The Sunyaev–Zel’dovich Effect in Cosmology and Cluster Physics

Birkinshaw, Mark; Lancaster, Katy

doi:10.1007/978-1-4020-6941-3_8

Cited by 2 publications

(2 citation statements)

References 28 publications

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“…Sunyaev & Zeldovich 1970, Birkinshaw & Lancaster 2008, Olamaie, Hobson & Grainge 2013, Churazov, Vikhlinin & Sunyaev 2015, assuming hydrostatic equilibrium and calculating the intracluster medium (ICM) temperature from their X-ray emission (eg., Sarazin 2008, Martino et al 2014, Nelson et al 2014 or using the clusters' galaxy member velocities and assuming dynamical equilibrium (eg., Saro et al 2013, Sifón et al 2013, Tempel et al 2014 or not (eg., Diaferio & Geller 1997, Diaferio 1999). However, not all methods give the same results(eg., Hoekstra 2007, Peng et al 2009, Donahue et al 2014; each one of them has its own advantages and disadvantages (eg., Sadat 1997).…”

Section: Introductionmentioning

confidence: 99%

Galaxy cluster's rotation

Manolopoulou

Plionis

2016

Mon. Not. R. Astron. Soc.

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We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algorithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z 0.1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure velocities for rotation, provided by our Monte-Carlo simulation analysis, we find that ∼ 23% of our clusters are rotating under a set of strict criteria. Loosening the strictness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ∼ 28%. We correlate our rotation indicators with the cluster dynamical state, provided either by their Bautz-Morgan type or by their Xray isophotal shape and find for those clusters showing rotation within 1.5 h −1 70 Mpc that the significance of their rotation is related to the dynamically younger phases of cluster formation but after the initial anisotropic accretion and merging has been completed. Finally, finding rotational modes in galaxy clusters could lead to the necessity of correcting the dynamical cluster mass calculations.

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Section: Introductionmentioning

confidence: 99%

Galaxy cluster's rotation

Manolopoulou

Plionis

2016

Mon. Not. R. Astron. Soc.

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“…OCRA-p observed MS 1054-0321 for ∼ 11 hours using a combination of beam-switching and position-switching. Such a technique is efficient at subtracting atmospheric and ground signals, and removes such contaminating signals better than positionswitching or beam-switching alone (Birkinshaw & Lancaster 2008). The principles of the beam-and position-switching technique and the data reduction process are described in detail in Lancaster et al (2007).…”

Section: The X-ray Spectramentioning

confidence: 99%

The gas distribution in the high-redshift cluster MS 1054−0321

Mirakhor

Birkinshaw

2016

Mon. Not. R. Astron. Soc.

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We investigate the gas mass distribution in the high redshift cluster MS 1054-0321 using Chandra X-ray and OCRA SZ effect data. We use a superposition of offset β-type models to describe the composite structure of MS 1054-0321. We find gas mass fractions f X-ray gas = 0.087 −0.014 for the western component. The gas mass fraction for the eastern component is in agreement with some results reported in the literature, but inconsistent with the cosmic baryon fraction. The low gas mass fraction for the western component is likely to be a consequence of gas stripping during the ongoing merger. The gas mass fraction of the integrated system is 0.060−0.009 : we suggest that the missing baryons from the western component are present as hot diffuse gas which is poorly represented in existing X-ray images. The missing gas could appear in sensitive SZ maps.

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The Sunyaev–Zel’dovich Effect in Cosmology and Cluster Physics

Cited by 2 publications

References 28 publications

Galaxy cluster's rotation

Galaxy cluster's rotation

The gas distribution in the high-redshift cluster MS 1054−0321

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