We present new measurements of cosmic microwave background (CMB) lensing over 9400 deg^{2}of the sky. These lensing measurements are derived from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB data set, which consists of five seasons of ACT CMB temperature and polarization observations. We determine the amplitude of the CMB lensing power spectrum at 2.3% precision (43
We show the improvement to cosmological constraints from galaxy cluster surveys with the addition of cosmic microwave background (CMB)cluster lensing data. We explore the cosmological implications of adding mass information from the 3.1
 NSFPAR ID:
 10486170
 Author(s) / Creator(s):
 ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
 Publisher / Repository:
 DOI PREFIX: 10.3847
 Date Published:
 Journal Name:
 The Astrophysical Journal
 Volume:
 931
 Issue:
 2
 ISSN:
 0004637X
 Format(s):
 Medium: X Size: Article No. 139
 Size(s):
 ["Article No. 139"]
 Sponsoring Org:
 National Science Foundation
More Like this

Abstract σ significance) using a novel pipeline that minimizes sensitivity to foregrounds and to noise properties. To ensure that our results are robust, we analyze an extensive set of null tests, consistency tests, and systematic error estimates and employ a blinded analysis framework. Our CMB lensing power spectrum measurement provides constraints on the amplitude of cosmic structure that do not depend on Planck or galaxy survey data, thus giving independent information about largescale structure growth and potential tensions in structure measurements. The baseline spectrum is well fit by a lensing amplitude ofA _{lens}= 1.013 ± 0.023 relative to the Planck 2018 CMB power spectra bestfit ΛCDM model andA _{lens}= 1.005 ± 0.023 relative to the ACT DR4 + WMAP bestfit model. From our lensing power spectrum measurement, we derive constraints on the parameter combination of ${S}_{8}^{\mathrm{CMBL}}\equiv {\sigma}_{8}{\left({\mathrm{\Omega}}_{m}/0.3\right)}^{0.25}$ from ACT DR6 CMB lensing alone and ${S}_{8}^{\mathrm{CMBL}}=0.818\pm 0.022$ when combining ACT DR6 and Planck ${S}_{8}^{\mathrm{CMBL}}=0.813\pm 0.018$NPIPE CMB lensing power spectra. These results are in excellent agreement with ΛCDM model constraints from Planck or ACT DR4 + WMAP CMB power spectrum measurements. Our lensing measurements from redshiftsz ∼ 0.5–5 are thus fully consistent with ΛCDM structure growth predictions based on CMB anisotropies probing primarilyz ∼ 1100. We find no evidence for a suppression of the amplitude of cosmic structure at low redshifts. 
Abstract We present cosmological constraints from a gravitational lensing mass map covering 9400 deg^{2}reconstructed from measurements of the cosmic microwave background (CMB) made by the Atacama Cosmology Telescope (ACT) from 2017 to 2021. In combination with measurements of baryon acoustic oscillations and big bang nucleosynthesis, we obtain the clustering amplitude
σ _{8}= 0.819 ± 0.015 at 1.8% precision, , and the Hubble constant ${S}_{8}\equiv {\sigma}_{8}{({\mathrm{\Omega}}_{\mathrm{m}}/0.3)}^{0.5}=0.840\pm 0.028$H _{0}= (68.3 ± 1.1) km s^{−1}Mpc^{−1}at 1.6% precision. A joint constraint with Planck CMB lensing yieldsσ _{8}= 0.812 ± 0.013, , and ${S}_{8}\equiv {\sigma}_{8}{({\mathrm{\Omega}}_{\mathrm{m}}/0.3)}^{0.5}=0.831\pm 0.023$H _{0}= (68.1 ± 1.0) km s^{−1}Mpc^{−1}. These measurements agree with ΛCDM extrapolations from the CMB anisotropies measured by Planck. We revisit constraints from the KiDS, DES, and HSC galaxy surveys with a uniform set of assumptions and find thatS _{8}from all three are lower than that from ACT+Planck lensing by levels ranging from 1.7σ to 2.1σ . This motivates further measurements and comparison, not just between the CMB anisotropies and galaxy lensing but also between CMB lensing probingz ∼ 0.5–5 on mostly linear scales and galaxy lensing atz ∼ 0.5 on smaller scales. We combine with CMB anisotropies to constrain extensions of ΛCDM, limiting neutrino masses to ∑m _{ν}< 0.13 eV (95% c.l.), for example. We describe the mass map and related data products that will enable a wide array of crosscorrelation science. Our results provide independent confirmation that the universe is spatially flat, conforms with general relativity, and is described remarkably well by the ΛCDM model, while paving a promising path for neutrino physics with lensing from upcoming groundbased CMB surveys. 
Abstract In this followup analysis, we update previous constraints on the transitional Planck mass (TPM) modified gravity model using the latest version of EFTCAMB and provide new constraints using South Pole Telescope (SPT) and Planck anisotropy data along with Planck cosmic microwave background lensing, baryon acoustic oscillations, and Type Ia supernovae data and a Hubble constant,
H _{0}, prior from local measurements. We find that large shifts in the Planck mass lead to large suppression of power on small scales that is disfavored by both the SPT and Planck data. Using only the SPT temperaturepolarization–polarizationpolarization (TEEE) data, this suppression of power can be compensated for by an upward shift of the scalar index ton _{s}= 1.003 ± 0.016, resulting in km m^{−1}Mpc^{−1}and a ∼7% shift in the Planck mass. Including the Planck temperaturetemperature (TT) ${H}_{0}\phantom{\rule{0.50em}{0ex}}=\phantom{\rule{0.50em}{0ex}}{71.94}_{0.85}^{+0.86}$ℓ ≤ 650 and Planck TEEE data restricts the shift to be <5% at 2σ withH _{0}= 70.65 ± 0.66 km m^{−1}Mpc^{−1}. Excluding theH _{0}prior, the SPT and Planck data constrain the shift in the Planck mass to be <3% at 2σ with a bestfit value of 0.04%, consistent with the Λ cold dark matter limit. In this case km s^{−1}Mpc^{−1}, which is partially elevated by the dynamics of the scalar field in the late Universe. This differs from early dark energy models that prefer higher values of ${H}_{0}\phantom{\rule{0.50em}{0ex}}=\phantom{\rule{0.50em}{0ex}}{69.09}_{0.68}^{+0.69}$H _{0}when the highℓ Planck TT data are excluded. We additionally constrain TPM using redshift space distortion data from BOSS DR12 and cosmic shear, galaxy–galaxy lensing, and galaxy clustering data from DES Y1, finding both disfavor transitions close to recombination, but earlier Planck mass transitions are allowed. 
Abstract The cluster mass–richness relation (MRR) is an observationally efficient and potentially powerful cosmological tool for constraining the matter density Ω_{m}and the amplitude of fluctuations
σ _{8}using the cluster abundance technique. We derive the MRR relation usingGalWCat19 , a publicly available galaxy cluster catalog we created from the Sloan Digital Sky SurveyDR13 spectroscopic data set. In the MRR, cluster mass scales with richness as . We find that the MRR we derive is consistent with both the IllustrisTNG and miniUchuu cosmological numerical simulations, with a slope of $\mathrm{log}{M}_{200}=\alpha +\beta \mathrm{log}{N}_{200}$β ≈ 1. We use the MRR we derived to estimate cluster masses from theGalWCat19 catalog, which we then use to set constraints on Ω_{m}andσ _{8}. Utilizing the allmember MRR, we obtain constraints of Ω_{m}= and ${0.31}_{0.03}^{+0.04}$σ _{8}= , and utilizing the red member MRR only, we obtain Ω_{m}= ${0.82}_{0.04}^{+0.05}$ and ${0.31}_{0.03}^{+0.04}$σ _{8}= . Our constraints on Ω_{m}and ${0.81}_{0.04}^{+0.05}$σ _{8}are consistent and very competitive with the Planck 2018 results. 
Abstract We present a detection of 21 cm emission from largescale structure (LSS) between redshift 0.78 and 1.43 made with the Canadian Hydrogen Intensity Mapping Experiment. Radio observations acquired over 102 nights are used to construct maps that are foreground filtered and stacked on the angular and spectral locations of luminous red galaxies (LRGs), emissionline galaxies (ELGs), and quasars (QSOs) from the eBOSS clustering catalogs. We find decisive evidence for a detection when stacking on all three tracers of LSS, with the logarithm of the Bayes factor equal to 18.9 (LRG), 10.8 (ELG), and 56.3 (QSO). An alternative frequentist interpretation, based on the likelihood ratio test, yields a detection significance of 7.1
σ (LRG), 5.7σ (ELG), and 11.1σ (QSO). These are the first 21 cm intensity mapping measurements made with an interferometer. We constrain the effective clustering amplitude of neutral hydrogen (Hi ), defined as , where Ω_{Hi}is the cosmic abundance of H ${\mathit{\ue22d}}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}\equiv {10}^{3}\phantom{\rule{0.25em}{0ex}}{\mathrm{\Omega}}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}\left({b}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}+\u3008\phantom{\rule{0.25em}{0ex}}f{\mu}^{2}\u3009\right)$i ,b _{Hi}is the linear bias of Hi , and 〈f μ ^{2}〉 = 0.552 encodes the effect of redshiftspace distortions at linear order. We find for LRGs ( ${\mathit{\ue22d}}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}={1.51}_{0.97}^{+3.60}$z = 0.84), for ELGs ( ${\mathit{\ue22d}}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}={6.76}_{3.79}^{+9.04}$z = 0.96), and for QSOs ( ${\mathit{\ue22d}}_{\mathrm{H}\phantom{\rule{0.25em}{0ex}}\mathrm{I}}={1.68}_{0.67}^{+1.10}$z = 1.20), with constraints limited by modeling uncertainties at nonlinear scales. We are also sensitive to bias in the spectroscopic redshifts of each tracer, and we find a nonzero bias Δv = − 66 ± 20 km s^{−1}for the QSOs. We split the QSO catalog into three redshift bins and have a decisive detection in each, with the upper bin atz = 1.30 producing the highestredshift 21 cm intensity mapping measurement thus far.