H I gas in higher density regions of the IGM

Details H I gas in higher density regions of the IGM H I gas in higher density regions of the IGM

Mar 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005pgqa.conf..454m&link_type=abstract

Probing Galaxies through Quasar Absorption Lines, IAU Colloquium Proceedings of the International Astronomical Union 199, held M

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Scientific paper

Using H I absorption alone, we attempt to separate H I absorption lines in quasar spectra into two categories; hdls (higher density lines) and ldls (lower density lines), and we discuss the difference in their physical properties. We deblend and fit all H I lines with voigt profiles, and make an unbiased sample of H I lines covering a wide column density range (12 cm-2). To reduce the influence of line blending, we simultaneously fit several Lyman series lines. As a result of a two-point correlation analysis, we found that higher column density H I lines are clustering at δ v km s-1, while lower ones at δ v km s-1. We define hdls as H I lines with 15 cm-2 and all H I lines within ±200 km s-1 of a line with log nHI > 15 cm-2, and ldls as others with 12 cm-2. We found that the hdls have smaller minimum b-values for a given column density than the ldls. This difference is successfully reproduced by our hydrodynamic simulation. The ldls seem to be cool or shock-heated difFUSE igm gas, while the hdls are likely to be cooler dense gas near to galaxies.

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