- M. Archipley, et al., — Millimeter-wave observations of Euclid Deep Field South using the South
Pole Telescope: A data release of temperature maps and catalogs
- Context. The South Pole Telescope third-generation camera (SPT-3G) has
observed over 10,000 square degrees of sky at 95, 150, and 220 GHz (3.3, 2.0,
1.4 mm, respectively) overlapping the ongoing 14,000 square-degree Euclid Wide
Survey. The Euclid collaboration recently released Euclid Deep Field
observations in the first quick data release (Q1). Aims. With the goal of
releasing complementary millimeter-wave data and encouraging legacy science, we
performed dedicated observations of a 57-square-degree field overlapping the
Euclid Deep Field South (EDF-S). Methods. The observing time totaled 20 days
and we reached noise depths of 4.3, 3.8, and 13.2 $\mu$K-arcmin at 95, 150, and
220 GHz, respectively. Results. In this work we present the temperature maps
and two catalogs constructed from these data. The emissive source catalog
contains 601 objects (334 inside EDF-S) with 54% synchrotron-dominated sources
and 46% thermal dust emission-dominated sources. The 5$\sigma$ detection
thresholds are 1.7, 2.0, and 6.5 mJy in the three bands. The cluster catalog
contains 217 cluster candidates (121 inside EDF-S) with median mass
$M_{500c}=2.12 \times 10^{14} M_{\odot}/h_{70}$ and median redshift $z$ = 0.70,
corresponding to an order-of-magnitude improvement in cluster density over
previous tSZ-selected catalogs in this region (3.81 clusters per square
degree). Conclusions. The overlap between SPT and Euclid data will enable a
range of multiwavelength studies of the aforementioned source populations. This
work serves as the first step towards joint projects between SPT and Euclid and
provides a rich dataset containing information on galaxies, clusters, and their
environments.
- J. A. Zebrowski, et al., — Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G
Data
- 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 $\sigma(r) = 0.067$.
- Frank J. Qu, et al., — Unified and consistent structure growth measurements from joint ACT, SPT
and \textit{Planck} CMB lensing
- We present the tightest cosmic microwave background (CMB) lensing constraints
to date on the growth of structure by combining CMB lensing measurements from
the Atacama Cosmology Telescope (ACT), the South Pole Telescope (SPT) and
\textit{Planck}. Each of these surveys individually provides lensing
measurements with similarly high statistical power, achieving signal-to-noise
ratios of approximately 40. The combined lensing bandpowers represent the most
precise CMB lensing power spectrum measurement to date with a signal-to-noise
ratio of 61 and an amplitude of $A_\mathrm{lens}^\mathrm{recon} = 1.025 \pm
0.017$ with respect to the theory prediction from the best-fit CMB
\textit{Planck}-ACT cosmology. The bandpowers from all three lensing datasets,
analyzed jointly, yield a $1.6\%$ measurement of the parameter combination
$S_8^\mathrm{CMBL} \equiv \sigma_8\,(\Omega_m/0.3)^{0.25} =
0.825^{+0.015}_{-0.013}$. Including Dark Energy Spectroscopic Instrument (DESI)
Baryon Acoustic Oscillation (BAO) data improves the constraint on the amplitude
of matter fluctuations to $\sigma_8 = 0.829 \pm 0.009$ (a $1.1\%$
determination). When combining with uncalibrated supernovae from
\texttt{Pantheon+}, we present a $4\%$ sound-horizon-independent estimate of
$H_0=66.4\pm2.5\,\mathrm{km\,s^{-1}\,Mpc^{-1}} $. The joint lensing constraints
on structure growth and present-day Hubble rate are fully consistent with a
$\Lambda$CDM model fit to the primary CMB data from \textit{Planck} and ACT.
While the precise upper limit is sensitive to the choice of data and underlying
model assumptions, when varying the neutrino mass sum within the
$\Lambda\mathrm{CDM}$ cosmological model, the combination of primary CMB, BAO
and CMB lensing drives the probable upper limit for the mass sum towards lower
values, comparable to the minimum mass prior required by neutrino oscillation
experiments.