{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:357GQVOMH4F43NU7Y54B2HHDTX","short_pith_number":"pith:357GQVOM","schema_version":"1.0","canonical_sha256":"df7e6855cc3f0bcdb69fc7781d1ce39def17bab88737fde5a4e2913e715d1848","source":{"kind":"arxiv","id":"2306.09403","version":2},"attestation_state":"computed","paper":{"title":"Breaking degeneracies in the first galaxies with clustering","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Jordan Mirocha, Julian B. Mu\\~noz, Nashwan Sabti, Steven Furlanetto","submitted_at":"2023-06-15T18:00:00Z","abstract_excerpt":"The high-redshift galaxy UV luminosity function (UVLF) has become essential for understanding the formation and evolution of the first galaxies. Yet, UVLFs only measure galaxy abundances, giving rise to a degeneracy between the mean galaxy luminosity and its stochasticity. Here, we show that upcoming clustering measurements with the James Webb Space Telescope (JWST), as well as with Roman, will be able to break this degeneracy, even at redshifts $z \\gtrsim 10$. First, we demonstrate that current Subaru Hyper Suprime-Cam (HSC) measurements of the galaxy bias at $z\\sim 4-6$ point to a relatively"},"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":"2306.09403","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-06-15T18:00:00Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"36d0fa2409b7c9747f2cb2eef36a060b76f9a4a2ebc4de7f6ba4acd097bb94da","abstract_canon_sha256":"f58c6ec7ea61d3d99578197cc71e4dbd7a1b824e4cebfa0fd5cc52315cbbb47f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:43:03.304754Z","signature_b64":"ido2Rv8LreXpCRFtxXpe+gMiewikLTiUhcc/p7bTFMPaju0WQap3ha960uvAoACbSvrVqmxC7EmggLo5nZGXCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"df7e6855cc3f0bcdb69fc7781d1ce39def17bab88737fde5a4e2913e715d1848","last_reissued_at":"2026-07-05T06:43:03.304171Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:43:03.304171Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Breaking degeneracies in the first galaxies with clustering","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Jordan Mirocha, Julian B. Mu\\~noz, Nashwan Sabti, Steven Furlanetto","submitted_at":"2023-06-15T18:00:00Z","abstract_excerpt":"The high-redshift galaxy UV luminosity function (UVLF) has become essential for understanding the formation and evolution of the first galaxies. Yet, UVLFs only measure galaxy abundances, giving rise to a degeneracy between the mean galaxy luminosity and its stochasticity. Here, we show that upcoming clustering measurements with the James Webb Space Telescope (JWST), as well as with Roman, will be able to break this degeneracy, even at redshifts $z \\gtrsim 10$. First, we demonstrate that current Subaru Hyper Suprime-Cam (HSC) measurements of the galaxy bias at $z\\sim 4-6$ point to a relatively"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.09403","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/2306.09403/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":"2306.09403","created_at":"2026-07-05T06:43:03.304234+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.09403v2","created_at":"2026-07-05T06:43:03.304234+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.09403","created_at":"2026-07-05T06:43:03.304234+00:00"},{"alias_kind":"pith_short_12","alias_value":"357GQVOMH4F4","created_at":"2026-07-05T06:43:03.304234+00:00"},{"alias_kind":"pith_short_16","alias_value":"357GQVOMH4F43NU7","created_at":"2026-07-05T06:43:03.304234+00:00"},{"alias_kind":"pith_short_8","alias_value":"357GQVOM","created_at":"2026-07-05T06:43:03.304234+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.14312","citing_title":"An Improved Fit for Linear Halo Bias at High Redshift","ref_index":46,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX","json":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX.json","graph_json":"https://pith.science/api/pith-number/357GQVOMH4F43NU7Y54B2HHDTX/graph.json","events_json":"https://pith.science/api/pith-number/357GQVOMH4F43NU7Y54B2HHDTX/events.json","paper":"https://pith.science/paper/357GQVOM"},"agent_actions":{"view_html":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX","download_json":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX.json","view_paper":"https://pith.science/paper/357GQVOM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.09403&json=true","fetch_graph":"https://pith.science/api/pith-number/357GQVOMH4F43NU7Y54B2HHDTX/graph.json","fetch_events":"https://pith.science/api/pith-number/357GQVOMH4F43NU7Y54B2HHDTX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX/action/storage_attestation","attest_author":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX/action/author_attestation","sign_citation":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX/action/citation_signature","submit_replication":"https://pith.science/pith/357GQVOMH4F43NU7Y54B2HHDTX/action/replication_record"}},"created_at":"2026-07-05T06:43:03.304234+00:00","updated_at":"2026-07-05T06:43:03.304234+00:00"}