UVIT imaging of WLM : Demographics of star forming regions in the nearby
  dwarf irregular galaxy
  We present a study of star forming regions and its demographics in the nearby
dwarf irregular galaxy WLM using the Ultra-Violet Imaging Telescope (UVIT)
multi band observations in three filters F148W, N245M and N263M. We find that
the UV emission is extended at least up to 1.7 kpc, with the NUV emission more
extended than the FUV. We create UV color maps ((F148W$-$N245M) and
(F148W$-$N263M)) to study the temperature morphology of young stellar complexes
with the help of theoretical models. We identify several complexes with
temperature T $>$ 17500 K which are likely to be the OB associations present in
the galaxy. These complexes show good spatial correlation with the H$\alpha$
emitting regions, H$~$I distribution and HST detected hot stars. The hot star
forming regions are found to be clumpy in nature and show a hierarchical
structure, with sizes in the range of 4 - 50 pc, with a large number with sizes
$<$ 10 pc. The south western part of the galaxy shows many hot star forming
regions, high level of H$\alpha$ emission and low column density of H$~$I which
altogether denote a vigorous recent star formation. WLM is likely to have a
large fraction of low mass compact star forming regions with mass M $< 10^3
M_{\odot}$, in agreement with the size and mass of the CO clouds. We estimate
the star formation rate of WLM to be $\sim$ 0.008 $M_{\odot}/yr$, which is
similar to the average value measured for nearby dwarf irregular galaxies.
