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Follow-up survey for the binary black hole merger GW200224_222234 using Subaru/HSC and GTC/OSIRIS

The LIGO/Virgo detected a gravitational wave (GW) event, named GW200224_222234 (a.k.a. S200224ca) and classified as a binary-black-hole coalescence, on February 24, 2020. Given its relatively small localization skymap (71 deg\(^2\) for a 90% credible region; revised to 50 deg\(^2\) in GWTC-3), we pe...

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Published in:arXiv.org 2023-02
Main Authors: Ohgami, Takayuki, Josefa Becerra Gonzalez, Tominaga, Nozomu, Morokuma, Tomoki, Utsumi, Yousuke, Niino, Yuu, Tanaka, Masaomi, Banerjee, Smaranika, Poidevin, Frederick, Acosta-Pulido, Jose Antonio, Perez-Fournon, Ismael, Munoz-Darias, Teo, Akitaya, Hiroshi, Yanagisawa, Kenshi, Sasada, Mahito, Yoshida, Michitoshi, Simunovic, Mirko, Ohsawa, Ryou, Tanaka, Ichi, Terai, Tsuyoshi, Takagi, Yuhei, The J-GEM collaboration
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Language:English
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Summary:The LIGO/Virgo detected a gravitational wave (GW) event, named GW200224_222234 (a.k.a. S200224ca) and classified as a binary-black-hole coalescence, on February 24, 2020. Given its relatively small localization skymap (71 deg\(^2\) for a 90% credible region; revised to 50 deg\(^2\) in GWTC-3), we performed target-of-opportunity observations using the Subaru/Hyper Suprime-Cam (HSC) in the \(r2\)- and \(z\)-bands. Observations were conducted on February 25 and 28 and March 23, 2020, with the first epoch beginning 12.3 h after the GW detection. The survey covered the highest probability sky area of 56.6 deg\(^2\), corresponding to a 91% probability. This was the first deep follow-up (\(m_{r}\gtrsim24, m_{z}\gtrsim23\)) for a binary-black-hole merger covering \(>\)90% of the localization. By performing image subtraction and candidate screening including light curve fitting with transient templates and examples, we found 22 off-nucleus transients that were not ruled out as the counterparts of GW200224_222234 with only our Subaru/HSC data. We also performed GTC/OSIRIS spectroscopy of the probable host galaxies for five candidates; two are likely to be located within the 3D skymap, whereas the others are not. In conclusion, 19 transients remain as possible optical counterparts of GW200224_222234; however, we could not identify a unique promising counterpart. If there are no counterparts in the remaining candidates, the upper limits of optical luminosity are \(\nu L_{\nu} < 5.2^{+2.4}_{-1.9}\times 10^{41}\) erg s\(^{-1}\) and \(\nu L_{\nu} < 1.8^{+0.8}_{-0.6}\times 10^{42}\) erg s\(^{-1}\) in the \(r2\)- and \(z\)-bands, respectively, at \(\sim\)12 h after GW detection. We also discuss improvements in the strategies of optical follow-ups for future GW events.
ISSN:2331-8422
DOI:10.48550/arxiv.2302.09269