Journal article

K-CLASH: Strangulation and ram pressure stripping in galaxy cluster members at 0.3 < z < 0.6

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

Monthly Notices of the Royal Astronomical Society | Royal Astronomical Society | Published : 2020


Galaxy clusters have long been theorized to quench the star formation of their members. This study uses integral-field unit observations from the K-band MultiObject Spectrograph (KMOS) – Cluster Lensing And Supernova survey with Hubble (CLASH) survey (K-CLASH) to search for evidence of quenching in massive galaxy clusters at redshifts 0.3 < z < 0.6. We first construct mass-matched samples of exclusively star-forming cluster and field galaxies, then investigate the spatial extent of their H α emission and study their interstellar medium conditions using emission line ratios. The average ratio of H α half-light radius to optical half-light radius (⁠re,Hα/re,Rcre,Hα/re,Rc⁠) for all galaxies is ..

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University of Melbourne Researchers


Awarded by ESO programme(s)

Awarded by Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)

Awarded by UK Science and Technology Facilities Council (STFC)

Awarded by STFC

Awarded by ERC advanced Grant DUSTYGAL

Awarded by consolidated grants 'Astrophysics at Oxford' from the STFC

Funding Acknowledgements

This work was based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO programme(s) 097.A-0397, 098.A-0224, 099.A0207, and 0100.A-0296. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. SPV acknowledges support from a doctoral studentship from the UK Science and Technology Facilities Council (STFC) grant ST/N504233/1. ALT acknowledges support from a Forrest Research Foundation Fellowship, STFC (ST/L00075X/1 and ST/P000541/1), the ERC advanced Grant DUSTYGAL (321334), and an STFC Studentship. RLD acknowledges travel and computer grants from Christ Church, Oxford, and support from the Oxford Hintze Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. MB was supported by the consolidated grants 'Astrophysics at Oxford' ST/H002456/1 and ST/K00106X/1 from the STFC.