只要一秒钟就转过去了。

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Title:		The UFFO (Ultra Fast Flash Observatory) Pathfinder: Science and Mission
Authors:		Chen, P.; Ahmad, S.; Ahn, K.; Barrillon, P.; Blin-Bondil, S.; Brandt, S.; Budtz-Jorgensen, C.; Castro-Tirado, A. J.; Choi, H. S.; Choi, Y. J.; Connell, P.; Dagoret-Campagne, S.; De La Taille, C.;Eyles, C.; Grossan, B.; Hermann, I.; Huang, M. -H. A.; Jeong, S.; Jung, A.; Kim, J. E.; Kim, S. H.;Kim, Y. W.; Lee, J.; Lim, H.; Linder, E. V.; Liu, T. -C.; Lund, Niels; Min, K. W.; Na, G. W.;Nam, J. W.; Nam, K.; Panayuk, M. I.; Park, I. H.; Re-Glero, V.; Rodrigo, J. M.; Smoot, G. F.;Suh, Y. D.; Svelitov, S.; Vedenken, N.; Wang, M. -Z; Yashin, I.; Zhao, M. H.
Publication:		eprint arXiv:1106.3929
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Comment:		4 pages, 5 figures, to appear in the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011
Bibliographic Code:		2011arXiv1106.3929C

Abstract

Hundreds of gamma-ray burst (GRB) optical light curves have been measured since the discovery of optical afterglows. However, even after nearly 7 years of operation of the Swift Observatory, only a handful of measurements have been made soon (within a minute) after the gamma ray signal. This lack of early observations fails to address burst physics at short time scales associated with prompt emissions and progenitors. Because of this lack of sub-minute data, the characteristics of the rise phase of optical light curve of short-hard type GRB and rapid-rising GRB, which may account for ~30% of all GRB, remain practically unknown. We have developed methods for reaching sub-minute and sub-second timescales in a small spacecraft observatory. Rather than slewing the entire spacecraft to aim the optical instrument at the GRB position, we use rapidly moving mirror to redirect our optical beam. As a first step, we employ motorized slewing mirror telescope (SMT), which can point to the event within 1s, in the UFFO Pathfinder GRB Telescope onboard the Lomonosov satellite to be launched in Nov. 2011. UFFO's sub-minute measurements of the optical emission of dozens of GRB each year will result in a more rigorous test of current internal shock models, probe the extremes of bulk Lorentz factors, provide the first early and detailed measurements of fast-rise GRB optical light curves, and help verify the prospect of GRB as a new standard candle. We will describe the science and the mission of the current UFFO Pathfinder project, and our plan of a full-scale UFFO-100 as the next step.

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Bibtex entry for this abstract   Preferred format for this abstract (see Preferences) · Find Similar Abstracts (with default settings below) · arXiv e-print (arXiv:1106.3850) · References in the Article · Also-Read Articles (Reads History) · · Translate This Page Title: Optical Performances of Slewing Mirror Telescope for UFFO-Pathfinder Authors: Jeong, S.; Ahn, K. -B.; Nam, J. W.; Park, I. H.; Kim, S. -W.; Choi, H. S.; Grossan, B.; Hermann, I.;Jung, A.; Kim, Y. W.; Kim, J. E.; Linder, E. V.; Lee, J.; Lim, H.; Min, K. W.; Na, G. W.; Nam, K. H.;Panasyuk, M. I.; Smoot, G. F.; Svertilov, S.; Suh, Y. D.; Vedenkin, N.; Yashin, I.; Zhao, M. H.;For the UFFO collaboration Publication: eprint arXiv:1106.3850 Publication Date: 06/2011 Origin: ARXIV Keywords: Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics Comment: 4 pages, 6 figures, proceeding paper for the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011 Bibliographic Code: 2011arXiv1106.3850J Abstract The Ultra-Fast Flash Observatory-Pathfinder (UFFO-P) is to be launched onboard Lomonosov spacecraft in November 2011. It is to measure early UV/Optical photons from Gamma Ray Bursts (GRBs). Slewing Mirror Telescope (SMT) is one of two instruments designed for detection of UV/Optical images of the GRBs. SMT is a Ritchey-Chr\'etien telescope of 100 mm in diameter with a motorized slewing mirror at the entrance providing 17\times17 arcmin2 in Field of View (FOV) and 4 arcsec in pixel resolution. Its sky coverage can be further expanded up to 35 degrees in FOV by tilting a motorized slewing mirror. All mirrors were fabricated to about RMS 0.02 waves in wave front error (WFE) and 84.7% (in average reflectivity) over 200nm~650nm range. SMT was aligned to RMS 0.05 waves in WFE (test wavelength 632.8nm). From the static gravity test result, SMT optics system is expected to survive during launch. The technical details of SMT assembly and laboratory performance test results are reported. Bibtex entry for this abstract   Preferred format for this abstract (see Preferences) · Find Similar Abstracts (with default settings below) · arXiv e-print (arXiv:1106.3804) · Also-Read Articles (Reads History) · · Translate This Page Title: Data Acquisition System for the UFFO Pathfinder Authors: Na, G. W.; Ahn, K. -B.; Choi, H. S.; Choi, Y. J.; Grossan, B.; Hermann, I.; Jeong, S.; Jung, A.;Kim, J. E.; Kim, S. -W.; Kim, Y. W.; Lee, J.; Lim, H.; Linder, E. V.; Min, K. W.; Nam, J. W.;Nam, K. H.; Panasyuk, M. I.; Park, I. H.; Smoot, G. F.; Suh, Y. D.; Svertilov, S.; Vedenkin, N.;Yashin, I.; Zhao, M. H.; For The Uffo Collaboration Publication: eprint arXiv:1106.3804 Publication Date: 06/2011 Origin: ARXIV Keywords: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics, Physics - Instrumentation and Detectors Comment: 4 pages, 7 figures, 2 tables, proceeding paper for the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011 Bibliographic Code: 2011arXiv1106.3804N Abstract The Ultra-Fast Flash Observatory (UFFO) Pathfinder is a payload on the Russian Lomonosov satellite, scheduled to be launched in November 2011. The Observatory is designed to detect early UV/Optical photons from Gamma-Ray Bursts (GRBs). There are two telescopes and one main data acquisition system: the UFFO Burst Alert & Trigger Telescope (UBAT), the Slewing Mirror Telescope (SMT), and the UFFO Data Acquisition (UDAQ) system. The UDAQ controls and manages the operation and communication of each telescope, and is also in charge of the interface with the satellite. It will write the data taken by each telescope to the NOR flash memory and sends them to the satellite via the Bus-Interface system (BI). It also receives data from the satellite including the coordinates and time of an external trigger from another payload, and distributes them to two telescopes. These functions are implemented in field programmable gates arrays (FPGA) for low power consumption and fast processing without a microprocessor. The UDAQ architecture, control of the system, and data flow will be presented. Bibtex entry for this abstract   Preferred format for this abstract (see Preferences) · Find Similar Abstracts (with default settings below) · arXiv e-print (arXiv:1106.3803) · Also-Read Articles (Reads History) · · Translate This Page Title: Implementation of the readout system in the UFFO Slewing Mirror Telescope Authors: Kim, J. E.; Lim, H.; Jung, A.; Ahn, K. -B; Choi, H. S.; Choi, Y. J.; Grossan, B.; Hermann, I.;Jeong, S.; Kim, S. -W.; Kim, Y. W.; Lee, J.; Linder, E. V.; Min, K. W.; Na, G. W.; Nam, J. W.;Nam, K. H.; Panayuk, M. I.; Park, I. H.; Smoot, G. F.; Suh, Y. D.; Svelitov, S.; Vedenken, N.;Yashin, I.; Zhao, M. H.; For The Uffo Collaboration Publication: eprint arXiv:1106.3803 Publication Date: 06/2011 Origin: ARXIV Keywords: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics, Physics - Instrumentation and Detectors Bibliographic Code: 2011arXiv1106.3803K Abstract The Ultra-Fast Flash Observatory (UFFO) is a new space-based experiment to observe Gamma-Ray Bursts (GRBs). GRBs are the most luminous electromagnetic events in the universe and occur randomly in any direction. Therefore the UFFO consists of two telescopes; UFFO Burst Alert & Trigger Telescope (UBAT) to detect GRBs using a wide field-of-view (FOV), and a Slewing Mirror Telescope (SMT) to observe UV/optical events rapidly within the narrow, targeted FOV. The SMT is a Ritchey-Chretien telescope that uses a motorized mirror system and an Intensified Charge-Coupled Device (ICCD). When the GRB is triggered by the UBAT, the SMT receives the position information and rapidly tilts the mirror to the target. The ICCD start to take the data within a second after GRB is triggered. Here we give the details about the SMT readout electronics that deliver the data. Bibtex entry for this abstract   Preferred format for this abstract (see Preferences) · Find Similar Abstracts (with default settings below) · arXiv e-print (arXiv:1106.3802) · References in the Article · Also-Read Articles (Reads History) · · Translate This Page Title: Design and Fabrication of Detector Module for UFFO Burst Alert & Trigger Telescope Authors: Jung, A.; Ahmad, S.; Ahn, K. -B.; Barrillon, P.; Blin-Bondil, S.; Brandt, S.; Budtz-JØRgensen, C.;CaStro-Tirado, A. J.; Chen, P.; Choi, H. S.; Choi, Y. J.; Connell, P.; Dagoret-Campagne, S.;De La Taille, C.; Eyles, C.; Grossan, B.; Hermann, I.; Huang, M. -H. A.; Jeong, S.; Kim, J. E.;Kim, S. -W.; Kim, Y. W.; Lee, J.; Lim, H.; Linder, E. V.; Liu, T. -C.; Lund, N.; Min, K. W.; Na, G. W.;Nam, J. W.; Nam, K. H.; Panasyuk, M. I.; Park, I. H.; Reglero, V.; Rodrigo, J. M.; Smoot, G. F.;Suh, Y. D.; Svertilov, S.; Vedenkin, N.; Wang, M. -Z; Yashin, I.; Zhao, M. H.;For The Uffo Collaboration Publication: eprint arXiv:1106.3802 Publication Date: 06/2011 Origin: ARXIV Keywords: Astrophysics - Cosmology and Extragalactic Astrophysics Comment: 4 pages, 7 figures, 3 tables, ICRC conference proceeding paper; Beijing, August 11-18, 2011 Bibliographic Code: 2011arXiv1106.3802J Abstract The Ultra-Fast Flash Observatory (UFFO) pathfinder is a space mission devoted to the measurement of Gamma-Ray Bursts (GRBs), especially their early light curves which will give crucial information on the progenitor stars and central engines of the GRBs. It consists of two instruments: the UFFO Burst Alert & Trigger telescope (UBAT) for the detection of GRB locations and the Slewing Mirror Telescope (SMT) for the UV/optical afterglow observations, upon triggering by UBAT. The UBAT employs a coded-mask {\gamma}/X-ray camera with a wide field of view (FOV), and is comprised of three parts: a coded mask, a hopper, and a detector module (DM). The UBAT DM consists of a LYSO scintillator crystal array, multi-anode photo multipliers, and analog and digital readout electronics. We present here the design and fabrication of the UBAT DM, as well as its preliminary test results. Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Domainko 2011 球状星团Terzan 5中的VHE可能是伽马暴遗迹

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Title:		Finding short GRB remnants in globular clusters: the VHE gamma-ray source in Terzan 5
Authors:		Domainko, Wilfried F.
Publication:		eprint arXiv:1106.4397
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		4 pages, submitted, comments welcome
Bibliographic Code:		2011arXiv1106.4397D

Abstract

Globular cluster are believed to boost the rate of compact binary mergers which may launch a certain type of cosmological gamma-ray bursts (GRBs). Therefore globular clusters appear to be potential sites to search for remnants of such GRBs. The very-high-energy (VHE) gamma-ray source HESS J1747-248 recently discovered in the direction of the Galactic globular cluster Terzan 5 is investigated for being a GRB remnant. Signatures created by the ultra-relativistic outflow, the sub-relativistic ejecta and the ionizing radiation of a short GRB are estimated for an expected age of such a remnant of t > 10^4 years. The kinetic energy of a short GRB could roughly be adequate to power the VHE source in a hadronic scenario. The age of the proposed remnant estimated from its extension possibly agrees with the occurrence of such events in the Galaxy. Sub-relativistic merger ejecta could shock-heat the ambient medium. Further VHE observations can probe the presence of a break towards lower energies expected for particle acceleration in ultra-relativistic shocks. Deep X-ray observations would have the potential to examine the presence of thermal plasma heated by the sub-relativistic ejecta. The identification of a GRB remnant in our own Galaxy may also help to explore the effect of such a highly energetic event on the Earth.

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Stratta 2011 GRB 050904的路上尘埃

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Title:		Is GRB 050904 at z=6.3 absorbed by dust?
Authors:		Stratta, G.; Gallerani, S.; Maiolino, R.
Publication:		eprint arXiv:1106.4441
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		8 pages, 3 figures, accepted for publication in Astronomy and Astrophysics; figure 1 has been degraded, full resolution version at http://dl.dropbox.com/u/1670579/fig01.ps
Bibliographic Code:		2011arXiv1106.4441S

Abstract

Claim of dust extinction for this GRB has been debated in the past. We suggest that the discrepant results occur primarily because most of previous studies have not simultaneously investigated the X-ray to near-IR spectral energy distribution of this GRB. The difficulty with this burst is that the X-ray afterglow is dominated by strong flares at early times and is poorly monitored at late times. In addition, the Z band photometry, which is the most sensitive to dust extinction, has been found to be affected by strong systematics. In this paper we carefully re-analyze the Swift/XRT afterglow observations of this GRB, using extensive past studies of X-ray flare properties when computing the X-ray afterglow flux level and exploiting the recent reanalysis of the optical (UV rest frame) data of the same GRB. We extract the X-ray to optical/near-IR afterglow SED for the three epochs where the best spectral coverage is available: 0.47, 1.25, and 3.4 days after the trigger. A spectral power-law model has been fitted to the extracted SEDs. We discuss that no spectral breaks or chromatic temporal breaks are expected in the epochs of interest. To fit any UV rest-frame dust absorption, we tested the Small Magellanic Cloud (SMC) extinction curve, the mean extinction curve (MEC) found for a sample of QSO at $z>4$ and its corresponding attenuation curve, as well as a starburst attenuation curve, and the extinction curve consistent with a supernova dust origin (SN-type). The SMC extinction curve and the SN-type one provide good fit to the data at all epochs, with an average amount of dust absorption at $\lambda_{rest} = 3000 \AA$ of $A_{3000} = 0.25\pm 0.07$ mag. These results indicate that the primeval galaxy at $z = 6.3$ hosting this GRB has already enriched its ISM with dust.

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Bucciantini 2011 部分有延展辐射的短暴可能是磁星

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考虑这种磁星起源的喷流及其准直。

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Title:		Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation
Authors:		Bucciantini, N.; Metzger, B. D.; Thompson, T. A.; Quataert, E.
Publication:		eprint arXiv:1106.4668
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		10 pages, 5 figures, submitted to MNRAS
Bibliographic Code:		2011arXiv1106.4668B

Abstract

Approximately 1/4-1/2 of short duration Gamma-Ray Bursts are followed by variable X-ray emission lasting ~ 100 s with a fluence comparable or exceeding that of the initial burst itself. The long duration and significant energy of this `extended emission'(EE) poses a major challenge to the standard binary neutron star merger model. metzger08 recently proposed that the EE is powered by the spin-down of a strongly magnetized neutron star. However, the effects of surrounding material on the magnetar outflow have not yet been considered. Here we present time-dependent axisymmetric relativistic magnetohydrodynamic simulations of the interaction of the relativistic proto-magnetar wind with a surrounding 10^-1 10^-3 M_\odot envelope, which represents material ejected during the merger; the supernova following AIC; or via outflows from the accretion disk. The collision between the relativistic magnetar wind and the expanding ejecta produces a magnetized nebula inside the ejecta. A strong toroidal magnetic field builds up in the nebula, which drives a bipolar jet out through the ejecta, similar to the magnetar model developed in the case of long duration GRBs. We quantify the `break-out' time and opening angle of the jet theta_j as a function of the wind energy flux dot{E} and ejecta mass M_ej. We show that dot{E} and theta_j are inversely correlated, such that the beaming-corrected (isotropic) luminosity of the jet is primarily a function of M_ej. Both variability arguments, and the lower limit on the power of magnetar outflows capable of producing bright emission, suggest that the true opening angle of the magnetar jet must be relatively large. The model thus predicts a class of events for which the EE is observable with no associated short GRB. These may appear as long-duration GRBs or X-Ray Flashes, which may be detected by future all-sky X-ray survey missions.

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Gräfener 2011 WR星的星风的质量损失的Eddington因子

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Title:		The Eddington factor as the key to understand the winds of the most massive stars. Evidence for a Gamma-dependence of Wolf-Rayet type mass loss
Authors:		Gräfener, G.; Vink, J. S.; de Koter, A.; Langer, N.
Publication:		eprint arXiv:1106.5361
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - Solar and Stellar Astrophysics
Bibliographic Code:		2011arXiv1106.5361G

Abstract

The most massive stars are thought to be hydrogen-rich Wolf-Rayet stars of late spectral subtype (WNh stars). In previous theoretical studies the enhanced mass loss of these stars has been attributed to their proximity to the Eddington limit. Here we investigate observed trends in the mass-loss properties of such young, very massive stars. We derive theoretical mass-luminosity relations for very massive stars, based on a large grid of stellar structure models. Using these relations, we estimate Eddington factors for a sample of stars, under different assumptions of their evolutionary status. We evaluate the resulting mass-loss relations, and compare them with theoretical predictions. We find observational evidence that the mass loss in the WR regime is dominated by the Eddington parameter Gamma_e, which has important consequences for the way we understand Wolf-Rayet stars and their mass loss. In addition, we derive wind masses that support the picture that the WNh stars in young stellar clusters are very massive, hydrogen-burning stars. Our findings suggest that the proximity to the Eddington limit is the physical reason for the onset of Wolf-Rayet type mass loss. This means that, e.g. in stellar evolution models, the Wolf-Rayet stage should be identified by large Eddington parameters, instead of a helium-enriched surface composition. The latter is most likely only a consequence of strong mass loss, in combination with internal mixing. For very massive stars, the enhanced Gamma-dependent mass loss is responsible for the formation of late WNh subtypes with high hydrogen surface abundances, partly close to solar. Because mass loss dominates the evolution of very massive stars, we expect a strong impact of this effect on their end products, in particular on the potential formation of black holes, and Gamma-Ray Bursts, as well as the observed upper mass limit of stars.

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Scholz 2011 磁星1E 1547-5408在2009年的爆发

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Title:		The 2009 outburst of magnetar 1E 1547-5408: Persistent radiative and burst properties
Authors:		Scholz, Paul; Kaspi, Victoria M.
Publication:		eprint arXiv:1106.5445
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		10 pages, 9 figures. Accepted for publication in ApJ
Bibliographic Code:		2011arXiv1106.5445S

Abstract

The magnetar 1E~1547$-$5408 recently exhibited two periods of outburst, beginning on 2008 October 3 and 2009 January 22. Here we present an analysis of the persistent radiative evolution and a statistical study of the burst properties during the 2009 outburst using the {\em Swift} X-ray Telescope (XRT). We find that the 1--10 keV flux increased by a factor of $\sim500$ and hardened significantly, peaking $\sim6$ hours after the onset of the outburst. The pulsed fraction decreased to zero at the peak of the outburst, exhibiting an anti-correlation with phase-averaged flux. Properties of the several hundred X-ray bursts during the 2009 outburst were determined and compared to tho from other magnetar outburst events. We find that the peaks of the bursts occur randomly in phase but that the folded counts that compose the bursts exhibit a pulse which is misaligned with the persistent pulse phase. We also report a correlation between burst hardness and flux. We compare the hardness-flux evolution of the persistent emission of both outbursts to those from other magnetars and find that although there does exist an overall trend, the degree of hardening for a given increase in flux is not uniform from source to source. These results are discussed in the context of previous results and within the magnetar model.

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Tsutsui 2011 Ep-TL-Lp之间的统计关系

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企图用于作为标准烛光关系，不过很多outliers。

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Title:		The Improved Ep-TL-Lp Diagram and a Robust Regression Method
Authors:		Tsutsui, Ryo; Nakamura, Takashi; Yonetoku, Daisuke; Murakami, Toshio; Morihara, Yoshiyuki;Takahashi, Keitaro
Publication:		eprint arXiv:1106.5373
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		24 pages, 7 figures, accepted for publication in PASJ
Bibliographic Code:		2011arXiv1106.5373T

Abstract

The accuracy and reliability of gamma-ray bursts (GRBs) as distance indicators are strongly restricted by their systematic errors which are larger than statistical errors. These systematic errors might come from either intrinsic variations of GRBs, or systematic errors in observations. In this paper, we consider the possible origins of systematic errors in the following observables, (i) the spectral peak energies (Ep) estimated by Cut-off power law (CPL) function, (ii) the peak luminosities (Lp) estimated by 1 second in observer time. Removing or correcting them, we reveal the true intrinsic variation of the Ep-TL-Lp relation of GRBs. Here TL is the third parameter of GRBs defined as TL ~ Eiso / Lp. Not only the time resolution of Lp is converted from observer time to GRB rest frame time, the time resolution with the largest likelihood is sought for. After removing obvious origin of systematic errors in observation mentioned above, there seems to be still remain some outliers. For this reason, we take account another origin of the systematic error as below, (iii) the contamination of short GRBs or other populations. To estimate the best fit parameters of the Ep-TL-Lp relations from data including outliers, we develop a new method which combine robust regression and an outlier identification technique. Using our new method for 18 GRBs with {\sigma}Ep/Ep < 0.1, we detect 6 outliers and find the Ep-TL-Lp relation become the tightest around 3 second.

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