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In this study we present high-resolution VIsible Multi-Object Spectrographintegral field unit spectroscopy (VIMOS-IFU) of the extremely metal-poorHII/blue compact dwarf (BCD) galaxy Tol 65. The optical appearance of thisgalaxy shows clearly a cometary morphology with a bright main body and anextended and diffuse stellar tail. We focus on the detection of metallicitygradients or inhomogeneities as expected if the ongoing star-formation activityis sustained by the infall/accretion of metal-poor gas. No evidences ofsignificant spatial variations of abundances were found within ouruncertainties. However, our findings show a slight anticorrelation between gasmetallicity and star-formation rate at spaxel scales, in the sense that highstar-formation is found in regions of low-metallicity, but the scatter in thisrelation indicates that the metals are almost fully diluted. Our observationsshow the presence of extended H$\alpha$ emission in the stellar tail of thegalaxy. We estimated that the mass of the ionized gas in the tailM(HII)$_{tail} \sim$1.7$\times$10$^5$ M$_{\odot}$ corresponds with $\sim$ 24per cent of the total mass of the ionized gas in the galaxy. We found that theH$\alpha$ velocity dispersion of the main body and the tail of the galaxy arecomparable with the one found in the neutral gas by previous studies. Thissuggests that the ionized gas still retains the kinematic memory of itsparental cloud and likely a common origin. Finally, we suggest that theinfall/accretion of cold gas from the outskirts of the galaxy and/or minormerger/interaction may have produced the almost flat abundance gradient and thecometary morphology in Tol 65.

monthly notices of the royal astronomical society

On the properties of the interstellar medium in extremely metal-poor  blue compact dwarf galaxies. A VIMOS-IFU study of the cometary galaxy and Ly  $\alpha$ absorber Tol 65