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We present the 3 mm wavelength spectra of 28 local galaxy merger remnantsobtained with the Large Millimeter Telescope. Fifteen molecular lines from 13different molecular species and isotopologues were identified, and 21 out of 28sources were detected in one or more molecular lines. On average, the lineratios of the dense gas tracers, such as HCN (1-0) and HCO$^{+}$(1-0), to$^{13}$CO (1-0) are 3-4 times higher in ultra/luminous infrared galaxies(U/LIRGs) than in non-LIRGs in our sample. These high line ratios could beexplained by the deficiency of $^{13}$CO and high dense gas fractions suggestedby high HCN (1-0)/$^{12}$CO (1-0) ratios. We calculate the IR-to-HCN (1-0)luminosity ratio as a proxy of the dense gas star formation efficiency. Thereis no correlation between the IR/HCN ratio and the IR luminosity, while theIR/HCN ratio varies from source to source (1.1-6.5) $\times 10^{3}$$L_{\odot}$/(K km s$^{-1}$ pc$^{2}$). Compared with the control sample, we findthat the average IR/HCN ratio of the merger remnants is higher by a factor of2-3 than those of the early/mid-stage mergers and non-merging LIRGs, and it iscomparable to that of the late-stage mergers. The IR-to-$^{12}$CO (1-0) ratiosshow a similar trend to the IR/HCN ratios. These results suggest that starformation efficiency is enhanced by the merging process and maintained at highlevels even after the final coalescence. The dynamical interactions and mergerscould change the star formation mode and continue to impact the star formationproperties of the gas in the post-merger phase.

Cold Molecular Gas in Merger Remnants. II. The properties of dense molecular gas