Observations of the Sunyaev–Zel'dovich effect at high angular resolution towards the galaxy clusters A665, A2163 and CL0016+16

Désert, F.‐X.; Benoı̂t, A.; Gaertner, S.; Bernard, J.-P.; Coron, N.; Delabrouille, J.; Marcillac, P. de; Giard, M.; Lamarre, J.-M.; Lefloch, B.; Puget, J.‐L.; Sirbi, A.

doi:10.1016/s1384-1076(98)00032-3

Cited by 21 publications

(23 citation statements)

References 32 publications

(48 reference statements)

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“…A highly nonrelaxed state in the cluster inner region is confirmed by the recent Chandra results (Markevitch et al 2000). A strong Sunyaev-Zel'dovich (SZ) effect has been reported in this cluster (Holzapfel et al 1997;Désert et al 1998).…”

Section: Introductionmentioning

confidence: 69%

The giant radio halo in Abell 2163

Feretti

Fusco-Femiano²,

Giovannini

et al. 2001

A&A

161

176

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Abstract. New radio data is presented for the rich cluster Abell 2163. The cluster radio emission is characterized by the presence of a radio halo, which is one of the most powerful and extended halos known so far. In the NE peripheral cluster region, we also detect diffuse elongated emission, which we classify as a cluster relic. The cluster A2163 is very hot and luminous in X-ray. Its central region is probably in a highly non relaxed state, suggesting that this cluster is likely to be a recent merger. The existence of a radio halo in this cluster confirms that halos are associated with hot massive clusters, and confirms the connection between radio halos and cluster merger processes. The comparison between the radio emission of the halo and the cluster X-ray emission shows a close structural similarity. A power law correlation is found between the radio and X-ray brightness, with index =0.64. We also report the upper limit to the hard X-ray emission, obtained from a BeppoSAX observation. We discuss the implications of our results.

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Section: Introductionmentioning

confidence: 69%

The giant radio halo in Abell 2163

Feretti

Fusco-Femiano²,

Giovannini

et al. 2001

A&A

161

176

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“…In particular the SZ effect spectrum has been observed from BIMA at 28.5 GHz (LaRoque et al 2002), from DIABOLO at 140 GHz (Desert et al 1998) and from SuZIE at 140, 218 and 270 GHz (Holzapfel et al 1997; these data are dust-corrected in LaRoque et al 2002) thus including and bracketing the null of the thermal SZ effect. Considering a pure thermal SZ effect, the previous data on A2163 are fitted with a Compton parameter y th = (3.65 ± 0.40) × 10 −4 and with the addition of a kinematic SZ effect whose amplitude corresponds to a positive peculiar velocity V p = 415 +920 −765 km s −1 (Carlstrom et al 2002) whose large uncertainties, however, makes it consistent with a zero value.…”

Section: The Case Of A2163mentioning

confidence: 99%

The non-thermal Sunyaev–Zel'dovich effect in clusters of galaxies

Colafrancesco

Marchegiani

Palladino

2002

A&A

101

250

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Abstract. In this paper we provide a general derivation of the non-thermal Sunyaev-Zel'dovich (SZ) effect in galaxy clusters which is exact in the Thomson limit to any approximation order in the optical depth τ. The general approach we use also allows us to obtain an exact derivation of the thermal SZ effect in a self-consistent framework. Such a general derivation is obtained using the full relativistic formalism and overcoming the limitations of the Kompaneets and of the single scattering approximations. We compare our exact results with those obtained at different approximation orders in τ and we give estimates of the precision fit. We verified that the third order approximation yields a quite good description of the spectral distortion induced by the Comptonization of CMB photons in the cluster atmosphere. In our general derivation, we show that the spectral shape of the thermal and non-thermal SZ effect depends not only on the frequency but also on the cluster parameters, like the electron pressure and optical depth and from the energy spectrum of the electron population. We also show that the spatial distribution of the thermal and non-thermal SZ effect in clusters depends on a combination of the cluster parameters and on the spectral features of the effect. To have a consistent description of the SZ effect in clusters containing non-thermal phenomena, we also evaluate in a consistent way -for the first time -the total SZ effect produced by a combination of thermal and nonthermal electron population residing in the same environment, like is the case in radio-halo clusters. In this context, we show that the location of the zero of the total SZ effect increases non-linearly with increasing values of the pressure ratio between the non-thermal and thermal electron populations and its determination provides a unique way to determine the pressure of the relativistic particles residing in the cluster atmosphere. We discuss in detail both the spectral and the spatial features of the total (thermal plus non-thermal) SZ effect and we provide specific predictions for a well studied radio-halo cluster like A2163. Our general derivation allows also to discuss the overall SZ effect produced by a combination of different thermal populations residing in the cluster atmosphere. Such a general derivation of the SZ effect allows to consider also the CMB Comptonization induced by several electron populations. In this context, we discuss how the combined observations of the thermal and non-thermal SZ effect and of the other non-thermal emission features occurring in clusters (radio-halo, hard X-ray and EUV excesses) provide relevant constraints of the spectrum of the relativistic electron population and, in turn, on the presence and on the origin of non-thermal phenomena in galaxy clusters. We finally discuss how SZ experiments with high sensitivity and narrow-band spectral coverage, beyond the coming PLANCK satellite, can definitely probe the presence of a non-thermal SZ effect in galaxy clusters and disentangle this source o...

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“…Doré, e-mail: dore@iap.fr Due to observational progress, increasingly high quality data are available that enable multi-wavelength investigation of clusters down to an arc-minute scale (the most recent is the spectacular progress in SZ measurements, e.g. Reese et al (2000) and Désert et al (1998). In contrast with past decades, it is now possible to analyse clusters of galaxies using X-ray, WL and SZ data at almost the same resolution, and to produce from them self consistent models.…”

Section: Introductionmentioning

confidence: 99%

Cluster physics from joint weak gravitational lensing and Sunyaev-Zel'dovich data

Doré

Bouchet²,

Mellier³

et al. 2001

A&A

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Abstract. We present a self consistent method to perform a joint analysis of Sunyaev-Zel'dovich and weak gravitational lensing observation of galaxy clusters. The spatial distribution of the cluster main components is described by a perturbative approach. Assuming hydrostatic equilibrium and the equation of state, we are able to deduce, from observations, maps of projected gas density and gas temperature. The method then naturally entails a X-ray emissivity prediction which can be compared to observed X-ray emissivity maps. By comparing with 2 simulated clusters we find that this prediction turns out to be in very good agreement with the simulations. The simulated and predicted surface brightness images have a correlation coefficient higher than 0.9 and their total flux differs by 0.9% or 9%. The method should be able to deal with real data in order to provide a physical description of the state of the cluster and of its constituents. The tests performed show that we can recover the amount and the spatial distributions of both the baryonic and non-baryonic material with an accuracy better than 10%. So, in principle, it might indeed help to alleviate some well known biases affecting, e.g. baryon fraction measurements.

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Observations of the Sunyaev–Zel'dovich effect at high angular resolution towards the galaxy clusters A665, A2163 and CL0016+16

Cited by 21 publications

References 32 publications

The giant radio halo in Abell 2163

The giant radio halo in Abell 2163

The non-thermal Sunyaev–Zel'dovich effect in clusters of galaxies

Cluster physics from joint weak gravitational lensing and Sunyaev-Zel'dovich data

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