GW190425: Pan-STARRS and ATLAS coverage of the skymap and limits on optical emission associated with FRB 20190425A
GW190425: Pan-STARRS and ATLAS coverage of the skymap and limits on optical emission associated with FRB 20190425A
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DOI：
10.1093/mnras/stae100
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发表时间：
2024-01
影响因子：
4.8
通讯作者：
S. Smartt;M. Nicholl;S. Srivastav;M. Huber;K. C. Chambers;K. Smith;D. Young;M. Fulton;J. Tonry;C. W. Stubbs;L. Denneau;A. J. Cooper;A. Aamer;J. Anderson;A. Andersson;J. Bulger;T. -. Chen;P. Clark;T. de Boer-T.-de Boer-2282799674;H. Gao;J. Gillanders;A. Lawrence;C. C. Lin-C.;T. Lowe;E. Magnier;P. Minguez;T. Moore;A. Rest;L. Shingles;R. Siverd;I. A. Smith;B. Stalder;H. Stevance;R. Wainscoat;R. Williams
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文献类型：
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作者：
S. Smartt;M. Nicholl;S. Srivastav;M. Huber;K. C. Chambers;K. Smith;D. Young;M. Fulton;J. Tonry;C. W. Stubbs;L. Denneau;A. J. Cooper;A. Aamer;J. Anderson;A. Andersson;J. Bulger;T. -. Chen;P. Clark;T. de Boer-T.-de Boer-2282799674;H. Gao;J. Gillanders;A. Lawrence;C. C. Lin-C.;T. Lowe;E. Magnier;P. Minguez;T. Moore;A. Rest;L. Shingles;R. Siverd;I. A. Smith;B. Stalder;H. Stevance;R. Wainscoat;R. Williams
GW190425 是激光干涉引力波 (GW) 天文台 (LIGO)、Virgo 和神冈引力波 (KAGRA) 探测器网络显着探测到的两个双中子星 (BNS) 合并事件中的第二个。仅在 LIGO 利文斯顿进行了探测，包含源的星图很大，并且在 2019 年的实时搜索中没有发现合理的电磁对应物。在这里，我们总结了小行星陆地撞击最后警报系统 (ATLAS) 和全景巡天望远镜和快速响应系统 (Pan-STARRS) 分别在 GW190425 合并时间的 1 小时和 3 小时内开始的星图广域光学覆盖。最近，考虑到 GW190425 和快速无线电爆发 FRB 20190425A 的空间和时间巧合，有人提出它们之间可能存在巧合。 FRB 20190425A 较小的天空定位区域及其色散测量导致在 141 ± 10 Mpc 距离处识别出可能的宿主星系 UGC 10667。我们的光学成像在检测到 GW190425 后 6.0 小时和 FRB 20190425A 后 3.5 小时覆盖了该星系。没有检测到光学发射，并且+1.2和+13.2天的进一步成像也显示没有发射。如果 FRB 20190425A 和 GW190425 关联是真实的，我们会在 UGC 10667 中强调对 BNS 合并产生的千新星发射的限制。从 BNS 合并产生 FRB 20190425A 的模型涉及一颗超大质量磁化中子星，在数小时的时间尺度上通过偶极子发射而旋转。我们证明磁星增强的千新星发射被光学上限排除。 UGC 10667 中缺乏检测到的千新星光发射，不利于但并不反驳该源的 FRB-GW 链路。
GW190425 is the second of two binary neutron star (BNS) merger events to be significantly detected by the Laser Interferometer Gravitational Wave (GW) Observatory (LIGO), Virgo and the Kamioka Gravitational Wave (KAGRA) detector network. With a detection only in LIGO Livingston, the skymap containing the source was large and no plausible electromagnetic counterpart was found in real-time searching in 2019. Here, we summarize Asteroid Terrestrial-Impact Last Alert System (ATLAS) and Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) wide-field optical coverage of the skymap beginning within 1 and 3 h, respectively, of the GW190425 merger time. More recently, a potential coincidence between GW190425 and a fast radio burst FRB 20190425A has been suggested, given their spatial and temporal coincidences. The smaller sky localization area of FRB 20190425A and its dispersion measure led to the identification of a likely host galaxy, UGC 10667 at a distance of 141 ± 10 Mpc. Our optical imaging covered the galaxy 6.0 h after GW190425 was detected and 3.5 h after the FRB 20190425A. No optical emission was detected and further imaging at +1.2 and +13.2 d also revealed no emission. If the FRB 20190425A and GW190425 association were real, we highlight our limits on kilonova emission from a BNS merger in UGC 10667. The model for producing FRB 20190425A from a BNS merger involves a supramassive magnetized neutron star spinning down by dipole emission on the time-scale of hours. We show that magnetar-enhanced kilonova emission is ruled out by optical upper limits. The lack of detected optical emission from a kilonova in UGC 10667 disfavours, but does not disprove, the FRB–GW link for this source.