Exploring Cluster Physics with High-Resolution Sunyaev-Zel’dovich Effect Images and X-Ray Data: The Case of the Most X-Ray-Luminous Galaxy Cluster RX J1347—1145

Kitayama, Tetsu; Komatsu, Eiichiro; Ota, Naomi; Kuwabara, Takeshi; Suto, Yasushi; Yoshikawa, Kohji; Hattori, Makoto; Matsuo, Hiroshi

doi:10.1093/pasj/56.1.17

Cited by 94 publications

(143 citation statements)

References 59 publications

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“…These multi-wavelength observations indicate that RX J1347.5−1145 is a massive (>10 15 M ) cluster at redshift z = 0.4510 which has recently undergone a merger with a smaller object. The cluster's SZ signal has been measured using single-dish (Pointecouteau et al 1999;Komatsu et al 2001;Kitayama et al 2004;Mason et al 2010;Korngut et al 2011) and interferometric (Carlstrom et al 2002;Bonamente et al 2008Bonamente et al , 2011 imaging instruments, and its spectrum near the thermal SZ null has also been characterized (Zemcov et al 2012). The higher angular resolution measurements have revealed a compact region of very hot (∼20 keV) gas to the southeast of the X-ray emission peak, while the low-resolution data indicate a lower-amplitude arcminute-scale SZ signal than suggested by a spherical fit to the X-ray data.…”

Section: Rx J13475−1145mentioning

confidence: 99%

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Plagge¹,

Marrone²,

Abdulla³

et al. 2013

ApJ

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We demonstrate the Sunyaev-Zel'dovich (SZ) effect imaging capabilities of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by presenting an SZ map of the galaxy cluster RX J1347.5−1145. By combining data from multiple CARMA bands and configurations, we are able to capture the structure of this cluster over a wide range of angular scales, from its bulk properties to its core morphology. We find that roughly 9% of this cluster's thermal energy is associated with sub-arcminute-scale structure imparted by a merger, illustrating the value of high-resolution SZ measurements for pursuing cluster astrophysics and for understanding the scatter in SZ scaling relations. We also find that the cluster's SZ signal is lower in amplitude than suggested by a spherically symmetric model derived from X-ray data, consistent with compression along the line of sight relative to the plane of the sky. Finally, we discuss the impact of upgrades currently in progress that will further enhance CARMA's power as an SZ imaging instrument.

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Section: Rx J13475−1145mentioning

confidence: 99%

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Plagge¹,

Marrone²,

Abdulla³

et al. 2013

ApJ

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“…Early single target SZ studies were limited to the clusters' inner regions (i.e., within R 500 ), and were not really competitive with the X-ray measurements in terms of resolution and sensitivity (see e.g., Pointecouteau et al 2001;Halverson et al 2009;Korngut et al 2011). However, the combination of SZ and X-ray tracers has already shown its potential in terms of structural studies of clusters (Pointecouteau et al 2002;Kitayama et al 2004;Jia et al 2008;Basu et al 2010). The first studies working on SZ cluster samples were presented by the SPT and ACT collaborations (Plagge et al 2010;Sehgal et al 2011), with 15 and 9 high significance clusters, respectively.…”

Section: The Inner Profilementioning

confidence: 99%

Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2013

A&A

291

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Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal indicates that most clusters are individually detected at least out to R 500 . By stacking the radial profiles, we have statistically detected the radial SZ signal out to 3 × R 500 , i.e., at a density contrast of about 50-100, though the dispersion about the mean profile dominates the statistical errors across the whole radial range. Our measurement is fully consistent with previous Planck results on integrated SZ fluxes, further strengthening the agreement between SZ and X-ray measurements inside R 500 . Correcting for the effects of the Planck beam, we have calculated the corresponding pressure profiles. This new constraint from SZ measurements is consistent with the X-ray constraints from XMM-Newton in the region in which the profiles overlap (i.e., [0.1-1] R 500 ), and is in fairly good agreement with theoretical predictions within the expected dispersion. At larger radii the average pressure profile is slightly flatter than most predictions from numerical simulations. Combining the SZ and X-ray observed profiles into a joint fit to a generalised pressure profile gives best-fit parameters [P 0 , c 500 , γ, α, β] = [6.41, 1.81, 0.31, 1.33, 4.13]. Using a reasonable hypothesis for the gas temperature in the cluster outskirts we reconstruct from our stacked pressure profile the gas mass fraction profile out to 3 R 500 . Within the temperature driven uncertainties, our Planck constraints are compatible with the cosmic baryon fraction and expected gas fraction in halos. Key words. cosmology: observations -galaxies: clusters: general -galaxies: clusters: intracluster medium -submillimeter: general -X-rays: general Appendices are available in electronic form at

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“…Pressure or temperature profiles of individual clusters have started to be derived from combined analysis of X-ray and SZE imaging data, using non-parametric deprojection methods (Nord et al 2009) or more realistic models than the β-model (Kitayama et al 2004;Mroczkowski et al 2009). Interestingly, the profiles are found to be consistent with profiles derived using X-ray spectroscopic data (see also Jia et al 2008;Halverson et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and theY_SZ–M₅₀₀relation

Arnaud¹,

Pratt

Piffaretti³

et al. 2010

A&A

946

139

1,685

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We investigate the regularity of cluster pressure profiles with REXCESS, a representative sample of 33 local (z < 0.2) clusters drawn from the REFLEX catalogue and observed with XMM-Newton. The sample spans a mass range of 10 14 M < M 500 < 10 15 M , where M 500 is the mass corresponding to a density contrast of 500. We derive an average profile from observations scaled by mass and redshift according to the standard self-similar model, and find that the dispersion about the mean is remarkably low, at less than 30 per cent beyond 0.2 R 500 , but increases towards the center. Deviations about the mean are related to both the mass and the thermo-dynamical state of the cluster. Morphologically disturbed systems have systematically shallower profiles while cooling core systems are more concentrated. The scaled profiles exhibit a residual mass dependence with a slope of ∼0.12, consistent with that expected from the empirically-derived slope of the M 500 − Y X relation; however, the departure from standard scaling decreases with radius and is consistent with zero at R 500 . The scatter in the core and departure from self-similar mass scaling is smaller compared to that of the entropy profiles, showing that the pressure is the quantity least affected by dynamical history and non-gravitational physics. Comparison with scaled data from several state of the art numerical simulations shows good agreement outside the core. Combining the observational data in the radial range [0.03−1] R 500 with simulation data in the radial range [1−4] R 500 , we derive a robust measure of the universal pressure profile, that, in an analytical form, defines the physical pressure profile of clusters as a function of mass and redshift up to the cluster "boundary". Using this profile and direct spherical integration of the observed pressure profiles, we estimate the integrated Compton parameter Y and investigate its scaling with M 500 and L X , the soft band X-ray luminosity. We consider both the spherically integrated quantity, Y sph (R), proportional to the gas thermal energy, and the cylindrically integrated quantity,A , which is directly related to the Sunyaev-Zel'dovich (SZ) effect signal. From the low scatter of the observed Y sph (R 500 )−Y X relation we show that variations in pressure profile shape do not introduce extra scatter into the Y sph (R 500 )− M 500 relation as compared to that from the Y X − M 500 relation. The Y sph (R 500 )− M 500 and Y sph (R 500 )−L X relations derived from the data are in excellent agreement with those expected from the universal profile. This profile is used to derive the expected Y SZ − M 500 and Y SZ − L X relations for any aperture.

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Exploring Cluster Physics with High-Resolution Sunyaev-Zel’dovich Effect Images and X-Ray Data: The Case of the Most X-Ray-Luminous Galaxy Cluster RX J1347—1145

Cited by 94 publications

References 59 publications

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Planckintermediate results

The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and theY_SZ–M₅₀₀relation

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Exploring Cluster Physics with High-Resolution Sunyaev-Zel’dovich Effect Images and X-Ray Data: The Case of the Most X-Ray-Luminous Galaxy Cluster RX J1347—1145

Cited by 94 publications

References 59 publications

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Carma Measurements of the Sunyaev-Zel'dovich Effect in Rx J1347.5–1145

Planckintermediate results

The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and theYSZ–M500relation

Contact Info

Product

Resources

About

The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and theY_SZ–M₅₀₀relation