The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

Piña, Pavel E. Mancera; Aguerri, J. A. L.; Peletier, Reynier F.; Venhola, Aku; Trager, S. C.; Choque-Challapa, Nelvy

doi:10.1093/mnras/stz238

Cited by 69 publications

(48 citation statements)

References 69 publications

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“…tidal effects) from the blue field ones, which we will discuss in later subsections. Note that similar environmental dependencies of UDG morphology have been also found in Mancera Piña et al (2019) for eight nearby clusters.…”

Section: Halo Masses Spins and Morphologysupporting

confidence: 76%

Ultra-diffuse galaxies in the Auriga simulations

Liao

Gao

Frenk

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the formation of ultra-diffuse galaxies (UDGs) using the Auriga highresolution cosmological magneto-hydrodynamical simulations of Milky Way-sized galaxies. We identify a sample of 92 UDGs in the simulations that match a wide range of observables such as sizes, central surface brightness, Sérsic indices, colors, spatial distribution and abundance. Auriga UDGs have dynamical masses similar to normal dwarfs. In the field, the key to their origin is a strong correlation present in low-mass dark matter haloes between galaxy size and halo spin parameter. Field UDGs form in dark matter haloes with larger spins compared to normal dwarfs in the field, in agreement with previous semi-analytical models. Satellite UDGs, on the other hand, have two different origins: ∼ 55% of them formed as field UDGs before they were accreted; the remaining ∼ 45% were normal field dwarfs that subsequently turned into UDGs as a result of tidal interactions.

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Section: Halo Masses Spins and Morphologysupporting

confidence: 76%

Ultra-diffuse galaxies in the Auriga simulations

Liao

Gao

Frenk

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…They have been identified in different galactic environments for decades (e.g., Sandage & Binggeli 1984;Impey et al 1988). These galaxies have recently experienced a revival (Crnojević et al 2014;van Dokkum et al 2015a;Koda et al 2015;van der Burg et al 2016;Martínez-Delgado et al 2016;Merritt et al 2016;Román & Trujillo 2017a;Venhola et al 2017;Wittmann et al 2017;Müller et al 2018;Mancera Piña et al 2019). In galaxy clusters, UDGs do not contain gas while in sparser environments, they can be gas dominated (van Dokkum et al 2015a;Shi et al 2017;Leisman et al 2017;Papastergis et al 2017;Sardone et al 2019), following the well-known densitymorphology relation (Dressler 1980).…”

Section: Introductionmentioning

confidence: 99%

Discussing the first velocity dispersion profile of an ultra-diffuse galaxy in MOND

Bílek

Müller

Famaey

2019

A&A

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Using Jeans modelling, we calculate the velocity dispersion profile of the ultra-diffuse galaxy (UDG) Dragonfly 44 in MOND. For the nominal mass-to-light ratio from the literature and an isotropic profile, the agreement with the data is excellent near the center of the galaxy. However, in modified gravity, close to the cluster core, the gravitational environment should bring the galaxy back towards the Newtonian behavior. This success of the isolated MOND prediction for the central velocity dispersion could then mean that the galaxy is at large distances ( 5 Mpc) from the cluster core, as hinted by the fact that close-by UDGs share similar velocities with a dispersion well below that of the cluster itself. There is however a two-sigma tension in the outer part of the UDG due to an increase of the observed dispersion profile with respect to the flat MOND prediction. This deviation could simply be a measurement error. Other possibilities could be, for a UDG far from the cluster, a higher-than-nominal baryonic mass with a tangentially anisotropic dispersion profile, or even a sign of a dark baryonic halo. If the UDG is closer to the cluster core, the deviation could be a sign that it is in the process of disruption.

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“…Indeed, this property has been exploited by several authors in their studies of UDGs in such environments (e.g. Koda et al 2015;Muñoz et al 2015;Yagi et al 2016;van der Burg et al 2016van der Burg et al , 2017Janssens et al 2017;Venhola et al 2017;Zaritsky et al 2019;Mancera Piña et al 2019). This bias towards studies in dense environments is exacerbated by the difficulty of obtaining spectroscopic redshifts (and therefore distances) for large samples of LSB galaxies.…”

Section: Introductionmentioning

confidence: 99%

Observational properties of ultra-diffuse galaxies in low-density environments: field UDGs are predominantly blue and star forming

Prole

Burg

Hilker

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Abstract While we have learnt much about ultradiffuse galaxies (UDGs) in groups and clusters, relatively little is known about them in less dense environments. More isolated UDGs are important for our understanding of UDG formation scenarios because they form via secular mechanisms, allowing us to determine the relative importance of environmentally driven formation in groups and clusters. We have used the public Kilo-Degree Survey together with the Hyper Suprime-Cam Subaru Strategic Program to constrain the abundance and properties of UDGs in the field, targeting sources with low surface brightness (24.0 ≤ $\bar{\mu }_{\mathrm{ e},r}$ ≤ 26.5) and large apparent sizes (3.0 arcsec ≤ $\bar{r}_{\mathrm{ e},r}$ ≤ 8.0 arcsec). Accounting for several sources of interlopers in our selection based on canonical scaling relations, and using an empirical UDG model based on measurements from the literature, we show that a scenario in which cluster-like red-sequence UDGs occupy a significant number of field galaxies is unlikely, with most field UDGs being significantly bluer and showing signs of localized star formation. An immediate conclusion is that UDGs are much more efficiently quenched in high-density environments. We estimate an upper limit on the total field abundance of UDGs of 8 ± 3 × 10−3 cMpc−3 within our selection range. We also compare the total field abundance of UDGs to a measurement of the abundance of H i-rich UDGs from the literature, suggesting that they occupy at least one-fifth of the overall UDG population. The mass formation efficiency of UDGs implied by this upper limit is similar to what is measured in groups and clusters.

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The evolution of ultra-diffuse galaxies in nearby galaxy clusters from the Kapteyn IAC WEAVE INT Clusters Survey

Cited by 69 publications

References 69 publications

Ultra-diffuse galaxies in the Auriga simulations

Ultra-diffuse galaxies in the Auriga simulations

Discussing the first velocity dispersion profile of an ultra-diffuse galaxy in MOND

Observational properties of ultra-diffuse galaxies in low-density environments: field UDGs are predominantly blue and star forming

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