{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:C4DTOCLXROJ4JPVSFOH4XXOYA2","short_pith_number":"pith:C4DTOCLX","schema_version":"1.0","canonical_sha256":"17073709778b93c4beb22b8fcbddd806b777c6c1e687c56a5cceaf769f5e1b7c","source":{"kind":"arxiv","id":"1801.04667","version":2},"attestation_state":"computed","paper":{"title":"X-ray Detectability of Accreting Isolated Black Holes in Our Galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Daichi Tsuna, Norita Kawanaka, Tomonori Totani","submitted_at":"2018-01-15T05:20:10Z","abstract_excerpt":"Detectability of isolated black holes (IBHs) without a companion star but emitting X-rays by accretion from dense interstellar medium (ISM) or molecular cloud gas is investigated. We calculate orbits of IBHs in the Galaxy to derive a realistic spatial distribution of IBHs, for various mean values of kick velocity at their birth $\\upsilon_{\\rm avg}$. X-ray luminosities of these IBHs are then calculated considering various phases of ISM and molecular clouds, for a wide range of the accretion efficiency $\\lambda$ (a ratio of the actual accretion rate to the Bondi rate) that is rather uncertain. I"},"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":"1801.04667","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-01-15T05:20:10Z","cross_cats_sorted":[],"title_canon_sha256":"ab7fafcb8a459861b1c9528afa9ea2f470dd2e8aaf40aa9f9919d96ddad3690b","abstract_canon_sha256":"b5ca71a69d42d5e79e2d1cf49d8ea7aa609d631a0afe95cb7affc6a17c423f07"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:20:02.620573Z","signature_b64":"PSlFEfYV7tJGas5QQsSYjPwq62oXsvnbrjRabVFlLYXH9NZDiPROXMYRvJGC12eU0dAYfC9FpiBHqffDQ3wwCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"17073709778b93c4beb22b8fcbddd806b777c6c1e687c56a5cceaf769f5e1b7c","last_reissued_at":"2026-05-18T00:20:02.619916Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:20:02.619916Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"X-ray Detectability of Accreting Isolated Black Holes in Our Galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Daichi Tsuna, Norita Kawanaka, Tomonori Totani","submitted_at":"2018-01-15T05:20:10Z","abstract_excerpt":"Detectability of isolated black holes (IBHs) without a companion star but emitting X-rays by accretion from dense interstellar medium (ISM) or molecular cloud gas is investigated. We calculate orbits of IBHs in the Galaxy to derive a realistic spatial distribution of IBHs, for various mean values of kick velocity at their birth $\\upsilon_{\\rm avg}$. X-ray luminosities of these IBHs are then calculated considering various phases of ISM and molecular clouds, for a wide range of the accretion efficiency $\\lambda$ (a ratio of the actual accretion rate to the Bondi rate) that is rather uncertain. I"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1801.04667","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":"1801.04667","created_at":"2026-05-18T00:20:02.620011+00:00"},{"alias_kind":"arxiv_version","alias_value":"1801.04667v2","created_at":"2026-05-18T00:20:02.620011+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1801.04667","created_at":"2026-05-18T00:20:02.620011+00:00"},{"alias_kind":"pith_short_12","alias_value":"C4DTOCLXROJ4","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_16","alias_value":"C4DTOCLXROJ4JPVS","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_8","alias_value":"C4DTOCLX","created_at":"2026-05-18T12:32:16.446611+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07068","citing_title":"Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors","ref_index":7,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2","json":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2.json","graph_json":"https://pith.science/api/pith-number/C4DTOCLXROJ4JPVSFOH4XXOYA2/graph.json","events_json":"https://pith.science/api/pith-number/C4DTOCLXROJ4JPVSFOH4XXOYA2/events.json","paper":"https://pith.science/paper/C4DTOCLX"},"agent_actions":{"view_html":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2","download_json":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2.json","view_paper":"https://pith.science/paper/C4DTOCLX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1801.04667&json=true","fetch_graph":"https://pith.science/api/pith-number/C4DTOCLXROJ4JPVSFOH4XXOYA2/graph.json","fetch_events":"https://pith.science/api/pith-number/C4DTOCLXROJ4JPVSFOH4XXOYA2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2/action/storage_attestation","attest_author":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2/action/author_attestation","sign_citation":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2/action/citation_signature","submit_replication":"https://pith.science/pith/C4DTOCLXROJ4JPVSFOH4XXOYA2/action/replication_record"}},"created_at":"2026-05-18T00:20:02.620011+00:00","updated_at":"2026-05-18T00:20:02.620011+00:00"}