J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817

Yousuke Utsumi; Masaomi Tanaka; Nozomu Tominaga; Michitoshi Yoshida; Sudhanshu Barway; Takahiro Nagayama; Tetsuya Zenko; Kentaro Aoki; Takuya Fujiyoshi; Hisanori Furusawa; Koji S. Kawabata; Shintaro Koshida; Chien Hsiu Lee; Tomoki Morokuma; Kentaro Motohara; Fumiaki Nakata; Ryou Ohsawa; Kouji Ohta; Hirofumi Okita; Akito Tajitsu; Ichi Tanaka; Tsuyoshi Terai; Naoki Yasuda; Fumio Abe; Yuichiro Asakura; Ian A. Bond; Shota Miyazaki; Takahiro Sumi; Paul J. Tristram; Satoshi Honda; Ryosuke Itoh; Yoichi Itoh; Miho Kawabata; Kumiko Morihana; Hiroki Nagashima; Tatsuya Nakaoka; Tomohito Ohshima; Jun Takahashi; Masaki Takayama; Wako Aoki; Stefan Baar; Mamoru Doi; Francois Finet; Nobuyuki Kanda; Nobuyuki Kawai; Ji Hoon Kim; Daisuke Kuroda; Wei Liu; Kazuya Matsubayashi; Katsuhiro L. Murata; Hiroshi Nagai; Tomoki Saito; Yoshihiko Saito; Shigeyuki Sako; Yuichiro Sekiguchi; Yoichi Tamura; Masayuki Tanaka; Makoto Uemura; Masaki S. Yamaguchi

doi:10.1093/pasj/psx118

J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817

Yousuke Utsumi, Masaomi Tanaka, Nozomu Tominaga, Michitoshi Yoshida, Sudhanshu Barway, Takahiro Nagayama, Tetsuya Zenko, Kentaro Aoki, Takuya Fujiyoshi, Hisanori Furusawa, Koji S. Kawabata, Shintaro Koshida, Chien Hsiu Lee, Tomoki Morokuma, Kentaro Motohara, Fumiaki Nakata, Ryou Ohsawa, Kouji Ohta, Hirofumi Okita, Akito TajitsuIchi Tanaka, Tsuyoshi Terai, Naoki Yasuda, Fumio Abe, Yuichiro Asakura, Ian A. Bond, Shota Miyazaki, Takahiro Sumi, Paul J. Tristram, Satoshi Honda, Ryosuke Itoh, Yoichi Itoh, Miho Kawabata, Kumiko Morihana, Hiroki Nagashima, Tatsuya Nakaoka, Tomohito Ohshima, Jun Takahashi, Masaki Takayama, Wako Aoki, Stefan Baar, Mamoru Doi, Francois Finet, Nobuyuki Kanda, Nobuyuki Kawai, Ji Hoon Kim, Daisuke Kuroda, Wei Liu, Kazuya Matsubayashi, Katsuhiro L. Murata, Hiroshi Nagai, Tomoki Saito, Yoshihiko Saito, Shigeyuki Sako, Yuichiro Sekiguchi, Yoichi Tamura, Masayuki Tanaka, Makoto Uemura, Masaki S. Yamaguchi

理学研究科・天文学専攻

研究成果: Article › 査読

72 被引用数 (Scopus)

抄録

GW170817 is the first detected gravitational wave source from a neutron star merger. We present the Japanese collaboration for gravitational-wave electro-magnetic (J-GEM) follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5mag decline in the z band during the period between 1.7 and 7.7 d after the merger. Such a rapid decline is not comparable with supernovae light curves at any epoch. The color of SSS17a also evolves rapidly and becomes redder during later epochs: the z - H color has changed by approximately 2.5mag during the period between 0.7 and 7.7 d. The rapid evolutions of both the color and the optical brightness are consistent with the expected properties of a kilonova that is powered by the radioactive decay of newly synthesized r-process nuclei. Kilonova models with Lanthanide elements can reproduce the aforementioned observed properties well, which suggests that r-process nucleosynthesis beyond the second peak takes place in SSS17a. However, the absolute magnitude of SSS17a is brighter than the expected brightness of the kilonova models with an ejectamass of 0.01M⊙, which suggests a more intensemass ejection (~0.03M⊙) or possibly an additional energy source.

本文言語	English
論文番号	101
ジャーナル	Publications of the Astronomical Society of Japan
巻	69
号	6
DOI	https://doi.org/10.1093/pasj/psx118
出版ステータス	Published - 2017

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

文献へのアクセス

10.1093/pasj/psx118

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引用スタイル

Utsumi, Y., Tanaka, M., Tominaga, N., Yoshida, M., Barway, S., Nagayama, T., Zenko, T., Aoki, K., Fujiyoshi, T., Furusawa, H., Kawabata, K. S., Koshida, S., Lee, C. H., Morokuma, T., Motohara, K., Nakata, F., Ohsawa, R., Ohta, K., Okita, H., ... Yamaguchi, M. S. (2017). J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817. Publications of the Astronomical Society of Japan, 69(6), [101]. https://doi.org/10.1093/pasj/psx118

J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817. / Utsumi, Yousuke; Tanaka, Masaomi; Tominaga, Nozomu; Yoshida, Michitoshi; Barway, Sudhanshu; Nagayama, Takahiro; Zenko, Tetsuya; Aoki, Kentaro; Fujiyoshi, Takuya; Furusawa, Hisanori; Kawabata, Koji S.; Koshida, Shintaro; Lee, Chien Hsiu; Morokuma, Tomoki; Motohara, Kentaro; Nakata, Fumiaki; Ohsawa, Ryou; Ohta, Kouji; Okita, Hirofumi; Tajitsu, Akito; Tanaka, Ichi; Terai, Tsuyoshi; Yasuda, Naoki; Abe, Fumio; Asakura, Yuichiro; Bond, Ian A.; Miyazaki, Shota; Sumi, Takahiro; Tristram, Paul J.; Honda, Satoshi; Itoh, Ryosuke; Itoh, Yoichi; Kawabata, Miho; Morihana, Kumiko; Nagashima, Hiroki; Nakaoka, Tatsuya; Ohshima, Tomohito; Takahashi, Jun; Takayama, Masaki; Aoki, Wako; Baar, Stefan; Doi, Mamoru; Finet, Francois; Kanda, Nobuyuki; Kawai, Nobuyuki; Kim, Ji Hoon; Kuroda, Daisuke; Liu, Wei; Matsubayashi, Kazuya; Murata, Katsuhiro L.; Nagai, Hiroshi; Saito, Tomoki; Saito, Yoshihiko; Sako, Shigeyuki; Sekiguchi, Yuichiro; Tamura, Yoichi; Tanaka, Masayuki; Uemura, Makoto; Yamaguchi, Masaki S.

In: Publications of the Astronomical Society of Japan, Vol. 69, No. 6, 101, 2017.

研究成果: Article › 査読

Utsumi, Y, Tanaka, M, Tominaga, N, Yoshida, M, Barway, S, Nagayama, T, Zenko, T, Aoki, K, Fujiyoshi, T, Furusawa, H, Kawabata, KS, Koshida, S, Lee, CH, Morokuma, T, Motohara, K, Nakata, F, Ohsawa, R, Ohta, K, Okita, H, Tajitsu, A, Tanaka, I, Terai, T, Yasuda, N, Abe, F, Asakura, Y, Bond, IA, Miyazaki, S, Sumi, T, Tristram, PJ, Honda, S, Itoh, R, Itoh, Y, Kawabata, M, Morihana, K, Nagashima, H, Nakaoka, T, Ohshima, T, Takahashi, J, Takayama, M, Aoki, W, Baar, S, Doi, M, Finet, F, Kanda, N, Kawai, N, Kim, JH, Kuroda, D, Liu, W, Matsubayashi, K, Murata, KL, Nagai, H, Saito, T, Saito, Y, Sako, S, Sekiguchi, Y, Tamura, Y, Tanaka, M, Uemura, M & Yamaguchi, MS 2017, 'J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817', Publications of the Astronomical Society of Japan, vol. 69, no. 6, 101. https://doi.org/10.1093/pasj/psx118

Utsumi, Yousuke ; Tanaka, Masaomi ; Tominaga, Nozomu ; Yoshida, Michitoshi ; Barway, Sudhanshu ; Nagayama, Takahiro ; Zenko, Tetsuya ; Aoki, Kentaro ; Fujiyoshi, Takuya ; Furusawa, Hisanori ; Kawabata, Koji S. ; Koshida, Shintaro ; Lee, Chien Hsiu ; Morokuma, Tomoki ; Motohara, Kentaro ; Nakata, Fumiaki ; Ohsawa, Ryou ; Ohta, Kouji ; Okita, Hirofumi ; Tajitsu, Akito ; Tanaka, Ichi ; Terai, Tsuyoshi ; Yasuda, Naoki ; Abe, Fumio ; Asakura, Yuichiro ; Bond, Ian A. ; Miyazaki, Shota ; Sumi, Takahiro ; Tristram, Paul J. ; Honda, Satoshi ; Itoh, Ryosuke ; Itoh, Yoichi ; Kawabata, Miho ; Morihana, Kumiko ; Nagashima, Hiroki ; Nakaoka, Tatsuya ; Ohshima, Tomohito ; Takahashi, Jun ; Takayama, Masaki ; Aoki, Wako ; Baar, Stefan ; Doi, Mamoru ; Finet, Francois ; Kanda, Nobuyuki ; Kawai, Nobuyuki ; Kim, Ji Hoon ; Kuroda, Daisuke ; Liu, Wei ; Matsubayashi, Kazuya ; Murata, Katsuhiro L. ; Nagai, Hiroshi ; Saito, Tomoki ; Saito, Yoshihiko ; Sako, Shigeyuki ; Sekiguchi, Yuichiro ; Tamura, Yoichi ; Tanaka, Masayuki ; Uemura, Makoto ; Yamaguchi, Masaki S. / J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817. In: Publications of the Astronomical Society of Japan. 2017 ; Vol. 69, No. 6.

@article{9a088a3b8e1246fba6e7864d69165b88,

title = "J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817",

abstract = "GW170817 is the first detected gravitational wave source from a neutron star merger. We present the Japanese collaboration for gravitational-wave electro-magnetic (J-GEM) follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5mag decline in the z band during the period between 1.7 and 7.7 d after the merger. Such a rapid decline is not comparable with supernovae light curves at any epoch. The color of SSS17a also evolves rapidly and becomes redder during later epochs: the z - H color has changed by approximately 2.5mag during the period between 0.7 and 7.7 d. The rapid evolutions of both the color and the optical brightness are consistent with the expected properties of a kilonova that is powered by the radioactive decay of newly synthesized r-process nuclei. Kilonova models with Lanthanide elements can reproduce the aforementioned observed properties well, which suggests that r-process nucleosynthesis beyond the second peak takes place in SSS17a. However, the absolute magnitude of SSS17a is brighter than the expected brightness of the kilonova models with an ejectamass of 0.01M⊙, which suggests a more intensemass ejection (~0.03M⊙) or possibly an additional energy source.",

keywords = "Abundances, Gravitational waves, Nuclear reactions, Nucleosynthesis, Stars: neutron",

author = "Yousuke Utsumi and Masaomi Tanaka and Nozomu Tominaga and Michitoshi Yoshida and Sudhanshu Barway and Takahiro Nagayama and Tetsuya Zenko and Kentaro Aoki and Takuya Fujiyoshi and Hisanori Furusawa and Kawabata, {Koji S.} and Shintaro Koshida and Lee, {Chien Hsiu} and Tomoki Morokuma and Kentaro Motohara and Fumiaki Nakata and Ryou Ohsawa and Kouji Ohta and Hirofumi Okita and Akito Tajitsu and Ichi Tanaka and Tsuyoshi Terai and Naoki Yasuda and Fumio Abe and Yuichiro Asakura and Bond, {Ian A.} and Shota Miyazaki and Takahiro Sumi and Tristram, {Paul J.} and Satoshi Honda and Ryosuke Itoh and Yoichi Itoh and Miho Kawabata and Kumiko Morihana and Hiroki Nagashima and Tatsuya Nakaoka and Tomohito Ohshima and Jun Takahashi and Masaki Takayama and Wako Aoki and Stefan Baar and Mamoru Doi and Francois Finet and Nobuyuki Kanda and Nobuyuki Kawai and Kim, {Ji Hoon} and Daisuke Kuroda and Wei Liu and Kazuya Matsubayashi and Murata, {Katsuhiro L.} and Hiroshi Nagai and Tomoki Saito and Yoshihiko Saito and Shigeyuki Sako and Yuichiro Sekiguchi and Yoichi Tamura and Masayuki Tanaka and Makoto Uemura and Yamaguchi, {Masaki S.}",

note = "Funding Information: We are grateful to the staff of Subaru Telescope, South African Astronomical Observatory, and University of Canterbury Mt. John Observatory for their help for the observations of this work. We thank Dr. Masato Onodera and Prof. Takashi Nakamura who provided insightful comments, and Dr. Nobuhiro Okabe who provided a computational resource. This work was supported by MEXT KAK-ENHI (JP17H06363, JP15H00788, JP24103003, JP10147214, JP10147207) and JSPS KAKENHI (JP16H02183, JP15H02075, JP15H02069, JP26800103, JP25800103), the research grant program of the Toyota Foundation (D11-R-0830), the natural science grant of the Mitsubishi Foundation, the research grant of the Yamada Science Foundation, the National Institute of Natural Sciences (NINS) program for cross-disciplinary science study, Inoue Science Research Award from Inoue Foundation for Science, Optical & Near-Infrared Astronomy Inter-University Cooperation Program from the MEXT, and the National Research Foundation of South Africa. This work is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, NINS.",

year = "2017",

doi = "10.1093/pasj/psx118",

language = "English",

volume = "69",

journal = "Publications of the Astronomical Society of Japan",

issn = "0004-6264",

publisher = "Astronomical Society of Japan",

number = "6",

}

TY - JOUR

T1 - J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817

AU - Utsumi, Yousuke

AU - Tanaka, Masaomi

AU - Tominaga, Nozomu

AU - Yoshida, Michitoshi

AU - Barway, Sudhanshu

AU - Nagayama, Takahiro

AU - Zenko, Tetsuya

AU - Aoki, Kentaro

AU - Fujiyoshi, Takuya

AU - Furusawa, Hisanori

AU - Kawabata, Koji S.

AU - Koshida, Shintaro

AU - Lee, Chien Hsiu

AU - Morokuma, Tomoki

AU - Motohara, Kentaro

AU - Nakata, Fumiaki

AU - Ohsawa, Ryou

AU - Ohta, Kouji

AU - Okita, Hirofumi

AU - Tajitsu, Akito

AU - Tanaka, Ichi

AU - Terai, Tsuyoshi

AU - Yasuda, Naoki

AU - Abe, Fumio

AU - Asakura, Yuichiro

AU - Bond, Ian A.

AU - Miyazaki, Shota

AU - Sumi, Takahiro

AU - Tristram, Paul J.

AU - Honda, Satoshi

AU - Itoh, Ryosuke

AU - Itoh, Yoichi

AU - Kawabata, Miho

AU - Morihana, Kumiko

AU - Nagashima, Hiroki

AU - Nakaoka, Tatsuya

AU - Ohshima, Tomohito

AU - Takahashi, Jun

AU - Takayama, Masaki

AU - Aoki, Wako

AU - Baar, Stefan

AU - Doi, Mamoru

AU - Finet, Francois

AU - Kanda, Nobuyuki

AU - Kawai, Nobuyuki

AU - Kim, Ji Hoon

AU - Kuroda, Daisuke

AU - Liu, Wei

AU - Matsubayashi, Kazuya

AU - Murata, Katsuhiro L.

AU - Nagai, Hiroshi

AU - Saito, Tomoki

AU - Saito, Yoshihiko

AU - Sako, Shigeyuki

AU - Sekiguchi, Yuichiro

AU - Tamura, Yoichi

AU - Tanaka, Masayuki

AU - Uemura, Makoto

AU - Yamaguchi, Masaki S.

N1 - Funding Information: We are grateful to the staff of Subaru Telescope, South African Astronomical Observatory, and University of Canterbury Mt. John Observatory for their help for the observations of this work. We thank Dr. Masato Onodera and Prof. Takashi Nakamura who provided insightful comments, and Dr. Nobuhiro Okabe who provided a computational resource. This work was supported by MEXT KAK-ENHI (JP17H06363, JP15H00788, JP24103003, JP10147214, JP10147207) and JSPS KAKENHI (JP16H02183, JP15H02075, JP15H02069, JP26800103, JP25800103), the research grant program of the Toyota Foundation (D11-R-0830), the natural science grant of the Mitsubishi Foundation, the research grant of the Yamada Science Foundation, the National Institute of Natural Sciences (NINS) program for cross-disciplinary science study, Inoue Science Research Award from Inoue Foundation for Science, Optical & Near-Infrared Astronomy Inter-University Cooperation Program from the MEXT, and the National Research Foundation of South Africa. This work is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, NINS.

PY - 2017

Y1 - 2017

N2 - GW170817 is the first detected gravitational wave source from a neutron star merger. We present the Japanese collaboration for gravitational-wave electro-magnetic (J-GEM) follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5mag decline in the z band during the period between 1.7 and 7.7 d after the merger. Such a rapid decline is not comparable with supernovae light curves at any epoch. The color of SSS17a also evolves rapidly and becomes redder during later epochs: the z - H color has changed by approximately 2.5mag during the period between 0.7 and 7.7 d. The rapid evolutions of both the color and the optical brightness are consistent with the expected properties of a kilonova that is powered by the radioactive decay of newly synthesized r-process nuclei. Kilonova models with Lanthanide elements can reproduce the aforementioned observed properties well, which suggests that r-process nucleosynthesis beyond the second peak takes place in SSS17a. However, the absolute magnitude of SSS17a is brighter than the expected brightness of the kilonova models with an ejectamass of 0.01M⊙, which suggests a more intensemass ejection (~0.03M⊙) or possibly an additional energy source.

AB - GW170817 is the first detected gravitational wave source from a neutron star merger. We present the Japanese collaboration for gravitational-wave electro-magnetic (J-GEM) follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5mag decline in the z band during the period between 1.7 and 7.7 d after the merger. Such a rapid decline is not comparable with supernovae light curves at any epoch. The color of SSS17a also evolves rapidly and becomes redder during later epochs: the z - H color has changed by approximately 2.5mag during the period between 0.7 and 7.7 d. The rapid evolutions of both the color and the optical brightness are consistent with the expected properties of a kilonova that is powered by the radioactive decay of newly synthesized r-process nuclei. Kilonova models with Lanthanide elements can reproduce the aforementioned observed properties well, which suggests that r-process nucleosynthesis beyond the second peak takes place in SSS17a. However, the absolute magnitude of SSS17a is brighter than the expected brightness of the kilonova models with an ejectamass of 0.01M⊙, which suggests a more intensemass ejection (~0.03M⊙) or possibly an additional energy source.

KW - Abundances

KW - Gravitational waves

KW - Nuclear reactions

KW - Nucleosynthesis

KW - Stars: neutron

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