Kavli Affiliate: Chao-Lin Kuo
| First 5 Authors: J. A. Zebrowski, C. L. Reichardt, A. J. Anderson, B. Ansarinejad, M. Archipley
| Summary:
We present a measurement of the $B$-mode polarization power spectrum of the
cosmic microwave background anisotropies at 32 $le$ $ell$ $<$ 502 for three
bands centered at 95, 150, and 220 GHz using data from the SPT-3G receiver on
the South Pole Telescope. This work uses SPT-3G observations from the 2019 and
2020 winter observing seasons of a $sim$1500 deg$^2$ patch of sky that
directly overlaps with fields observed with the BICEP/Keck family of
telescopes, and covers part of the proposed Simons Observatory and CMB-S4 deep
fields. Employing new techniques for mitigating polarized atmospheric noise,
the SPT-3G data demonstrates a white noise level of 9.3 (6.7) $mu$K-arcmin at
$ell sim 500$ for the 95 GHz (150 GHz) data, with a $1/ell$ noise knee at
$ell$=128 (182). We fit the observed six auto- and cross-frequency $B$-mode
power spectra to a model including lensed $Lambda$CDM $B$-modes and a
combination of Galactic and extragalactic foregrounds. This work characterizes
foregrounds in the vicinity of the BICEP/Keck survey area, finding foreground
power consistent with that reported by the BICEP/Keck collaboration within the
same region, and a factor of $sim$ 3 higher power over the full SPT-3G survey
area. Using SPT-3G data over the BICEP/Keck survey area, we place a 95% upper
limit on the tensor-to-scalar ratio of $r < 0.25$ and find the statistical
uncertainty on $r$ to be $sigma(r) = 0.067$.
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