  We present a near-infrared spectrum of the hot ($T_{\rm eff}$ $\approx$
55,000 K) DA white dwarf PG 1234+482. We confirm that a very low mass companion
is responsible for the previously recognised infrared photometric excess. We
compare spectra of M and L dwarfs, combined with an appropriate white dwarf
model, to the data to constrain the spectral type of the secondary. We find
that uncertainties in the 2MASS $HK$ photometry of the white dwarf prevent us
from distinguishing whether the secondary is stellar or substellar, and assign
a spectral type of L0$\pm$1 (M9-L1).Therefore, this is the hottest and youngest
($\approx 10^6$ yr) DA white dwarf with a possible brown dwarf companion.
