{"work":{"id":"abcbecb3-ae6f-4748-a925-133dc8647d67","openalex_id":null,"doi":null,"arxiv_id":"2503.14452","raw_key":null,"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","authors":null,"authors_text":"Thibaut Louis, Adrien La Posta, Zachary Atkins, Hidde T. Jense, Irene Abril-Cabezas, Graeme E. Addison","year":2025,"venue":"astro-ph.CO","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 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.","external_url":"https://arxiv.org/abs/2503.14452","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-25T07:20:28.635470+00:00","pith_arxiv_id":"2503.14452","created_at":"2026-05-10T07:16:54.930718+00:00","updated_at":"2026-06-05T21:23:00.469572+00:00","title_quality_ok":true,"display_title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","render_title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters"},"hub":{"state":{"work_id":"abcbecb3-ae6f-4748-a925-133dc8647d67","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":69,"external_cited_by_count":null,"distinct_field_count":4,"first_pith_cited_at":"2025-03-20T17:13:57+00:00","last_pith_cited_at":"2026-05-21T13:25:27+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-06T10:40:41.336540+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"dataset","n":16},{"context_role":"background","n":14},{"context_role":"baseline","n":3}],"polarity_counts":[{"context_polarity":"use_dataset","n":16},{"context_polarity":"background","n":9},{"context_polarity":"baseline","n":3},{"context_polarity":"unclear","n":3},{"context_polarity":"support","n":2}],"runs":{"context_extract":{"job_type":"context_extract","status":"succeeded","result":{"enqueued_papers":25},"error":null,"updated_at":"2026-05-20T02:52:04.780222+00:00"},"graph_features":{"job_type":"graph_features","status":"succeeded","result":{"co_cited":[{"title":"Planck 2018 results. 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CMB power spectra and likelihoods","work_id":"b5433e4f-7783-4472-a549-bdc3a40bb515","shared_citers":8},{"title":"Reconciling Nonminimally Coupled Higgs Inflation with ACT DR6 Observations through Reheating","work_id":"c74bc499-219e-4434-9224-d5323f1e3e93","shared_citers":8},{"title":"The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters","work_id":"021a3bdb-75ad-4121-9a13-62e68965c6e7","shared_citers":8},{"title":"The Dark Energy Survey: Cosmology Results With ~1500 New High-redshift Type Ia Supernovae Using The Full 5-year Dataset","work_id":"4519bda9-0cf9-4402-a6b1-2d04e3ed5744","shared_citers":8},{"title":"Zharov, O","work_id":"75b8a8c4-fa20-4e85-81e9-52ee3edd16b7","shared_citers":8}],"time_series":[{"n":17,"year":2025},{"n":38,"year":2026}],"dependency_candidates":[{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Einstein-Cartan pseudoscalaron inflation, reheating and nonthermal leptogenesis","primary_cat":"astro-ph.CO","context_text":"f0(ϕ) = γsinhX(ϕ)−1 p p−1 ,(27) where X(ϕ) = r 2 3 ϕ Mp + sinh−1(γ−1).(28) 7 Dataset Scalar spectral indexn s Tensor-to-scalar ratior k (r) ∗ Planck + BICEP Planck + lowE + lensing + BK15[129]0.9651±0.0041<0.056 0.002 Planck + lowE + lensing + BK15 + BAO[129]0.9668±0.0037< 0.058 0.002 Planck + ACT + DESI Planck + ACT DR6 + lensing + DESI-DR1[130]0.9743±0.0034- - Planck + ACT DR6 + lensing + DESI-DR2[130]0.9752±0.0030- - Planck + ACT + SPT Planck + ACT DR6 + SPT-3G-D1[131]0.9684±0.0030- - Planck + ACT DR6 + SPT-3G-D1 + DESI-DR2[131]0.9728±0.0027- - Planck + ACT + SPT + DESI + BICEP Planck + ACT DR6 + SPT-3G-D1 + BK18[132]0.9682±0.0032< 0.034 0.05 Planck + ACT DR6 + SPT-3G-D1 + DESI-DR2 + BK18[132]0.","citing_arxiv_id":"2605.09571"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"F-Term Hybrid Inflation with T-Model K\\\"ahler Geometry and Beyond","primary_cat":"hep-ph","context_text":"While the results of these experiments are broadly consistent, recent analyses reveal a mild tension in the preferred values of the scalar spectral index,n s. In particular, the combination ofPlanckwith BICEP2/Keck Arrayyields [2, 3] ns ≃0.9652±0.0084(P-BK-LBdata at 95% c.l.),(1.1) whereas the ACTdata release 6(DR6), combined withPlanck, BICEP2/Keck Arrayand DESI BAO measurements, prefers [4, 5] ns = 0.9743±0.0068⇒0.967≲n s ≲0.981(P-ACT -LB-BK18data at 95% c.l.) (1.2) 1 where then s elevation above is mainly attributed to a tension between CMB data and DESI BAO data [6]. On the other hand, the SPT measurements, when combined withPlanckand ACT data, yield an intermediate value [7] ns = 0.9684±0.006⇒0.962≲n s ≲0.974(P-ACT -SPTdata at 95% c.","citing_arxiv_id":"2605.08931"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"The Status of Gravitational Vector Perturbations with Recent CMB Data","primary_cat":"astro-ph.CO","context_text":"[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:2503.14452. [27] ACT Collaboration, Erminia Calabrese et al., The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models , arXiv:2503.14454. [28] ACT Collaboration, Sigurd Naess et al., The Atacama Cosmology Telescope: DR6 Maps ,","citing_arxiv_id":"2605.08907"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"The End of the First Act: Spectral Running, Interacting Dark Radiation, and the Hubble Tension in Light of ACT DR6 Data","primary_cat":"astro-ph.CO","context_text":"tracting cosmological information relies on accurate foreground removal. While we take ACT DR6 data at face value in this work, relying on the sophisticated foreground modelling of the ACT collaboration, one may also consider the hypothesis that the extra power in DR6 data is due to a residual foreground effect. In this context, it is interesting to note that the South Pole Telescope (SPT) [4] does not find evidence for a bluer spectral index, and their constraints onN eff = 3.18+0.29 −0.33 are looser than previous constraints from Planck Neff = 2.86±0.19. As a side remark, one may note that spectral running has been reported in previous data releases, in that case by SPT and with an opposite sign [42], and gone away in their current data release.","citing_arxiv_id":"2604.26541"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"String-inspired Gauss-Bonnet Gravity Inflation and ACT","primary_cat":"gr-qc","context_text":"These results have become a benchmark for testing inflationary scenarios and have led to the rejection of a significant number of models. The recent sixth release (DR6.02) of data from the Atacama Cosmology Telescope (ACT) has opened up new research opportunities by providing high-resolution measurements of polarization spectra at small angular scales [46, 47]. A joint analysis of the Planck and ACT data revealed a partial discrepancy in the (ns, r) plane, with ACT preferring slightly higher values of the spectral index of scalar perturbations. This raises the question of which inflationary models are able to satisfy both datasets, and what the preferences of the different models are between the two datasets.","citing_arxiv_id":"2604.18861"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"A data-driven prediction for the primordial deuterium abundance","primary_cat":"astro-ph.CO","context_text":"6 MeV, with sim- ilar uncertainties to Ref. [21], would no longer require the GP to extrapolate and reduce our prediction uncertain- ties. Statistics of the D/H posteriors are shown in the bot- tom panels of Figure 2. On average, the mean is in agree- FIG. 4. Deuterium abundance posteriors for four different CMB inferences ofω b:Planck2018 [3], ACT DR6 [28], SPT-3G [5], and a combined inference from all three (Joint SPA) [5]. Inferences including large-scale structure data are not considered. A Gaussian fit is overlayed on each. The mea- sured D/H from Cookeet al.[6] is shown as shaded bands (1σ and 2σuncertainties). ACT prefers the highestω b, giving the most discrepant D/H prediction. ment with the true value, coming in at≲0.","citing_arxiv_id":"2604.16600"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Dilaton-Flattened Axion Inflation","primary_cat":"hep-ph","context_text":"[23] C. P. Burgess, M. Horbatsch, S. P. Patil, and M. Williams, Inflating in a trough: Single-field effective theory from multiple-field curved valleys, JHEP (01), 133, arXiv:1209.5701 [hep-th]. [24] T. Louiset al., The atacama cosmology telescope: Dr6 power spectra, likelihoods and ΛCDM parameters, arXiv e-prints (2025), arXiv:2503.14452 [astro-ph.CO]. [25] E. Camphuiset al., Spt-3g d1: Cmb temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the spt-3g main field, arXiv e-prints (2025), arXiv:2506.20707 [astro-ph.CO]. [26] BICEP/Keck Collaboration, Constraining inflation with the bicep/keck cmb polarization experiments, arXiv e- prints (2024), arXiv:2405.19469 [astro-ph.","citing_arxiv_id":"2604.15194"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect","primary_cat":"astro-ph.CO","context_text":"arXiv:2503.14451, The Atacama Cosmology Telescope: DR6 Maps [26] Naess, S., et al. 2020, Journal of Cosmology and As- troparticle Physics, 2020, 046, The Atacama Cosmol- ogy Telescope: Arcminute-Resolution Maps Of 18 000 Square Degrees Of The Microwave Sky From Act 2008- 2018 Data Combined With Planck, https://dx.doi.org/ 10.1088/1475-7516/2020/12/046 [27] Louis, T., et al. 2025, arXiv:2503.14452, The Ata- cama Cosmology Telescope: DR6 Power Spectra, Like- lihoods and ΛCDM Parameters, https://arxiv.org/abs/ 2503.14452 [28] Aguado, D. S., et al. 2019, The Astrophysical Jour- nal Supplement Series, 240, 23, The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Re- lease of MaNGA-derived Quantities, Data Visualization","citing_arxiv_id":"2604.14327"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Into the Gompverse: A robust Gompertzian reionization model for CMB analyses","primary_cat":"astro-ph.CO","context_text":"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 galactic and extragalactic components. Following [34], we use a combination of Planck PR4 and ACT DR6 data for high-ℓTTTEEE. We further complement this state-of-the-art CMB dataset with the Planck low-ℓTT and EE measurements. We refer to this combination simply as 'CMB'.","citing_arxiv_id":"2604.13423"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","primary_cat":"astro-ph.CO","context_text":"03863 [astro-ph.CO]. [10] D. Broutet al., Astrophys. J.938, 110 (2022), arXiv:2202.04077 [astro-ph.CO]. [11] D. Rubinet al., Astrophys. J.986, 231 (2025), arXiv:2311.12098 [astro-ph.CO]. [12] A. G. Adameet al.(DESI), JCAP02, 021, arXiv:2404.03002 [astro-ph.CO]. [13] M. Abdul Karimet al.(DESI), Phys. Rev. D112, 083515 (2025), arXiv:2503.14738 [astro-ph.CO]. [14] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062, arXiv:2503.14452 [astro-ph.CO]. [15] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [16] M. Asgariet al.(KiDS), Astron. Astrophys.645, A104","citing_arxiv_id":"2604.12987"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Disentangling cosmic distance tensions with early and late dark energy","primary_cat":"astro-ph.CO","context_text":"data atℓ <1000 in TT andℓ <600 in TE and EE, and using only ACT DR6 data above those multipole values. Because of the small sky overlap between SPT-3G D1 and ACT/Planck, we use the full multipole range of the SPT-3G D1 likelihood, as in [5]. We uselitelikelihoods as supplied by thePlanckcollaboration and bycandl[114]. 6 CMB lensing: We use the combinedPlanck PR4 lensing [116] and ACT DR6 lensing [117] datasets, accounting for their cross-correlations. To these, we add SPT-3G MUSE lensing data [118] as an independent dataset and neglect cross-correlations which are negligible due to the small but deep sky coverage [119]. •BAO: We use the DESI DR2 likelihood based on Table IV in Ref. [10] forD V /rd for the lowest redshift bin andD M /rd,D H /rd, and their cross-","citing_arxiv_id":"2604.08530"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Beyond $f(\\phi)\\mathcal{G}$: Gauss--Bonnet inflation with $\\mu(\\phi,X)$","primary_cat":"astro-ph.CO","context_text":"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, andg X = 0.03, while all other parameters are kept fixed. This choice of the parameters ensures that the bump effect is localized around pivot scaleN ⋆ and clarifies the impact of the explicitXdependence in the coupling.","citing_arxiv_id":"2604.03828"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Non-minimally coupled quintessence with sign-switching interaction","primary_cat":"astro-ph.CO","context_text":"• 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 priors for all cosmological and model pa- rameters used in the nested-sampling analysis. Cosmological Parameters Model Parameters Ωbh2 U [0.020, 0.025] w0 U [−3, 1] Ωch2 U [0.1, 0.15] wa U [−3, 2] H0 U [60, 80] α U [0, 1.2] ln(1010As) U [3.0, 3.1] β U [0, 0.","citing_arxiv_id":"2604.02204"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Induced-Gravity Palatini-Like Higgs Inflation in Supergravity Confronts ACT DR6","primary_cat":"hep-ph","context_text":"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 models that can accommodate such a s hift [4-58] - for a review see Ref. [59]. Indeed, the combination of the aforementioned data with the measurements from other experiments [3, 60, 61] too, named P-ACT -LB-BK18data, suggests that ns, its running as and the tensor-to-scalar","citing_arxiv_id":"2602.05623"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Evidence for deviation in gravitational light deflection from general relativity at cosmological scales with KiDS-Legacy and CMB lensing","primary_cat":"astro-ph.CO","context_text":"to lensing effects deviating abnormally from GR predictions; see, e.g., Refs. [10, 117-120]. We explore the impact ofA lens and the total neutrino mass ( P mν) on our constraints in Appendix A. ness requires further verification. Meanwhile, the Ata- cama Cosmology Telescope (ACT) and the South Pole Telescope (SPT) collaborations recently jointly released small-scale CMB anisotropy measurements [123, 124] and the most precise lensing reconstruction data derived from ACT, SPT, and Planck experiments [125]. CMB lens- ing probes the integrated Weyl potential to the last scattering surface, forming a complementarity with the low-redshift galaxy weak-lensing effects probed by KiDS. Therefore, integrating these latest high-precision cosmo- logical datasets to effectively constrain phenomenological","citing_arxiv_id":"2602.03110"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","primary_cat":"astro-ph.CO","context_text":"208, 20 (2013), arXiv:1212.5225 [astro-ph.CO]. [2] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [3] N. Aghanimet al.(Planck), Astron. Astrophys.641, A1 (2020), arXiv:1807.06205 [astro-ph.CO]. [4] S. Aiolaet al.(ACT), JCAP12, 047, arXiv:2007.07288 [astro-ph.CO]. [5] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062, arXiv:2503.14452 [astro-ph.CO]. [6] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [7] F. Beutler, C. Blake, M. Colless, D. H. Jones, L. Staveley-Smith, L.","citing_arxiv_id":"2601.14222"}]},"error":null,"updated_at":"2026-05-20T02:51:56.085811+00:00"},"identity_refresh":{"job_type":"identity_refresh","status":"succeeded","result":{"items":[{"title":"Qwen3 Technical Report","outcome":"unchanged","work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e","resolver":"local_arxiv","confidence":0.98,"old_work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e"}],"counts":{"fixed":0,"merged":0,"unchanged":1,"quarantined":0,"needs_external_resolution":0},"errors":[],"attempted":1},"error":null,"updated_at":"2026-05-20T02:52:01.276100+00:00"},"summary_claims":{"job_type":"summary_claims","status":"succeeded","result":{"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","claims":[{"claim_text":"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 ","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"[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.","claim_type":"dataset","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"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","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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,","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"• 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","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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 ","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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:","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (13 contexts).","role_counts":[{"n":13,"context_role":"background"},{"n":13,"context_role":"dataset"},{"n":3,"context_role":"baseline"}]},"error":null,"updated_at":"2026-05-20T02:51:55.980482+00:00"}},"summary":{"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","claims":[{"claim_text":"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 ","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"[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.","claim_type":"dataset","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"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","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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,","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"• 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","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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 ","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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:","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (13 contexts).","role_counts":[{"n":13,"context_role":"background"},{"n":13,"context_role":"dataset"},{"n":3,"context_role":"baseline"}]},"graph":{"co_cited":[{"title":"Planck 2018 results. VI. 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CMB power spectra and likelihoods","work_id":"b5433e4f-7783-4472-a549-bdc3a40bb515","shared_citers":8},{"title":"Reconciling Nonminimally Coupled Higgs Inflation with ACT DR6 Observations through Reheating","work_id":"c74bc499-219e-4434-9224-d5323f1e3e93","shared_citers":8},{"title":"The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters","work_id":"021a3bdb-75ad-4121-9a13-62e68965c6e7","shared_citers":8},{"title":"The Dark Energy Survey: Cosmology Results With ~1500 New High-redshift Type Ia Supernovae Using The Full 5-year Dataset","work_id":"4519bda9-0cf9-4402-a6b1-2d04e3ed5744","shared_citers":8},{"title":"Zharov, O","work_id":"75b8a8c4-fa20-4e85-81e9-52ee3edd16b7","shared_citers":8}],"time_series":[{"n":17,"year":2025},{"n":38,"year":2026}],"dependency_candidates":[{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Einstein-Cartan pseudoscalaron inflation, reheating and nonthermal leptogenesis","primary_cat":"astro-ph.CO","context_text":"f0(ϕ) = γsinhX(ϕ)−1 p p−1 ,(27) where X(ϕ) = r 2 3 ϕ Mp + sinh−1(γ−1).(28) 7 Dataset Scalar spectral indexn s Tensor-to-scalar ratior k (r) ∗ Planck + BICEP Planck + lowE + lensing + BK15[129]0.9651±0.0041<0.056 0.002 Planck + lowE + lensing + BK15 + BAO[129]0.9668±0.0037< 0.058 0.002 Planck + ACT + DESI Planck + ACT DR6 + lensing + DESI-DR1[130]0.9743±0.0034- - Planck + ACT DR6 + lensing + DESI-DR2[130]0.9752±0.0030- - Planck + ACT + SPT Planck + ACT DR6 + SPT-3G-D1[131]0.9684±0.0030- - Planck + ACT DR6 + SPT-3G-D1 + DESI-DR2[131]0.9728±0.0027- - Planck + ACT + SPT + DESI + BICEP Planck + ACT DR6 + SPT-3G-D1 + BK18[132]0.9682±0.0032< 0.034 0.05 Planck + ACT DR6 + SPT-3G-D1 + DESI-DR2 + BK18[132]0.","citing_arxiv_id":"2605.09571"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"F-Term Hybrid Inflation with T-Model K\\\"ahler Geometry and Beyond","primary_cat":"hep-ph","context_text":"While the results of these experiments are broadly consistent, recent analyses reveal a mild tension in the preferred values of the scalar spectral index,n s. In particular, the combination ofPlanckwith BICEP2/Keck Arrayyields [2, 3] ns ≃0.9652±0.0084(P-BK-LBdata at 95% c.l.),(1.1) whereas the ACTdata release 6(DR6), combined withPlanck, BICEP2/Keck Arrayand DESI BAO measurements, prefers [4, 5] ns = 0.9743±0.0068⇒0.967≲n s ≲0.981(P-ACT -LB-BK18data at 95% c.l.) (1.2) 1 where then s elevation above is mainly attributed to a tension between CMB data and DESI BAO data [6]. On the other hand, the SPT measurements, when combined withPlanckand ACT data, yield an intermediate value [7] ns = 0.9684±0.006⇒0.962≲n s ≲0.974(P-ACT -SPTdata at 95% c.","citing_arxiv_id":"2605.08931"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"The Status of Gravitational Vector Perturbations with Recent CMB Data","primary_cat":"astro-ph.CO","context_text":"[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:2503.14452. [27] ACT Collaboration, Erminia Calabrese et al., The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models , arXiv:2503.14454. [28] ACT Collaboration, Sigurd Naess et al., The Atacama Cosmology Telescope: DR6 Maps ,","citing_arxiv_id":"2605.08907"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"The End of the First Act: Spectral Running, Interacting Dark Radiation, and the Hubble Tension in Light of ACT DR6 Data","primary_cat":"astro-ph.CO","context_text":"tracting cosmological information relies on accurate foreground removal. While we take ACT DR6 data at face value in this work, relying on the sophisticated foreground modelling of the ACT collaboration, one may also consider the hypothesis that the extra power in DR6 data is due to a residual foreground effect. In this context, it is interesting to note that the South Pole Telescope (SPT) [4] does not find evidence for a bluer spectral index, and their constraints onN eff = 3.18+0.29 −0.33 are looser than previous constraints from Planck Neff = 2.86±0.19. As a side remark, one may note that spectral running has been reported in previous data releases, in that case by SPT and with an opposite sign [42], and gone away in their current data release.","citing_arxiv_id":"2604.26541"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"String-inspired Gauss-Bonnet Gravity Inflation and ACT","primary_cat":"gr-qc","context_text":"These results have become a benchmark for testing inflationary scenarios and have led to the rejection of a significant number of models. The recent sixth release (DR6.02) of data from the Atacama Cosmology Telescope (ACT) has opened up new research opportunities by providing high-resolution measurements of polarization spectra at small angular scales [46, 47]. A joint analysis of the Planck and ACT data revealed a partial discrepancy in the (ns, r) plane, with ACT preferring slightly higher values of the spectral index of scalar perturbations. This raises the question of which inflationary models are able to satisfy both datasets, and what the preferences of the different models are between the two datasets.","citing_arxiv_id":"2604.18861"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"A data-driven prediction for the primordial deuterium abundance","primary_cat":"astro-ph.CO","context_text":"6 MeV, with sim- ilar uncertainties to Ref. [21], would no longer require the GP to extrapolate and reduce our prediction uncertain- ties. Statistics of the D/H posteriors are shown in the bot- tom panels of Figure 2. On average, the mean is in agree- FIG. 4. Deuterium abundance posteriors for four different CMB inferences ofω b:Planck2018 [3], ACT DR6 [28], SPT-3G [5], and a combined inference from all three (Joint SPA) [5]. Inferences including large-scale structure data are not considered. A Gaussian fit is overlayed on each. The mea- sured D/H from Cookeet al.[6] is shown as shaded bands (1σ and 2σuncertainties). ACT prefers the highestω b, giving the most discrepant D/H prediction. ment with the true value, coming in at≲0.","citing_arxiv_id":"2604.16600"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Dilaton-Flattened Axion Inflation","primary_cat":"hep-ph","context_text":"[23] C. P. Burgess, M. Horbatsch, S. P. Patil, and M. Williams, Inflating in a trough: Single-field effective theory from multiple-field curved valleys, JHEP (01), 133, arXiv:1209.5701 [hep-th]. [24] T. Louiset al., The atacama cosmology telescope: Dr6 power spectra, likelihoods and ΛCDM parameters, arXiv e-prints (2025), arXiv:2503.14452 [astro-ph.CO]. [25] E. Camphuiset al., Spt-3g d1: Cmb temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the spt-3g main field, arXiv e-prints (2025), arXiv:2506.20707 [astro-ph.CO]. [26] BICEP/Keck Collaboration, Constraining inflation with the bicep/keck cmb polarization experiments, arXiv e- prints (2024), arXiv:2405.19469 [astro-ph.","citing_arxiv_id":"2604.15194"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect","primary_cat":"astro-ph.CO","context_text":"arXiv:2503.14451, The Atacama Cosmology Telescope: DR6 Maps [26] Naess, S., et al. 2020, Journal of Cosmology and As- troparticle Physics, 2020, 046, The Atacama Cosmol- ogy Telescope: Arcminute-Resolution Maps Of 18 000 Square Degrees Of The Microwave Sky From Act 2008- 2018 Data Combined With Planck, https://dx.doi.org/ 10.1088/1475-7516/2020/12/046 [27] Louis, T., et al. 2025, arXiv:2503.14452, The Ata- cama Cosmology Telescope: DR6 Power Spectra, Like- lihoods and ΛCDM Parameters, https://arxiv.org/abs/ 2503.14452 [28] Aguado, D. S., et al. 2019, The Astrophysical Jour- nal Supplement Series, 240, 23, The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Re- lease of MaNGA-derived Quantities, Data Visualization","citing_arxiv_id":"2604.14327"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Into the Gompverse: A robust Gompertzian reionization model for CMB analyses","primary_cat":"astro-ph.CO","context_text":"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 galactic and extragalactic components. Following [34], we use a combination of Planck PR4 and ACT DR6 data for high-ℓTTTEEE. We further complement this state-of-the-art CMB dataset with the Planck low-ℓTT and EE measurements. We refer to this combination simply as 'CMB'.","citing_arxiv_id":"2604.13423"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","primary_cat":"astro-ph.CO","context_text":"03863 [astro-ph.CO]. [10] D. Broutet al., Astrophys. J.938, 110 (2022), arXiv:2202.04077 [astro-ph.CO]. [11] D. Rubinet al., Astrophys. J.986, 231 (2025), arXiv:2311.12098 [astro-ph.CO]. [12] A. G. Adameet al.(DESI), JCAP02, 021, arXiv:2404.03002 [astro-ph.CO]. [13] M. Abdul Karimet al.(DESI), Phys. Rev. D112, 083515 (2025), arXiv:2503.14738 [astro-ph.CO]. [14] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062, arXiv:2503.14452 [astro-ph.CO]. [15] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [16] M. Asgariet al.(KiDS), Astron. Astrophys.645, A104","citing_arxiv_id":"2604.12987"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Disentangling cosmic distance tensions with early and late dark energy","primary_cat":"astro-ph.CO","context_text":"data atℓ <1000 in TT andℓ <600 in TE and EE, and using only ACT DR6 data above those multipole values. Because of the small sky overlap between SPT-3G D1 and ACT/Planck, we use the full multipole range of the SPT-3G D1 likelihood, as in [5]. We uselitelikelihoods as supplied by thePlanckcollaboration and bycandl[114]. 6 CMB lensing: We use the combinedPlanck PR4 lensing [116] and ACT DR6 lensing [117] datasets, accounting for their cross-correlations. To these, we add SPT-3G MUSE lensing data [118] as an independent dataset and neglect cross-correlations which are negligible due to the small but deep sky coverage [119]. •BAO: We use the DESI DR2 likelihood based on Table IV in Ref. [10] forD V /rd for the lowest redshift bin andD M /rd,D H /rd, and their cross-","citing_arxiv_id":"2604.08530"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Beyond $f(\\phi)\\mathcal{G}$: Gauss--Bonnet inflation with $\\mu(\\phi,X)$","primary_cat":"astro-ph.CO","context_text":"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, andg X = 0.03, while all other parameters are kept fixed. This choice of the parameters ensures that the bump effect is localized around pivot scaleN ⋆ and clarifies the impact of the explicitXdependence in the coupling.","citing_arxiv_id":"2604.03828"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Non-minimally coupled quintessence with sign-switching interaction","primary_cat":"astro-ph.CO","context_text":"• 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 priors for all cosmological and model pa- rameters used in the nested-sampling analysis. Cosmological Parameters Model Parameters Ωbh2 U [0.020, 0.025] w0 U [−3, 1] Ωch2 U [0.1, 0.15] wa U [−3, 2] H0 U [60, 80] α U [0, 1.2] ln(1010As) U [3.0, 3.1] β U [0, 0.","citing_arxiv_id":"2604.02204"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Induced-Gravity Palatini-Like Higgs Inflation in Supergravity Confronts ACT DR6","primary_cat":"hep-ph","context_text":"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 models that can accommodate such a s hift [4-58] - for a review see Ref. [59]. Indeed, the combination of the aforementioned data with the measurements from other experiments [3, 60, 61] too, named P-ACT -LB-BK18data, suggests that ns, its running as and the tensor-to-scalar","citing_arxiv_id":"2602.05623"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Evidence for deviation in gravitational light deflection from general relativity at cosmological scales with KiDS-Legacy and CMB lensing","primary_cat":"astro-ph.CO","context_text":"to lensing effects deviating abnormally from GR predictions; see, e.g., Refs. [10, 117-120]. We explore the impact ofA lens and the total neutrino mass ( P mν) on our constraints in Appendix A. ness requires further verification. Meanwhile, the Ata- cama Cosmology Telescope (ACT) and the South Pole Telescope (SPT) collaborations recently jointly released small-scale CMB anisotropy measurements [123, 124] and the most precise lensing reconstruction data derived from ACT, SPT, and Planck experiments [125]. CMB lens- ing probes the integrated Weyl potential to the last scattering surface, forming a complementarity with the low-redshift galaxy weak-lensing effects probed by KiDS. Therefore, integrating these latest high-precision cosmo- logical datasets to effectively constrain phenomenological","citing_arxiv_id":"2602.03110"},{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","primary_cat":"astro-ph.CO","context_text":"208, 20 (2013), arXiv:1212.5225 [astro-ph.CO]. [2] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [3] N. Aghanimet al.(Planck), Astron. Astrophys.641, A1 (2020), arXiv:1807.06205 [astro-ph.CO]. [4] S. Aiolaet al.(ACT), JCAP12, 047, arXiv:2007.07288 [astro-ph.CO]. [5] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062, arXiv:2503.14452 [astro-ph.CO]. [6] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [7] F. Beutler, C. Blake, M. Colless, D. H. Jones, L. Staveley-Smith, L.","citing_arxiv_id":"2601.14222"}]},"authors":[]}}