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Galaxies selected on the basis of their emission line strength show lowmetallicities, regardless of their redshifts. We conclude this from a sample offaint galaxies at redshifts between 0.6 < z < 2.4, selected by their prominentemission lines in low-resolution grism spectra in the optical with the AdvancedCamera for Surveys (ACS) on the Hubble Space Telescope (HST) and in thenear-infrared using Wide-Field Camera 3 (WFC3). Using a sample of 11 emissionline galaxies (ELGs) at 0.6 < z < 2.4 with luminosities of -22 < M_B < -19,which have [OII], H\beta, and [OIII] line flux measurements from thecombination of two grism spectral surveys, we use the R23 method to derive thegas-phase oxygen abundances: 7.5 < 12+log(O/H) < 8.5. The galaxy stellar massesare derived using Bayesian based Markov Chain Monte Carlo (\piMC^2) fitting oftheir Spectral Energy Distribution (SED), and span the mass range 8.1 <log(M_*/M_\sun) < 10.1. These galaxies show a mass-metallicity (M-L) andLuminosity-Metallicity (L-Z) relation, which is offset by --0.6 dex inmetallicity at given absolute magnitude and stellar mass relative to the localSDSS galaxies, as well as continuum selected DEEP2 samples at similarredshifts. The emission-line selected galaxies most resemble the local "greenpeas" galaxies and Lyman-alpha galaxies at z~0.3 and z~2.3 in the M-Z and L-Zrelations and their morphologies. The G-M_{20} morphology analysis shows that10 out of 11 show disturbed morphology, even as the star-forming regions arecompact. These galaxies may be intrinsically metal poor, being at early stagesof formation, or the low metallicities may be due to gas infall and accretiondue to mergers.

Metallicities of Emission-Line Galaxies from HST ACS PEARS and HST WFC3 ERS Grism Spectroscopy at 0.6 < z < 2.4