VEGAS-SSS. A VST early-type galaxy survey: analysis of small stellar systems

Cantiello, M.; Capaccioli, M.; Napolitano, N. R.; Grado, A.; Limatola, L.; Paolillo, M.; Iodice, E.; Romanowsky, Aaron J.; Forbes, Duncan A.; Raimondo, Gabriella; Spavone, M.; Barbera, F. La; Puzia, Thomas H.; Schipani, P.

doi:10.1051/0004-6361/201425165

Cited by 25 publications

(41 citation statements)

References 97 publications

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“…As hypothesized in their paper, this could mean they either detected a single offset black hole, or an inspiralling black hole offset from another at the galaxy center, or that there is simply a single black hole at the galaxy center and the offset emission de- Figure 2. VLA image of Stokes I emission near 10 GHz centered on a background source with a X-ray counterpart (Lin et al 2015) and an ugi counterpart (Cantiello et al 2015(Cantiello et al , 2018. The symbols encode the counterpart positions and their errors at the 95% confidence level.…”

Section: Ghz Measurement Resultsmentioning

confidence: 99%

Investigating the Candidate Displaced Active Galactic Nucleus in NGC 3115

Jones

Burke-Spolaor

Nyland

et al. 2019

ApJ

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The nearby galaxy NGC 3115 contains a known radio-emitting, low-luminosity active galactic nucleus (AGN), and was recently claimed to host a candidate AGN displaced 14.3 pc from the galaxy's optical photocenter. Our goal is to understand whether this represents a single offset AGN, an AGN in orbit around a central black hole, or something else. We present a new, sensitive (RMS = 4.4 µJy beam −1 ) 10 GHz image, which finds evidence for only one AGN. We place a stringent limit on the radio luminosity of any secondary supermassive black hole of L 10 GHz < 5.8 × 10 33 ergs/s. An analysis of the relative positioning of the radio core, X-ray nucleus, and stellar bulge in this galaxy indicate that the radio source is centrally located, and not offset from the galactic bulge. This provides an argument against a single offset AGN in NGC 3115, however does not provide conclusive evidence against the purported offset AGN as an in-spiralling secondary black hole.

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Section: Ghz Measurement Resultsmentioning

confidence: 99%

Investigating the Candidate Displaced Active Galactic Nucleus in NGC 3115

Jones

Burke-Spolaor

Nyland

et al. 2019

ApJ

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“…For galaxies in the local universe ( 30 Mpc), the properties of the stellar halos can also be addressed using discrete tracers such as globular clusters (GCs) and planetary nebulae (PNe). Observations show that the red GC populations have numberdensity profiles consistent with that of the stars in the parent galaxy, while the blue GCs are spatially more extended in the intracluster space and trace the metal-poor component of the halo (Forbes et al 2012;Pota et al 2013;Durrell et al 2014;Cantiello et al 2015;Hilker et al 2015). In the Hydra cluster, the location of blue GCs coincides with a group of dwarf galaxies under disruption, suggesting a young stellar halo that is still forming (Arnaboldi et al 2012;Hilker et al 2015).…”

Section: Introductionmentioning

confidence: 86%

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

164

335

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We have started a new, deep multi-imaging survey of the Fornax cluster, dubbed the Fornax Deep Survey (FDS), at the VLT Survey Telescope (VST). In this paper we present the deep photometry inside two square degrees around the bright galaxy NGC1399 in the core of the cluster. We found that the core of the Fornax cluster is characterized by a very extended and diffuse envelope surrounding the luminous galaxy NGC1399: we map the surface brightness out to 33 arcmin (∼192 kpc) from the galaxy center and down to μ g ∼31 mag arcsec −2 in the g band. The deep photometry allows us to detect a faint stellar bridge in the intracluster region on the west side of NGC1399 and toward NGC1387. By analyzing the integrated colors of this feature, we argue that it could be due to the ongoing interaction between the two galaxies, where the outer envelope of NGC1387 on its east side is stripped away. By fitting the light profile, we found that there exists a physical break radius in the total light distribution at R=10 arcmin (∼58 kpc) that sets the transition region between the bright central galaxy and the outer exponential halo, and that the stellar halo contributes 60% of the total light of the galaxy (Section 3.5). We discuss the main implications of this work on the build-up of the stellar halo at the center of the Fornax cluster. By comparing with the numerical simulations of the stellar halo formation for the most massive bright cluster galaxies (i.e., M M 13 log 14, we find that the observed stellar halo mass fraction is consistent with a halo formed through the multiple accretion of progenitors with stellar mass in the range 10 8 -10 11 M e . This might suggest that the halo of NGC1399 has also gone through a major merging event. The absence of a significant number of luminous stellar streams and tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early formation epoch. Therefore, different from the Virgo cluster, the extended stellar halo around NGC1399 is characterized by a more diffuse and well-mixed component, including the intracluster light.

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“…The spatial resolution of VST/OmegaCam is insufficient to resolve the typical half-light radii of GCs with r h < 10 pc (Masters et al 2010;Puzia et al 2014). Although the size of UCDs with r h > 20 pc can be resolved using our imaging data (Cantiello et al 2015), measuring UCD sizes is not the focus of this paper and will be deferred to a future work. It is established that a sharp magnitude cut cannot perfectly separate UCDs from GCs.…”

Section: Classification Of Fornax Objectsmentioning

confidence: 99%

The Fornax Cluster VLT Spectroscopic Survey – I. VIMOS spectroscopy of compact stellar systems in the Fornax core region

Pota

Napolitano

Hilker

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the results of a wide spectroscopic survey aimed at detecting extragalactic globular clusters (GCs) in the core of the Fornax cluster. About 4500 low resolution spectra (from 4800 to 10000Å) were observed in 25 VLT/VIMOS masks covering the central 1 deg 2 around the dominant galaxy NGC 1399 corresponding to ∼175 kpc galactocentric radius. We describe the methodology used for data reduction and data analysis. We found a total of 387 unique physical objects (372 GCs and 15 ultra compact dwarfs) in the field covered by our observations. Most of these objects are associated with NGC 1399, with only 10% likely belonging to other giant galaxies. The new VIMOS dataset is complementary to the many GC catalogues already present in the literature and it brings the total number of tracer particles around NGC 1399 to more than 1130 objects. With this comprehensive radial velocity sample we have found that the velocity dispersion of the GC population (equally for red and blue GC populations) shows a relatively sharp increase from low velocity dispersion (∼ 250 − 350 km s −1 ) to high velocity dispersion (∼ 300 − 400 km s −1 ) at projected radius of ≈ 10 arcmin (∼ 60 kpc) from the galaxy centre. This suggests that at a projected radius of ≈ 60 kpc both blue and red GC populations begin to be governed by the dominating Fornax cluster potential, rather than by the central NGC 1399 galaxy potential. This kinematic evidence corroborates similar results found using surface brightness analysis and planetary nebulae kinematics.

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VEGAS-SSS. A VST early-type galaxy survey: analysis of small stellar systems

Cited by 25 publications

References 97 publications

Investigating the Candidate Displaced Active Galactic Nucleus in NGC 3115

Investigating the Candidate Displaced Active Galactic Nucleus in NGC 3115

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

The Fornax Cluster VLT Spectroscopic Survey – I. VIMOS spectroscopy of compact stellar systems in the Fornax core region

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