  We present the results from a detailed deprojection analysis of Abell 1835 as
observed by {\it XMM-Newton}. If we fit the spectra with an isothermal plasma
model, the deprojected temperature profile is flat in the outer region around
7.6 keV and decreases to $\sim$ 5.6 keV in the center, which may be connected
with the gas cooling. In the central part, a two-component thermal plasma model
can fit the spectrum significantly better. Moreover, the cool component (T
$\sim$ 1.8 keV) has a much lower metal abundance than the hot component (T
$\sim$ 8 keV), which may be due to the longer cooling time for the cool gas
with lower abundance. In addition, it was found that without a main isothermal
component, the standard cooling flow model cannot fit the spectrum
satisfactorily. From the isothermal model fitting results we also derived the
electron density $n_e$, and fitted its radial distribution with a
double-$\beta$ model. The $n_e$ profile inferred with the double-$\beta$ model
and the deprojected X-ray gas temperature profile were then combined to derive
the total mass and the total projected mass of the cluster. The projected mass
is lower than that derived from the weak lensing method. However, assuming that
the cluster extends to a larger radius $\sim15'$ as found by Clowe & Schneider
(2002), the two results are consistent within the error bars. Furthermore, we
calculated the projected mass within the radius of $\sim$ 153 kpc implied by
the presence of a gravitational lensing arc, which is about half of the mass
determined from the optical lensing.
