快速射电暴主环境的高分辨率观测
A High-Resolution View of Fast Radio Burst Host Environments
摘要：
利用哈勃空间望远镜（HST/WFC 3）对8个具有亚弧秒局域的快速射电暴（FRB）宿主星系进行了紫外和红外观测，其中包括3个已知的重复FRB宿主星系。我们量化了它们的空间分布和相对于宿主星系光分布的位置，发现它们发生在1.4 $r_e$（[0.6，2.1] $r_e$ ; 68%的间隔）的中等宿主归一化偏移处，发生在它们的宿主的红外光较暗的区域，但总体上追踪了它们星系中红外光的径向分布。我们测试的分布中的FRB没有清楚地追踪任何其他具有已知祖细胞的瞬时群体的分布，并且在统计上与LGRB、H-贫SLSNe、SGRB和富Ca瞬变的位置不同。我们进一步发现，大多数FRB是不是在当地的恒星形成率和恒星质量表面密度的平均值相比，他们的主机的区域。我们还把上限的红外线流量在FRB的位置$m_{\rm IR}\gtrsim\!24.8-27.6$ ~AB~马格，卫星和背景星系的光度远低于主机光度FRB 121102。我们发现，5/8 FRB主机在红外光下表现出清晰的旋臂特征，并且位于此类主机中的所有本地化FRB的位置与其旋臂一致，尽管不在其最亮区域。我们的研究结果并不强烈支持的主要祖通道的FRB连接无论是与最大质量（剥离信封）的明星，或与事件，需要踢和长延迟时间（中子星合并）。
英文摘要：
We present Hubble Space Telescope (HST/WFC3) ultraviolet and infrared observations of eight fast radio burst (FRB) host galaxies with sub-arcsecond localizations, including the hosts of three known repeating FRBs. We quantify their spatial distributions and locations with respect to their host galaxy light distributions, finding that they occur at moderate host normalized-offsets of 1.4 $r_e$ ([0.6,2.1] $r_e$; 68% interval), occur on fainter regions of their hosts in terms of IR light, but overall trace the radial distribution of IR light in their galaxies. The FRBs in our tested distribution do not clearly trace the distributions of any other transient population with known progenitors, and are statistically distinct from the locations of LGRBs, H-poor SLSNe, SGRBs, and Ca-rich transients. We further find that most FRBs are not in regions of elevated local star formation rate and stellar mass surface densities in comparison to the mean global values of their hosts. We also place upper limits to the IR flux at the FRB positions of $m_{\rm IR}\gtrsim\!24.8-27.6$~AB~mag, constraining both satellite and background galaxies to luminosities well below the host luminosity of FRB121102. We find that 5/8 FRB hosts exhibit clear spiral arm features in IR light, and that the positions of all well-localized FRBs located in such hosts are consistent with their spiral arms, although not on their brightest regions. Our results do not strongly support the primary progenitor channel of FRBs being connected either with the most massive (stripped-envelope) stars, or with events which require kicks and long delay times (neutron star mergers).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
