{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:SBYPZCUNN7SVN6XO6JOGRAOX7P","short_pith_number":"pith:SBYPZCUN","schema_version":"1.0","canonical_sha256":"9070fc8a8d6fe556faeef25c6881d7fbe0d4c7f9d2bda91774eb05e3ec17df89","source":{"kind":"arxiv","id":"1604.01036","version":2},"attestation_state":"computed","paper":{"title":"The high mass end of the stellar mass function: Dependence on stellar population models and agreement between fits to the light profile","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. Meert, C. Maraston, F. Shankar, J.-L. Fischer, M. Bernardi, M. Huertas-Company, R. K. Sheth, V. Vikram","submitted_at":"2016-04-04T20:00:25Z","abstract_excerpt":"We quantify the systematic effects on the stellar mass function which arise from assumptions about the stellar population, as well as how one fits the light profiles of the most luminous galaxies at z ~ 0.1. When comparing results from the literature, we are careful to separate out these effects. Our analysis shows that while systematics in the estimated comoving number density which arise from different treatments of the stellar population remain of order < 0.5 dex, systematics in photometry are now about 0.1 dex, despite recent claims in the literature. Compared to these more recent analyses"},"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":"1604.01036","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-04-04T20:00:25Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"f6893c4c1439c54b4a2f0d94dbd58e74c1c409a1ea795c7bdad54960f421ada7","abstract_canon_sha256":"424ff748046eab73eee2b389fe58ed255cd6f8a58c7fa38a5a60832c6e848d43"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:49:52.349939Z","signature_b64":"xYcCSe1EIGxduN5KKhMroMixy3YUl3Ra6dpRAMJmBflgfAt/Yjiw/zY0mCLPkK8dFbxibvISbJBvzTgAZBzzAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9070fc8a8d6fe556faeef25c6881d7fbe0d4c7f9d2bda91774eb05e3ec17df89","last_reissued_at":"2026-05-18T00:49:52.349574Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:49:52.349574Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The high mass end of the stellar mass function: Dependence on stellar population models and agreement between fits to the light profile","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"A. Meert, C. Maraston, F. Shankar, J.-L. Fischer, M. Bernardi, M. Huertas-Company, R. K. Sheth, V. Vikram","submitted_at":"2016-04-04T20:00:25Z","abstract_excerpt":"We quantify the systematic effects on the stellar mass function which arise from assumptions about the stellar population, as well as how one fits the light profiles of the most luminous galaxies at z ~ 0.1. When comparing results from the literature, we are careful to separate out these effects. Our analysis shows that while systematics in the estimated comoving number density which arise from different treatments of the stellar population remain of order < 0.5 dex, systematics in photometry are now about 0.1 dex, despite recent claims in the literature. Compared to these more recent analyses"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1604.01036","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":""},"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":"1604.01036","created_at":"2026-05-18T00:49:52.349630+00:00"},{"alias_kind":"arxiv_version","alias_value":"1604.01036v2","created_at":"2026-05-18T00:49:52.349630+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1604.01036","created_at":"2026-05-18T00:49:52.349630+00:00"},{"alias_kind":"pith_short_12","alias_value":"SBYPZCUNN7SV","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_16","alias_value":"SBYPZCUNN7SVN6XO","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_8","alias_value":"SBYPZCUN","created_at":"2026-05-18T12:30:44.179134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21599","citing_title":"JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: stellar population catalogue for galaxies in GOODS-N and GOODS-S","ref_index":68,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P","json":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P.json","graph_json":"https://pith.science/api/pith-number/SBYPZCUNN7SVN6XO6JOGRAOX7P/graph.json","events_json":"https://pith.science/api/pith-number/SBYPZCUNN7SVN6XO6JOGRAOX7P/events.json","paper":"https://pith.science/paper/SBYPZCUN"},"agent_actions":{"view_html":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P","download_json":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P.json","view_paper":"https://pith.science/paper/SBYPZCUN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1604.01036&json=true","fetch_graph":"https://pith.science/api/pith-number/SBYPZCUNN7SVN6XO6JOGRAOX7P/graph.json","fetch_events":"https://pith.science/api/pith-number/SBYPZCUNN7SVN6XO6JOGRAOX7P/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P/action/storage_attestation","attest_author":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P/action/author_attestation","sign_citation":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P/action/citation_signature","submit_replication":"https://pith.science/pith/SBYPZCUNN7SVN6XO6JOGRAOX7P/action/replication_record"}},"created_at":"2026-05-18T00:49:52.349630+00:00","updated_at":"2026-05-18T00:49:52.349630+00:00"}