Detection of C I in Absorption toward PKS 1830 - 211 with the eSMA

Details Detection of C I in Absorption toward PKS 1830 - 211 with the eSMA Detection of C I in Absorption toward PKS 1830 - 211 with the eSMA

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...690l.130b&link_type=abstract

The Astrophysical Journal Letters, Volume 690, Issue 2, pp. L130-L134 (2009).

Astronomy and Astrophysics

Astronomy

3

Galaxies: Ism, Ism: Abundances, Quasars: Absorption Lines, Quasars: Individual: Pks 1830

Scientific paper

We report the first science observations and results obtained with the "extended" SMA (eSMA), which is composed of the SMA (Submillimeter Array), JCMT (James Clerk Maxwell Telescope), and CSO (Caltech Submillimeter Observatory). Redshifted absorptions at z = 0.886 of C I (3 P 1-3 P 0) were observed with the eSMA with an angular resolution of 0farcs55 × 0farcs22 at 1.1 mm toward the southwestern image of the remarkable lensed quasar PKS 1830 - 211, but not toward the northeastern component at a separation of ~1''. Additionally, SMA observations of CO, 13CO, and C18O (all J = 4-3) were obtained toward this object: CO was also detected toward the southwest component, but none of the isotopologues were. This is the first time [C I] has been detected in this object, allowing the first direct determination of relative abundances of neutral atomic carbon to CO in the molecular clouds of a spiral galaxy at z > 0.1. The [C I] and CO profiles can be decomposed into two and three velocity components, respectively. We derive C/CO column density ratios ranging from lsim0.5 (representative of dense cores) to ~2.5 (close to translucent cloud values). This could indicate that we are seeing environments with different physical conditions or that we are witnessing the chemical evolution of regions where C has not completely been converted into CO.

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