{"work":{"id":"eeae0089-7b56-4c63-ace2-a31de468f6c5","openalex_id":"https://openalex.org/W4404624357","doi":"10.1007/jhep11(2024)108","arxiv_id":"1807.06209","raw_key":null,"title":"Planck 2018 results. VI. Cosmological parameters","authors":null,"authors_text":"Planck Collaboration: N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi, M. Ballardini","year":2018,"venue":"astro-ph.CO","abstract":"We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base $\\Lambda$CDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\\Omega_c h^2 = 0.120\\pm 0.001$, baryon density $\\Omega_b h^2 = 0.0224\\pm 0.0001$, scalar spectral index $n_s = 0.965\\pm 0.004$, and optical depth $\\tau = 0.054\\pm 0.007$ (in this abstract we quote $68\\,\\%$ confidence regions on measured parameters and $95\\,\\%$ on upper limits). The angular acoustic scale is measured to $0.03\\,\\%$ precision, with $100\\theta_*=1.0411\\pm 0.0003$. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-$\\Lambda$CDM cosmology, the inferred late-Universe parameters are: Hubble constant $H_0 = (67.4\\pm 0.5)$km/s/Mpc; matter density parameter $\\Omega_m = 0.315\\pm 0.007$; and matter fluctuation amplitude $\\sigma_8 = 0.811\\pm 0.006$. We find no compelling evidence for extensions to the base-$\\Lambda$CDM model. Combining with BAO we constrain the effective extra relativistic degrees of freedom to be $N_{\\rm eff} = 2.99\\pm 0.17$, and the neutrino mass is tightly constrained to $\\sum m_\\nu< 0.12$eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base -$\\Lambda$CDM at over $2\\,\\sigma$, which pulls some parameters that affect the lensing amplitude away from the base-$\\Lambda$CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. (Abridged)","external_url":"https://arxiv.org/abs/1807.06209","cited_by_count":10,"metadata_source":"pith","metadata_fetched_at":"2026-08-05T02:28:24.338817+00:00","pith_arxiv_id":"1807.06209","created_at":"2026-05-09T05:50:26.543701+00:00","updated_at":"2026-08-05T02:28:24.338817+00:00","title_quality_ok":true,"display_title":"Planck 2018 results. VI. Cosmological parameters","render_title":"Planck 2018 results. VI. Cosmological parameters"},"hub":{"state":{"work_id":"eeae0089-7b56-4c63-ace2-a31de468f6c5","tier":"super_hub","tier_reason":"100+ Pith inbound or 10,000+ external citations","pith_inbound_count":667,"external_cited_by_count":10,"distinct_field_count":17,"first_pith_cited_at":"2018-11-30T17:34:09+00:00","last_pith_cited_at":"2026-07-09T17:31:44+00:00","author_build_status":"needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-20T18:29:19.697089+00:00","tier_text":"super_hub"},"tier":"super_hub","role_counts":[{"context_role":"background","n":178},{"context_role":"dataset","n":32},{"context_role":"method","n":12},{"context_role":"baseline","n":8}],"polarity_counts":[{"context_polarity":"background","n":167},{"context_polarity":"use_dataset","n":31},{"context_polarity":"use_method","n":12},{"context_polarity":"baseline","n":8},{"context_polarity":"support","n":7},{"context_polarity":"unclear","n":5}],"runs":{"ask_index":{"job_type":"ask_index","status":"succeeded","result":{"title":"Planck 2018 results. VI. Cosmological parameters","claims":[{"claim_text":"We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base $\\Lambda$CDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\\Omega_c h^2 = 0.120\\pm 0.001$, baryon density $\\Omega_b h^2 = 0.0224\\pm 0.0001$, scalar spectral index $n_s = 0.965\\pm 0.004$, and optical depth $\\tau = 0.054\\pm","claim_type":"abstract","evidence_strength":"source_metadata"}],"why_cited":"Pith tracks Planck 2018 results. VI. Cosmological parameters because it crossed a citation-hub threshold.","role_counts":[]},"error":null,"updated_at":"2026-05-13T22:33:38.581041+00:00"},"author_expand":{"job_type":"author_expand","status":"succeeded","result":{"authors_linked":[{"id":"c9973a10-233d-4f9d-9fec-19bc884d8d89","orcid":null,"display_name":"Planck Collaboration: N. Aghanim"},{"id":"8569cc07-e456-42f3-8858-614f48808b4f","orcid":null,"display_name":"Y. Akrami"},{"id":"6e803416-541f-419b-8f53-e0651715273b","orcid":null,"display_name":"M. Ashdown"},{"id":"fa07b8c1-6d5e-47d1-9a55-dedd7786b72f","orcid":null,"display_name":"J. Aumont"},{"id":"dfb6dcb9-6424-4875-92c3-5d8f239cc330","orcid":null,"display_name":"C. Baccigalupi"},{"id":"189b63d7-a2ec-43ff-bcb5-9ba9feadf34f","orcid":null,"display_name":"M. Ballardini"}]},"error":null,"updated_at":"2026-05-13T22:33:38.486863+00:00"},"context_extract":{"job_type":"context_extract","status":"succeeded","result":{"enqueued_papers":25},"error":null,"updated_at":"2026-05-13T22:23:37.648148+00:00"},"graph_features":{"job_type":"graph_features","status":"succeeded","result":{"co_cited":[{"title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","work_id":"d54834f3-4944-4c0b-9fa4-3008a4c0122d","shared_citers":38},{"title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","work_id":"abaeab8e-c412-45ac-813e-f53689657023","shared_citers":26},{"title":"A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team","work_id":"5dac78be-e29e-4ec2-9a41-4adf05fc6a6a","shared_citers":23},{"title":"The Pantheon+ Analysis: Cosmological Constraints","work_id":"fafba1aa-4e44-42c3-8b9a-f0e78a38ad17","shared_citers":22},{"title":"G., Filippenko , A","work_id":"f4711f38-d7d5-454b-a88b-02642c09bbd4","shared_citers":17},{"title":"The Pantheon+ Analysis: The Full Dataset and Light-Curve Release","work_id":"cd546dcd-767f-46a9-b6e1-64cc3460d5b7","shared_citers":17},{"title":"1999, , 517, 565, 10.1086/307221","work_id":"2900b415-082f-4e4e-ad2c-7cba94498108","shared_citers":15},{"title":"SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field","work_id":"28ba80a8-b3e4-4c84-9f61-ba65da9b0aff","shared_citers":15},{"title":"Torrado and A","work_id":"579c5ab4-f42d-4271-a145-ce28660998d9","shared_citers":15},{"title":"Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Cosmological Implications from Two Decades of Spectroscopic Surveys at the Apache Point Observatory","work_id":"5fcfe3bb-de1b-4cd2-868e-f137ebf5c19b","shared_citers":14},{"title":"Chevallier and D","work_id":"7789cbe1-9129-4380-a7e9-282bec1dbc92","shared_citers":13},{"title":"Tensions between the Early and the Late Universe","work_id":"69d336d2-640b-48c0-bc97-7da81b659851","shared_citers":12},{"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","work_id":"abcbecb3-ae6f-4748-a925-133dc8647d67","shared_citers":12},{"title":"Aghanimet al.(Planck), Astron","work_id":"b5433e4f-7783-4472-a549-bdc3a40bb515","shared_citers":11},{"title":"Alam , M","work_id":"fd19ed7c-981b-4e7f-bdf4-3b82b6e29714","shared_citers":11},{"title":"arXiv e-prints , keywords =","work_id":"97bd2e42-29ac-4c1b-97fc-3c1b21056327","shared_citers":11},{"title":"Calabreseet al.(Atacama Cosmology Telescope), JCAP11, 063, arXiv:2503.14454 [astro-ph.CO]","work_id":"7d6a673d-1b44-4be4-8cb8-4500ebb3b4ea","shared_citers":11},{"title":"Carron, M","work_id":"67541cb5-f32b-463c-839a-bcab07f84fa8","shared_citers":11},{"title":"Data Release 1 of the Dark Energy Spectroscopic Instrument","work_id":"a536800a-8f7c-4eb1-b9ac-29718dc7c858","shared_citers":11},{"title":"Di Valentino, J","work_id":"55fbfccb-c90f-4492-affd-a96c16c9cf0b","shared_citers":11},{"title":"Di Valentino, O","work_id":"bfa51bc2-7198-4351-9514-5ef4574eed61","shared_citers":11},{"title":"Lewis, GetDist: a Python package for analysing Monte Carlo samples , 1910.13970","work_id":"f8674deb-70f7-4881-a67c-f177a925133d","shared_citers":11},{"title":"The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration","work_id":"226fee18-690f-45fa-b4c8-8854be9e86e2","shared_citers":11},{"title":"Lewis, A","work_id":"366015e5-cd86-4996-8a5e-81ec18d1971c","shared_citers":10}],"time_series":[{"n":1,"year":2018},{"n":1,"year":2019},{"n":1,"year":2022},{"n":1,"year":2024},{"n":1,"year":2025},{"n":146,"year":2026}]},"error":null,"updated_at":"2026-05-13T22:33:38.577323+00:00"},"identity_refresh":{"job_type":"identity_refresh","status":"succeeded","result":{"fixed":1,"items":[{"title":"Qwen3 Technical Report","work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e","resolver":"local_arxiv","confidence":0.98,"old_work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e"}],"errors":[],"attempted":1},"error":null,"updated_at":"2026-05-13T22:23:43.066820+00:00"},"role_polarity":{"job_type":"role_polarity","status":"succeeded","result":{"title":"Planck 2018 results. VI. Cosmological parameters","claims":[{"claim_text":"We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base $\\Lambda$CDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\\Omega_c h^2 = 0.120\\pm 0.001$, baryon density $\\Omega_b h^2 = 0.0224\\pm 0.0001$, scalar spectral index $n_s = 0.965\\pm 0.004$, and optical depth $\\tau = 0.054\\pm","claim_type":"abstract","evidence_strength":"source_metadata"}],"why_cited":"Pith tracks Planck 2018 results. VI. Cosmological parameters because it crossed a citation-hub threshold.","role_counts":[]},"error":null,"updated_at":"2026-05-13T22:33:38.093024+00:00"},"summary_claims":{"job_type":"summary_claims","status":"succeeded","result":{"title":"Planck 2018 results. VI. Cosmological parameters","claims":[{"claim_text":"We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base $\\Lambda$CDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\\Omega_c h^2 = 0.120\\pm 0.001$, baryon density $\\Omega_b h^2 = 0.0224\\pm 0.0001$, scalar spectral index $n_s = 0.965\\pm 0.004$, and optical depth $\\tau = 0.054\\pm","claim_type":"abstract","evidence_strength":"source_metadata"}],"why_cited":"Pith tracks Planck 2018 results. VI. Cosmological parameters because it crossed a citation-hub threshold.","role_counts":[]},"error":null,"updated_at":"2026-05-13T22:33:38.582643+00:00"}},"summary":{"title":"Planck 2018 results. VI. Cosmological parameters","claims":[{"claim_text":"We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base $\\Lambda$CDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\\Omega_c h^2 = 0.120\\pm 0.001$, baryon density $\\Omega_b h^2 = 0.0224\\pm 0.0001$, scalar spectral index $n_s = 0.965\\pm 0.004$, and optical depth $\\tau = 0.054\\pm","claim_type":"abstract","evidence_strength":"source_metadata"}],"why_cited":"Pith tracks Planck 2018 results. VI. Cosmological parameters because it crossed a citation-hub threshold.","role_counts":[]},"graph":{"co_cited":[{"title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","work_id":"d54834f3-4944-4c0b-9fa4-3008a4c0122d","shared_citers":38},{"title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","work_id":"abaeab8e-c412-45ac-813e-f53689657023","shared_citers":26},{"title":"A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team","work_id":"5dac78be-e29e-4ec2-9a41-4adf05fc6a6a","shared_citers":23},{"title":"The Pantheon+ Analysis: Cosmological Constraints","work_id":"fafba1aa-4e44-42c3-8b9a-f0e78a38ad17","shared_citers":22},{"title":"G., Filippenko , A","work_id":"f4711f38-d7d5-454b-a88b-02642c09bbd4","shared_citers":17},{"title":"The Pantheon+ Analysis: The Full Dataset and Light-Curve Release","work_id":"cd546dcd-767f-46a9-b6e1-64cc3460d5b7","shared_citers":17},{"title":"1999, , 517, 565, 10.1086/307221","work_id":"2900b415-082f-4e4e-ad2c-7cba94498108","shared_citers":15},{"title":"SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field","work_id":"28ba80a8-b3e4-4c84-9f61-ba65da9b0aff","shared_citers":15},{"title":"Torrado and A","work_id":"579c5ab4-f42d-4271-a145-ce28660998d9","shared_citers":15},{"title":"Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Cosmological Implications from Two Decades of Spectroscopic Surveys at the Apache Point Observatory","work_id":"5fcfe3bb-de1b-4cd2-868e-f137ebf5c19b","shared_citers":14},{"title":"Chevallier and D","work_id":"7789cbe1-9129-4380-a7e9-282bec1dbc92","shared_citers":13},{"title":"Tensions between the Early and the Late Universe","work_id":"69d336d2-640b-48c0-bc97-7da81b659851","shared_citers":12},{"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","work_id":"abcbecb3-ae6f-4748-a925-133dc8647d67","shared_citers":12},{"title":"Aghanimet al.(Planck), Astron","work_id":"b5433e4f-7783-4472-a549-bdc3a40bb515","shared_citers":11},{"title":"Alam , M","work_id":"fd19ed7c-981b-4e7f-bdf4-3b82b6e29714","shared_citers":11},{"title":"arXiv e-prints , keywords =","work_id":"97bd2e42-29ac-4c1b-97fc-3c1b21056327","shared_citers":11},{"title":"Calabreseet al.(Atacama Cosmology Telescope), JCAP11, 063, arXiv:2503.14454 [astro-ph.CO]","work_id":"7d6a673d-1b44-4be4-8cb8-4500ebb3b4ea","shared_citers":11},{"title":"Carron, M","work_id":"67541cb5-f32b-463c-839a-bcab07f84fa8","shared_citers":11},{"title":"Data Release 1 of the Dark Energy Spectroscopic Instrument","work_id":"a536800a-8f7c-4eb1-b9ac-29718dc7c858","shared_citers":11},{"title":"Di Valentino, J","work_id":"55fbfccb-c90f-4492-affd-a96c16c9cf0b","shared_citers":11},{"title":"Di Valentino, O","work_id":"bfa51bc2-7198-4351-9514-5ef4574eed61","shared_citers":11},{"title":"Lewis, GetDist: a Python package for analysing Monte Carlo samples , 1910.13970","work_id":"f8674deb-70f7-4881-a67c-f177a925133d","shared_citers":11},{"title":"The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration","work_id":"226fee18-690f-45fa-b4c8-8854be9e86e2","shared_citers":11},{"title":"Lewis, A","work_id":"366015e5-cd86-4996-8a5e-81ec18d1971c","shared_citers":10}],"time_series":[{"n":1,"year":2018},{"n":1,"year":2019},{"n":1,"year":2022},{"n":1,"year":2024},{"n":1,"year":2025},{"n":146,"year":2026}]},"authors":[{"id":"dfb6dcb9-6424-4875-92c3-5d8f239cc330","orcid":null,"display_name":"C. Baccigalupi","source":"manual","import_confidence":0.72},{"id":"fa07b8c1-6d5e-47d1-9a55-dedd7786b72f","orcid":null,"display_name":"J. Aumont","source":"manual","import_confidence":0.72},{"id":"6e803416-541f-419b-8f53-e0651715273b","orcid":null,"display_name":"M. Ashdown","source":"manual","import_confidence":0.72},{"id":"189b63d7-a2ec-43ff-bcb5-9ba9feadf34f","orcid":null,"display_name":"M. Ballardini","source":"manual","import_confidence":0.72},{"id":"c9973a10-233d-4f9d-9fec-19bc884d8d89","orcid":null,"display_name":"Planck Collaboration: N. Aghanim","source":"manual","import_confidence":0.72},{"id":"8569cc07-e456-42f3-8858-614f48808b4f","orcid":null,"display_name":"Y. Akrami","source":"manual","import_confidence":0.72}]}}