N131 bubble CO integrated intensity maps Virtual Observatory Resource

Authors

1. Zhang C.-P.
2. Li G.-X.
3. Wyrowski F.
4. Wang J.-J.
5. Yuan J.-H.
6. Xu J.-L.,Gong Y.
7. Yeh C.C.
8. Menten K.M.

Published by

CDS

Abstract

OB-type stars have strong ionizing radiation and drive energetic winds. The ultraviolet radiation from ionizing stars may heat dust and ionize gas to sweep up an expanding bubble shell. This shell may be the result of feedback leading to a new generation of stars. N131 is an infrared dust bubble residing in a molecular filament. We study the formation and fragmentation of this bubble with multiwavelength dust and gas observations. Towards the bubble N131, we analysed archival multiwavelength observations including 3.6, 4.5, 5.8, 8.0, 24, 70, 160, 250, 350, 500um, 1.1mm, and 21cm. In addition, we performed new observations of CO (2-1), CO (1-0), and ^13^CO (1-0) with the IRAM 30m telescope.

Keywords

1. interstellar-medium
2. molecular-clouds
3. co-line-emission

Bibliographic source Bibcode

2016A&A...585A.117Z

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/585/A117

IVOA Identifier IVOID

ivo://CDS.VizieR/J/A+A/585/A117

Document Object Identifer DOI

doi:10.26093/cds/vizier.35850117

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