Extending the Frequency Reach of Pulsar Timing Array-based Gravitational Wave Search without High-cadence Observations
Extending the Frequency Reach of Pulsar Timing Array-based Gravitational Wave Search without High-cadence Observations
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DOI：
10.3847/2041-8213/abd9bd
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发表时间：
2020-12
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影响因子：
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通讯作者：
Yan Wang;S. Mohanty;Zhoujian Cao
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文献类型：
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作者：
Yan Wang;S. Mohanty;Zhoujian Cao
假设使用脉冲星定时阵列（pta）的引力波（GW）搜索受到单个脉冲星的典型平均观测频率（1/（2周））的限制，到GW频率≤4 × 10−7 Hz。我们证明这种假设是不正确的，PTA可以通过利用来自多个脉冲星的异步观测来检测由于混叠而保存在数据中的更高频率的信号。这使得观测策略可以扩展到未来包含O（103）脉冲星的大型pta，由500米口径球面望远镜和平方公里阵列实现，而不需要更高的每颗脉冲星观测节奏。我们发现，使用平方公里阵列时代的PTA进行更高频率的GW观测，达到4 × 10−4 Hz，具有重要的天体物理学意义，例如：(i)比目前在[10,400]μHz波段对GW应变的高频率观测有三个数量级的更好的约束，以及（ii）使用它们的启发，合并和环落信号对超大质量黑洞双星质量范围内的无毛定理进行敏感测试。
Gravitational wave (GW) searches using pulsar timing arrays (PTAs) are assumed to be limited by the typical average observational cadence of 1/(2 weeks) for a single pulsar to GW frequencies ≲4 × 10−7 Hz. We show that this assumption is incorrect and that a PTA can detect signals with much higher frequencies, which are preserved in the data due to aliasing, by exploiting asynchronous observations from multiple pulsars. This allows an observation strategy that is scalable to future large-scale PTAs containing O(103) pulsars, enabled by the Five-hundred meter Aperture Spherical Telescope and the Square Kilometer Array, without requiring a higher per-pulsar observation cadence. We show that higher frequency GW observations, reaching up to 4 × 10−4 Hz with an Square Kilometer Array-era PTA, have significant astrophysical implications, such as (i) a three orders of magnitude better constraint than current high-cadence observations on GW strain in the [10, 400] μHz band, and (ii) sensitive tests of the no-hair theorem in the mass range of supermassive black hole binaries using their inspiral, merger, and ringdown signals.