The Panchromatic Afterglow of GW170817: The Full Uniform Data Set, Modeling, Comparison with Previous Results, and Implications-猫眼课题宝

DOI：

10.3847/1538-4357/ac1ffc

发表时间：

2020-06

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

S. Makhathini;Kunal Mooley;M. Brightman;K. Hotokezaka;A. Nayana;H. Intema;D. Dobie;E. Lenc;D. Perley;C. Fremling;J. Moldón;Davide Lazzati;David L. Kaplan;A. Balasubramanian;Ian Brown;D. Carbone;P. Chandra;A. Corsi;F. Camilo;Adam T. Deller;D. Frail;Tara Murphy;Eric J. Murphy;E. Nakar;O. Smirnov;R. Beswick;Rob Fender;G. Hallinan;I. Heywood;M. Kasliwal;Bomee Lee;Wenbin Lu;J. Rana;S. Perkins;Sarah V. White;G. I. Józsa;B. Hugo;P. Kamphuis

我们提供了 GW170817 合并后 0.5 至 940 天的完整全色余辉光曲线数据，包括新的无线电数据以及档案光学和 X 射线数据。通过编译所有档案数据并重新处理其中的一个子集，我们评估了不同群体使用的数据处理或通量确定方法差异的影响，并试图减轻这些差异以提供更统一的数据集。均匀余辉光曲线的简单幂律拟合表明 t 0.86±0.04 上升，t -1.92±0.12 下降，峰值出现在 155 ± 4 天。余辉在其整个演化过程中光学上都很薄，与所有时期的单一光谱指数（−0.584±0.002）一致。这给出了电子幂律指数的精确且更新的估计，p = 2.168 ± 0.004。通过研究宿主星系的漫射 X 射线发射，我们对热电离星际介质密度设定了一个保守的上限，<0.01 cm−3，与之前的余辉研究一致。使用晚余辉数据，我们排除了磁场强度在 1010.4 到 1016 G 之间的任何长寿命中子星遗迹。我们使用分析模型（包括 Mooley 等人的甚长基线干涉测量自行）和忽略自行的结构化喷流模型对余辉数据进行拟合，表明在寻求准确估计视角时需要考虑自行测量。

We present the full panchromatic afterglow light-curve data of GW170817, including new radio data as well as archival optical and X-ray data, between 0.5 and 940 days post-merger. By compiling all archival data and reprocessing a subset of it, we have evaluated the impact of differences in data processing or flux determination methods used by different groups and attempted to mitigate these differences to provide a more uniform data set. Simple power-law fits to the uniform afterglow light curve indicate a t 0.86±0.04 rise, a t −1.92±0.12 decline, and a peak occurring at 155 ± 4 days. The afterglow is optically thin throughout its evolution, consistent with a single spectral index (−0.584 ± 0.002) across all epochs. This gives a precise and updated estimate of the electron power-law index, p = 2.168 ± 0.004. By studying the diffuse X-ray emission from the host galaxy, we place a conservative upper limit on the hot ionized interstellar medium density, <0.01 cm−3, consistent with previous afterglow studies. Using the late-time afterglow data we rule out any long-lived neutron star remnant having a magnetic field strength between 1010.4 and 1016 G. Our fits to the afterglow data using an analytical model that includes Very Long Baseline Interferometry proper motion from Mooley et al., and a structured jet model that ignores the proper motion, indicates that the proper-motion measurement needs to be considered when seeking an accurate estimate of the viewing angle.

The Panchromatic Afterglow of GW170817: The Full Uniform Data Set, Modeling, Comparison with Previous Results, and Implications

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