{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:7JQ2S72YH42MCL2IK4AOMB4Z32","short_pith_number":"pith:7JQ2S72Y","schema_version":"1.0","canonical_sha256":"fa61a97f583f34c12f485700e60799dea410be291f84974bbef00f6c8e7f91c9","source":{"kind":"arxiv","id":"1911.11144","version":2},"attestation_state":"computed","paper":{"title":"Probing the Small-Scale Matter Power Spectrum with Large-Scale 21-cm Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Cora Dvorkin, Francis-Yan Cyr-Racine, Julian B. Mu\\~noz","submitted_at":"2019-11-25T19:00:00Z","abstract_excerpt":"The distribution of matter fluctuations in our universe is key for understanding the nature of dark matter and the physics of the early cosmos. Different observables have been able to map this distribution at large scales, corresponding to wavenumbers $k\\lesssim 10$ Mpc$^{-1}$, but smaller scales remain much less constrained. The 21-cm line is a promising tracer of early stellar formation, which took place in small haloes (with masses $M\\sim 10^6-10^8M_\\odot$), formed out of matter overdensities with wavenumbers as large as $k\\approx100$ Mpc$^{-1}$. Here we forecast how well both the 21-cm glo"},"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":"1911.11144","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-11-25T19:00:00Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"5003cd30ce4a71ec76db89a93593e12dfa756881bf131cd7c0e293759e762fcc","abstract_canon_sha256":"605d71717b4d8ad8b83301d7d20101588f2d8bb9690ad6972e6ef082f053804d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:51:34.810512Z","signature_b64":"X48ROyn5qztcTrbftYUlppoji7Is8bkn6TVaU5anBIPBoY7yT+NxKGONay+zAZm6gZrrzzPL0yjMPt06AZFCDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fa61a97f583f34c12f485700e60799dea410be291f84974bbef00f6c8e7f91c9","last_reissued_at":"2026-07-05T00:51:34.810084Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:51:34.810084Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing the Small-Scale Matter Power Spectrum with Large-Scale 21-cm Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Cora Dvorkin, Francis-Yan Cyr-Racine, Julian B. Mu\\~noz","submitted_at":"2019-11-25T19:00:00Z","abstract_excerpt":"The distribution of matter fluctuations in our universe is key for understanding the nature of dark matter and the physics of the early cosmos. Different observables have been able to map this distribution at large scales, corresponding to wavenumbers $k\\lesssim 10$ Mpc$^{-1}$, but smaller scales remain much less constrained. The 21-cm line is a promising tracer of early stellar formation, which took place in small haloes (with masses $M\\sim 10^6-10^8M_\\odot$), formed out of matter overdensities with wavenumbers as large as $k\\approx100$ Mpc$^{-1}$. Here we forecast how well both the 21-cm glo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1911.11144","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/1911.11144/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":"1911.11144","created_at":"2026-07-05T00:51:34.810137+00:00"},{"alias_kind":"arxiv_version","alias_value":"1911.11144v2","created_at":"2026-07-05T00:51:34.810137+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1911.11144","created_at":"2026-07-05T00:51:34.810137+00:00"},{"alias_kind":"pith_short_12","alias_value":"7JQ2S72YH42M","created_at":"2026-07-05T00:51:34.810137+00:00"},{"alias_kind":"pith_short_16","alias_value":"7JQ2S72YH42MCL2I","created_at":"2026-07-05T00:51:34.810137+00:00"},{"alias_kind":"pith_short_8","alias_value":"7JQ2S72Y","created_at":"2026-07-05T00:51:34.810137+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.13527","citing_title":"Machine Learning Does It and Does It Better: Unearthing Primordial Dark-Matter Velocities from the Matter Power Spectrum","ref_index":42,"is_internal_anchor":false},{"citing_arxiv_id":"2510.17977","citing_title":"Growth of Structure in Multi-species Wave Dark Matter","ref_index":85,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32","json":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32.json","graph_json":"https://pith.science/api/pith-number/7JQ2S72YH42MCL2IK4AOMB4Z32/graph.json","events_json":"https://pith.science/api/pith-number/7JQ2S72YH42MCL2IK4AOMB4Z32/events.json","paper":"https://pith.science/paper/7JQ2S72Y"},"agent_actions":{"view_html":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32","download_json":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32.json","view_paper":"https://pith.science/paper/7JQ2S72Y","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1911.11144&json=true","fetch_graph":"https://pith.science/api/pith-number/7JQ2S72YH42MCL2IK4AOMB4Z32/graph.json","fetch_events":"https://pith.science/api/pith-number/7JQ2S72YH42MCL2IK4AOMB4Z32/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32/action/storage_attestation","attest_author":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32/action/author_attestation","sign_citation":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32/action/citation_signature","submit_replication":"https://pith.science/pith/7JQ2S72YH42MCL2IK4AOMB4Z32/action/replication_record"}},"created_at":"2026-07-05T00:51:34.810137+00:00","updated_at":"2026-07-05T00:51:34.810137+00:00"}