Kouroumpatzakis, KKKouroumpatzakisZezas, AAZezasWOLTER, AnnaAnnaWOLTERFruscione, AAFruscioneAnastasopoulou, KKAnastasopoulouPrestwich, AAPrestwich2025-02-142025-02-1420200035-8711http://hdl.handle.net/20.500.12386/35952We present a systematic study of the metallicity variations within the collisional ring galaxy NGC 922 based on long-slit optical spectroscopic observations. We find a metallicity difference between star-forming regions in the bulge and the ring, with metallicities ranging from almost solar to significantly sub-solar ($\rm{[12+\log(O/H)]\sim 8.2}$). We detect $\rm He\,_I$ emission in the bulge and the ring star-forming regions indicating ionization from massive stars associated with recent ($<10$ Myr) star-formation, in agreement with the presence of very young star-clusters in all studied regions. We find an anti-correlation between the X-ray luminosity and metallicity of the sub-galactic regions of NGC 922. The different regions have similar stellar population ages leaving metallicity as the main driver of the anti-correlation. The dependence of the X-ray emission of the different regions in NGC 922 on metallicity is in agreement with similar studies of the integrated X-ray output of galaxies and predictions from X-ray binary population models.STAMPAenArticle10.1093/mnras/staa32902-s2.0-85099905978https://academic.oup.com/mnras/article/500/1/962/59366602021MNRAS.500..962KFIS/05 - ASTRONOMIA E ASTROFISICA