Mon. Not. R. Astron. Soc., 305, 849-858 (1999/June-1)
Extended Ly-alpha emission from a damped Ly-alpha absorber at z = 1.93, and the relation between damped Ly-alpha absorbers and Lyman-break galaxies.
FYNBO J.U., MOLLER P. and WARREN S.J.
Abstract (from CDS):
The number of damped Lyα absorbers (DLAs) currently known is about 100, but our knowledge of their sizes and morphologies is still very sparse, as very few have been detected in emission. Here we present narrow-band and broad-band observations of a DLA in the field of the quasar pair Q0151+048A (qA) and Q0151+048B (qB). These two quasars have very similar redshifts, zem=1.922 and 1.937 respectively, and an angular separation of 3.27 arcsec. The spectrum of qA contains a DLA at zabs = 1.9342 (close to the emission redshift) which shows an emission line in the trough, detected at 4σ. Our narrow-band image confirms this detection, and we find Lyα emission from an extended area covering 6x3 arcsec2, corresponding to 25x12 h–2 kpc2 (q0=0.5, H0 = 100 h km.s–1). The total Lyα luminosity from the DLA is 1.2x1043 h–2 erg.s–1, which is several times higher than the Lyα luminosity found from other DLAs. The narrow-band image also indicates that qB is not covered by the DLA. This fact, together with the large equivalent width of the emission line from the Lyα cloud, the large luminosity, and the ∼ 300 km.s–1 blueshift relative to the DLA, can plausibly be explained if qB is the source of ionizing photons, lying to the near side of the DLA at a distance from the DLA of <20 h–1 kpc. In this case the size of the emission-line region corresponds to the area over which the cloud is optically thick, i.e., is indicative of the size of a Lyman-limit system. We also consider the relation between DLAs and Lyman-break galaxies (LBGs). If DLAs are gaseous discs surrounding LBGs, and if the apparent brightnesses and impact parameters of the few identified DLAs are representative of the brighter members of the population, then the luminosity distribution of DLAs is nearly flat, and we would expect that some 70 per cent of the galaxy counterparts to DLAs at z ~ 3 are fainter than mR=28.
1999, Royal Astronomical Society
galaxies: formation - quasars: absorption lines - quasars: individual: Q0151+048
Table 3, text: [FMW99] SN (Nos S4-S5), [FMW99] gA (Nos gA-gB), [FMW99] s, [FMW99] psf A (Nos A-B).
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