The Acs Fornax Cluster Survey. Vi. The Nuclei of Early-Type Galaxies in the Fornax Cluster

Turner, Monica L.; Côté, Patrick; Ferrarese, Laura; Jordán, Andrés; Blakeslee, John P.; Mei, S.; Peng, Eric W.; West, Michael J.

doi:10.1088/0067-0049/203/1/5

Cited by 142 publications

(282 citation statements)

References 205 publications

(224 reference statements)

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“…Observationally, a NSC in a galactic nucleus is identified as an evident edge in the host galaxy surface brightness profile Turner et al 2012;Georgiev & Böker 2014;Arca-Sedda et al 2015). However, we did not found any evident edge neither in our model surface density profile, nor in the projected radial velocity profile, which is shown in Fig.…”

Section: Dynamical Friction and Tidal Disruptioncontrasting

confidence: 52%

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

Sedda

Capuzzo-Dolcetta

2017

Monthly Notices of the Royal Astronomical Society

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We investigated the evolution of a massive galactic nucleus hosting a super-massive black hole (SMBH) with mass M SMBH = 10 8 M ⊙ surrounded by a population of 42 heavy star clusters (GCs). Using direct N -body modelling, we show here that the assembly of an NSC through GCs orbital decay and merger is efficiently inhibited by the tidal forces exerted from the SMBH. The GCs mass loss induced by tidal forces causes a significant modification of their mass function, leading to a population of low-mass (< 10 4 ) clusters. Nonetheless, the GCs debris accumulated around the SMBH give rise to well-defined kinematical and morphological properties, leading to the formation of a disk-like structure. Interestingly, the disk is similar to the one observed in the M31 galaxy nucleus, which has properties similar to our numerical model. The simulation produced a huge amount of data, which we used to investigate whether the GC debris deposited around the SMBH can enhance the rate of tidal disruption events (TDEs) in our galaxy inner density distribution. Our results suggest that the GCs disruption shapes the SMBH neighbourhoods leading to a TDE rate of ∼ 2 × 10 −4 yr −1 , a value slightly larger than what expected in previous theoretical modelling of galaxies with similar density profiles and central SMBHs. The simulation presented here is the first of its kind, representing a massive galactic nucleus and its star cluster population on scales ∼ 100 pc.

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Section: Dynamical Friction and Tidal Disruptioncontrasting

confidence: 52%

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

Sedda

Capuzzo-Dolcetta

2017

Monthly Notices of the Royal Astronomical Society

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“…The estimate of the number of galaxies hosting a NSC is ∼70% Turner et al 2012). It turns out therefore that the future facilities like E-ELT and TMT -that together are able to cover the whole sky-will provide the fundamental data to unveil the mechanisms of formation of the nuclear clusters of galaxies.…”

Section: Discussionmentioning

confidence: 99%

“…NSCs in spheroidal galaxies has been studied by Côté et al (2006) and Turner et al (2012). NSCs are 3−4 mag (Georgiev & Böker 2014) more luminous than Milky Way globular clusters, but they share similar sizes (a few parsecs, see e.g.…”

Section: Introductionmentioning

confidence: 99%

Probing the nuclear star cluster of galaxies with extremely large telescopes

Gullieuszik

Greggio

Falomo

et al. 2014

A&A

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The unprecedented sensitivity and spatial resolution of next-generation, ground-based, extremely large telescopes (ELTs) will open a completely new window on the study of resolved stellar populations. In this paper we study the feasibility of the analysis of nuclear star cluster (NSC) stellar populations with ELTs. To date, NSC stellar population studies are based on the properties of their integrated light. NSCs are in fact observed as unresolved sources even with the HST. We explore the possibility of obtaining direct estimates of the age of NSC stellar populations from the photometry of main-sequence turn-off stars. We simulated ELT observations of NSCs at different distances and with different stellar populations. Photometric measurements on each simulated image were analysed in detail and results about photometric accuracy and completeness are reported here. We found that the main-sequence turn-off is detectableand therefore the age of stellar populations can be directly estimated -up to 2 Mpc for old, up to 3 Mpc for intermediate-age and up to 4−5 Mpc for young stellar populations. We found that for this particular science case, the performances of TMT and E-ELT are of comparable quality.

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“…From photometric analysis, NGC 1396 also contains a distinct nuclear star cluster (NSC) component. With an effective (half-light) radius in the g-and z-bands of 0.047±0.003, this NSC accounts for a ∼ 1% contribution to the luminosity profile of the galaxy outside of 0.5 arcsec (Turner et al 2012). It is therefore not possible to study the properties of the NSC using ground based data, without adaptive optics assistance.…”

Section: General Properties Of Ngc 1396mentioning

confidence: 99%

Abundance ratios and IMF slopes in the dwarf elliptical galaxy NGC 1396 with MUSE

Mentz¹,

Barbera²,

Peletier³

et al. 2016

Mon. Not. R. Astron. Soc.

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Deep observations of the dwarf elliptical (dE) galaxy NGC 1396 (M V = −16.60, Mass ∼ 4 × 10 8 M ), located in the Fornax cluster, have been performed with the VLT/ MUSE spectrograph in the wavelength region from 4750 − 9350 Å. In this paper we present a stellar population analysis studying chemical abundances, the star formation history (SFH) and the stellar initial mass function (IMF) as a function of galacto-centric distance. Different, independent ways to analyse the stellar populations result in a luminosity-weighted age of ∼ 6 Gyr and a metallicity [Fe/H]∼ −0.4, similar to other dEs of similar mass. We find unusually overabundant values of [Ca/Fe] ∼ +0.1, and under-abundant Sodium, with [Na/Fe] values around −0.1, while [Mg/Fe] is overabundant at all radii, increasing from ∼ +0.1 in the centre to ∼ +0.2 dex. We notice a significant metallicity and age gradient within this dwarf galaxy.To constrain the stellar IMF of NGC 1396, we find that the IMF of NGC 1396 is consistent with either a Kroupa-like or a top-heavy distribution, while a bottom-heavy IMF is firmly ruled out.An analysis of the abundance ratios, and a comparison with galaxies in the Local Group, shows that the chemical enrichment history of NGC 1396 is similar to the Galactic disc, with an extended star formation history. This would be the case if the galaxy originated from a LMC-sized dwarf galaxy progenitor, which would lose its gas while falling into the Fornax cluster.

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The Acs Fornax Cluster Survey. Vi. The Nuclei of Early-Type Galaxies in the Fornax Cluster

Cited by 142 publications

References 205 publications

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

Probing the nuclear star cluster of galaxies with extremely large telescopes

Abundance ratios and IMF slopes in the dwarf elliptical galaxy NGC 1396 with MUSE

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