{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1996:MO7Z3GNGC46JJR63PIUIV46D7B","short_pith_number":"pith:MO7Z3GNG","schema_version":"1.0","canonical_sha256":"63bf9d99a6173c94c7db7a288af3c3f8754a66b002dddec9c7aa3d1c9181b882","source":{"kind":"arxiv","id":"astro-ph/9608184","version":1},"attestation_state":"computed","paper":{"title":"ROSAT observation of GRS 1739-278","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"J. Greiner, K. Dennerl, P. Predehl","submitted_at":"1996-08-28T14:41:09Z","abstract_excerpt":"We have observed GRS 1739-278 with the ROSAT HRI on March 31, 1996. The improved X-ray position proves the identification with an earlier discovered variable radio source. We derive an extinction of A_V = 14+/-2 from the dust scattering halo, which implies a distance of d approx. 6-8.5 kpc. Thus, GRS 1739-278 radiates at least near the Eddington limit for a 1 M_sun compact object. The existence of the dust scattering halo necessitates a prolonged X-ray activity period prior to the ROSAT observation. Combined with the non-detection by Granat during an earlier galactic center observation, we spe"},"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":"astro-ph/9608184","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1996-08-28T14:41:09Z","cross_cats_sorted":[],"title_canon_sha256":"c389844b20c1a0be43b20081248b50bdf7c80312526d00711ecafdb0f9215125","abstract_canon_sha256":"db4c40f61dd8068625178acacf9d308b2e73b2ebce919a8994c82314509583ae"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:14:53.751322Z","signature_b64":"/bXqLHnlAGlwpTluMjssbCtDaxwZMv8DNJTNzF3S+Lx8dTcYjZdqyAk58j8YMUFFF68/MSU0qe6jiHC3PK+3CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"63bf9d99a6173c94c7db7a288af3c3f8754a66b002dddec9c7aa3d1c9181b882","last_reissued_at":"2026-07-04T14:14:53.750908Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:14:53.750908Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"ROSAT observation of GRS 1739-278","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"J. Greiner, K. Dennerl, P. Predehl","submitted_at":"1996-08-28T14:41:09Z","abstract_excerpt":"We have observed GRS 1739-278 with the ROSAT HRI on March 31, 1996. The improved X-ray position proves the identification with an earlier discovered variable radio source. We derive an extinction of A_V = 14+/-2 from the dust scattering halo, which implies a distance of d approx. 6-8.5 kpc. Thus, GRS 1739-278 radiates at least near the Eddington limit for a 1 M_sun compact object. The existence of the dust scattering halo necessitates a prolonged X-ray activity period prior to the ROSAT observation. Combined with the non-detection by Granat during an earlier galactic center observation, we spe"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9608184","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/astro-ph/9608184/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":"astro-ph/9608184","created_at":"2026-07-04T14:14:53.750973+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9608184v1","created_at":"2026-07-04T14:14:53.750973+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9608184","created_at":"2026-07-04T14:14:53.750973+00:00"},{"alias_kind":"pith_short_12","alias_value":"MO7Z3GNGC46J","created_at":"2026-07-04T14:14:53.750973+00:00"},{"alias_kind":"pith_short_16","alias_value":"MO7Z3GNGC46JJR63","created_at":"2026-07-04T14:14:53.750973+00:00"},{"alias_kind":"pith_short_8","alias_value":"MO7Z3GNG","created_at":"2026-07-04T14:14:53.750973+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.12121","citing_title":"The population of NuSTAR Black Hole X-ray Binaries","ref_index":36,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B","json":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B.json","graph_json":"https://pith.science/api/pith-number/MO7Z3GNGC46JJR63PIUIV46D7B/graph.json","events_json":"https://pith.science/api/pith-number/MO7Z3GNGC46JJR63PIUIV46D7B/events.json","paper":"https://pith.science/paper/MO7Z3GNG"},"agent_actions":{"view_html":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B","download_json":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B.json","view_paper":"https://pith.science/paper/MO7Z3GNG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9608184&json=true","fetch_graph":"https://pith.science/api/pith-number/MO7Z3GNGC46JJR63PIUIV46D7B/graph.json","fetch_events":"https://pith.science/api/pith-number/MO7Z3GNGC46JJR63PIUIV46D7B/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B/action/storage_attestation","attest_author":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B/action/author_attestation","sign_citation":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B/action/citation_signature","submit_replication":"https://pith.science/pith/MO7Z3GNGC46JJR63PIUIV46D7B/action/replication_record"}},"created_at":"2026-07-04T14:14:53.750973+00:00","updated_at":"2026-07-04T14:14:53.750973+00:00"}