Tutorial on models pre-built by Halotools

This section of the documentation reviews the pre-built composite models provided by Halotools. For a quick reference, instead see List of All Preloaded Models Grouped by Type.

All pre-built models can directly populate a simulation with a mock catalog and make observational predictions that can be compared to measurements made on a real galaxy sample. You need only choose the pre-built model and simulation snapshot that is appropriate for your science application. By following the links below, you can find a step-by-step tutorial for how to get going with any of the Halotools-provided pre-built models.

HOD-Style Models

HOD-style models make predictions for galaxy samples selected to be brighter or more massive than some threshold lower bound. The fundamental quantity in HOD-style models is \(P(N_{\rm gal} | M_{\rm halo})\), the probability that a halo of mass \(M_{\rm halo}\) contains \(N_{\rm gal}\) galaxies in some sample. All HOD models are based on host halos only; this distinguishes them from “subhalo-based models”: in HOD-style models there is no connection between subhalo and satellite abundance. All the models in this section are built by the PrebuiltHodModelFactory

Traditional HOD models

The following models are some the most widely used HODs in the literature. These are all designed to model either luminosity-threshold or stellar mass-threshold galaxy samples.

Traditional CLF models

The following model is described as a Conditional Luminosity Function model. However, the model works equally well to model the Conditional Stellar Mass Function.

Decorated HOD models

Decorated HOD models relax the assumption that halo mass is the only relevant halo property governing galaxy occupation statistics. This class of model naturally inherits all of the flexibility provided by the traditional HOD, while at the same time providing further flexibility to study the co-evolution of galaxies and their halos.

HOD models with color/SFR

While traditional HOD models have historically been applied to color-selected samples, such models do not contain any parameters controlling the dependence of color/SFR on halo properties. The HOD models in this section do contain such parametric freedom, making these models much more useful to constrain the physics of star formation and quenching.

Subhalo-based Models

Subhalo models presume a one-to-one correspondence between galaxies and (sub)halos. Central galaxies reside at the center of host halos, satellite galaxies at the center of subhalos. This assumption relaxes many of the “spherical cow” assumptions typical of HOD-style models, though this is at the expense of fine-grained control over the galaxy distribution. All the models in this section are built by the PrebuiltSubhaloModelFactory

Stellar-to-halo mass models (SMHM)

An SMHM model presumes that there is a one-to-one correspondence between stellar mass and subhalo mass. The SMHM relation is given by some parameterized form typically motivated by results based on abundance matching.

Abundance matching models

Abundance matching models do not parameterize the stellar-to-halo mass relation. In abundance matching, the SMHM relation is defined by the condition that the stellar mass function of the model must be exactly correct.