A cold component and the complex velocity structure of DLA1331 + 170

Abstract

We examine the velocity structure in the gas associated with Hi in the damped Lyα absorption system at redshift z= 1.7764 towards the QSO 1331 + 170 using Arecibo Hi 21-cm data, optical spectra from the Keck High Resolution Echelle Spectrograph (HIRES) and European Southern Observatory (ESO) Very Large Telescope (VLT) Ultraviolet and Visual Echelle Spectrograph (UVES), and a previously published Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) ultraviolet spectrum. From the optical data we find at least two, and possibly three, components showing Ci lines. One of these has very narrow lines with Doppler parameter b= 0.55 kms-1, corresponding to a kinetic temperature of 220K if the broadening is thermal and with a 2σ upper limit of 480K. We re-examine the H2 analysis undertaken by Cui et al. using the neutral carbon velocity structure, and find a model which is, unlike theirs, consistent with a mixture of collisional and background radiation excitation of the observed H2 rotational levels. Using Voigt profile fits to absorption lines from a range of singly ionized heavy elements we find eight components covering a velocity range of ~110 kms-1, with a further outlier over 120 kms-1 away from the nearest in the main group. The Hi structure is expected to follow some combination of the singly ionized and neutral gas, but the 21-cm absorption profile is considerably different. We suggest, as have others, that this may be because the different extent and brightness distributions of the radio and optical background sources mean that the sightlines are not the same, and so the spin temperature derived by comparing the Lyα and 21-cm line strengths has little physical meaning. The neutral and singly ionized heavy element line profiles also show significant differences, and so the dominant components in each appear to be physically distinct. Attempts to use the range of atomic masses to separate thermal and turbulent components of their Doppler widths were not generally successful, since there are several blended components and the useful mass range (about a factor of 2) is not very large. The velocity structure in all ionization stages up to +3, apart from the neutral heavy elements, is sufficiently complex that it is difficult to separate out the corresponding velocity components for different ionization levels and determine their column densities. © 2010 The Authors Monthly Notices of the Royal Astronomical Society © 2010 RAS.