A Systematic Exploration of Kilonova Candidates from Neutron Star Mergers during the Third Gravitational-wave Observing Run
A Systematic Exploration of Kilonova Candidates from Neutron Star Mergers during the Third Gravitational-wave Observing Run
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DOI：
10.3847/1538-4357/ac4d34
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发表时间：
2021-12
期刊：
影响因子：
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通讯作者：
J. Rastinejad;K. Paterson;W. Fong;D. Sand;M. Lundquist;G. Hosseinzadeh;E. Christensen;P. Daly-P.-Dal
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文献类型：
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作者：
J. Rastinejad;K. Paterson;W. Fong;D. Sand;M. Lundquist;G. Hosseinzadeh;E. Christensen;P. Daly-P.-Dal
我们提出了一个全面的分析，在第三次引力波（GW）观测运行期间报告的653个光学候选对应物。我们的样本集中在15个事件（发表在GWTC-2，GWTC-3，或没有在GraceDB上撤回）的候选者中，这些事件有>1%的机会包括中子星星，以评估它们作为真正千新星的可行性。特别是，我们利用真实的可用工具，包括合并前检测和与目录的交叉匹配（即，点源，变星，类星体和宿主星系红移数据集），以消除我们样本中65%的候选者。我们进一步采用光谱分类，后期检测，和光曲线行为分析，并得出结论，66个候选人仍然可行的kilonovae。这些候选者缺乏足够的信息来确定它们的分类，大多数都需要比AT 2017 gfo更大的光度。合并前的公开测光调查数据的检测和编目的主星系红移与GW事件距离的比较是至关重要的，纳入审查程序，因为这些工具消除了>20%和>30%的候选人，分别。我们预计，这些工具，利用档案信息将显着减少压力的光谱和光度的后续资源在未来的观测运行。最后，我们讨论了从GW天文学家到EM社区的及时更新在减少需要审查的候选人数量方面发挥的关键作用。
We present a comprehensive analysis of 653 optical candidate counterparts reported during the third gravitational-wave (GW) observing run. Our sample concentrates on candidates from the 15 events (published in GWTC-2, GWTC-3, or not retracted on GraceDB) that had a >1% chance of including a neutron star in order to assess their viability as true kilonovae. In particular, we leverage tools available in real time, including pre-merger detections and cross-matching with catalogs (i.e., point-source, variable-star, quasar and host-galaxy redshift data sets), to eliminate 65% of candidates in our sample. We further employ spectroscopic classifications, late-time detections, and light-curve behavior analyses and conclude that 66 candidates remain viable kilonovae. These candidates lack sufficient information to determine their classifications, and the majority would require luminosities greater than that of AT 2017gfo. Pre-merger detections in public photometric survey data and comparison of cataloged host-galaxy redshifts with the GW event distances are critical to incorporate into vetting procedures, as these tools eliminated >20% and >30% of candidates, respectively. We expect that such tools that leverage archival information will significantly reduce the strain on spectroscopic and photometric follow-up resources in future observing runs. Finally, we discuss the critical role prompt updates from GW astronomers to the EM community play in reducing the number of candidates requiring vetting.