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tokens: the SDSS data from at least one star-forming region in each galaxy in the sample suggest that the sample galaxies are undergoing young massive star formation phase having a significant population of WR stars. Figure 8. The blue WR bump detected in the spatially resolved star-forming regions of SBS 1222+614. The dashed-dot line represents the continuum fit. The solid line represents a Gaussian fit to the blue bump. Figure 9. The detection of the red WR bump in the spatially resolved star-forming region of SBS 1222+614. The dashed-dot line represents the continuum fit. The solid line represents a Gaussian fit to the red bump. 3.3 Ionization mechanism The detection of high ionization emission lines of He ii λ4686, [O iii ] λ4363, [O iii ] λ4959, 5007, and [Ar iii ] λ7135 and low ionization emission lines of [O ii ] λ3726, [N ii ] λ6584 and [S ii ] λ6717, 6731 etc., in the galaxy spectrum can be an indication of mix of many excitation sources such as photoionization mainly from massive ionizing stars and shocks generated by WR stars, supernovae explosions, and energetic active galactic nuclei-related mechanisms as discussed by Garnett et al. ( 1991 ), Garnett, Kennicutt Bresolin ( 2004 ), Guseva et al. (2000 ), and López-Sánchez Esteban ( 2010a ). Therefore, it is necessary to identify the dominant excitation mechanism in these galaxies. The nature of the dominant ionizing source can be inferred using the quantitative classification scheme proposed by Baldwin, Phillips Terlevich ( 1981 ) using combinations of line ratios. Subsequently, other similar diagnostic schemes were proposed by Dopita et al. ( 2000 ) and Kewley et al. ( 2001 ). All these diagnostic schemes use the emission line ratios of [O iii ] λ5007/H β, [N ii ] λ6583/H α and [S ii ] λ6717, 6731/H α. The optical emission line ratios for all the spatially resolved ionized regions in our galaxy sample are listed in Table 3 and the locations of all the star-forming regions are presented in Fig. 10 , which shows typical plots for [O iii ] λ5007/Hβ versus [N ii ] λ6583/Hα (top panel) and [O iii ] λ5007/H β versus [S ii ] λ6717, 6731/H α (bottom panel). Here, we used the latest Kewley et al. ( 2001 ) diagnostic criteria to identify source of excitation mechanism. In these figures, it can be seen that the primary and dominating source of ionization is photoionization in all the cases. Figure 10. A comparison of the observed flux line ratios obtained from the star-forming regions in our sample of dwarf galaxies with the diagnostic diagrams proposed by Kewley et al. ( 2001 ). 3.4 Physical conditions of the ionized gas The electron temperature ( T e ) and density ( n e ) of the ionized gas in the H ii regions are estimated here. Since the faint auroral [O iii ] λ4363 emission line along with the [O iii ] λ4959, 5007 emission lines were detected in many cases, the electron temperature could be estimated directly using their relative line intensities. A two-zone approximation was assumed to