ASCA observations of the supernova remnant VRO 42.05.01

Zhiyu Guo; David N. Burrows

doi:10.1086/310605

ASCA observations of the supernova remnant VRO 42.05.01

Zhiyu Guo, David N. Burrows

Astronomy & Astrophysics

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Abstract

We present the results of our ASCA SIS and GIS observations of the supernova remnant VRO 42.05.01. Our spectral fits indicate that the SNR is isothermal (∼8.3 × 10⁶ K), consistent with our ROSAT analysis results. The absorbing column density (∼2.9 × 10²¹ cm^-2) obtained from these spectral fits is much smaller than expected for the nominal distance of 5 kpc, which indicates that the line of sight toward VRO 42.05.01 has an unusually low gas density. The spectral resolution of ASCA allows us to determine elemental abundances for the hot X-ray-emitting plasma in the bright "wing" component of this remnant. We find that Mg, Si, and Fe are underabundant and attribute these low abundances to the Galactic metallicity gradient and to the location of the remnant in the outer Milky Way.

Original language	English (US)
Pages (from-to)	L51-L54
Journal	Astrophysical Journal
Volume	480
Issue number	1 PART II
DOIs	https://doi.org/10.1086/310605
State	Published - 1997

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/310605

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@article{d426ee2fecbe473fb78e7b758771b430,

title = "ASCA observations of the supernova remnant VRO 42.05.01",

abstract = "We present the results of our ASCA SIS and GIS observations of the supernova remnant VRO 42.05.01. Our spectral fits indicate that the SNR is isothermal (∼8.3 × 106 K), consistent with our ROSAT analysis results. The absorbing column density (∼2.9 × 1021 cm-2) obtained from these spectral fits is much smaller than expected for the nominal distance of 5 kpc, which indicates that the line of sight toward VRO 42.05.01 has an unusually low gas density. The spectral resolution of ASCA allows us to determine elemental abundances for the hot X-ray-emitting plasma in the bright {"}wing{"} component of this remnant. We find that Mg, Si, and Fe are underabundant and attribute these low abundances to the Galactic metallicity gradient and to the location of the remnant in the outer Milky Way.",

author = "Zhiyu Guo and Burrows, {David N.}",

note = "Funding Information: We would like to thank Eric Gotthelf at ASCA GOF for useful discussions on making the images, and Richard Edgar and Jon Slavin for providing NEI spectral models for comparison with our data. This work has been sponsored by NASA grant NAG5-2537.",

year = "1997",

doi = "10.1086/310605",

language = "English (US)",

volume = "480",

pages = "L51--L54",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 PART II",

}

TY - JOUR

T1 - ASCA observations of the supernova remnant VRO 42.05.01

AU - Guo, Zhiyu

AU - Burrows, David N.

N1 - Funding Information: We would like to thank Eric Gotthelf at ASCA GOF for useful discussions on making the images, and Richard Edgar and Jon Slavin for providing NEI spectral models for comparison with our data. This work has been sponsored by NASA grant NAG5-2537.

PY - 1997

Y1 - 1997

N2 - We present the results of our ASCA SIS and GIS observations of the supernova remnant VRO 42.05.01. Our spectral fits indicate that the SNR is isothermal (∼8.3 × 106 K), consistent with our ROSAT analysis results. The absorbing column density (∼2.9 × 1021 cm-2) obtained from these spectral fits is much smaller than expected for the nominal distance of 5 kpc, which indicates that the line of sight toward VRO 42.05.01 has an unusually low gas density. The spectral resolution of ASCA allows us to determine elemental abundances for the hot X-ray-emitting plasma in the bright "wing" component of this remnant. We find that Mg, Si, and Fe are underabundant and attribute these low abundances to the Galactic metallicity gradient and to the location of the remnant in the outer Milky Way.

AB - We present the results of our ASCA SIS and GIS observations of the supernova remnant VRO 42.05.01. Our spectral fits indicate that the SNR is isothermal (∼8.3 × 106 K), consistent with our ROSAT analysis results. The absorbing column density (∼2.9 × 1021 cm-2) obtained from these spectral fits is much smaller than expected for the nominal distance of 5 kpc, which indicates that the line of sight toward VRO 42.05.01 has an unusually low gas density. The spectral resolution of ASCA allows us to determine elemental abundances for the hot X-ray-emitting plasma in the bright "wing" component of this remnant. We find that Mg, Si, and Fe are underabundant and attribute these low abundances to the Galactic metallicity gradient and to the location of the remnant in the outer Milky Way.

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U2 - 10.1086/310605

DO - 10.1086/310605

M3 - Article

AN - SCOPUS:21744448269

SN - 0004-637X

VL - 480

SP - L51-L54

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART II

ER -

ASCA observations of the supernova remnant VRO 42.05.01

Abstract

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