Globular cluster numbers in dark matter haloes in a dual formation scenario: an empirical model within <scp>emerge</scp>

Valenzuela, Lucas M.; Moster, Benjamin P.; Remus, Rhea-Silvia; O'Leary, Joseph A.; Burkert, Andreas

doi:10.1093/mnras/stab1701

Cited by 18 publications

(8 citation statements)

References 78 publications

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“…The number of GCs in a galaxy (𝑁 GC ) is known to scale more strongly with the total mass of the host galaxy (𝑀 total ) (Harris et al 2013) than with the stellar mass. This somewhat surprising result can be recovered for massive galaxies with the total masses typically larger than 10 11 𝑀 , at least, as the natural outcome of hierarchical formation (Boylan-Kolchin 2017;El-Badry et al 2019;Valenzuela et al 2021). Recent simulations incorporating GC formation in cosmological hydrodynamical simulations (E-MOSAICS, Kruĳssen et al 2019;Pfeffer et al 2018) also reproduce the sense of the relation between 𝑁 GC and 𝑀 total (Bastian et al 2020) for galaxies more massive than 5 × 10 11 𝑀 .…”

Section: Gc Numbermentioning

confidence: 87%

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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Section: Gc Numbermentioning

confidence: 87%

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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“…(3) simulations linking GC formation to specific conditions at in the high-redshift Universe (e.g., Mandelker et al 2018;Madau et al 2020;Lake et al 2021); and (4) empirical models connecting GCs to high-redshift halos (e.g., Trenti et al 2015;Boylan-Kolchin 2017;Valenzuela et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Formation of proto-globular cluster candidates in cosmological simulations of dwarf galaxies at $z>4$

Sameie¹,

Boylan-Kolchin²,

Hopkins³

et al. 2022

Preprint

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We perform cosmological hydrodynamical simulations to study the formation of proto-globular cluster candidates in progenitors of present-day dwarf galaxies (𝑀 vir ≈ 10 10 M at 𝑧 = 0) as part of the "Feedback in Realistic Environment" (FIRE) project. Compact (𝑟 1/2 < 30 pc), relatively massive (0.5 × 10 5 𝑀 ★ /M 5 × 10 5 ), self-bound stellar clusters form at 11 𝑧 5 in progenitors with 𝑀 vir ≈ 10 9 M . Cluster formation is triggered when at least 10 7 M of dense, turbulent gas reaches Σ gas ≈ 10 4 M pc −2 as a result of the compressive effects of supernova feedback or from cloud-cloud collisions. The clusters can survive for 2 − 3 Gyr; absent numerical effects, they would likely survive substantially longer, perhaps to 𝑧 = 0. The longest-lived clusters are those that form at significant distance -several hundreds of pc -from their host galaxy. We therefore predict that globular clusters forming in progenitors of present-day dwarf galaxies will be offset from any pre-existing stars within their host dark matter halos as opposed to deeply embedded within a well-defined galaxy. Properties of the nascent clusters are consistent with observations of some of the faintest and most compact high-redshift sources in Hubble Space Telescope lensing fields and are at the edge of what will be detectable as point sources in deep imaging of non-lensed fields with the James Webb Space Telescope. By contrast, the star clusters' host galaxies will remain undetectable.

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“…The physical implication of our results is that the formation of red GCs is closely connected to the stellar mass build-up of galaxies. According to the model of Valenzuela et al (2021), subhalos with a total mass of 𝑀 seedGC ≈ 4 × 10 8 M form on average one GC in parallel to their stars. As these subhalos merge with others, the number of red GCs increases hierarchically in parallel to the stellar mass of the galaxy.…”

Section: Discussionmentioning

confidence: 99%

A Trail of the Invisible: Blue Globular Clusters Trace the Radial Density Distribution of the Dark Matter -- Case Study of NGC 4278

Kluge¹,

Remus²,

Babyk³

et al. 2023

Preprint

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We present new, deep optical observations of the early-type galaxy NGC 4278, which is located in a small loose group. We find that the galaxy lacks fine substructure, i.e., appears relaxed, out to a radius of ∼70 kpc. Our 𝑔-and 𝑖-band surface brightness profiles are uniform down to our deepest levels of ∼28 mag arcsec −2 . Combined with archival globular cluster (GC) number density maps and a new analysis of the total mass distribution, we find that the red GC subpopulation traces well the stellar mass density profile between 2.4 and 14 half-mass radii while the blue GC subpopulation traces the total mass density profile of the galaxy.Furthermore, the red GC spatial distribution has an ellipticity consistent with the stellar mass (𝜖 ≈ 0.1) and is well centered on it. On the other hand, the blue GC distribution is more elongated (0.25 < 𝜖 < 0.4) and offset in the northwest direction by 2-3 kpc. Our results reinforce the scenario that red GCs form mostly in-situ along with the stellar component of the galaxy, while the blue GCs are more closely aligned with the total mass distribution in the halo and were accreted along with halo matter.

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Globular cluster numbers in dark matter haloes in a dual formation scenario: an empirical model within emerge

Cited by 18 publications

References 78 publications

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

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

Formation of proto-globular cluster candidates in cosmological simulations of dwarf galaxies at $z>4$

A Trail of the Invisible: Blue Globular Clusters Trace the Radial Density Distribution of the Dark Matter -- Case Study of NGC 4278

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