The Anisotropy of the Microwave Background to<i>l</i>= 3500: Deep Field Observations with the Cosmic Background Imager

Mason, B. S.; Pearson, T. J.; Readhead, A. C. S.; Shepherd, M. C.; Sievers, Jonathan; Udomprasert, P. S.; Cartwright, J. K.; Farmer, Alison J.; Padin, S.; Myers, Steven T.; Bond, J. R.; Contaldi, C. R.; Pen, Ue-Li; Prunet, S.; Pogosyan, D.; Carlstrom, J. E.; Kovac, J. M.; Leitch, E. M.; Pryke, C.; Halverson, N. W.; Holzapfel, W. L.; Altamirano, Pablo; Bronfman, L.; Casassus, S.; May, J.; Joy, M.

doi:10.1086/375507

Cited by 265 publications

(151 citation statements)

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“…Treating the XBAC clusters as point sources, we estimate their ( Ricci et al 2004); triangles: from the 9C survey at 15 GHz ( Waldram et al 2003); squares: from the Very Small Array ( VSA) at 33 GHz (Cleary et al 2005). The parallelogram is from the Cosmic Background Imager (CBI ) experiment at 31 GHz ( Mason et al 2003). Several models for dN/dS are shown for comparison: the solid curve is the 44 GHz dN/dS model from Toffolatti et al (1998), the dotted curve is the Toffolatti model rescaled by 0.66 (found to be a good fit to the first-year data), and the dashed curve is an updated 40.7 GHz model from de Zotti et al (2005).…”

Section: Sunyaev-zeldovich (Sz ) Effectmentioning

confidence: 99%

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Hinshaw

Nolta

Bennett

et al. 2007

ASTROPHYS J SUPPL S

1,178

1,209

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We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on data from the first 3 years of the WMAP sky survey. The new maps are consistent with the first-year maps and are more sensitive. The 3 year maps incorporate several improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include several new consistency tests as well as refinements in the gain calibration and beam response models. We employ two forms of multifrequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved ''Internal Linear Combination'' (ILC) map, based solely on WMAP data, by adding a bias-correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission instead of the 408 MHz sky survey. The WMAP point source catalog is updated to include 115 new sources whose detection is made possible by the improved sky map sensitivity. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l > 30. The resulting multifrequency spectra are analyzed for residual point source contamination. At 94 GHz the unmasked sources contribute 128 AE 27 K 2 to l(l þ 1)C l /2 at l ¼ 1000. After subtracting this contribution, our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l ¼ 400, and the signal-to-noise ratio per l-mode exceeds unity up to l ¼ 850. For bins of width Ál/l ¼ 3%, the signal-to-noise ratio exceeds unity up to l ¼ 1000. The first two acoustic peaks are seen at l ¼ 220:8 AE 0:7 and l ¼ 530:9 AE 3:8, respectively, while the first two troughs are seen at l ¼ 412:4 AE 1:9 and l ¼ 675:2 AE 11:1. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established. Spergel et al. use the 3 year temperature and polarization data to constrain cosmological model parameters. A simple six-parameter ÃCDM model continues to fit CMB data and other measures of large-scale structure remarkably well. The new polarization data produce a better measurement of the optical depth to reionization, ¼ 0:089 AE 0:03. This new and tighter constraint on helps break a degeneracy with the scalar spectral index, which is now found to be n s ¼ 0:960 AE 0:016. If additional cosmological data sets are included in the analysis, the spectral index is found to be n s ¼ 0:947 AE 0:015.

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Section: Sunyaev-zeldovich (Sz ) Effectmentioning

confidence: 99%

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Hinshaw

Nolta

Bennett

et al. 2007

ASTROPHYS J SUPPL S

1,178

1,209

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“…The CMB contribution to the simulated maps is a realization of the WMAP5 CMB power spectrum (Nolta et al 2009). The point-source contribution is a spatially random distribution of sources drawn from models based on the Borys et al (2003) counts for dusty protogalaxies and a version of the Toffolatti et al (1998) counts for radio-loud active galactic nuclei (AGNs) modified to match the DASI, CBI, and VSA counts at 30 GHz (Kovac et al 2002;Mason et al 2003;Cleary et al 2005). (As predicted in Section 2.4.2, the contribution of the unresolved AGN population to the power in the simulated maps turns out to be negligible.)…”

Section: False Detection Simulationsmentioning

confidence: 99%

Galaxy Clusters Discovered With a Sunyaev-Zel'dovich Effect Survey

Staniszewski

Ade

Aird

et al. 2009

ApJ

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266

235

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The South Pole Telescope (SPT) is conducting a Sunyaev-Zel'dovich (SZ) effect survey over large areas of the southern sky, searching for massive galaxy clusters to high redshift. In this preliminary study, we focus on a 40 deg 2 area targeted by the Blanco Cosmology Survey (BCS), which is centered roughly at right ascension 5 h 30 m , declination −53 • (J2000). Over two seasons of observations, this entire region has been mapped by the SPT at 95 GHz, 150 GHz, and 225 GHz. We report the four most significant SPT detections of SZ clusters in this field, three of which were previously unknown and, therefore, represent the first galaxy clusters discovered with an SZ survey. The SZ clusters are detected as decrements with greater than 5σ significance in the highsensitivity 150 GHz SPT map. The SZ spectrum of these sources is confirmed by detections of decrements at the corresponding locations in the 95 GHz SPT map and nondetections at those locations in the 225 GHz SPT map. Multiband optical images from the BCS survey demonstrate significant concentrations of similarly colored galaxies at the positions of the SZ detections. Photometric redshift estimates from the BCS data indicate that two of the clusters lie at moderate redshift (z ∼ 0.4) and two at high redshift (z 0.8). One of the SZ detections was previously identified as a galaxy cluster in the optical as part of the Abell supplementary southern cluster catalog and in the X-ray using data from the ROSAT All-Sky Survey (RASS). Potential RASS counterparts (not previously identified as clusters) are also found for two of the new discoveries. These first four galaxy clusters are the most significant SZ detections from a subset of the ongoing SPT survey. As such, they serve as a demonstration that SZ surveys, and the SPT in particular, can be an effective means for finding galaxy clusters.

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“…The maps are created from a large-volume, high-resolution Nbody simulation containing a '' fair sample '' of the universe, in a manner tuned to reproduce the results of the hydrodynamic simulations reported in White, Hernquist, & Springel (2002). The normalization has been adjusted to pass through the lower envelope of the Cosmic Background Imager (CBI) deep-field results reported in Mason et al (2003) and through the Berkeley-Illinois-Maryland Association (BIMA) point (Dawson et al 2001) at higher '. This is close to the power seen in more recent CBI data (A. Readhead 2003, private communication) and a factor of approximately 4 (in power) larger than would be predicted by the simulations of the '' concordance '' cosmology reported in ; we discuss lower normalizations in x 7.…”

Section: Simulated Observationsmentioning

confidence: 99%

Studying Clusters withPlanck

White

2003

ApJ

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We use mock Sunyaev-Zeldovich effect maps to investigate how well the Planck mission might find and characterize clusters of galaxies. We discuss different combinations of frequency maps and different methods for identifying cluster candidates. For the simplest methods, the catalogs are not complete, even for relatively high mass thresholds, but the all-sky nature of the mission ensures a large sample of massive, high-z clusters that will be ideal for many studies. We make a preliminary attempt to identify the X-ray, optical, and weak-lensing properties of the Planck sample.

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The Anisotropy of the Microwave Background tol= 3500: Deep Field Observations with the Cosmic Background Imager

Cited by 265 publications

References 50 publications

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Three‐YearWilkinson Microwave Anisotropy Probe(WMAP) Observations: Temperature Analysis

Galaxy Clusters Discovered With a Sunyaev-Zel'dovich Effect Survey

Studying Clusters withPlanck

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