The Fornax 3D project: Globular clusters tracing kinematics and metallicities

Fahrion, Katja; Lyubenova, M.; Hilker, M.; Ven, Glenn van de; Falcón-Barroso, J.; Leaman, Ryan; Martín-Navarro, Ignacio; Bittner, A.; Coccato, L.; Corsini, E. M.; Gadotti, Dimitri A.; Iodice, E.; McDermid, Richard M.; Pinna, Francesca; Sarzi, Marc; Viaene, S.; Zeeuw, P. T. de; Zhu, Ling

doi:10.1051/0004-6361/202037685

Cited by 35 publications

(33 citation statements)

References 121 publications

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“…The simultaneous extraction of the spectrum of the stellar body of a galaxy and the spectra of its associated star clusters makes it (Côté et al 2001;Pota et al 2013;Forbes et al 2017;Laporte et al 2019;Fahrion et al 2020b). For the brightest galaxy in our sample -KK 197 -five discrete tracers are available.…”

Section: Internal Dynamics Of Kk 197mentioning

confidence: 99%

The properties of dwarf spheroidal galaxies in the Cen A group

Müller

Fahrion

Rejkuba

et al. 2021

A&A

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Dwarf spheroidal galaxies (dSphs) have been extensively investigated in the Local Group, but their low luminosity and surface brightness make similar work in more distant galaxy groups challenging. Modern instrumentation unlocks the possibility of scrutinizing these faint systems in other environments, expanding the parameter space of group properties. We use MUSE spectroscopy to study the properties of 14 known or suspected dSph satellites of Cen A. Twelve targets are confirmed to be group members based on their radial velocities. Two targets are background galaxies at ∼50 Mpc: KK 198 is a face-on spiral galaxy, and dw1315-45 is an ultradiffuse galaxy with an effective radius of ∼2300 pc. The 12 confirmed dSph members of the Cen A group have old and metal-poor stellar populations and follow the stellar metallicity-luminosity relation defined by the dwarf galaxies in the Local Group. In the three brightest dwarf galaxies (KK 197, KKs 55, and KKs 58), we identify globular clusters, as well as a planetary nebula in KK 197, although its association with this galaxy and/or the extended halo of Cen A is uncertain. Using four discrete tracers, we measure the velocity dispersion and dynamical mass of KK 197. This dSph appears dark matter dominated and lies on the radial acceleration relation of star-forming galaxies within the uncertainties. It also is consistent with predictions stemming from modified Newtonian dynamics (MOND). Surprisingly, in the dwarf KK 203 we find an extended Hα ring. Careful examination of Hubble Space Telescope photometry reveals a very low level of star formation at ages between 30-300 Myr. The Hα emission is most likely linked to a ∼40 Myr old supernova remnant, although other possibilities for its origin cannot be entirely ruled out.

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Section: Internal Dynamics Of Kk 197mentioning

confidence: 99%

The properties of dwarf spheroidal galaxies in the Cen A group

Müller

Fahrion

Rejkuba

et al. 2021

A&A

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“…The relation between GCs and the underlying galaxy stellar population is less straightforward (Forbes & Remus 2018). In general GCs do not necessarily follow the surface brightness distribution and kinematics of the stars (e.g., Brodie & Strader 2006;Coccato et al 2013;Veljanoski et al 2014), although there is growing evidence for red, metal-rich GCs to be tracers of the host galaxy properties (Fahrion et al 2020;Dolfi et al 2020). Therefore we here compare the kinematics of the simulated galaxies and their stellar halos at large radii with PN kinematic results from the ePN.S early-type galaxy survey (Arnaboldi et al 2017, and in prep.…”

Section: Observed Parameters Of Etgsmentioning

confidence: 99%

The stellar halos of ETGs in the IllustrisTNG simulations: The photometric and kinematic diversity of galaxies at large radii

Pulsoni

Gerhard

Arnaboldi

et al. 2020

A&A

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Context. Early-type galaxies (ETGs) are found to follow a wide variety of merger and accretion histories in cosmological simulations. Aims. We characterize the photometric and kinematic properties of simulated ETG stellar halos, and compare them to the observations. Methods. We selected a sample of 1114 ETGs in the TNG100 simulation and 80 in the higher-resolution TNG50. These ETGs span a stellar mass range of 1010.3 − 1012 M⊙ and they were selected within the range of g − r colour and λ-ellipticity diagram populated by observed ETGs. We determined photometric parameters, intrinsic shapes, and kinematic observables in their extended stellar halos. We compared the results with central IFU kinematics and ePN.S planetary nebula velocity fields at large radii, studying the variation in kinematics from center to halo, and connecting it to a change in the intrinsic shape of the galaxies. Results. We find that the simulated galaxy sample reproduces the diversity of kinematic properties observed in ETG halos. Simulated fast rotators (FRs) divide almost evenly in one third having flat λ profiles and high halo rotational support, a third with gently decreasing profiles, and another third with low halo rotation. However, the peak of rotation occurs at larger R than in observed ETG samples. Slow rotators (SRs) tend to have increased rotation in the outskirts, with half of them exceeding λ = 0.2. For M* > 1011.5 M⊙ halo rotation is unimportant. A similar variety of properties is found for the stellar halo intrinsic shapes. Rotational support and shape are deeply related: the kinematic transition to lower rotational support is accompanied by a change towards rounder intrinsic shape. Triaxiality in the halos of FRs increases outwards and with stellar mass. Simulated SRs have relatively constant triaxiality profiles. Conclusions. Simulated stellar halos show a large variety of structural properties, with quantitative but no clear qualitative differences between FRs and SRs. At the same stellar mass, stellar halo properties show a more gradual transition and significant overlap between the two families, despite the clear bimodality in the central regions. This is in agreement with observations of extended photometry and kinematics.

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“…Decades after the pioneering work of Searle & Zinn (1978) demonstrated the potential of GCs as tracers of galaxy formation, new studies began to exploit it (e.g. Côté, Marzke & West 1998;Bekki et al 2005;Rhode, Zepf & Santos 2005;Muratov & Gnedin 2010;Arnold et al 2011;Tonini 2013;Beasley et al 2018;Choksi, Gnedin & Li 2018;Fahrion et al 2020;Ramos-Almendares et al 2020). Theoretical studies of the formation and co-evolution of galaxies and GCs have shown that GCs trace the build-up of L * galaxies across cosmic time (Reina-Campos et al 2019), and that their abundances and ages contain a record of the assembly history of their host (Kruijssen et al 2019a, b;Massari et al 2019).…”

mentioning

confidence: 99%

The kinematics of globular cluster populations in the E-MOSAICS simulations and their implications for the assembly history of the Milky Way

Trujillo-Gomez

Kruijssen

Reina-Campos

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a detailed comparison of the Milky Way (MW) globular cluster (GC) kinematics with the 25 Milky Way-mass cosmological simulations from the E-MOSAICS project. While the MW falls within the kinematic distribution of GCs spanned by the simulations, the relative kinematics of its metal-rich ($[\rm {Fe}/\rm {H}]>-1.2$) versus metal-poor ($[\rm {Fe}/\rm {H}]<-1.2$), and inner (r < 8 kpc) versus outer (r > 8 kpc) populations are atypical for its mass. To understand the origins of these features, we perform a comprehensive statistical analysis of the simulations, and find 18 correlations describing the assembly of L* galaxies and their dark matter haloes based on their GC population kinematics. The correlations arise because the orbital distributions of accreted and in-situ GCs depend on the masses and accretion redshifts of accreted satellites, driven by the combined effects of dynamical fraction, tidal stripping, and dynamical heating. Because the kinematics of in-situ/accreted GCs are broadly traced by the metal-rich/metal-poor and inner/outer populations, the observed GC kinematics are a sensitive probe of galaxy assembly. We predict that relative to the population of L* galaxies, the MW assembled its dark matter and stellar mass rapidly through a combination of in-situ star formation, more than a dozen low-mass mergers, and 1.4 ± 1.2 early (z = 3.1 ± 1.3) major mergers. The rapid assembly period ended early, limiting the fraction of accreted stars. We conclude by providing detailed quantitative predictions for the assembly history of the MW.

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The Fornax 3D project: Globular clusters tracing kinematics and metallicities

Cited by 35 publications

References 121 publications

The properties of dwarf spheroidal galaxies in the Cen A group

The properties of dwarf spheroidal galaxies in the Cen A group

The stellar halos of ETGs in the IllustrisTNG simulations: The photometric and kinematic diversity of galaxies at large radii

The kinematics of globular cluster populations in the E-MOSAICS simulations and their implications for the assembly history of the Milky Way

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