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We study the properties of 30 spectroscopically-identified pairs of galaxiesobserved during the peak epoch of star formation in the universe. These systemsare drawn from the MOSFIRE Deep Evolution Field (MOSDEF) Survey at $1.4 \leq z\leq 3.8$, and are interpreted as early-stage galaxy mergers. Galaxy pairs inour sample are identified as two objects whose spectra were collected on thesame Keck/MOSFIRE spectroscopic slit. Accordingly, all pairs in the sample haveprojected separations $R_{{\rm proj}}\leq 60$ kpc. The velocity separation forpairs was required to be $\Delta v \leq 500 \mbox{ km s}^{-1}$, which is astandard threshold for defining interacting galaxy pairs at low redshift.Stellar mass ratios in our sample range from 1.1 to 550, with 12 ratios closerthan or equal to 3:1, the common definition of a "major merger." Studies ofmerging pairs in the local universe indicate anenhancement in star-formationactivity and deficit in gas-phase oxygen abundance relative to isolatedgalaxies of the same mass. We compare the MOSDEF pairs sample to a controlsample of isolated galaxies at the same redshift, finding no measurable SFRenhancement or metallicity deficit at fixed stellar mass for the pairs sample.The lack of significant difference between the average properties of pairs andcontrol samples appears in contrast to results from low-redshift studies,although the small sample size and lower signal-to-noise of the high-redshiftdata limit definitive conclusions on redshift evolution. These results areconsistent with some theoretical works suggesting a reduced differential effectof pre-coalescence mergers on galaxy properties at high redshift --specifically that pre-coalescence mergers do not drive strong starbursts.

The MOSDEF Survey: No Significant Enhancement in Star Formation or Deficit in Metallicity in Merging Galaxy Pairs at 1.5<=z<=3.5