The Atacama Cosmology Telescope: Measurement and Analysis of 1D Beams for DR4. (arXiv:2112.12226v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lungu_M/0/1/0/all/0/1">Marius Lungu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Storer_E/0/1/0/all/0/1">Emilie R. Storer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasselfield_M/0/1/0/all/0/1">Matthew Hasselfield</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:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</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:+Choi_S/0/1/0/all/0/1">Steve K. Choi</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:+Gallardo_P/0/1/0/all/0/1">Patricio A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golec_J/0/1/0/all/0/1">Joseph E. Golec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guan_Y/0/1/0/all/0/1">Yilun Guan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Colin Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hincks_A/0/1/0/all/0/1">Adam D. Hincks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubmayr_J/0/1/0/all/0/1">Johannes Hubmayr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madhavacheril_M/0/1/0/all/0/1">Mathew S. Madhavacheril</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mallaby_Kay_M/0/1/0/all/0/1">Maya Mallaby-Kay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">Jeff McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moodley_K/0/1/0/all/0/1">Kavilan Moodley</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:+Nati_F/0/1/0/all/0/1">Federico Nati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemack_M/0/1/0/all/0/1">Michael D. Niemack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Page_L/0/1/0/all/0/1">Lyman A. Page</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Partridge_B/0/1/0/all/0/1">Bruce Partridge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puddu_R/0/1/0/all/0/1">Roberto Puddu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schillaci_A/0/1/0/all/0/1">Alessandro Schillaci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sifon_C/0/1/0/all/0/1">Crist&#xf3;bal Sif&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Staggs_S/0/1/0/all/0/1">Suzanne Staggs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sunder_D/0/1/0/all/0/1">Dhaneshwar D. Sunder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wollack_E/0/1/0/all/0/1">Edward J. Wollack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Z/0/1/0/all/0/1">Zhilei Xu</a>

We describe the measurement and treatment of the telescope beams for the
Atacama Cosmology Telescope’s fourth data release, DR4. Observations of Uranus
are used to measure the central portion (<12′) of the beams to roughly -40 dB
of the peak. Such planet maps in intensity are used to construct azimuthally
averaged beam profiles, which are fit with a physically motivated model before
being transformed into Fourier space. We investigate and quantify a number of
percent-level corrections to the beam, all of which are important for precision
cosmology. Uranus maps in polarization are used to measure the
temperature-to-polarization leakage in the main part of the beams, which is <1%
(2.5%) at 150 GHz (98 GHz). The beams also have polarized sidelobes, which are
measured with observations of Saturn and deprojected from the ACT time-ordered
data. Notable changes relative to past ACT beam analyses include an improved
subtraction of the atmospheric effects from Uranus calibration maps,
incorporation of a scattering term in the beam profile model, and refinements
to the beam model uncertainties and the main temperature-to-polarization
leakage terms in the ACT power spectrum analysis.

We describe the measurement and treatment of the telescope beams for the
Atacama Cosmology Telescope’s fourth data release, DR4. Observations of Uranus
are used to measure the central portion (<12′) of the beams to roughly -40 dB
of the peak. Such planet maps in intensity are used to construct azimuthally
averaged beam profiles, which are fit with a physically motivated model before
being transformed into Fourier space. We investigate and quantify a number of
percent-level corrections to the beam, all of which are important for precision
cosmology. Uranus maps in polarization are used to measure the
temperature-to-polarization leakage in the main part of the beams, which is <1%
(2.5%) at 150 GHz (98 GHz). The beams also have polarized sidelobes, which are
measured with observations of Saturn and deprojected from the ACT time-ordered
data. Notable changes relative to past ACT beam analyses include an improved
subtraction of the atmospheric effects from Uranus calibration maps,
incorporation of a scattering term in the beam profile model, and refinements
to the beam model uncertainties and the main temperature-to-polarization
leakage terms in the ACT power spectrum analysis.

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