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We investigate the three-point correlation function (3PCF) in the squeezedlimit by considering galaxy pairs as discrete objects and cross-correlatingthem with the galaxy field. We develop an efficient algorithm using FastFourier Transforms to compute such cross-correlations and their associatedpair-galaxy bias bpg and the squeezed 3PCF coefficient Qeff. We implement ourmethod using N-body cosmological simulations and a fiducial Halo OccupationDistribution (HOD) and present the results in both the real space and redshiftspace. In real space, we observe a peak in bpg and Qeff at pair separation of ~2 Mpc, attributed to the fact that galaxy pairs at 2 Mpc separation trace themost massive dark matter halos. We also see strong anisotropy in the bpg andQeff signals that track the large-scale filamentary structure. In redshiftspace, both the 2 Mpc peak and the anisotropy are significantly smeared outalong the line-of-sight due to Finger-of-God effect. In both the real space andredshift space, the squeezed 3PCF shows a factor of 2 variation, contradictingthe hierarchical ansatz but offering rich information on the galaxy-haloconnection. Thus, we explore the possibility of using the squeezed 3PCF toconstrain the HOD. When we compare two simple HOD models that are closelymatched in their projected two-point correlation function (2PCF), we do not yetsee a strong variation in the 3PCF that is clearly disentangled from variationsin the projected 2PCF. Nevertheless, we propose that more complicated HODmodels, e.g. those incorporating assembly bias, can break degeneracies in the2PCF and show a distinguishable squeezed 3PCF signal.

Using galaxy pairs to investigate the three-point correlation function in the squeezed limit