A search for H I 21 cm absorption and emission from a damped Ly alpha absorption line system at redshift z approximately equal to 3.06 in the direction of PKS 0336-017

Details A search for H I 21 cm absorption and emission from a damped Ly alpha absorption line system at redshift z approximately equal to 3.06 in the direction of PKS 0336-017 A search for H I 21 cm absorption and emission from a damped Ly alpha absorption line system at redshift z approximately equal to 3.06 in the direction of PKS 0336-017

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109..480t&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 109, no. 2, p. 480-485

Astronomy and Astrophysics

Astronomy

5

Absorption Spectra, Emission Spectra, Hydrogen, Line Spectra, Quasars, Radio Astronomy, Lyman Alpha Radiation, Radio Spectra, Red Shift, Very Large Array (Vla)

Scientific paper

A search for absorption and emission in the 21 cm line of neutral hydrogen using the Very Large Array (VLA) has been made in a field selected by presence of a damped Ly alpha absorption-line system (zabs = 3.0619) observed in the spectrum of the background radio-loud QSO PKS 0336-017. No significant absorption or emission due to redshifted 21 cm radiation was detected. An upper limit to the size of possible H I masses in the surveyed volume is 1.3 x 1014 solar mass, which for the 3.5 min x 2.5 min one-beam area around the direction of PKS 0336-017 becomes 0.8 x 1014 solar mass for a full width at half maximum (FWHM) velocity of 167 km/s, (omega0 = 1, H0 = 100 km/s/Mpc). In order for the absorbing gas in the damped Ly alpha absorption system to escape detection in absorption against the radio continuum of the quasar, the spin temperature in the intervening absorber must be greater than 450 K if the bulk of the H I is contained in a cloud with Doppler parameter b approximately equals 13 km/s; if the intervening cloud is described by a single component with b as high as 100 km/s, then the spin temperature must be greater than 100 K.

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