Other
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4802t&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #48.02; Bulletin of the American Astronomical Society, Vol. 24, p.806
Other
1
Scientific paper
The spectrum of the bright high redshift (zem = 4.11) QSO 0000-2619 reveals the presence of a foreground damped Lyalpha absorption line system at zabs = 3.3900. The line-of-sight toward Q0000-2619 is therefore of great interest because a damped Lyalpha absorption line is the expected signature of a galactic or proto-galactic HI disk. We are continuing our investigation of objects in the direction of this sight-line in order to find emission from young or primeval galaxies near z = 3.4. We report here on the discovery of a second radio quiet emission line galaxy displaced ~ 86 arcsec to the southeast of the QSO. The spectrum of the galaxy contains a strong emission line at ~ 5383 Angstroms which has observed equivalent width W > 720 Angstroms and FWHM =~ 1000 km s(-1) . Identifying this emission line with Lyalpha puts the redshift of the galaxy at z = 3.428. We have reported a lower limit on the observed equivalent width of the emission line because the continuum of the galaxy (corresponding to rest frame ultraviolet) is very weak with m_V =~ 24.5. The velocity separation between the damped Lyalpha absorber and the emission line galaxy is Delta v =~ 2600 km s(-1) . Lyalpha emission from the galaxy is resolved, having a size of ~ 3.5 arcsec. Thus, for q_O = 0.5 and H_O = 50 km sec(-1) Mpc(-1) , we find that the projected separation between the galaxy and the damped absorber at z = 3.4 is ~ 600 kpc, while the extent of the galaxy's Lyalpha emission is ~ 25 kpc. The continuum absolute magnitude of the galaxy in the rest frame ultraviolet is ~ -20.5. The existence of this new object supports the conclusion that there is an association or cluster of radio quiet galactic objects along the line-of-sight to Q0000-2619 near z = 3.4. In another poster paper presented at this meeting (Giavalisco et al.), further interpretation of these new observations is given. We thank M. Bencke for his early work on this project.
Giavalisco Mauro
Hazard Cyril
Lipari Sebastian
Macchetto Ferdinando
McMahon Richard
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