Making the observational parsimonious richness a working mass proxy

Andreon, S.

doi:10.1051/0004-6361/201526081

Cited by 25 publications

(49 citation statements)

References 48 publications

(75 reference statements)

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“…This 0.02 dex intrinsic scatter in mass is comparable to or better than the values derived for other proxies, such as the integrated pressure Y SZ or pseudo pressure Y X , X-ray luminosity L X , gas mass M gas , and stellar mass (Andreon 2015 (Andreon 2015), and L X (Andreon & Hurn 2010). We note that Eq.…”

Section: Introductionsupporting

confidence: 75%

“…2 for the two example clusters. Andreon (2015) showed that results do not change when using another number of iterations because convergence is achieved earlier, whereas in Sect. 4 we show that the starting position does not matter when using duplicate clusters (objects with center offsets larger than 3 arcmin in different cluster catalogs, and therefore listed twice in our initial list of clusters to be analyzed).…”

Section: Cluster Sample and Derivation Of Cluster Richness And Massmentioning

confidence: 96%

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Richness-based masses of rich and famous galaxy clusters

Andreon¹

2016

A&A

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We present a catalog of galaxy cluster masses derived by exploiting the tight correlation between mass and richness, i.e., a properly computed number of bright cluster galaxies. The richness definition adopted in this work is properly calibrated, shows a small scatter with mass, and has a known evolution, which means that we can estimate accurate (0.16 dex) masses more precisely than by adopting any other richness estimates or X-ray or SZ-based proxies based on survey data. We measured a few hundred galaxy clusters at 0.05 < z < 0.22 in the low-extinction part of the Sloan Digital Sky Survey footprint that are in the 2015 catalog of Planck-detected clusters, that have a known X-ray emission, that are in the Abell catalog, or that are among the most most cited in the literature. Diagnostic plots and direct images of clusters are individually inspected and we improved cluster centers and, when needed, we revised redshifts. Whenever possible, we also checked for indications of contamination from other clusters on the line of sight, and found ten such cases. All this information, with the derived cluster mass values, are included in the distributed value-added cluster catalog of the 275 clusters with a derived mass larger than 10 14 M . Finally, in a technical appendix we illustrate with Planck clusters how to minimize the sensitivity of comparisons between masses listed in different catalogs to the specific overlapping of the considerd subsamples, a problem recognized but not solved in the literature.

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Section: Introductionsupporting

confidence: 75%

Section: Cluster Sample and Derivation Of Cluster Richness And Massmentioning

confidence: 96%

Richness-based masses of rich and famous galaxy clusters

Andreon¹

2016

A&A

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“…The large variety is indirectly confirmed by Andreon & Moretti (2011), who observed a 0.5 dex scatter at a given richness, which is known to be a low scatter proxy of mass (e.g., Andreon & Hurn 2010;Andreon 2015). That sample, however, lacks direct measurements of mass.…”

Section: X-ray Luminosity Vs Massesmentioning

confidence: 79%

“…Observations also indicate that caustic masses cannot be much noisier than their quoted error (i.e., cannot have have understimated errors) because they correlate with almost no scatter with richness (Andreon 2015), which in turns correlates with almost no scatter with weak-lensing mass (Andreon & Congdon 2014). This latter correlation adopts fixed-aperture masses and, therefore, the source of the tight relation cannot be an effect introduced using mass-related apertures such as r 200 .…”

Section: Is Variety Due To Wrong Cluster Masses?mentioning

confidence: 96%

The amazing diversity in the hot gas content of an X-ray unbiased massive galaxy clusters sample

Andreon

Serra

Moretti

et al. 2016

A&A

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We aim to determine the intrinsic variety, at a given mass, of the properties of the intracluster medium in clusters of galaxies. This requires a cluster sample selected independently of the intracluster medium content for which reliable masses and subsequent X-ray data can be obtained. We present one such sample, consisting of 34 galaxy clusters selected independently of their X-ray properties in the nearby (0.050 < z < 0.135) Universe and mostly with 14 < log M 500 /M 14.5, where masses are dynamically estimated. We collected the available X-ray observations from the archives and then observed the remaining clusters with the low-background Swift X-ray telescope, which is extremely useful for sampling a cluster population expected to have low surface brightness. We found that clusters display a large range (up to a factor 50) in X-ray luminosities within r 500 at a given mass, whether or not the central emission (r < 0.15r 500 ) is excised, unveiling a wider cluster population than seen in Sunayev-Zeldovich surveys or inferred from the population seen in X-ray surveys. The measured dispersion is 0.5 dex in L X at a given mass.

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“…membership_paper_AA_corrected_for_editing_after_proofs (2015); Saro et al (2015); Bocquet et al (2016). The cluster richness is also used as independent cluster mass proxy (e.g., Andreon 2015). Robust membership assignments can be exploited to estimate the richness ; however, the correct identification of both field sources and cluster members is needed.…”

Section: Introductionmentioning

confidence: 99%

A new method to assign galaxy cluster membership using photometric redshifts

Castignani

Benoist

2016

A&A

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We introduce a new effective strategy to assign group and cluster membership probabilities Pmem to galaxies using photometric redshift information. Large dynamical ranges both in halo mass and cosmic time are considered. The method takes into account the magnitude distribution of both cluster and field galaxies as well as the radial distribution of galaxies in clusters using a non-parametric formalism, and relies on Bayesian inference to take photometric redshift uncertainties into account. We successfully test the method against 1, 208 galaxy clusters within redshifts z = 0.05−2.58 and masses 10 13.29−14.80 M drawn from wide field simulated galaxy mock catalogs mainly developed for the forthcoming Euclid mission. Median purity and completeness values of (55 +17 −15 )% and (95 +5 −10 )% are reached for galaxies brighter than 0.25L * within r200 of each simulated halo and for a statistical photometric redshift accuracy σ((zs −zp)/(1+zs)) = 0.03.The mean values p = 56% and c = 93% are consistent with the median and have negligible sub-percent uncertainties. Accurate photometric redshifts (σ((zs − zp)/(1 + zs)) 0.05) and robust estimates for the cluster redshift and cluster center coordinates are required. The dependence of the assignments on photometric redshift accuracy, galaxy magnitude and distance from the halo center, and halo properties such as mass, richness, and redshift are investigated. Variations in the mean values of both purity and completeness are globally limited to a few percent. The largest departures from the mean values are found for galaxies associated with distant z 1.5 halos, faint (∼ 0.25 L * ) galaxies, and those at the outskirts of the halo (at cluster-centric projected distances ∼ r200) for which the purity is decreased, ∆p 20% at most, with respect to the mean value. The proposed method is applied to derive accurate richness estimates. A statistical comparison between the true (Ntrue) vs. estimated richness (λ = Pmem) yields on average to unbiased results, Log(λ/Ntrue) = −0.0051 ± 0.15. The scatter around the mean of the logarithmic difference between λ and the halo mass is 0.10 dex for massive halos 10 14.5 M . Our estimates could therefore be useful to constrain the cluster mass function and to calibrate independent cluster mass estimates such as those obtained from weak lensing, Sunyaev-Zel'dovich, and X-ray studies. Our method can be applied to any list of galaxy clusters or groups in both present and forthcoming surveys such as SDSS, CFHTLS, Pan-STARRS, DES, LSST, and Euclid.

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Making the observational parsimonious richness a working mass proxy

Cited by 25 publications

References 48 publications

Richness-based masses of rich and famous galaxy clusters

Richness-based masses of rich and famous galaxy clusters

The amazing diversity in the hot gas content of an X-ray unbiased massive galaxy clusters sample

A new method to assign galaxy cluster membership using photometric redshifts

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