{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:6ZAPBWYFJWKVSGV2FPSCKMJFQS","short_pith_number":"pith:6ZAPBWYF","schema_version":"1.0","canonical_sha256":"f640f0db054d95591aba2be425312584bb9d71078220977d409015c6a4ad8778","source":{"kind":"arxiv","id":"2109.01161","version":2},"attestation_state":"computed","paper":{"title":"A buyer's guide to the Hubble Constant","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ofer Lahav (UCL), Pablo Lemos (UCL, Paul Shah (UCL), Sussex U.)","submitted_at":"2021-09-02T18:09:34Z","abstract_excerpt":"Since the expansion of the universe was first established by Edwin Hubble and Georges Lemaitre about a century ago, the Hubble constant H0 which measures its rate has been of great interest to astronomers. Besides being interesting in its own right, few properties of the universe can be deduced without it. In the last decade a significant gap has emerged between different methods of measuring it, some anchored in the nearby universe, others at cosmological distances. The SH0ES team has found $H_0 = 73.2 \\pm 1.3$ km sec$^{-1}$ Mpc$^{-1}$ locally, whereas the value found for the early universe b"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2109.01161","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-09-02T18:09:34Z","cross_cats_sorted":[],"title_canon_sha256":"baee362a01a01915353fc897481ff987e799a087c08c90fa12977f8708a8934d","abstract_canon_sha256":"382209b62f2fc98737191c4129be26697d5513a5d378daeaf7d3ffe244ba5792"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:40:44.198695Z","signature_b64":"kCuOJFJgXVZ4XfykzAHaocjZ66mqG9UYZa/Y3e0vW1zCEYD+nHtL4IKQDvV4MgUe4AX0KjUSDjPErtDzwVWkDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f640f0db054d95591aba2be425312584bb9d71078220977d409015c6a4ad8778","last_reissued_at":"2026-07-05T03:40:44.198254Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:40:44.198254Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A buyer's guide to the Hubble Constant","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ofer Lahav (UCL), Pablo Lemos (UCL, Paul Shah (UCL), Sussex U.)","submitted_at":"2021-09-02T18:09:34Z","abstract_excerpt":"Since the expansion of the universe was first established by Edwin Hubble and Georges Lemaitre about a century ago, the Hubble constant H0 which measures its rate has been of great interest to astronomers. Besides being interesting in its own right, few properties of the universe can be deduced without it. In the last decade a significant gap has emerged between different methods of measuring it, some anchored in the nearby universe, others at cosmological distances. The SH0ES team has found $H_0 = 73.2 \\pm 1.3$ km sec$^{-1}$ Mpc$^{-1}$ locally, whereas the value found for the early universe b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2109.01161","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2109.01161/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2109.01161","created_at":"2026-07-05T03:40:44.198310+00:00"},{"alias_kind":"arxiv_version","alias_value":"2109.01161v2","created_at":"2026-07-05T03:40:44.198310+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2109.01161","created_at":"2026-07-05T03:40:44.198310+00:00"},{"alias_kind":"pith_short_12","alias_value":"6ZAPBWYFJWKV","created_at":"2026-07-05T03:40:44.198310+00:00"},{"alias_kind":"pith_short_16","alias_value":"6ZAPBWYFJWKVSGV2","created_at":"2026-07-05T03:40:44.198310+00:00"},{"alias_kind":"pith_short_8","alias_value":"6ZAPBWYF","created_at":"2026-07-05T03:40:44.198310+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":18,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.20434","citing_title":"The Hubble tension: A decade review","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2606.19090","citing_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2606.07854","citing_title":"Measurements of the Angular Homogeneity Scale from DESI DR1","ref_index":8,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05539","citing_title":"Dissipative Cosmology and the Nature of Dark Energy: Insights from Bulk Viscosity with DESI DR2 observations","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2607.01226","citing_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","ref_index":99,"is_internal_anchor":false},{"citing_arxiv_id":"2605.26116","citing_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31362","citing_title":"Running into tension: primordial black holes from ultra-slow-roll inflation, spectral running, and the Hubble tension","ref_index":162,"is_internal_anchor":false},{"citing_arxiv_id":"2402.07716","citing_title":"$\\Lambda_{\\rm s}$CDM cosmology from a type-II minimally modified gravity","ref_index":9,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21456","citing_title":"Negative neutrino mass or negative dark energy?","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2510.18741","citing_title":"Nonlinear Matter Power Spectrum from relativistic $N$-body Simulations: $\\Lambda_{\\rm s}$CDM versus $\\Lambda$CDM","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2211.04492","citing_title":"The Hubble Tension and Early Dark Energy","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2601.14222","citing_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","ref_index":51,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2112.04510","citing_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","ref_index":129,"is_internal_anchor":false},{"citing_arxiv_id":"2604.28013","citing_title":"Cosmological intercept tension","ref_index":12,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25813","citing_title":"Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension","ref_index":6,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13535","citing_title":"Double the axions, half the tension: multi-field early dark energy eases the Hubble tension","ref_index":5,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS","json":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS.json","graph_json":"https://pith.science/api/pith-number/6ZAPBWYFJWKVSGV2FPSCKMJFQS/graph.json","events_json":"https://pith.science/api/pith-number/6ZAPBWYFJWKVSGV2FPSCKMJFQS/events.json","paper":"https://pith.science/paper/6ZAPBWYF"},"agent_actions":{"view_html":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS","download_json":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS.json","view_paper":"https://pith.science/paper/6ZAPBWYF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2109.01161&json=true","fetch_graph":"https://pith.science/api/pith-number/6ZAPBWYFJWKVSGV2FPSCKMJFQS/graph.json","fetch_events":"https://pith.science/api/pith-number/6ZAPBWYFJWKVSGV2FPSCKMJFQS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS/action/storage_attestation","attest_author":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS/action/author_attestation","sign_citation":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS/action/citation_signature","submit_replication":"https://pith.science/pith/6ZAPBWYFJWKVSGV2FPSCKMJFQS/action/replication_record"}},"created_at":"2026-07-05T03:40:44.198310+00:00","updated_at":"2026-07-05T03:40:44.198310+00:00"}