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We investigate the connection between star formation and molecular gasproperties in galaxy mergers at low redshift (z$\leq$0.06). The study wepresent is based on IRAM 30-m CO(1-0) observations of 11 galaxies with a closecompanion selected from the Sloan Digital Sky Survey (SDSS). The pairs havemass ratios $\leq$4, projected separations r$_{\mathrm{p}} \leq$30 kpc andvelocity separations $\Delta$V$\leq$300 km s$^{-1}$, and have been selected toexhibit enhanced specific star formation rates (sSFR). We calculate moleculargas (H$_{2}$) masses, assigning to each galaxy a physically motivatedconversion factor $\alpha_{\mathrm{CO}}$, and we derive molecular gas fractionsand depletion times. We compare these quantities with those of isolatedgalaxies from the extended CO Legacy Data base for the GALEX Arecibo SDSSSurvey sample (xCOLDGASS, Saintonge et al. 2017) with gas quantities computedin an identical way. Ours is the first study which directly compares the gasproperties of galaxy pairs and those of a control sample of normal galaxieswith rigorous control procedures and for which SFR and H$_{2}$ masses have beenestimated using the same method. We find that the galaxy pairs have shorterdepletion times and an average molecular gas fraction enhancement of 0.4 dexcompared to the mass matched control sample drawn from xCOLDGASS. However, thegas masses (and fractions) in galaxy pairs and their depletion times areconsistent with those of non-mergers whose SFRs are similarly elevated. Weconclude that both external interactions and internal processes may lead tomolecular gas enhancement and decreased depletion times.

Galaxy pairs in the SDSS - XIII. The connection between enhanced star formation and molecular gas properties in galaxy mergers