{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:DIDWX5OZN6YOVGR5I6PP3DNZDA","short_pith_number":"pith:DIDWX5OZ","schema_version":"1.0","canonical_sha256":"1a076bf5d96fb0ea9a3d479efd8db918101d3ac58ca974c76f3acaacbaacb4f0","source":{"kind":"arxiv","id":"1801.07260","version":1},"attestation_state":"computed","paper":{"title":"Does the Hubble constant tension call for new physics?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Edvard M\\\"ortsell, Suhail Dhawan","submitted_at":"2018-01-22T19:00:03Z","abstract_excerpt":"The $\\Lambda$ Cold Dark Matter model ($\\Lambda$CDM) represents the current standard model in cosmology. Within this, there is a tension between the value of the Hubble constant, $H_0$, inferred from local distance indicators and the angular scale of fluctuations in the Cosmic Microwave Background (CMB). We investigate whether the tension is significant enough to warrant new physics in the form of modifying or adding energy components to the standard cosmological model. We find that late time dark energy explanations are slightly disfavoured whereas a pre-CMB decoupling extra dark energy compon"},"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":"1801.07260","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-01-22T19:00:03Z","cross_cats_sorted":[],"title_canon_sha256":"d14394f79a9b02ce2a040125a453a4c38f2d8eb37248ddf4eb794918f615e44c","abstract_canon_sha256":"e79f1ef6571fc6a95f2594b458ade440800d340dddcef931e17386d252e3ea93"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:04:59.687100Z","signature_b64":"+e5GyM25gkKbxaeFTFkUK+clvdwwxxYsLsdfyqB3QMsZkf85qbqlhHqNwFMCWtB2+bTL64TBCuDUvkxu25cFCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1a076bf5d96fb0ea9a3d479efd8db918101d3ac58ca974c76f3acaacbaacb4f0","last_reissued_at":"2026-05-18T00:04:59.686658Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:04:59.686658Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Does the Hubble constant tension call for new physics?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Edvard M\\\"ortsell, Suhail Dhawan","submitted_at":"2018-01-22T19:00:03Z","abstract_excerpt":"The $\\Lambda$ Cold Dark Matter model ($\\Lambda$CDM) represents the current standard model in cosmology. Within this, there is a tension between the value of the Hubble constant, $H_0$, inferred from local distance indicators and the angular scale of fluctuations in the Cosmic Microwave Background (CMB). We investigate whether the tension is significant enough to warrant new physics in the form of modifying or adding energy components to the standard cosmological model. We find that late time dark energy explanations are slightly disfavoured whereas a pre-CMB decoupling extra dark energy compon"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1801.07260","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"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":"1801.07260","created_at":"2026-05-18T00:04:59.686720+00:00"},{"alias_kind":"arxiv_version","alias_value":"1801.07260v1","created_at":"2026-05-18T00:04:59.686720+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1801.07260","created_at":"2026-05-18T00:04:59.686720+00:00"},{"alias_kind":"pith_short_12","alias_value":"DIDWX5OZN6YO","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_16","alias_value":"DIDWX5OZN6YOVGR5","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_8","alias_value":"DIDWX5OZ","created_at":"2026-05-18T12:32:19.392346+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2402.07716","citing_title":"$\\Lambda_{\\rm s}$CDM cosmology from a type-II minimally modified gravity","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2602.11936","citing_title":"Probing Dynamical Dark Energy with Late-Time Data: Evidence, Tensions, and the Limits of the $w_0w_a$CDM Framework","ref_index":102,"is_internal_anchor":true},{"citing_arxiv_id":"2507.11526","citing_title":"Gravitational wave propagation in bigravity in the late universe","ref_index":17,"is_internal_anchor":true},{"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":146,"is_internal_anchor":true},{"citing_arxiv_id":"2103.01183","citing_title":"In the Realm of the Hubble tension $-$ a Review of Solutions","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2604.25813","citing_title":"Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension","ref_index":90,"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":28,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA","json":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA.json","graph_json":"https://pith.science/api/pith-number/DIDWX5OZN6YOVGR5I6PP3DNZDA/graph.json","events_json":"https://pith.science/api/pith-number/DIDWX5OZN6YOVGR5I6PP3DNZDA/events.json","paper":"https://pith.science/paper/DIDWX5OZ"},"agent_actions":{"view_html":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA","download_json":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA.json","view_paper":"https://pith.science/paper/DIDWX5OZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1801.07260&json=true","fetch_graph":"https://pith.science/api/pith-number/DIDWX5OZN6YOVGR5I6PP3DNZDA/graph.json","fetch_events":"https://pith.science/api/pith-number/DIDWX5OZN6YOVGR5I6PP3DNZDA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA/action/storage_attestation","attest_author":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA/action/author_attestation","sign_citation":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA/action/citation_signature","submit_replication":"https://pith.science/pith/DIDWX5OZN6YOVGR5I6PP3DNZDA/action/replication_record"}},"created_at":"2026-05-18T00:04:59.686720+00:00","updated_at":"2026-05-18T00:04:59.686720+00:00"}