2022MNRAS.516.6180P

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 NGC 6503. 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 H I observations, reveals, however, the difference with that of NGC 6503, ΔV ∼ 400 km s^–1. 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 α and H β emission is detected in two adjacent compact regions, the southern and northern, separated by ∼2 arcsec (∼60 pc). Their mean radial velocity is V_hel = -66 km s^–1, ∼100 km s^–1 lower than that of NGC 6503. 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 the [S II] doublet to H α is consistent with the value of 12+log (O/H) ∼7.35 ± 0.18 dex, expected for a stripped void dIrr galaxy.