Detecting clusters and groups of galaxies populating the local Universe in large optical spectroscopic surveys

Abstract

Wide-field cosmological surveys provide hundreds of thousands of spectroscopically confirmed galaxy groups and clusters, valuable for tracing baryonic matter distribution. However, controlling systematics in identifying host dark matter halos and estimating their properties is crucial. We evaluate three group detection methods on a simulated dataset replicating the GAMA selection to understand systematics and selection effects. This is key for interpreting data from SDSS, GAMA, DESI, WAVES, and leveraging optical catalogues in the (X-ray) eROSITA era to quantify baryonic mass in galaxy groups. Using a lightcone from the Magneticum hydrodynamical simulation, we simulate a spectroscopic galaxy survey in the local Universe (down to $z<0.2$ and stellar mass completeness $M_{\star }\ge 10^{9.8}{M}_{\odot }$). We assess completeness and contamination of reconstructed halo catalogues, evaluate membership accuracy, and analyse the halo mass recovery rate of group finders. All three group finders achieve high completeness ($>80\%$) at group and cluster scales, confirming optical selection's suitability for dense regions. Contamination at low masses ($M_{200}<10^{13}{M}_{\odot }$) arises from interlopers and fragmentation. Membership is at least 70\% accurate above the group mass scale, but inaccuracies bias halo mass estimates using galaxy velocity dispersion. Alternative proxies, like total stellar luminosity or mass, yield more accurate halo masses. The cumulative luminosity function of galaxy members matches predictions, showing the group finders' accuracy in identifying galaxy populations. These results confirm the reliability and completeness of spectroscopic catalogues produced by state-of-the-art group finders. This supports studies requiring large spectroscopic samples of galaxy groups and clusters, as well as investigations into galaxy evolution across diverse environments.

submitted to A&A, 17 pages, 9 figures. Abstract reduced for ArXiv submission

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• The hot gas mass fraction in halos. From Milky Way-like groups to massive clusters
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• The eROSITA view on the halo mass-temperature relation: From low-mass groups to massive clusters
• Modelling the selection of galaxy groups with end to end simulations
• On the baryon budget in the X-ray-emitting circumgalactic medium of Milky Way-mass galaxies
• Dwarf Galaxy Number Counts within 25 Mpc: Predictions from Local Group Analogues in TNG50
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• Bound or blown: the fate of hot gas in galaxy groups