Optical Mass Estimates of Galaxy Clusters

Girardi, M.; Giuricin, G.; Mardirossian, F.; Mezzetti, M.; Boschin, W.

doi:10.1086/306157

Cited by 359 publications

(584 citation statements)

References 141 publications

(107 reference statements)

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“…The procedure is repeated until there are no more interlopers and the list of members is used to estimate cluster properties. We perform virial analysis in an analogous way to Girardi et al (1998), Popesso et al (2005), Biviano et al (2006) and Popesso et al (2007). First, we compute the robust aperture velocity dispersion (σap) of the cluster depending on the number of members available: gapper (< 15) or bi-weight ( 15, Beers et al 1990).…”

Section: Num (Mamon; Phase Space Richness)mentioning

confidence: 99%

“…First, we compute the robust aperture velocity dispersion (σap) of the cluster depending on the number of members available: gapper (< 15) or bi-weight ( 15, Beers et al 1990). Then, σap is corrected for redshift errors (Danese et al 1980) and an estimate of virial radius is obtained following Girardi et al (1998). These steps lead us to an initial virial mass estimate (equation 5 of Girardi et al 1998), which is then corrected for the surface pressure term (The & White 1986).…”

Section: Num (Mamon; Phase Space Richness)mentioning

confidence: 99%

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Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M 200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ∼1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under-or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used.

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Section: Num (Mamon; Phase Space Richness)mentioning

confidence: 99%

Section: Num (Mamon; Phase Space Richness)mentioning

confidence: 99%

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…i j is the projected virial radius and R i j are the projected distances between each pair of the N = 39 galaxies (Heisler et al 1985;Girardi et al 1998). For the sole purpose of displaying the morphology of the density field we show, in Fig.…”

Section: Galaxy Clusters In the Chandra Deep Field Southmentioning

confidence: 99%

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

Trèvese

Castellano

Fontana

et al. 2006

A&A

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Aims. We study galaxy clustering and explore the dependence of galaxy properties on the the environment up to a redshift z ∼ 1, on the basis of a deep multi-band survey in the Chandra Deep Field South. Methods. We have developed a new method which combines galaxy angular positions and photometric redshifts to estimate the local galaxy number-density. This allows both the detection of overdensities in the galaxy distribution and the study of the properties of the galaxy population as a function of the environmental density. Results. We detect two moderate overdensities at z ∼ 0.7 and z ∼ 1 previously identified spectroscopically. We find that the fraction of red galaxies within each structure increases with volume density, extending to z ∼ 1 previous results. We measure "red sequence" slopes consistent with the values found in X-ray selected clusters, supporting the notion that the mass-metallicity relation hold constant up to z ∼ 1. Conclusions. Our method based on photometric redshifts allows to extend structure detection and density estimates up to the limits of photometric surveys, i.e. considerably deeper than spectroscopic surveys. Since X-ray cluster detection at high redshift is presently limited to massive relaxed structures, galaxy volume density based on photometric redshift appears as a valuable tool in the study of galaxy evolution.

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“…• 72). Optical studies of the galaxy members within A3667 (Proust et al 1988;Sodre et al 1992;Girardi et al 1996Girardi et al , 1998Johnston-Hollitt, Hunstead & Corbett 2008;Owers, Couch & Nulsen 2009) have revealed that A3667 is relatively nearby with an average redshift of z = 0.0553 (Owers et al 2009). Optical observations have also revealed a high galaxy density within A3667, with an elongated spatial distribution of galaxies in the south-east (SE) to north-west (NW) direction.…”

mentioning

confidence: 99%

The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

Hindson¹,

Johnston‐Hollitt²,

Hurley‐Walker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present the first Murchison Widefield Array observations of the well-known cluster of galaxies Abell 3667 (A3667) between 105 and 241 MHz. A3667 is one of the best known examples of a galaxy cluster hosting a double radio relic and has been reported to contain a faint radio halo and bridge. The origin of radio haloes, relics and bridges is still unclear, however galaxy cluster merger seems to be an important factor. We clearly detect the north-west (NW) and south-east radio relics in A3667 and find an integrated flux density at 149 MHz of 28.1 ± 1.7 and 2.4 ± 0.1 Jy, respectively, with an average spectral index, between 120 and 1400 MHz, of −0.9 ± 0.1 for both relics. We find evidence of a spatial variation in the spectral index across the NW relic steepening towards the centre of the cluster, which indicates an ageing electron population. These properties are consistent with higher frequency observations. We detect emission that could be associated with a radio halo and bridge. However, due to the presence of poorly sampled large-scale Galactic emission and blended point sources we are unable to verify the exact nature of these features.

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Optical Mass Estimates of Galaxy Clusters

Cited by 359 publications

References 141 publications

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

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