Literature Benchmarks

Observational reference data organised by tracer population. Three benchmark collections provide measured summary statistics that can be directly compared with pipeline outputs and theoretical predictions from semi-analytic models, hydrodynamic simulations, and halo-model calculations.

Benchmark	N papers	Description
Galaxy Benchmark	~100	Galaxy luminosity functions, stellar mass functions, projected and redshift-space two-point clustering, galaxy-galaxy lensing ΔΣ(R), and Stage-III cosmic shear. Surveys from 2dFGRS and SDSS to DESI DR1, HSC Y3, and Euclid.
AGN Benchmark	44	AGN clustering wp(rp) and P(k) multipoles, AGN host-halo weak lensing ΔΣ(R), and AGN luminosity functions in the X-ray, optical, and infrared bands. Surveys from XMM/Chandra pencil-beam fields to eROSITA, SDSS, eBOSS, DESI, and WISE.
Gas Benchmark	~30	Intracluster medium (ICM) scaling relations (YSZ–M, YX–M, TX–M, LX–M) and cross- correlations of galaxy positions with tSZ Compton-y, kSZ, and X-ray surface brightness maps. Surveys from Planck, ACT, SPT, XMM-REXCESS, and eROSITA.

• Galaxy Benchmark
• AGN Benchmark
• Gas Benchmark
• Survey Completeness

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Cross-benchmark connections

The three benchmarks are physically connected through the baryon cycle and the galaxy–halo–gas co-evolution:

• Galaxies ↔ AGN: AGN reside in the same group-scale haloes as luminous red galaxies (M_halo ~ 10^12.5–13M_☉). The AGN LF and the galaxy SMF share the same halo mass function, connected by the stellar-to-halo and SMBH-to-halo mass relations. See Galaxy Benchmark and AGN Benchmark.

• Galaxies ↔ Gas: The gas fraction, pressure profile, and entropy of the ICM are set by the same feedback processes that determine the bright end of the SMF and the clustering of massive galaxies. Galaxy × tSZ and galaxy × X-ray cross-correlations probe the gas content of the same haloes that host the galaxy clustering signal. See Galaxy Benchmark and Gas Benchmark.

• AGN ↔ Gas: AGN feedback heats and expels gas from haloes, lowering the gas fraction and pressure amplitude. The Y_SZ–M normalisation and its scatter encode the cumulative AGN energy injection. eROSITA simultaneously detects AGN and clusters, enabling direct AGN–gas cross-correlations. See AGN Benchmark and Gas Benchmark.