The Next Generation Virgo Cluster Survey (Ngvs). I. Introduction To
                    the Survey*

Ferrarese, Laura; Côté, Patrick; Cuillandre, Jean-Charles; Gwyn, Stephen; Peng, Eric W.; MacArthur, Lauren A.; Duc, Pierre–Alain; Boselli, A.; Mei, S.; Erben, T.; McConnachie, Alan W.; Durrell, Patrick R.; Mihos, J. Christopher; Jordán, Andrés; Lançon, A.; Puzia, Thomas H.; Emsellem, Éric; Balogh, Michael L.; Blakeslee, John P.; Waerbeke, Ludovic Van; Gavazzi, R.; Vollmer, B.; Kavelaars, J. J.; Woods, David; Ball, Nicholas M.; Boissier, S.; Courteau, Stéphane; Ferriere, Etienne; Gavazzi, G.; Hildebrandt, Hendrik; Hudelot, P.; Huertas-Company, M.; Liu, Chengze; McLaughlin, Dean E.; Mellier, Y.; Milkeraitis, Martha; Schade, David; Balkowski, C.; Bournaud, F.; Carlberg, R. G.; Chapman, Scott; Hoekstra, Henk; Peng, Chien Y.; Sawicki, Marcin; Simard, Luc; Taylor, James E.; Tully, R. Brent; Driel, W. van; Wilson, C. D.; Burdullis, Todd; Mahoney, Billy; Manset, N.

doi:10.1088/0067-0049/200/1/4

Cited by 344 publications

(351 citation statements)

References 381 publications

(486 reference statements)

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“…Observations were obtained by using a step-dither observing sequence, consisting of a cycle of short exposures, one centered on the core of the Fornax cluster and others on three adjacent fields all around it (Δ=±1°) on the SW and NW sides. This approach, already adopted in other photometric surveys (Ferrarese et al 2012), allows a very accurate estimate of the sky background around bright and extended galaxies.…”

Section: Observations Data Reduction and Analysismentioning

confidence: 99%

“…In the recent years, a big effort has been made to develop deep photometric surveys aimed at studying galaxy structures up to the faintest levels of surface brightness, which reveal lowluminosity structures and trace the stellar halos at very large distances from the galaxy center (Mihos et al 2005;Janowiecki et al 2010;Martínez-Delgado et al 2010;Roediger et al 2011;Ferrarese et al 2012;van Dokkum et al 2014;Duc et al 2015;Muñoz et al 2015;Trujillo & Fliri 2015). Recently, deep images of the Virgo cluster have revealed several faint (μ V =26-29 mag arcsec −2 ) streams of ICL among the galaxy members and made it possible to map the stellar halos of the bright cluster galaxies (BCGs) at very large distances from the center (Janowiecki et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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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

165

342

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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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Section: Observations Data Reduction and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

165

342

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show abstract

“…Their projected distances to M87 are between 0°.88, 0°.89, and 2°. 76, respectively (the virial radius of the Virgo cluster, considering M87 at its center, is R 200 =5°.38=1.55 Mpc; Ferrarese et al 2012).…”

Section: Globular Cluster Systems Of Vcc1539 Vcc1545 and Vcc1861mentioning

confidence: 99%

“…The GCs targeted are selected from the Next Generation Virgo Cluster Survey (NGVS; Ferrarese et al 2012) and from the ACS Virgo Cluster Survey (ACSVCS; Peng et al 2006;Jordán et al 2009). The NGVS is a ∼900 hr program carried out at the Canada-France-Hawaii Telescope (CFHT) between the years 2008 and 2013.…”

Section: Introductionmentioning

confidence: 99%

The Next Generation Virgo Cluster Survey Xvi: The Angular Momentum of Dwarf Early-Type Galaxies From Globular Cluster Satellites

Toloba

Guhathakurta

et al. 2016

ApJ

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We analyze the kinematics of six Virgo cluster dwarf early-type galaxies (dEs) from their globular cluster (GC) systems. We present new Keck/DEIMOS spectroscopy for three of them and re-analyze the data found in the literature for the remaining three. We use two independent methods to estimate the rotation amplitude (V rot ) and velocity dispersion (σ GC ) of the GC systems and evaluate their statistical significance by simulating non-rotating GC systems with the same number of GC satellites and velocity uncertainties. Our measured kinematics agree with the published values for the three galaxies from the literature and, in all cases, some rotation is measured. However, our simulations show that the null hypothesis of being non-rotating GC systems cannot be ruled out. In the case of VCC1861, the measured V rot and the simulations indicate that it is not rotating. In the case of VCC1528, the null hypothesis can be marginally ruled out, and thus it might be rotating although further confirmation is needed. In our analysis, we find that, in general, the measured V rot tends to be overestimated and the measured σ GC tends to be underestimated by amounts that depend on the intrinsic V rot /σ GC , the number of observed GCs (N GC ), and the velocity uncertainties. The bias is negligible when N GC  20. In those cases where a large N GC is not available, it is imperative to obtain data with small velocity uncertainties. For instance, errors of 2 km s −1 lead to V rot < 10 km s −1 for a system that is intrinsically not rotating.

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“…Mihos et al 2005;van Dokkum et al 2014), extremely long exposures on small telescopes (e.g. Martínez-Delgado et al 2010), or LSB-optimized surveys, such as the Next Generation Virgo Cluster Survey (NGVS, Ferrarese et al 2012), or the MegaCam component of the ATLAS 3D project (Duc et al 2014), to be completed thanks to the MATLAS CFHT Large Programme. Fig.…”

Section: Introductionmentioning

confidence: 99%

Applying galactic archeology to massive galaxies using deep imaging surveys

Duc

2014

Proc. IAU

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Abstract. Various programs aimed at exploring the still largely unknown low surface brightness Universe with deep imaging optical surveys have recently started. They open a new window for studies of galaxy evolution, pushing the technique of galactic archeology outside the Local Group (LG). The method, based on the detection and analysis of the diffuse light emitted by collisional debris or extended stellar halos (rather than on stellar counts as done for LG systems), faces however a number of technical difficulties, like the contamination of the images by reflection halos and Galactic cirrus. I review here the on-going efforts to address them and highlight the preliminary promising results obtained with a systematic survey with MegaCam on the CFHT of nearby massive early-type galaxies done as part of the ATLAS 3D , NGVS and MATLAS collaborations.

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The Next Generation Virgo Cluster Survey (Ngvs). I. Introduction To the Survey*

Cited by 344 publications

References 381 publications

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

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

The Next Generation Virgo Cluster Survey Xvi: The Angular Momentum of Dwarf Early-Type Galaxies From Globular Cluster Satellites

Applying galactic archeology to massive galaxies using deep imaging surveys

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