WALLABY Pilot Survey: H i in the Host Galaxy of a Fast Radio Burst
WALLABY Pilot Survey: H i in the Host Galaxy of a Fast Radio Burst
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DOI：
10.3847/1538-4357/acc1e3
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发表时间：
2023-05
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通讯作者：
M. Głowacki;K. Lee-Waddell;A. Deller;N. Deg;A. Gordon;J. A. Grundy;L. Marnoch;A. Shen;S. Ryder;R. Shannon;O. I. Wong;H. Dénes;B. Koribalski;C. Murugeshan;J. Rhee;T. Westmeier;S. Bhandari;A. Bosma;B. Holwerda;J. Prochaska
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作者：
M. Głowacki;K. Lee-Waddell;A. Deller;N. Deg;A. Gordon;J. A. Grundy;L. Marnoch;A. Shen;S. Ryder;R. Shannon;O. I. Wong;H. Dénes;B. Koribalski;C. Murugeshan;J. Rhee;T. Westmeier;S. Bhandari;A. Bosma;B. Holwerda;J. Prochaska
本文报道了对快射电暴（FRB）20211127 I的ASKAP探测和对WALLABY J131913-185018（以下简称W13-18）中中性氢（H i）辐射的探测。CRAFT和WALLABY调查小组之间的合作标志着在H i中发现的第五个也是最遥远的FRB宿主星系，不包括银河系。我们发现W13-18的氢质量为MHI = 6.5 × 109 M ~（-1），氢-恒星质量比为2.17，与1.4GHz的流量密度为1.3mJy的连续射电源相吻合。W13-18的H i整体光谱似乎是不对称的，尽管H i观测的信噪比（S/N）很低，星系本身似乎没有受到干扰。将这些特性与迄今为止在其他FRB宿主中检测到的H i发射的早期文献进行比较，其中H i全局光谱强烈不对称，或者H i强度图分布明显被破坏。W13-18缺乏足够的S/N来确定它的H i分布是否比以前的FRB宿主星系的例子更不对称。然而，在宿主星系的光学图像中，没有强烈的迹象表明会刺激星星形成的爆发，从而产生与大质量恒星及其致密残余物有关的假定的FRB祖先。
We report on the commensal ASKAP detection of a fast radio burst (FRB), FRB 20211127I, and the detection of neutral hydrogen (H i) emission in the FRB host galaxy, WALLABY J131913–185018 (hereafter W13–18). This collaboration between the CRAFT and WALLABY survey teams marks the fifth, and most distant, FRB host galaxy detected in H i, not including the Milky Way. We find that W13–18 has an H i mass of M HI = 6.5 × 109 M ⊙, an H i-to-stellar mass ratio of 2.17, and coincides with a continuum radio source of flux density at 1.4 GHz of 1.3 mJy. The H i global spectrum of W13–18 appears to be asymmetric, albeit the H i observation has a low signal-to-noise ratio (S/N), and the galaxy itself appears modestly undisturbed. These properties are compared to the early literature of H i emission detected in other FRB hosts to date, where either the H i global spectra were strongly asymmetric, or there were clearly disrupted H i intensity map distributions. W13–18 lacks a sufficient S/N to determine whether it is significantly less asymmetric in its H i distribution than previous examples of FRB host galaxies. However, there are no strong signs of a major interaction in the optical image of the host galaxy that would stimulate a burst of star formation and hence the production of putative FRB progenitors related to massive stars and their compact remnants.