Optimizing Cadences with Realistic Light-curve Filtering for Serendipitous Kilonova Discovery with Vera Rubin Observatory
Optimizing Cadences with Realistic Light-curve Filtering for Serendipitous Kilonova Discovery with Vera Rubin Observatory
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DOI：
10.3847/1538-4365/ac3bae
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发表时间：
2021-06
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通讯作者：
I. Andreoni;M. Coughlin;M. Almualla;E. Bellm;F. Bianco;M. Bulla;A. Cucchiara;T. Dietrich;A. Goobar;E. Kool;Xiaolong Li;F. Ragosta;Ana Sagués-Carracedo;L. Singer
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作者：
I. Andreoni;M. Coughlin;M. Almualla;E. Bellm;F. Bianco;M. Bulla;A. Cucchiara;T. Dietrich;A. Goobar;E. Kool;Xiaolong Li;F. Ragosta;Ana Sagués-Carracedo;L. Singer
当前和未来的光学和近红外宽视场调查有可能发现千新星，即中子星合并的光学和红外对应体，独立于引力波或高能伽马射线爆发的触发。发现快速和微弱的瞬变（如千新星）的能力在很大程度上取决于观测的区域、这些观测的深度、在给定时间框架内每个领域的访问次数以及调查采用的过滤器；它还取决于进行快速后续观测以确认瞬变性质的能力。在这项工作中，我们评估了Vera C. Rubin宽快深调查遗留时空调查策略的现有模拟中的千新星可探测性，重点是将滚动节奏与基线节奏进行比较。虽然目前可用的节奏可以在10年的调查中检测到大约300千新星到1400 Mpc，但我们预计只有3-32千新星类似于GW170817被识别为快速演变的瞬态。我们还探讨了千新星在似是而非的参数空间上的可探测性，重点是观测角度和抛射质量。我们发现，在较红波段的观测对于识别附近（在300 Mpc以内）的千新星至关重要，这些千新星比更远的源更容易进行光谱分类。鲁宾偶然发现千新星的潜力可以通过使用单个30秒曝光（而不是2 × 15秒快照对）的效率增加，加上红色波段观测加上g或r波段的当晚观测，以及可能进一步发展新的滚动节奏策略来增加。
Current and future optical and near-infrared wide-field surveys have the potential to find kilonovae, the optical and infrared counterparts to neutron star mergers, independently of gravitational-wave or high-energy gamma-ray burst triggers. The ability to discover fast and faint transients such as kilonovae largely depends on the area observed, the depth of those observations, the number of revisits per field in a given time frame, and the filters adopted by the survey; it also depends on the ability to perform rapid follow-up observations to confirm the nature of the transients. In this work, we assess kilonova detectability in existing simulations of the Legacy Survey of Space and Time strategy for the Vera C. Rubin Wide Fast Deep survey, with focus on comparing rolling to baseline cadences. Although currently available cadences can enable the detection of >300 kilonovae out to ∼1400 Mpc over the 10 year survey, we can expect only 3–32 kilonovae similar to GW170817 to be recognizable as fast-evolving transients. We also explore the detectability of kilonovae over the plausible parameter space, focusing on viewing angle and ejecta masses. We find that observations in redder izy bands are crucial for identification of nearby (within 300 Mpc) kilonovae that could be spectroscopically classified more easily than more distant sources. Rubin’s potential for serendipitous kilonova discovery could be increased by gain of efficiency with the employment of individual 30 s exposures (as opposed to 2 × 15 s snap pairs), with the addition of red-band observations coupled with same-night observations in g or r bands, and possibly with further development of a new rolling-cadence strategy.