Western Magellanic Bridge HI observations

The 21-cm line emission from a 7x6deg^2^ region east of and adjoining the Small Magellanic Cloud (SMC) has been observed with the Australia Telescope Compact Array and the Parkes telescopes. This region represents the westernmost part of the Magellanic Bridge, a gas-rich tail extending ~14{deg} to the Large Magellanic Cloud. A rich and complex neutral hydrogen (HI) structure containing shells, bubbles and filaments is revealed. On the larger scale, the HI of the Bridge is organized into two velocity components. This bimodality, which appears to originate in the SMC, converges to a single velocity component within the observed region. A census of shell-like structures suggests a shell population with characteristics similar to that of the SMC.

Cone search capability for table J/MNRAS/339/105/table1 (Table of Magellanic Bridge shell parameters)

Source https://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/MNRAS/339/105
Related Identifier https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/339/105
Related Identifier http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/339/105
Metadata Access http://dc.g-vo.org/rr/q/pmh/pubreg.xml?verb=GetRecord&metadataPrefix=oai_b2find&identifier=ivo://CDS.VizieR/J/MNRAS/339/105
Creator Muller E.; Staveley-Smith L.; Zealey W.; Stanimirovic S.
Publisher CDS
Publication Year 2006
Rights https://cds.unistra.fr/vizier-org/licences_vizier.html
OpenAccess true
Contact CDS support team <cds-question(at)unistra.fr>
Resource Type Dataset; AstroObjects
Discipline Astrophysics and Astronomy; Exoplanet Astronomy; Galactic and extragalactic Astronomy; Interstellar medium; Natural Sciences; Observational Astronomy; Physics