{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:F64SLZIZVCKHFMLBWT6UIZV2K2","short_pith_number":"pith:F64SLZIZ","schema_version":"1.0","canonical_sha256":"2fb925e519a89472b161b4fd4466ba56952d15da838e33522124976a36136538","source":{"kind":"arxiv","id":"1505.00400","version":2},"attestation_state":"computed","paper":{"title":"Measuring Infrared Surface Brightness Fluctuation Distances with HST WFC3: Calibration and Advice","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"(2) NRC Herzberg Astrophysics, (3) The University of Texas Rio Grande Valley, (4) INAF-Osservatorio Astronomico di Teramo, (5) Brigham Young University, (6) Yonsei University), Gabriella Raimondo (4), Hyejeon Cho (6) ((1) Utah Valley University, Hyun-chul Lee (3), John P. Blakeslee (2), Joseph B. Jensen (1), Michele Cantiello (4), Nathan Boyer (5), Zachary Gibson (1)","submitted_at":"2015-05-03T07:12:31Z","abstract_excerpt":"We present new calibrations of the near-infrared surface brightness fluctuation (SBF) distance method for the F110W (J) and F160W (H) bandpasses of the Wide Field Camera 3 Infrared Channel (WFC3/IR) on the Hubble Space Telescope. The calibrations are based on data for 16 early-type galaxies in the Virgo and Fornax clusters observed with WFC3/IR and are provided as functions of both the optical (g-z) and near-infrared (J-H) colors. The scatter about the linear calibration relations for the luminous red galaxies in the sample is approximately 0.10 mag, corresponding to a statistical error of 5% "},"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":"1505.00400","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2015-05-03T07:12:31Z","cross_cats_sorted":[],"title_canon_sha256":"5b27e39ac34cbf7d187ecba70094d5ecb1d3106d409f8f82afc980dc73b3dfc1","abstract_canon_sha256":"285aa66c9f879c4f279ea9b836a6ea39147da0bd4f0278d7896f27677f2aa94f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:33:43.389147Z","signature_b64":"BoQS9zZJomPCwMzX0psdlrZzuXfFNl9L/NIGrJKKKZ1HyWq9CSV/MdIQv8wUhjvJVAic2htJgL9kIYFjbb7JAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2fb925e519a89472b161b4fd4466ba56952d15da838e33522124976a36136538","last_reissued_at":"2026-05-18T01:33:43.388507Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:33:43.388507Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measuring Infrared Surface Brightness Fluctuation Distances with HST WFC3: Calibration and Advice","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"(2) NRC Herzberg Astrophysics, (3) The University of Texas Rio Grande Valley, (4) INAF-Osservatorio Astronomico di Teramo, (5) Brigham Young University, (6) Yonsei University), Gabriella Raimondo (4), Hyejeon Cho (6) ((1) Utah Valley University, Hyun-chul Lee (3), John P. Blakeslee (2), Joseph B. Jensen (1), Michele Cantiello (4), Nathan Boyer (5), Zachary Gibson (1)","submitted_at":"2015-05-03T07:12:31Z","abstract_excerpt":"We present new calibrations of the near-infrared surface brightness fluctuation (SBF) distance method for the F110W (J) and F160W (H) bandpasses of the Wide Field Camera 3 Infrared Channel (WFC3/IR) on the Hubble Space Telescope. The calibrations are based on data for 16 early-type galaxies in the Virgo and Fornax clusters observed with WFC3/IR and are provided as functions of both the optical (g-z) and near-infrared (J-H) colors. The scatter about the linear calibration relations for the luminous red galaxies in the sample is approximately 0.10 mag, corresponding to a statistical error of 5% "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1505.00400","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":"1505.00400","created_at":"2026-05-18T01:33:43.388601+00:00"},{"alias_kind":"arxiv_version","alias_value":"1505.00400v2","created_at":"2026-05-18T01:33:43.388601+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1505.00400","created_at":"2026-05-18T01:33:43.388601+00:00"},{"alias_kind":"pith_short_12","alias_value":"F64SLZIZVCKH","created_at":"2026-05-18T12:29:19.899920+00:00"},{"alias_kind":"pith_short_16","alias_value":"F64SLZIZVCKHFMLB","created_at":"2026-05-18T12:29:19.899920+00:00"},{"alias_kind":"pith_short_8","alias_value":"F64SLZIZ","created_at":"2026-05-18T12:29:19.899920+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/F64SLZIZVCKHFMLBWT6UIZV2K2","json":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2.json","graph_json":"https://pith.science/api/pith-number/F64SLZIZVCKHFMLBWT6UIZV2K2/graph.json","events_json":"https://pith.science/api/pith-number/F64SLZIZVCKHFMLBWT6UIZV2K2/events.json","paper":"https://pith.science/paper/F64SLZIZ"},"agent_actions":{"view_html":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2","download_json":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2.json","view_paper":"https://pith.science/paper/F64SLZIZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1505.00400&json=true","fetch_graph":"https://pith.science/api/pith-number/F64SLZIZVCKHFMLBWT6UIZV2K2/graph.json","fetch_events":"https://pith.science/api/pith-number/F64SLZIZVCKHFMLBWT6UIZV2K2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2/action/storage_attestation","attest_author":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2/action/author_attestation","sign_citation":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2/action/citation_signature","submit_replication":"https://pith.science/pith/F64SLZIZVCKHFMLBWT6UIZV2K2/action/replication_record"}},"created_at":"2026-05-18T01:33:43.388601+00:00","updated_at":"2026-05-18T01:33:43.388601+00:00"}