Optical follow-up observation for GW event S190510g using Subaru/Hyper Suprime-Cam

Abstract A gravitational wave event, S190510g, which was classified as a binary-neutron-star coalescence at the time of preliminary alert, was detected by LIGO/Virgo collaboration on 2019 May 10. At 1.7 hours after the issue of its preliminary alert, we started a target-of-opportunity imaging observ...

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Veröffentlicht in:Publications of the Astronomical Society of Japan 2021-04, Vol.73 (2), p.350-364
Hauptverfasser: Ohgami, Takayuki, Tominaga, Nozomu, Utsumi, Yousuke, Niino, Yuu, Tanaka, Masaomi, Banerjee, Smaranika, Hamasaki, Ryo, Yoshida, Michitoshi, Terai, Tsuyoshi, Takagi, Yuhei, Morokuma, Tomoki, Sasada, Mahito, Akitaya, Hiroshi, Yasuda, Naoki, Yanagisawa, Kenshi, Ohsawa, Ryou
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container_issue 2
container_start_page 350
container_title Publications of the Astronomical Society of Japan
container_volume 73
creator Ohgami, Takayuki
Tominaga, Nozomu
Utsumi, Yousuke
Niino, Yuu
Tanaka, Masaomi
Banerjee, Smaranika
Hamasaki, Ryo
Yoshida, Michitoshi
Terai, Tsuyoshi
Takagi, Yuhei
Morokuma, Tomoki
Sasada, Mahito
Akitaya, Hiroshi
Yasuda, Naoki
Yanagisawa, Kenshi
Ohsawa, Ryou
description Abstract A gravitational wave event, S190510g, which was classified as a binary-neutron-star coalescence at the time of preliminary alert, was detected by LIGO/Virgo collaboration on 2019 May 10. At 1.7 hours after the issue of its preliminary alert, we started a target-of-opportunity imaging observation in the Y band to search for its optical counterpart using the Hyper Suprime-Cam (HSC) on the Subaru Telescope. The observation covers a 118.8 deg2 sky area corresponding to $11.6\%$ confidence in the localization skymap released in the preliminary alert and $1.2\%$ in the updated skymap. We divided the observed area into two fields based on the availability of HSC reference images. For the fields with the HSC reference images, we applied an image subtraction technique; for the fields without the HSC reference images, we sought individual HSC images by matching a catalog of observed objects with the PS1 catalog. The search depth is 22.28 mag in the former method and the limit of search depth is 21.3 mag in the latter method. Subsequently, we performed visual inspection and obtained 83 candidates using the former method and 50 candidates using the latter method. Since we only have the one-day photometric data, we evaluated the probability of candidates being located inside the 3D skymap by estimating their distances with photometry of associated extended objects. We found three candidates are likely located inside the 3D skymap and concluded they could be a counterpart of S190510g, while most of the 133 candidates were likely to be supernovae because the number density of candidates was consistent with the expected number of supernova detections. By comparing our observational depth with a light-curve model of such a kilonova reproducing AT2017gfo, we show that early deep observations with the Subaru/HSC can capture the rising phase of the blue component of a kilonova at the estimated distance of S190510g (∼230 Mpc).
doi_str_mv 10.1093/pasj/psab002
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At 1.7 hours after the issue of its preliminary alert, we started a target-of-opportunity imaging observation in the Y band to search for its optical counterpart using the Hyper Suprime-Cam (HSC) on the Subaru Telescope. The observation covers a 118.8 deg2 sky area corresponding to $11.6\%$ confidence in the localization skymap released in the preliminary alert and $1.2\%$ in the updated skymap. We divided the observed area into two fields based on the availability of HSC reference images. For the fields with the HSC reference images, we applied an image subtraction technique; for the fields without the HSC reference images, we sought individual HSC images by matching a catalog of observed objects with the PS1 catalog. The search depth is 22.28 mag in the former method and the limit of search depth is 21.3 mag in the latter method. Subsequently, we performed visual inspection and obtained 83 candidates using the former method and 50 candidates using the latter method. Since we only have the one-day photometric data, we evaluated the probability of candidates being located inside the 3D skymap by estimating their distances with photometry of associated extended objects. We found three candidates are likely located inside the 3D skymap and concluded they could be a counterpart of S190510g, while most of the 133 candidates were likely to be supernovae because the number density of candidates was consistent with the expected number of supernova detections. By comparing our observational depth with a light-curve model of such a kilonova reproducing AT2017gfo, we show that early deep observations with the Subaru/HSC can capture the rising phase of the blue component of a kilonova at the estimated distance of S190510g (∼230 Mpc).</description><identifier>ISSN: 0004-6264</identifier><identifier>EISSN: 2053-051X</identifier><identifier>DOI: 10.1093/pasj/psab002</identifier><language>eng</language><publisher>Japan: Oxford University Press</publisher><subject>abundances ; ASTRONOMY AND ASTROPHYSICS ; gravitational waves ; nuclear reactions ; nucleosynthesis ; stars: neutron</subject><ispartof>Publications of the Astronomical Society of Japan, 2021-04, Vol.73 (2), p.350-364</ispartof><rights>The Author(s) 2021. 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Since we only have the one-day photometric data, we evaluated the probability of candidates being located inside the 3D skymap by estimating their distances with photometry of associated extended objects. We found three candidates are likely located inside the 3D skymap and concluded they could be a counterpart of S190510g, while most of the 133 candidates were likely to be supernovae because the number density of candidates was consistent with the expected number of supernova detections. 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subjects abundances
ASTRONOMY AND ASTROPHYSICS
gravitational waves
nuclear reactions
nucleosynthesis
stars: neutron
title Optical follow-up observation for GW event S190510g using Subaru/Hyper Suprime-Cam
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