Abstract
We present the detection and detailed analysis of a diffuse molecular cloud atzabs= 2.4636 towards the quasar SDSS J 1513+0352 (zem≃ 2.68) observed with the X-shooter spectrograph at the Very Large Telescope. We measured very high column densities of atomic and molecular hydrogen with logN(H I, H2) ≃ 21.8, 21.3. This is the highest H2column density ever measured in an intervening damped Lyman-αsystem but we did not detect CO, implying logN(CO)/N(H2) < −7.8, which could be due to a low metallicity of the cloud. From the metal absorption lines, we derived the metallicity to beZ≃ 0.15Z⊙and determined the amount of dust by measuring the induced extinction of the background quasar light,AV≃ 0.4. We simultaneously detected Lyman-αemission at the same redshift with a centroid located at a most probable impact parameter of onlyρ≃ 1.4 kpc. We argue that the line of sight is therefore likely passing through the interstellar medium (ISM), as opposed to the circumgalactic medium (CGM), of a galaxy. The relation between the surface density of gas and that of star formation seems to follow the global empirical relation derived in the nearby Universe although our constraints on the star formation rate (SFR) and the galaxy extent remain too loose to be conclusive. We study the transition from atomic to molecular hydrogen using a theoretical description based on the microphysics of molecular hydrogen. We use the derived chemical properties of the cloud and physical conditions (Tk≃ 90 K andn≃ 250 cm−3) derived through the excitation of H2rotational levels and neutral carbon fine structure transitions to constrain the fundamental parameters that govern this transition. By comparing the theoretical and observed H Icolumn densities, we are able to bring an independent constraint on the incident ultra-violet (UV) flux, which we find to be in agreement with that estimated from the observed SFR.
Highlights
Stars are known to form from the gravitational collapse of cold dense gas clumps in the interstellar medium (ISM; see Leroy et al 2008)
By comparing the theoretical and observed H i column densities, we are able to bring an independent constraint on the incident ultra-violet (UV) flux, which we find to be in agreement with that estimated from the observed star formation rate (SFR)
This allows us to study the global relationship between the gas phase and galactic properties on one side, and to investigate the physical conditions and microphysics of the H i–H2 transition on the other side
Summary
Stars are known to form from the gravitational collapse of cold dense gas clumps in the interstellar medium (ISM; see Leroy et al 2008). Pontzen et al 2008) and observed over a wide range of redshifts (Zwaan et al 2005; Rao et al 2011; Krogager et al 2012) Based on these considerations, Noterdaeme et al (2014) searched for extremely strong DLAs (ESDLAs; with log N(H i) > 21.7) in the Sloan Digital Sky Survey (SDSS) (York et al 2000). We present the simultaneous detection of molecular gas with very high H2 column density and star formation activity from a galaxy at z ≈ 2.46 aligned with the background quasar SDSS J 151349.52+035211.68 (hereafter J 1513+0352).
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