Relationships between the HI 21-cm line strength, MgII equivalent width and metallicity in damped Lyman-alpha absorption systems

TL;DR

This study investigates the relationship between 21-cm line strength, MgII equivalent width, and metallicity in damped Lyman-alpha systems, revealing correlations and implications for cold gas detection and galaxy properties across redshifts.

Contribution

It provides new observational data on 21-cm absorption in DLAs and explores the connections between line strength, MgII absorption, and metallicity, highlighting the role of geometry and velocity structure.

Findings

21-cm detections are more common at low angular diameter distances.

A correlation exists between 21-cm line strength and MgII equivalent width.

Possible anti-correlation between spin temperature and metallicity.

Abstract

We present the results of a survey for 21-cm absorption in four never previously searched damped Lyman-alpha absorption systems (DLAs) with the Westerbork Synthesis Radio Telescope. We add our results to other recent studies in order to address the important issues regarding the detection of cold gas, through 21-cm absorption, in DLAs: Although, due to the DLAs identified with spiral galaxies, there is a mix of spin temperature/covering factor ratios at low redshift, two recent high redshift end points confirm that this ratio does not generally rise over the whole redshift range searched (up to z = 3.39). That is, if the covering factors of many of these galaxies were a factor of >2 smaller than for the spirals, then no significant difference in the spin temperatures between these two classes would be required. Furthermore, although it is difficult to separate the relative contributions of the spin temperature and covering factor, the new results confirm that 21-cm detections tend to occur at low angular diameter distances, where the coverage of a given absorption cross section is maximised. Finally, we also find an apparent 21-cm line strength--MgII equivalent width correlation, which appears to be due to a coupling of the velocity structure between the components that each species traces. That is, the gas seen in 21-cm absorption could be the same as that seen in optical absorption. Combined with the known equivalent width--metallicity relation, this may be manifest as a spin temperature--metallicity anti-correlation, which is non-evolutionary in origin.