Application of a Self-Similar Pressure Profile to Sunyaev-Zel'dovich Effect Data From Galaxy Clusters

Mroczkowski, Tony; Bonamente, Massimiliano; Carlstrom, J. E.; Culverhouse, T.; Greer, Christopher H.; Hawkins, David; Hennessy, Ryan; Joy, M.; Lamb, James W.; Leitch, E. M.; Loh, Michael; Maughan, Ben; Marrone, Daniel P.; Miller, Amber; Muchovej, Stephen; Nagai, Daisuke; Pryke, C.; Sharp, Matthew; Woody, D. P.

doi:10.1088/0004-637x/694/2/1034

Cited by 89 publications

(151 citation statements)

References 46 publications

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“…From their observations, no such objects are present within the NIKA field. From the residual between the MUSTANG map and the SZA pressure model of Mroczkowski et al (2009), Korngut et al (2011) have inferred the presence of a possible submillimeter source 10 arcsec north of the X-ray peak. Using the NIKA 260 GHz frequency band, we searched for such a contaminant and do not observe any point source within a 1.5 arcmin radius around the map center, apart from PS260.…”

Section: Point Source Contaminationmentioning

confidence: 99%

“…Following Mroczkowski et al (2009) and since we use the work of Comis et al (2011), the electron density profile is described by a simplified version (SVM) of the model suggested by Vikhlinin et al (2006) n e (r) = n e0…”

Section: Density Profilementioning

confidence: 99%

“…More recent Chandra observations also agree that CL J1226.9+3332 is a hot system (Bonamente et al 2006, T e = 14.0 +2.1 −1.8 keV). The pressure profile of the cluster was measured at arcmin angular scales using the interferometric SZA observations at 30 and 90 GHz (Muchovej et al 2007;Mroczkowski et al 2009;Mroczkowski 2011), providing a detailed picture of the ICM on these scales. First indications of a disturbed core were made by an XMM/Chandra analysis, showing an asymmetry in the temperature map with a hotter southwest region (Maughan et al 2007).…”

Section: Introductionmentioning

confidence: 99%

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Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Adam

Comis

Macías-Pérez

et al. 2015

A&A

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The thermal Sunyaev-Zel'dovich (tSZ) effect is expected to provide a low scatter mass proxy for galaxy clusters since it is directly proportional to the cluster thermal energy. The tSZ observations have proven to be a powerful tool for detecting and studying them, but high angular resolution observations are now needed to push their investigation to a higher redshift. In this paper, we report high angular (<20 arcsec) resolution tSZ observations of the high-redshift cluster CL J1226.9+3332 (z = 0.89). It was imaged at 150 and 260 GHz using the NIKA camera at the IRAM 30-m telescope. The 150 GHz map shows that CL J1226.9+3332 is morphologically relaxed on large scales with evidence of a disturbed core, while the 260 GHz channel is used mostly to identify point source contamination. NIKA data are combined with those of Planck and X-ray from Chandra to infer the cluster's radial pressure, density, temperature, and entropy distributions. The total mass profile of the cluster is derived, and we find M 500 = 5.96 +1.02 −0.79 × 10 14 M within the radius R 500 = 930 +50 −43 kpc, at a 68% confidence level. (R 500 is the radius within which the average density is 500 times the critical density at the cluster's redshift.) NIKA is the prototype camera of NIKA2, a KIDs (kinetic inductance detectors) based instrument to be installed at the end of 2015. This work is, therefore, part of a pilot study aiming at optimizing tSZ NIKA2 large programs.

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Section: Point Source Contaminationmentioning

confidence: 99%

Section: Density Profilementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Adam

Comis

Macías-Pérez

et al. 2015

A&A

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“…Dedicated instruments now produce high resolution images of single objects (e.g. Kitayama et al 2004;Halverson et al 2009;Nord et al 2009) and moderately large samples of high-quality SZ measurements of previously-known clusters (e.g., Mroczkowski et al 2009;Plagge et al 2010). In addition, large-scale surveys for clusters using the SZ effect are underway, both from space with the Planck mission (Valenziano et al 2007;Lamarre et al 2003) and from the ground with several dedicated telescopes, such as the South Pole Telescope ) leading to the first discoveries of clusters solely through their SZ signal (Staniszewski et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data

Melin

Bartlett

Delabrouille

et al. 2010

A&A

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We use multifrequency matched filters to estimate, in the WMAP 5-year data, the Sunyaev-Zel'dovich (SZ) fluxes of 893 ROSAT NORAS/REFLEX clusters spanning the luminosity range L X,[0.1−2.4] keV = 2×10 41 −3.5×10 45 erg s −1 . The filters are spatially optimised by using the universal pressure profile recently obtained from combining XMM-Newton observations of the REXCESSsample and numerical simulations. Although the clusters are individually only marginally detected, we are able to firmly measure the SZ signal (>10σ) when averaging the data in luminosity/mass bins. The comparison between the bin-averaged SZ signal versus luminosity and X-ray model predictions shows excellent agreement, implying that there is no deficit in SZ signal strength relative to expectations from the X-ray properties of clusters. Using the individual cluster SZ flux measurements, we directly constrain the Y 500 −L X and Y 500 −M 500 relations, where Y 500 is the Compton y-parameter integrated over a sphere of radius r 500 . The Y 500 −M 500 relation, derived for the first time in such a wide mass range, has a normalisation Y * 500 = [1.60 ± 0.19] × 10 −3 arcmin 2 at M 500 = 3 × 10 14 h −1 M , in excellent agreement with the X-ray prediction of 1.54 × 10 −3 arcmin 2 , and a mass exponent of α = 1.79 ± 0.17, consistent with the self-similar expectation of 5/3. Constraints on the redshift exponent are weak due to the limited redshift range of the sample, although they are compatible with self-similar evolution.

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“…Such improved analyses are specially important when the physical quantity one derives from the data is particularly sensitive to the core and/or outskirt properties. This includes the hydrostatic mass profile in the center (critical for dark matter concentration estimates) and on a large scale (critical for precise cluster mass estimates), but also the integrated SZ decrement at large radii, for which more realistic models are beginning to be used (Mroczkowski et al 2009). …”

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confidence: 99%

Theβ-model of the intracluster medium

Arnaud¹

2009

A&A

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The space between the galaxies in clusters of galaxies is filled with a hot tenous gas. Its high temperature (0.5-15 keV) is set by the the virialization process in the cluster's deep potential well, and the gas emits in X-rays predominantly through thermal Bremsstrahlung. This intracluster medium (ICM) is the main baryonic components of clusters and accounts for about 10% of the total dark matter dominated mass. While this is now wellestablished, it was not the case in the mid 70s, when the pioneering paper by Cavaliere & Fusco-Femiano (1976), which set the basis of the powerful β-model, was written.The idea of an ICM was proposed as early as 1959, but it took 10 years after its first detection in 1966 to definitively prove the existence of the hot ICM (see also Sarazin 1986; Biviano 2000, for a historical review). Limber (1959) stated that it is "rather likely that there is an appreciable quantity of intracluster gas pervading (...) clusters", primordial gas left over from galaxy formation, gas swept out of galaxies during galaxy collisions, or both. However, "it (was) not at all clear at (that) time whether one should expect the intracluster gas to be hot or cold". The first observational clue was the detection of M 87 in the Virgo cluster with the Geiger counters onboard an Aerobee rocket (Byram et al. 1966), which was also the first detection of an X-ray source associated with a cluster. The next major advance was made with Uhuru, the first satellite dedicated to X-ray astronomy, launched in 1970. Uhuru performed an all-sky X-ray survey and permitted longer observations of individual sources than with rockets experiments. This established that clusters are X-ray luminous sources and that the X-ray emission is extended and not time variable (e.g. Gursky et al. 1972, online).The detectors onboard Uhuru and rocket experiments were non-imaging proportional counters equipped with collimators to limit the field of view. Because of the crude spectral and spatial resolution (∼1 • ) of the detectors, the origin of the X-ray emission was ambiguous. Three possibilities were considered: 1) thermal bremsstrahlung from a hot tenuous gas; 2) inverse Compton (IC) scattering of CMB photons by relativistic electrons within the clusters; and 3) summed contributions of stellar sources (binaries or globular clusters). This was discussed very early by Felten et al. (1966) who correctly favored the thermal model on energetics arguments (unfortunately based on a spurious detection of the Coma cluster).In their paper, Cavaliere and Fusco-Femiano outlined several problems with the IC interpretation and, in particular, with the low value of the magnetic field implied by the ratio of the X-ray and Synchrotron radio luminosity. On the other hand, they emphasized that the IC emission is expected to stand out at energies above the thermal emission's exponential cut-off, E ∼ > 10 keV. The IC emission was indeed searched later on as an excess over the thermal emission in the hard X-ray band with Beppo-SAX, RXTE, and now Suzaku. Its level r...

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Application of a Self-Similar Pressure Profile to Sunyaev-Zel'dovich Effect Data From Galaxy Clusters

Cited by 89 publications

References 46 publications

Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data

Theβ-model of the intracluster medium

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Application of a Self-Similar Pressure Profile to Sunyaev-Zel'dovich Effect Data From Galaxy Clusters

Cited by 89 publications

References 46 publications

Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

The galaxy clusterYSZ−LXandYSZ−Mrelations from the WMAP 5-yr data

Theβ-model of the intracluster medium

Contact Info

Product

Resources

About

The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data