  Blue metal-poor stars are main-sequence stars that are bluer and brighter
than typical turn-off stars in metal-poor globular clusters. They are thought
to have either evolved through post-mass transfer mechanisms as field blue
straggler stars or have accreted from Milky Way dwarf satellite galaxies. It
has been found that a considerable fraction of blue metal poor stars are
binaries, possibly with a compact companion. We observed 27 blue metal poor
stars using UV imaging telescope of AstroSat in two far-UV filters, F148W and
F169M. In this work, we explain the possible formation channels of two stars,
BMP17 and BMP37. We fit BMP17 with a single-component spectral energy
distribution whereas BMP37 with a binary-component spectral energy
distribution. As both of them are known SB1s, we suggest that the WD companion
of BMP17 may have cooled down so that it is out of UV imaging telescope
detection limit. On the other hand, we discover a normal mass white dwarf as
the hot companion of BMP37, indicating mass transfer as the possible formation
channel
