Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z=1.39

被引:46
作者
Chan, Jeffrey C. C. [1 ,2 ]
Beifiori, Alessandra [1 ,2 ]
Mendel, J. Trevor [1 ]
Saglia, Roberto P. [1 ,2 ]
Bender, Ralf [1 ,2 ]
Fossati, Matteo [1 ,2 ]
Galametz, Audrey [1 ]
Wegner, Michael [2 ]
Wilman, David J. [1 ,2 ]
Cappellari, Michele [3 ]
Davies, Roger L. [3 ]
Houghton, Ryan C. W. [3 ]
Prichard, Laura J. [3 ]
Lewis, Ian J. [3 ]
Sharples, Ray [4 ]
Stott, John P. [3 ]
机构
[1] Max Planck Inst Extraterr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany
[2] Univ Munich, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany
[3] Univ Oxford, Dept Phys, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England
[4] Univ Durham, Dept Phys, Ctr Adv Instrumentat, South Rd, Durham DH1 3LE, England
基金
英国科学技术设施理事会;
关键词
Galaxy: evolution; galaxies: clusters: general; galaxies: elliptical and lenticular; cD; galaxies: formation; galaxies: fundamental parameters; galaxies: high-redshift; SIMILAR-TO; 2; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; INSIDE-OUT GROWTH; ULTRA-DEEP-FIELD; PASSIVELY EVOLVING GALAXIES; LESS-THAN; ELLIPTIC GALAXIES; QUIESCENT GALAXIES;
D O I
10.1093/mnras/stw502
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 (HST) imaging. We derive light-weighted Sersic fits in five HST bands (i(775), z(850), Y-105, J(125), H-160), and find that the size decreases by similar to 20 per cent going from i(775) to H-160 band, consistent with recent studies. We then generate spatially resolved stellarmassmaps using an empirical relationship between M-*/L-H160 and (z(850) - H-160) and use these to derive mass-weighted Sersic fits: the mass-weighted sizes are similar to 41 per cent smaller than their rest-frame r-band counterparts compared with an average of similar to 12 per cent at z similar to 0. We attribute this evolution to the evolution in the M-*/L-H160 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 (del(z -H)) are mostly negative, with a median value of similar to 0.45 mag dex(-1), twice the local value. The evolution is caused by an evolution in age gradients along the semimajor axis (a), with del(age) = dlog (age)/dlog (a) similar to-0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with del(Z) = dlog (Z)/dlog (a) similar to-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.
引用
收藏
页码:3181 / 3209
页数:29
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