A Non-parametric Method for the Inference of Halo Occupation Distributions

TL;DR

This paper introduces a non-parametric method using an emulator to infer galaxy-halo relationships from the galaxy two-point correlation function, allowing more flexible modeling and improved accuracy over traditional parametric approaches.

Contribution

The authors develop a non-parametric HOD inference framework that leverages emulators trained on simulations, enabling more flexible and precise galaxy-halo connection modeling.

Findings

Successfully recovers HODs within 0.2 dex accuracy.

Achieves comparable or better precision than parametric models.

Framework accelerates likelihood evaluations for observational data.

Abstract

The galaxy-halo connection traces processes by which galaxies form and evolve. The halo occupation distribution (HOD) describes the relationship between galaxies and their host dark matter haloes. Measurements of the galaxy two-point correlation function (2PCF) allow us to extract information about the HODs of observed galaxy samples. Several parametric HOD models have been proposed in the literature, but the choice of parameterization restricts the space of possible HODs. To resolve this issue, we introduce a non-parametric HOD fitting method in which we train an emulator to learn the mappings among the galaxy 2PCF, physical properties used to select galaxy samples, and the HOD, all obtained from simulated past lightcones constructed with the Santa Cruz semi-analytic models. Implementing this emulator within a likelihood analysis framework, we derive constraints on the HOD of a galaxy sample when provided with a measurement of its 2PCF. Using the emulator to accelerate likelihood evaluations, we test the non-parametric HOD approach on a set of 2PCFs for mock galaxy samples drawn from the TNG100-1 simulation and selected above threshold values of stellar mass and star formation rate. Our framework is able to recover TNG100-1 HODs within 0.2 dex. We use the TNG100-1 mocks to tune the reported uncertainties to estimate those expected in the analysis of observations. Comparing to parametric HOD modeling routines applied to the same mock galaxy samples, our approach consistently infers the HOD with comparable or greater precision and accuracy.