MUSE spectroscopy and deep observations of a unique compact JWST target, lensing cluster CLIO
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We present the results of a VLT MUSE/FORS2 and Spitzer survey of a unique compact lensing cluster CLIO at z = 0.42, discovered through the GAMA survey using spectroscopic redshifts. Compact and massive clusters such as this are understudied, but provide a unique prospective on dark matter distributions and for finding background lensed high-z galaxies. The CLIO cluster was identified for follow-up observations due to its almost unique combination of high-mass and dark matter halo concentration, as well as having observed lensing arcs from ground-based images. Using dual band optical and infra-red imaging from FORS2 and Spitzer, in combination with MUSE optical spectroscopy we identify 89 cluster members and find background sources out to z = 6.49. We describe the physical state of this cluster, finding a strong correlation between environment and galaxy spectral type. Under the assumption of an NFW profile, we measure the total mass of CLIO to be M200 = (4.49 ± 0.25) × 1014 M⊙. We build and present an initial strong-lensing model for this cluster, and measure a relatively low intracluster light (ICL) fraction of 7.21 ± 1.53 per cent through galaxy profile fitting. Due to its strong potential for lensing background galaxies and its low ICL, the CLIO cluster will be a target for our 110 h James Webb Space Telescope ‘Webb Medium-Deep Field’ (WMDF) GTO program.
Griffiths , A , Conselice , C J , Alpaslan , M , Frye , B L , Diego , J M , Zitrin , A , Yan , H , Ma , Z , Barone-Nugent , R , Bhatawdekar , R , Driver , S P , Robotham , A S G , Windhorst , R A & Wyithe , J S B 2018 , ' MUSE spectroscopy and deep observations of a unique compact JWST target, lensing cluster CLIO ' , Monthly Notices of the Royal Astronomical Society , vol. 475 , no. 3 , pp. 2853-2869 . https://doi.org/10.1093/mnras/stx3364
Monthly Notices of the Royal Astronomical Society
© 2018, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stx3364
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