Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant

• Autores: Gomez, H.L.; Dunne, L.; Ivison, R.J.; Reynoso, E.M.; Thompson, M.A.; Sibthorpe, B.; Eales, S.A.; Delaney, T.M.; Maddox, S.; Isaak, K.
• Año de publicación: 2009
• Idioma: inglés
• Tipo de recurso: artículo
• Fuente: Mon. Not. R. Astron. Soc. 2009;397(3):1621-1632
• Materia: Galaxies: abundances; ISM: submillimetre dust; Radio lines: ISM; Submillimetre; Supernovae: Kepler
• Institución: Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales

Whether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 μm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the sub-mm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H i, 12CO(J = 2-1) and 13CO(J = 2-1). We detect weak CO emission (peak T* A = 0.2-1 K, 1-2 km s -1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler's remnant is 0.1-1.2 M ⊙, about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts. © 2009 RAS.
Fil:Reynoso, E.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.