{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:2V5DWODB7K43T63YNWN34IACPC","short_pith_number":"pith:2V5DWODB","schema_version":"1.0","canonical_sha256":"d57a3b3861fab9b9fb786d9bbe200278a31c8dfa7fa6dd08eec8614b5c76effa","source":{"kind":"arxiv","id":"1702.01660","version":1},"attestation_state":"computed","paper":{"title":"The Chandra COSMOS legacy survey: Energy Spectrum of the Cosmic X-ray Background and constraints on undetected populations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"Alexis Finoguenov, Andrea Comastri, Angelo Ricarte, Bhaskar Agarwal, C. Megan Urry, E. Treister, Fabio Pacucci, Francesca Civano, Guenther Hasinger, Marco Ajello, Martin Elvis, Nico Cappelluti, Priyamvada Natarajan, Roberto Gilli, Stefano Marchesi, Tonima Tasnim Ananna, Viola Allevato, Yanxia Li","submitted_at":"2017-02-03T18:59:54Z","abstract_excerpt":"Using {\\em Chandra} observations in the 2.15 deg$^{2}$ COSMOS legacy field, we present one of the most accurate measurements of the Cosmic X-ray Background (CXB) spectrum to date in the [0.3-7] keV energy band. The CXB has three distinct components: contributions from two Galactic collisional thermal plasmas at kT$\\sim$0.27 and 0.07 keV and an extragalactic power-law with photon spectral index $\\Gamma$=1.45$\\pm{0.02}$. The 1 keV normalization of the extragalactic component is 10.91$\\pm{0.16}$ keV cm$^{-2}$ s$^{-1}$ sr$^{-1}$ keV$^{-1}$. Removing all X-ray detected sources, the remaining unreso"},"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":"1702.01660","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2017-02-03T18:59:54Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"8e5b5a510e2a5e5ffa4f879a93740b0934116fa2e110ca34521fe6b178f4387a","abstract_canon_sha256":"63271ad6adb0f181c03a89d54c436ed84852075413b7e692b0c5ed23572cd798"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:49:09.239061Z","signature_b64":"XobkP7Bt/Y6BfljRq+FpdC50lmPcc1mTswS7wP3aiyPAkoqFq02lsVJSrtxGJr2wlw4foXLOk3KUte5mwEJDBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d57a3b3861fab9b9fb786d9bbe200278a31c8dfa7fa6dd08eec8614b5c76effa","last_reissued_at":"2026-05-18T00:49:09.238601Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:49:09.238601Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Chandra COSMOS legacy survey: Energy Spectrum of the Cosmic X-ray Background and constraints on undetected populations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"Alexis Finoguenov, Andrea Comastri, Angelo Ricarte, Bhaskar Agarwal, C. Megan Urry, E. Treister, Fabio Pacucci, Francesca Civano, Guenther Hasinger, Marco Ajello, Martin Elvis, Nico Cappelluti, Priyamvada Natarajan, Roberto Gilli, Stefano Marchesi, Tonima Tasnim Ananna, Viola Allevato, Yanxia Li","submitted_at":"2017-02-03T18:59:54Z","abstract_excerpt":"Using {\\em Chandra} observations in the 2.15 deg$^{2}$ COSMOS legacy field, we present one of the most accurate measurements of the Cosmic X-ray Background (CXB) spectrum to date in the [0.3-7] keV energy band. The CXB has three distinct components: contributions from two Galactic collisional thermal plasmas at kT$\\sim$0.27 and 0.07 keV and an extragalactic power-law with photon spectral index $\\Gamma$=1.45$\\pm{0.02}$. The 1 keV normalization of the extragalactic component is 10.91$\\pm{0.16}$ keV cm$^{-2}$ s$^{-1}$ sr$^{-1}$ keV$^{-1}$. Removing all X-ray detected sources, the remaining unreso"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1702.01660","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":"1702.01660","created_at":"2026-05-18T00:49:09.238665+00:00"},{"alias_kind":"arxiv_version","alias_value":"1702.01660v1","created_at":"2026-05-18T00:49:09.238665+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1702.01660","created_at":"2026-05-18T00:49:09.238665+00:00"},{"alias_kind":"pith_short_12","alias_value":"2V5DWODB7K43","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_16","alias_value":"2V5DWODB7K43T63Y","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_8","alias_value":"2V5DWODB","created_at":"2026-05-18T12:30:55.937587+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.17547","citing_title":"Population synthesis of active galactic nuclei based on the radiation-regulated unification model","ref_index":14,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC","json":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC.json","graph_json":"https://pith.science/api/pith-number/2V5DWODB7K43T63YNWN34IACPC/graph.json","events_json":"https://pith.science/api/pith-number/2V5DWODB7K43T63YNWN34IACPC/events.json","paper":"https://pith.science/paper/2V5DWODB"},"agent_actions":{"view_html":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC","download_json":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC.json","view_paper":"https://pith.science/paper/2V5DWODB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1702.01660&json=true","fetch_graph":"https://pith.science/api/pith-number/2V5DWODB7K43T63YNWN34IACPC/graph.json","fetch_events":"https://pith.science/api/pith-number/2V5DWODB7K43T63YNWN34IACPC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC/action/storage_attestation","attest_author":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC/action/author_attestation","sign_citation":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC/action/citation_signature","submit_replication":"https://pith.science/pith/2V5DWODB7K43T63YNWN34IACPC/action/replication_record"}},"created_at":"2026-05-18T00:49:09.238665+00:00","updated_at":"2026-05-18T00:49:09.238665+00:00"}