Other
Scientific paper
Jul 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009hst..prop12263m&link_type=abstract
HST Proposal ID #12263. Cycle 18
Other
Scientific paper
The Magellanic Bridge {the MB} is a physical connection between the Large Magellanic Cloud {LMC} and the Small Magellanic Cloud {SMC}. The MB contains a young stellar population that was probably formed in local molecular clouds, while it is still not fully settled whether the larger Magellanic Stream, produced by the LMC/SMC unit sweeping through the Milky Way halo, contains only gas or has any stellar populations. We propose HST/COS spectroscopy of four sight-lines of the MB toward QSOs/AGNs behind it, covering various absorption lines such as O I, Fe II, Si II, C II, Si IV, and C IV. This will be combined with one existing STIS observation of B0312-770 which we have already modeled in detail, and with our recent high resolution VLT/UVES observations of all five sight-lines, covering Ca II H,K and Na I D_1, D_2. The five sight-lines cover a range of H I column densities from 10^19 {cm^-2} up to above the damped Lya {DLA} threshold. Effectively, the proposed COS observations of multiple sightlines through the MB will provide a map of the surroundings of a DLA absorber, allowing us to study how it connects with other classes of absorbers, and with the surrounding structures. Our goals are to {1} evaluate physical conditions of gas clouds in the MB along multiple sight-lines derived from the photoionization models, {2} search for correlations between the physical conditions of the MB gas, the H I 21cm radio emission density, and the distance from the SMC, and {3} compare the physical conditions of the MB to those of high-z absorption systems like DLA systems because the MB, with its low metallicity and possible dust deficiency, could be a local analog.;
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