{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:LR5G4B567ZRPFD2CHYOELBLRPA","short_pith_number":"pith:LR5G4B56","schema_version":"1.0","canonical_sha256":"5c7a6e07befe62f28f423e1c45857178265c5a37d831eba8f894a05156b66d73","source":{"kind":"arxiv","id":"1902.09554","version":2},"attestation_state":"computed","paper":{"title":"The MOSDEF Survey: Kinematic and Structural Evolution of Star-Forming Galaxies at $1.4\\leq z\\leq 3.8$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Alice E. Shapley, Alison L. Coil, Bahram Mobasher, Brian Siana, Gene C. K. Leung, Guillermo Barro, Hannah \\\"Ubler, Irene Shivaei, Laura de Groot, Mariska Kriek, Mojegan Azadi, Natascha M. F\\\"orster Schreiber, Naveen A. Reddy, Ryan L. Sanders, Sedona H. Price, Tara Fetherolf, Tom O. Zick, William R. Freeman","submitted_at":"2019-02-25T19:00:02Z","abstract_excerpt":"We present ionized gas kinematics for 681 galaxies at $z\\sim 1.4-3.8$ from the MOSFIRE Deep Evolution Field survey, measured using models which account for random galaxy-slit misalignments together with structural parameters derived from CANDELS Hubble Space Telescope (HST) imaging. Kinematics and sizes are used to derive dynamical masses. Baryonic masses are estimated from stellar masses and inferred gas masses from dust-corrected star formation rates (SFRs) and the Kennicutt-Schmidt relation. We measure resolved rotation for 105 galaxies. For the remaining 576 galaxies we use models based on"},"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":"1902.09554","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-02-25T19:00:02Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"258da7a0177b855077ac5eff32243968a471ca93a4d265429538635dd7e1bb7d","abstract_canon_sha256":"7cb141209279414684a595860a63079c9d794728d6d8187cd62063c095e52fc3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:03:58.227764Z","signature_b64":"xCwYNJM6fi6iTOyXatj1YDGPK+4rxYuRbGlNeOyZip+jGODg52a40i2YGr7F+WC9ttKG7ce93/qTRMr/u/8eAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5c7a6e07befe62f28f423e1c45857178265c5a37d831eba8f894a05156b66d73","last_reissued_at":"2026-07-05T01:03:58.227263Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:03:58.227263Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The MOSDEF Survey: Kinematic and Structural Evolution of Star-Forming Galaxies at $1.4\\leq z\\leq 3.8$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Alice E. Shapley, Alison L. Coil, Bahram Mobasher, Brian Siana, Gene C. K. Leung, Guillermo Barro, Hannah \\\"Ubler, Irene Shivaei, Laura de Groot, Mariska Kriek, Mojegan Azadi, Natascha M. F\\\"orster Schreiber, Naveen A. Reddy, Ryan L. Sanders, Sedona H. Price, Tara Fetherolf, Tom O. Zick, William R. Freeman","submitted_at":"2019-02-25T19:00:02Z","abstract_excerpt":"We present ionized gas kinematics for 681 galaxies at $z\\sim 1.4-3.8$ from the MOSFIRE Deep Evolution Field survey, measured using models which account for random galaxy-slit misalignments together with structural parameters derived from CANDELS Hubble Space Telescope (HST) imaging. Kinematics and sizes are used to derive dynamical masses. Baryonic masses are estimated from stellar masses and inferred gas masses from dust-corrected star formation rates (SFRs) and the Kennicutt-Schmidt relation. We measure resolved rotation for 105 galaxies. For the remaining 576 galaxies we use models based on"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1902.09554","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/1902.09554/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":"1902.09554","created_at":"2026-07-05T01:03:58.227323+00:00"},{"alias_kind":"arxiv_version","alias_value":"1902.09554v2","created_at":"2026-07-05T01:03:58.227323+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1902.09554","created_at":"2026-07-05T01:03:58.227323+00:00"},{"alias_kind":"pith_short_12","alias_value":"LR5G4B567ZRP","created_at":"2026-07-05T01:03:58.227323+00:00"},{"alias_kind":"pith_short_16","alias_value":"LR5G4B567ZRPFD2C","created_at":"2026-07-05T01:03:58.227323+00:00"},{"alias_kind":"pith_short_8","alias_value":"LR5G4B56","created_at":"2026-07-05T01:03:58.227323+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA","json":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA.json","graph_json":"https://pith.science/api/pith-number/LR5G4B567ZRPFD2CHYOELBLRPA/graph.json","events_json":"https://pith.science/api/pith-number/LR5G4B567ZRPFD2CHYOELBLRPA/events.json","paper":"https://pith.science/paper/LR5G4B56"},"agent_actions":{"view_html":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA","download_json":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA.json","view_paper":"https://pith.science/paper/LR5G4B56","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1902.09554&json=true","fetch_graph":"https://pith.science/api/pith-number/LR5G4B567ZRPFD2CHYOELBLRPA/graph.json","fetch_events":"https://pith.science/api/pith-number/LR5G4B567ZRPFD2CHYOELBLRPA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA/action/storage_attestation","attest_author":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA/action/author_attestation","sign_citation":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA/action/citation_signature","submit_replication":"https://pith.science/pith/LR5G4B567ZRPFD2CHYOELBLRPA/action/replication_record"}},"created_at":"2026-07-05T01:03:58.227323+00:00","updated_at":"2026-07-05T01:03:58.227323+00:00"}