The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Pastorello, Nicola; Forbes, Duncan A.; Usher, Christopher; Brodie, Jean P.; Romanowsky, Aaron J.; Strader, Jay; Spitler, Lee R.; Alabi, Adebusola B.; Foster, Caroline; Jennings, Zachary G.; Kartha, Sreeja S.; Pota, Vincenzo

doi:10.1093/mnras/stv1131

Cited by 23 publications

(22 citation statements)

References 96 publications

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“…Because the chemical composition of GCs is linked to that of their progenitor galaxy (e.g., Liu et al 2016;Pastorello et al 2015), it is of interest to identify the spectrum of galaxy masses contributing GCs within a galaxy cluster. The top panel in Fig.…”

Section: Building the Intracluster Gcs Componentmentioning

confidence: 99%

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Ramos

Sales

Abadi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at infall time and their tidal removal and distribution within the cluster is followed later self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (M vir ) and mass in GCs (M GC ) as found in observations. We find that the GCs specific frequency S N as a function of V-band magnitude naturally reproduces the observed "U"-shape, due to the combination of a power law M GC -M vir relation and the non-linear M * -M vir relation from the simulation. Additional scatter in the S N values are traced back to galaxies with early infall times due to the evolution in the M * -M vir relation with redshift. GCs that have been tidally removed from their galaxies form today the intra-cluster component from which about ∼ 60% were brought in by galaxies that orbit today within the cluster potential. The remaining "orphan" GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intra-cluster component is a good dynamical tracer of the dark matter potential providing an estimate of the velocity dispersion of the dark matter with 25% accuracy. As a consequence of the accreted nature of most intra-cluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87 or NGC 1407. † Hellman Fellow cause of their inferred old ages (Vandenberg et al. 1996) clustered distribution around galaxies, they are believed to be surviving probes of the early star formation in the universe.GCs are, however, more metal poor than the bulk of the stars in their host galaxy. In fact, GCs display a wide range of colors and metallicities suggestive of a separation where the youngest and more metal rich GCs are formed insitu -and perhaps associated to major mergers-while the metal poor component is likely acquired hierarchically via the accretion of smaller galaxies (e.g.

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Section: Building the Intracluster Gcs Componentmentioning

confidence: 99%

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Ramos

Sales

Abadi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Our sample consists of 5 ETGs imaged by the SLUGGS survey and 16 others from the literature. We also include the average value derived for six BCGs by Harris (2009a), and the average value for six high mass ETGs of the SLUGGS survey by Pastorello et al (2015).…”

Section: The Samplementioning

confidence: 99%

Metallicity gradients in the globular cluster systems of early-type galaxies: in situ and accreted components?

Forbes

Remus

2018

Monthly Notices of the Royal Astronomical Society

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Massive early-type galaxies typically have two subpopulations of globular clusters (GCs) which often reveal radial colour (metallicity) gradients. Collating gradients from the literature, we show that the gradients in the metal-rich and metal-poor GC subpopulations are the same, within measurement uncertainties, in a given galaxy. Furthermore, these GC gradients are similar in strength to the stellar metallicity gradient of the host galaxy. At the very largest radii (e.g. greater than 8 galaxy effective radii) there is some evidence that the GC gradients become flat with near constant mean metallicity. Using stellar metallicity gradients as a proxy, we probe the assembly histories of massive early-type galaxies with hydrodynamical simulations from the Magneticum suite of models. In particular, we measure the stellar metallicity gradient for the in-situ and accreted components over a similar radial range as those observed for GC subpopulations. We find that the in-situ and accreted stellar metallicity gradients are similar but have a larger scatter than the metal-rich and metal-poor GC subpopulations gradients in a given galaxy. We conclude that although metal-rich GCs are predominately formed during the in-situ phase and metal-poor GCs during the accretion phase of massive galaxy formation, they do not have a strict one-to-one connection.

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“…To explain the formation and evolution of early-type galaxies (ETG), the so-called two-phase scenario of Oser et al 2010 has been quite extensively used and discussed (Arnold et al 2014;Pastorello et al 2015, and references therein), and suggested for NGC 3115 by Arnold et al (2011). According to this scenario, ETG growth would first be dominated by in situ star formation at high redshift (z 2−3), triggered by dissipative gas collapse forming most of the central stellar mass.…”

Section: Formation and Evolution Scenarios For Ngc 3115mentioning

confidence: 99%

Exploring the mass assembly of the early-type disc galaxy NGC 3115 with MUSE

Guérou

Emsellem

Krajnović

et al. 2016

A&A

103

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We present MUSE integral field spectroscopic data of the S0 galaxy NGC 3115 obtained during the instrument commissioning at the ESO Very Large Telescope (VLT). We analyse the galaxy stellar kinematics and stellar populations and present two-dimensional maps of their associated quantities. We thus illustrate the capacity of MUSE to map extra-galactic sources to large radii in an efficient manner, i.e. ∼4 R e , and provide relevant constraints on its mass assembly. We probe the well-known set of substructures of NGC 3115 (nuclear disc, stellar rings, outer kpc-scale stellar disc, and spheroid) and show their individual associated signatures in the MUSE stellar kinematics and stellar populations maps. In particular, we confirm that NGC 3115 has a thin fast-rotating stellar disc embedded in a fast-rotating spheroid, and that these two structures show clear differences in their stellar age and metallicity properties. We emphasise an observed correlation between the radial stellar velocity, V, and the Gauss-Hermite moment, h 3 , which creates a butterfly shape in the central 15 of the h 3 map. We further detect the previously reported weak spiral-and ring-like structures, and find evidence that these features can be associated with regions of younger mean stellar ages. We provide tentative evidence for the presence of a bar, although the V-h 3 correlation can be reproduced by a simple axisymmetric dynamical model. Finally, we present a reconstruction of the two-dimensional star formation history of NGC 3115 and find that most of its current stellar mass was formed at early epochs (>12 Gyr ago), while star formation continued in the outer (kpc-scale) stellar disc until recently. Since z ∼2 and within ∼4 R e , we suggest that NGC 3115 has been mainly shaped by secular processes.

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The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Cited by 23 publications

References 96 publications

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Metallicity gradients in the globular cluster systems of early-type galaxies: in situ and accreted components?

Exploring the mass assembly of the early-type disc galaxy NGC 3115 with MUSE

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