Status of CMB polarization measurements from DASI and other experiments

Carlstrom, J. E.; Kovac, J. M.; Leitch, E. M.; Pryke, C.

doi:10.1016/j.newar.2003.09.007

Cited by 9 publications

(11 citation statements)

References 49 publications

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“…Studies of the cosmic microwave background (CMB) have dramatically progressed over the past two decades (e.g., Smoot et al 1992;Cheng et al 1997;Baker et al 1999;Miller et al 1999;de Bernardis et al 2000;Knox & Page 2000;Hanany et al 2000;Lee et al 2001;Romeo et al 2001;Netterfield et al 2002;Halverson et al 2002;Kovac et al 2002;Carlstrom et al 2003;Pearson et al 2003;Scott et al 2003;Benoît et al 2003;Spergel et al 2003;Johnson et al 2007;Chiang et al 2010). The current ΛCDM cosmological model provides an excellent fit to the CMB data across a wide range of angular scales, and is supported by complementary observations of large scale structure (e.g., Reid et al 2012;Ho et al 2012), Baryon Acoustic Oscillations (BAO e.g., Blake et al 2011;Anderson et al 2012;Busca et al 2013), Type Ia supernovae (e.g., Hicken et al 2009;Kessler et al 2009;Conley et al 2011), galaxy cluster measurements (e.g., Vikhlinin et al 2009;Mantz et al 2010;Rozo et al 2010;Tinker et al 2012) and observations of gravitational lensing (e.g., Massey et al 2007;Fu et al 2008;Schrabback et al 2010;Suyu et al 2010;Heymans et al 2012;Kilbinger et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Atacama Cosmology Telescope: cosmological parameters from three seasons of data

Sievers

Hložek

Nolta

et al. 2013

J. Cosmol. Astropart. Phys.

326

287

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We present constraints on cosmological and astrophysical parameters from high-resolution microwave background maps at 148 GHz and 218 GHz made by the Atacama Cosmology Telescope (ACT) in three seasons of observations from 2008 to 2010. A model of primary cosmological and secondary foreground parameters is fit to the map power spectra and lensing deflection power spectrum, including contributions from both the thermal Sunyaev-Zeldovich (tSZ) effect and the kinematic Sunyaev-Zeldovich (kSZ) effect, Poisson and correlated anisotropy from unresolved infrared sources, radio sources, and the correlation between the tSZ effect and infrared sources. The power ℓ 2 C ℓ /2π of the thermal SZ power spectrum at 148 GHz is measured to be 3.4 ± 1.4 µK 2 at ℓ = 3000, while the corresponding amplitude of the kinematic SZ power spectrum has a 95% confidence level upper limit of 8.6 µK 2. Combining ACT power spectra with the WMAP 7-year temperature and polarization power spectra, we find excellent consistency with the LCDM model. We constrain the number of effective relativistic degrees of freedom in the early universe to be N eff = 2.79 ± 0.56, in agreement with the canonical value of N eff = 3.046 for three massless neutrinos. We constrain the sum of the neutrino masses to be Σm ν < 0.39 eV at 95% confidence when combining ACT and WMAP 7-year data with BAO and Hubble constant measurements. We constrain the amount of primordial helium to be Y p = 0.225 ± 0.034, and measure no variation in the fine structure constant α since recombination, with α/α 0 = 1.004 ± 0.005. We also find no evidence for any running of the scalar spectral index, dn s /d ln k = −0.004 ± 0.012.

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Section: Introductionmentioning

confidence: 99%

The Atacama Cosmology Telescope: cosmological parameters from three seasons of data

Sievers

Hložek

Nolta

et al. 2013

J. Cosmol. Astropart. Phys.

326

287

View full text Add to dashboard Cite

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“…For ground based observations the window channels at 40, 90 and 140 GHz are optimum due to the low atmospheric attenuation at these frequencies. To this date the 40 and 90 GHz channels have been used in several LNA based experiments [7], however, the LNA technology has not been sufficiently low noise at 140 GHz range. Thus, by adding the 140 GHz LNA capability the complete CMB measurement can be carried out using cryogenically cooled (T=20 K) InP MMIC LNAs.…”

Section: Cosmic Microwave Background Imagersmentioning

confidence: 99%

Broadband Characterization of a 100 to 180 GHz Amplifier

Kangaslahti

Deal

Mei

et al. 2008

2008 IEEE Aerospace Conference

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“…By comparing the measured CMB power spectra with theoretical predictions, the WMAP team determined the cosmological parameters with a few percent precision (Spergel et al , 2007Komatsu et al 2009Komatsu et al , 2011, and found that the observed CMB fluctuations are consistent with predictions of the concordance ΛCDM model with scaleinvariant adiabatic fluctuations generated during the inflationary epoch Peiris et al 2003;Komatsu et al 2011). Recent ground-based and balloon-borne experiments that have performed CMB power spectrum measurement and cosmological parameter estimation include the South Pole Telescope (SPT; Keisler et al 2011), the QUaD experiment (Brown et al 2009), the Arcminute Cosmology Bolometer Array Receiver (ACBAR; Reichardt et al 2009), the Cosmic Background Imager (CBI; Mason et al 2003), the Atacama Cosmology Telescope (ACT; Fowler et al 2010), the Degree Angular Scale Interferometer (DASI; Carlstrom et al 2003), BOOMERANG (Jones et al 2006), Archeops (Benoît et al 2003), and MAXIMA (Lee et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Local Anomalies Around the Third Peak in the CMB Angular Power Spectrum of Wmap 7-Year Data

Ko¹,

Park²,

Hwang³

2013

Journal of The Korean Astronomical Society

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We estimate the power spectra of the cosmic microwave background radiation (CMB) temperature anisotropy in localized regions of the sky using the Wilkinson Microwave Anisotropy Probe (WMAP) 7-year data. We find that the north and south hat regions at high Galactic latitude (|b| ≥ 30• ) show an anomaly in the power spectrum amplitude around the third peak, which is statistically significant up to 3σ. We try to explain the cause of the observed anomaly by analyzing the low Galactic latitude (|b| < 30• ) regions where the galaxy contamination is expected to be stronger, and the regions weakly or strongly dominated by WMAP instrument noise. We also consider the possible effect of unresolved radio point sources. We find another but less statistically significant anomaly in the low Galactic latitude north and south regions whose behavior is opposite to the one at high latitude. Our analysis shows that the observed north-south anomaly at high latitude becomes weaker on regions with high number of observations (weak instrument noise), suggesting that the anomaly is significant at sky regions that are dominated by the WMAP instrument noise. We have checked that the observed north-south anomaly has weak dependences on the bin-width used in the power spectrum estimation, and on the Galactic latitude cut. We also discuss the possibility that the detected anomaly may hinge on the particular choice of the multipole bin around the third peak. We anticipate that the issue of whether or not the anomaly is intrinsic one or due to WMAP instrument noise will be resolved by the forthcoming Planck data.

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Status of CMB polarization measurements from DASI and other experiments

Cited by 9 publications

References 49 publications

The Atacama Cosmology Telescope: cosmological parameters from three seasons of data

The Atacama Cosmology Telescope: cosmological parameters from three seasons of data

Broadband Characterization of a 100 to 180 GHz Amplifier

Local Anomalies Around the Third Peak in the CMB Angular Power Spectrum of Wmap 7-Year Data

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