Global Characteristics of X-Ray Flashes and X-Ray-Rich Gamma-Ray Bursts Observed by HETE-2

By T. Sakamoto, D. Lamb, N. Kawai, A. Yoshida, C. Graziani, E. Fenimore, T. Donaghy, M. Matsuoka, Motoko Suzuki, G. Ricker and 28 more. 2005

209 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fe42bf9b30036ad88ecd31b89f1e8eada9e3faa3

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In Astronomy and Astrophysics

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Citations in the corpus

• THE COSMIC RATE, LUMINOSITY FUNCTION, AND INTRINSIC CORRELATIONS OF LONG GAMMA-RAY BURSTS (2009, background): “Our resulting predicted Epk,obs curve for HETE-2 is an acceptable fit (PKS = 0.38) to the observed data (see, Sakamoto et al. 2005).”
• Gamma-Ray Bursts in the Swift Era (2009, methodology): “In particular, bursts with lower spectral energy peaks (Epeak) have been denoted X-Ray Flashes (XRFs) based on observations by BeppoSAX, BATSE and HETE-2 (Heise et al. 2001, Barraud et al. 2003, Kippen et al. 2003, Sakamoto et al. 2005).”
• The First Swift BAT Gamma-Ray Burst Catalog (2007, background): “The peak value of the PL photon index of 1.6 is close to themean value of the low-energy photon index of 1.0 and the high-energy photon index of 2.5 of the typical GRB spectrum (Kaneko et al. 2006; Sakamoto et al. 2005).”
• Short Gamma-Ray Bursts with Extended Emission (2006, background): “For instance, XRFs were essentially nonexistent in the BATSE sample, but constitute a third of the HETE-2 sample (Sakamoto et al. 2005).”
• Measuring the cosmological parameters with the Ep,i–Eiso correlation of gamma-ray bursts (2008, unknown): “…and uncertainties of Ep,i and Eiso: (1) Amati (2006) and references therein; (2) Ulanov et al. (2005) and refined analysis of BeppoSAXdata; (3) Sakamoto et al. (2005); (4) Stratta et al. (2006); (5) Cenko et al. (2006); (6) Krimm et al. (2006); (7) Sakamoto et al. (2008a); (8) Golenetskii et…”
• THE SECOND SWIFT BURST ALERT TELESCOPE GAMMA-RAY BURST CATALOG (2011, methodology): “The similar number of GRBs in the range Eobspeak > 100 keV and 30 keV < E obs peak ≤ 100 keV is consistent with the HETE-2 GRB sample (Sakamoto et al. 2005).”
• FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “XRT 080109 can be adequately fit by such a FRED profile (§ 9.1), but the transient’s duration is an order of magnitude longer than the median T90 for other XRFs and X-ray-rich GRBs (XRRs), which is roughly 30 s (Sakamoto et al. 2005, 2008).”
• The THESEUS space mission concept: science case, design and expected performances (2017, background): “Figure 16: Left: distributions in the spectral peak energy (Ep) - Fluence plane of soft X-Ray Rich (XRR) GRBs and X-Ray Flashes (XRFs) compared to that of normal GRBs (Sakamoto et al., 2005).”
• The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images (2009, background): “It is expected that the population of the X-ray rich GRB is comparable to that of the GRB with an ordinary energy band (Sakamoto et al. 2005).”
• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, methodology): “For those events contained in both samples, I took the spectral parameters from Sakamoto et al. (2005b), given that it reports results based on data from both WXM and FREGATE, whereas the analysis of Barraud et al. (2003) is based on FREGATE data only.”
• The Observable Effects of a Photospheric Component on GRB and XRF Prompt Emission Spectrum (2005, background): “This peak energy is consistent with the peak energy observed in X-ray flashes at ∼ 25 keV (Heise et al. 2001) and X-ray-rich GRB’s (XRR’s), which show peak energy clustering at ∼ 50 keV (Sakamoto et al. 2005).”
• Spectral properties of 438 GRBs detected by Fermi/GBM (2010, methodology): “These global spectral properties of GRBs have also been confirmed by other satellites (BeppoSAX, Hete–II and Swift) (Guidorzi et al. 2010; Sakamoto et al. 2005; Butler et al. 2007).”