The Atacama Cosmology Telescope: two-season ACTPol spectra and parameters

By T. Louis, E. Grace, M. Hasselfield, M. Lungu, L. Maurin, G. Addison, P. Ade, S. Aiola, R. Allison, M. Amiri and 73 more. Journal of Cosmology and Astroparticle Physics, 2016

203 citations recorded by the source corpus.

We present the temperature and polarization angular power spectra measured by the Atacama Cosmology Telescope Polarimeter (ACTPol). We analyze night-time data collected during 2013–14 using two detector arrays at 149 GHz, from 548 deg2 of sky on the celestial equator. We use these spectra, and the spectra measured with the MBAC camera on ACT from 2008–10, in combination with planck and wmap data to estimate cosmological parameters from the temperature, polarization, and temperature-polarization cross-correlations. We find the new ACTPol data to be consistent with the ΛCDM model. The ACTPol temperature-polarization cross-spectrum now provides stronger constraints on multiple parameters than the ACTPol temperature spectrum, including the baryon density, the acoustic peak angular scale, and the derived Hubble constant. The new ACTPol data provide information on damping tail parameters. The joint uncertainty on the number of neutrino species and the primordial helium fraction is reduced by 20% when adding ACTPol to Planck temperature data alone.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/91bd4737f8116a0945c54e0a1f1e11027f23a528

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Citations in the corpus

Sounds Discordant: Classical Distance Ladder and ΛCDM-based Determinations of the Cosmological Sound Horizon (2018, methodology): “We use the CMB data sets from the Atacama Cosmology Telescope (ACTPol; Louis et al. 2017), Planck (Planck Collaboration VI 2018), the South Pole Telescope: SPT-SZ (Aylor et al. 2017) and SPTpol (Henning et al. 2018), and the WMAP (Bennett et al. 2013).”
Early dark energy does not restore cosmological concordance (2020, background): “The cosmic microwave background (CMB) allows for a precise, albeit indirect, inference of the Hubble constant in the context of a cosmological model (Hinshaw et al. (2013); Ade et al. (2014, 2016); Aghanim et al. (2018); Louis et al. (2017); Bianchini et al. (2019)).”
Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data (2021, methodology): “1600), and ground-based observations extend these measurements to arcminute scales, at which point foregrounds begin to dominate over the primary CMB temperature signal [2, 3].”
The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth (2023, methodology): “We mask Fourier modes with |`x| < 90 and |`y| < 50 to remove this contamination as in Louis et al. (2017); Choi et al. (2020).”
The Simons Observatory: science goals and forecasts (2018, methodology): “…and CIB clustered component; 0.5 µK2 of Galactic dust emission; 1 µK2 for radio sources in EE (this is based on a very conservative upper level, as no polarized sources were masked in the analysis of Louis et al. 2017), and no emission in TE (consistently with what was found in Louis et al. 2017).”
Dark Energy Survey Year 1 Results: A Precise H0 Estimate from DES Y1, BAO, and D/H Data (2017, methodology): “A similar analysis to that of Henning et al. (2018) using data from the Atacama Cosmology Telescope is presented in Louis et al. (2017).”
Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy (2017, methodology): “Both ACT and ACTPol prefer a lower H0 value than WMAP alone (Sievers et al. 2013; Louis et al. 2017).”
A unified pseudo-Cℓ framework (2018, methodology): “…by current groundbased Stage-3 experiments such as BICEP/Keck (BICEP2 Collaboration et al. 2016), Advanced ACTPol (De Bernardis et al. 2016; Louis et al. 2017) or the Simons Array (Suzuki et al. 2016; POLARBEAR Collaboration et al. 2017), as well as next-generation facilities such as the…”
CMB-S4: Forecasting Constraints on Primordial Gravitational Waves (2020, methodology): “…performance, we use noise parameters (see Equation 7) that are more in tune with what has been achieved by LATs at the time of this forecasting (Louis et al. 2017; Henning et al. 2018), i.e., the 1/f noise component is characterized by an `knee = 200, keeping γ – the slope of this component –…”
PICO: Probe of Inflation and Cosmic Origins (2019, background): “Also shown are measurements of lensing from current experiments (left, orange) [27–30], Planck’s EE measurements (left, dark blue) [31], and the BB spectrum produced by an inflationary gravity wave (GW) signal with different values of r (cyan).”