O/H-N/O: the curious case of NGC 4670
  We use integral field spectroscopic (IFS) observations from Gemini North
Multi-Object Spectrograph (GMOS-N) of a group of four H II regions and the
surrounding gas in the central region of the blue compact dwarf (BCD) galaxy
NGC 4670. At spatial scales of $\sim$ 9 pc, we map the spatial distribution of
a variety of physical properties of the ionised gas: internal dust attenuation,
kinematics, stellar age, star-formation rate, emission line ratios and chemical
abundances. The region of study is found to be photoionised. Using the robust
direct T$_e$-method, we estimate metallicity, nitrogen-to-oxygen ratio and
helium abundance of the four H II regions. The same parameters are also mapped
for the entire region using the HII-CHI-mistry code. We find that log(N/O) is
increased in the region where the Wolf-Rayet bump is detected.The region
coincides with the continuum region, around which we detect a slight increase
in He abundance. We estimate the number of WC4, WN2-4 and WN7-9 stars from the
integrated spectrum of WR bump region. We study the relation between log(N/O)
and 12 + log(O/H) using the spatially-resolved data of the FOV as well as the
integrated data of the H II regions from ten BCDs. We find an unexpected
negative trend between N/O and metallicity. Several scenarios are explored to
explain this trend, including nitrogen enrichment, and variations in star
formation efficiency via chemical evolution models.
