Inflaton-gluon coupling during inflation requires p=2 plateau models to produce isocurvature-free QCD axion dark matter.
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The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\Lambda$CDM Parameters
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We present power spectra of the cosmic microwave background (CMB) anisotropy in temperature and polarization, measured from the Data Release 6 maps made from Atacama Cosmology Telescope (ACT) data. These cover 19,000 deg$^2$ of sky in bands centered at 98, 150 and 220 GHz, with white noise levels three times lower than Planck in polarization. We find that the ACT angular power spectra estimated over 10,000 deg$^2$, and measured to arcminute scales in TT, TE and EE, are well fit by the sum of CMB and foregrounds, where the CMB spectra are described by the $\Lambda$CDM model. Combining ACT with larger-scale Planck data, the joint P-ACT dataset provides tight limits on the ingredients, expansion rate, and initial conditions of the universe. We find similar constraining power, and consistent results, from either the Planck power spectra or from ACT combined with WMAP data, as well as from either temperature or polarization in the joint P-ACT dataset. When combined with CMB lensing from ACT and Planck, and baryon acoustic oscillation data from DESI DR1, we measure a baryon density of $\Omega_b h^2=0.0226\pm0.0001$, a cold dark matter density of $\Omega_c h^2=0.118\pm0.001$, a Hubble constant of $H_0=68.22\pm0.36$ km/s/Mpc, a spectral index of $n_s=0.974\pm0.003$, and an amplitude of density fluctuations of $\sigma_8=0.813\pm0.005$. Including the DESI DR2 data tightens the Hubble constant to $H_0=68.43\pm0.27$ km/s/Mpc; $\Lambda$CDM parameters agree between the P-ACT and DESI DR2 data at the $1.6\sigma$ level. We find no evidence for excess lensing in the power spectrum, and no departure from spatial flatness. The contribution from Sunyaev-Zel'dovich (SZ) anisotropy is detected at high significance; we find evidence for a tilt with suppressed small-scale power compared to our baseline SZ template spectrum, consistent with hydrodynamical simulations with feedback.
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- abstract We present power spectra of the cosmic microwave background (CMB) anisotropy in temperature and polarization, measured from the Data Release 6 maps made from Atacama Cosmology Telescope (ACT) data. These cover 19,000 deg$^2$ of sky in bands centered at 98, 150 and 220 GHz, with white noise levels three times lower than Planck in polarization. We find that the ACT angular power spectra estimated over 10,000 deg$^2$, and measured to arcminute scales in TT, TE and EE, are well fit by the sum of CMB and foregrounds, where the CMB spectra are described by the $\Lambda$CDM model. Combining ACT with
- dataset [24] SPT-3G Collaboration, E. Camphuis et al., SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field, arXiv:2506.20707. [25] SPT-3G Collaboration, W. Quan et al., SPT-3G D1: Maps of the millimeter-wave sky from 2019 and 2020 observations of the SPT-3G Main field , arXiv:2603.20163. [26] ACT Collaboration, Thibaut Louis et al., The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and ΛCDM Parameters, arXiv:2503.
- dataset 1 E QUATION OF MOTION . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21 A.2 E QUATION -OF-STATE PARAMETERS . . . . . . . . . . . . . . . . . . . . . . . . . 22 A.3 N UMBER OF E -F OLDINGS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23 1 I NTRODUCTION The Data Release 6 (DR6) from the Atacama Cosmology Telescope (ACT) [1, 2] favors a slightly higher scalar spectral index, ns, than the one indicated from the Planck data [3] prompting renewed interest in inflationary m
- dataset CMB analyses reportn s = 0.9649±0.0042 (Planck 2018 TT,TE,EE+lowE)[1] and ln(10 10As) = 3.044±0.014 at k⋆ = 0.05 Mpc−1, withn s = 0.9665±0.0038 when adding lensing+BAO[1];B-mode polarization further constrains tensors (e.g.r 0.05 <0.036 at 95% C.L. from BICEP/Keck)[2], while ACT DR6 reportsn s = 0.9743±0.0034 and ln(1010As) = 3.053±0.013 for the P-ACT-LB combination[3]. Next, to make the Gauss-Bonnet imprint at the pivot more visible, the coupling parameters are updated toA= 0.9, ∆ = 0.45,p= 12,
- dataset • CMB: the CamSpec likelihood based on the Planck PR4 NPIPE high-multipole ( ℓ > 30) TT, TE, and EE spectra [ 77], together with the low-multipole temperature and E-mode polarization power spec- tra, C T T ℓ and C EE ℓ , derived using Commander and SimAll [78], respectively. We also include the CMB lensing likelihood constructed from the combina- tion of Planck PR4 NPIPE [ 79] and ACT DR6 [ 80]. • BAO: the DESI Y3 BAO measurements listed in Table IV of the DR2 paper [ 24]. TABLE I. Uniform prior
- dataset likelihood [29] while the polarization one is given bySroll2[30]. •Planck PR4:The Planck PR4 TTTEEE, i.e. CMB temperature, polarization, and cross-correlation measurements at high-ℓusing the NPIPE pipeline [31] over≈80 % of the sky. The data is based on theCamSpeclikelihood [32, 33] and covers 30≤ℓ≤2500. •ACT DR6:The Atacama Cosmology telescope (ACT) Data Release 6 (DR6) CMB TTTEEE measurements [34]. The DR6 maps cover almost half the sky, but only roughly half of that is used after masking the
- background Karam, and A. Racioppi, JCAP11, 014 (2020), arXiv:2006.09124 [gr-qc]. [52] J. Kim, Z. Yang, and Y.-l. Zhang, (2025), arXiv:2503.16907 [astro-ph.CO]. [53] J. Kim, X. Wang, Y.-l. Zhang, and Z. Ren, (2025), arXiv:2504.12035 [astro-ph.CO]. [54] A. S. Koshelev, K. S. Kumar, and A. A. Starobinsky, Int. J. Mod. Phys. D29, 2043018 (2020), arXiv:2005.09550 [hep-th]. [55] T. Louiset al.(ACT), arXiv preprint (2025), arXiv:2503.14452 [astro-ph.CO]. [56] E. Calabreseet al.(ACT), arXiv preprint (2025), arXiv:
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