{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:ZK647KPCR5JOOBDSAIYKBMFHYK","short_pith_number":"pith:ZK647KPC","schema_version":"1.0","canonical_sha256":"cabdcfa9e28f52e704720230a0b0a7c295f7869841a12379bfc74f93c87a04a5","source":{"kind":"arxiv","id":"2204.10346","version":1},"attestation_state":"computed","paper":{"title":"Constraining Energy-dependent emissivity profiles of AGN inflows","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"D. I. Ashton, M. J. Middleton","submitted_at":"2022-04-21T18:05:07Z","abstract_excerpt":"The emissivity of the accretion flow is a key parameter affecting the shape of both the energy and variability power spectrum of AGN. We explore the energy-dependence of the power spectrum for five AGN, across the XMM-Newton bandpass, and across the 0.01-1 mHz frequency range, finding a ubiquitous flattening of the power spectrum towards higher energies. We develop a framework to explore this behaviour and thereby extract the energy dependence of the emissivity assuming a simple disc-like geometry for the inflow. We find that the emissivity ranges from R^-2 at energies around the soft excess a"},"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":"2204.10346","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-04-21T18:05:07Z","cross_cats_sorted":[],"title_canon_sha256":"9392be185f98fcc3e1ca5c978eb05c2c80db0b46645f54c74e06f9c8de70d657","abstract_canon_sha256":"20170496994797d530d3c7ce22adae7e68eb604d8544d8cf751f239107ae372b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:19:59.216830Z","signature_b64":"0gBjH3/4HXMGOriGSePo9nILvg9WW1nbJPDvxtd2oyhArVLrTPv0m8nWql2yf2AHhs/VcgR6GPAVIfCkJH9xAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cabdcfa9e28f52e704720230a0b0a7c295f7869841a12379bfc74f93c87a04a5","last_reissued_at":"2026-07-05T04:19:59.216434Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:19:59.216434Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining Energy-dependent emissivity profiles of AGN inflows","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"D. I. Ashton, M. J. Middleton","submitted_at":"2022-04-21T18:05:07Z","abstract_excerpt":"The emissivity of the accretion flow is a key parameter affecting the shape of both the energy and variability power spectrum of AGN. We explore the energy-dependence of the power spectrum for five AGN, across the XMM-Newton bandpass, and across the 0.01-1 mHz frequency range, finding a ubiquitous flattening of the power spectrum towards higher energies. We develop a framework to explore this behaviour and thereby extract the energy dependence of the emissivity assuming a simple disc-like geometry for the inflow. We find that the emissivity ranges from R^-2 at energies around the soft excess a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.10346","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/2204.10346/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":"2204.10346","created_at":"2026-07-05T04:19:59.216492+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.10346v1","created_at":"2026-07-05T04:19:59.216492+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.10346","created_at":"2026-07-05T04:19:59.216492+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZK647KPCR5JO","created_at":"2026-07-05T04:19:59.216492+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZK647KPCR5JOOBDS","created_at":"2026-07-05T04:19:59.216492+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZK647KPC","created_at":"2026-07-05T04:19:59.216492+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03291","citing_title":"Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference","ref_index":48,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK","json":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK.json","graph_json":"https://pith.science/api/pith-number/ZK647KPCR5JOOBDSAIYKBMFHYK/graph.json","events_json":"https://pith.science/api/pith-number/ZK647KPCR5JOOBDSAIYKBMFHYK/events.json","paper":"https://pith.science/paper/ZK647KPC"},"agent_actions":{"view_html":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK","download_json":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK.json","view_paper":"https://pith.science/paper/ZK647KPC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.10346&json=true","fetch_graph":"https://pith.science/api/pith-number/ZK647KPCR5JOOBDSAIYKBMFHYK/graph.json","fetch_events":"https://pith.science/api/pith-number/ZK647KPCR5JOOBDSAIYKBMFHYK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK/action/storage_attestation","attest_author":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK/action/author_attestation","sign_citation":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK/action/citation_signature","submit_replication":"https://pith.science/pith/ZK647KPCR5JOOBDSAIYKBMFHYK/action/replication_record"}},"created_at":"2026-07-05T04:19:59.216492+00:00","updated_at":"2026-07-05T04:19:59.216492+00:00"}