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CO / CI observations of N83C in the early stage of star formation in SMC with ALMA

Published online by Cambridge University Press:  30 October 2019

Sarolta Zahorecz ,
Toshikazu Onishi ,
Kazuyuki Muraoka ,
Aya Homma ,
Ryohei Harada ,
Shota Takada ,
Hiroyuki Maezawa ,
Kazuki Tokuda ,
Kazuya Saigo  and
Akiko Kawamura
...Show all authors
Sarolta Zahorecz
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Toshikazu Onishi
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Kazuyuki Muraoka
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Aya Homma
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Ryohei Harada
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Shota Takada
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Hiroyuki Maezawa
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp
Kazuki Tokuda
Affiliation:
Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan email: s.zahorecz@p.s.osakafu-u.ac.jp Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Kazuya Saigo
Affiliation:
Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Akiko Kawamura
Affiliation:
Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Norikazu Mizuno
Affiliation:
Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Tetsuhiro Minamidani
Affiliation:
Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Margaret Meixner
Affiliation:
Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
Remy Indebetouw
Affiliation:
Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USA National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
Marta Sewilo
Affiliation:
NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA
Yasuo Fukui
Affiliation:
Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan
Alberto Bolatto
Affiliation:
Astronomy Department and Laboratory for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742, USA
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Abstract

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The Magellanic Clouds offer the opportunity to obtain a spatially resolved view of external galaxies at reduced metallicity with no distance ambiguity. Our ALMA observations of the active star-forming region N83C in the Small Magellanic Cloud (SMC) revealed subparsec-scale molecular structures in 12CO and 13CO (2-1) emission Muraoka et al. (2017). We found strong CO peaks associated with Young Stellar Objects(YSOs) and derived a typical gas density of ∽104 cm−3 and gas temperature of 40-60 K from the excitation analysis. The high gas density and temperature are presumably due to the effect of the HII region under the low-metallicity environment. We have found that the column density ratios N(CI)/N(CO) are generally high throughout the cloud compared with the Galaxy, ranging from 0.2 to 2.0. A peak of the ratio is observed toward a CO peak associated with a massive protostar.

Keywords

ISM: structuregalaxies: dwarfMagellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 313 - 315
Copyright
© International Astronomical Union 2019 

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