The Fornax 3D project: Thick disks in a cluster environment

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

doi:10.1051/0004-6361/201935154

Cited by 47 publications

(21 citation statements)

References 86 publications

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“…In Fahrion et al (2019b), we argued that the old age and high metallicity of the NSC in FCC 47 indicates an efficient formation at early times. Similar arguments were made in the detailed analysis of FCC 170 by Pinna et al (2019a) using the same F3D MUSE data which showed that FCC 170 assembled very rapidly and efficiently at early times (see also Poci et al 2021). Their SFH of the central region of FCC 170 is similar to the one presented here.…”

Section: Most Massive Galaxiessupporting

confidence: 86%

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Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories

Fahrion,

Lyubenova,

van de Ven

et al. 2021

Preprint

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Nuclear star clusters (NSCs) are the densest stellar systems in the Universe and are found in the centres of all types of galaxies. They are thought to form via mergers of star clusters such as ancient globular clusters (GCs) that spiral to the centre as a result of dynamical friction or through in-situ star formation directly at the galaxy centre. There is evidence that both paths occur, but the relative contribution of either channel and their correlation with galaxy properties are not yet constrained observationally. We aim to derive the dominant NSC formation channel for a sample of 25 nucleated galaxies, mostly in the Fornax galaxy cluster, with stellar masses between M gal ∼ 10 8 and 10 10.5 M and NSC masses between M NSC ∼ 10 5 and 10 8.5 M . Using Multi-Unit Spectroscopic Explorer (MUSE) data from the Fornax 3D survey and the ESO archive, we derive star formation histories, mean ages and metallicities of NSCs, and compare them to the host galaxies. In many low-mass galaxies, the NSCs are significantly more metal-poor than their hosts with properties similar to GCs. In contrast, in the massive galaxies, we find diverse star formation histories and cases of ongoing or recent in-situ star formation. Massive NSCs (> 10 7 M ) occupy a different region in the mass-metallicity diagram than lower mass NSCs and GCs, indicating a different enrichment history. We find a clear transition of the dominant NSC formation channel with both galaxy and NSC mass. We hypothesise that while GC-accretion forms the NSCs of the dwarf galaxies, central star formation is responsible for the efficient mass build up in the most massive NSCs in our sample. At intermediate masses, both channels can contribute. The transition between these formation channels seems to occur at galaxy masses M gal ∼ 10 9 M and NSC masses M NSC ∼ 10 7 M .

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Section: Most Massive Galaxiessupporting

confidence: 86%

“…FCC 170 is an edge-on S0 galaxy with multiple structural components including a thin disk, thick disk, and a X-shaped bulge component (see e.g. Pinna et al 2019a;Poci et al 2021). Modelling this galaxy with imfit is challenging.…”

Section: Appendix B: Exemplary Binned Metallicity Mapsmentioning

confidence: 99%

Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories

Fahrion,

Lyubenova,

van de Ven

et al. 2021

Preprint

Self Cite

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“…Williams et al (2011) suggested that this galaxy may have a small classical bulge, which would make it different from M 31 with its sizeable classical bulge. Pinna et al (2019b) studied another galaxy with a B/P bulge, FCC 177. However, this one does not have obvious signs of the B/P bulge in metallicity and certainly not in [Mg/Fe].…”

Section: Comparison With Other Galaxiesmentioning

confidence: 99%

Unravelling stellar populations in the Andromeda Galaxy

Gajda

Gerhard

Blaña

et al. 2021

A&A

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To understand the history and formation mechanisms of galaxies, it is crucial to determine their current multidimensional structure. In this work, we focus on the properties that characterise stellar populations, such as metallicity and [α/Fe] enhancement. We devised a new technique to recover the distribution of these parameters using spatially resolved, line-of-sight averaged data. Our chemodynamical method is based on the made-to-measure framework and results in an N-body model for the abundance distribution. Following a test on a mock data set we found that the radial and azimuthal profiles were well-recovered, however, only the overall shape of the vertical profile matches the true profile. We applied our procedure to spatially resolved maps of mean [Z/H] and [α/Fe] for the Andromeda Galaxy, using an earlier barred dynamical model of M 31. We find that the metallicity is enhanced along the bar, with a possible maxima at the ansae. In the edge-on view, the [Z/H] distribution has an X shape due to the boxy/peanut bulge; the average vertical metallicity gradient is equal to −0.133 ± 0.006 dex kpc−1. We identify a metallicity-enhanced ring around the bar, which also has relatively lower [α/Fe]. The highest [α/Fe] is found in the centre, due to the classical bulge. Away from the centre, the α-overabundance in the bar region increases with height, which could be an indication of a thick disc. We argue that the galaxy assembly resulted in a sharp peak of metallicity in the central few hundred parsecs and a more gentle negative gradient in the remaining disc, but no [α/Fe] gradient. The formation of the bar leads to the re-arrangement of the [Z/H] distribution, causing a flat gradient along the bar. Subsequent star formation close to the bar ends may have produced the metallicity enhancements at the ansae and the [Z/H] enhanced lower-α ring.

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“…Nevertheless, the presence of different structures is expected to modify the orbit of stars and leave distinct. For example, features such as a double thin-thick disc structure (Burstein 1979;Tsikoudi 1979), warps (Reshetnikov & Combes 1998;Ann & Park 2006;Reshetnikov et al 2016), rings (Few & Madore 1986), single and double bars (Shlosman, Frank & Begelman 1989;de Lorenzo-Cáceres et al 2019), disc breaks (van der Kruit 1979; Pohlen et al 2004;Martín-Navarro et al 2012), and spiral arms (Danver 1942;Bittner et al 2020a) leave different imprints in the kinematics and stellar populations properties that help us disentangle different evolutionary paths (Pinna et al 2019;Gadotti et al 2020;Rosado-Belza et al 2020;Bittner et al 2020b) This type of analysis is extremely useful in the Milky Way, where we have access to the full six-dimensional (6D) information E-mail: dwalo@iac.es, danielwalo@hotmail.com (positions and velocities), chemical abundances, and ages of the stars. Thanks to missions like GAIA (Gaia Collaboration et al 2016) and APOGEE (Majewski et al 2017), we now have access to the properties of millions of stars in a large region of our Galaxy which allows us to study the spatial variations of the stellar kinematics beyond the solar neighbourhood.…”

Section: Introductionmentioning

confidence: 99%

Local variations of the Stellar Velocity Ellipsoid-I: the disc of galaxies in the Auriga simulations

Walo-Martín

Pérez

Grand

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The connection between the Stellar Velocity Ellipsoid (SVE) and the dynamical evolution of galaxies has been a matter of debate in the last years and there is no clear consensus whether different heating agents (e.g. spiral arms, giant molecular clouds, bars and mergers) leave clear detectable signatures in the present day kinematics. Most of these results are based on a single and global SVE and have not taken into account that these agents do not necessarily equally affect all regions of the stellar disc.We study the 2D spatial distribution of the SVE across the stellar discs of Auriga galaxies, a set of high resolution magneto-hydrodynamical cosmological zoom-in simulations, to unveil the connection between local and global kinematic properties in the disc region. We find very similar, global, σz/σr = 0.80 ± 0.08 values for galaxies of different Hubble types. This shows that the global properties of the SVE at z=0 are not a good indicator of the heating and cooling events experienced by galaxies. We also find that similar σz/σr radial profiles are obtained through different combinations of σz and σr trends: at a local level, the vertical and radial components can evolve differently, leading to similar σz/σr profiles at z=0. By contrast, the 2D spatial distribution of the SVE varies a lot more from galaxy to galaxy. Present day features in the SVE spatial distribution may be associated with specific interactions such as fly-by encounters or the accretion of low mass satellites even in the cases when the global SVE is not affected. The stellar populations decomposition reveals that young stellar populations present colder and less isotropic SVEs and more complex 2D distributions than their older and hotter counterparts.

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The Fornax 3D project: Thick disks in a cluster environment

Cited by 47 publications

References 86 publications

Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories

Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories

Unravelling stellar populations in the Andromeda Galaxy

Local variations of the Stellar Velocity Ellipsoid-I: the disc of galaxies in the Auriga simulations

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