Chandra observation of the magellanic cloud supernova remnant 0454-67.2 in N9

F. D. Seward; R. M. Williams; Y. H. Chu; J. R. Dickel; R. C. Smith; S. D. Points

doi:10.1086/499767

Chandra observation of the magellanic cloud supernova remnant 0454-67.2 in N9

F. D. Seward, R. M. Williams, Y. H. Chu, J. R. Dickel, R. C. Smith, S. D. Points

Astronomy

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Abstract

A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2.′3 × 3.′6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O II] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova (SN) energy release was ≥5 × 10⁵⁰ ergs, and the age is ∼3 × 10⁴ yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out.

Original language	English (US)
Pages (from-to)	327-334
Number of pages	8
Journal	Astrophysical Journal
Volume	640
Issue number	1 I
DOIs	https://doi.org/10.1086/499767
State	Published - Mar 20 2006

Keywords

ISM: Individual (SNR 0454-67.2)
Supernova remnants
X-rays: ISM

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/499767

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title = "Chandra observation of the magellanic cloud supernova remnant 0454-67.2 in N9",

abstract = "A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2.′3 × 3.′6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O II] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova (SN) energy release was ≥5 × 1050 ergs, and the age is ∼3 × 104 yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out.",

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author = "Seward, {F. D.} and Williams, {R. M.} and Chu, {Y. H.} and Dickel, {J. R.} and Smith, {R. C.} and Points, {S. D.}",

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month = mar,

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doi = "10.1086/499767",

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T1 - Chandra observation of the magellanic cloud supernova remnant 0454-67.2 in N9

AU - Seward, F. D.

AU - Williams, R. M.

AU - Chu, Y. H.

AU - Dickel, J. R.

AU - Smith, R. C.

AU - Points, S. D.

PY - 2006/3/20

Y1 - 2006/3/20

N2 - A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2.′3 × 3.′6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O II] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova (SN) energy release was ≥5 × 1050 ergs, and the age is ∼3 × 104 yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out.

AB - A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2.′3 × 3.′6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O II] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova (SN) energy release was ≥5 × 1050 ergs, and the age is ∼3 × 104 yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out.

KW - ISM: Individual (SNR 0454-67.2)

KW - Supernova remnants

KW - X-rays: ISM

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DO - 10.1086/499767

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JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

Chandra observation of the magellanic cloud supernova remnant 0454-67.2 in N9

Abstract

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