Pressure Profiles of Distant Galaxy Clusters in the Planck Catalogue

Bourdin, H.; Mazzotta, P.; Kozmanyan, A.; Jones, C.; Vikhlinin, A.

doi:10.3847/1538-4357/aa74d0

Cited by 26 publications

(45 citation statements)

References 40 publications

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“…In the second step, we jointly fit the X-ray projected temperature kT obs X (r) and SZ y obs (r) signal profiles. kT obs X (r) was extracted from the XMM-Newton, while y obs (r) was extracted from the six Planck HFI maps (see Bourdin et al 2017 for details).…”

Section: Derivation Of P(r) and Kt (R)mentioning

confidence: 99%

“…It spatially resolves and maps clusters near r 500 , allowing constraints on cluster pressure profile shapes and dispersion. On the analysis side, the Planck multi-frequency coverage allows an accurate cleaning of foregrounds and backgrounds for the separation of the SZ signal (see Bourdin et al 2017). All of these factors substantially minimise many uncertainties on the Compton parameter y that were present previously as a result of the limited frequency coverage and impossibility of foreground cleaning (e.g.…”

Section: Comparison With Other Measurements Using Sz and X-ray Datamentioning

confidence: 99%

“…The fre-Article number, page 1 of 15 arXiv:1809.09560v2 [astro-ph.CO] 25 Mar 2019 A&A proofs: manuscript no. hubble_sz quency coverage of the CMB spectrum offered by the highfrequency instrument of Planck (100 -857 GHz) allows mapping the Compton parameter y, that is, the amplitude of the SZ effect, with an unprecedented accuracy at intermediate cluster-centric radii (Bourdin et al 2017). It thus permits us to perform precise, spatially resolved comparisons with X-ray measurements.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

Kozmanyan

Bourdin

Mazzotta

et al. 2019

A&A

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The possibility of determining the value of the Hubble constant using observations of galaxy clusters in X-ray and microwave wavelengths through the Sunyaev Zel'dovich (SZ) effect has long been known. Previous measurements have been plagued by relatively large errors in the observational data and severe biases induced, for example, by cluster triaxiality and clumpiness. The advent of Planck allows us to map the Compton parameter y, that is, the amplitude of the SZ effect, with unprecedented accuracy at intermediate cluster-centric radii, which in turn allows performing a detailed spatially resolved comparison with X-ray measurements. Given such higher quality observational data, we developed a Bayesian approach that combines informed priors on the physics of the intracluster medium obtained from hydrodynamical simulations of massive clusters with measurement uncertainties. We applied our method to a sample of 61 galaxy clusters with redshifts up to z < 0.5 observed with Planck and XMM-Newton and find H 0 = 67 ± 3km s −1 Mpc −1 .

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Section: Derivation Of P(r) and Kt (R)mentioning

confidence: 99%

Section: Comparison With Other Measurements Using Sz and X-ray Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

Kozmanyan

Bourdin

Mazzotta

et al. 2019

A&A

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“…The general approach for this is as follows (see also Bourdin et al 2017;Kozmanyan et al 2019). From the Xray data, the density and temperature profiles can be constrained [i.e., n e (r) and T sl (r)], and from the SZ data the pressure profile, P e (r) can be constrained through the measurements of y assuming the distortion is wholly non-relativistic.…”

Section: Applications To the Determination Of Hmentioning

confidence: 99%

Relativistic SZ temperature scaling relations of groups and clusters derived from the BAHAMAS and MACSIS simulations

Lee

Chluba

Kay

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Sunyaev-Zeldovich (SZ) effect has long been recognized as a powerful cosmological probe. Using the BAHAMAS and MACSIS simulations to obtain > 10, 000 simulated galaxy groups and clusters, we compute three temperature measures and quantify the differences between them. The first measure is related to the X-ray emission of the cluster, while the second describes the non-relativistic thermal SZ (tSZ) effect. The third measure determines the lowest order relativistic correction to the tSZ signal, which is seeing increased observational relevance. Our procedure allows us to accurately model the relativistic SZ (rSZ) contribution and we show that a 10% − 40% underestimation of this rSZ cluster temperature is expected when applying standard X-ray relations. The correction also exhibits significant mass and redshift evolution, as we demonstrate here. We present the mass dependence of each temperature measure alongside their profiles and a short analysis of the temperature dispersion as derived from the aforementioned simulations. We also discuss a new relation connecting the temperature and Compton-y parameter, which can be directly used for rSZ modelling. Simple fits to the obtained scaling relations and profiles are provided. These should be useful for future studies of the rSZ effect and its relevance to cluster cosmology.

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“…Following Meisner & Finkbeiner (2015) (see also Bourdin et al 2017), we model the thermal dust as a double grey body, i.e. assuming two populations of dust grains, instead of the idealised case of a single grey body spectrum.…”

Section: Modelling Of Thermal Dustmentioning

confidence: 99%

Spectral imaging of the thermal Sunyaev–Zel’dovich effect in X-COP galaxy clusters: method and validation

Baldi

Bourdin

Mazzotta

et al. 2019

A&A

Self Cite

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The imaging of galaxy clusters through the Sunyaev-Zel'dovich effect is a valuable tool to probe the thermal pressure of the intra-cluster gas especially in the outermost regions, where X-ray observations suffer from photon statistics. For the first time, we produce maps of the Comptonization parameter by applying a locally parametric algorithm for sparse component separation to the latest frequency maps released by Planck. The algorithm takes into account properties of real cluster data through a two-component modelling of the spectral energy density of thermal dust, and a masking of bright point sources. Its robustness has been improved in the low signal-to-noise regime, thanks to the implementation of a deconvolution of Planck beams in the chi-square minimization of each wavelet coefficient. We apply this procedure to twelve low-redshift galaxy clusters detected by Planck with the highest signal-to-noise ratio, considered for the XMM Cluster Oustkirts Project (X-COP). Our images show the presence of anisotropic features, such as small-scale blobs and filamentary substructures, located in the outskirts of a number of clusters in the sample. The significance of their detection is established via a bootstrap-based procedure we propose here for the first time. In particular, we present a qualitative comparison with X-ray data for two interesting systems, namely A2029 and RXC1825. Our results show an agreement on the features detected in the outskirts of the clusters in the two bands.

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Pressure Profiles of Distant Galaxy Clusters in the Planck Catalogue

Cited by 26 publications

References 40 publications

Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

Relativistic SZ temperature scaling relations of groups and clusters derived from the BAHAMAS and MACSIS simulations

Spectral imaging of the thermal Sunyaev–Zel’dovich effect in X-COP galaxy clusters: method and validation

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