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Sizes, Colour gradients and Resolved Stellar Mass Distributions for the Massive Cluster Galaxies in XMMUJ2235-2557 at z = 1.39

Chan, J.C.C.; Beifiori, A.; Mendel, J.T.; Saglia, R.P.; Bender, R.; Fossati, M.; Galametz, A.; Wegner, M.; Wilman, D.J.; Cappellari, M.; Davies, R.L.; Houghton, R.C.W.; Prichard, L.J.; Lewis, I.J.; Sharples, R.; Stott, J.P.

Sizes, Colour gradients and Resolved Stellar Mass Distributions for the Massive Cluster Galaxies in XMMUJ2235-2557 at z = 1.39 Thumbnail


Authors

J.C.C. Chan

A. Beifiori

J.T. Mendel

R.P. Saglia

R. Bender

M. Fossati

A. Galametz

M. Wegner

D.J. Wilman

M. Cappellari

R.L. Davies

R.C.W. Houghton

L.J. Prichard

I.J. Lewis

J.P. Stott



Abstract

We analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and near-infrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i775, z850, Y105, J125, H160), and find that the size decreases by ∼20% going from i775 to H160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M∗/LH160M∗/LH160 and (z850 − H160) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼41% smaller than their rest-frame r-band counterparts compared with an average of ∼12% at z ∼ 0. We attribute this evolution to the evolution in the M∗/LH160M∗/LH160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M★/L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇z − H) are mostly negative, with a median value of ∼0.45 mag dex−1, twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇age = dlog (age)/dlog (a) ∼−0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇Z = dlog (Z)/dlog (a) ∼−0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.

Citation

Chan, J., Beifiori, A., Mendel, J., Saglia, R., Bender, R., Fossati, M., …Stott, J. (2016). Sizes, Colour gradients and Resolved Stellar Mass Distributions for the Massive Cluster Galaxies in XMMUJ2235-2557 at z = 1.39. Monthly Notices of the Royal Astronomical Society, 458(3), 3181-3209. https://doi.org/10.1093/mnras/stw502

Journal Article Type Article
Acceptance Date Feb 29, 2016
Online Publication Date Mar 7, 2016
Publication Date May 21, 2016
Deposit Date Mar 29, 2016
Publicly Available Date Mar 29, 2016
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 458
Issue 3
Pages 3181-3209
DOI https://doi.org/10.1093/mnras/stw502
Public URL https://durham-repository.worktribe.com/output/1388195
Related Public URLs http://arxiv.org/pdf/1603.00468v1.pdf

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Copyright Statement
Advance online version This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.






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