Dust in the bright supernova remnant N49 in the LMC - Astrophysics > Cosmology and Nongalactic AstrophysicsReportar como inadecuado




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Abstract: We investigate the dust associated with the supernova remnant SNR N49 inthe Large Magellanic Cloud LMC as observed with the Herschel SpaceObservatory. N49 is unusually bright because of an interaction with a molecularcloud along its eastern edge. We have used PACS and SPIRE to measure the far IRflux densities of the entire SNR and of a bright region on the eastern edge ofthe SNR where the SNR shock is encountering the molecular cloud. Using thesefluxes supplemented with archival data at shorter wavelengths, we estimate thedust mass associated with N49 to be about 10 Msun. The bulk of the dust in oursimple two-component model has a temperature of 20-30 K, similar to that ofnearby molecular clouds. Unfortunately, as a result of the limited angularresolution of Herschel at the wavelengths sampled with SPIRE, the uncertaintiesare fairly large. Assuming this estimate of the dust mass associated with theSNR is approximately correct, it is probable that most of the dust in the SNRarises from regions where the shock speed is too low to produce significantX-ray emission. The total amount of warm 50-60 K dust is ~0.1 or 0.4 Msun,depending on whether the dust is modeled in terms of carbonaceous or silicategrains. This provides a firm lower limit to the amount of shock heated dust inN49.



Autor: 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. Mis

Fuente: https://arxiv.org/







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