Abstract
We study the average Ly$\alpha$ emission associated with high-$z$ strong (log
$N$(H I) $\ge$ 21) damped Ly$\alpha$ systems (DLAs). We report Ly$\alpha$
luminosities ($L_Ly\alpha$) for the full as well as various sub-samples
based on $N$(H I), $z$, $(r-i)$ colours of QSOs and rest equivalent width of Si
II$łambda$1526 line (i.e., $W_1526$). For the full sample, we find $L_\rm
Ly\alpha$$< 10^41 (3\sigma)\ erg\ s^-1$ with a $2.8\sigma$ level
detection of Ly$\alpha$ emission in the red part of the DLA trough. The $L_\rm
Ly\alpha$ is found to be higher for systems with higher $W_1526$ with its
peak, detected at $3\sigma$, redshifted by about 300-400 $km\ s^-1$
with respect to the systemic absorption redshift, as seen in Lyman Break
Galaxies (LBGs) and Ly$\alpha$ emitters. A clear signature of a double-hump
Ly$\alpha$ profile is seen when we consider $W_1526 0.4$ \AA\ and $(r-i)
< 0.05$. Based on the known correlation between metallicity and $W_1526$, we
interpret our results in terms of star formation rate (SFR) being higher in
high metallicity (mass) galaxies with high velocity fields that facilitates
easy Ly$\alpha$ escape. The measured Ly$\alpha$ surface brightness requires
local ionizing radiation that is 4 to 10 times stronger than the metagalactic
UV background at these redshifts. The relationship between the SFR and surface
mass density of atomic gas seen in DLAs is similar to that of local dwarf and
metal poor galaxies. We show that the low luminosity galaxies will contribute
appreciably to the stacked spectrum if the size-luminosity relation seen for H
I at low-$z$ is also present at high-$z$. Alternatively, large Ly$\alpha$ halos
seen around LBGs could also explain our measurements.
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