The Fornax 3D project: Unveiling the thick disk origin in FCC 170; possible signs of accretion

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

doi:10.1051/0004-6361/201833193

Cited by 79 publications

(78 citation statements)

References 126 publications

(208 reference statements)

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“…The two-dimensional stellar kinematics and stellar population analysis of FCC 170 from the Fornax3D (F3D) project with MUSE (Sarzi et al 2018) reveal the presence of a fast-rotating and flaring thin disc and a slower rotating thick disc in this galaxy (Pinna et al 2019). Preliminary results from the F3D survey for the other two galaxies, FCC 153 and FCC 177, also confirm the existence of a flaring disc (Pinna et al, in prep.).…”

Section: Flaring Of the Discs In The Edge-on S0 Galaxiesmentioning

confidence: 76%

“…The different morphology and colours of the flaring observed in the three edge-on S0s of the sample (FCC 153, FCC 170, and FCC 177, see Sect. 5.1) and the presence of a thick disc in FCC 170 (see also Pinna et al 2019), which is in the core of the sub-clump and close to the core of the cluster, could be reconciled with different kinds of interactions. During the infalling of a group in a cluster, the field late-type galaxies could be swept up and interact for a short time with the galaxies in the group before becoming cluster members (Vijayaraghavan & Ricker 2013).…”

Section: The Building-up Of the Fornax Clustermentioning

confidence: 96%

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The Fornax Deep Survey with the VST

Iodice

Spavone

Capaccioli

et al. 2019

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Context. This paper is based on the multi-band (ugri) Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We study bright early-type galaxies (mB ≤ 15 mag) in the 9 square degrees around the core of the Fornax cluster, which covers the virial radius (Rvir ∼ 0.7 Mpc). Aims. The main goal of the present work is to provide an analysis of the light distribution for all galaxies out to unprecedented limits (in radius and surface brightness) and to release the main products resulting from this analysis in all FDS bands. We give an initial comprehensive view of the galaxy structure and evolution as a function of the cluster environment. Methods. From the isophote fit, we derived the azimuthally averaged surface brightness profiles, the position angle, and ellipticity profiles as a function of the semi-major axis. In each band, we derived the total magnitudes, effective radii, integrated colours, and stellar mass-to-light ratios. Results. The long integration times, the arcsec-level angular resolution of OmegaCam at VST, and the large covered area of FDS allow us to map the light and colour distributions out to large galactocentric distances (up to about 10−15 Re) and surface brightness levels beyond μr = 27 mag arcsec−2 (μB ≥ 28 mag arcsec−2). Therefore, the new FDS data allow us to explore in great detail the morphology and structure of cluster galaxies out to the region of the stellar halo. The analysis presented in this paper allows us to study how the structure of galaxies and the stellar population content vary with the distance from the cluster centre. In addition to the intra-cluster features detected in previous FDS works, we found a new faint filament between FCC 143 and FCC 147, suggesting an ongoing interaction. Conclusions. The observations suggest that the Fornax cluster is not completely relaxed inside the virial radius. The bulk of the gravitational interactions between galaxies happens in the W-NW core region of the cluster, where most of the bright early-type galaxies are located and where the intra-cluster baryons (diffuse light and globular clusters) are found. We suggest that the W-NW sub-clump of galaxies results from an infalling group onto the cluster, which has modified the structure of the galaxy outskirts (making asymmetric stellar halos) and has produced the intra-cluster baryons (ICL and GCs), concentrated in this region of the cluster.

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Section: Flaring Of the Discs In The Edge-on S0 Galaxiesmentioning

confidence: 76%

Section: The Building-up Of the Fornax Clustermentioning

confidence: 96%

The Fornax Deep Survey with the VST

Iodice

Spavone

Capaccioli

et al. 2019

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192

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“…These provide two values of [α/Fe], namely 0.00 (solar abundance) and 0.40 (supersolar abundance). While the use of a SSP model library that covers only two values of [α/Fe] is not optimal, pPXF is capable of interpolating between these two values and returns intermediate [α/Fe] enhancements (see also Pinna et al 2019). We note that full-spectral fitting codes are typically measuring an average [α/Fe] ratio.…”

Section: Discussionmentioning

confidence: 99%

Inside-out formation of nuclear discs and the absence of old central spheroids in barred galaxies of the TIMER survey

Bittner

Sánchez‐Blázquez

Gadotti

et al. 2020

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The centres of disc galaxies host a variety of structures built via both internal and external processes. In this study, we constrain the formation and evolution of these central structures, in particular, nuclear rings and nuclear discs, by deriving maps of mean stellar ages, metallicities, and [α/Fe] abundances. We use observations obtained with the MUSE integral-field spectrograph for the TIMER sample of 21 massive barred galaxies. Our results indicate that nuclear discs and nuclear rings are part of the same physical component, with nuclear rings constituting the outer edge of nuclear discs. All nuclear discs in the sample are clearly distinguished based on their stellar population properties. As expected in the picture of bar-driven secular evolution, nuclear discs are younger, more metal-rich, and exhibit lower [α/Fe] enhancements, as compared to their immediate surroundings. Moreover, nuclear discs exhibit well-defined radial gradients, with ages and metallicities decreasing, and [α/Fe] abundances increasing with radius out to the nuclear ring. Often, these gradients show no breaks from the edge of the nuclear disc up through the centre, suggesting that these structures extend to the very centres of galaxies. We argue that continuous (stellar) nuclear discs may form from a series of bar-built (initially gas-rich) nuclear rings that expand in their radius as the bar evolves. In this picture, nuclear rings are simply the (often) star-forming outer edge of nuclear discs. Finally, by combining our results with those taken from a accompanying kinematic study, we do not find evidence for the presence of large, dispersion-dominated components in the centres of these galaxies. This could be a result of quiet merger histories, despite the large galaxy masses, or, perhaps, due to high angular momentum and strong feedback processes preventing the formation of these kinematically hot components.

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“…On the one hand, a clear distinction in age between the thick and the thin disk has been shown in most of the analyzed galaxies (see also Comerón et al 2015). On the other hand, two very old S0 galaxies were found in clusters by Comerón et al (2016) and Pinna et al (2019) (hereafter Paper I, this was the first paper of the series on thick disks within the Fornax 3D project). The thin and thick disks of these two galaxies showed approximately the same age, but a clear difference in their chemical properties unveiled the different origin and evolution of the two disks.…”

Section: Introductionmentioning

confidence: 89%

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

Pinna

Falcón-Barroso

Martig

et al. 2019

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We used deep MUSE observations to perform a stellar-kinematic and population analysis of FCC 153 and FCC 177, two edge-on S0 galaxies in the Fornax cluster. The geometrical definition of the different structural components of these two galaxies allows us to describe the nature of their thick disks. These are both old, relatively metal poor and [Mg/Fe]-enhanced, and their star formation history (SFH) reveals a minor younger component whose chemical properties suggest its later accretion. Moreover, the outer regions of these geometrically defined thick disks show higher values of metallicity and lower values of [Mg/Fe]. These stars probably formed in the thin-disk region and they were dynamically heated to form the flares present in these two galaxies. We propose different formation scenarios for the three populations of these thick disks: in-situ formation, accretion and disk heating. A clear distinction in age is found between the metal poor and [Mg/Fe]-enhanced thick disks (old, ∼ 12 − 13 Gyr), and the metal rich and less [Mg/Fe]-enhanced thin disks (young, ∼ 4 − 5 Gyr). These two galaxies show signs of relatively recent star formation in their thin disks and nuclear regions. While the thin disks show more continuous SFHs, the nuclei display a rather bursty SFH. These two galaxies are located outside of the densest region of the Fornax cluster where FCC 170 resides. This other edge-on S0 galaxy was studied by Pinna et al. (2019). We compare and discuss our results with this previous study. The differences between these three galaxies, at different distances from the cluster center, suggest that the environment can have a strong effect on the galaxy evolutionary path.

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The Fornax 3D project: Unveiling the thick disk origin in FCC 170; possible signs of accretion

Cited by 79 publications

References 126 publications

The Fornax Deep Survey with the VST

The Fornax Deep Survey with the VST

Inside-out formation of nuclear discs and the absence of old central spheroids in barred galaxies of the TIMER survey

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

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