Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 416, Issue 4, Pages 3118-3137Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2011.19261.x
Keywords
galaxies: haloes; galaxies: ISM; quasars: absorption lines
Categories
Funding
- Australian Research Council [DP0877998]
- National Science Foundation [AST-0708210]
- W.M. Keck Foundation
- Australian Research Council [DP0877998] Funding Source: Australian Research Council
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We have used Galaxy IMage 2D (GIM2D) to quantify the morphological properties of 40 intermediate-redshift MgII absorption-selected galaxies [0.03 <= W-r(2796) <= 2.9 angstrom], imaged with WFPC-2/Hubble Space Telescope (HST), and compared them to the halo gas properties measured from HIRES/Keck and UVES/VLT quasar spectra. We find that as the quasar-galaxy separation, D, increases the Mg II equivalent decreases with large scatter, implying that D is not the only physical parameter affecting the distribution and quantity of halo gas. Our main result shows that inclination correlates with MgII absorption properties after normalizing out the relationship (and scatter) between the absorption properties and D. We find a 4.3 sigma correlation between W-r(2796) and galaxy inclination, normalized by impact parameter, i/D. Other measures of absorption optical depth also correlate with i/D at greater than 3.2 sigma significance. Overall, this result suggests that MgII gas has a co-planer geometry, not necessarily disc-like, that is coupled to the galaxy inclination. It is plausible that the absorbing gas arises from tidal streams, satellites, filaments, etc., which tend to have somewhat co-planer distributions. This result does not support a picture in which MgII absorbers with W-r(2796) less than or similar to 1 angstrom are predominantly produced by star formation driven winds. We further find that: (1) MgII host galaxies have quantitatively similar bulge and disc scalelength distribution to field galaxies at similar redshifts and have a mean disc and bulge scalelength of 3.8 and 2.5 kpc, respectively; (2) Galaxy colour and luminosity do not correlate strongly with absorption properties, implying a lack of a connection between host galaxy star formation rates and absorption strength; and (3) parameters such as scalelengths and bulge-to-total ratios do not significantly correlate with the absorption parameters, suggesting that the absorption is independent of galaxy size or mass.
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