J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817
The first detected gravitational wave from a neutron star merger was GW170817. In this study, we present J-GEM follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5-mag decline in the \(z\)-band from 1.7 days to 7.7 days after the merger. Such a rapid decli...
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| creator | 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, François 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 the J-GEM collaboration |
| description | The first detected gravitational wave from a neutron star merger was GW170817. In this study, we present J-GEM follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5-mag decline in the \(z\)-band from 1.7 days to 7.7 days 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 for later epochs; the \(z-H\) color changed by approximately 2.5 mag in the period of 0.7 days to 7.7 days. The rapid evolution of both the optical brightness and the color 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 the ejecta mass of 0.01 \(\Msun\), which suggests a more intense mass ejection (\(\sim 0.03 \Msun\)) or possibly an additional energy source. |
| doi_str_mv | 10.48550/arxiv.1710.05848 |
| format | Article |
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In this study, we present J-GEM follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5-mag decline in the \(z\)-band from 1.7 days to 7.7 days 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 for later epochs; the \(z-H\) color changed by approximately 2.5 mag in the period of 0.7 days to 7.7 days. The rapid evolution of both the optical brightness and the color 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 the ejecta mass of 0.01 \(\Msun\), which suggests a more intense mass ejection (\(\sim 0.03 \Msun\)) or possibly an additional energy source.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1710.05848</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Brightness ; Color ; Ejecta ; Gravitational waves ; Light curve ; Neutron stars ; Neutrons ; Nuclear fusion ; Nuclei (nuclear physics) ; Optical properties ; Physics - High Energy Astrophysical Phenomena ; Radioactive decay ; Star mergers ; Supernovae</subject><ispartof>arXiv.org, 2017-10</ispartof><rights>2017. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.1093/pasj/psx118$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1710.05848$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Utsumi, Yousuke</creatorcontrib><creatorcontrib>Tanaka, Masaomi</creatorcontrib><creatorcontrib>Tominaga, Nozomu</creatorcontrib><creatorcontrib>Yoshida, Michitoshi</creatorcontrib><creatorcontrib>Barway, Sudhanshu</creatorcontrib><creatorcontrib>Nagayama, Takahiro</creatorcontrib><creatorcontrib>Zenko, Tetsuya</creatorcontrib><creatorcontrib>Aoki, Kentaro</creatorcontrib><creatorcontrib>Fujiyoshi, Takuya</creatorcontrib><creatorcontrib>Furusawa, Hisanori</creatorcontrib><creatorcontrib>Kawabata, Koji S</creatorcontrib><creatorcontrib>Koshida, Shintaro</creatorcontrib><creatorcontrib>Lee, Chien-Hsiu</creatorcontrib><creatorcontrib>Morokuma, Tomoki</creatorcontrib><creatorcontrib>Motohara, Kentaro</creatorcontrib><creatorcontrib>Nakata, Fumiaki</creatorcontrib><creatorcontrib>Ohsawa, Ryou</creatorcontrib><creatorcontrib>Ohta, Kouji</creatorcontrib><creatorcontrib>Okita, Hirofumi</creatorcontrib><creatorcontrib>Tajitsu, Akito</creatorcontrib><creatorcontrib>Tanaka, Ichi</creatorcontrib><creatorcontrib>Terai, Tsuyoshi</creatorcontrib><creatorcontrib>Yasuda, Naoki</creatorcontrib><creatorcontrib>Abe, Fumio</creatorcontrib><creatorcontrib>Asakura, Yuichiro</creatorcontrib><creatorcontrib>Bond, Ian A</creatorcontrib><creatorcontrib>Miyazaki, Shota</creatorcontrib><creatorcontrib>Sumi, Takahiro</creatorcontrib><creatorcontrib>Tristram, Paul J</creatorcontrib><creatorcontrib>Honda, Satoshi</creatorcontrib><creatorcontrib>Itoh, Ryosuke</creatorcontrib><creatorcontrib>Itoh, Yoichi</creatorcontrib><creatorcontrib>Kawabata, Miho</creatorcontrib><creatorcontrib>Morihana, Kumiko</creatorcontrib><creatorcontrib>Nagashima, Hiroki</creatorcontrib><creatorcontrib>Nakaoka, Tatsuya</creatorcontrib><creatorcontrib>Ohshima, Tomohito</creatorcontrib><creatorcontrib>Takahashi, Jun</creatorcontrib><creatorcontrib>Takayama, Masaki</creatorcontrib><creatorcontrib>Aoki, Wako</creatorcontrib><creatorcontrib>Baar, Stefan</creatorcontrib><creatorcontrib>Doi, Mamoru</creatorcontrib><creatorcontrib>Finet, François</creatorcontrib><creatorcontrib>Kanda, Nobuyuki</creatorcontrib><creatorcontrib>Kawai, Nobuyuki</creatorcontrib><creatorcontrib>Kim, Ji Hoon</creatorcontrib><creatorcontrib>Kuroda, Daisuke</creatorcontrib><creatorcontrib>Liu, Wei</creatorcontrib><creatorcontrib>Matsubayashi, Kazuya</creatorcontrib><creatorcontrib>Murata, Katsuhiro L</creatorcontrib><creatorcontrib>Nagai, Hiroshi</creatorcontrib><creatorcontrib>Saito, Tomoki</creatorcontrib><creatorcontrib>Saito, Yoshihiko</creatorcontrib><creatorcontrib>Sako, Shigeyuki</creatorcontrib><creatorcontrib>Sekiguchi, Yuichiro</creatorcontrib><creatorcontrib>Tamura, Yoichi</creatorcontrib><creatorcontrib>Tanaka, Masayuki</creatorcontrib><creatorcontrib>Uemura, Makoto</creatorcontrib><creatorcontrib>Yamaguchi, Masaki S</creatorcontrib><creatorcontrib>the J-GEM collaboration</creatorcontrib><title>J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817</title><title>arXiv.org</title><description>The first detected gravitational wave from a neutron star merger was GW170817. In this study, we present J-GEM follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5-mag decline in the \(z\)-band from 1.7 days to 7.7 days 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 for later epochs; the \(z-H\) color changed by approximately 2.5 mag in the period of 0.7 days to 7.7 days. The rapid evolution of both the optical brightness and the color 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 the ejecta mass of 0.01 \(\Msun\), which suggests a more intense mass ejection (\(\sim 0.03 \Msun\)) or possibly an additional energy source.</description><subject>Brightness</subject><subject>Color</subject><subject>Ejecta</subject><subject>Gravitational waves</subject><subject>Light curve</subject><subject>Neutron stars</subject><subject>Neutrons</subject><subject>Nuclear fusion</subject><subject>Nuclei (nuclear physics)</subject><subject>Optical properties</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Radioactive decay</subject><subject>Star 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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, François ; 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 ; the J-GEM 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Hoon</creatorcontrib><creatorcontrib>Kuroda, Daisuke</creatorcontrib><creatorcontrib>Liu, Wei</creatorcontrib><creatorcontrib>Matsubayashi, Kazuya</creatorcontrib><creatorcontrib>Murata, Katsuhiro L</creatorcontrib><creatorcontrib>Nagai, Hiroshi</creatorcontrib><creatorcontrib>Saito, Tomoki</creatorcontrib><creatorcontrib>Saito, Yoshihiko</creatorcontrib><creatorcontrib>Sako, Shigeyuki</creatorcontrib><creatorcontrib>Sekiguchi, Yuichiro</creatorcontrib><creatorcontrib>Tamura, Yoichi</creatorcontrib><creatorcontrib>Tanaka, Masayuki</creatorcontrib><creatorcontrib>Uemura, Makoto</creatorcontrib><creatorcontrib>Yamaguchi, Masaki S</creatorcontrib><creatorcontrib>the J-GEM collaboration</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Utsumi, Yousuke</au><au>Tanaka, Masaomi</au><au>Tominaga, Nozomu</au><au>Yoshida, Michitoshi</au><au>Barway, Sudhanshu</au><au>Nagayama, Takahiro</au><au>Zenko, Tetsuya</au><au>Aoki, Kentaro</au><au>Fujiyoshi, Takuya</au><au>Furusawa, Hisanori</au><au>Kawabata, Koji S</au><au>Koshida, Shintaro</au><au>Lee, Chien-Hsiu</au><au>Morokuma, Tomoki</au><au>Motohara, Kentaro</au><au>Nakata, Fumiaki</au><au>Ohsawa, Ryou</au><au>Ohta, Kouji</au><au>Okita, Hirofumi</au><au>Tajitsu, Akito</au><au>Tanaka, Ichi</au><au>Terai, Tsuyoshi</au><au>Yasuda, Naoki</au><au>Abe, Fumio</au><au>Asakura, Yuichiro</au><au>Bond, Ian A</au><au>Miyazaki, Shota</au><au>Sumi, Takahiro</au><au>Tristram, Paul J</au><au>Honda, Satoshi</au><au>Itoh, Ryosuke</au><au>Itoh, Yoichi</au><au>Kawabata, Miho</au><au>Morihana, Kumiko</au><au>Nagashima, Hiroki</au><au>Nakaoka, Tatsuya</au><au>Ohshima, Tomohito</au><au>Takahashi, Jun</au><au>Takayama, Masaki</au><au>Aoki, Wako</au><au>Baar, Stefan</au><au>Doi, Mamoru</au><au>Finet, François</au><au>Kanda, Nobuyuki</au><au>Kawai, Nobuyuki</au><au>Kim, Ji Hoon</au><au>Kuroda, Daisuke</au><au>Liu, Wei</au><au>Matsubayashi, Kazuya</au><au>Murata, Katsuhiro L</au><au>Nagai, Hiroshi</au><au>Saito, Tomoki</au><au>Saito, Yoshihiko</au><au>Sako, Shigeyuki</au><au>Sekiguchi, Yuichiro</au><au>Tamura, Yoichi</au><au>Tanaka, Masayuki</au><au>Uemura, Makoto</au><au>Yamaguchi, Masaki S</au><au>the J-GEM collaboration</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817</atitle><jtitle>arXiv.org</jtitle><date>2017-10-16</date><risdate>2017</risdate><eissn>2331-8422</eissn><abstract>The first detected gravitational wave from a neutron star merger was GW170817. In this study, we present J-GEM follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5-mag decline in the \(z\)-band from 1.7 days to 7.7 days 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 for later epochs; the \(z-H\) color changed by approximately 2.5 mag in the period of 0.7 days to 7.7 days. The rapid evolution of both the optical brightness and the color 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 the ejecta mass of 0.01 \(\Msun\), which suggests a more intense mass ejection (\(\sim 0.03 \Msun\)) or possibly an additional energy source.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1710.05848</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2017-10 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1710_05848 |
| source | arXiv.org; Free E- Journals |
| subjects | Brightness Color Ejecta Gravitational waves Light curve Neutron stars Neutrons Nuclear fusion Nuclei (nuclear physics) Optical properties Physics - High Energy Astrophysical Phenomena Radioactive decay Star mergers Supernovae |
| title | J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817 |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-04T05%3A08%3A53IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=J-GEM%20observations%20of%20an%20electromagnetic%20counterpart%20to%20the%20neutron%20star%20merger%20GW170817&rft.jtitle=arXiv.org&rft.au=Utsumi,%20Yousuke&rft.date=2017-10-16&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.1710.05848&rft_dat=%3Cproquest_arxiv%3E2076318160%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2076318160&rft_id=info:pmid/&rfr_iscdi=true |