  Extensive optical and infrared photometry as well as low and high resolution
spectroscopy are used as inputs in deriving robust estimates of the reddening,
distance and nature of the progenitor of V838 Mon. The reddening is found to
obey the R_V=3.1 law and amounts to (i) E(B-V)=0.86 from the interstellar NaI
and KI lines, (ii) E(B-V)=0.88 from the energy distribution of the B3V
component and (iii) E(B-V)=0.87 from the progression of extinction along the
line of sight. The adopted E(B-V)=0.87(+/-0.01) is also the amount required by
fitting the progenitor with theoretical isochrones of appropriate metallicity.
The distance is estimated from (a) the galactic kinematics of the three
components of the interstellar lines, (b) the amount of extinction vs the HI
column density and vs the dust emission through the whole Galaxy in that
direction, from (c) spectrophotometric parallax to the B3V companion, from (d)
comparison of the observed color-magnitude diagram of field stars with 3D
stellar population models of the Galaxy, from (e) comparison of theoretical
isochrones with the components of the binary system in quiescence and found to
be around 10 kpc. Pre-outburst optical and IR energy distributions show that
the component erupting in 2002 was brighter and hotter than the B3V companion.
The best fit is obtained for a 50,000 K source, 0.5 mag brighter than the B3V
companion. Comparison with theoretical isochrones suggests an age of 4 million
year for the system and a mass around 65 M(sun) for the progenitor of the
outbursting component, which at the time of the outburst was approaching the
Carbon ignition stage in its core. The 2002 event is probably just a shell
thermonuclear event in the outer envelope of the star.
