{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:F4H3TERPBNE7PFTKBWDUSTLHZS","short_pith_number":"pith:F4H3TERP","schema_version":"1.0","canonical_sha256":"2f0fb9922f0b49f7966a0d87494d67cca8cc0e2b9ee808a996f624576a21b294","source":{"kind":"arxiv","id":"1706.01471","version":3},"attestation_state":"computed","paper":{"title":"Constraining the CO intensity mapping power spectrum at intermediate redshifts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Hamsa Padmanabhan (ETH Zurich)","submitted_at":"2017-06-05T18:00:12Z","abstract_excerpt":"We compile available constraints on the carbon monoxide (CO) 1-0 luminosity functions and abundances at redshifts 0-3. This is used to develop a data driven halo model for the evolution of the CO galaxy abundances and clustering across intermediate redshifts. It is found that the recent constraints from the CO Power Spectrum Survey ($z \\sim 3$; Keating et al. 2016), when combined with existing observations of local galaxies ($z \\sim 0$; Keres et al. 2003), lead to predictions which are consistent with the results of smaller surveys at intermediate redshifts ($z \\sim 1-2$). We provide convenien"},"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":"1706.01471","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-06-05T18:00:12Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"30fb11a718dc033098a022ef70f25e298b9c7dfaa9b59a041f6597cd4fe0ff90","abstract_canon_sha256":"10bdabde961693f900fd2fb743d4aa9b8ea09e4f2c476bcb00774a8a71dab951"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:24:17.424311Z","signature_b64":"dbp+k+HuNqj3lXbSLCAfoMjJFiMD24wOH1OVvEABvi7SRmrBfEGdwMDe1FiL29MlTvav551NWGQ7i1F4CsgWBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2f0fb9922f0b49f7966a0d87494d67cca8cc0e2b9ee808a996f624576a21b294","last_reissued_at":"2026-05-18T00:24:17.423543Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:24:17.423543Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining the CO intensity mapping power spectrum at intermediate redshifts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Hamsa Padmanabhan (ETH Zurich)","submitted_at":"2017-06-05T18:00:12Z","abstract_excerpt":"We compile available constraints on the carbon monoxide (CO) 1-0 luminosity functions and abundances at redshifts 0-3. This is used to develop a data driven halo model for the evolution of the CO galaxy abundances and clustering across intermediate redshifts. It is found that the recent constraints from the CO Power Spectrum Survey ($z \\sim 3$; Keating et al. 2016), when combined with existing observations of local galaxies ($z \\sim 0$; Keres et al. 2003), lead to predictions which are consistent with the results of smaller surveys at intermediate redshifts ($z \\sim 1-2$). We provide convenien"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1706.01471","kind":"arxiv","version":3},"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":"1706.01471","created_at":"2026-05-18T00:24:17.423692+00:00"},{"alias_kind":"arxiv_version","alias_value":"1706.01471v3","created_at":"2026-05-18T00:24:17.423692+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1706.01471","created_at":"2026-05-18T00:24:17.423692+00:00"},{"alias_kind":"pith_short_12","alias_value":"F4H3TERPBNE7","created_at":"2026-05-18T12:31:15.632608+00:00"},{"alias_kind":"pith_short_16","alias_value":"F4H3TERPBNE7PFTK","created_at":"2026-05-18T12:31:15.632608+00:00"},{"alias_kind":"pith_short_8","alias_value":"F4H3TERP","created_at":"2026-05-18T12:31:15.632608+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.08128","citing_title":"Delensing Degree-Scale $B$-Mode Polarization with High-Redshift Line Intensity Mapping","ref_index":52,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS","json":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS.json","graph_json":"https://pith.science/api/pith-number/F4H3TERPBNE7PFTKBWDUSTLHZS/graph.json","events_json":"https://pith.science/api/pith-number/F4H3TERPBNE7PFTKBWDUSTLHZS/events.json","paper":"https://pith.science/paper/F4H3TERP"},"agent_actions":{"view_html":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS","download_json":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS.json","view_paper":"https://pith.science/paper/F4H3TERP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1706.01471&json=true","fetch_graph":"https://pith.science/api/pith-number/F4H3TERPBNE7PFTKBWDUSTLHZS/graph.json","fetch_events":"https://pith.science/api/pith-number/F4H3TERPBNE7PFTKBWDUSTLHZS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS/action/storage_attestation","attest_author":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS/action/author_attestation","sign_citation":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS/action/citation_signature","submit_replication":"https://pith.science/pith/F4H3TERPBNE7PFTKBWDUSTLHZS/action/replication_record"}},"created_at":"2026-05-18T00:24:17.423692+00:00","updated_at":"2026-05-18T00:24:17.423692+00:00"}