論文

査読有り
2019年10月

First Subarcsecond Submillimeter-wave [C I] Image of 49 Ceti with ALMA

The Astrophysical Journal
  • Higuchi, Aya E
  • ,
  • Saigo, Kazuya
  • ,
  • Kobayashi, Hiroshi
  • ,
  • Iwasaki, Kazunari
  • ,
  • Momose, Munetake
  • ,
  • Soon, Kang Lou
  • ,
  • Sakai, Nami
  • ,
  • Kunitomo, Masanobu
  • ,
  • Ishihara, Daisuke
  • ,
  • Yamamoto, Satoshi

883
2
開始ページ
180
終了ページ
記述言語
英語
掲載種別
研究論文(学術雑誌)
DOI
10.3847/1538-4357/ab3d26

We present the first subarcsecond images of 49 Ceti in the [C I] <SUP>3</SUP> P <SUB>1</SUB>─<SUP>3</SUP> P <SUB>0</SUB> emission and the 614 μm dust continuum emission observed with Atacama Large Millimeter/submillimeter Array (ALMA), as well as that in the CO(J = 3─2) emission prepared by using the ALMA archival data. The spatial distribution of the 614 μm dust continuum emission is found to have a broad-ring structure with a radius of about 100 au around the central star. A substantial amount of gas is also associated with 49 Ceti. The [C I] emission map shows two peaks inside the dust ring, and its overall extent is comparable to that of the dust continuum emission and the CO emission. We find that the [C I]/CO(J = 3─2) intensity ratio significantly varies along the major axis. The ratio takes the minimum value of 1.8 around the dust peak position, and increases inward and outward. The enhanced ratio around the central star (∼3) likely originates from the stellar UV radiation, while that in the outer disk (∼10) is from the interstellar UV radiation. Such complex distributions of the [C I] and CO(J = 3─2) emission will be key to understanding the origin of the gas in 49 Ceti, and will also provide a stringent constraint on physical and chemical models of gaseous debris disks....

リンク情報
DOI
https://doi.org/10.3847/1538-4357/ab3d26
arXiv
http://arxiv.org/abs/arXiv:1908.07032
URL
http://orcid.org/0000-0002-1932-3358
ID情報
  • DOI : 10.3847/1538-4357/ab3d26
  • ORCIDのPut Code : 62755756
  • arXiv ID : arXiv:1908.07032
  • BibTex Code : 2019ApJ...883..180H

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