In this study we present high-resolution VIsible Multi-Object Spectrograph integral field unit spectroscopy ( VIMOS-IFU ) of the extremely metal-poor H ii /blue compact dwarf ( BCD ) galaxy Tol 65 .
The optical appearance of this galaxy shows clearly a cometary morphology with a bright main body and an extended and diffuse stellar tail .
We focus on the detection of metallicity gradients or inhomogeneities as expected if the ongoing star-formation activity is sustained by the infall/accretion of metal-poor gas .
No evidences of significant spatial variations of abundances were found within our uncertainties .
However , our findings show a slight anticorrelation between gas metallicity and star-formation rate at spaxel scales , in the sense that high star-formation is found in regions of low-metallicity , but the scatter in this relation indicates that the metals are almost fully diluted .
Our observations show the presence of extended H \alpha emission in the stellar tail of the galaxy .
We estimated that the mass of the ionized gas in the tail M ( H ii ) _ { tail } \sim 1.7 \times 10 ^ { 5 } M _ { \odot } corresponds with \sim 24 per cent of the total mass of the ionized gas in the galaxy .
We found that the H \alpha velocity dispersion of the main body and the tail of the galaxy are comparable with the one found in the neutral gas by previous studies .
This suggests that the ionized gas still retains the kinematic memory of its parental cloud and likely a common origin .
Finally , we suggest that the infall/accretion of cold gas from the outskirts of the galaxy and/or minor merger/interaction may have produced the almost flat abundance gradient and the cometary morphology in Tol 65 .