The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

Zahid, H. Jabran; Geller, Margaret J.; Damjanov, Ivana; Sohn, Jubee

doi:10.3847/1538-4357/ab21b9

Cited by 15 publications

(15 citation statements)

References 174 publications

(256 reference statements)

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“…they need to add mass in the outskirts. In addition, the pivot mass in the size-mass relation for quiescent galaxies decreases from log(M * /M ) ≈ 10.8 at z ∼ 2 to log(M * /M ) ≈ 10.2 at z ∼ 0 (see Figure 11, similar to star-forming galaxies), which is similar to the mass where the fraction of star-forming galaxies is 50%, indicating that the pivot mass reflects a transition from in-situ, dissipational to ex-situ, dissipationaless growth (see also Zahid et al 2019). This is also consistent with the decline in the scatter of sizes toward high stellar masses (see Section 5.4).…”

Section: Interpretation Of the Size Evolution Of Quiescent Galaxiesmentioning

confidence: 81%

Galaxy Sizes Since $z=2$ from the Perspective of Stellar Mass Distribution within Galaxies

Mosleh,

Hosseinnejad,

Hosseini-ShahiSavandi

et al. 2020

Preprint

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How stellar mass assembles within galaxies is still an open question. We present measurements of the stellar mass distribution on kpc-scale for ∼ 5500 galaxies with stellar masses above log(M * /M ) 9.8 up to the redshift 2.0. We create stellar mass maps from Hubble Space Telescope observations by means of the pixel-by-pixel SED fitting method. These maps are used to derive radii encompassing 20%, 50%, and 80% (r 20 , r 50 and r 80 ) of the total stellar mass from the best-fit Sérsic models. The reliability and limitations of the structural parameter measurements are checked extensively using a large sample (∼ 3000) of simulated galaxies. The size-mass relations and redshift evolution of r 20 , r 50 and r 80 are explored for star-forming and quiescent galaxies. At fixed mass, the star-forming galaxies do not show significant changes in their r 20 , r 50 and r 80 sizes, indicating self-similar growth. Only above the pivot stellar mass of log(M * /M ) 10.5, r 80 evolves as r 80 ∝ (1 + z) −0.85±0.20 , indicating that mass builds up in the outskirts of these systems (inside-out growth). The Sérsic values also increase for the massive star-forming galaxies towards late cosmic time. Massive quiescent galaxies show stronger size evolution at all radii, in particular the r 20 sizes. For these massive galaxies, Sérsic values remain almost constant since at least z ∼ 1.3, indicating that the strong size evolution is related to the changes in the outer parts of these galaxies. We make all the structural parameters publicly available.

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Section: Interpretation Of the Size Evolution Of Quiescent Galaxiesmentioning

confidence: 81%

Galaxy Sizes Since $z=2$ from the Perspective of Stellar Mass Distribution within Galaxies

Mosleh,

Hosseinnejad,

Hosseini-ShahiSavandi

et al. 2020

Preprint

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“…Bernardi 2009;Ascaso et al 2011;Bai et al 2014;Furnell et al 2018) and massive galaxies in general (e.g. Hopkins et al 2009Hopkins et al , 2010Wuyts et al 2010;Sonnenfeld et al 2013;Zahid et al 2019), including the relative contribution of stars from dry mergers versus in-situ star formation and the importance of feedback processes.…”

Section: Bcg Stellar Mass Profilesmentioning

confidence: 99%

The baryon content of groups and clusters of galaxies in the FABLE simulations

Henden,

Puchwein,

Sijacki

2019

Preprint

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We study the gas and stellar mass content of galaxy groups and clusters in the fable suite of cosmological hydrodynamical simulations, including the evolution of their central brightest cluster galaxies (BCGs), satellite galaxies and intracluster light (ICL). The total gas and stellar mass of fable clusters are in very good agreement with observations and show negligible redshift evolution at fixed halo mass for M 500 3×10 14 M at z 1, in line with recent findings from Sunyaev-Zel'dovich (SZ)-selected cluster samples. Importantly, the simulations predict significant redshift evolution in these quantities in the low mass (M 500 ∼ 10 14 M ) regime, which will be testable with upcoming SZ surveys such as SPT-3G. While the stellar masses of fable BCGs are in reasonable agreement with observations, the total stellar mass in satellite galaxies is lower than observed and the total mass in ICL is somewhat higher. This may be caused by enhanced tidal stripping of satellite galaxies due to their large sizes. BCGs are characterised by moderate stellar mass growth at z < 1 coincident with a late-time development of the ICL. The level of BCG mass growth is in good agreement with recent observations, however, we caution that the inferred growth depends sensitively on the mass definition. We further show that in-situ star formation contributes more than half the mass of a BCG over its lifetime, the bulk of which is gained at z > 1 where star formation rates are highest. The stellar mass profiles of the BCG+ICL component are similar to observed profiles out to ∼ 100 kpc at z ≈ 0 and follow a close to power law shape out to several hundred kpc. We further demonstrate that the inferred size growth of BCGs can be severely biased by the choice of parametric model and the outer radius of the fit.

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“…The figure also reveals that the BHAR/SGR relation at z = 1 −4 has a steeper slope ( ∼1.40 ± 0.25) than the BHAR/SFR relation. This finding implies that the SFR increases more strongly with increasing stellar mass than the SGR, while the opposite behaviour would have been expected based on the increased galaxy merging activity in massive galaxies (Ferreras et al 2014(Ferreras et al , 2016Zahid et al 2019 ). Ho we ver, the SGR dif fers from the SFR not only by the additional merger contribution but also by the decrease in stellar mass of stars already present at time t − t avg , i.e.…”

Section: Sfr Versus Bhar and Inferred Luminositiesmentioning

confidence: 91%

Black hole–galaxy scaling relations in FIRE: the importance of black hole location and mergers

Çatmabacak

Feldmann

Anglés-Alcázar

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The concurrent growth of supermassive black holes (SMBHs) and their host galaxies remains to be fully explored, especially at high redshift. While often understood as a consequence of self-regulation via AGN feedback, it can also be explained by alternative SMBH accretion models. Here, we expand on previous work by studying the growth of SMBHs with the help of a large suite of cosmological zoom-in simulations (MassiveFIRE) that are part of the Feedback in Realistic Environments (FIRE) project. The growth of SMBHs is modelled in post-processing with different black hole accretion models, placements, and merger treatments, and validated by comparing to on-the-fly calculations. Scaling relations predicted by the gravitational torque driven accretion (GTDA) model agree with observations at low redshift without the need for AGN feedback, in contrast to models in which the accretion rate depends strongly on SMBH mass. At high redshift, we find deviations from the local scaling relations in line with previous theoretical results. In particular, SMBHs are under-massive, presumably due to stellar feedback, but start to grow efficiently once their host galaxies reach M* ∼ 1010M⊙. We analyse and explain these findings in the context of a simple analytic model. Finally, we show that the predicted scaling relations depend sensitively on the SMBH location and the efficiency of SMBH merging, particularly in low-mass systems. These findings highlight the relevance of understanding the evolution of SMBH-galaxy scaling relations to predict the rate of gravitational wave signals from SMBH mergers across cosmic history.

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The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

Cited by 15 publications

References 174 publications

Galaxy Sizes Since $z=2$ from the Perspective of Stellar Mass Distribution within Galaxies

Galaxy Sizes Since $z=2$ from the Perspective of Stellar Mass Distribution within Galaxies

The baryon content of groups and clusters of galaxies in the FABLE simulations

Black hole–galaxy scaling relations in FIRE: the importance of black hole location and mergers

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