A translucent interstellar cloud at z = 2.69

CO, H₂, and HD in the line-of-sight to SDSS J123714.60 + 064759.5^⋆

¹ Departamento de AstronomíaUniversidad de Chile, Casilla 36-D, Santiago, Chile
e-mail: pasquier@das.uchile.cl; slopez@das.uchile.cl
² Université Paris 6, Institut d’Astrophysique de Paris, CNRS UMR 7095, 98bis bd Arago, 75014 Paris, France
e-mail: petitjean@iap.fr
³ European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
e-mail: cledoux@eso.org
⁴ Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India
e-mail: anand@iucaa.ernet.in
⁵ Université Paris 7, APC, CNRS UMR 7164, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
⁶ GEPI, Observatoire de Paris, CNRS UMR 8111, 5 place Jules Janssen, 92195 Meudon, France
e-mail: vergani@apc.univ-paris7.fr

Received: 3 June 2010
Accepted: 2 August 2010

Abstract

We present the analysis of a sub-damped Lyman-α system with neutral hydrogen column density, log N(H⁰) (cm^-2) = 20.0 ± 0.15 at z_abs = 2.69 toward SDSS J123714.60 + 064759.5 (z_em = 2.78). Using the VLT/UVES and X-shooter spectrographs, we detect H₂, HD, and CO molecules in absorption with log N(H₂, HD, CO) (cm^-2) = 19.21, 14.48 ± 0.05 and 14.17 ± 0.09 respectively. The overall metallicity of the system is super-solar ([Zn/H] = +0.34 relative to solar) and iron is highly depleted ([Fe/Zn] =  −1.39), revealing metal-rich and dusty gas. Three H₂ velocity components spanning  ~125 km s^-1 are detected. The strongest H₂ component, at z_abs = 2.68955, with log N(H₂) = 19.20, does not coincide with the centre of the H i absorption. This implies that the molecular fraction in this component, f_H2 = 2N(H₂)/(2N(H₂)+N(H⁰)), is higher than the mean molecular fraction ⟨f_H2⟩ = 1/4 in the system. We also found the Cl⁰ associated with this H₂ component to have N(Cl⁰)/N(Cl⁺)  >  0.4, which points in the same direction. Cl⁰ is tied to H₂ by charge exchange reactions, this means that the molecular fraction in this component is not far from unity. The kinetic temperature derived from the J    =    0 and 1 rotational levels of H₂ is  K and the particle density derived from the C⁰ ground-state fine structure level populations is n_H0  ~  50–60 cm^-3. We derive an electronic density  <2 cm^-3 for a UV field similar to the Galactic one and show that the carbon-to-sulphur ratio in the cloud is close to the solar ratio. The size of the molecular cloud is probably smaller than 1 pc. Both the CO/H₂ = 10^-5 and CO/C⁰  ~  1 ratios for f_H2 > 0.24 indicate that the cloud classifies as translucent, i.e., a regime where carbon is found both in atomic and molecular form. The corresponding extinction, A_V = 0.14, albeit lower than the definition of a translucent sightline (based on extinction properties), is high for the observed H⁰ column density. This means that intervening clouds with similar local properties but with higher column densities (i.e. larger physical extent) could be missed by current magnitude-limited QSO surveys. The excitation of CO is dominated by radiative interaction with the cosmic microwave background radiation (CMBR) and we derive T_ex(CO) = 10.5 K when T_CMBR(z = 2.69) = 10.05 K is expected. We measure N(HD) / 2N(H₂) = 10^-5. This is about 10 times higher than what is measured in the Galactic ISM for f_H2 = 1/4 but similar to what is measured in the Galactic ISM for higher molecular fractions. The astration factor of deuterium with respect to the primordial D/H ratio is only about 3. This can be the consequence of accretion ofunprocessed gas from the intergalactic medium onto the associated galaxy. In the future, it will be possible to search efficiently for molecular-rich DLAs/sub-DLAs with X-shooter, but detailed studies of the physical state of the gas will still need UVES observations.