TY - JOUR

T1 - K-CLASH

T2 - Strangulation and ram pressure stripping in galaxy cluster members at 0.3 < z < 0.6

AU - Vaughan, Sam P.

AU - Tiley, Alfred L.

AU - Davies, Roger L.

AU - Prichard, Laura J.

AU - Croom, Scott M.

AU - Bureau, Martin

AU - Stott, John P.

AU - Bunker, Andrew

AU - Cappellari, Michele

AU - Ansarinejad, Behzad

AU - Jarvis, Matt J.

N1 - This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthyl Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version Sam P Vaughan, Alfred L Tiley, Roger L Davies, Laura J Prichard, Scott M Croom, Martin Bureau, John P Stott, Andrew Bunker, Michele Cappellari, Behzad Ansarinejad, Matt J Jarvis, K-CLASH: Strangulation and ram pressure stripping in galaxy cluster members at 0.3 < z < 0.6, Monthly Notices of the Royal Astronomical Society, Volume 496, Issue 3, August 2020, Pages 3841–3861, https://doi.org/10.1093/mnras/staa1837 is available online at: https://academic.oup.com/mnras/article-abstract/496/3/3841/5863222

PY - 2020/8/1

Y1 - 2020/8/1

N2 - Galaxy clusters have long been theorized to quench the star formation oftheir members. This study uses integral-field unit observations from theK-band MultiObject Spectrograph (KMOS) – Cluster Lensing AndSupernova survey with Hubble (CLASH) survey (K-CLASH) to search forevidence of quenching in massive galaxy clusters at redshifts 0.3 = 0.96 ± 0.09 compared to 1.22 ± 0.08 (smaller at a 98 percent credibility level). These values are uncorrected for the wavelengthdifference between H α emission and Rc-band stellarlight but implementing such a correction only reinforces our results. Wealso show that whilst the cluster and field samples followindistinguishable mass–metallicity (MZ) relations, the residualsaround the MZ relation of cluster members correlate with cluster-centricdistance; galaxies residing closer to the cluster centre tend to haveenhanced metallicities (significant at the 2.6σ level). Finally,in contrast to previous studies, we find no significant differences inelectron number density between the cluster and field galaxies. We usesimple chemical evolution models to conclude that the effects of discstrangulation and ram-pressure stripping can quantitatively explain ourobservations.

AB - Galaxy clusters have long been theorized to quench the star formation oftheir members. This study uses integral-field unit observations from theK-band MultiObject Spectrograph (KMOS) – Cluster Lensing AndSupernova survey with Hubble (CLASH) survey (K-CLASH) to search forevidence of quenching in massive galaxy clusters at redshifts 0.3 = 0.96 ± 0.09 compared to 1.22 ± 0.08 (smaller at a 98 percent credibility level). These values are uncorrected for the wavelengthdifference between H α emission and Rc-band stellarlight but implementing such a correction only reinforces our results. Wealso show that whilst the cluster and field samples followindistinguishable mass–metallicity (MZ) relations, the residualsaround the MZ relation of cluster members correlate with cluster-centricdistance; galaxies residing closer to the cluster centre tend to haveenhanced metallicities (significant at the 2.6σ level). Finally,in contrast to previous studies, we find no significant differences inelectron number density between the cluster and field galaxies. We usesimple chemical evolution models to conclude that the effects of discstrangulation and ram-pressure stripping can quantitatively explain ourobservations.

KW - galaxies: clusters: general

KW - galaxies: evolution

KW - galaxies: ISM

U2 - 10.1093/mnras/staa1837

DO - 10.1093/mnras/staa1837

M3 - Journal article

VL - 496

SP - 3841

EP - 3861

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -