LIGO-India时代中子星-黑洞并合电磁后随观测的前景
Prospects of electromagnetic follow-up of neutron star-black hole mergers in the LIGO-India era
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中文总结 AI 辅助
本研究模拟LIGO-India时代NSBH并合，提出事件特定曝光优化策略，使EM后随观测数翻倍，年探测率最高达4.19，并有助于测量哈勃常数。
中文摘要 AI 辅助
中子星-黑洞（NSBH）并合是有前景的多信使源，但预计只有一部分能产生可探测的电磁（EM）对应体，这取决于双星质量比、黑洞（BH）自旋和中子星（NS）状态方程（EoS）。我们利用Vera C. Rubin天文台（Rubin）研究了在LIGO-India时代探测NSBH并合千新星对应体的前景。我们模拟了受GW230529启发的NSBH族群，具有两个有效潮汐形变范围，估算了LHV（LIGO-Livingston、LIGO-Hanford、Virgo）和LHVA（LHV加上位于Aundha的LIGO-India）探测器网络的引力波探测，并模拟了Rubin对相关千新星辐射的可探测性。我们发现，加入LIGO-India后，电磁后随观测的数量大约翻倍，这主要通过提高工作周期和减小中位天空定位区域实现，并且显著增加了大距离处此类探测的数量。对于固定曝光策略，电磁探测率在几百秒的曝光时间处饱和，反映了深度和天空覆盖之间的权衡。因此，我们提出了一种基于预期对应体亮度和天空定位区域的事件特定曝光时间优化策略。采用该策略，LHVA网络下预期的NSBH引力波+电磁年探测率为乐观族群4.19（-3.58，+9.66）和保守族群0.79（-0.68，+1.83），而LHV网络下分别为1.46（-1.25，+3.37）和0.27（-0.23，+0.62）。所需的Rubin后随观测时间保持在预期的目标机会（Target-of-Opportunity）分配范围内。这些结果表明，在下一个十年中，可能发生少数此类NSBH后随观测，其中一部分位于红移约0.1-0.2范围内，这不仅对测量哈勃常数有用，还能帮助我们探测哈勃参数。
英文摘要
Neutron star-black hole (NSBH) mergers are promising multimessenger sources, but only a subset is expected to produce detectable electromagnetic (EM) counterparts, depending on the binary mass ratio, black hole (BH) spin, and neutron star (NS) equation of state (EoS). We investigate the prospects for detecting kilonova counterparts to NSBH mergers in the LIGO-India era using the Vera C. Rubin Observatory (Rubin). We simulate GW230529-motivated NSBH populations with two effective tidal deformability ranges, estimate gravitational-wave detections for the LHV (LIGO-Livingston, LIGO-Hanford, Virgo) and LHVA (LHV with LIGO-India at Aundha) detector networks, and model the detectability of the associated kilonova emission with Rubin. We find that adding LIGO-India approximately doubles the number of EM follow-ups, primarily by increasing the duty cycle and reducing the median sky-localization area, and notably increases the number of such detections at large distances. For fixed-exposure strategies, the EM detection rate saturates at exposure times of a few hundred seconds, reflecting the trade-off between depth and sky coverage. We therefore introduce an event-specific exposure-time optimization strategy based on the expected counterpart brightness and sky-localization area. With this strategy, the expected NSBH GW+EM detection rate per year is 4.19(-3.58,+9.66) for the optimistic and 0.79(-0.68,+1.83) for the conservative population with the LHVA network, compared to 1.46(-1.25,+3.37) and 0.27(-0.23,+0.62), respectively, for LHV. The required Rubin follow-up time remains within the expected Target-of-Opportunity allocation. These results show that in the next decade, a few such NSBH follow-ups may take place, with a fraction of them in the redshift range of about 0.1-0.2, which will not only be useful for measuring the Hubble constant but can also help us in probing the Hubble parameter.
发表机构
- Inter University Centre for Astronomy and Astrophysics（大学天体物理中心）
- Syracuse University（雪城大学）
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