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We investigate the stellar masses of the class of star-forming objects knownas Luminous Compact Blue Galaxies (LCBGs) by studying a sample of galaxies inthe distant cluster MS$~$0451.6-0305 at $z\approx0.54$ with ground-basedmulticolor imaging and spectroscopy. For a sample of 16spectroscopically-confirmed cluster LCBGs (colour $B-V < 0.5$, surfacebrightness $\mu_B < 21$ mag arcsec$^{-2}$, and magnitude $M_B < -18.5$), wemeasure stellar masses by fitting spectral energy distribution (SED) models tomultiband photometry, and compare with dynamical masses (determined fromvelocity dispersion between 10 $<$ $\sigma_v (\rm km~ s^{-1})$ $<$ 80), wepreviously obtained from their emission-line spectra. We compare two differentstellar population models that measure stellar mass in star-bursting galaxies,indicating correlations between the stellar age, extinction, and stellar massderived from the two different SED models. The stellar masses of cluster LCBGsare distributed similarly to those of field LCBGs, but the cluster LCBGs showlower dynamical-to-stellar mass ratios ($\rm M_{dyn}/M_{\ast} = 2.6$) thantheir field LCBG counterparts ($\rm M_{dyn}/M_{\ast}=4.8$), echoing trendsnoted previously in low-redshift dwarf elliptical galaxies. Within this limitedsample, the specific star formation rate declines steeply with increasing mass,suggesting that these cluster LCBGs have undergone vigorous star formation.

Star-forming Galaxies in Intermediate Redshift Clusters: Stellar vs. Dynamical Masses of Luminous Compact Blue Galaxies