Supernova remnant W49B and its environment

Abstract

We study Gamma-ray supernova remnant W49B and its environment using recent radio and infrared data. {\it Spitzer} IRS low resolution data of W49B shows shocked excitation lines of H${}_2$ (0,0) S(0)-S(7) from the SNR-molecular cloud interaction. The H${}_2$ gas is composed of two components with temperature of $\sim$260 K and $\sim$1060 K respectively. Various spectral lines from atomic and ionic particles are detected towards W49B. We suggest the ionic phase has an electron density of $\sim$500 cm${}^{-3}$ and a temperature of $\sim$$10^4$ K by the spectral line diagnoses. The mid- and far-infrared data from {\it MSX}, {\it Spitzer} and {\it Herschel} reveals a 151 $\pm$ 20 K hot dust component with a mass of 7.5 $\pm$ 6.6 $\times$ ${10}^{-4} {\Msol}$ and a 45 $\pm$ 4 K warm dust component with a mass of 6.4 $\pm$ 3.2 ${\Msol}$. The hot dust is likely from materials swept up by the shock of W49B. The warm dust may possibly originate from the evaporation of clouds interacting with W49B. We build the HI absorption spectra of W49B and nearby four {\HII} regions (W49A, G42.90+0.58, G42.43-0.26 and G43.19-0.53), and study the relation between W49B and the surrounding molecular clouds by employing the 2.12 $\mu$m infrared and CO data. We therefore obtain a kinematic distance of $\sim$10 kpc for W49B and suggest that the remnant is likely associated with the CO cloud at about 40 km s${}^{-1}$.

11 pages, 13 figures, accepted for publication in ApJ

References in corpus (7)

• The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey
• The VLA Galactic Plane Survey
• A Near-Infrared and X-ray Study of W49B: A Wind Cavity Explosion
• Spitzer spectral line mapping of supernova remnants: I. Basic data and principal component analysis
• The Distance and Age of the SNR Kes 73 and AXP 1E 1841-045
• The X-ray emission of the supernova remnant W49B observed with XMM-Newton
• Radio and X-ray images of SNR G18.8+0.3 interacting with molecular clouds

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