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Issue A&A
Volume 392, Number 3, September IV 2002
Page(s) 781 - 789
Section Cosmology
DOI 10.1051/0004-6361:20021187



A&A 392, 781-789 (2002)
DOI: 10.1051/0004-6361:20021187

Detection of molecular hydrogen in a near Solar-metallicity damped Lyman- $\alpha$ system at $z_\mathsf{abs}$ $\approx$ 2 toward Q 0551-366

C. Ledoux1, R. Srianand2 and P. Petitjean3, 4

1  European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile
2  IUCAA, Post Bag 4, Ganesh Khind, Pune 411 007, India
    e-mail: anand@iucaa.ernet.in
3  Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago, 75014 Paris, France
    e-mail: petitjean@iap.fr
4  LERMA, Observatoire de Paris, 61 avenue de l'Observatoire, 75014, Paris, France

(Received 11 May 2001 / Accepted 24 June 2002 )

Abstract
We report the detection of H 2, C I, C I $^\star$, C I $^{\star\star }$ and Cl I lines in a near Solar-metallicity ([ Zn/H ]=-0.13) damped Lyman- $\alpha$ (DLA) system at $z_{\rm abs}=1.962$ observed on the line of sight to the quasar Q 0551-366. The iron-peak elements, ${\rm X}={\rm Fe}$, Cr and Mn are depleted compared to zinc, [ X/Zn $]\sim -0.8$, probably because they are tied up onto dust grains. Among the three detected H 2-bearing clouds, spanning 55 km s -1 in velocity space, we derive a total molecular hydrogen column density N(H $_2)=2.6\times 10^$ cm -2 and a mean molecular fraction f=2N(H 2)/(2N(H 2)+N(H I $))=1.7\times 10^$. The depletion of heavy elements (S, Si, Mg, Mn, Cr, Fe, Ni and Ti) in the central component is similar to that observed in the diffuse neutral gas of the Galactic halo. This depletion is approximately the same in the six C I-detected components independently of the presence or absence of H 2. The gas clouds in which H 2 is detected always have large densities, $n_{\rm H}>30$ cm -3, and low temperatures, $T_{\rm01}\la 100$ K. This shows that presence of dust, high particle density and/or low temperature is required for molecules to be present. The photo-dissociation rate derived in the components where H 2 is detected suggests the existence of a local UV radiation field similar in strength to the one in the Galaxy. Star formation therefore probably occurs near these H 2-bearing clouds.


Key words: cosmology: observations -- galaxies: halos -- galaxies: ISM -- quasars: absorption lines -- quasars: individual: Q 0551-366

Offprint request: C. Ledoux, cledoux@eso.org

SIMBAD Objects in preparation



© ESO 2002


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