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Dust in the bright supernova remnant N49 in the LMC

Otsuka, M. and van Loon, J. Th. and Long, K. S. and Meixner, M. and Matsuura, M. and Reach, W. T. and Roman-Duval, J. and Gordon, K. and Sauvage, M. and Hony, S. and Misselt, K. and Engelbracht, C. and Panuzzo, P. and Okumura, K. and Woods, P. M. and Kemper, F. and Sloan, G. C. (2010) Dust in the bright supernova remnant N49 in the LMC. Astronomy and Astrophysics, 518 . L139. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20101122-095222728

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Abstract

We investigate the dust associated with the supernova remnant (SNR) N49 in the Large Magellanic Cloud (LMC) as observed with the Herschel Space Observatory. N49 is unusually bright because of an interaction with a molecular cloud along its eastern edge. We have used PACS and SPIRE to measure the far IR flux densities of the entire SNR and of a bright region on the eastern edge of the SNR where the SNR shock is encountering the molecular cloud. Using these fluxes supplemented with archival data at shorter wavelengths, we estimate the dust mass associated with N49 to be about 10 M_☉. The bulk of the dust in our simple two-component model has a temperature of 20–30 K, similar to that of nearby molecular clouds. Unfortunately, as a result of the limited angular resolution of Herschel at the wavelengths sampled with SPIRE, the uncertainties are fairly large. Assuming this estimate of the dust mass associated with the SNR is approximately correct, it is probable that most of the dust in the SNR arises from regions where the shock speed is too low to produce significant X-ray emission. The total amount of warm 50–60 K dust is ~0.1 or 0.4 M_☉, depending on whether the dust is modeled in terms of carbonaceous or silicate grains. This provides a firm lower limit to the amount of shock heated dust in N49.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201014642DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014642&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Reach, W. T.0000-0001-8362-4094
Additional Information:© ESO 2010. Received 31 March 2010; Accepted 30 April 2010; Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We acknowledge financial support from the NASA Herschel Science Center, J.P.L. contract # 1381522. We are grateful for the contributions and support from the European Space Agency (ESA), the PACS and SPIRE teams, the Herschel Science Center and the NASA Herschel Science Center (esp. A. Barbar and K. Xu) and the PACS and SPIRE instrument control center at CEA-Saclay, without which none of this work would be possible.
Funders:
Funding AgencyGrant Number
NASA Herschel Science CenterJPL 1381522
European Space Agency (ESA)UNSPECIFIED
PACS and SPIRE teamsUNSPECIFIED
Herschel Science CenterUNSPECIFIED
Commissariat à l'Énergie Atomique-Saclay (CEA-Saclay)UNSPECIFIED
Subject Keywords:ISM: supernova remnants; dust, extinction; submillimeter: ISM; Magellanic Clouds
Record Number:CaltechAUTHORS:20101122-095222728
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20101122-095222728
Official Citation:Dust in the bright supernova remnant N49 in the LMC M. Otsuka, J. Th. van Loon, K. S. Long, M. Meixner, M. Matsuura, W. T. Reach, J. Roman-Duval, K. Gordon, M. Sauvage, S. Hony, K. Misselt, C. Engelbracht, P. Panuzzo, K. Okumura, P. M. Woods, F. Kemper and G. C. Sloan A&A 518 L139 (2010) DOI: 10.1051/0004-6361/201014642
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:20935
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:23 Nov 2010 00:58
Last Modified:02 Mar 2017 04:18

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