Volume 469, Number 2, July II 2007
|Page(s)||425 - 436|
|Published online||11 April 2007|
Physical conditions in the neutral interstellar medium at z = 2.43 toward Q 2348-011*
European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile e-mail: [pnoterda;cledoux]@eso.org
2 Institut d'Astrophysique de Paris, CNRS - Université Pierre et Marie Curie, 98bis boulevard Arago, 75014 Paris, France e-mail: firstname.lastname@example.org
3 LERMA, Observatoire de Paris, 61 avenue de l'Observatoire, 75014 Paris, France
4 IUCAA, Post Bag 4, Ganesh Khind, Pune 411 007, India e-mail: email@example.com
5 LUTH, Observatoire de Paris, 61 Avenue de l'Observatoire, 75014 Paris, France e-mail: firstname.lastname@example.org
Accepted: 6 March 2007
Aims.We aim at deriving the physical conditions in the neutral gas associated with damped Lyman-α systems using observation and analysis of H2 and C i absorptions.
Methods.We obtained a high-resolution VLT-UVES spectrum of the quasar Q 2348-011 over a wavelength range that covers most of the prominent metal and molecular absorption lines from the (H i) = 20.50 ± 0.10 damped Lyman-α system at . We detected H2 in this system and measured column densities of H2, C i, C i*, C i Si ii, P ii, S ii, Fe ii, and Ni ii. From the column density ratios and, in particular, the relative populations of H2 rotational and C i fine-structure levels, we derived the physical conditions in the gas (relative abundances, dust-depletion, particle density, kinetic temperature, and ionising flux) and discuss physical conditions in the neutral phase.
Results.Molecular hydrogen was detected in seven components in the first four rotational levels (J = 0–3) of the vibrational ground state. Absorption lines of H2 (resp. J = 5) rotational levels are detected in six (resp. two) of these components. This leads to a total molecular fraction of . Fourteen components are needed to reproduce the metal-line profiles. The overall metallicity is found to be -0.80, -0.62, -1.17 ± 0.10 for, respectively, [Si/H], [S/H] and [Fe/H]. We confirm the earlier findings that there is a correlation between (Fe ii)/N(S ii) and (Si ii)/N(S ii) from different components indicative of a dust-depletion pattern. Surprisingly, however, the depletion of metals onto dust in the H2 components is not large in this system: [Fe/S] = -0.8 to -0.1. The gas in H2-bearing components is found to be cold but still hotter than similar gas in our Galaxy ( K, instead of typically 80 K) and dense ( cm-3). There is an anti-correlation () between the logarithm of the photo-absorption rate, , and (H2)/N(C i) derived for each H2 component. We show that this is mostly due to shielding effects and imply that the photo-absorption rate is a good indicator of the physical conditions in the gas. We find that the gas is immersed in an intense UV field, about one order of magnitude higher than in the solar vicinity. These results suggest that the gas in H2-bearing DLAs is clumpy, and star-formation occurs in the associated object.
Key words: galaxies: ISM / quasars: absorption lines / quasars: individuals: Q 2348-011
© ESO, 2007
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