Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding Hi Flows

Kisetsu Tsuge, Hidetoshi Sano, Kengo Tachihara, Cameron Yozin, Kenji Bekki, Tsuyoshi Inoue, Norikazu Mizuno, Akiko Kawamura, Toshikazu Onishi, Yasuo Fukui

Research output: Contribution to journalArticle

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Abstract

The second most active site of high-mass star formation next to R136 in the Large Magellanic Cloud (LMC) is N44. We carried out a detailed analysis of H i at 60″ resolution by using the ATCA and Parkes data. We presented decomposition of the H i emission into two velocity components (the L and D components) with a velocity separation of ∼60 km s -1 . In addition, we newly defined the I component whose velocity is intermediate between the L and D components. The D component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve. Toward the active cluster-forming region of LHA 120-N 44, the three velocity components of H i gas show signatures of dynamical interaction, including bridges and complementary spatial distributions. We hypothesize that the L and D components have been colliding with each other since 5 Myr ago, and the interaction triggered formation of the O and early-B stars ionizing N44. In the hypothesis, the I component is interpreted as decelerated gas in terms of momentum exchange in the collisional interaction of the L and D components. In the N44 region, the Planck submillimeter dust optical depth is correlated with the H i intensity, which is well approximated by a linear regression. We found that the N44 region shows a significantly steeper regression line than in the bar region, indicating less dust abundance in the N44 region, which is ascribed to the tidal interaction between the LMC and the SMC 0.2 Gyr ago.

Original languageEnglish
Article number44
JournalAstrophysical Journal
Volume871
Issue number1
DOIs
Publication statusPublished - 20 Jan 2019

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stars
Magellanic clouds
dust
gas
regression analysis
optical depth
momentum
interactions
early stars
stellar rotation
decomposition
spatial distribution
B stars
curves
gases
optical thickness
star formation
signatures

Cite this

Tsuge, Kisetsu ; Sano, Hidetoshi ; Tachihara, Kengo ; Yozin, Cameron ; Bekki, Kenji ; Inoue, Tsuyoshi ; Mizuno, Norikazu ; Kawamura, Akiko ; Onishi, Toshikazu ; Fukui, Yasuo. / Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding Hi Flows. In: Astrophysical Journal. 2019 ; Vol. 871, No. 1.
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abstract = "The second most active site of high-mass star formation next to R136 in the Large Magellanic Cloud (LMC) is N44. We carried out a detailed analysis of H i at 60″ resolution by using the ATCA and Parkes data. We presented decomposition of the H i emission into two velocity components (the L and D components) with a velocity separation of ∼60 km s -1 . In addition, we newly defined the I component whose velocity is intermediate between the L and D components. The D component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve. Toward the active cluster-forming region of LHA 120-N 44, the three velocity components of H i gas show signatures of dynamical interaction, including bridges and complementary spatial distributions. We hypothesize that the L and D components have been colliding with each other since 5 Myr ago, and the interaction triggered formation of the O and early-B stars ionizing N44. In the hypothesis, the I component is interpreted as decelerated gas in terms of momentum exchange in the collisional interaction of the L and D components. In the N44 region, the Planck submillimeter dust optical depth is correlated with the H i intensity, which is well approximated by a linear regression. We found that the N44 region shows a significantly steeper regression line than in the bar region, indicating less dust abundance in the N44 region, which is ascribed to the tidal interaction between the LMC and the SMC 0.2 Gyr ago.",
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Tsuge, K, Sano, H, Tachihara, K, Yozin, C, Bekki, K, Inoue, T, Mizuno, N, Kawamura, A, Onishi, T & Fukui, Y 2019, 'Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding Hi Flows' Astrophysical Journal, vol. 871, no. 1, 44. https://doi.org/10.3847/1538-4357/aaf4fb

Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding Hi Flows. / Tsuge, Kisetsu; Sano, Hidetoshi; Tachihara, Kengo; Yozin, Cameron; Bekki, Kenji; Inoue, Tsuyoshi; Mizuno, Norikazu; Kawamura, Akiko; Onishi, Toshikazu; Fukui, Yasuo.

In: Astrophysical Journal, Vol. 871, No. 1, 44, 20.01.2019.

Research output: Contribution to journalArticle

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T1 - Formation of the Active Star-forming Region LHA 120-N 44 Triggered by Tidally Driven Colliding Hi Flows

AU - Tsuge, Kisetsu

AU - Sano, Hidetoshi

AU - Tachihara, Kengo

AU - Yozin, Cameron

AU - Bekki, Kenji

AU - Inoue, Tsuyoshi

AU - Mizuno, Norikazu

AU - Kawamura, Akiko

AU - Onishi, Toshikazu

AU - Fukui, Yasuo

PY - 2019/1/20

Y1 - 2019/1/20

N2 - The second most active site of high-mass star formation next to R136 in the Large Magellanic Cloud (LMC) is N44. We carried out a detailed analysis of H i at 60″ resolution by using the ATCA and Parkes data. We presented decomposition of the H i emission into two velocity components (the L and D components) with a velocity separation of ∼60 km s -1 . In addition, we newly defined the I component whose velocity is intermediate between the L and D components. The D component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve. Toward the active cluster-forming region of LHA 120-N 44, the three velocity components of H i gas show signatures of dynamical interaction, including bridges and complementary spatial distributions. We hypothesize that the L and D components have been colliding with each other since 5 Myr ago, and the interaction triggered formation of the O and early-B stars ionizing N44. In the hypothesis, the I component is interpreted as decelerated gas in terms of momentum exchange in the collisional interaction of the L and D components. In the N44 region, the Planck submillimeter dust optical depth is correlated with the H i intensity, which is well approximated by a linear regression. We found that the N44 region shows a significantly steeper regression line than in the bar region, indicating less dust abundance in the N44 region, which is ascribed to the tidal interaction between the LMC and the SMC 0.2 Gyr ago.

AB - The second most active site of high-mass star formation next to R136 in the Large Magellanic Cloud (LMC) is N44. We carried out a detailed analysis of H i at 60″ resolution by using the ATCA and Parkes data. We presented decomposition of the H i emission into two velocity components (the L and D components) with a velocity separation of ∼60 km s -1 . In addition, we newly defined the I component whose velocity is intermediate between the L and D components. The D component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve. Toward the active cluster-forming region of LHA 120-N 44, the three velocity components of H i gas show signatures of dynamical interaction, including bridges and complementary spatial distributions. We hypothesize that the L and D components have been colliding with each other since 5 Myr ago, and the interaction triggered formation of the O and early-B stars ionizing N44. In the hypothesis, the I component is interpreted as decelerated gas in terms of momentum exchange in the collisional interaction of the L and D components. In the N44 region, the Planck submillimeter dust optical depth is correlated with the H i intensity, which is well approximated by a linear regression. We found that the N44 region shows a significantly steeper regression line than in the bar region, indicating less dust abundance in the N44 region, which is ascribed to the tidal interaction between the LMC and the SMC 0.2 Gyr ago.

KW - (galaxies:) Magellanic Clouds

KW - galaxies: ISM

KW - galaxies: star formation

KW - H II regions

KW - ISM: atoms

KW - stars: massive

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