X-rays from superbubbles in the large magellanic cloud. V. The H II complex N11

Mordecai Mark Mac Low; Thomas H. Chang; You Hua Chu; Sean D. Points; R. Chris Smith; Bart P. Wakker

doi:10.1086/305110

X-rays from superbubbles in the large magellanic cloud. V. The H II complex N11

Mordecai Mark Mac Low, Thomas H. Chang, You Hua Chu, Sean D. Points, R. Chris Smith, Bart P. Wakker

Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

The giant H II complex N11 in the Large Magellanic Cloud contains OB associations at several different stages in their life histories. We have obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images, echelle spectra in Hα and [N 11] lines, and IUE interstellar absorption line observations of this region. The central bubble of Nil has an X-ray luminosity a factor of only 3-7 brighter than that predicted for an energy-conserving superbubble, making this the first detection of X-ray emission from a superbubble without a strong X-ray excess. The region N11B contains an extremely young OB association analogous to the central association of the Carina Nebula, apparently still embedded in its natal molecular cloud. We find that NUB emits diffuse X-ray emission, probably powered by stellar winds. Finally, we compare the tight cluster HD 32228 in Nil to R136 in 30 Dor. The latter is a strong X-ray source, while the former is not detected, showing that strong X-ray emission from compact objects is not a universal property of such tight clusters.

Original language	English (US)
Pages (from-to)	260-273
Number of pages	14
Journal	Astrophysical Journal
Volume	493
Issue number	1 PART I
DOIs	https://doi.org/10.1086/305110
State	Published - 1998

Keywords

ISM: bubbles
ISM: individual (Nil)
Magellanic Clouds
X-rays: ISM

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/305110

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title = "X-rays from superbubbles in the large magellanic cloud. V. The H II complex N11",

abstract = "The giant H II complex N11 in the Large Magellanic Cloud contains OB associations at several different stages in their life histories. We have obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images, echelle spectra in Hα and [N 11] lines, and IUE interstellar absorption line observations of this region. The central bubble of Nil has an X-ray luminosity a factor of only 3-7 brighter than that predicted for an energy-conserving superbubble, making this the first detection of X-ray emission from a superbubble without a strong X-ray excess. The region N11B contains an extremely young OB association analogous to the central association of the Carina Nebula, apparently still embedded in its natal molecular cloud. We find that NUB emits diffuse X-ray emission, probably powered by stellar winds. Finally, we compare the tight cluster HD 32228 in Nil to R136 in 30 Dor. The latter is a strong X-ray source, while the former is not detected, showing that strong X-ray emission from compact objects is not a universal property of such tight clusters.",

keywords = "ISM: bubbles, ISM: individual (Nil), Magellanic Clouds, X-rays: ISM",

author = "{Mac Low}, {Mordecai Mark} and Chang, {Thomas H.} and Chu, {You Hua} and Points, {Sean D.} and Smith, {R. Chris} and Wakker, {Bart P.}",

year = "1998",

doi = "10.1086/305110",

language = "English (US)",

volume = "493",

pages = "260--273",

journal = "Astrophysical Journal",

issn = "0004-637X",

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number = "1 PART I",

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TY - JOUR

T1 - X-rays from superbubbles in the large magellanic cloud. V. The H II complex N11

AU - Mac Low, Mordecai Mark

AU - Chang, Thomas H.

AU - Chu, You Hua

AU - Points, Sean D.

AU - Smith, R. Chris

AU - Wakker, Bart P.

PY - 1998

Y1 - 1998

N2 - The giant H II complex N11 in the Large Magellanic Cloud contains OB associations at several different stages in their life histories. We have obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images, echelle spectra in Hα and [N 11] lines, and IUE interstellar absorption line observations of this region. The central bubble of Nil has an X-ray luminosity a factor of only 3-7 brighter than that predicted for an energy-conserving superbubble, making this the first detection of X-ray emission from a superbubble without a strong X-ray excess. The region N11B contains an extremely young OB association analogous to the central association of the Carina Nebula, apparently still embedded in its natal molecular cloud. We find that NUB emits diffuse X-ray emission, probably powered by stellar winds. Finally, we compare the tight cluster HD 32228 in Nil to R136 in 30 Dor. The latter is a strong X-ray source, while the former is not detected, showing that strong X-ray emission from compact objects is not a universal property of such tight clusters.

AB - The giant H II complex N11 in the Large Magellanic Cloud contains OB associations at several different stages in their life histories. We have obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images, echelle spectra in Hα and [N 11] lines, and IUE interstellar absorption line observations of this region. The central bubble of Nil has an X-ray luminosity a factor of only 3-7 brighter than that predicted for an energy-conserving superbubble, making this the first detection of X-ray emission from a superbubble without a strong X-ray excess. The region N11B contains an extremely young OB association analogous to the central association of the Carina Nebula, apparently still embedded in its natal molecular cloud. We find that NUB emits diffuse X-ray emission, probably powered by stellar winds. Finally, we compare the tight cluster HD 32228 in Nil to R136 in 30 Dor. The latter is a strong X-ray source, while the former is not detected, showing that strong X-ray emission from compact objects is not a universal property of such tight clusters.

KW - ISM: bubbles

KW - ISM: individual (Nil)

KW - Magellanic Clouds

KW - X-rays: ISM

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JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART I

ER -

X-rays from superbubbles in the large magellanic cloud. V. The H II complex N11

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