Physics
Scientific paper
Jul 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8651k&link_type=abstract
HST Proposal ID #8651
Physics
Hst Proposal Id #8651 Quasar Absorption Lines And Igm
Scientific paper
We are proposing STIS echelle UV absorption line spectroscopy through the Magellanic Bridge {near the SMC} to probe the temperature, ionization, and kinematic structure in a metal- poor environment like those observed in the early universe. The sightline toward the QSO B0312-770 is especially interesting because of the proximity of the absorber { 60 kpc} and the radio loud background source. Using 21-cm absorption and emission spectroscopy we have measured H I column densities of 10^20 cm^-2 which approach those in damped LyAlpha systems. Most importantly, we measure well- constrained spin temperatures for the absorbing neutral hydrogen components, T_S=30-200 K. By comparing the velocity structure and optical depths of common UV lines like Mg I, Mg II, Si II, Si IV, C IV, with the 21-cm diagnostics, we will identify the mixture of physical phases {hot and cold} and kinematic structure that comprise a nearby metal-poor environment for comparison to the high-z universe. If this sightline resembles the high-z UV absorbers, then the existence of ongoing star formation in the Magellanic Bridge implies that QSOs absorption line systems may be active sites of star formation as well.
No associations
LandOfFree
STIS UV Spectroscopy in the Magellanic Bridge: A Typical QSO Absorption Line System? does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with STIS UV Spectroscopy in the Magellanic Bridge: A Typical QSO Absorption Line System?, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and STIS UV Spectroscopy in the Magellanic Bridge: A Typical QSO Absorption Line System? will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1720335