The luminosity function of the Virgo Cluster from MB=-22 to −11

Trentham, Neil; Hodgkin, S. T.

doi:10.1046/j.1365-8711.2002.05440.x

Cited by 102 publications

(189 citation statements)

References 67 publications

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“…The vertical dotted line is the completeness limit of this work. Trentham & Hodgkin 2002). In conclusion, the observed differences in the LFs do not seem to be related to the mass distribution of the systems in the four subsamples.…”

Section: Caveats Of the Resultsmentioning

confidence: 63%

Fossil group origins

Zarattini

Aguerri

Sánchéz-Janssen

et al. 2015

A&A

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Context. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm 12 ). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found among the so-called fossil systems. The observed distribution of magnitude gaps is thought to be a consequence of the orbital decay of M * galaxies in massive halos and the associated growth of the central object. As a result, to first order the amplitude of this gap is a good statistical proxy for the dynamical age of a system of galaxies. Fossil and non-fossil systems could therefore have different galaxy populations that should be reflected in their luminosity functions. Aims. In this work we study, for the first time, the dependence of the luminosity function parameters on Δm 12 using data obtained by the fossil group origins (FOGO) project. Methods. We constructed a hybrid luminosity function for 102 groups and clusters at z ≤ 0.25 using both photometric data from the SDSS-DR7 and redshifts from the DR7 and the FOGO surveys. The latter consists of ∼1200 new redshifts in 34 fossil system candidates. We stacked all the individual luminosity functions, dividing them into bins of Δm 12 , and studied their best-fit Schechter parameters. We additionally computed a "relative" luminosity function, expressed as a function of the central galaxy luminosity, which boosts our capacity to detect differences -especially at the bright end. Results. We find trends as a function of Δm 12 at both the bright and faint ends of the luminosity function. In particular, at the bright end, the larger the magnitude gap, the fainter the characteristic magnitude M * . The characteristic luminosity in systems with negligible gaps is more than a factor three brighter than in fossil-like ones. Remarkably, we also find differences at the faint end. In this region, the larger the gap, the flatter the faint-end slope α. Conclusions. The differences found at the bright end support a dissipationless, dynamical friction-driven merging model for the growth of the central galaxy in group-and cluster-sized halos. The differences in the faint end cannot be explained by this mechanism. Other processes -such as enhanced tidal disruption due to early infall and/or prevalence of eccentric orbits -may play a role. However, a larger sample of systems with Δm 12 > 1.5 is needed to establish the differences at the faint end.

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Section: Caveats Of the Resultsmentioning

confidence: 63%

Fossil group origins

Zarattini

Aguerri

Sánchéz-Janssen

et al. 2015

A&A

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“…If we assume that the luminosity function of our clusters are similar to that measured in Virgo by Trentham & Hodgkin (2002), we find that at most 2% of the cluster luminosity can be lost in this way. Similarly, from spectroscopic observations of cluster galaxies at similar redshifts, Wilson et al (1997) estimate the contamination rate for bright galaxies to be no higher than 25% over the entire cluster, and it is likely to be significantly smaller in the cluster core.…”

Section: Isophotal Measurementsmentioning

confidence: 59%

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Feldmeier¹,

Mihos²,

Morrison³

et al. 2004

ApJ

132

150

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We report the search for intracluster light in four Abell type II-III (non-cD) galaxy clusters: A801, A1234, A1553, and A1914. We find that on average these clusters contain $10% of their detected stellar luminosity in a diffuse component. We show that for two of the clusters the intracluster light closely follows the galaxy distribution, but in the other two cases, there are noticeable differences between the spatial distribution of the galaxies and the intracluster light. We report the results of a search for intracluster tidal debris in each cluster and note that A1914 in particular has a number of strong tidal features likely due to its status as a recent cluster merger. One of the A1914 features appears to be spatially coincident with an extension seen in weak lensing maps, implying that the feature traces a large amount of mass. We compare these results with numerical simulations of hierarchically formed galaxy clusters and find good general agreement between the observed and simulated images, although we also find that our observations sample only the brightest features of the intracluster light. Together, these results suggest that intracluster light can be a valuable tool in determining the evolutionary state of galaxy clusters.

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“…For example the more extensive Coma survey by Mobasher et al (2004) recovers a flat and invariant LD/LF (α = −1) to M B ≈ −14 mag. The phenomena of an upturn in the LD has also been seen in Virgo (Impey & Bothun 1988;Trentham & Hodgkin 2002), A963 (Driver et al 1994), A868 , A2554 (Smith et al 1997), and A2218 (Pracey et al 2004) for example. However, apart from these 'active' core environments, the overall LDs from the field, to the local group, to the local…”

Section: Introductionmentioning

confidence: 87%

Beyond the Galaxy Luminosity Function

Driver¹

2004

Publ. – Astron. Soc. Aust

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Abstract:With the advent of large-scale surveys (i.e. Legacy Surveys) it is now possible to start looking beyond the galaxy luminosity function (LF) to more detailed statistical representations of the galaxy population, i.e multivariate distributions. In this review I first summarise the current state-of-play of the B-band global and cluster LFs and then briefly present two promising bivariate distributions: the luminosity-surface brightness plane (LSP) and the colour-luminosity plane (CLP). In both planes galaxy bulges and galaxy disks form marginally overlapping but distinct distributions, indicating two key formation/evolutionary processes (presumably merger and accretion). Forward progress in this subject now requires the routine application of reliable bulge-disk decomposition codes to allow independent investigation of these two key components.

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The luminosity function of the Virgo Cluster from MB=-22 to −11

Abstract: We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes MB=‐22 and −11 from wide‐field charge‐coupled device (CCD) imaging data. The LF is only gradually rising for ‐22 Show more

Cited by 102 publications

References 67 publications

Fossil group origins

Fossil group origins

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Beyond the Galaxy Luminosity Function

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