  X-rays in intermediate polars (IPs) originate in a compact region near the
surface of a magnetic white dwarf (WD) and interact with the complex
environment surrounding the emission region. Here we report a case study of two
IPs, TV Col and V2731 Oph with selected archival X-ray observations (NuSTAR,
Swift, Suzaku, and XMM-Newton). For TV Col, we were successful in
simultaneously accounting for the primary X-rays, the secondary X-rays due to
Compton scattering and fluorescence, and the effects of local absorbers. In
this case, we were able to demonstrate that the shock height is small, based on
the high reflection amplitude, and hence the maximum temperature of the
post-shock region can be used to derive the WD mass of 0.735+/-0.015 Msun.
Despite the high specific accretion rate required to explain the small shock
height, we do not detect any spin modulation in our NuSTAR data, consistent
with the modest amount of complex absorption seen spectroscopically. We argue
that our results are robust because they are based on the joint
temporal-spectral analysis of broadband X-ray data. The spectrum of V2731 Oph
is more highly absorbed. Through our analysis of the Suzaku data, we present a
spectral model with nitrogen overabundance without the previously claimed soft
blackbody that should be further explored. We have been unable to constrain
reflection amplitude for V2731 Oph; this and the detection of spin modulation
above 10 keV suggest that it may have a tall shock, hence we only derive a
lower limit to the mass of its WD (> 0.9 Msun).

High Energy Astrophysical Phenomena;Solar and Stellar Astrophysics