{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:SKEARG5UFGNNVVXYUWSNBX76X7","short_pith_number":"pith:SKEARG5U","schema_version":"1.0","canonical_sha256":"9288089bb4299adad6f8a5a4d0dffebffaf03c10d0899fdadde98741cd3f573d","source":{"kind":"arxiv","id":"1903.05795","version":1},"attestation_state":"computed","paper":{"title":"The XMM-Newton/HST view of the obscuring outflow in the Seyfert Galaxy Mrk 335 observed at extremely low X-ray flux","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Anil Pradhan (Ohio State University), Anna Lia Longinotti (CONACyT-INAOE), Bonn), Dan Wilkins (KIPAC, Dirk Grupe (Morehead State University), Gerard Kriss (STScI), Karla Arellano-Cordova (IAC), Luigi Gallo (Saint Mary's University), Michael Parker (ESAC), Smita Mathur (Ohio State University), Stanford University), Stefanie Komossa (Max Planck, Yair Krongold (UNAM)","submitted_at":"2019-03-14T02:49:55Z","abstract_excerpt":"The Seyfert Galaxy Mrk 335 is known for its frequent changes of flux and spectral shape in the X-ray band occurred during recent years. These variations may be explained by the onset of a wind that previous, non-contemporaneous high-resolution spectroscopy in X-ray and UV bands located at accretion disc scale. A simultaneous new campaign by XMM-Newton and HST caught the source at an historical low flux in the X-ray band. The soft X-ray spectrum is dominated by prominent emission features, and by the effect of a strong ionized absorber with an outflow velocity of 5-6X10$^3$~km~s$^{-1}$. The bro"},"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":"1903.05795","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-03-14T02:49:55Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"2d6954cea71496878649f65fa2318b5b2e0605805f911b9920a842dc61740cef","abstract_canon_sha256":"3ce35e1a4de035858e995e6c71dc036b6137bc9d74d9aa67077a9ed4b9cf6ca0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:47:25.350602Z","signature_b64":"3pqhnWAM4uYEu+qTymSgeIHrANNbQHLwhIlXhxqnq8Ym5d9D2dc0CEWwh2aYPTJh1V+RpeYEoCo6ySBUtlR0BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9288089bb4299adad6f8a5a4d0dffebffaf03c10d0899fdadde98741cd3f573d","last_reissued_at":"2026-05-17T23:47:25.349991Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:47:25.349991Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The XMM-Newton/HST view of the obscuring outflow in the Seyfert Galaxy Mrk 335 observed at extremely low X-ray flux","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Anil Pradhan (Ohio State University), Anna Lia Longinotti (CONACyT-INAOE), Bonn), Dan Wilkins (KIPAC, Dirk Grupe (Morehead State University), Gerard Kriss (STScI), Karla Arellano-Cordova (IAC), Luigi Gallo (Saint Mary's University), Michael Parker (ESAC), Smita Mathur (Ohio State University), Stanford University), Stefanie Komossa (Max Planck, Yair Krongold (UNAM)","submitted_at":"2019-03-14T02:49:55Z","abstract_excerpt":"The Seyfert Galaxy Mrk 335 is known for its frequent changes of flux and spectral shape in the X-ray band occurred during recent years. These variations may be explained by the onset of a wind that previous, non-contemporaneous high-resolution spectroscopy in X-ray and UV bands located at accretion disc scale. A simultaneous new campaign by XMM-Newton and HST caught the source at an historical low flux in the X-ray band. The soft X-ray spectrum is dominated by prominent emission features, and by the effect of a strong ionized absorber with an outflow velocity of 5-6X10$^3$~km~s$^{-1}$. The bro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1903.05795","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":"1903.05795","created_at":"2026-05-17T23:47:25.350095+00:00"},{"alias_kind":"arxiv_version","alias_value":"1903.05795v1","created_at":"2026-05-17T23:47:25.350095+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1903.05795","created_at":"2026-05-17T23:47:25.350095+00:00"},{"alias_kind":"pith_short_12","alias_value":"SKEARG5UFGNN","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_16","alias_value":"SKEARG5UFGNNVVXY","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_8","alias_value":"SKEARG5U","created_at":"2026-05-18T12:33:27.125529+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/SKEARG5UFGNNVVXYUWSNBX76X7","json":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7.json","graph_json":"https://pith.science/api/pith-number/SKEARG5UFGNNVVXYUWSNBX76X7/graph.json","events_json":"https://pith.science/api/pith-number/SKEARG5UFGNNVVXYUWSNBX76X7/events.json","paper":"https://pith.science/paper/SKEARG5U"},"agent_actions":{"view_html":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7","download_json":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7.json","view_paper":"https://pith.science/paper/SKEARG5U","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1903.05795&json=true","fetch_graph":"https://pith.science/api/pith-number/SKEARG5UFGNNVVXYUWSNBX76X7/graph.json","fetch_events":"https://pith.science/api/pith-number/SKEARG5UFGNNVVXYUWSNBX76X7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7/action/storage_attestation","attest_author":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7/action/author_attestation","sign_citation":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7/action/citation_signature","submit_replication":"https://pith.science/pith/SKEARG5UFGNNVVXYUWSNBX76X7/action/replication_record"}},"created_at":"2026-05-17T23:47:25.350095+00:00","updated_at":"2026-05-17T23:47:25.350095+00:00"}