Galaxy populations in the Hydra I cluster from the VEGAS survey

Marca, Antonio La; Iodice, E.; Cantiello, M.; Forbes, Duncan A.; Rejkuba, M.; Hilker, M.; Arnaboldi, M.; Greggio, L.; Spiniello, C.; Mieske, S.; Venhola, Aku; Spavone, M.; D’Ago, G.; Raj, M. A.; Ragusa, Rossella; Mirabile, M.; Rampazzo, R.; Peletier, R. F.; Paolillo, M.; Choque-Challapa, Nelvy; Schipani, P.

doi:10.1051/0004-6361/202142367

Cited by 24 publications

(9 citation statements)

References 115 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our findings clearly point to there being at least two pathways for forming UDGs, as the dearth of GCs in our field sample is incompatible with the GC-rich UDGs typically found in clusters. However, we note that UDGs in the Hydra cluster (Iodice et al 2020;La Marca et al 2022) appear to host far fewer GCs than those in Coma, and some of these UDGs might have had progenitors similar to the field UDGs presented in this work.…”

Section: Could Field Ultra-diffuse Galaxies Represent Thementioning

confidence: 49%

Gas-rich, Field Ultra-diffuse Galaxies Host Few Gobular Clusters

Jones

Karunakaran

Bennet

et al. 2022

ApJL

View full text Add to dashboard Cite

We present Hubble Space Telescope imaging of 14 gas-rich, low-surface-brightness galaxies in the field at distances of 25–36 Mpc, with mean effective radii and g-band central surface brightnesses of 1.9 kpc and 24.2 mag arcsec−2. Nine meet the standard criteria to be considered ultra-diffuse galaxies (UDGs). An inspection of point-like sources brighter than the turnover magnitude of the globular cluster luminosity function and within twice the half-light radii of each galaxy reveals that, unlike those in denser environments, gas-rich, field UDGs host very few old globular clusters (GCs). Most of the targets (nine) have zero candidate GCs, with the remainder having one or two candidates each. These findings are broadly consistent with expectations for normal dwarf galaxies of similar stellar mass. This rules out gas-rich, field UDGs as potential progenitors of the GC-rich UDGs that are typically found in galaxy clusters. However, some in galaxy groups may be directly accreted from the field. In line with other recent results, this strongly suggests that there must be at least two distinct formation pathways for UDGs, and that this subpopulation is simply an extreme low surface brightness extension of the underlying dwarf galaxy population. The root cause of their diffuse stellar distributions remains unclear, but the formation mechanism appears to only impact the distribution of stars (and potentially dark matter), without strongly impacting the distribution of neutral gas, the overall stellar mass, or the number of GCs.

show abstract

Section: Could Field Ultra-diffuse Galaxies Represent Thementioning

confidence: 49%

Gas-rich, Field Ultra-diffuse Galaxies Host Few Gobular Clusters

Jones

Karunakaran

Bennet

et al. 2022

ApJL

View full text Add to dashboard Cite

show abstract

“…On the other hand, ELVES includes several more massive hosts than our search and SAGA do, and consequently bias the UDG abundance. We plot the UDG abundances from these surveys in the left panel of Figure 7, together with the results for larger galaxy groups and clusters (Koda et al 2015;Muñoz et al 2015;Román & Trujillo 2017b, 2017aJanssens et al 2017;van der Burg et al 2017;La Marca et al 2022). The power-law regression result from van der Burg et al The UDG abundance of this work is highlighted as the red square.…”

Section: Abundance Of Mass-size Outliersmentioning

confidence: 89%

Beyond Ultra-diffuse Galaxies. I. Mass–Size Outliers among the Satellites of Milky Way Analogs

Li 李,

Greene,

Greco

et al. 2023

ApJ

View full text Add to dashboard Cite

Large diffuse galaxies are hard to find, but understanding the environments where they live, their numbers, and ultimately their origins, is of intense interest and importance for galaxy formation and evolution. Using Subaru’s Hyper Suprime-Cam Strategic Survey Program, we perform a systematic search for low surface brightness galaxies and present novel and effective methods for detecting and modeling them. As a case study, we surveyed 922 Milky Way analogs in the nearby Universe (0.01 < z < 0.04) and built a large sample of satellite galaxies that are outliers in the mass–size relation. These “ultra-puffy” galaxies (UPGs), defined to be 1.5σ above the average mass–size relation, represent the tail of the satellite size distribution. We find that each MW analog hosts N UPG = 0.31 ± 0.05 UPGs on average, which is consistent with but slightly lower than the observed abundance at this halo mass in the Local Volume. We also construct a sample of ultra-diffuse galaxies (UDGs) in MW analogs and find an abundance of N UDG = 0.44 ± 0.05 per host. With literature results, we confirm that the UDG abundance scales with the host halo mass following a sublinear power law. We argue that our definition of UPGs, which is based on the mass–size relation, is more physically motivated than the common definition of UDGs, which depends on the surface brightness and size cuts and thus yields different surface mass density cuts for quenched and star-forming galaxies.

show abstract

“…In addition to the smooth components with elliptical symmetry, maze-like webs of tails, plumes and spurs can be present. Exemplary testimony of such intricate luminous substructures is provided by the extremely deep images, reaching surface brightness levels below 1% of the night sky: see for example those obtained for the Virgo (Mihos et al, 2005;Mihos et al, 2013;Spavone et al, 2017), Fornax (Iodice et al, 2016) and the Hydra-I (Arnaboldi et al, 2012;Barbosa et al, 2018;La Marca et al, 2022a;La Marca et al, 2022b) clusters.…”

Section: Introductionmentioning

confidence: 99%

Kinematics of the diffuse intragroup and intracluster light in groups and clusters of galaxies in the local universe within 100 Mpc distance

Arnaboldi

Gerhard

2022

Front. Astron. Space Sci.

Self Cite

View full text Add to dashboard Cite

Nearly all intragroup (IGL) and intracluster light (ICL) comes from stars that are not bound to any single galaxy but were formed in galaxies and later unbound from them. In this review we focus on the physical properties–phase space properties, metallicity and age distribution–of the ICL and IGL components of the groups and clusters in the local universe, within 100 Mpc distance. Kinematic–information on these very low surface brightness structures mostly comes from discrete tracers such as planetary nebulae and globular clusters, showing highly unrelaxed velocity distributions. Cosmological hydrodynamical simulations provide key predictions for the dynamical state of IGL and ICL and find that most IC stars are dissolved from galaxies that subsequently merge with the central galaxy. The increase of the measured velocity dispersion with radius in the outer halos of bright galaxies is a physical feature that makes it possible to identify IGL and ICL components. In the local groups and clusters, IGL and ICL are located in the dense regions of these structures. Their light fractions relative to the total luminosity of the satellite galaxies in a given group or cluster are between a few to ten percent, significantly lower than the average values in more evolved, more distant clusters. IGL and ICL in the Leo I and M49 groups, and the Virgo cluster core around M87, has been found to arise from mostly old (≥10 Gyr) metal-poor ([Fe/H] <-1.0) stars of low-mass progenitor galaxies. New imaging facilities such as LSST, Euclid, and the “big eyes’’ on the sky–ELT and JWST with their advanced instrumentation–promise to greatly increase our knowledge of the progenitors of the IGL and ICL stars, their ages, metal content, masses and evolution, there by increasing our understanding of this enigmatic component.

show abstract

Galaxy populations in the Hydra I cluster from the VEGAS survey

Cited by 24 publications

References 115 publications

Gas-rich, Field Ultra-diffuse Galaxies Host Few Gobular Clusters

Gas-rich, Field Ultra-diffuse Galaxies Host Few Gobular Clusters

Beyond Ultra-diffuse Galaxies. I. Mass–Size Outliers among the Satellites of Milky Way Analogs

Kinematics of the diffuse intragroup and intracluster light in groups and clusters of galaxies in the local universe within 100 Mpc distance

Contact Info

Product

Resources

About