Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3
Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3
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DOI：
10.3847/1538-4357/abc335
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发表时间：
2020-06
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通讯作者：
M. Kasliwal;S. Anand;T. Ahumada;R. Stein;A. Carracedo;I. Andreoni;M. Coughlin;L. Singer;E. Kool;K. De;H. Kumar;M. Almualla;Yuhan Yao;M. Bulla;D. Dobie;S. Reusch;D. Perley;S. Cenko;V. Bhalerao;D. Kaplan;J. Sollerman;A. Goobar;C. Copperwheat;E. Bellm;G. Anupama;A. Corsi;S. Nissanke;I. Agudo;A. Bagdasaryan;S. Barway;J. Belicki;J. Bloom;B. Bolin;D. Buckley;K. Burdge;R. Burruss;M. Caballero-Garcia;C. Cannella;A. Castro-Tirado;D. Cook;J. Cooke;V. Cunningham;A. Dahiwale;K. Deshmukh;S. Dichiara;D. Duev;Anirban Dutta;M. Feeney;A. Franckowiak;S. Frederick;C. Fremling;A. Gal-yam;P. Gatkine;Shaon Ghosh;D. Goldstein;V. Golkhou;M. Graham;M. Graham;M. Hankins;G. Helou;Youdong Hu;W. Ip;A. Jaodand;V. Karambelkar;A. Kong;M. Kowalski;Maitreya Khandagale;S. Kulkarni;B. Kumar;R. Laher;K. L. Li;A. Mahabal;F. Masci;Adam A. Miller;M. Mogotsi;S. Mohite;K. Mooley;P. Mróz;J. Newman;C. Ngeow;S. Oates;Atharva Patil;S. Pandey;M. Pavana;E. Pian;R. Riddle;R. Sánchez-Ramírez;Y. Sharma;Avinash Singh;Roger M. Smith;M. Soumagnac;Kirsty Taggart;H. Tan;A. Tzanidakis;E. Troja;A. Valeev;R. Walters;G. Waratkar;S. Webb;P. Yu;Bin-Bin Zhang-Bin;R. Zhou;J. Zolkower
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作者：
M. Kasliwal;S. Anand;T. Ahumada;R. Stein;A. Carracedo;I. Andreoni;M. Coughlin;L. Singer;E. Kool;K. De;H. Kumar;M. Almualla;Yuhan Yao;M. Bulla;D. Dobie;S. Reusch;D. Perley;S. Cenko;V. Bhalerao;D. Kaplan;J. Sollerman;A. Goobar;C. Copperwheat;E. Bellm;G. Anupama;A. Corsi;S. Nissanke;I. Agudo;A. Bagdasaryan;S. Barway;J. Belicki;J. Bloom;B. Bolin;D. Buckley;K. Burdge;R. Burruss;M. Caballero-Garcia;C. Cannella;A. Castro-Tirado;D. Cook;J. Cooke;V. Cunningham;A. Dahiwale;K. Deshmukh;S. Dichiara;D. Duev;Anirban Dutta;M. Feeney;A. Franckowiak;S. Frederick;C. Fremling;A. Gal-yam;P. Gatkine;Shaon Ghosh;D. Goldstein;V. Golkhou;M. Graham;M. Graham;M. Hankins;G. Helou;Youdong Hu;W. Ip;A. Jaodand;V. Karambelkar;A. Kong;M. Kowalski;Maitreya Khandagale;S. Kulkarni;B. Kumar;R. Laher;K. L. Li;A. Mahabal;F. Masci;Adam A. Miller;M. Mogotsi;S. Mohite;K. Mooley;P. Mróz;J. Newman;C. Ngeow;S. Oates;Atharva Patil;S. Pandey;M. Pavana;E. Pian;R. Riddle;R. Sánchez-Ramírez;Y. Sharma;Avinash Singh;Roger M. Smith;M. Soumagnac;Kirsty Taggart;H. Tan;A. Tzanidakis;E. Troja;A. Valeev;R. Walters;G. Waratkar;S. Webb;P. Yu;Bin-Bin Zhang-Bin;R. Zhou;J. Zolkower
我们提出了一个系统的搜索光学对应物，以13引力波（GW）触发涉及至少一个中子星星在LIGO/Virgo的第三次观测运行（O3）。我们用Zwicky瞬态设施（ZTF）搜索了双中子星星（BNS）和中子星星黑洞（NSBH）合并定位，并与观测瞬态发生的全球中继观测站（GROWTH）合作进行了后续工作。GW触发器的平均定位面积为4480 deg 2，平均距离为267 Mpc，误报率为1.5 - 10−25 yr−1。在g和r波段的ZTF覆盖范围的中位数封闭概率为39%，中位数深度为20.8等，合并和开始观测之间的中位数时间差为1.5 hr.O3后续由增长团队包括340紫外/光学/红外（UVOIR）测光点，64 OIR光谱，和三个无线电图像使用17个不同的望远镜。我们没有找到有前途的kilonovae（放射性供电的同行），我们展示了如何转换的上限，以约束底层kilonova光度函数。最初，我们假设所有的GW触发器是真正的天体物理事件，无论误报率和kilonovae伴随BNS和NSBH合并是从一个共同的人口，后来，我们放松了这些假设。假设所有的千新星都至少和发现的GW 170817等（-16.1等）一样亮，我们计算出检测到零千新星的联合概率只有4.2%。如果我们假设所有的千新星都比-16.6等（GW 170817的外推峰值星等）亮，并且以1等/天-1的速率衰减（类似于GW 170817），则零探测的联合概率为7%。如果我们根据在线分类将NSBH和BNS星群分开，假设所有千新星都比-16.6等亮，则NSBH和BNS合并的零探测概率分别为9.7%和7.9%。此外，不超过10−4，或θ> 30°才符合我们的极限。我们期待着在第四次GW观测运行中进行搜索;即使是17颗中子星星合并，只有50%的覆盖率达到-16等的深度，也会将明亮千新星的最大比例限制在<25%。
We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo’s third observing run (O3). We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization area of 4480 deg2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10−25 yr−1. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (−16.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than −16.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day−1 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than −16.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than 10−4, or ϕ > 30° to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of −16 mag would constrain the maximum fraction of bright kilonovae to <25%.