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Chemical abundances for 15 elements (C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V,Cr, Mn, Fe, and Ni) are presented for 83 stellar members of the 4 Gyr oldsolar-metallicity open cluster M67. The sample contains stars spanning a widerange of evolutionary phases, from G dwarfs to red clump stars. The abundanceswere derived from near-IR ($\lambda$1.5 -- 1.7$\mu$m) high-resolution spectra($R$ = 22,500) from the SDSS-IV/APOGEE survey. A 1-D LTE abundance analysis wascarried out using the APOGEE synthetic spectral libraries, via chi-squareminimization of the synthetic and observed spectra with the qASPCAP code. Wefound significant abundance differences ($\sim$0.05 -- 0.30 dex) between theM67 member stars as a function of the stellar mass (or position on the HRdiagram), where the abundance patterns exhibit a general depletion (in [X/H])in stars at the main-sequence turnoff. The amount of the depletion is differentfor different elements. We find that atomic diffusion models provide, ingeneral, good agreement with the abundance trends for most chemical species,supporting recent studies indicating that measurable atomic diffusion operatesin M67 stars.

Chemical Abundances of Main-Sequence, Turnoff, Subgiant and red giant Stars from APOGEE spectra II: Atomic Diffusion in M67 Stars