THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 AND 218 GHz FROM THE 2008 SOUTHERN SURVEY

Das, Sudeep; Marriage, Tobias A.; Ade, Peter A. R.; Aguirre, Paula; Amiri, M.; Appel, John W.; Barrientos, L. Felipe; Battistelli, E. S.; Bond, J. R.; Brown, Ben; Burger, B.; Chervenak, J. A.; Devlin, Mark J.; Dicker, Simon; Doriese, W. B.; Dunkley, Joanna; Dünner, Rolando; Essinger‐Hileman, T.; Fisher, R. P.; Fowler, Joseph W.; Hajian, Amir; Halpern, M.; Hasselfield, Matthew; Hernández-Monteagudo, C.; Hilton, G. C.; Hilton, Matt; Hincks, Adam D.; Hložek, Renée; Huffenberger, K. M.; Hughes, D. H.; Hughes, John P.; Infante, L.; Irwin, K. D.; Juin, J. B.; Kaul, Madhuri; Klein, Jeff; Kosowsky, Arthur; Lau, Judy M.; Limon, M.; Lin, Yen-Ting; Lupton, Robert H.; Marsden, Danica; Martocci, Krista; Mauskopf, Philip Daniel; Menanteau, F.; Moodley, Kavilan; Moseley, H.; Netterfield, C. B.; Niemack, Michael D.; Nolta, Michael R.; Page, Lyman A.; Parker, Lucas; Partridge, B.; Reid, Beth; Sehgal, Neelima; Sherwin, Blake D.; Sievers, Jonathan; Spergel, David N.; Staggs, Suzanne T.; Swetz, Daniel S.; Switzer, Eric R.; Thornton, Robert J.; Trac, Hy; Tucker, C.; Warne, Ryan; Wollack, Edward J.; Zhao, Yue

doi:10.1088/0004-637x/729/1/62

Cited by 162 publications

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“…Together with the measurements of the CMB damping tail by the Atacama Cosmology Telescope (ACT) [97,98] and the South Pole Telescope (SPT) [99,100] this provides a beautiful picture of the first seven acoustic peaks of the CMB power spectrum. In this section, we summarize how the CMB results have tested the physics of inflation [9,10].…”

Section: Current Tests Of Inflationmentioning

confidence: 91%

“…CMB observations continue to provide important measurements of the primordial fluctuations, especially on small angular scales [97][98][99][100]. A large number of ground-based and balloon-borne experiments are targeting high-precision measurements of CMB polarization.…”

Section: Future Tests Of Inflationmentioning

confidence: 99%

“…Although the KS throat provides a rare example of a warped throat that is smooth in the infrared, here we will also consider more general warped Calabi-Yau cones, with ten-dimensional line element 96) where Vol(X 5 ) denotes the volume of X 5 (in string units). For a throat of the form (5.95), the range of the canonically-normalized D3-brane position is given, as in (5.28), by [243] ∆φ 97) and in particular is independent of X 5 . We will see in §5.3.5 that if one manages to achieve a DBI phase, (5.97) provides a stringent upper bound on the tensor-to-scalar ratio.…”

Section: Dirac-born-infeld Inflationmentioning

confidence: 99%

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Inflation and String Theory

2015

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Section: Current Tests Of Inflationmentioning

confidence: 91%

Section: Future Tests Of Inflationmentioning

confidence: 99%

Section: Dirac-born-infeld Inflationmentioning

confidence: 99%

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Inflation and String Theory

2015

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“…The ∆N eff is equal to the energy fraction of a Goldstone boson relative to a single neutrino: ∆N eff = T 4 α /(7/4T 4 ν ) = 4/7(43/57) 4/3 = 0.39. Actually WMAP9 and ground-based observations [53][54][55] give N eff = 3.89 ± 0.67 and Planck, the WMAP9 polarization and ground-based observations [56][57][58][59] give N eff = 3.36 ± 0.34, both at the 68% confidence leve, suggesting possible deviation from the SM prediction although the errors are large. For example, with λ Hϕ = −0.005(−0.0001) and m H = 125 GeV, the dark scalar with mass 500 MeV (70 MeV) can satisfy the condition.…”

Section: Jhep09(2014)153mentioning

confidence: 99%

Can Zee-Babu model implemented with scalar dark matter explain both Fermi-LAT 130 GeV γ-ray excess and neutrino physics?

Baek¹,

Ko²,

Okada³

et al. 2014

J. High Energ. Phys.

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Abstract:We extend the Zee-Babu model for the neutrino masses and mixings by first incorporating a scalar dark matter X with Z 2 symmetry and then X and a dark scalar ϕ with global U(1) symmetry. In the latter scenario the singly and doubly charged scalars that are new in the Zee-Babu model can explain the large annihilation cross section of a dark matter pair into two photons as hinted by the recent analysis of the Fermi γ-ray space telescope data. These new scalars can also enhance the B(H → γγ), as the recent LHC results may suggest. The dark matter relic density can be explained. The direct detection rate of the dark matter is predicted to be about one order of magnitude down from the current experimental bound in the first scenario.

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“…It has been measured over the whole sky by COBE and WMAP, and over smaller regions by ground-based and sub-orbital experiments (e.g., Tristram et al 2005;Jones et al 2006;Reichardt et al 2009;Fowler et al 2010;Das et al 2011;Keisler et al 2011;Story et al 2013;Das et al 2014). By mapping the whole sky to scales of a few arc minutes, Planck now measures the power spectrum over an unprecedented range of scales from a single experiment.…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XV. CMB power spectra and likelihood

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

392

263

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This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, , covering 2 ≤ ≤ 2500. The main source of uncertainty at < ∼ 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher s. For < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At ≥ 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high-cross-spectra with residuals below a few µK 2 at < ∼ 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ΛCDM cosmology is in excellent agreement with preliminary Planck EE and T E polarisation spectra. We find that the standard ΛCDM cosmology is well constrained by Planck from the measurements at < ∼ 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4σ deviation from scale invariance, n s = 1. Increasing the multipole range beyond 1500 does not increase our accuracy for the ΛCDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the ΛCDM framework. Finally, we report a tension between the Planck best-fit ΛCDM model and the low-spectrum in the form of a power deficit of 5-10% at < ∼ 40, with a statistical significance of 2.5-3σ. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.

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THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 AND 218 GHz FROM THE 2008 SOUTHERN SURVEY

Cited by 162 publications

References 50 publications

Inflation and String Theory

Inflation and String Theory

Can Zee-Babu model implemented with scalar dark matter explain both Fermi-LAT 130 GeV γ-ray excess and neutrino physics?

Planck2013 results. XV. CMB power spectra and likelihood

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