STUDYING THE WARM HOT INTERGALACTIC MEDIUM WITH GAMMA-RAY BURSTS
STUDYING THE WARM HOT INTERGALACTIC MEDIUM WITH GAMMA-RAY BURSTS
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DOI：
10.1088/0004-637x/697/1/328
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发表时间：
2009-05
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通讯作者：
E. Branchini;E. Ursino;A. Corsi;D. Martizzi;L. Amati;J. Herder;M. Galeazzi;B. Gendre;J. Kaastra;L. Moscardini;F. Nicastro;T. Ohashi;F. Paerels;L. Piro;M. Roncarelli;Y. Takei;M. Viel
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作者：
E. Branchini;E. Ursino;A. Corsi;D. Martizzi;L. Amati;J. Herder;M. Galeazzi;B. Gendre;J. Kaastra;L. Moscardini;F. Nicastro;T. Ohashi;F. Paerels;L. Piro;M. Roncarelli;Y. Takei;M. Viel
我们评估的可能性，检测和表征的物理状态的失踪重子在低红移的伽马射线暴（GRB）余辉，测量基于微热计的探测器3 eV的分辨率和1000平方厘米的有效面积，能够快速重定向，类似于最近提出的X射线卫星EDGE和XENIA板上的X射线吸收光谱分析。为此，我们分析了模拟吸收光谱提取不同的流体动力学模拟用于模拟温暖的热星系际介质（WHIM）的属性。这些模型预测的正确丰度的O VI吸收线观察到的UV和满足当前的X射线的限制。根据这些模型，EDGE和XENIA等空间飞行任务每年应该能够通过O vii线探测到1060个WHIM吸收器。其中约45%的谱线除了O vii外，还具有至少两条可检测的谱线，可用于确定气体的密度和温度。气体密度和温度的估计中的系统误差可以以稳健的、基本上独立于模型的方式进行校正。对三年内收集的伽玛射线暴吸收光谱的分析也将允许测量WHIM的宇宙质量密度，精度为15%，尽管这一估计取决于WHIM模型。我们的研究结果表明，伽玛暴是一个有效的，如果不是优选的，替代活动星系核研究WHIM的吸收。吸收光谱的分析很好地补充了发射中WHIM的研究，由于其高灵敏度和大视场，EDGE和XENIA的光谱仪将能够进行。
We assess the possibility of detecting and characterizing the physical state of the missing baryons at low redshift by analyzing the X-ray absorption spectra of the gamma-ray burst (GRB) afterglows, measured by a microcalorimeter-based detector with 3 eV resolution and 1000 cm2 effective area and capable of fast repointing, similar to that on board of the recently proposed X-ray satellites EDGE and XENIA. For this purpose we have analyzed mock absorption spectra extracted from different hydrodynamical simulations used to model the properties of the warm hot intergalactic medium (WHIM). These models predict the correct abundance of O vi absorption lines observed in UV and satisfy current X-ray constraints. According to these models space missions such as EDGE and XENIA should be able to detect ∼60 WHIM absorbers per year through the O vii line. About 45% of these have at least two more detectable lines in addition to O vii that can be used to determine the density and the temperature of the gas. Systematic errors in the estimates of the gas density and temperature can be corrected for in a robust, largely model-independent fashion. The analysis of the GRB absorption spectra collected in three years would also allow to measure the cosmic mass density of the WHIM with ∼15% accuracy, although this estimate depends on the WHIM model. Our results suggest that GRBs represent a valid, if not preferable, alternative to active galactic nuclei to study the WHIM in absorption. The analysis of the absorption spectra nicely complements the study of the WHIM in emission that the spectrometer proposed for EDGE and XENIA would be able to carry out thanks to its high sensitivity and large field of view.