Cold molecules in HI 21cm absorbers across redshifts 0.1-4

TL;DR

This study investigates cold molecular gas in high-redshift HI 21cm absorbers using IRAM-30m and NOEMA, revealing new detections, molecular gas properties, and the importance of spatial resolution for absorption studies.

Contribution

It provides new detections of molecular emission and absorption in high-redshift HI 21cm absorbers, and analyzes the physical conditions and media traced by these lines.

Findings

Eight targets detected in emission, five are new.

Four new absorption detections reported.

Disparity between molecular and HI absorption lines indicates different media.

Abstract

Absorption lines at high redshift in front of quasars are rare in the mm domain. Only five associated and five intervening systems have been reported in the literature. These bring very useful information complementary to emission lines, for instance, to distinguish between inflows and outflows. They are also good candidates to study the variations of the fundamental constants. We report here the search for molecules in emission and absorption in front of a sample of 30 targets, comprising 16 associated and 14 intervening HI 21-cm absorbers. The observations have been done with the IRAM-30m telescope, simultaneously at 3mm and 2mm, exploring CO ladder and HCO+ lines. Eight targets have been detected in emission, of which five are new. Their molecular gas masses range from 10^9 to 7 10^11 Mo. We also report four new detections in absorption. Two of the associated CO absorption line detections at high redshift (z=1.211 and 1.275) resulted from the high spatial resolution follow-up with NOEMA. The disparity between the mm molecular and HI 21-cm absorption lines for these and another intervening system detected in HNC at z = 1.275, is attributable to radio and mm sight lines tracing different media. Comparing HI and H2 in the 14 known high redshift molecular absorbers, associated HI absorption lines are broad, with multiple components and the molecular absorption corresponds to the broader and weaker 21-cm absorption component. This indicates two distinct phases: one near galaxy centers with a larger CO-to-HI abundance ratio, and another with lower molecular abundance in the outer regions of the galaxy. The comparison of interferometric and single dish observations shows that the detection of absorption requires sufficient spatial resolution to overcome the dilution by emission, and will be an important criterion for mm follow-up of 21-cm absorbers from ongoing large-scale surveys.