Towards a census of supercompact massive galaxies in the Kilo Degree Survey

Tortora, C.; Barbera, F. La; Napolitano, N. R.; Roy, N.; Radovich, M.; Cavuoti, S.; Brescia, M.; Longo, Giuseppe; Getman, F.; Capaccioli, M.; Grado, A.; Kuijken, Konrad; Jong, J. T. A. de; McFarland, John; Puddu, E.

doi:10.1093/mnras/stw184

Cited by 40 publications

(64 citation statements)

References 79 publications

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“…Recent investigations of quiescent samples at 0.2 < z < 0.8 link the local and z > 1 samples (Carollo et al 2013;Damjanov et al 2015a;Tortora et al 2016;Charbonnier et al 2017). These studies confirm that compact systems experience at most a moderate change in number density from z 1 to z ∼ 0.…”

Section: Introductionmentioning

confidence: 69%

Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Damjanov

Zahid

Geller

et al. 2019

ApJ

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We explore the relations between size, stellar mass and average stellar population age (indicated by D n 4000 indices) for a sample of ∼ 11000 intermediate-redshift galaxies from the SHELS spectroscopic survey (Geller et al. 2014) augmented by high-resolution Subaru Telescope Hyper Suprime-Cam imaging. In the redshift interval 0.1 < z < 0.6, star forming galaxies are on average larger than their quiescent counterparts. The mass-complete sample of ∼ 3500 M * > 10 10 M quiescent galaxies shows that the average size of a 10 11 M quiescent galaxy increases by 25% from z ∼ 0.6 to z ∼ 0.1. This growth rate is a function of stellar mass: the most massive (M * > 10 11 M ) galaxies grow significntly more slowly in size than an order of magnitude less massive quiescent systems that grow by 70% in the 0.1 z 0.3 redshift interval. For M * < 10 11 M galaxies age and size are anti-correlated at fixed mass; more massive quiescent systems show no significant trend in size with average stellar population age. The evolution in absolute and fractional abundances of quiescent systems at intermediate redshift are also a function of galaxy stellar mass. The suite of evolutionary trends suggests that galaxies more massive than ∼ 10 11 M have mostly assembled their mass by z ∼ 0.6. Quiescent galaxies with lower stellar masses show more complex evolution that is characterized by a combination of individual quiescent galaxy size growth (through mergers) and an increase in the size of newly quenched galaxies joining the population at later times (progenitor bias). The low-mass population (M * ∼ 10 10 M ) grows predominantly as a result of progenitor bias. For more massive (M * ∼ 5 × 10 10 M ) quiescent galaxies, (predominantly minor) mergers and progenitor bias make more comparable contributions to the size growth. At intermediate redshift quiescent size growth is mass-dependent; the most massive (M * > 10 11 M ) galaxies experience the least rapid increase in size from z ∼ 0.6 to z ∼ 0.1.

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Section: Introductionmentioning

confidence: 69%

Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Damjanov

Zahid

Geller

et al. 2019

ApJ

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“…The sample adopted in this analysis consists of galaxies extracted from 153 square degree of the KiDS survey (de Jong et al 2015) which have been already presented in Tortora et al (2016). Details about the data reduction and calibration can be found in de Jong et al (2015).…”

Section: Sample Selectionmentioning

confidence: 99%

Evolution of galaxy size–stellar mass relation from the Kilo-Degree Survey

Roy

Napolitano

Barbera

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We have obtained structural parameters of about 340, 000 galaxies from the Kilo Degree Survey (KiDS) in 153 square degrees of data release 1, 2 and 3. We have performed a seeing convolved 2D single Sérsic fit to the galaxy images in the 4 photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands.We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their Sérsic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, R e and stellar mass, M ⋆ , versus redshift, for both mass complete samples of spheroids and disc-dominated galaxies up to z∼ 0.6.Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids (Log M * /M ⊙ > 11, Chabrier IMF), while almost no evolution has found for less massive ones (Log M * /M ⊙ < 11). On the other hand, disc dominated systems show a milder evolution in the less massive systems (Log M * /M ⊙ < 11) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z ∼ 0.6, although in some cases the scatter of the data is large to drive final conclusions.These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route toward more accurate results, expected with the the next survey releases.

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“…Several observations highlighted the existence of a large population of compact or ultra-compact Q galaxies at high redshift. Their existence and number density at low redshift is still matter of debate, with some studies predicting an almost constant number density of compact galaxies as a function of redshift (Poggianti et al 2013), and others claiming that compact galaxies are very rare in the Local Universe (Tortora et al 2016). Several hypotheses on the fate of these galaxies have been proposed, including an increase of their sizes due mainly to mergers (in particular multiple minor mergers) or a re-ignition of star formation due to the accretion of new gaseous material.…”

Section: Compact Q Galaxiesmentioning

confidence: 99%

The evolution of sizes and specific angular momenta in hierarchical models of galaxy formation and evolution

Zoldan

Lucia

Xie

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We extend our previous work focused at z ∼ 0, studying the redshift evolution of galaxy dynamical properties using the state-of-the-art semi-analytic model GAEA: we show that the predicted size-mass relation for disky/star forming and quiescent galaxies is in good agreement with observational estimates, up to z ∼ 2. Bulge dominated galaxies have sizes that are offset low with respect to observational estimates, mainly due to our implementation of disk instability at high redshift. At large masses, both quiescent and bulge dominated galaxies have sizes smaller than observed. We interpret this as a consequence of our most massive galaxies having larger gas masses than observed, and therefore being more affected by dissipation. We argue that a proper treatment of quasar driven winds is needed to alleviate this problem. Our model compact galaxies have number densities in agreement with observational estimates and they form most of their stars in small and low angular momentum high-z halos. GAEA predicts that a significant fraction of compact galaxies forming at high-z is bound to merge with larger structures at lower redshifts: therefore they are not the progenitors of normalsize passive galaxies at z = 0. Our model also predicts a stellar-halo size relation that is in good agreement with observational estimates. The ratio between stellar size and halo size is proportional to the halo spin and does not depend on stellar mass but for the most massive galaxies, where AGN feedback leads to a significant decrease of the retention factor (from about 80 per cent to 20 per cent).

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Towards a census of supercompact massive galaxies in the Kilo Degree Survey

Cited by 40 publications

References 79 publications

Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Evolution of galaxy size–stellar mass relation from the Kilo-Degree Survey

The evolution of sizes and specific angular momenta in hierarchical models of galaxy formation and evolution

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