{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:Z6NTHK532FR32MM6FNKHA462H7","short_pith_number":"pith:Z6NTHK53","schema_version":"1.0","canonical_sha256":"cf9b33abbbd163bd319e2b547073da3ff91ed0fc6085807f3eaf30d05d9706dd","source":{"kind":"arxiv","id":"1803.08508","version":1},"attestation_state":"computed","paper":{"title":"Probing black hole accretion in quasar pairs at high redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), (2) INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, (3) INAF - Osservatorio Astronomico di Roma, (4) INAF - Osservatorio Astrofisico di Arcetri, (5) Department of Physics, 6), (6) Max-Planck-Institut fur Astronomie, (7) Dipartimento di Fisica \"G. Occhialini\", (8) Department of Astronomy, 9) ((1) Dipartimento di Fisica e Astronomia, (9) Center for Cosmology, A. Comastri (2), Astro-Particle Physics (CCAPP), Columbus, C. Vignali (1, E. Piconcelli (3), Firenze, Germany, G. Zamorani (2), Heidelberg, Italy, J. Hennawi (5, M. Dotti (7), M. Perna (4), R. Gilli (2), S. Mathur (8, The Ohio State University, Universita` di Bologna, Universita` di Milano-Bicocca, University of California, USA, USA)","submitted_at":"2018-03-22T18:00:02Z","abstract_excerpt":"Models and observations suggest that luminous quasar activity is triggered by mergers, so it should preferentially occur in the most massive primordial dark matter haloes, where the frequency of mergers is expected to be the highest. Since the importance of galaxy mergers increases with redshift, we identify the high-redshift Universe as the ideal laboratory for studying dual AGN. Here we present the X-ray properties of two systems of dual quasars at z=3.0-3.3 selected from the SDSS-DR6 at separations of 6-8 arcsec (43-65kpc) and observed by Chandra for 65ks each. Both members of each pair are"},"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":"1803.08508","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-03-22T18:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"a1ace7778a8385e8dfdefc805c4863bb8a2e358b4ba818bb991f072f31c9e2b6","abstract_canon_sha256":"89b3deed40a2d4553bcfcd2c81a3d37a16a8bd6458c6c12539750209491c906c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:19:20.125182Z","signature_b64":"1iH1Vpfw1sLNEM7xbkLNYaRNrMiYlvTONX4jVvzToeT1TxtEbnuJPnkNSUJcIW16CO/e20xnqugc0fEX4V2wAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cf9b33abbbd163bd319e2b547073da3ff91ed0fc6085807f3eaf30d05d9706dd","last_reissued_at":"2026-05-18T00:19:20.124651Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:19:20.124651Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing black hole accretion in quasar pairs at high redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), (2) INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, (3) INAF - Osservatorio Astronomico di Roma, (4) INAF - Osservatorio Astrofisico di Arcetri, (5) Department of Physics, 6), (6) Max-Planck-Institut fur Astronomie, (7) Dipartimento di Fisica \"G. Occhialini\", (8) Department of Astronomy, 9) ((1) Dipartimento di Fisica e Astronomia, (9) Center for Cosmology, A. Comastri (2), Astro-Particle Physics (CCAPP), Columbus, C. Vignali (1, E. Piconcelli (3), Firenze, Germany, G. Zamorani (2), Heidelberg, Italy, J. Hennawi (5, M. Dotti (7), M. Perna (4), R. Gilli (2), S. Mathur (8, The Ohio State University, Universita` di Bologna, Universita` di Milano-Bicocca, University of California, USA, USA)","submitted_at":"2018-03-22T18:00:02Z","abstract_excerpt":"Models and observations suggest that luminous quasar activity is triggered by mergers, so it should preferentially occur in the most massive primordial dark matter haloes, where the frequency of mergers is expected to be the highest. Since the importance of galaxy mergers increases with redshift, we identify the high-redshift Universe as the ideal laboratory for studying dual AGN. Here we present the X-ray properties of two systems of dual quasars at z=3.0-3.3 selected from the SDSS-DR6 at separations of 6-8 arcsec (43-65kpc) and observed by Chandra for 65ks each. Both members of each pair are"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1803.08508","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":"1803.08508","created_at":"2026-05-18T00:19:20.124733+00:00"},{"alias_kind":"arxiv_version","alias_value":"1803.08508v1","created_at":"2026-05-18T00:19:20.124733+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1803.08508","created_at":"2026-05-18T00:19:20.124733+00:00"},{"alias_kind":"pith_short_12","alias_value":"Z6NTHK532FR3","created_at":"2026-05-18T12:33:04.347982+00:00"},{"alias_kind":"pith_short_16","alias_value":"Z6NTHK532FR32MM6","created_at":"2026-05-18T12:33:04.347982+00:00"},{"alias_kind":"pith_short_8","alias_value":"Z6NTHK53","created_at":"2026-05-18T12:33:04.347982+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/Z6NTHK532FR32MM6FNKHA462H7","json":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7.json","graph_json":"https://pith.science/api/pith-number/Z6NTHK532FR32MM6FNKHA462H7/graph.json","events_json":"https://pith.science/api/pith-number/Z6NTHK532FR32MM6FNKHA462H7/events.json","paper":"https://pith.science/paper/Z6NTHK53"},"agent_actions":{"view_html":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7","download_json":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7.json","view_paper":"https://pith.science/paper/Z6NTHK53","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1803.08508&json=true","fetch_graph":"https://pith.science/api/pith-number/Z6NTHK532FR32MM6FNKHA462H7/graph.json","fetch_events":"https://pith.science/api/pith-number/Z6NTHK532FR32MM6FNKHA462H7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7/action/storage_attestation","attest_author":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7/action/author_attestation","sign_citation":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7/action/citation_signature","submit_replication":"https://pith.science/pith/Z6NTHK532FR32MM6FNKHA462H7/action/replication_record"}},"created_at":"2026-05-18T00:19:20.124733+00:00","updated_at":"2026-05-18T00:19:20.124733+00:00"}