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首页> 外文期刊>The Astrophysical journal >HIGH ENERGY TRANSIENT EXPLORER 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903
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HIGH ENERGY TRANSIENT EXPLORER 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903

机译：高能瞬态探测器2极端软X射线XRF 020903的观察

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摘要

We report High Energy Transient Explorer 2 (HETE-2) Wide Field X-Ray Monitor/French Gamma Telescope observations of the X-ray flash XRF 020903. This event was extremely soft: the ratio log (S_X/S_γ) = 0.7, where S_X and S_γ are the fluences in the 2-30 and 30-400 keV energy bands, is the most extreme value observed so far by HETE-2. In addition, the spectrum has an observed peak energy of E_(peak)~(obs) < 5.0 keV (99.7% probability upper limit), and no photons were detected above ～10 keV. The burst is shorter at higher energies, which is similar to the behavior of long gamma-ray bursts (GRBs). We consider the possibility that the burst lies at very high redshift and that the low value of E_(peak)~(obs) is due to the cosmological redshift, and show that this is very unlikely. We find that the properties of XRF 020903 are consistent with the relation between the fluences S(7-30 keV) and S(30-400 keV), found by Barraud et al. for GRBs and X-ray-rich GRBs, and are consistent with the extension by a decade of the hardness-intensity correlation found by the same authors. Assuming that XRF 020903 lies at a redshift z = 0.25, as implied by the host galaxy of the candidate optical and radio afterglows of this burst, we find that the properties of XRF 020903 are consistent with an extension by a factor ～300 of the relation between the isotropic-equivalent energy E_(iso) and the peak Speak of the νF_ν spectrum (in the source frame of the burst) found by Amati et al. for GRBs. The results presented in this paper therefore provide evidence that X-ray flashes (XRFs), X-ray-rich GRBs, and GRBs form a continuum and are a single phenomenon. The results also impose strong constraints on models of XRFs and X-ray-rich GRBs.
机译：我们报告了X射线闪光XRF 020903的高能瞬态资源管理器2（HETE-2）宽视场X射线监视器/法国伽玛望远镜观测到的结果。此事件非常软：比率对数（S_X /S_γ）= 0.7，其中S_X和S_γ是2-30和30-400 keV能带的能量密度，是迄今为止HETE-2观测到的最极端值。另外，该光谱具有观察到的峰值能量E_（peak）〜（obs）<5.0 keV（99.7％的概率上限），并且在〜10 keV以上未检测到光子。脉冲在较高能量下较短，这类似于长伽马射线脉冲（GRB）的行为。我们认为，爆发可能存在很高的红移，而E_（peak）〜（obs）的值较低是由于宇宙学的红移造成的，这表明这种可能性很小。我们发现XRF 020903的特性与Barraud等人发现的注量S（7-30 keV）和S（30-400 keV）之间的关系一致。对于GRB和富含X射线的GRB，并且与同一作者发现的硬度-强度相关性扩展了十倍相一致。假设XRF 020903的红移z的主星系暗示了XRF 020903的红移z = 0.25，我们发现XRF 020903的性质与该关系的约300倍扩展一致在等向当量能量E_（iso）和由Amati等人发现的νF_ν谱的峰值Speak（在突发的源帧中）之间。用于GRB。因此，本文提出的结果提供了证据，即X射线闪光（XRF），富含X射线的GRB和GRB形成一个连续体，并且是一个单一现象。结果还对XRF和富含X射线的GRB模型施加了严格的约束。

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