{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:7ME2GZOSGIN42LXCLGB4IVRWET","short_pith_number":"pith:7ME2GZOS","schema_version":"1.0","canonical_sha256":"fb09a365d2321bcd2ee25983c4563624f8d7ef8fe352bc2255a901c919ff4207","source":{"kind":"arxiv","id":"1708.01315","version":1},"attestation_state":"computed","paper":{"title":"Observations of the Ultraviolet-Bright Star Y453 in the Globular Cluster M4 (NGC 6121)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) Dr. Karl Remeis-Observatory & ECAP, (3) Instituto de Astrofisica de La Plata, (4) University of Wisconsin-Whitewater), Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg, Marcelo Miguel Miller Bertolami (3), Marilyn Latour (2), Pierre Chayer (1), Robert A. Benjamin (4) ((1) Space Telescope Science Institute, William V. Dixon (1)","submitted_at":"2017-08-03T21:34:31Z","abstract_excerpt":"We present a spectral analysis of the UV-bright star Y453 in M4. Model fits to the star's optical spectrum yield T_eff ~ 56,000 K. Fits to the star's FUV spectrum, obtained with the Cosmic Origins Spectrograph (COS) on board the Hubble Space Telescope, reveal it to be considerably hotter, with T_eff ~ 72,000 K. We adopt T_eff = 72,000 +/- 2000 K and log g = 5.7 +/- 0.2 as our best-fit parameters. Scaling the model spectrum to match the star's optical and near-infrared magnitudes, we derive a mass M_* = 0.53 +/- 0.24 M_sun and luminosity log L/L_sun = 2.84 +/- 0.05, consistent with the values e"},"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":"1708.01315","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-08-03T21:34:31Z","cross_cats_sorted":[],"title_canon_sha256":"fe98e7bb7ec4f2f66329a1c53ffc6b73eae6debadedb348e5bc25a4239d17eb3","abstract_canon_sha256":"ab4ca33ed3a83d9638f521eadb83c261af120414c947da4b7891a9b74d4c70ba"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:36:02.776539Z","signature_b64":"gvzXY4JSiPW2gFSkre2WxQysWH2pUOUZvlMjXKnhyxag4HkqczQvCE5ZITiG0gip0qcOfM/jWPNRXBXir+gjDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fb09a365d2321bcd2ee25983c4563624f8d7ef8fe352bc2255a901c919ff4207","last_reissued_at":"2026-05-18T00:36:02.776109Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:36:02.776109Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observations of the Ultraviolet-Bright Star Y453 in the Globular Cluster M4 (NGC 6121)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) Dr. Karl Remeis-Observatory & ECAP, (3) Instituto de Astrofisica de La Plata, (4) University of Wisconsin-Whitewater), Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg, Marcelo Miguel Miller Bertolami (3), Marilyn Latour (2), Pierre Chayer (1), Robert A. Benjamin (4) ((1) Space Telescope Science Institute, William V. Dixon (1)","submitted_at":"2017-08-03T21:34:31Z","abstract_excerpt":"We present a spectral analysis of the UV-bright star Y453 in M4. Model fits to the star's optical spectrum yield T_eff ~ 56,000 K. Fits to the star's FUV spectrum, obtained with the Cosmic Origins Spectrograph (COS) on board the Hubble Space Telescope, reveal it to be considerably hotter, with T_eff ~ 72,000 K. We adopt T_eff = 72,000 +/- 2000 K and log g = 5.7 +/- 0.2 as our best-fit parameters. Scaling the model spectrum to match the star's optical and near-infrared magnitudes, we derive a mass M_* = 0.53 +/- 0.24 M_sun and luminosity log L/L_sun = 2.84 +/- 0.05, consistent with the values e"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1708.01315","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":"1708.01315","created_at":"2026-05-18T00:36:02.776176+00:00"},{"alias_kind":"arxiv_version","alias_value":"1708.01315v1","created_at":"2026-05-18T00:36:02.776176+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1708.01315","created_at":"2026-05-18T00:36:02.776176+00:00"},{"alias_kind":"pith_short_12","alias_value":"7ME2GZOSGIN4","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_16","alias_value":"7ME2GZOSGIN42LXC","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_8","alias_value":"7ME2GZOS","created_at":"2026-05-18T12:31:05.417338+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/7ME2GZOSGIN42LXCLGB4IVRWET","json":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET.json","graph_json":"https://pith.science/api/pith-number/7ME2GZOSGIN42LXCLGB4IVRWET/graph.json","events_json":"https://pith.science/api/pith-number/7ME2GZOSGIN42LXCLGB4IVRWET/events.json","paper":"https://pith.science/paper/7ME2GZOS"},"agent_actions":{"view_html":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET","download_json":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET.json","view_paper":"https://pith.science/paper/7ME2GZOS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1708.01315&json=true","fetch_graph":"https://pith.science/api/pith-number/7ME2GZOSGIN42LXCLGB4IVRWET/graph.json","fetch_events":"https://pith.science/api/pith-number/7ME2GZOSGIN42LXCLGB4IVRWET/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET/action/storage_attestation","attest_author":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET/action/author_attestation","sign_citation":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET/action/citation_signature","submit_replication":"https://pith.science/pith/7ME2GZOSGIN42LXCLGB4IVRWET/action/replication_record"}},"created_at":"2026-05-18T00:36:02.776176+00:00","updated_at":"2026-05-18T00:36:02.776176+00:00"}