Giant molecular cloud formation at the interface of colliding supershells in the large magellanic cloud

Kosuke Fujii*, Norikazu Mizuno, J. R. Dawson, Tsuyoshi Inoue, Kazufumi Torii, Toshikazu Onishi, Akiko Kawamura, Erik Muller, Tetsuhiro Minamidani, Kisetsu Tsuge, Yasuo Fukui

*Corresponding author for this work

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Abstract

We investigate the H i envelope of the young, massive GMCs in the star-forming regions N48 and N49, which are located within the high column density H i ridge between two kpc-scale supergiant shells, LMC 4 and LMC 5. New long-baseline H i 21 cm line observations with the Australia Telescope Compact Array (ATCA) were combined with archival shorter baseline data and single dish data from the Parkes telescope, for a final synthesized beam size of 24.75 arcsec by 20.48 arcsec, which corresponds to a spatial resolution of ∼6 pc in the LMC. It is newly revealed that the H i gas is highly filamentary and that the molecular clumps are distributed along filamentary H i features. In total 39 filamentary features are identified and their typical width is ∼21 (8-49) [pc]. We propose a scenario in which the GMCs were formed via gravitational instabilities in atomic gas which was initially accumulated by the two shells and then further compressed by their collision. This suggests that GMC formation involves the filamentary nature of the atomic medium.

Original languageEnglish
Pages (from-to)459-479
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume505
Issue number1
DOIs
Publication statusPublished - 1 Jul 2021

Bibliographical note

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 505, Issue 1, July 2021, Pages 459–479, https://doi.org/10.1093/mnras/stab1202. Copyright 2021 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Keywords

  • galaxies: star formation
  • ISM: bubbles
  • ISM: clouds
  • ISM: structure
  • Magellanic Clouds
  • radio lines: ISM

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