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Eextaemely Lumnous Supernova 2006gy at Late Phase: Detection of Optical Emission From Supernova

https://hiroshima.repo.nii.ac.jp/records/2006336
https://hiroshima.repo.nii.ac.jp/records/2006336
1edde91b-1eb2-4c6a-b987-e9cc7561e2df
名前 / ファイル ライセンス アクション
ApJ_697_747.pdf ApJ_697_747.pdf (1.3 MB)
Item type デフォルトアイテムタイプ_(フル)(1)
公開日 2023-03-18
タイトル
タイトル Eextaemely Lumnous Supernova 2006gy at Late Phase: Detection of Optical Emission From Supernova
言語 en
作成者 Kawabata, Koji

× Kawabata, Koji

en Kawabata, Koji

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Tanaka, Masaomi

× Tanaka, Masaomi

en Tanaka, Masaomi

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Maeda, Keiichi

× Maeda, Keiichi

en Maeda, Keiichi

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Hattori, Takashi

× Hattori, Takashi

en Hattori, Takashi

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Nomoto, Ken'ichi

× Nomoto, Ken'ichi

en Nomoto, Ken'ichi

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Tominaga, Nozomu

× Tominaga, Nozomu

en Tominaga, Nozomu

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Yamanaka, Masayuki

× Yamanaka, Masayuki

en Yamanaka, Masayuki

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アクセス権
アクセス権 open access
アクセス権URI http://purl.org/coar/access_right/c_abf2
主題
主題Scheme Other
主題 supernovae
主題
主題Scheme Other
主題 general
主題
主題Scheme Other
主題 supernovae
主題
主題Scheme Other
主題 individual (SN 2006gy)
主題
主題Scheme NDC
主題 440
内容記述
内容記述 Supernova (SN) 2006gy is an extremely luminous Type IIn SN characterized by the bright peak magnitude M-R similar to -22 mag and its long duration. The mechanism giving rise to its huge luminosity is still unclear. We performed optical spectroscopy and photometry of SN 2006gy at late time, similar to 400 days after the explosion, with the Subaru/FOCAS in a good seeing condition. We carefully extracted the SN component, although there is an ambiguity because of the contamination by bright nucleus of the host galaxy. We found that the SN faded by similar to 3 mag from similar to 200 to similar to 400 days after the explosion (i.e., by similar to 5 mag from peak to similar to 400 days) in R band. The overall light curve is marginally consistent with the Ni-56 heating model, although the flattening around 200 days suggests the optical flux declined more steeply between similar to 200 and similar to 400 days. The late time spectrum was quite peculiar among all types of SNe. It showed many intermediate width (similar to 2000 km s(-1) FWHM) emission lines, e. g., [Fe II], [Ca II], and Ca II. The absence of the broad [O I] 6300, 6364 line and weakness of [Fe II] and [Ca II] lines compared with Ca II IR triplet would be explained by a moderately high electron density in the line emitting region. This high-density assumption seems to be consistent with the large amount of ejecta and low expansion velocity of SN 2006gy. The H alpha line luminosity was as small as similar to 1 x 10(39) erg s(-1), being comparable with those of normal Type II SNe at similar epochs. Our observation indicates that the strong circumstellar medium interaction had almost finished by similar to 400 days. If the late time optical flux is purely powered by radioactive decay, at least M(Ni-56) similar to 3 M-circle dot should be produced at the SN explosion. In the late phase spectrum, there were several unusual emission lines at 7400 angstrom-8800 angstrom and some of them might be due to Ti or Ni synthesized at the explosion.
言語 en
出版者
出版者 Iop Publishing Ltd
言語
言語 eng
資源タイプ
資源タイプ識別子 http://purl.org/coar/resource_type/c_6501
資源タイプ journal article
出版タイプ
出版タイプ AO
出版タイプResource http://purl.org/coar/version/c_b1a7d7d4d402bcce
関連情報
識別子タイプ DOI
関連識別子 10.1088/0004-637X/697/1/747
関連情報
識別子タイプ DOI
関連識別子 http://dx.doi.org/10.1088/0004-637X/697/1/747
収録物識別子
収録物識別子タイプ ISSN
収録物識別子 0004-637X
収録物識別子
収録物識別子タイプ NCID
収録物識別子 AA00553275
開始ページ
開始ページ 747
書誌情報 Astrophysical Journal
Astrophysical Journal

巻 697, 号 1, p. 747-757, 発行日 2009
旧ID 27691
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