The following document lists the file abstract/CWALKER_CW_C2ALS.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
We propose to study the [C II] emission line of 3 quasar absorption line systems toward S4 0248+43, PKS 0038-019 and PKS 1327-206. Their corres- ponding redshifts are 0.0515, 0.0177 and 0.0175, respectively. The ab- sorption line system toward S4 0248+43 has been identified with a nearby starburst galaxy. These 3 absorber galaxies offer excellent sites to study the starburst and normal star formation activity at low redshifts. Since they are at low redshift, optical and radio wavelength spectrosco- py, optical and near-IR imaging and IRAS observations provide a great deal of direct information about the physical properties of the absorber galaxies. Toward these 3 sources (and almost 2 dozen other absorption line systems at different redshifts), we have obtained detections or li- mits on the CO (and in some instances, [C I]) emission at radio wave- lengths. We also have programs at several radio telescopes to observe [C II] toward high-z galaxies. The absorbers toward S4 0248+43, PKS 0038-019 and PKS 1327-206 are among the most luminous CO emitters in our millimeter-wave survey of low redshift quasar absorption line systems, and will be good candidates for further mm- and sub-mm work. Here we propose to obtain the redshifted 158 um [C II] emission line spectrum to enable a comparison of these systems with other quasar absorption line systems at higher z. The LWS data will complement the radio obser- vations to give a more complete picture of the physical conditions in these galaxies. From the [C II] emission line measurements in associ- ation with complementary observations, we will be able to study the chemical abundance, molecular content, UV radiation field and dust-to- gas ratio of the ISM in the absorber galaxies. In particular, from the [C II]/CO ratio we will be able to determine whether any of the ab- sorption line systems are undergoing a starburst.