Intracluster Planetary Nebulae in the Virgo Cluster. III. Luminosity of the Intracluster Light and Tests of the Spatial Distribution

Feldmeier, John J.; Ciardullo, Robin; Jacoby, George H.; Durrell, Patrick R.

doi:10.1086/424372

Cited by 119 publications

(184 citation statements)

References 109 publications

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“…(2009) find 7% of diffuse intracluster light (ICL) in the Virgo cluster, while Feldmeier et al (2004) find 15% in Virgo; but Lin & Mohr (2004) find as much as 50% in clusters, suggesting that η strip might be even higher than we found.…”

Section: Tidal Strippingmentioning

confidence: 48%

How do galaxies acquire their mass?

Cattaneo

Mamon

Warnick

et al. 2011

A&A

122

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We study the growth of galaxy masses, via gas accretion and galaxy mergers. We introduce a toy model that describes (in a single equation) how much baryonic mass is accreted and retained into galaxies as a function of halo mass and redshift. In our model, the evolution of the baryons differs from that of the dark matter because 1) gravitational shock heating and AGN jets suppress gas accretion mainly above a critical halo mass of M shock ∼ 10 12 M ; 2) the intergalactic medium after reionisation is too hot for accretion onto haloes with circular velocities v circ < ∼ 40 km s −1 ; 3) stellar feedback drives gas out of haloes, mainly those with v circ < ∼ 120 km s −1 . We run our model on the merger trees of the haloes and sub-haloes of a high-resolution dark matter cosmological simulation. The galaxy mass is taken as the maximum between the mass given by the toy model and the sum of the masses of its progenitors (reduced by tidal stripping). Designed to reproduce the present-day stellar mass function of galaxies, our model matches fairly well the evolution of the cosmic stellar density. It leads to the same z = 0 relation between central galaxy stellar and halo mass as the one found by abundance matching and also as that previously measured at high mass on SDSS centrals. Our model also predicts a bimodal distribution (centrals and satellites) of stellar masses for given halo mass, in very good agreement with SDSS observations. The relative importance of mergers depends strongly on stellar mass (more than on halo mass). Massive galaxies with m stars > m crit ∼ Ω b /Ω m M shock ∼ 10 11 M acquire most of their final mass through mergers (mostly major and gas-poor), as expected from our model's shutdown of gas accretion at high halo masses. However, although our mass resolution should see the effects of mergers down to m stars 10 10.6 h −1 M , we find that mergers are rare for m stars 10 11 h −1 M . This is a consequence of the curvature of the stellar vs. halo mass relation set by the physical processes of our toy model and found with abundance matching. So gas accretion must be the dominant growth mechanism for intermediate and low mass galaxies, including dwarf ellipticals in clusters. The contribution of galaxy mergers terminating in haloes with mass M halo < M shock (thus presumably gas-rich) to the mass buildup of galaxies is small at all masses, but accounts for the bulk of the growth of ellipticals of intermediate mass (∼10 10.5 h −1 M ), which we predict must be the typical mass of ULIRGs.

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Section: Tidal Strippingmentioning

confidence: 48%

How do galaxies acquire their mass?

Cattaneo

Mamon

Warnick

et al. 2011

A&A

122

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“…The remaining fields have areas of 34 × 34 arcmin 2 (Core, RCN1, LSF and LP* fields). The shaded fields indicate the areas surveyed by Feldmeier et al (1998Feldmeier et al ( , 2003Feldmeier et al ( , 2004a; they are designated as F04-n in the text, where n is the number given in the respective shaded area on the figure. fields' position and compare our results with previous works. We discuss the distribution of the ICL from the Virgo core to the outer distant fields at ∼200 = 0.8 Mpc, and its implications for current models for the formation of ICL in clusters, in Sect.…”

Section: Introductionmentioning

confidence: 99%

Intracluster light in the Virgo cluster: large scale distribution

Castro-Rodríguez

Arnaboldi

Aguerri

et al. 2009

A&A

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Aims. The intracluster light (ICL) is a faint diffuse stellar component of clusters made of stars that are not bound to individual galaxies. We have carried out a large scale study of this component in the nearby Virgo cluster. Methods. The diffuse light is traced using planetary nebulae (PNe). The surveyed areas were observed with a narrow-band filter centered on the [OIII]λ5007 Å emission line redshifted to the Virgo cluster distance (the on-band image), and a broad-band filter (the off-band image). For some fields, additional narrow band imaging data corresponding to the Hα emission were also obtained. The PNe are detected in the on-band image due to their strong emission in the [OIII]λ5007 Å line, but disappear in the off-band image. The contribution of Ly-α emitters at z = 3.14 are corrected statistically using blank field surveys, when the Hα image at the field position is not available. Results. We have surveyed a total area of 3.3 square degrees in the Virgo cluster with eleven fields located at different radial distances. Those fields located at smaller radii than 80 arcmin from the cluster center contain most of the detected diffuse light. In this central region of the cluster, the ICL has a surface brightness in the range μ B = 28.8−30 mag arsec −2 , it is not uniformly distributed, and represents about 7% of the total galaxy light in this area. At distances larger than 80 arcmin the ICL is confined to single fields and individual sub-structures, e.g. in the sub-clump B, the M 60/M 59 group. For several fields at 2 and 3 degrees from the Virgo cluster center we set only upper limits. Conclusions. These results indicate that the ICL is not homogeneously distributed in the Virgo core, and it is concentrated in the high density regions of the Virgo cluster, e.g. the cluster core and other sub-structures. Outside these regions, the ICL is confined within areas of ∼100 kpc in size, where tidal effects may be at work. These observational results link the formation of the ICL with the formation history of the most luminous cluster galaxies.

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“…It has been detected either through direct deep imaging (Mihos et al 2005) or using planetary nebulae as stellar light tracers (ICPNe, e.g., Arnaboldi et al 2002;Aguerri et al 2005). In the area around NGC 4472, evidence of ICL has been obtained with PNe by Feldmeier et al (2004) (see also Castro-Rodriguéz et al 2009 for a summary of ICPNe observations over a range of Virgo cluster-centric distances). However, none of these studies has addressed a detailed 2D distribution of the ICL around NGC 4472 and its connection with the giant galaxy.…”

Section: Discussionmentioning

confidence: 99%

VEGAS: A VST Early-type GAlaxy Survey

Capaccioli

Spavone

Grado

et al. 2015

A&A

141

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Context. We present the VST Early-type GAlaxy Survey (VEGAS), which is designed to obtain deep multiband photometry in g, r, i, of about one hundred nearby galaxies down to 27.3, 26.8, and 26 mag/arcsec 2 respectively, using the ESO facility VST/OmegaCAM. Aims. The goals of the survey are 1) to map the light distribution up to ten effective radii, r e ; 2) to trace color gradients and surface brightness fluctuation gradients out to a few r e for stellar population characterization; and 3) to obtain a full census of the satellite systems (globular clusters and dwarf galaxies) out to 20% of the galaxy virial radius. The external regions of galaxies retain signatures of the formation and evolution mechanisms that shaped them, and the study of nearby objects enables a detailed analysis of their morphology and interaction features. To clarify the complex variety of formation mechanisms of early-type galaxies (ETGs), wide and deep photometry is the primary observational step, which at the moment has been pursued with only a few dedicated programs. The VEGAS survey has been designated to provide these data for a volume-limited sample with exceptional image quality. Methods. In this commissioning photometric paper we illustrate the capabilities of the survey using g-and i-band VST/OmegaCAM images of the nearby galaxy NGC 4472 and of smaller ETGs in the surrounding field. Results. Our surface brightness profiles reach rather faint levels and agree excellently well with previous literature. Genuine new results concern the detection of an intracluster light tail in NGC 4472 and of various substructures at increasing scales. We have also produced extended (g − i) color profiles. Conclusions. The VST/OmegaCAM data that we acquire in the context of the VEGAS survey provide a detailed view of substructures in the optical emission from extended galaxies, which can be as faint as a hundred times below the sky level.

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Intracluster Planetary Nebulae in the Virgo Cluster. III. Luminosity of the Intracluster Light and Tests of the Spatial Distribution

Cited by 119 publications

References 109 publications

How do galaxies acquire their mass?

How do galaxies acquire their mass?

Intracluster light in the Virgo cluster: large scale distribution

VEGAS: A VST Early-type GAlaxy Survey

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