Artículos de revistas
Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
Fecha
2009-12Registro en:
Gomez, H. L.; Dune, L.; Ivison, R. J.; Reynoso, Estela Marta; Thompson, M.; et al.; Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 397; 3; 12-2009; 1621-1632
0035-8711
CONICET Digital
CONICET
Autor
Gomez, H. L.
Dune, L.
Ivison, R. J.
Reynoso, Estela Marta
Thompson, M.
Sibthorpe, B.
Eales, S. A.
Delaney, T. M.
Maddox, S.
Isaak, K.
Resumen
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 submm 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.