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2005ApJ...618..297R - Astrophys. J., 618, 297-320 (2005/January-1)
Shocked molecular gas in the supernova remnants W28 and W44: near-infrared and millimeter-wave observations.
REACH W.T., RHO J. and JARRETT T.H.
Abstract (from CDS):
Both the near-infrared and millimeter-wave emission are attributed to shocks into gas with density higher than 103/cm3. Individual shock structures are resolved in the H2emission, with inferred edge-on shock thicknesses of ∼1017 cm, consistent with nondissociative shocks into gas densities of 103-104/cm3. Bright 1720 MHz OH masers are located within the shocked H2gas complexes and highlight only localized areas, where the conditions for masing are optimal. The Hα and X-ray emission, which trace hotter shocked gas, have morphologies very different from the radio. We find a detailed correlation of the radio and H2emission for some long filaments, indicating cosmic-ray acceleration or reacceleration due to shocks into moderately dense gas. Compared to the interclump gas and the very dense cores, the synchrotron emissivity of the moderate-density (CO emitting) medium is highest, which explains the radio-H2 correlation and the very bright radio emission of these two supernova remnants despite their relatively advanced age. The different morphologies of these two remnants at different wavelengths are explained by the highly nonuniform structure of giant molecular clouds, with low-density (∼5/cm3) gas occupying most (∼90%) of the volume, moderate-density gas (∼103/cm3) gas occupying most of the rest of the volume, and dense gas in the cores.
Abstract Copyright: ∼
Journal keyword(s): ISM: Individual: Alphanumeric: W28 - ISM: Individual: Alphanumeric: W44 - ISM: Molecules - Shock Waves - ISM: Supernova Remnants
Nomenclature: Table 2, Fig.13: [RRJ2005] W28 BML N (Nos 1-5).
Simbad objects: 21
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