A Measurement of the Damping Tail of the Cosmic Microwave Background Power Spectrum With the South Pole Telescope

Keisler, R.; Reichardt, Christian; Aird, K. A.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Cho, H. M.; Crawford, T. M.; Crites, A. T.; Haan, T. de; Dobbs, M.; Dudley, J. P.; George, E. M.; Halverson, N. W.; Holder, G. P.; Holzapfel, W. L.; Hoover, S.; Hou, Z.; Hrubes, J. D.; Joy, M.; Knox, L.; Lee, A. T.; Leitch, E. M.; Lueker, M.; Luong-Van, D.; McMahon, Jeffrey; Mehl, J.; Meyer, S. S.; Millea, M.; Mohr, J. J.; Montroy, T. E.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Ruhl, J. E.; Schaffer, K. K.; Shaw, L.; Shirokoff, E.; Spieler, H.; Staniszewski, Z.; Stark, A. A.; Story, K. T.; Engelen, Alexander van; Vanderlinde, K.; Vieira, J. D.; Williamson, A. R.; Zahn, O.

doi:10.1088/0004-637x/743/1/28

Cited by 465 publications

(576 citation statements)

References 62 publications

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“…Our derived value of Ω b h 2 is in agreement, within the errors, with the ones derived from the WMAP-7 and Planck CMB data of respectively 0.0222±0.0004 (Keisler et al 2011) and 0.0221±0.00033 (68% CL) (Ade et al 2013).…”

Section: Cosmological Implicationssupporting

confidence: 90%

“…Although the data are still scarce -there are only ten absorption systems for which such a D/H measurement has been carried out (Pettini & Cooke 2012) -the measurements appear to converge to a mean primordial value D/H ∼ (2.5 -2.9) × 10 −5 , which corresponds to Ω b h 2 ∼ 0.0222 -0.0223 (Iocco et al 2009;Noterdaeme et al 2012;Pettini & Cooke 2012;Cooke et al 2014). This estimate of Ω b h 2 is in excellent agreeement with the value of 0.0221 -0.0222 obtained from studies of the fluctuations of the cosmic microwave background (CMB) with WMAP and Planck (Keisler et al 2011;Ade et al 2013). …”

Section: Introductionsupporting

confidence: 86%

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A new determination of the primordial He abundance using the He i λ10830 Å emission line: cosmological implications

Izotov¹,

Thuan²,

Гусева³

2014

Monthly Notices of the Royal Astronomical Society

254

355

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We present near-infrared spectroscopic observations of the high-intensity He i λ10830Å emission line in 45 low-metallicity H ii regions. We combined these NIR data with spectroscopic data in the optical range to derive the primordial He abundance. The use of the He i λ10830Å line, the intensity of which is very sensitive to the density of the H ii region, greatly improves the determination of the physical conditions in the He + zone. This results in a considerably tighter Y -O/H linear regression compared to all previous studies. We extracted a final sample of 28 H ii regions with Hβ equivalent width EW(Hβ) 150Å, excitation parameter O 2+ /O 0.8, and with helium mass fraction Y derived with an accuracy better than 3%. With this final sample we derived a primordial 4 He mass fraction Y p = 0.2551 ± 0.0022. The derived value of Y p is higher than the one predicted by the standard big bang nucleosynthesis (SBBN) model. Using our derived Y p together with D/H = (2.53±0.04)×10 −5 , and the χ 2 technique, we found that the best agreement between these light element abundances is achieved in a cosmological model with a baryon mass density Ω b h 2 = 0.0240±0.0017 (68% CL), ±0.0028 (95.4% CL), ±0.0034 (99% CL) and an effective number of neutrino species N eff = 3.58±0.25 (68% CL), ±0.40 (95.4% CL), ±0.50 (99% CL). A non-standard value of N eff is preferred at the 99% CL, implying the possible existence of additional types of neutrino species.

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Section: Cosmological Implicationssupporting

confidence: 90%

Section: Introductionsupporting

confidence: 86%

A new determination of the primordial He abundance using the He i λ10830 Å emission line: cosmological implications

Izotov¹,

Thuan²,

Гусева³

2014

Monthly Notices of the Royal Astronomical Society

254

355

View full text Add to dashboard Cite

show abstract

“…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%

“…The top-down naturalness of this mechanism remains to be established, and in particular no complete string theory realization has been constructed. 99 Another recent proposal, which we will now describe in some detail, is that inflation can be achieved by coupling an axion to non-Abelian gauge fields with suitable vevs [625,797] (see [815][816][817] and the review article [818] for 99 One way to achieve large α is to fine-tune two axion decay constants to be nearly coincident [767].…”

Section: Magnetic Driftmentioning

confidence: 99%

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