Global Characteristics of X‐Ray Flashes and X‐Ray–Rich Gamma‐Ray Bursts Observed by<i>HETE</i>‐<i>2</i>

Sakamoto, T.; Lamb, D. Q.; Kawai, N.; Yoshida, A.; Graziani, C.; Fenimore, E. E.; Donaghy, T.; Matsuoka, M.; Suzuki, M.; Ricker, G.; Atteia, J. L.; Shirasaki, Y.; Tamagawa, T.; Torii, K.; Galassi, M.; Doty, J.; Vanderspek, R.; Crew, G. B.; Villaseñor, J.; Butler, N.; Prigozhin, G.; Jernigan, J. G.; Barraud, C.; Boër, M.; Dezalay, J. P.; Olive, J. F.; Hurley, K.; Levine, Alan M.; Monnelly, G.; Martel, F.; Morgan, E.; Woosley, S. E.; Cline, T. L.; Braga, J.; Manchanda, R. K.; Pizzichini, G.; Takagishi, K.; Yamauchi, M.

doi:10.1086/431235

Cited by 231 publications

(290 citation statements)

References 28 publications

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“…Sakamoto et al 2005). The timescale of the main flares and the late-time powerlaw decays seen in XRT 110103 and XRT 000519 are consistent with the early Xray emission typically seen in GRB lightcurves (e.g.…”

Section: Xrt 110103supporting

confidence: 77%

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Two fast X-ray transients in archival Chandra data

Glennie

Jonker

Fender

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the discovery of two new X-ray transients in archival Chandra data. The first transient, XRT110103, occurred in January 2011 and shows a sharp rise of at least three orders of magnitude in count rate in less than 10 s, a flat peak for about 20 s and decays by two orders of magnitude in the next 60 s. We find no optical or infrared counterpart to this event in preexisting survey data or in an observation taken by the SIRIUS instrument at the Infrared Survey Facility ∼ 2.1 yr after the transient, providing limiting magnitudes of J > 18.1, H > 17.6 and K s > 16.3. This event shows similarities to the transient previously reported in Jonker et al. which was interpreted as the possible tidal disruption of a white dwarf by an intermediate mass black hole. We discuss the possibility that these transients originate from the same type of event. If we assume these events are related a rough estimate of the rates gives 1.4×10 5 per year over the whole sky with a peak 0.3 -7 keV X-ray flux greater than 2×10 −10 erg cm −2 s −1 . The second transient, XRT120830, occurred in August 2012 and shows a rise of at least three orders of magnitude in count rate and a subsequent decay of around one order of magnitude all within 10 s, followed by a slower quasi-exponential decay over the remaining 30 ks of the observation. We detect a likely infrared counterpart with magnitudes J = 16.70 ± 0.06, H = 15.92 ± 0.04 and K s = 15.37 ± 0.06 which shows an average proper motion of 74 ± 19 milliarcsec per year compared to archival 2MASS observations. The JHK s magnitudes, proper motion and X-ray flux of XRT 120830 are consistent with a bright flare from a nearby late M or early L dwarf.

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Section: Xrt 110103supporting

confidence: 77%

“…O'Brien et al 2006). Figure 7 in Sakamoto et al (2005) shows the peak energy constraints on X-ray flashes, X-ray-rich GRBs and Hard GRBs. Of these scenarios, the upper limits on the peak energy of XRT 110103 and XRT 000519 from the power law fits could only be consistent with an X-ray flash.…”

Section: Xrt 110103mentioning

confidence: 99%

Two fast X-ray transients in archival Chandra data

Glennie

Jonker

Fender

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…These low energetic events have been classified as X-ray flashes (XRF) or X-ray rich bursts (XRB) (see e.g. Heise & in 't Zand 2001;Sakamoto et al 2005). However, it is very likely that XRFs and XRBs are nothing else than weak and long GRBs (see Kippen et al 2004, and references therein).…”

Section: Analysis Of the Gbm Datamentioning

confidence: 99%

Rest-frame properties of 32 gamma-ray bursts observed by theFermiGamma-ray Burst Monitor

Gruber

Greiner

Kienlin

et al. 2011

A&A

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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 (E p,rest ), the duration in the rest-frame, defined as the time in which 90% of the burst fluence was observed (T 90,rest ) and the isotropic equivalent bolometric energy (E iso ). Results. The distribution of E p,rest 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-E p population is found but the distribution is biased against low E p values. We find the lowest possible E p that GBM can recover to be ≈15 keV. The T 90,rest distribution of long GRBs peaks at ∼10 s. The distribution of E iso has mean and median values of 8.9 × 10 52 erg and 8.2 × 10 52 erg, respectively. We confirm the tight correlation between E p,rest and E iso (Amati relation) and the one between E p,rest 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 E p is located at the lower end of the detector energy range. Moreover, we do not find any significant cosmic evolution of neither E p,rest nor T 90,rest .

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“…Bursts with peak energies less than 50 keV (X-ray flashes) have been detected by Ginga and HETE-2 (Strohmayer et al 1998;Sakamoto et al 2005), but few have measured redshifts. Their T 90 distribution is, nonetheless, remarkably similar to that of the harder spectrum bursts, which suggests that the low E pk is not primarily due to a large cosmological redshift.…”

Section: E Imentioning

confidence: 99%

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

Thompson¹,

Mészáros²,

Rees³

2007

ApJ

164

182

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We present an interpretation of the phenomenological relations between the spectral peak, isotropic luminosity, and duration of long gamma-ray bursts that have been discovered by Amati and coworkers, Ghirlanda and coworkers, Firmani and coworkers, and Liang & Zhang. In our proposed model, a jet undergoes internal dissipation which prevents its bulk Lorentz factor from exceeding 1/ ( being the jet opening angle) until it escapes from the core of its progenitor star, at a radius of order 10 10 cm; dissipation may continue at larger radii. The dissipated radiation will be partially thermalized, and we identify its thermal peak ( Doppler boosted by the outflow) with E pk . The radiation comes, in effect, from within the jet photosphere. The nonthermal, high-energy part of the GRB emission arises from Comptonization of this radiation by relativistic electrons and positrons outside the effective photosphere. This model can account naturally not only for the surprisingly small scatter in the various claimed correlations, but also for the normalization, as well as the slopes. It then has further implications for the jet energy, the limiting jet Lorentz factor, and the relation of the energy, opening angle and burst duration to the mass and radius of the stellar stellar progenitor. The observed relation between pulse width and photon frequency can be reproduced by inverse Compton emission at $10 14 cm from the engine, but there are significant constraints on the energy distribution and isotropy of the radiating particles.

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Global Characteristics of X‐Ray Flashes and X‐Ray–Rich Gamma‐Ray Bursts Observed byHETE‐2

Cited by 231 publications

References 28 publications

Two fast X-ray transients in archival Chandra data

Two fast X-ray transients in archival Chandra data

Rest-frame properties of 32 gamma-ray bursts observed by theFermiGamma-ray Burst Monitor

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

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