Degree Angular Scale Interferometer First Results: A Measurement of the Cosmic Microwave Background Angular Power Spectrum

Halverson, N. W.; Leitch, E. M.; Pryke, C.; Kovac, J. M.; Carlstrom, J. E.; Holzapfel, W. L.; Dragovan, M.; Cartwright, J. K.; Mason, B. S.; Padin, S.; Pearson, T. J.; Readhead, A. C. S.; Shepherd, M. C.

doi:10.1086/338879

Cited by 669 publications

(356 citation statements)

References 35 publications

Supporting

Mentioning

334

Contrasting

Unclassified

Order By: Relevance

“…(Fig. 10) with the measurements from BOOMERANG (Netterfield et al 2002), DASI (Halverson et al 2002), and MAXIMA (Lee et al 2001). The rectangles indicate the 68% confidence intervals on band power; for BOOMERANG, the filled rectangles indicate the 68% confidence interval for the statistical and sample variance errors, while the hatched rectangles show the amount by which a AE1 error in the beamwidth (12<9 AE 1<4) would shift the estimates (all up or all down together).…”

Section: Joint Mosaic Power Spectrummentioning

confidence: 86%

“…The power of accurate measurements of the CMB power spectrum to constrain cosmological models and obtain precise estimates of critical cosmological parameters has been demonstrated by many theoretical and observational studies. The most recent experiments, i.e., the BOOMERANG (Netterfield et al 2002) and MAXIMA (Lee et al 2001) balloon-borne bolometers and the DASI interferometer array at the South Pole (Halverson et al 2002), have measured the power spectrum at multipoles ld1000 (angular scales e20 0 ). The CBI has the potential to extend these measurements to l $ 3500.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Pearson

Mason

Readhead

et al. 2003

ApJ

Self Cite

265

157

View full text Add to dashboard Cite

Using the Cosmic Background Imager (CBI), a 13-element interferometer array operating in the 26-36 GHz frequency band, we have observed 40 deg 2 of sky in three pairs of fields, each $145 0 Â 165 0 , using overlapping pointings (mosaicking). We present images and power spectra of the cosmic microwave background radiation in these mosaic fields. We remove ground radiation and other low-level contaminating signals by differencing matched observations of the fields in each pair. The primary foreground contamination is due to point sources (radio galaxies and quasars). We have subtracted the strongest sources from the data using higher resolution measurements, and we have projected out the response to other sources of known position in the power spectrum analysis. The images show features on scales $6 0 -15 0 , corresponding to masses $ð5 80Þ Â 10 14 M at the surface of last scattering, which are likely to be the seeds of clusters of galaxies. The power spectrum estimates have a resolution Dl % 200 and are consistent with earlier results in the multipole range ld1000. The power spectrum is detected with high signal-to-noise ratio in the range 300dld1700. For 1700dld3000 the observations are consistent with the results from more sensitive CBI deep field observations. The results agree with the extrapolation of cosmological models fitted to observations at lower l and show the predicted drop at high l (the '' damping tail '').

show abstract

Section: Joint Mosaic Power Spectrummentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

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

Pearson

Mason

Readhead

et al. 2003

ApJ

Self Cite

265

157

View full text Add to dashboard Cite

show abstract

“…The astonishing advances in our understanding of the basic properties of the Universe and in precision determinations of its fundamental parameters made possible by the recent accurate measurements of acoustic peaks of the Cosmic Microwave Background (CMB) anisotropy power spectrum by the TOCO (Miller et al 1999), BOOMERanG (de Bernardis et al 2002), MAXIMA (Lee et al 2001), DASI (Halverson et al 2002), and CBI (Pearson et al 2002) experiments, have put further impetus in experimental efforts to exploit the extraordinary wealth of cosmological information carried by the CMB.…”

Section: Introductionmentioning

confidence: 99%

Polarization properties of extragalactic radio sources and their contribution to microwave polarization fluctuations

Mesa

Baccigalupi

Zotti

et al. 2002

A&A

103

View full text Add to dashboard Cite

Abstract. We investigate the statistical properties of the polarized emission of extragalactic radio sources and estimate their contribution to the power spectrum of polarization fluctuations in the microwave region. The basic ingredients of our analysis are the NVSS polarization data, the multifrequency study of polarization properties of the B3-VLA sample (Mack et al. 2002) which has allowed us to quantify Faraday depolarization effects, and the 15 GHz survey by Taylor et al. (2001), which has provided strong constraints on the high-frequency spectral indices of sources. The polarization degree of both steep-and flatspectrum sources at 1.4 GHz is found to be anti-correlated with the flux density. The median polarization degree at 1.4 GHz of both steep-and flat-spectrum sources brighter than S (1.4 GHz) = 80 mJy is 2.2%. The data by Mack et al. (2002) indicate a substantial mean Faraday depolarization at 1.4 GHz for steep spectrum sources, while the depolarization is undetermined for most flat/inverted-spectrum sources. Exploiting this complex of information we have estimated the power spectrum of polarization fluctuations due to extragalactic radio sources at microwave frequencies. We confirm that extragalactic sources are expected to be the main contaminant of Cosmic Microwave Background (CMB) polarization maps on small angular scales. At frequencies <30 GHz the amplitude of their power spectrum is expected to be comparable to that of the E-mode of the CMB. At higher frequencies, however, the CMB dominates.

show abstract

“…A plethora of phenomena are explained by the best-fit ΛCDM model, which complies with the cosmological principles of homogeneity and isotropy. For over a decade it has withstood serious challenges brought forth by comparison with high-precision data delivered by the WMAP satellite (Bennett et al 2003(Bennett et al , 2013Hinshaw et al 2007Hinshaw et al , 2009Jarosik et al 2011), not to mention other numerous experiments, such as BOOMERanG (de Bernardis et al 2002), MAXIMA (Lee et al 2001), DASI (Halverson et al 2002), ACBAR (Kuo et al 2007), and others.…”

Section: Introductionmentioning

confidence: 99%

Testing for foreground residuals in thePlanckforeground cleaned maps: A new method for designing confidence masks

Axelsson

Ihle

Scodeller

et al. 2015

A&A

View full text Add to dashboard Cite

We test for foreground residuals in the foreground-cleaned Planck cosmic microwave background (CMB) maps outside and inside the U73 mask commonly used for cosmological analysis. The aim of this paper is to introduce a new method of validating masks by looking at the differences in cleaned maps obtained by different component-separation methods. By analyzing the power spectrum, as well as the mean, rms, and skewness of needlet coefficients on separate equatorial bands running from the poles to the equator outside and inside the U73 mask, we first confirm that the pixels already masked by U73 are highly contaminated and cannot be used for cosmological analysis. We further find that the U73 mask needs extension in order to reduce large-scale foreground residuals to a level of less than 20% of the standard deviation of CMB fluctuations within the bands closest to the galactic equator. We also find 276 point-like residuals in the cleaned foreground maps that are currently not masked by the U73 mask. About 80 of these are identified as sz clusters that have not been properly subtracted by the component separation methods, and the rest are strongly correlated with the Planck dust map, indicating point-like dust residuals. Our final publicly available extended mask leaves 65.9% of the sky for cosmological analysis. This extended mask may be important for analyses on local sky patches; for the full sky power spectrum, we have shown that the unmasked residuals have very little impact.

show abstract

Degree Angular Scale Interferometer First Results: A Measurement of the Cosmic Microwave Background Angular Power Spectrum

Cited by 669 publications

References 35 publications

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

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

Polarization properties of extragalactic radio sources and their contribution to microwave polarization fluctuations

Testing for foreground residuals in thePlanckforeground cleaned maps: A new method for designing confidence masks

Contact Info

Product

Resources

About