{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:HQ2HVZTWMBBQDIWLLT2QZD65F6","short_pith_number":"pith:HQ2HVZTW","schema_version":"1.0","canonical_sha256":"3c347ae676604301a2cb5cf50c8fdd2fa548b48dbb9e53a9c71b42025c9e5fbc","source":{"kind":"arxiv","id":"0812.2346","version":1},"attestation_state":"computed","paper":{"title":"Optical SBFs of shell galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Brocato, G. Raimondo, I. Biscardi, M. Cantiello","submitted_at":"2008-12-12T10:59:56Z","abstract_excerpt":"We measure F814W Surface Brightness Fluctuations (SBFs) for a sample of distant shell galaxies observed with the Advanced Camera for Survey (ACS) on board of HST. To evaluate the distance at galaxies, theoretical SBF magnitudes for the ACS@HST filters are computed for single burst stellar populations covering a wide range of ages (t=1.5-14 Gyr) and metallicities (Z=0.008-0.04). Using these stellar population models we provide the first M_SBF,F814W versus (F475W-F814W)0 calibration. The results suggest that optical SBFs can be measured at d>100 Mpc using high resolution spatial optical data."},"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":"0812.2346","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-12-12T10:59:56Z","cross_cats_sorted":[],"title_canon_sha256":"06dd28e65a8123637bf6e4579db417927d547a2ec3d1417d205b804cef310e20","abstract_canon_sha256":"dc50d03988c2410235aae40cb32e492a86297f04c4dd6caa3c43f537252a30db"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:33:42.847413Z","signature_b64":"tHX7zgzAoukj1SIVmhScMI8ILztKjlnSfEE4tUii6bbyBg2uoSt6PvOmLt0QNk8bubm0XGDcOcPen/rlDkfIBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3c347ae676604301a2cb5cf50c8fdd2fa548b48dbb9e53a9c71b42025c9e5fbc","last_reissued_at":"2026-07-04T15:33:42.847074Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:33:42.847074Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Optical SBFs of shell galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Brocato, G. Raimondo, I. Biscardi, M. Cantiello","submitted_at":"2008-12-12T10:59:56Z","abstract_excerpt":"We measure F814W Surface Brightness Fluctuations (SBFs) for a sample of distant shell galaxies observed with the Advanced Camera for Survey (ACS) on board of HST. To evaluate the distance at galaxies, theoretical SBF magnitudes for the ACS@HST filters are computed for single burst stellar populations covering a wide range of ages (t=1.5-14 Gyr) and metallicities (Z=0.008-0.04). Using these stellar population models we provide the first M_SBF,F814W versus (F475W-F814W)0 calibration. The results suggest that optical SBFs can be measured at d>100 Mpc using high resolution spatial optical data."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0812.2346","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0812.2346/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":"0812.2346","created_at":"2026-07-04T15:33:42.847132+00:00"},{"alias_kind":"arxiv_version","alias_value":"0812.2346v1","created_at":"2026-07-04T15:33:42.847132+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0812.2346","created_at":"2026-07-04T15:33:42.847132+00:00"},{"alias_kind":"pith_short_12","alias_value":"HQ2HVZTWMBBQ","created_at":"2026-07-04T15:33:42.847132+00:00"},{"alias_kind":"pith_short_16","alias_value":"HQ2HVZTWMBBQDIWL","created_at":"2026-07-04T15:33:42.847132+00:00"},{"alias_kind":"pith_short_8","alias_value":"HQ2HVZTW","created_at":"2026-07-04T15:33:42.847132+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.28725","citing_title":"A Simulation Based Inference Approach to Modelling of Type Ia Supernova Populations","ref_index":63,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6","json":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6.json","graph_json":"https://pith.science/api/pith-number/HQ2HVZTWMBBQDIWLLT2QZD65F6/graph.json","events_json":"https://pith.science/api/pith-number/HQ2HVZTWMBBQDIWLLT2QZD65F6/events.json","paper":"https://pith.science/paper/HQ2HVZTW"},"agent_actions":{"view_html":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6","download_json":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6.json","view_paper":"https://pith.science/paper/HQ2HVZTW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0812.2346&json=true","fetch_graph":"https://pith.science/api/pith-number/HQ2HVZTWMBBQDIWLLT2QZD65F6/graph.json","fetch_events":"https://pith.science/api/pith-number/HQ2HVZTWMBBQDIWLLT2QZD65F6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6/action/storage_attestation","attest_author":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6/action/author_attestation","sign_citation":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6/action/citation_signature","submit_replication":"https://pith.science/pith/HQ2HVZTWMBBQDIWLLT2QZD65F6/action/replication_record"}},"created_at":"2026-07-04T15:33:42.847132+00:00","updated_at":"2026-07-04T15:33:42.847132+00:00"}