利用DECam为引力波事件设计最优千新星搜寻策略
Designing an Optimal Kilonova Search using DECam for Gravitational Wave Events
AI总结：
本文针对LIGO/Virgo/KAGRA O4运行，基于引力波事件与千新星模拟，为DECam设计最优观测策略，在190 Mpc处将电磁对应体发现概率提升至约80%，并显著减少望远镜时间。
摘要：
我们致力于解决在即将到来的LIGO/Virgo/KAGRA合作观测运行O4中，最优识别所有通过引力波辐射探测到的千新星的问题。O4预计对双中子星警报的灵敏度将比以往提高约7倍。对这些新事件中除最亮者以外的所有事件进行电磁后续观测，将需要口径大于1米的望远镜，而这类望远镜的可用时间十分有限。我们提出了一种针对暗能量相机（Dark Energy Camera, DECam）在O4期间的最优观测策略。我们的研究基于对O4预期引力波事件的模拟以及宽先验千新星模拟。我们推导了在真实观测条件下事件的探测能力。我们优化策略的目标是在确认千新星的同时最小化望远镜时间。对于大范围的千新星参数——对应于比GW170817/AT2017gfo更暗的千新星——我们发现，采用这一最优策略，在下一轮LVK观测运行的双中子星引力波标称探测极限（190 Mpc）处，暗能量相机对电磁对应体的发现概率约为80%，相比上一轮观测运行所采用的策略提高了约30%。对于更远的事件（约330 Mpc），我们达到约60%的探测概率，提高了约2倍。对于一个以蓝色分量为主导、能够再现GW170817/AT2017gfo观测结果的更亮千新星模型，我们发现可以在330 Mpc范围内达到约90%的探测概率，提高了约20%，同时将后续观测所需的总望远镜时间减少了约20%。
英文摘要：
We address the problem of optimally identifying all kilonovae detected via gravitational wave emission in the upcoming LIGO/Virgo/KAGRA Collaboration observing run, O4, which is expected to be sensitive to a factor of $\sim 7$ more Binary Neutron Stars alerts than previously. Electromagnetic follow-up of all but the brightest of these new events will require $>1$ meter telescopes, for which limited time is available. We present an optimized observing strategy for the Dark Energy Camera during O4. We base our study on simulations of gravitational wave events expected for O4 and wide-prior kilonova simulations. We derive the detectabilities of events for realistic observing conditions. We optimize our strategy for confirming a kilonova while minimizing telescope time. For a wide range of kilonova parameters, corresponding to a fainter kilonova compared to GW170817/AT2017gfo we find that, with this optimal strategy, the discovery probability for electromagnetic counterparts with the Dark Energy Camera is $\sim 80\%$ at the nominal binary neutron star gravitational wave detection limit for the next LVK observing run (190 Mpc), which corresponds to a $\sim 30\%$ improvement compared to the strategy adopted during the previous observing run. For more distant events ($\sim 330$ Mpc), we reach a $\sim 60\%$ probability of detection, a factor of $\sim 2$ increase. For a brighter kilonova model dominated by the blue component that reproduces the observations of GW170817/AT2017gfo, we find that we can reach $\sim 90\%$ probability of detection out to 330 Mpc, representing an increase of $\sim 20 \%$, while also reducing the total telescope time required to follow-up events by $\sim 20\%$.
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