The Atacama Cosmology Telescope: DR4 Maps and Cosmological Parameters. (arXiv:2007.07288v1 [astro-ph.CO])

The Atacama Cosmology Telescope: DR4 Maps and Cosmological Parameters. (arXiv:2007.07288v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Aiola_S/0/1/0/all/0/1">Simone Aiola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maurin_L/0/1/0/all/0/1">Lo&#xef;c Maurin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naess_S/0/1/0/all/0/1">Sigurd Naess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmitt_B/0/1/0/all/0/1">Benjamin L. Schmitt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abitbol_M/0/1/0/all/0/1">Maximilian H. Abitbol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Addison_G/0/1/0/all/0/1">Graeme E. Addison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">Peter A. R. Ade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_D/0/1/0/all/0/1">David Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amiri_M/0/1/0/all/0/1">Mandana Amiri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amodeo_S/0/1/0/all/0/1">Stefania Amodeo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angile_E/0/1/0/all/0/1">Elio Angile</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austermann_J/0/1/0/all/0/1">Jason E. Austermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baildon_T/0/1/0/all/0/1">Taylor Baildon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nick Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beall_J/0/1/0/all/0/1">James A. Beall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_R/0/1/0/all/0/1">Rachel Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_D/0/1/0/all/0/1">Daniel T. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_J/0/1/0/all/0/1">J Richard Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruno_S/0/1/0/all/0/1">Sarah Marie Bruno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calafut_V/0/1/0/all/0/1">Victoria Calafut</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campusano_L/0/1/0/all/0/1">Luis E. Campusano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carrero_F/0/1/0/all/0/1">Felipe Carrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chesmore_G/0/1/0/all/0/1">Grace E. Chesmore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cho%2E_H/0/1/0/all/0/1">Hsiao-mei Cho.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">Steve K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_S/0/1/0/all/0/1">Susan E. Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cothard_N/0/1/0/all/0/1">Nicholas F. Cothard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crichton_D/0/1/0/all/0/1">Devin Crichton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crowley_K/0/1/0/all/0/1">Kevin T. Crowley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Darwish_O/0/1/0/all/0/1">Omar Darwish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Datta_R/0/1/0/all/0/1">Rahul Datta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Denison_E/0/1/0/all/0/1">Edward V. Denison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark J. Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duell_C/0/1/0/all/0/1">Cody J. Duell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duff_S/0/1/0/all/0/1">Shannon M. Duff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_A/0/1/0/all/0/1">Adriaan J. Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">Jo Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunner_R/0/1/0/all/0/1">Rolando D&#xfc;nner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Essinger_Hileman_T/0/1/0/all/0/1">Thomas Essinger-Hileman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fankhanel_M/0/1/0/all/0/1">Max Fankhanel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fox_A/0/1/0/all/0/1">Anna E. Fox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuzia_B/0/1/0/all/0/1">Brittany Fuzia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_P/0/1/0/all/0/1">Patricio A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gluscevic_V/0/1/0/all/0/1">Vera Gluscevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golec_J/0/1/0/all/0/1">Joseph E. Golec</a>, et al. (93 additional authors not shown)

We present new arcminute-resolution maps of the Cosmic Microwave Background
temperature and polarization anisotropy from the Atacama Cosmology Telescope,
using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than
17,000 deg$^2$, the deepest 600 deg$^2$ with noise levels below $10$
$mu$K-arcmin. We use the power spectrum derived from almost 6,000 deg$^2$ of
these maps to constrain cosmology. The ACT data enable a measurement of the
angular scale of features in both the divergence-like polarization and the
temperature anisotropy, tracing both the velocity and density at
last-scattering. From these one can derive the distance to the last-scattering
surface and thus infer the local expansion rate, $H_0$. By combining ACT data
with large-scale information from WMAP we measure $H_0=67.6pm 1.1$ km/s/Mpc,
at 68% confidence, in excellent agreement with the independently-measured
Planck satellite estimate (from ACT alone we find $H_0=67.9pm 1.5$ km/s/Mpc).
The $Lambda$CDM model provides a good fit to the ACT data, and we find no
evidence for deviations: both the spatial curvature, and the departure from the
standard lensing signal in the spectrum, are zero to within 1$sigma$; the
number of relativistic species, the primordial Helium fraction, and the running
of the spectral index are consistent with $Lambda$CDM predictions to within
1.5-2$sigma$. We compare ACT, WMAP, and Planck at the parameter level and find
good consistency; we investigate how the constraints on the correlated spectral
index and baryon density parameters readjust when adding CMB large-scale
information that ACT does not measure. The DR4 products presented here will be
publicly released on the NASA Legacy Archive for Microwave Background Data
Analysis.

We present new arcminute-resolution maps of the Cosmic Microwave Background
temperature and polarization anisotropy from the Atacama Cosmology Telescope,
using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than
17,000 deg$^2$, the deepest 600 deg$^2$ with noise levels below $10$
$mu$K-arcmin. We use the power spectrum derived from almost 6,000 deg$^2$ of
these maps to constrain cosmology. The ACT data enable a measurement of the
angular scale of features in both the divergence-like polarization and the
temperature anisotropy, tracing both the velocity and density at
last-scattering. From these one can derive the distance to the last-scattering
surface and thus infer the local expansion rate, $H_0$. By combining ACT data
with large-scale information from WMAP we measure $H_0=67.6pm 1.1$ km/s/Mpc,
at 68% confidence, in excellent agreement with the independently-measured
Planck satellite estimate (from ACT alone we find $H_0=67.9pm 1.5$ km/s/Mpc).
The $Lambda$CDM model provides a good fit to the ACT data, and we find no
evidence for deviations: both the spatial curvature, and the departure from the
standard lensing signal in the spectrum, are zero to within 1$sigma$; the
number of relativistic species, the primordial Helium fraction, and the running
of the spectral index are consistent with $Lambda$CDM predictions to within
1.5-2$sigma$. We compare ACT, WMAP, and Planck at the parameter level and find
good consistency; we investigate how the constraints on the correlated spectral
index and baryon density parameters readjust when adding CMB large-scale
information that ACT does not measure. The DR4 products presented here will be
publicly released on the NASA Legacy Archive for Microwave Background Data
Analysis.

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