{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:5GSUNCWHECVYCAXHSC7B4IKF2F","short_pith_number":"pith:5GSUNCWH","schema_version":"1.0","canonical_sha256":"e9a5468ac720ab8102e790be1e2145d14cea8c8251216e871f14778806e5c49c","source":{"kind":"arxiv","id":"astro-ph/0009217","version":3},"attestation_state":"computed","paper":{"title":"The Milky Way in Molecular Clouds: A New Complete CO Survey","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Dap Hartmann, P. Thaddeus (Harvard-Smithsonian Center for Astrophysics), T. M. Dame","submitted_at":"2000-09-13T22:40:54Z","abstract_excerpt":"New large-scale CO surveys of the first and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the CfA 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth (1/8-deg) sample the entire Galactic plane over a strip 4-10 deg wide in latitude, and beamwidth or 1/4-deg sample nearly all large local clouds at higher "},"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":"astro-ph/0009217","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-09-13T22:40:54Z","cross_cats_sorted":[],"title_canon_sha256":"e50ff056a933fe6448e592ebc8b68f80fc57a81d9d1830c4ac79804a8b54819e","abstract_canon_sha256":"751e788c2f2f8b8c1c49164c4ae7ee3f82f9eb38b4e45857bdce901d472cfee0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:17:09.403232Z","signature_b64":"WEhPKvKEnLrgd3nQREinq5t3tWcpdvtu5HnMJapXhgQAQ8ZSyTYwBfEmiyuGsVCC9+PX6g7DnafdvnRm1vlvCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e9a5468ac720ab8102e790be1e2145d14cea8c8251216e871f14778806e5c49c","last_reissued_at":"2026-07-04T16:17:09.402893Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:17:09.402893Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Milky Way in Molecular Clouds: A New Complete CO Survey","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Dap Hartmann, P. Thaddeus (Harvard-Smithsonian Center for Astrophysics), T. M. Dame","submitted_at":"2000-09-13T22:40:54Z","abstract_excerpt":"New large-scale CO surveys of the first and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the CfA 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth (1/8-deg) sample the entire Galactic plane over a strip 4-10 deg wide in latitude, and beamwidth or 1/4-deg sample nearly all large local clouds at higher "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0009217","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0009217/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":"astro-ph/0009217","created_at":"2026-07-04T16:17:09.402941+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0009217v3","created_at":"2026-07-04T16:17:09.402941+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0009217","created_at":"2026-07-04T16:17:09.402941+00:00"},{"alias_kind":"pith_short_12","alias_value":"5GSUNCWHECVY","created_at":"2026-07-04T16:17:09.402941+00:00"},{"alias_kind":"pith_short_16","alias_value":"5GSUNCWHECVYCAXH","created_at":"2026-07-04T16:17:09.402941+00:00"},{"alias_kind":"pith_short_8","alias_value":"5GSUNCWH","created_at":"2026-07-04T16:17:09.402941+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":34,"internal_anchor_count":23,"sample":[{"citing_arxiv_id":"2607.07451","citing_title":"Milky Way Atlas: A radial-velocity-resolved, three-dimensional map of H I within 1.25 kpc","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01886","citing_title":"Distance Determination of Southern Galactic Plane Supernova Remnants with the Mopra CO Survey and DECaPS 3D Dust Map","ref_index":17,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09604","citing_title":"Modelling Galactic neutrino emission: contributions from massive star clusters and interstellar cosmic rays","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00872","citing_title":"Kolmogorov turbulence across multi-fractal gas in Polaris Flare","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26278","citing_title":"The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27853","citing_title":"MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec","ref_index":227,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28314","citing_title":"The Role of Scintillation in Detecting HI Absorption in FRB Spectra","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02028","citing_title":"A study of the Physical Properties and Star Formation Activity of a Large Sample of Molecular Clouds: I Distances","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2606.04309","citing_title":"CO-dark molecular gas traced by HCO$^+$ in the diffuse interstellar medium","ref_index":9,"is_internal_anchor":true},{"citing_arxiv_id":"2606.16403","citing_title":"Co-evolution of bar and spiral arms in TNG50 simulations using Information Theory","ref_index":104,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19694","citing_title":"PMO Polaris CO survey. II. Where is the dust?","ref_index":64,"is_internal_anchor":true},{"citing_arxiv_id":"2606.22354","citing_title":"EMU discovery of Thunder: a bow-shock PWN powered by PSR J1631-4722 escaping Nimbus SNR (G336.7+0.5)","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27346","citing_title":"3D Magnetic Field Vectors in Space: Bubbles, Clouds, and Filaments","ref_index":24,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26278","citing_title":"The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26320","citing_title":"Probing the molecular gas content of galaxies in an over-dense group at z~0.7: a test case for environmental quenching","ref_index":260,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24444","citing_title":"Statistical Properties of Molecular Clouds in the Milky Way: Insights from Three-Isotopologue CO Observations of the MWISP Project","ref_index":17,"is_internal_anchor":true},{"citing_arxiv_id":"2605.23136","citing_title":"A Gaia-linked High-purity QSO Candidate Catalog in Selected Fields with Extinction-binned Calibration and Spectrum-informed Training","ref_index":20,"is_internal_anchor":true},{"citing_arxiv_id":"2404.13520","citing_title":"An ALMA search for substructure and fragmentation in starless cores in Orion B North","ref_index":19,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21101","citing_title":"B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12","ref_index":134,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15659","citing_title":"Sub-kpc scale gas density histograms of the nearby barred spiral galaxy M83: Multi-component molecular gas structure reflecting the galactic environment","ref_index":50,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17253","citing_title":"HI Observations of Baryon-Dominated Dwarf Galaxy Candidates","ref_index":121,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17636","citing_title":"Diffuse gamma-ray emission in the vicinity of open cluster Berkeley 87","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15489","citing_title":"GeV {\\gamma}-ray emission in the low-mass star-forming region AFGL 490","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2603.05896","citing_title":"An updated model for the Perseus Spiral Arm from Trigonometric Parallax and 3-dimensional kinematic distances of distant massive stars","ref_index":11,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10294","citing_title":"Wolf-Rayet stars as tracers of gamma-ray emission: Isolated stars and stellar clusters/associations","ref_index":233,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F","json":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F.json","graph_json":"https://pith.science/api/pith-number/5GSUNCWHECVYCAXHSC7B4IKF2F/graph.json","events_json":"https://pith.science/api/pith-number/5GSUNCWHECVYCAXHSC7B4IKF2F/events.json","paper":"https://pith.science/paper/5GSUNCWH"},"agent_actions":{"view_html":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F","download_json":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F.json","view_paper":"https://pith.science/paper/5GSUNCWH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0009217&json=true","fetch_graph":"https://pith.science/api/pith-number/5GSUNCWHECVYCAXHSC7B4IKF2F/graph.json","fetch_events":"https://pith.science/api/pith-number/5GSUNCWHECVYCAXHSC7B4IKF2F/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F/action/storage_attestation","attest_author":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F/action/author_attestation","sign_citation":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F/action/citation_signature","submit_replication":"https://pith.science/pith/5GSUNCWHECVYCAXHSC7B4IKF2F/action/replication_record"}},"created_at":"2026-07-04T16:17:09.402941+00:00","updated_at":"2026-07-04T16:17:09.402941+00:00"}