{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:TZVFZZBV7QDOIBOAANY6RU5KTK","short_pith_number":"pith:TZVFZZBV","schema_version":"1.0","canonical_sha256":"9e6a5ce435fc06e405c00371e8d3aa9aa94361c6674a2c9dfab27caa91290323","source":{"kind":"arxiv","id":"1305.3917","version":1},"attestation_state":"computed","paper":{"title":"A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"A. Bongiorno, A. Comastri, A. Del Moro, A. Doi, C. Steinhardt, D. B. Sanders, D. M. Alexander, D. Masters, E. Lusso, E. S. Laird, E. Treister, F. Civano, G. Hasinger, G. Lanzuisi, G. Zamorani, J. D. Silverman, J. Kartaltepe, K. Matsuoka, K. Nandra, K. Ohta, K. Schawinski, L. C. Ho, M. Akiyama, M. Brightman, M. Brusa, M. Elvis, M. Mignoli, M. Salvato, M. Schramm, O. Shemmer, P. Capak, T. Nagao, V. Mainieri, W. N. Brandt, Y. Taniguchi, Y. Ueda","submitted_at":"2013-05-16T20:00:03Z","abstract_excerpt":"We present an investigation into how well the properties of the accretion flow onto a supermassive black hole may be coupled to those of the overlying hot corona. To do so, we specifically measure the characteristic spectral index, Gamma, of a power-law energy distribution, over an energy range of 2 to 10 keV, for X-ray selected, broad-lined radio-quiet AGN up to z~2 in COSMOS and E-CDF-S. We test the previously reported dependence between Gamma and black hole mass, FWHM and Eddington ratio using a sample of AGN covering a broad range in these parameters based on both the Mg ii and H-alpha emi"},"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":"1305.3917","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-05-16T20:00:03Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"686f65ce3398d914562cb3c1a014426c88f437e96e650b1f6c6afaf355346b70","abstract_canon_sha256":"b0074b1bf937fa7b7169b6af3dc12072d31822221ecfa9d08cb8ce99761b35f6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:49:49.555333Z","signature_b64":"PkKUOzPaQJshNdYoSjW1YN+86S2Glx8MytHqxK/b3DkdaW1U/S6h/171rzsCpuWkWfUiq/WaepxOuPmiS/qyDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9e6a5ce435fc06e405c00371e8d3aa9aa94361c6674a2c9dfab27caa91290323","last_reissued_at":"2026-05-18T01:49:49.554823Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:49:49.554823Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"A. Bongiorno, A. Comastri, A. Del Moro, A. Doi, C. Steinhardt, D. B. Sanders, D. M. Alexander, D. Masters, E. Lusso, E. S. Laird, E. Treister, F. Civano, G. Hasinger, G. Lanzuisi, G. Zamorani, J. D. Silverman, J. Kartaltepe, K. Matsuoka, K. Nandra, K. Ohta, K. Schawinski, L. C. Ho, M. Akiyama, M. Brightman, M. Brusa, M. Elvis, M. Mignoli, M. Salvato, M. Schramm, O. Shemmer, P. Capak, T. Nagao, V. Mainieri, W. N. Brandt, Y. Taniguchi, Y. Ueda","submitted_at":"2013-05-16T20:00:03Z","abstract_excerpt":"We present an investigation into how well the properties of the accretion flow onto a supermassive black hole may be coupled to those of the overlying hot corona. To do so, we specifically measure the characteristic spectral index, Gamma, of a power-law energy distribution, over an energy range of 2 to 10 keV, for X-ray selected, broad-lined radio-quiet AGN up to z~2 in COSMOS and E-CDF-S. We test the previously reported dependence between Gamma and black hole mass, FWHM and Eddington ratio using a sample of AGN covering a broad range in these parameters based on both the Mg ii and H-alpha emi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1305.3917","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":"1305.3917","created_at":"2026-05-18T01:49:49.554897+00:00"},{"alias_kind":"arxiv_version","alias_value":"1305.3917v1","created_at":"2026-05-18T01:49:49.554897+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1305.3917","created_at":"2026-05-18T01:49:49.554897+00:00"},{"alias_kind":"pith_short_12","alias_value":"TZVFZZBV7QDO","created_at":"2026-05-18T12:28:02.375192+00:00"},{"alias_kind":"pith_short_16","alias_value":"TZVFZZBV7QDOIBOA","created_at":"2026-05-18T12:28:02.375192+00:00"},{"alias_kind":"pith_short_8","alias_value":"TZVFZZBV","created_at":"2026-05-18T12:28:02.375192+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.05246","citing_title":"The emergence of X-ray emission lines during relativistic radio-jet formation in the changing-look active galactic nucleus 1ES 1927+654","ref_index":149,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK","json":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK.json","graph_json":"https://pith.science/api/pith-number/TZVFZZBV7QDOIBOAANY6RU5KTK/graph.json","events_json":"https://pith.science/api/pith-number/TZVFZZBV7QDOIBOAANY6RU5KTK/events.json","paper":"https://pith.science/paper/TZVFZZBV"},"agent_actions":{"view_html":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK","download_json":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK.json","view_paper":"https://pith.science/paper/TZVFZZBV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1305.3917&json=true","fetch_graph":"https://pith.science/api/pith-number/TZVFZZBV7QDOIBOAANY6RU5KTK/graph.json","fetch_events":"https://pith.science/api/pith-number/TZVFZZBV7QDOIBOAANY6RU5KTK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK/action/storage_attestation","attest_author":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK/action/author_attestation","sign_citation":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK/action/citation_signature","submit_replication":"https://pith.science/pith/TZVFZZBV7QDOIBOAANY6RU5KTK/action/replication_record"}},"created_at":"2026-05-18T01:49:49.554897+00:00","updated_at":"2026-05-18T01:49:49.554897+00:00"}