Exploring the origin of ultra-diffuse galaxies in clusters from their primordial alignment

Yu, Rong; Piña, Pavel E. Mancera; Tempel, Elmo; Puzia, Thomas H.; Rijcke, S. De

doi:10.1093/mnrasl/slaa129

Cited by 14 publications

(7 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Sample1: the publicly available 18 Coma UDG sample reported by Yagi et al (2016). These UDGs are distributed within R 200 (R 200 is the radius within which the mean cluster density is 200 times the critical density) of Coma, with r-band 19 17 There is also literature that alternatively suggests no UDG radial alignment in some galaxy clusters (Mancera Piña et al 2019;Rong et al 2019), but possible UDG primordial alignment (Rong et al 2020a).…”

Section: Udg Samplesmentioning

confidence: 99%

Intrinsic Morphology of Ultra-diffuse Galaxies

Dong

Puzia

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

With the published data of apparent axis ratios for 1109 ultra-diffuse galaxies (UDGs) located in 17 low-redshift (z ∼ 0.020-0.063) galaxy clusters and 84 UDGs in two intermediate-redshift (z ∼ 0.308-0.348) clusters, we take advantage of a Markov Chain Monte Carlo approach and assume a triaxial model to investigate the intrinsic morphologies of UDGs. In contrast to the conclusion of Burkert, i.e., the underlying shapes of UDGs are purely prolate (C=B<A), we find that the data favor the oblate-triaxial models (i.e., thick disks with <  C B A) over the nearly prolate ones. We also find that the intrinsic morphologies of UDGs are related to their stellar masses/ luminosities, environments, and redshifts. First, the more luminous UDGs have puffier morphologies compared with the less luminous counterparts; the UDG morphologic dependence on luminosity is distinct from that of the typical quiescent dwarf ellipticals (dEs) and dwarf spheroidals (dSphs); in this sense, UDGs may not be simply treated as an extension of the dE/dSph class with similar evolutionary histories; they may differ not only in size. Second, the UDGs with smaller clustercentric distances are more puffed up, compared with the counterparts with larger clustercentric distances; in combination with the UDG thickness dependence on luminosity, the puffier morphologies of UDGs with high luminosities or located in the denser environments are very likely to be attributed to tidal interactions with massive galaxies. Third, we find that the intermediate-redshift UDGs are more flattened, compared with the low-redshift counterparts, which plausibly suggests a "disky" origin for the high-redshift, newly born UDGs.

show abstract

Section: Udg Samplesmentioning

confidence: 99%

Intrinsic Morphology of Ultra-diffuse Galaxies

Dong

Puzia

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…To date, a significant population of UDGs has been found in dense environments, such as clusters and groups of galaxies, as well as in the field (Koda et al 2015;Román & Trujillo 2017;van der Burg et al 2017;Shi et al 2017;Müller et al 2018;Venhola et al 2017;Prole et al 2019b;Forbes et al 2019;Janssens et al 2019;Forbes et al 2020b;Habas et al 2020). Based on their colour distribution, morphology, stellar popula-tion, and globular cluster (GC) systems, a wide range of observed properties are found for UDGs, which do not fit into a single formation scenario (Leisman et al 2017;Román & Trujillo 2017;Ferré-Mateu et al 2018;Martín-Navarro et al 2019;Lim et al 2020;Forbes et al 2020a;Rong et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Formation of an ultra-diffuse galaxy in the stellar filaments of NGC 3314A: Caught in the act?

Iodice

Marca

Hilker

et al. 2021

A&A

View full text Add to dashboard Cite

The VEGAS imaging survey of the Hydra I cluster has revealed an extended network of stellar filaments to the south-west of the spiral galaxy NGC 3314A. Within these filaments, at a projected distance of ∼ 40 kpc from the galaxy, we discover an ultra-diffuse galaxy (UDG) with a central surface brightness of µ 0,g ∼ 26 mag arcsec −2 and effective radius R e ∼ 3.8 kpc. This UDG, named UDG 32, is one of the faintest and most diffuse low-surface-brightness galaxies in the Hydra I cluster. Based on the available data, we cannot exclude that this object is just seen in projection on top of the stellar filaments and is thus instead a foreground or background UDG in the cluster. However, the clear spatial coincidence of UDG 32 with the stellar filaments of NGC 3314A suggests that it might have formed from the material in the filaments, becoming a detached, gravitationally bound system. In this scenario, the origin of UDG 32 depends on the nature of the stellar filaments in NGC 3314A, which is still unknown. The stellar filaments could result from ram-pressure stripping or have a tidal origin. In this letter we focus on the comparison of the observed properties of the stellar filaments and of UDG 32 and speculate on their possible origin. The relatively red colour (g − r = 0.54 ± 0.14 mag) of the UDG, similar to that of the disk in NGC 3314A, combined with an age older than 1 Gyr and the possible presence of a few compact stellar systems, points towards a tidal formation scenario.

show abstract

“…The lack of this trend in Figure 6 suggests that GC-rich UDG quenching is not environmentally driven. Furthermore, the axial alignment of UDGs at radii > 0.5𝑅 200 of the cluster Abell 2634 suggests they have experienced little evolution in the cluster thus far (Rong et al 2020). If UDG quenching is not environmentally driven it may be either self induced or triggered via pre-processing of GCrich UDGs in a group environment.…”

Section: Udg Infall Timesmentioning

confidence: 99%

Ultra-Diffuse Galaxies in the Perseus Cluster: Comparing Galaxy Properties with Globular Cluster System Richness

Gannon,

Forbes,

Romanowsky

et al. 2021

Preprint

View full text Add to dashboard Cite

It is clear that within the class of ultra-diffuse galaxies (UDGs) there is an extreme range in the richness of their associated globular cluster (GC) systems. Here, we report the structural properties of five UDGs in the Perseus cluster based on deep Subaru / Hyper Suprime-Cam imaging. Three appear GC-poor and two appear GC-rich. One of our sample, PUDG_R24, appears to be undergoing quenching and is expected to fade into the UDG regime within the next ∼ 0.5 Gyr. We target this sample with Keck Cosmic Web Imager (KCWI) spectroscopy to investigate differences in their dark matter halos, as expected from their differing GC content. Our spectroscopy measures both recessional velocities, confirming Perseus cluster membership, and stellar velocity dispersions, to measure dynamical masses within their halflight radius. We supplement our data with that from the literature to examine trends in galaxy parameters with GC system richness. We do not find the correlation between GC numbers and UDG phase space positioning expected if GC-rich UDGs environmentally quench at high redshift. We do find GC-rich UDGs to have higher velocity dispersions than GC-poor UDGs on average, resulting in greater dynamical mass within the half-light radius. This agrees with the first order expectation that GC-rich UDGs have higher halo masses than GC-poor UDGs.

show abstract

Exploring the origin of ultra-diffuse galaxies in clusters from their primordial alignment

Cited by 14 publications

References 53 publications

Intrinsic Morphology of Ultra-diffuse Galaxies

Intrinsic Morphology of Ultra-diffuse Galaxies

Formation of an ultra-diffuse galaxy in the stellar filaments of NGC 3314A: Caught in the act?

Ultra-Diffuse Galaxies in the Perseus Cluster: Comparing Galaxy Properties with Globular Cluster System Richness

Contact Info

Product

Resources

About