The Atacama Cosmology Telescope: likelihood for small-scale CMB data

By J. Dunkley, E. Calabrese, Jonathan Sievers, G. Addison, Nicholas Battaglia, E. Battistelli, J. Richard Bond, S. Das, M. Devlin, R. Dunner and 25 more. 2013

150 citations recorded by the source corpus.

The Atacama Cosmology Telescope has measured the angular power spectra of microwave fluctuations to arcminute scales at frequencies of 148 and 218 GHz, from three seasons of data. At small scales the fluctuations in the primordial Cosmic Microwave Background (CMB) become increasingly obscured by extragalactic foregounds and secondary CMB signals. We present results from a nine-parameter model describing these secondary effects, including the thermal and kinematic Sunyaev-Zel'dovich (tSZ and kSZ) power; the clustered and Poisson-like power from Cosmic Infrared Background (CIB) sources, and their frequency scaling; the tSZ-CIB correlation coefficient; the extragalactic radio source power; and thermal dust emission from Galactic cirrus in two different regions of the sky. In order to extract cosmological parameters, we describe a likelihood function for the ACT data, fitting this model to the multi-frequency spectra in the multipole range 500 < ℓ < 10000. We extend the likelihood to include spectra from the South Pole Telescope at frequencies of 95, 150, and 220 GHz. Accounting for different radio source levels and Galactic cirrus emission, the same model provides an excellent fit to both datasets simultaneously, with χ2/dof= 675/697 for ACT, and 96/107 for SPT. We then use the multi-frequency likelihood to estimate the CMB power spectrum from ACT in bandpowers, marginalizing over the secondary parameters. This provides a simplified `CMB-only' likelihood in the range 500 < ℓ < 3500 for use in cosmological parameter estimation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/97e3210165c033eaee7084d1b7e80a63a6d05646

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Citations in the corpus

CMB-S4 Science Case, Reference Design, and Project Plan (2019, methodology): “The Galactic cirrus template comes from the treatment of [572].”
Planck2015 results (2015, unknown): “PPL13 and PCP13 used a parametric approach to modelling foregrounds, similar to the approach adopted in the analysis of the SPT and ACT experiments (Reichardt et al. 2012; Dunkley et al. 2013).”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, background): “These numbers have to be compared withD = (54±16) and (4.8±0.9) μK2CMB for ACT at 219.6 and 149.7 GHz, respectively (Dunkley et al. 2013); andD = (56±4) and (6.2 ± 0.5) μK2CMB for SPT at 219.6 and 153.8 GHz, respectively (Reichardt et al. 2012).”
Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy (2017, methodology): “The mixing of colors visible in the ACTPol and SPT panels reflects additional degeneracy between H0 and other parameters arising from the more limited range of angular scales provided by these data.”
THE 1% CONCORDANCE HUBBLE CONSTANT (2014, methodology): “A code that incorporates both ACT and SPT temperature likelihoods, called actlite, is described in Section 5 of Dunkley et al. (2013), and has been made available on LAMBDA1.”
The Atacama Cosmology Telescope: two-season ACTPol spectra and parameters (2016, methodology): “This model all follows Dunkley et al. (2013).”
The Phenomenology of Right Handed Neutrinos (2013, methodology): “this is consistent with the Neﬀ ≃ 4 predicted by a thermalized sterile neutrino with masses and mixing suggested by the oscillation anomalies, but also does not rule out the SS. In contrast, ACT+WMAP [293, 294] favours Neﬀ = 2.79 ± 0.56, which would clearly rule out thermal DR. This is in contrast t”
MontePython 3: Boosted MCMC sampler and other features (2018, background): “0 W [73] [74] Planck highl Planck 2015: TT high ` CMB 2.”
Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters (2015, methodology): “As described in Planck Collaboration XIII (2016), we then take a further step and extend the Gibbs technique presented in Dunkley et al. (2013) and Calabrese et al. (2013) (and applied to Planck alone in Sect.”
The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data (2013, methodology): “Dunkley et al. (2013) use the temperature band-powers reported in this work to generate likelihood functions which form the basis of the cosmological parameter constraints reported by Sievers et al. (2012).”
The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, unknown): “The total degrees of freedom are therefore 8169 or 8168 if we consider the 19 or 20 parameter models. c In Table 2 of Dunkley et al. (2013), the secondary parameters, including calibrations, are reported assuming a best-ﬁtting cosmological model.”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “Dunkley et al. (2013) use the power spectra presented in Das et al. (2014) to measure 3 DtSZ3000 = 3.3± 1.4µK2 and DkSZ3000 < 8.6µK2 (95% CL) at 150 GHz.”
The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000 (2014, unknown): “We repeat the same test with just the ACTPol TT data, including the foreground model as in Dunkley et al. (2013) to account for Poisson and clustered point sources and the thermal and kinematic Sunyaev-Zel’dovich effects.”
Planck 2015 results: XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation (2015, unknown): “The ACT collaboration sets an upper limit ρ < 0.2 on the tSZ-CIB cross correlation (Dunkley et al. 2013).”