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H2, C I, Metallicity, and Dust Depletion in the z = 2.34 Damped Lyα Absorption System toward QSO 1232+0815*

Jian Ge et al 2001 ApJ 547 L1-L5   doi: 10.1086/318890  Help

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Jian Ge1,2, Jill Bechtold1 and Varsha P. Kulkarni1,3
1 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065
2 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802
3 Permanent address: Clemson University, Department of Physics and Astronomy, 118 Kinard Laboratory, Clemson, SC 29634-0978
E-mail: jge@as.arizona.edu, jill@as.arizona.edu and kulkarni@as.arizona.edu

ABSTRACT. We report the detection of strong molecular hydrogen (H2) absorption lines in the z = 2.34 damped Lyα absorber (DLA) toward QSO 1232+0815. This is the second detection in our survey for high-redshift molecules. The new ultraviolet spectrum of the QSO 1232+0815 at 0.9 Å resolution, taken with the Multiple Mirror Telescope Blue Channel Spectrograph, shows the υ = 0-0 up to 10-0 Lyman bands and also the Werner υ = 0-0 band of H2 associated with the z = 2.34 DLA. We have estimated the total H2 column density in this system. It ranges from approx3 × 1019 cm-2 to approx3 × 1017 cm-2 depending on the Doppler parameters, b = 6 or 10 km s-1. Based on the best fit with b = 6 km s-1, the estimated kinetic temperature is TK approx 80 K. The measurements of the abundance of zinc and iron in the same DLA show that the metallicity measured by the relatively undepleted element zinc is [Zn/H] = -0.86, while the relative abundance ratio [Fe/Zn] is -1.04, indicating dust depletion. Combining our work with previous results on H2 and relative heavy-element depletion, we find that there is a correlation between them, which suggests that the formation of H2 on dust grains is perhaps the dominant formation process in high-redshift DLAs. Detections of strong absorption from the ground and excited states of neutral carbon (C I) in the z = 2.34 DLA are also presented. The excitation temperature between the two fine-structure levels of C I is 15.7 ± 3.5 K, an upper limit for the cosmic microwave background radiation temperature at z = 2.34. This value is consistent with the prediction by the standard big bang cosmology.

Subject headings: cosmic microwave background; dust, extinction; early universe; galaxies: abundances; ISM: molecules; quasars: absorption lines; quasars: individual (QSO 1232+0815)

* Observations here were obtained with the Multiple Mirror Telescope, a joint facility of the University of Arizona and the Smithsonian Institution.

Print publication: Issue 1 (2001 January 20)
Received 2000 October 2, accepted for publication 2000 November 7
Published 2001 January 16

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