{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:4TEMLJVJPQQRQO4LQPOX42WVF6","short_pith_number":"pith:4TEMLJVJ","schema_version":"1.0","canonical_sha256":"e4c8c5a6a97c21183b8b83dd7e6ad52fb00a1b070e80293d0ee5e11942c732dd","source":{"kind":"arxiv","id":"0810.2788","version":1},"attestation_state":"computed","paper":{"title":"A Steep Faint-End Slope of the UV Luminosity Function at z~2-3: Implications for the Global Stellar Mass Density and Star Formation in Low Mass Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Charles C. Steidel (Caltech), Naveen A. Reddy (NOAO)","submitted_at":"2008-10-15T20:00:45Z","abstract_excerpt":"We use the deep ground-based optical photometry of the Lyman Break Galaxy (LBG) Survey to derive robust measurements of the faint-end slope (alpha) of the UV LF at redshifts 1.9<z<3.4. Our sample includes >2000 spectroscopic redshifts and ~31000 LBGs in 31 spatially-independent fields over a total area of 3261 arcmin^2. These data allow us to select galaxies to 0.07L* and 0.10L* at z~2 and z~3, respectively. A maximum likelihood analysis indicates steep values of alpha(z=2)=-1.73+/-0.07 and alpha(z=3)=-1.73+/-0.13. This result is robust to luminosity dependent systematics in the Ly-alpha equiv"},"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":"0810.2788","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-10-15T20:00:45Z","cross_cats_sorted":[],"title_canon_sha256":"7bc44252fcc044e1edb33815f4f8c1e647f5c076ff1d7c7e768a991b1b49c836","abstract_canon_sha256":"4c1692ded2ba677c20d06a14d712633e65eeb487c407aac9021c4dc8c2575f4f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:29:25.992992Z","signature_b64":"wJjHIj42svPiFskx2gcxKBPCs/toqpSwESH8ZD6Hrim+4DtffHswTAugoRShGnFPkyxWYUTi3YlIB4rYyNOqDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e4c8c5a6a97c21183b8b83dd7e6ad52fb00a1b070e80293d0ee5e11942c732dd","last_reissued_at":"2026-05-18T04:29:25.992529Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:29:25.992529Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Steep Faint-End Slope of the UV Luminosity Function at z~2-3: Implications for the Global Stellar Mass Density and Star Formation in Low Mass Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Charles C. Steidel (Caltech), Naveen A. Reddy (NOAO)","submitted_at":"2008-10-15T20:00:45Z","abstract_excerpt":"We use the deep ground-based optical photometry of the Lyman Break Galaxy (LBG) Survey to derive robust measurements of the faint-end slope (alpha) of the UV LF at redshifts 1.9<z<3.4. Our sample includes >2000 spectroscopic redshifts and ~31000 LBGs in 31 spatially-independent fields over a total area of 3261 arcmin^2. These data allow us to select galaxies to 0.07L* and 0.10L* at z~2 and z~3, respectively. A maximum likelihood analysis indicates steep values of alpha(z=2)=-1.73+/-0.07 and alpha(z=3)=-1.73+/-0.13. This result is robust to luminosity dependent systematics in the Ly-alpha equiv"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0810.2788","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":""},"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":"0810.2788","created_at":"2026-05-18T04:29:25.992600+00:00"},{"alias_kind":"arxiv_version","alias_value":"0810.2788v1","created_at":"2026-05-18T04:29:25.992600+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0810.2788","created_at":"2026-05-18T04:29:25.992600+00:00"},{"alias_kind":"pith_short_12","alias_value":"4TEMLJVJPQQR","created_at":"2026-05-18T12:25:56.245647+00:00"},{"alias_kind":"pith_short_16","alias_value":"4TEMLJVJPQQRQO4L","created_at":"2026-05-18T12:25:56.245647+00:00"},{"alias_kind":"pith_short_8","alias_value":"4TEMLJVJ","created_at":"2026-05-18T12:25:56.245647+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.07970","citing_title":"MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys","ref_index":246,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6","json":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6.json","graph_json":"https://pith.science/api/pith-number/4TEMLJVJPQQRQO4LQPOX42WVF6/graph.json","events_json":"https://pith.science/api/pith-number/4TEMLJVJPQQRQO4LQPOX42WVF6/events.json","paper":"https://pith.science/paper/4TEMLJVJ"},"agent_actions":{"view_html":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6","download_json":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6.json","view_paper":"https://pith.science/paper/4TEMLJVJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0810.2788&json=true","fetch_graph":"https://pith.science/api/pith-number/4TEMLJVJPQQRQO4LQPOX42WVF6/graph.json","fetch_events":"https://pith.science/api/pith-number/4TEMLJVJPQQRQO4LQPOX42WVF6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6/action/storage_attestation","attest_author":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6/action/author_attestation","sign_citation":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6/action/citation_signature","submit_replication":"https://pith.science/pith/4TEMLJVJPQQRQO4LQPOX42WVF6/action/replication_record"}},"created_at":"2026-05-18T04:29:25.992600+00:00","updated_at":"2026-05-18T04:29:25.992600+00:00"}