Size Evolution of the Most Massive Galaxies at 1.7 &lt;
                    <i>z</i>
                    &lt; 3 from GOODS NICMOS Survey Imaging

Buitrago, F.; Trujillo, Ignacio; Conselice, Christopher J.; Bouwens, Rychard; Dickinson, Mark; Yan, Haojing

doi:10.1086/592836

Cited by 435 publications

(537 citation statements)

References 45 publications

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“…In addition, they can be very compact but massive. In some cases, at redshift ∼2 they are a factor of up to 6 times smaller in size than galaxies of the same mass today (Daddi et al 2005;Trujillo et al 2007;Buitrago et al 2008;van Dokkum et al 2008;van Dokkum et al 2010;Weinzirl et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Lange

Moffett

Driver

et al. 2016

Mon. Not. R. Astron. Soc.

120

131

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Section: Introductionmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Lange

Moffett

Driver

et al. 2016

Mon. Not. R. Astron. Soc.

120

131

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“…Trujillo et al 2006b;Longhetti et al 2007;Cimatti et al 2008;van der Wel et al 2008;Saglia et al 2010;Beifiori et al 2014), and a factor of ∼ 4 since z ∼ 2 (e.g. Trujillo et al 2007;Buitrago et al 2008;van Dokkum et al 2008;Newman et al 2012;Szomoru, Franx & van Dokkum 2012;Barro et al 2013;van der Wel et al 2014). This progressive growth appears to happen mainly at the outer envelopes, as several works have shown that massive (M * 1 × 10 11 M ) passive galaxies at high-redshift have comparable central densities to local ellipticals, suggesting the mass assemble took place mainly at outer radii over cosmic time (i.e.…”

Section: Introductionmentioning

confidence: 99%

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

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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(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). pp. 3181-3209. Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe 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 nearinfrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i 775 , z 850 ,Y 105 , J 125 , H 160 ), and find that the size decreases by ∼ 20% going from i 775 to H 160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M * /L H 160 and (z 850 − H 160 ) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼ 41% smaller than their restframe r-band counterparts compared with an average of ∼ 12% at z ∼ 0. We attribute this evolution to the evolution in the M * /L H 160 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 = d log(age)/d log(a) ∼ −0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇ Z = d log(Z)/d log(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.

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“…In addition, they ruled out any substantial evolution in the stellar mass-size relation for the same early-type galaxies, consistent with the passive evolution scenario. However, the evolution in the stellar mass-size relation has recently been stablished at higher redshifts (Trujillo et al 2007;Buitrago et al 2008) and the combination of Palomar massive galaxies sample and lower stellar masses galaxies from the GEMS survey conducted by Trujillo et al (2007) has shown a perceptible evolution in the stellar mass-size relation of early-type galaxies since z ∼ 0.65.…”

Section: Discussionmentioning

confidence: 99%

Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

Lorenzo

Cepa

Bongiovanni

et al. 2010

A&A

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Context. The fundamental plane links the structural properties of early-type galaxies such as its surface brightness and effective radius with its dynamics. The study of the fundamental plane evolution therefore has important implications for models of galaxy formation and evolution. Aims. This work aims to identify signs of evolution of early-type galaxies through the study of parameter correlations such as the fundamental plane, the Kormendy, and the Faber-Jackson relations, using a sample of 135 field galaxies extracted from the Extended Groth Strip in the redshift range 0.2 < z < 1.2. Methods. We calculate the internal velocity dispersions with DEEP2 data by extracting the stellar kinematics from absorption line spectra, using a maximum penalized-likelihood approach. Morphology was determined through visual classification of the V + I images of ACS. The structural parameters of these galaxies were obtained by fitting de Vaucouleurs stellar profiles to the ACS I-band images with the GALFIT code. To check the effect on the fundamental plane of the structural parameters, Sérsic and bulge-to-disc decomposition models were fitted to our sample of galaxies. A good agreement was found in the fundamental plane derived from the three models. Results. Assuming that effective radii and velocity dispersions do not evolve with redshift, we found a brightening of 0.68 mag in the B-band and 0.52 mag in the g-band at z = 0.7. However, the scatter in the fundamental plane for our high-redshift sample is reduced by half when we allow the fundamental plane slope to evolve, suggesting a different evolution of early-type galaxies according to their intrinsic properties such as total mass, size, or luminosity. The study of the Kormendy relation shows a population of very compact (R e < 2 Kpc) and bright galaxies (−21.5 > M g > −22.5), of which there are only a small fraction (0.4%) at z = 0. Studying the luminosity-size and stellar mass-size relations, we show that the evolution of these compact objects is mainly caused by an increase in size that could be explained by the action of dry minor mergers. We also detect an evolution in the fundamental plane caused mainly by this population of very compact and bright galaxies. Unfortunately, we cannot distinguish a change in the slope from an increase in the scatter of the fundamental plane because our high-redshift sample is biased to the brightest objects.

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Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging

Cited by 435 publications

References 45 publications

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

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

Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

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