Empirical Constraints on the Origin of Fast Radio Bursts: Volumetric Rates and Host Galaxy Demographics as a Test of Millisecond Magnetar Connection
Empirical Constraints on the Origin of Fast Radio Bursts: Volumetric Rates and Host Galaxy Demographics as a Test of Millisecond Magnetar Connection
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DOI：
10.3847/1538-4357/aa794d
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发表时间：
2017-03
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通讯作者：
M. Nicholl;P. G. Williams;E. Berger;V. Villar;K. Alexander;T. Eftekhari;B. Metzger
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作者：
M. Nicholl;P. G. Williams;E. Berger;V. Villar;K. Alexander;T. Eftekhari;B. Metzger
重复快速射电爆发(FRB)121102在z=0.193的低金属丰度矮小星系中的位置，以及它与发光的静止射电源的联系，表明FRB可能起源于由发生在此类星系中的不寻常超新星形成的磁星。我们通过比较磁星出生率、FRB体积速率和宿主星系的人口统计数据来研究这种可能性。我们计算了可能的毫秒磁星产生通道的平均体积速率，例如超光速超新星(SLSNe)、长和短伽马射线暴(GRB)，以及通过核心塌缩超新星产生的一般磁星(CCSNe)。对于每个通道，我们还使用它们的已知属性来探索预期的宿主星系人口统计数据。我们首次确定了FRB发射体的数密度(体积出生率和寿命的乘积)，GPC−3，假设FRB主要从类似于FRB 121102的重复源发射，并采用0.1的束流因子。通过比较，我们发现，通过稀有渠道(SLSNe，∼)生产的FRB意味着典型的FRB寿命为30-300年，与其他论点一致。在这段时间内发射的总能量与存储在磁场中的可用能量一致。另一方面，与正常的CCSNE产生的磁星的任何关系都导致∼寿命很短，只有0.5年，这与理论和观测都是矛盾的。我们证明，由于不同母体通道的宿主星系分布不同，可以通过宿主星系的识别来排除许多可能的FRB诞生来源。相反，对之前拥有数十年SLSNe和伽玛暴的星系进行定向搜索，对于发现新的FRB和相关的静止射电源，并确定它们的祖先的性质来说，可能是一个卓有成效的战略。
The localization of the repeating fast radio burst (FRB) 121102 to a low-metallicity dwarf galaxy at z = 0.193, and its association with a luminous quiescent radio source, suggests the possibility that FRBs originate from magnetars, formed by the unusual supernovae that occur in such galaxies. We investigate this possibility via a comparison of magnetar birth rates, the FRB volumetric rate, and host galaxy demographics. We calculate average volumetric rates of possible millisecond magnetar production channels, such as superluminous supernovae (SLSNe), long and short gamma-ray bursts (GRBs), and general magnetar production via core-collapse supernovae (CCSNe). For each channel, we also explore the expected host galaxy demographics using their known properties. We determine for the first time the number density of FRB emitters (the product of their volumetric birth rate and lifetime), Gpc−3, assuming that FRBs are predominantly emitted from repetitive sources similar to FRB 121102 and adopting a beaming factor of 0.1. By comparing rates, we find that production via rare channels (SLSNe, GRBs) implies a typical FRB lifetime of ∼30–300 years, in good agreement with other lines of argument. The total energy emitted over this time is consistent with the available energy stored in the magnetic field. On the other hand, any relation to magnetars produced via normal CCSNe leads to a very short lifetime of ∼0.5 years, in conflict with both theory and observation. We demonstrate that due to the diverse host galaxy distributions of the different progenitor channels, many possible sources of FRB birth can be ruled out with host galaxy identifications. Conversely, targeted searches of galaxies that have previously hosted decades-old SLSNe and GRBs may be a fruitful strategy for discovering new FRBs and related quiescent radio sources, and determining the nature of their progenitors.