CGRO/BATSE数据支持GRB瞬发发射的新范例和新的L-PDMATHAAC-$_{peak,i}^{nTh,rest}$关系
CGRO/BATSE Data Support the New Paradigm for GRB Prompt Emission and the New L$_{i}^{nTh}$-E$_{peak,i}^{nTh,rest}$ relation
摘要：
伽玛射线暴瞬发的模式正在发生变化。自CGRO时代早期以来，经验能带函数一直被认为是keV-MeV光谱的良好描述，尽管它的形状经常与纯同步辐射情景的预测不一致。我们最近建立了一个新的观测模型，分析了美国宇航局费米伽马射线太空望远镜的数据。在这个模型中，伽玛射线暴的瞬发辐射是三个主要辐射成分的组合：（i）一个热的成分，我们解释到目前为止的射流光球发射，（ii）一个非热的成分，我们解释到目前为止的同步辐射，和（iii）一个额外的非热（截止）的幂律最有可能逆康普顿起源。在这篇文章中，我们重新分析了CGRO/BATSE观测到的一些明亮的伽玛暴与新的模型，即伽玛暴941017，970111和990123。我们的结论是，BATSE数据是完全符合最近的结果与费米：一些明亮的BATSE伽玛暴表现出三个独立的组件在提示阶段与类似的光谱参数，这些报告从费米数据。此外，用新模型对BATSE伽玛暴的分析得到了非热分量的时间分辨能流与其相应的$ν$ F $_ν$峰值能量之间的关系（即，F $_{i}^{nTh}$ -E $_{peak,i}^{nTh}$），其具有与最初从费米数据导出的指数相似的指数。对于具有已知红移（z）的GRB，这导致在非热分量的光度与其在静止坐标系中的对应的$ν$ F $_ν$峰值能量之间的可能的普适关系（即，L $_{i}^{nTh}$ -E $_{peak,i}^{NT,rest}$）。我们使用GRB 990123（z=1.61）作为参考，估计了GRB 941017和970111的z。GRB 941017的估计z是长GRB的典型值，GRB 970111的估计z正好在这个爆发的预期值范围内。
英文摘要：
The paradigm for GRB prompt emission is changing. Since early in the CGRO era, the empirical Band function has been considered a good description of the keV-MeV spectra although its shape is very often inconsistent with the predictions of the pure synchrotron emission scenarios. We have recently established a new observational model analyzing data of the NASA Fermi Gamma-ray Space Telescope. In this model, GRB prompt emission is a combination of three main emission components: (i) a thermal-like component that we interpreted so far as the jet photosphere emission, (ii) a non-thermal component that we interpreted so far as synchrotron radiation, and (iii) an additional non-thermal (cutoff) power-law most likely of inverse Compton origin. In this article we reanalyze some of the bright GRBs observed with CGRO/BATSE with the new model, namely GRBs 941017, 970111 and 990123. We conclude that BATSE data are fully consistent with the recent results obtained with Fermi: some bright BATSE GRBs exhibit three separate components during the prompt phase with similar spectral parameters as these reported from Fermi data. In addition, the analysis of the BATSE GRBs with the new model results in a relation between the time-resolved energy flux of the non-thermal component and its corresponding $ν$F$_ν$ peak energy (i.e., F$_{i}^{nTh}$-E$_{peak,i}^{nTh}$) that has a similar index as the one initially derived from Fermi data. For GRBs with known redshift (z) this results in a possible universal relation between the luminosity of the non-thermal component and its corresponding $ν$F$_ν$ peak energy in the rest frame (i.e., L$_{i}^{nTh}$-E$_{peak,i}^{NT,rest}$). We estimated z for GRBs 941017 and 970111 using GRB 990123--with z=1.61--as a reference. The estimated z for GRB 941017 is typical for long GRBs and the estimated z for GRB 970111 is right in the range of the expected values for this burst.
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