  We investigate expected sub-mm emission and dust properties of the Lyman
Break Galaxies (LBGs) in the Hubble Deep Field (HDF). The SCUBA Deep Survey
(Hughes et al., 1998) provides an upper limit of the 850 micron flux densities
of the LBGs. With this constraint, we argue that a typical ultra-violet to
far-infrared spectral shape of the high-redshift LBGs is rather close to a
template spectrum of low-reddening starburst galaxies in the local universe but
different from that of heavily dust-enshrouded ultra-luminous far-infrared
galaxies like Arp220. We also evaluate the lower-limit temperature of dust in
LBGs assuming single- and two-component modified black-body spectrum. To
estimate the total amount of energy re-emitted in FIR wavelength, we take two
different approaches; model fitting of the UV spectra of LBGs and an empirical
method using the relationship between UV spectral shape and UV/FIR flux ratio
observed for local starburst galaxies. Both methods give lower-limit
temperature of the LBGs as around 40 K, which is higher than the typical dust
temperature of local optical- and infrared-selected galaxies. This result is
also supported by the comparison of the expected sub-mm flux of the LBGs with
the cosmic FIR background radiation. The high dust temperature may indicate the
effective massive-star formation or different dust properties in the
high-redshift LBGs.
