{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:AQLT4S276BPDZ4N23UN7FFXXDD","short_pith_number":"pith:AQLT4S27","schema_version":"1.0","canonical_sha256":"04173e4b5ff05e3cf1badd1bf296f718c101d7cd62f17afb4016d62439efd753","source":{"kind":"arxiv","id":"0902.3997","version":1},"attestation_state":"computed","paper":{"title":"A spectroscopic measure of the star-formation rate density in dwarf galaxies at z~1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Gilbank, G.K.T. Hau, G.T. Davies, I.H. Li, I.K. Baldry, Karl Glazebrook, Michael Balogh, P. McCarthy, Richard Bower, S. Savaglio","submitted_at":"2009-02-23T21:00:08Z","abstract_excerpt":"We use a K-selected (22.5 < K_AB < 24.0) sample of dwarf galaxies (8.4 < log(M*/Msun) < 10) at 0.89<z<1.15 in the Chandra Deep Field South (CDFS) to measure their contribution to the global star-formation rate density (SFRD), as inferred from their [OII] flux. By comparing with [OII]-based studies of higher stellar mass galaxies, we robustly measure a turnover in the [OII] luminosity density at a stellar mass of M~10^10 Msun. By comparison with the [OII]-based SFRD measured from the Sloan Digital Sky Survey we confirm that, while the SFRD of the lowest-mass galaxies changes very little with ti"},"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":"0902.3997","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-02-23T21:00:08Z","cross_cats_sorted":[],"title_canon_sha256":"3e0917a2bd6e6294af94d494996eb53ad6f356342211d292a8519b5f2daade32","abstract_canon_sha256":"54beba4becc906f4b8fd75b3cbe19608e68782757dec7278bf8c25434656cac3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:14:27.986426Z","signature_b64":"eLqy9Wlly5VVxsyeEfSF4+pQ3iPOYdkGWP6fjFcWN9YjB0h0ZuXLkGEIphFo5mGuH3cKngLFshszhNIvpIRMDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"04173e4b5ff05e3cf1badd1bf296f718c101d7cd62f17afb4016d62439efd753","last_reissued_at":"2026-07-04T17:14:27.986011Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:14:27.986011Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A spectroscopic measure of the star-formation rate density in dwarf galaxies at z~1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Gilbank, G.K.T. Hau, G.T. Davies, I.H. Li, I.K. Baldry, Karl Glazebrook, Michael Balogh, P. McCarthy, Richard Bower, S. Savaglio","submitted_at":"2009-02-23T21:00:08Z","abstract_excerpt":"We use a K-selected (22.5 < K_AB < 24.0) sample of dwarf galaxies (8.4 < log(M*/Msun) < 10) at 0.89<z<1.15 in the Chandra Deep Field South (CDFS) to measure their contribution to the global star-formation rate density (SFRD), as inferred from their [OII] flux. By comparing with [OII]-based studies of higher stellar mass galaxies, we robustly measure a turnover in the [OII] luminosity density at a stellar mass of M~10^10 Msun. By comparison with the [OII]-based SFRD measured from the Sloan Digital Sky Survey we confirm that, while the SFRD of the lowest-mass galaxies changes very little with ti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0902.3997","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0902.3997/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":"0902.3997","created_at":"2026-07-04T17:14:27.986075+00:00"},{"alias_kind":"arxiv_version","alias_value":"0902.3997v1","created_at":"2026-07-04T17:14:27.986075+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0902.3997","created_at":"2026-07-04T17:14:27.986075+00:00"},{"alias_kind":"pith_short_12","alias_value":"AQLT4S276BPD","created_at":"2026-07-04T17:14:27.986075+00:00"},{"alias_kind":"pith_short_16","alias_value":"AQLT4S276BPDZ4N2","created_at":"2026-07-04T17:14:27.986075+00:00"},{"alias_kind":"pith_short_8","alias_value":"AQLT4S27","created_at":"2026-07-04T17:14:27.986075+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/AQLT4S276BPDZ4N23UN7FFXXDD","json":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD.json","graph_json":"https://pith.science/api/pith-number/AQLT4S276BPDZ4N23UN7FFXXDD/graph.json","events_json":"https://pith.science/api/pith-number/AQLT4S276BPDZ4N23UN7FFXXDD/events.json","paper":"https://pith.science/paper/AQLT4S27"},"agent_actions":{"view_html":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD","download_json":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD.json","view_paper":"https://pith.science/paper/AQLT4S27","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0902.3997&json=true","fetch_graph":"https://pith.science/api/pith-number/AQLT4S276BPDZ4N23UN7FFXXDD/graph.json","fetch_events":"https://pith.science/api/pith-number/AQLT4S276BPDZ4N23UN7FFXXDD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD/action/storage_attestation","attest_author":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD/action/author_attestation","sign_citation":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD/action/citation_signature","submit_replication":"https://pith.science/pith/AQLT4S276BPDZ4N23UN7FFXXDD/action/replication_record"}},"created_at":"2026-07-04T17:14:27.986075+00:00","updated_at":"2026-07-04T17:14:27.986075+00:00"}