The Distance to Clusters: Correcting for Asphericity

Fox, David C.; Pen, Ue-Li

doi:10.1086/340897

Cited by 28 publications

(33 citation statements)

References 34 publications

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“…Therefore, an elongation along the line of sight can contribute to resolve the discrepancy between X-ray and lensing mass. a value for the Hubble constant is assumed (see also Fox & Pen 2002). Although the SZ effect is strongly affected by temperature gradients, we again assume isothermality of the ICM because of the lack of detailed temperature maps.…”

Section: Constraints From the Sunyaev-zel'dovich Effectmentioning

confidence: 99%

Aspherical galaxy clusters: Effects on cluster masses and gas mass fractions

Piffaretti

Jetzer

Schindler

2003

A&A

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Abstract. We present an investigation of the effects of asphericity on the estimates of total mass and gas mass fraction in galaxy clusters from X-ray observations. We model the aspherical shape of galaxy clusters by a triaxial model and compare the true total mass and the true total gas mass fraction with the corresponding quantities obtained with the assumption of spherical symmetry. In the triaxial model we allow the extent along the line of sight to vary in order to describe elongated and compressed cluster shapes. Using a sample of 10 ROSAT clusters and a recent CHANDRA observation we find the following results. For prolate or oblate shapes the difference between triaxial and spherical model both in the mass and in the gas mass fraction are negligible (less than 3%). For more aspherical shapes the total mass is underestimated (overestimated) in the centre, if the cluster is compressed (elongated). The gas mass fraction is overestimated for compressed clusters and slightly underestimated for elongated clusters. Comparing X-ray masses with gravitational lensing estimates, we find that elongations along the line of sight can resolve discrepancies of masses determined by the two different methods of up to ∼30%. The combination of SunyaevZel'dovich and X-ray observations is useful to measure the elongation of the cluster along the line of sight. As an application, we estimate the elongation of the cluster CL0016+16 with two different approaches, Sunyaev-Zel'dovich measurements and comparison of weak lensing and X-ray masses, and find reasonable agreement.

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Section: Constraints From the Sunyaev-zel'dovich Effectmentioning

confidence: 99%

Aspherical galaxy clusters: Effects on cluster masses and gas mass fractions

Piffaretti

Jetzer

Schindler

2003

A&A

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“…Individual clusters can be investigated with multi-probe approaches, see Zaroubi et al (1998), Reblinsky (2000), Doré et al (2001), Fox & Pen (2002), Puchwein & Bartelmann (2006), Mahdavi & Chang (2011), Morandi et al (2012). Joint X-ray and SZ analyses can probe the gas physics in detail, e.g.…”

Section: Introductionmentioning

confidence: 99%

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Sereno

Ettori

Meneghetti

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Multi-wavelength techniques can probe the distribution and the physical properties of baryons and dark matter in galaxy clusters from the inner regions out to the peripheries. We present a full three-dimensional analysis combining strong and weak lensing, X-ray surface brightness and temperature, and the Sunyaev-Zel'dovich effect. The method is applied to MACS J1206.2-0847, a remarkably regular, face-on, massive, M 200 = (1.1 ± 0.2) × 10 15 M /h, cluster at z = 0.44. The measured concentration, c 200 = 6.3 ± 1.2, and the triaxial shape are common to halos formed in a ΛCDM scenario. The gas has settled in and follows the shape of the gravitational potential, which is evidence of pressure equilibrium via the shape theorem. There is no evidence for significant non-thermal pressure and the equilibrium is hydrostatic.

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“…Doré et al (2001) proposed a method that with a perturbative approach and with the aid of SZ and weak-lensing data, could predict the cluster X-ray emissivity without resolving the full three-dimensional structure of the cluster. The degeneracy between the distance to galaxy clusters and the elongation of the cluster along the line of sight (LOS) was thoroughly discussed by Fox & Pen (2002). They introduced a specific method for finding the intrinsic three-dimensional shape of triaxial cluster and, at the same time, measuring the distance to the cluster corrected for asphericity, so providing an unbiased estimate of the Hubble constant H 0 .…”

Section: Introductionmentioning

confidence: 99%

Measuring the Three‐dimensional Structure of Galaxy Clusters. I. Application to a Sample of 25 Clusters

Filippis

Sereno

Bautz

et al. 2005

ApJ

194

341

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We discuss a method to constrain the intrinsic shapes of galaxy clusters by combining X-ray and SunyaevZel'dovich observations. The method is applied to a sample of 25 X-ray-selected clusters, with measured SunyaevZel'dovich temperature decrements. The sample turns out to be slightly biased, with strongly elongated clusters preferentially aligned along the line of sight. This result demonstrates that X-ray-selected cluster samples may be affected by morphological and orientation effects, even if a relatively high threshold signal-to-noise ratio is used to select the sample. A large majority of the clusters in our sample exhibit a marked triaxial structure; the spherical hypothesis is strongly rejected for most sample members. Cooling-flow clusters do not show preferentially regular morphologies. We also show that identification of multiple gravitationally lensed images, together with measurements of the Sunyaev-Zel'dovich effect and X-ray surface brightness, can provide a simultaneous determination of the three-dimensional structure of a cluster, of the Hubble constant, and of the cosmological energy density parameters.

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The Distance to Clusters: Correcting for Asphericity

Cited by 28 publications

References 34 publications

Aspherical galaxy clusters: Effects on cluster masses and gas mass fractions

Aspherical galaxy clusters: Effects on cluster masses and gas mass fractions

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Measuring the Three‐dimensional Structure of Galaxy Clusters. I. Application to a Sample of 25 Clusters

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