  H1426+428 is one of blazars that are observed by $\gamma$-rays in the TeV
region. Because TeV $\gamma$-rays from distant sources are subject to
attenuation by the extragalactic background light (EBL) via electron-positron
pair production, the intrinsic spectrum of the TeV $\gamma$-rays should be
inferred by using the models of radiation processes and EBL spectrum. We set
constraints on the physical condition of H1426+428 with the
synchrotron-self-Compton model applying several EBL models. We find that the
emission region of H1426+428 is moving toward us with the bulk Lorentz factor
of $\sim 20$ and that its magnetic field strength is $\sim 0.1$ G. These
properties are similar to other TeV blazars such as Mrk 421 and Mrk 501.
However, the ratio of the energy density of nonthermal electrons to that of the
magnetic fields is about 190 and fairly larger than those of Mrk 421 and Mrk
501, which are about 5 -- 20. It is also found that the intensity of EBL in the
middle and near infrared wavelengths should be low, i.e., the intensity at 10
$\mu$m is about 1 nW m$^{-2}$ sr$^{-1}$ to account for the observed TeV
$\gamma$-ray flux. Because the spectral data of H1426+428 in X-rays and
$\gamma$-rays used in our analysis were not obtained simultaneously, further
observations of TeV blazars are necessary to make the constraints on EBL more
stringent.
