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Title: KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA

Abstract

We present the ALMA Band 3 and Band 6 results of {sup 12}CO(2-1), {sup 13}CO(2-1), H30 α recombination line, free–free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star-forming face-on galaxy at a distance of 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ∼1 pc and several parsecs. The total molecular mass is 0.92 × 10{sup 5} M {sub ⊙} from the {sup 13}CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation H ii region. We found that a YSO associated with the Papillon Nebula has the mass of 35 M {sub ⊙} and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. reported a similar kinematic structure toward two YSOs in the N159 West region, which are the other YSOs that have the mass of ≳35 M {sub ⊙}. This suggests thatmore » the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with a sub-parsec scale. It is filled by free–free and H30 α emission. The temperature of the molecular gas around the hole reaches ∼80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.« less

Authors:
; ;  [1]; ; ;  [2]; ;  [3];  [4];  [5]; ; ; ; ;  [6];  [7];  [8]; ;  [9];  [10] more »; « less
  1. Chile Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
  2. Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531 (Japan)
  3. The Johns Hopkins University, Department of Physics and Astronomy, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218 (United States)
  4. NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 (United States)
  5. Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904 (United States)
  6. Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-8602 (Japan)
  7. Nobeyama Radio Observatory, 462-2 Nobeyama Minamimaki-mura, Minamisaku-gun, Nagano 384-1305 (Japan)
  8. Division of Theoretical Astronomy, National Astronomical Observatory (Japan)
  9. Laboratoire AIM, CEA, Universite Paris VII, IRFU/Service d’Astrophysique, Bat. 709, F-91191 Gif-sur-Yvette (France)
  10. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA (United Kingdom)
Publication Date:
OSTI Identifier:
22664005
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 835; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CARBON 12; CARBON 13; CARBON MONOXIDE; COLLISIONS; DUSTS; EMISSION; EXCITATION; FASTENERS; GHZ RANGE; MAGELLANIC CLOUDS; MASS; MOLECULES; NEBULAE; RECOMBINATION; STARS

Citation Formats

Saigo, Kazuya, Harada, Ryohei, Kawamura, Akiko, Onishi, Toshikazu, Tokuda, Kazuki, Morioka, Yuuki, Nayak, Omnarayani, Meixner, Margaret, Sewiło, Marta, Indebetouw, Remy, Torii, Kazufumi, Ohama, Akio, Hattori, Yusuke, Yamamoto, Hiroaki, Tachihara, Kengo, Minamidani, Tetsuhiro, Inoue, Tsuyoshi, Madden, Suzanne, Lebouteiller, Vianney, Galametz, Maud, and and others. KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA. United States: N. p., 2017. Web. doi:10.3847/1538-4357/835/1/108.
Saigo, Kazuya, Harada, Ryohei, Kawamura, Akiko, Onishi, Toshikazu, Tokuda, Kazuki, Morioka, Yuuki, Nayak, Omnarayani, Meixner, Margaret, Sewiło, Marta, Indebetouw, Remy, Torii, Kazufumi, Ohama, Akio, Hattori, Yusuke, Yamamoto, Hiroaki, Tachihara, Kengo, Minamidani, Tetsuhiro, Inoue, Tsuyoshi, Madden, Suzanne, Lebouteiller, Vianney, Galametz, Maud, & and others. KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA. United States. doi:10.3847/1538-4357/835/1/108.
Saigo, Kazuya, Harada, Ryohei, Kawamura, Akiko, Onishi, Toshikazu, Tokuda, Kazuki, Morioka, Yuuki, Nayak, Omnarayani, Meixner, Margaret, Sewiło, Marta, Indebetouw, Remy, Torii, Kazufumi, Ohama, Akio, Hattori, Yusuke, Yamamoto, Hiroaki, Tachihara, Kengo, Minamidani, Tetsuhiro, Inoue, Tsuyoshi, Madden, Suzanne, Lebouteiller, Vianney, Galametz, Maud, and and others. Fri . "KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA". United States. doi:10.3847/1538-4357/835/1/108.
@article{osti_22664005,
title = {KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA},
author = {Saigo, Kazuya and Harada, Ryohei and Kawamura, Akiko and Onishi, Toshikazu and Tokuda, Kazuki and Morioka, Yuuki and Nayak, Omnarayani and Meixner, Margaret and Sewiło, Marta and Indebetouw, Remy and Torii, Kazufumi and Ohama, Akio and Hattori, Yusuke and Yamamoto, Hiroaki and Tachihara, Kengo and Minamidani, Tetsuhiro and Inoue, Tsuyoshi and Madden, Suzanne and Lebouteiller, Vianney and Galametz, Maud and and others},
abstractNote = {We present the ALMA Band 3 and Band 6 results of {sup 12}CO(2-1), {sup 13}CO(2-1), H30 α recombination line, free–free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star-forming face-on galaxy at a distance of 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ∼1 pc and several parsecs. The total molecular mass is 0.92 × 10{sup 5} M {sub ⊙} from the {sup 13}CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation H ii region. We found that a YSO associated with the Papillon Nebula has the mass of 35 M {sub ⊙} and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. reported a similar kinematic structure toward two YSOs in the N159 West region, which are the other YSOs that have the mass of ≳35 M {sub ⊙}. This suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with a sub-parsec scale. It is filled by free–free and H30 α emission. The temperature of the molecular gas around the hole reaches ∼80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.},
doi = {10.3847/1538-4357/835/1/108},
journal = {Astrophysical Journal},
number = 1,
volume = 835,
place = {United States},
year = {Fri Jan 20 00:00:00 EST 2017},
month = {Fri Jan 20 00:00:00 EST 2017}
}