Bright X-ray emission from supernova remnant G349.7+0.2 interacting with a molecular cloud

J. Lazendic; P. Slane; Y. Chen; J. P. Hughes; D. Burrows; J. Nousek

Bright X-ray emission from supernova remnant G349.7+0.2 interacting with a molecular cloud

J. Lazendic, P. Slane, Y. Chen, J. P. Hughes, D. Burrows, J. Nousek

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › Academic › peer-review

Abstract

G349.7+0.2 is the third brightest Galactic supernova remnant (SNR) at radio wavelengths, after Cas A and the Crab Nebula. It is a distant (22 kpc), small diameter (2.5 arcmin) shell-type SNR. The presence of OH(1720 MHz) masers and shocked molecular gas show that the SNR is interacting with ambient molecular clouds. Our ASCA observations are consistent with this interpretation, revealing a large mass of swept-up material. We have obtained high resolution Chandra observations of G349.7+0.2 to fully explore its X-ray morphology, and to search for possible spectral variations across the remnant. We find that the X-ray morphology agrees well with that observed in the radio, which contrasts with the centrally dominated X-ray morphology often associated with remnants associated with OH(1720 MHz) masers (e.g., W28, W44, IC 443). We review our results of spectral investigations with Chandra, which appear to indicate a multi-phase shock structure, and compare the spatial structure with available data at other frequencies. This work was supported in part from Chandra grant GO2-3080A.

Original language	English
Title of host publication	American Astronomical Society, HEAD meeting 7
Publication status	Published - 1 Mar 2003
Externally published	Yes

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http://adsabs.harvard.edu/abs/2003HEAD....7.1015L

Cite this

@inproceedings{413b9948bd3c463fbcf0d30ea586b970,

title = "Bright X-ray emission from supernova remnant G349.7+0.2 interacting with a molecular cloud",

abstract = "G349.7+0.2 is the third brightest Galactic supernova remnant (SNR) at radio wavelengths, after Cas A and the Crab Nebula. It is a distant (22 kpc), small diameter (2.5 arcmin) shell-type SNR. The presence of OH(1720 MHz) masers and shocked molecular gas show that the SNR is interacting with ambient molecular clouds. Our ASCA observations are consistent with this interpretation, revealing a large mass of swept-up material. We have obtained high resolution Chandra observations of G349.7+0.2 to fully explore its X-ray morphology, and to search for possible spectral variations across the remnant. We find that the X-ray morphology agrees well with that observed in the radio, which contrasts with the centrally dominated X-ray morphology often associated with remnants associated with OH(1720 MHz) masers (e.g., W28, W44, IC 443). We review our results of spectral investigations with Chandra, which appear to indicate a multi-phase shock structure, and compare the spatial structure with available data at other frequencies. This work was supported in part from Chandra grant GO2-3080A.",

author = "J. Lazendic and P. Slane and Y. Chen and Hughes, {J. P.} and D. Burrows and J. Nousek",

year = "2003",

month = mar,

day = "1",

language = "English",

booktitle = "American Astronomical Society, HEAD meeting 7",

}

TY - GEN

T1 - Bright X-ray emission from supernova remnant G349.7+0.2 interacting with a molecular cloud

AU - Lazendic, J.

AU - Slane, P.

AU - Chen, Y.

AU - Hughes, J. P.

AU - Burrows, D.

AU - Nousek, J.

PY - 2003/3/1

Y1 - 2003/3/1

N2 - G349.7+0.2 is the third brightest Galactic supernova remnant (SNR) at radio wavelengths, after Cas A and the Crab Nebula. It is a distant (22 kpc), small diameter (2.5 arcmin) shell-type SNR. The presence of OH(1720 MHz) masers and shocked molecular gas show that the SNR is interacting with ambient molecular clouds. Our ASCA observations are consistent with this interpretation, revealing a large mass of swept-up material. We have obtained high resolution Chandra observations of G349.7+0.2 to fully explore its X-ray morphology, and to search for possible spectral variations across the remnant. We find that the X-ray morphology agrees well with that observed in the radio, which contrasts with the centrally dominated X-ray morphology often associated with remnants associated with OH(1720 MHz) masers (e.g., W28, W44, IC 443). We review our results of spectral investigations with Chandra, which appear to indicate a multi-phase shock structure, and compare the spatial structure with available data at other frequencies. This work was supported in part from Chandra grant GO2-3080A.

AB - G349.7+0.2 is the third brightest Galactic supernova remnant (SNR) at radio wavelengths, after Cas A and the Crab Nebula. It is a distant (22 kpc), small diameter (2.5 arcmin) shell-type SNR. The presence of OH(1720 MHz) masers and shocked molecular gas show that the SNR is interacting with ambient molecular clouds. Our ASCA observations are consistent with this interpretation, revealing a large mass of swept-up material. We have obtained high resolution Chandra observations of G349.7+0.2 to fully explore its X-ray morphology, and to search for possible spectral variations across the remnant. We find that the X-ray morphology agrees well with that observed in the radio, which contrasts with the centrally dominated X-ray morphology often associated with remnants associated with OH(1720 MHz) masers (e.g., W28, W44, IC 443). We review our results of spectral investigations with Chandra, which appear to indicate a multi-phase shock structure, and compare the spatial structure with available data at other frequencies. This work was supported in part from Chandra grant GO2-3080A.

M3 - Conference contribution

BT - American Astronomical Society, HEAD meeting 7

ER -

Bright X-ray emission from supernova remnant G349.7+0.2 interacting with a molecular cloud

Abstract

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