Follow-up Survey for the Binary Black Hole Merger GW200224_222234 Using Subaru/HSC and GTC/OSIRIS

Medientyp: E-Artikel
Titel: Follow-up Survey for the Binary Black Hole Merger GW200224_222234 Using Subaru/HSC and GTC/OSIRIS
Beteiligte: Ohgami, Takayuki; González, Josefa Becerra; Tominaga, Nozomu; Morokuma, Tomoki; Utsumi, Yousuke; Niino, Yuu; Tanaka, Masaomi; Banerjee, Smaranika; Poidevin, Frédérick; Acosta-Pulido, Jose Antonio; Pérez-Fournon, Ismael; Muñoz-Darias, Teo; Akitaya, Hiroshi; Yanagisawa, Kenshi; Sasada, Mahito; Yoshida, Michitoshi; Simunovic, Mirko; Ohsawa, Ryou; Tanaka, Ichi; Terai, Tsuyoshi; Takagi, Yuhei
Erschienen: American Astronomical Society, 2023
Erschienen in: The Astrophysical Journal
Sprache: Nicht zu entscheiden
DOI: 10.3847/1538-4357/acbd42
ISSN: 0004-637X; 1538-4357
Schlagwörter: Space and Planetary Science ; Astronomy and Astrophysics
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Beschreibung: <jats:title>Abstract</jats:title> <jats:p>The LIGO/Virgo detected a gravitational wave (GW) event, named GW200224_222234 (also known as S200224ca) and classified as a binary-black hole coalescence, on 2020 February 24. Given its relatively small localization skymap (71 deg<jats:sup>2</jats:sup> for a 90% credible region; revised to 50 deg<jats:sup>2</jats:sup> in GWTC-3), we performed target-of-opportunity observations using the Subaru/Hyper Suprime-Cam (HSC) in the <jats:italic>r</jats:italic>2 and <jats:italic>z</jats:italic> bands. Observations were conducted on 2020 February 25 and 28 and March 23, with the first epoch beginning 12.3 hr after the GW detection. The survey covered the highest-probability sky area of 56.6 deg<jats:sup>2</jats:sup>, corresponding to a 91% probability. This was the first deep follow-up (<jats:italic>m</jats:italic> <jats:sub> <jats:italic>r</jats:italic> </jats:sub> ≳ 24, <jats:italic>m</jats:italic> <jats:sub> <jats:italic>z</jats:italic> </jats:sub> ≳ 23) 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 our Subaru/HSC data alone. 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; but we could not identify a unique promising counterpart. If there are no counterparts in the remaining candidates, the upper limits of the optical luminosity are <jats:inline-formula> <jats:tex-math> <?CDATA $\nu {L}_{\nu }\lt {5.2}_{-1.9}^{+2.4}\times {10}^{41}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>ν</mml:mi> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>ν</mml:mi> </mml:mrow> </mml:msub> <mml:mo><</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>5.2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.9</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>2.4</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>41</mml:mn> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjacbd42ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> erg s<jats:sup>−1</jats:sup> and <jats:inline-formula> <jats:tex-math> <?CDATA $\nu {L}_{\nu }\lt {1.8}_{-0.6}^{+0.8}\times {10}^{42}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>ν</mml:mi> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>ν</mml:mi> </mml:mrow> </mml:msub> <mml:mo><</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.8</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>42</mml:mn> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjacbd42ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> erg s<jats:sup>−1</jats:sup> in the <jats:italic>r</jats:italic>2 and <jats:italic>z</jats:italic> bands, respectively, at ∼12 hr after GW detection. We also discuss improvements in the strategies of optical follow-ups for future GW events.</jats:p>
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