  KK242 is a LV dwarf of transition type residing in the void environment. Koda
et al. present clear indications on its connection with Scd galaxy NGC6503.
This implies the distance to KK242 of ~6.3 Mpc and its M_B = -10.5 mag. Its
radial velocity, known from the Effelsberg radio telescope \HI\ observations,
reveals, however, the difference with that of NGC6503, dV ~ 400 km/s. If real,
this fact implies the substantial constraints on its origin. To clear-up the
issue of KK242 radial velocity, we obtained with the SAO 6-m telescope spectra
of its faint star-forming (SF) complex. H-alpha and H-beta emission is detected
in two adjacent compact regions, the southern and northern, separated by ~2"
(~60 pc). Their mean radial velocity is V_hel = -66 km/s, ~100 km/s lower than
that of NGC6503. We use the HST Legacy Archive images and photometry of
individual stars from the Extragalactic Distance Database, available for KK242,
to identify in the SF complex the exciting hot stars, the probable BHeB and
RHeB stars and a supernova remnant. We address, based on the possible range of
its gas metallicity, the probable evolutionary paths of KK242. Using package
Cloudy and parameters of the exciting B0V stars, we conclude that the observed
flux ratio of [Sii] doublet to H-alpha is consistent with the value of
12+log(O/H) ~7.35+/-0.18 dex, expected for a stripped void dIrr galaxy.
