Quiescent ultra-diffuse galaxies in the field originating from backsplash orbits

Benavides, José Antonio Chacón; Sales, Laura V.; Abadi, Mario G.; Pillepich, Annalisa; Nelson, Dylan; Marinacci, Federico; Cooper, Michael C.; Pakmor, Rüdiger; Torrey, Paul; Vogelsberger, Mark; Hernquist, Lars

doi:10.1038/s41550-021-01458-1

Cited by 49 publications

(44 citation statements)

References 58 publications

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“…The connection between halo spin and galaxy size is closely related to the idea that low surface brightness galaxies (LSBGs), as well as ultradiffuse galaxies (UDGs), might form at the centres of faster-spinning haloes (Amorisco & Loeb 2016;Pérez-Montaño & Cervantes Sodi 2019;Salinas & Galaz 2021). These tendencies for LSBGs and (isolated) UDGs have been recently verified using hydrodynamic simulations (Di Cintio et al 2019;Kulier et al 2020;Benavides et al 2021;Pérez-Montaño et al, in prep. ).…”

Section: Halo Spin and Galaxy Sizementioning

confidence: 83%

Galactic angular momentum in the IllustrisTNG simulation -- I. Connection to morphology, halo spin, and black hole mass

Rodriguez-Gomez,

Genel,

Fall

et al. 2022

Preprint

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We use the TNG100 simulation of the IllustrisTNG project to investigate the stellar specific angular momenta (j * ) of ∼12 000 central galaxies at z = 0 in a full cosmological context, with stellar masses (M * ) ranging from 10 9 to 10 12 M . We find that the j * -M * relations for early-type and late-type galaxies in IllustrisTNG are in good overall agreement with observations, and that these galaxy types typically 'retain' ∼10-20 and ∼50-60 per cent of their host haloes' specific angular momenta, respectively, with some dependence on the methodology used to measure galaxy morphology. We present results for kinematic as well as visual-like morphological measurements of the simulated galaxies. Next, we explore the scatter in the j * -M * relation with respect to the spin of the dark matter halo and the mass of the supermassive black hole (BH) at the galactic centre. We find that galaxies residing in faster-spinning haloes, as well as those hosting less massive BHs, tend to have a higher specific angular momentum. We also find that, at fixed galaxy or halo mass, halo spin and BH mass are anticorrelated with each other, probably as a consequence of more efficient gas flow toward the galactic centre in slowly rotating systems. Finally, we show that halo spin plays an important role in determining galaxy sizes -larger discs form at the centres of faster-rotating haloes -although the trend breaks down for massive galaxies with M * 10 11 M , roughly the mass scale at which a galaxy's stellar mass becomes dominated by accreted stars.

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Section: Halo Spin and Galaxy Sizementioning

confidence: 83%

Galactic angular momentum in the IllustrisTNG simulation -- I. Connection to morphology, halo spin, and black hole mass

Rodriguez-Gomez,

Genel,

Fall

et al. 2022

Preprint

Self Cite

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“…• The initial UDG studies suggested that UDGs represent a population of failed galaxies that assembled their dark matter haloes and were rapidly quenched at high redshift due to environmental processes in galaxy clusters, mainly ram pressure stripping (van Dokkum et al 2015a;Koda et al 2015;Yozin & Bekki 2015;Benavides et al 2021). Additionally, as a consequence of the passive evolution of their stellar populations, UDGs surface brightness have decreased with time (Román & Trujillo 2017;Román et al 2019;Tremmel et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Saifollahi,

Zaritsky,

Trujillo

et al. 2022

Preprint

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We present an analysis of Hubble Space Telescope observations of globular clusters (GCs) in six ultra-diffuse galaxies (UDGs) in the Coma cluster, a sample that represents UDGs with large effective radii (𝑅 e ), and use the results to evaluate competing formation models. We eliminate two significant sources of systematic uncertainty in the determination of the number of GCs, 𝑁 GC by using sufficiently deep observations that (i) reach the turnover of the GC luminosity function and (ii) provide a sufficient number of GCs with which to measure the GC number radial distribution. We find that 𝑁 GC for these galaxies is on average ∼ 20, which implies an average total mass, 𝑀 total , ∼ 10 11 𝑀 when applying the relation between 𝑁 GC and 𝑀 total . This value of 𝑁 GC lies at the upper end of the range observed for dwarf galaxies of the same stellar mass and is roughly a factor of two larger than the mean. The GC luminosity function, radial profile and average colour are more consistent with those observed for dwarf galaxies than with those observed for the more massive (𝐿 * ) galaxies, while both the radial and azimuthal GC distributions closely follow those of the stars in the host galaxy. Finally, we discuss why our observations, specifically the GC number and GC distribution around these six UDGs, pose challenges for several of the currently favoured UDG formation models.

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“…UDGs are low surface-brightness dwarf galaxies, typically with larger stellar sizes than field dwarfs. Many UDGs are located near clusters and have intrinsic properties similar to those expected of backsplash galaxies (Benavides et al 2021;Trujillo 2021). Additionally, the challenges of simulating backsplash galaxies make them an excellent testing ground for the accuracy of numerical models.…”

Section: Introductionmentioning

confidence: 99%

There and back again: understanding the critical properties of backsplash galaxies

Borrow¹,

Vogelsberger²,

O’Neil³

et al. 2022

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Backsplash galaxies are galaxies that once resided inside a cluster, and have migrated back oustide as they move towards the apocenter of their orbit. The kinematic properties of these galaxies are well understood, thanks to the significant study of backsplashers in dark matter-only simulations, but their intrinsic properties are not well constrained due to modelling uncertainties in sub-grid physics, ram pressure stripping, dynamical friction, and tidal forces. In this paper, we use the Illustris-TNG-300-1 simulation, with a baryonic resolution of M b ≈ 1.1 × 10 7 M , to study backsplash galaxies around 1302 isolated galaxy clusters with mass 10 13.0 < M 200,mean /M < 10 15.5 . We employ a decision tree classifier to extract features of galaxies that make them likely to be backsplash galaxies, compared to nearby field galaxies, and find that backsplash galaxies have low gas fractions, high mass-to-light ratios, large stellar sizes, and low black hole occupation fractions. We investigate in detail the origins of these large sizes, and hypothesise their origins are linked to the tidal environments in the cluster. We show that the black hole recentering scheme employed in many cosmological simulations leads to the loss of black holes from galaxies accreted into clusters, and suggest improvements to these models. Generally, we find that backsplash galaxies are a useful population to test and understand numerical galaxy formation models.

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Quiescent ultra-diffuse galaxies in the field originating from backsplash orbits

Cited by 49 publications

References 58 publications

Galactic angular momentum in the IllustrisTNG simulation -- I. Connection to morphology, halo spin, and black hole mass

Galactic angular momentum in the IllustrisTNG simulation -- I. Connection to morphology, halo spin, and black hole mass

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

There and back again: understanding the critical properties of backsplash galaxies

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