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The three-point correlation function (3PCF) for galaxies provides anopportunity to measure the non-Gaussianity generated from nonlinear structureformation and also probes information about galaxy formation and evolution thatis generally not available from the two-point correlation function (2PCF). Wemeasure the 3PCF of the Sloan Digital Sky Survey DR7 main sample galaxies inboth redshift and projected spaces on scales up to 40Mpc/h. We explore thedependence of the 3PCF on galaxy stellar mass and color in order to constrainthe formation and evolution for galaxies of different properties. The study ofthe dependence on these properties also helps better constrain the relationbetween galaxy stellar mass and color and the properties of their hostingdark-matter halos. We focus on the study of the reduced 3PCF, Q, defined as theratio between the 3PCF and the sum of the products of the 2PCFs. We find a veryweak stellar mass dependence of Q in both redshift and projected spaces. Onsmall scales, more massive galaxies tend to have slightly higher amplitudes ofQ. The shape dependence of Q is also weak on these small scales, regardless ofstellar mass and color. The reduced 3PCF has a strong color dependence for thelow-mass galaxies, while no significant dependence on color is found for thehigh-mass galaxies. Low-mass red galaxies have higher amplitudes and strongershape dependence of the reduced 3PCF than the blue galaxies, implying thatthese low-mass red galaxies tend to populate filamentary structures. The lineargalaxy bias model fails to interpret the color dependence of Q, emphasizing theimportance of a nonvanishing quadratic bias parameter in the correct modelingof the galaxy color distribution.

Stellar Mass and color dependence of the three-point correlation function of galaxies in the local universe