On the galaxy–halo connection in the EAGLE simulation

Desmond, Harry; Mao, Yao-Yuan; Crain, Robert A.; Schaye, Joop

doi:10.1093/mnrasl/slx093

Cited by 47 publications

(44 citation statements)

References 45 publications

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“…• The halo properties we explore -including spin and concentration -do not reduce the scatter in the GHSR in our sample of low-mass, dispersion supported galaxies in FIREbox. Our weak dependence on spin disagrees with classical theoretical ideas of galaxy formation (Mo et al 1998), but agrees with recent numerical works of more massive galaxies (Desmond et al 2017;Garrison-Kimmel et al 2018;Jiang et al 2019). At a fixed halo size, the weak correlation of galaxy sizes with halo spin and concentration agree with FIRE-2 zoom simulations (Garrison-Kimmel et al 2018) and semi-empirical models (Zanisi et al 2020(Zanisi et al , 2021a of more massive, rotationally supported galaxies.…”

Section: Discussionsupporting

confidence: 88%

“…Recent simulations provide a deeper understanding of, and challenge long-standing assumptions about, galaxy formation and evolution. Perhaps contrary to the expectation based on specific angular momentum conservation (Fall & Efstathiou 1980;Mo et al 1998), Desmond et al (2017) find in the EAGLE simulation that at a fixed stellar mass, the galaxy size weakly correlates with halo mass, concentration or spin. On top of that, Somerville et al (2018) conclude from their sample of Galaxy And Mass Assembly (GAMA) and the Cosmic Assembly Near Infrared Deep Extragalactic Legacy (CANDELS) surveys mapped to the Bolshoi-Planck dissipationless 𝑁−body simulation that the ratio of galaxy to halo size decreases slightly with cosmic time for less massive galaxies, while the ratio of galaxy size to halo size times halo spin -𝑅 1/2 /(𝑅 vir 𝜆) -is lower for more massive galaxies below 𝑧 3.…”

Section: Introductioncontrasting

confidence: 99%

“…Many theoretical and empirical works suggest that the halo spin and concentration are significant in setting the galaxy sizes, especially in rotationally supported disk galaxies (Fall & Efstathiou 1980;Mo et al 1998;Somerville et al 2008;Diemer & Kravtsov 2015;Desmond & Wechsler 2015;Desmond et al 2017;Somerville et al 2018). We study the halo spin lg 𝜆, lg 𝜆 𝑒 (top left panel of Figure 8) employing the definition of Bullock et al (2001):…”

Section: Halo Propertiesmentioning

confidence: 99%

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The galaxy-halo size relation of low-mass galaxies in FIRE

Rohr,

Feldmann,

Bullock

et al. 2021

Preprint

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Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (𝑀 ★ ∼ 10 7−9 M ) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size 𝑅 1/2 and the parent dark matter halo virial radius 𝑅 vir . This relation evolves only weakly since redshift 𝑧 = 5: 𝑅 1/2 [kpc] = (0.053 ± 0.002) (𝑅 vir /35 kpc) 0.934±0.054 , with a nearly constant scatter 𝜎 = 0.084 [dex]. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios 𝑣 rot /𝑣 circ ∼ 0.15. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate -including spin and concentrationsuggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.

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Section: Discussionsupporting

confidence: 88%

Section: Introductioncontrasting

confidence: 99%

Section: Halo Propertiesmentioning

confidence: 99%

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The galaxy-halo size relation of low-mass galaxies in FIRE

Rohr,

Feldmann,

Bullock

et al. 2021

Preprint

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“…Crain et al (2015) found that galaxy sizes can serve as important constraints on feedback models, Ferrero et al (2017) showed that realistic sizes and their evolution are crucial for reproducing the Tully-Fisher relation and its evolution, and Desmond et al (2016) found that galaxy sizes depend very weakly on halo properties, at a given stellar mass. Furlong et al (2017), separating active and quenched galaxies, found a good match between the sizes of EAGLE galaxies and observed ones.…”

Section: Introductionmentioning

confidence: 99%

The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation

Genel

Nelson

Pillepich

et al. 2017

Monthly Notices of the Royal Astronomical Society

298

240

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We analyze scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, starformation rate and redshift are reproduced, and a quantitative comparison of projected r-band sizes at 0 z 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M * ,z=0 10 9.5 M , the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M * ,z=0 10 9.5 M experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies with M * ,z=010 11 M , the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main-sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.

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“…Some works also highlighted a further correlation between the size of a galaxy, , and that of its host dark matter halo, ℎ (e.g. Fall 1983;Mo et al 1998;Kravtsov 2013;Huang et al 2017;Desmond 2017;Hearin et al 2019;Desmond et al 2018;Somerville et al 2018;Lapi et al 2018b;Mowla et al 2019;Zanisi et al 2020, but see also Desmond et al 2017 ). When coupled together in a semi-empirical model, the SMHM and − ℎ relations become powerful tools to simultaneously probe the mass and structural evolution of galaxies in a full cosmological context.…”

Section: Introductionmentioning

confidence: 99%

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

Zanisi

Shankar

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The mean size ( effective radius Re) of Massive Galaxies (MGs, Mstar > 1011.2M⊙) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g., mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass-halo mass (SMHM) relations with varying high-mass slopes and scatters σSMHM in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically-motivated, constant and linear relationship between Re and the host dark matter halo radius Rh. We find that: 1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; 2) the numbers of compact MGs grow steadily until z ≳ 2 and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; 3) a time-independent scatter σSMHM is consistent with a scenario in which compact starforming MGs transition into quiescent MGs in a few 108yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the starforming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution.

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On the galaxy–halo connection in the EAGLE simulation

Cited by 47 publications

References 45 publications

The galaxy-halo size relation of low-mass galaxies in FIRE

The galaxy-halo size relation of low-mass galaxies in FIRE

The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

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