Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-19T10:30:24.804Z Has data issue: false hasContentIssue false
  • English
  • Français

ALMA resolved views of molecular filaments/clumps in the Large Magellanic Cloud: A possible gas flow penetrating one of the most massive protocluster systems in the Local Group

Published online by Cambridge University Press:  09 June 2023

Kazuki Tokuda Open the ORCID record for Kazuki Tokuda [Opens in a new window]
Kazuki Tokuda*
Affiliation:
Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University, Nishi-ku, Fukuoka 819-0395, Japan National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present spatially resolved molecular filaments and clumps in the high-mass star-forming regions N159E-Papillon, W-South, and W-North in the Large Magellanic Cloud (LMC). Our ALMA observations in CO isotopes and millimeter continuum revealed remarkable hub-filament systems with a typical width of 0.1 pc. The most massive clump in the observed regions, N159W-North MMS-2, shows an especially massive/dense nature whose total H2 mass and peak column density are ∼104 M⊙ and ∼1024 cm−2, respectively, and harbors massive (∼100 M⊙) starless core candidates. The hub-filamentary clouds in the three regions share a common orientation and have 10–30 pc scale head-tail structures with active star formation at the tips. Their striking similarity proposes a “teardrops-inflow” model, i.e., substructured conversing H i flow, that explains the synchronized, extreme star formation across ∼50 pc, including one of the most massive protocluster clumps in the Local Group.

Keywords

Interstellar filamentsLarge Magellanic CloudProtostarsLocal Group
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 70 - 74
Check for updates
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Fukui, Y., Kawamura, A., Minamidani, T., et al. 2008, ApJS, 178, 56 10.1086/589833CrossRefGoogle Scholar
Fukui, Y., Tsuge, K., Sano, H., et al. 2017, PASJ, 69, L5 10.1093/pasj/psx032CrossRefGoogle Scholar
Tsuge, K., Sano, H., Tachihara, K., et al. 2019, ApJ, 871, 44 10.3847/1538-4357/aaf4fbCrossRefGoogle Scholar
Fukui, Y., Harada, R., Tokuda, K., et al. 2015, ApJL, 807, L4 10.1088/2041-8205/807/1/L4CrossRefGoogle Scholar
Saigo, K., Onishi, T., Nayak, O., et al. 2017, ApJ, 835, 108 10.3847/1538-4357/835/1/108CrossRefGoogle Scholar
Fukui, Y., Tokuda, K., Saigo, K., et al. 2019, ApJ 886, 14 10.3847/1538-4357/ab4900CrossRefGoogle Scholar
Tokuda, K., Fukui, Y., Harada, R., et al. 2019, ApJ, 886, 15 10.3847/1538-4357/ab48ffCrossRefGoogle Scholar
Andr, P., Revret, V., Knyves, V., et al. 2016, A&A, 592, A54 Google Scholar
Tokuda, K., Minami, T., Fukui, Y., et al. 2022, ApJ, 933, 20 10.3847/1538-4357/ac6b3cCrossRefGoogle Scholar
Inoue, T., Hennebelle, P., Fukui, Y., et al. 2018, PASJ, 70, S5310.1093/pasj/psx089CrossRefGoogle Scholar