  It has been well established from a variety of observations that red
supergiants (RSGs) loose a lot of mass in stellar wind. Dust formed in this
emitted gas over a few decades before core-collapse can lead to substantial
extinction and obscure the intrinsic luminosity of the progenitor RSG. This may
lead to a difficulty in determining the range of progenitor masses that lead to
the different classes of supernovae. Even the nearby, well studied supernovae
with pre-explosion observations, such as SN 2013ej may suffer from this
uncertainty in the progenitor mass. We explore here two different masses
proposed for its progenitor. We compute their pre-supernova characteristics
using Modules for Experiments in Stellar Astrophysics (MESA). We show that a
non-rotating star with the initial mass of 26 M$_{\odot}$ would require a
considerable amount of circum-stellar medium (A$_V \sim$ 3) to obscure its high
luminosity given the observed pre-explosion magnitudes detected by the Hubble
Space Telescope (HST). Such a high value of visual extinction appears to be
inconsistent with that derived for SN 2013ej as well as SN 2003gd in the same
host galaxy M74. In contrast, the evolutionary models of lower mass (13
M$_{\odot}$) star are easily accommodated within the observed HST magnitudes.
Some of the 26 M$_{\odot}$ simulations show luminosity variation in the last
few years which could be discriminated by high cadence and multi-band
monitoring of supernova candidates in nearby galaxies. We demonstrate that our
calculations are well-resolved with adequate zoning and evolutionary
time-steps.
