{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:SYYVC43CARRFEZ465O3LVXPAQG","short_pith_number":"pith:SYYVC43C","schema_version":"1.0","canonical_sha256":"9631517362046252679eebb6badde081b24eab55f9c3c9ca9558488c9deecc4f","source":{"kind":"arxiv","id":"0804.2892","version":2},"attestation_state":"computed","paper":{"title":"On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"I. K. Baldry, K. Glazebrook, S. P. Driver","submitted_at":"2008-04-17T20:04:20Z","abstract_excerpt":"A comparison between published field galaxy stellar mass functions (GSMFs) shows that the cosmic stellar mass density is in the range 4--8 per cent of the baryon density (assuming Omega_b = 0.045). There remain significant sources of uncertainty for the dust correction and underlying stellar mass-to-light ratio even assuming a reasonable universal stellar initial mass function. We determine the z < 0.05 GSMF using the New York University - Value-Added Galaxy Catalog sample of 49968 galaxies derived from the Sloan Digital Sky Survey and various estimates of stellar mass. The GSMF shows clear ev"},"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":"0804.2892","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-04-17T20:04:20Z","cross_cats_sorted":[],"title_canon_sha256":"56b80e13b05b3cd9f807fd9e2c8b53a048ec5d051a303ebc3e11d410f83883f8","abstract_canon_sha256":"6a1337b4444faa6fa6dc0913c32c62d85cec57121b41e9b0ff5bb8ba27717508"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:10:24.354532Z","signature_b64":"ZSKisIL9WAMPy33LcqAafvUPhE3ljhkX3KstTJ9B+68gz4V9INYgqKuoYG/lm0WJ5udraIbQ4sjTwURQJ/CJBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9631517362046252679eebb6badde081b24eab55f9c3c9ca9558488c9deecc4f","last_reissued_at":"2026-07-04T17:10:24.354081Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:10:24.354081Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"I. K. Baldry, K. Glazebrook, S. P. Driver","submitted_at":"2008-04-17T20:04:20Z","abstract_excerpt":"A comparison between published field galaxy stellar mass functions (GSMFs) shows that the cosmic stellar mass density is in the range 4--8 per cent of the baryon density (assuming Omega_b = 0.045). There remain significant sources of uncertainty for the dust correction and underlying stellar mass-to-light ratio even assuming a reasonable universal stellar initial mass function. We determine the z < 0.05 GSMF using the New York University - Value-Added Galaxy Catalog sample of 49968 galaxies derived from the Sloan Digital Sky Survey and various estimates of stellar mass. The GSMF shows clear ev"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0804.2892","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/0804.2892/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":"0804.2892","created_at":"2026-07-04T17:10:24.354142+00:00"},{"alias_kind":"arxiv_version","alias_value":"0804.2892v2","created_at":"2026-07-04T17:10:24.354142+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0804.2892","created_at":"2026-07-04T17:10:24.354142+00:00"},{"alias_kind":"pith_short_12","alias_value":"SYYVC43CARRF","created_at":"2026-07-04T17:10:24.354142+00:00"},{"alias_kind":"pith_short_16","alias_value":"SYYVC43CARRFEZ46","created_at":"2026-07-04T17:10:24.354142+00:00"},{"alias_kind":"pith_short_8","alias_value":"SYYVC43C","created_at":"2026-07-04T17:10:24.354142+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.21260","citing_title":"Dark-matter-induced transients over cosmic time: The role of star formation history profiles","ref_index":52,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG","json":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG.json","graph_json":"https://pith.science/api/pith-number/SYYVC43CARRFEZ465O3LVXPAQG/graph.json","events_json":"https://pith.science/api/pith-number/SYYVC43CARRFEZ465O3LVXPAQG/events.json","paper":"https://pith.science/paper/SYYVC43C"},"agent_actions":{"view_html":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG","download_json":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG.json","view_paper":"https://pith.science/paper/SYYVC43C","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0804.2892&json=true","fetch_graph":"https://pith.science/api/pith-number/SYYVC43CARRFEZ465O3LVXPAQG/graph.json","fetch_events":"https://pith.science/api/pith-number/SYYVC43CARRFEZ465O3LVXPAQG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG/action/storage_attestation","attest_author":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG/action/author_attestation","sign_citation":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG/action/citation_signature","submit_replication":"https://pith.science/pith/SYYVC43CARRFEZ465O3LVXPAQG/action/replication_record"}},"created_at":"2026-07-04T17:10:24.354142+00:00","updated_at":"2026-07-04T17:10:24.354142+00:00"}