  The old open cluster M67, populated with blue straggler stars (BSSs), is a
well known test bed to study the BSS formation pathways. Here, we report the
first direct detection of a white dwarf (WD) companion to a BSS in M67, using
far-UV images from the \textit{Ultra Violet Imaging telescope} ({\it UVIT}) on
{\it ASTROSAT}. Near-simultaneous observations in three far-UV bands combined
with {\it GALEX}, {\it IUE}, ground and space based photometric data covering
0.14 -11.5 $\mu$m range for WOCS1007 were found to require a binary fit to its
spectral energy distribution (SED), consisting of a BSS and a hot companion. On
the other hand, a single spectral fit was found to be satisfactory for the SEDs
of two other BSSs, WOCS1006 and WOCS2011, with the latter showing a deficient
far-UV flux. The hot companion of WOCS1007 is found to have a T$_{eff}$ $\sim$
13250-13750K and a radius of 0.09$\pm$0.01 R$_\odot$. A comparison with WD
models suggests it to be a low mass WD ($\sim$ 0.18$M_\odot$), in agreement
with the kinematic mass from the literature. As a low mass WD ($<$
0.4$M_\odot$) necessitates formation through mass transfer (MT) in close
binaries, WOCS1007 with a known period of 4.2 days along with its fast
rotation, is likely to be formed by a case A or case B binary evolution.
