Speaker
Description
Understanding the scaling relations between galaxy cluster properties (such as mass, luminosity, richness, and luminosity) is crucial for unraveling the physical processes shaping them. However, these relations are highly sensitive to uncertainties in sample selection functions, requiring assumptions about the abundance and properties of unobserved populations. The potential impact of selection effects is substantial, as clusters selected via different methods appear to follow distinct scaling relations.
In this talk, I present the Compton Y vs. mass scaling relation derived from a statistical sample of galaxy clusters selected solely by gravity (shear), contrasting it with the scaling relations obtained from ICM-selected cluster samples. Even after accounting for selection effects and a mass bias that we found to be (1-b) = 0.72+-0.09,, analyses based on ICM-selected samples show significant discrepancies: an excessively large intercept, unusually low scatter, and a conspicuous absence of clusters that are exceptionally faint in Compton Y for their mass.
Finally, I outline potential paths forward for observing larger cluster samples with SZ facilities, leveraging ongoing surveys such as Euclid and LSST.
| Would you be interested in presenting a poster if the conference is oversubcribed? | Yes |
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