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• W3100681167 endingPage "A140" @default.
• W3100681167 startingPage "A140" @default.
• W3100681167 abstract "We study the abundance of star-forming and quiescent galaxies in a sample of 21 clusters at 0.5 < z < 0.7, detected with the Planck satellite. Thanks to the large volume probed by Planck , these systems are extremely massive, and provide an excellent laboratory to study any environmental effects on their galaxies’ properties. We measure the cluster galaxy stellar mass function (SMF), which is a fundamental observable to study and constrain the formation and evolution of galaxies. Our measurements are based on homogeneous and deep multi-band photometry spanning from the u - to the K s -band for each cluster and are supported by spectroscopic data from different programs. The galaxy population is separated into quiescent and star-forming galaxies based on their rest-frame U−V and V−J colours. The SMF is compared to that of field galaxies at the same redshifts using data from the COSMOS/UltraVISTA survey. We find that the shape of the SMF of star-forming galaxies does not depend on environment, while the SMF of quiescent galaxies has a significantly steeper low-mass slope in the clusters compared to the field. This indicates that a different quenching mechanism is at play in clusters compared to the field, accentuated by a quenched fraction that is much higher in the clusters. We estimate the environmental quenching efficiency ( f EQ ), that is, the probability for a galaxy that would normally be star forming in the field to be quenched due to its environment. The f EQ shows no stellar-mass dependence in any environment, but it increases from 40% in the cluster outskirts to ∼90% in the cluster centres. The radial signature of f EQ provides constraints on where the dominant quenching mechanism operates in these clusters and on what timescale. Exploring these using a simple model based on galaxy orbits obtained from an N-body simulation, we find a clear degeneracy between both parameters. For example, the quenching process may either be triggered on a long (∼3 Gyr) timescale at large radii ( r ∼ 8 R 500 ), or happen well within 1 Gyr at r < R 500 . The radius where quenching is triggered is at least r quench > 0.67 R 500 (95%CL). The ICM density at this location (as probed with XMM-Newton ) suggests that ram-pressure stripping of the cold gas is a likely cause of quenching. In addition to this cluster-quenching mechanism, we find that 20–32%, depending on the cluster-specific quenching process, of accreted galaxies were already pre-processed (i.e. quenched by the surrounding overdensities) before they fell into the clusters." @default.
• W3100681167 created "2020-11-23" @default.
• W3100681167 creator A5041193928 @default.
• W3100681167 creator A5042246851 @default.
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• W3100681167 creator A5057229420 @default.
• W3100681167 creator A5061383813 @default.
• W3100681167 creator A5064506668 @default.
• W3100681167 creator A5065432320 @default.
• W3100681167 date "2018-10-01" @default.
• W3100681167 modified "2023-10-17" @default.
• W3100681167 title "The stellar mass function of galaxies in <i>Planck</i>-selected clusters at 0.5 < <i>z</i> < 0.7: new constraints on the timescale and location of satellite quenching" @default.
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