{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:FQ65IAOQHDXW4ZDJDMCQZPZF7I","short_pith_number":"pith:FQ65IAOQ","schema_version":"1.0","canonical_sha256":"2c3dd401d038ef6e64691b050cbf25fa22415cc2a41bea459c93c8a3112cb33f","source":{"kind":"arxiv","id":"1304.4421","version":1},"attestation_state":"computed","paper":{"title":"Single Colour Diagnostics of the Mass-to-light Ratio: Predictions from Galaxy Formation Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Carlton M. Baugh, Cedric G. Lacey, Joe Zuntz, Stephen M. Wilkins, Violeta Gonzalez-Perez","submitted_at":"2013-04-16T12:49:28Z","abstract_excerpt":"Accurate galaxy stellar masses are crucial to better understand the physical mechanisms driving the galaxy formation process. We use synthetic star formation and metal enrichment histories predicted by the {\\sc galform} galaxy formation model to investigate the precision with which various colours $(m_{a}-m_{b})$ can alone be used as diagnostics of the stellar mass-to-light ratio. As an example, we find that, at $z=0$, the {\\em intrinsic} (B$_{f435w}-$V$_{f606w}$) colour can be used to determine the intrinsic rest-frame $V$-band stellar mass-to-light ratio ($\\log_{10}\\Gamma_{V}=\\log_{10}[(M/M_"},"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":"1304.4421","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-04-16T12:49:28Z","cross_cats_sorted":[],"title_canon_sha256":"c32c9bc20ca2f337cdf90bbdad57b8c3b0878ddba1bbc902e1a8fb2bb4e6bcca","abstract_canon_sha256":"f0f1289df526de6169ecfdd376660118789110c02f015f53bc68f0db66596af8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:50:32.276824Z","signature_b64":"bJ3oy6OzUYvMiJeIfwFsojgMvfFRHBwFKAdIp+RtG/TxP3210Da7C1ONrox4jpSHOexXSAwsQjqVsSOHcDFlAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2c3dd401d038ef6e64691b050cbf25fa22415cc2a41bea459c93c8a3112cb33f","last_reissued_at":"2026-05-18T01:50:32.276286Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:50:32.276286Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Single Colour Diagnostics of the Mass-to-light Ratio: Predictions from Galaxy Formation Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Carlton M. Baugh, Cedric G. Lacey, Joe Zuntz, Stephen M. Wilkins, Violeta Gonzalez-Perez","submitted_at":"2013-04-16T12:49:28Z","abstract_excerpt":"Accurate galaxy stellar masses are crucial to better understand the physical mechanisms driving the galaxy formation process. We use synthetic star formation and metal enrichment histories predicted by the {\\sc galform} galaxy formation model to investigate the precision with which various colours $(m_{a}-m_{b})$ can alone be used as diagnostics of the stellar mass-to-light ratio. As an example, we find that, at $z=0$, the {\\em intrinsic} (B$_{f435w}-$V$_{f606w}$) colour can be used to determine the intrinsic rest-frame $V$-band stellar mass-to-light ratio ($\\log_{10}\\Gamma_{V}=\\log_{10}[(M/M_"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1304.4421","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":"1304.4421","created_at":"2026-05-18T01:50:32.276365+00:00"},{"alias_kind":"arxiv_version","alias_value":"1304.4421v1","created_at":"2026-05-18T01:50:32.276365+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1304.4421","created_at":"2026-05-18T01:50:32.276365+00:00"},{"alias_kind":"pith_short_12","alias_value":"FQ65IAOQHDXW","created_at":"2026-05-18T12:27:45.050594+00:00"},{"alias_kind":"pith_short_16","alias_value":"FQ65IAOQHDXW4ZDJ","created_at":"2026-05-18T12:27:45.050594+00:00"},{"alias_kind":"pith_short_8","alias_value":"FQ65IAOQ","created_at":"2026-05-18T12:27:45.050594+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/FQ65IAOQHDXW4ZDJDMCQZPZF7I","json":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I.json","graph_json":"https://pith.science/api/pith-number/FQ65IAOQHDXW4ZDJDMCQZPZF7I/graph.json","events_json":"https://pith.science/api/pith-number/FQ65IAOQHDXW4ZDJDMCQZPZF7I/events.json","paper":"https://pith.science/paper/FQ65IAOQ"},"agent_actions":{"view_html":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I","download_json":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I.json","view_paper":"https://pith.science/paper/FQ65IAOQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1304.4421&json=true","fetch_graph":"https://pith.science/api/pith-number/FQ65IAOQHDXW4ZDJDMCQZPZF7I/graph.json","fetch_events":"https://pith.science/api/pith-number/FQ65IAOQHDXW4ZDJDMCQZPZF7I/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I/action/storage_attestation","attest_author":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I/action/author_attestation","sign_citation":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I/action/citation_signature","submit_replication":"https://pith.science/pith/FQ65IAOQHDXW4ZDJDMCQZPZF7I/action/replication_record"}},"created_at":"2026-05-18T01:50:32.276365+00:00","updated_at":"2026-05-18T01:50:32.276365+00:00"}