  One of the popular models for the low/hard state of Black Hole Binaries is
that the standard accretion disk is truncated and the hot inner region produces
via Comptonization, the hard X-ray flux. This is supported by the value of the
high energy photon index, which is often found to be small $\sim$ 1.7 ($<$ 2)
implying that the hot medium is seed photons starved. On the other hand, the
suggestive presence of a broad relativistic Fe line during the hard state would
suggest that the accretion disk is not truncated but extends all the way to the
inner most stable circle orbit. In such a case, it is a puzzle why the hot
medium would remain photon starved. The broad Fe line should be accompanied by
a broad smeared reflection hump at $\sim$ 30 keV and it may be that this
additional component makes the spectrum hard and the intrinsic photon index is
larger, i.e. $>$ 2. This would mean that the medium is not photon deficient,
reconciling the presence of a broad Fe line in the observed hard state. To test
this hypothesis, we have analyzed the RXTE observations of GX 339-4 from the
four outbursts during 2002-2011 and identify the observations when the system
was in the hard state and showed a broad Fe line. We have then attempted to fit
these observations with models, which include smeared reflection to understand
whether the intrinsic photon index can indeed be large. We find that, while for
some observations the inclusion of reflection does increase the photon index,
there are hard state observations with broad Fe line that have photon indices
less than 2.

High Energy Astrophysical Phenomena