{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:MMKMCBRVJSQHUXJZL7WQM2OQQX","short_pith_number":"pith:MMKMCBRV","schema_version":"1.0","canonical_sha256":"6314c106354ca07a5d395fed0669d085df9ef5716a2ceed7e606dabe9a2ec4c3","source":{"kind":"arxiv","id":"astro-ph/0509290","version":1},"attestation_state":"computed","paper":{"title":"Gamma-ray continuum emission from the inner Galactic region as observed with INTEGRAL/SPI","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.W. Strong, F. Lebrun, H. Halloin, L. Bouchet, P. Mandrou, R. Diehl, R. Terrier, V. Schoenfelder","submitted_at":"2005-09-12T13:04:50Z","abstract_excerpt":"The diffuse continuum emission from the Galactic plane in the energy range 18-1000 keV has been studied using 16 Ms of data from the SPI instrument on INTEGRAL. With such an exposure we can exploit the imaging properties of SPI to achieve a good separation of point sources from the various diffuse components. Using a candidate-source catalogue derived with IBIS on INTEGRAL and a number of sky distribution models we obtained spectra resolved in Galactic longitude. We can identify spectral components of a diffuse continuum of power law shape with index about 1.7, a positron annihilation componen"},"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":"astro-ph/0509290","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-09-12T13:04:50Z","cross_cats_sorted":[],"title_canon_sha256":"6dcf9f502378322729052775a67f19f3d5e4fcbb20cc9c267d78204b5c8afd84","abstract_canon_sha256":"1b2244fee29a38b64e6fd7f3b4089705638c7dbc5a99f19ea1c528c7af0f0853"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:48:24.541432Z","signature_b64":"SJl+stLgGWiEc/VpFV2b5IPdfWgJLgeTLkAj18fFbMnn1s1e44pCaH31xprWWQm06hysGKf91KzH1XvTkftxBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6314c106354ca07a5d395fed0669d085df9ef5716a2ceed7e606dabe9a2ec4c3","last_reissued_at":"2026-07-04T14:48:24.541042Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:48:24.541042Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gamma-ray continuum emission from the inner Galactic region as observed with INTEGRAL/SPI","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.W. Strong, F. Lebrun, H. Halloin, L. Bouchet, P. Mandrou, R. Diehl, R. Terrier, V. Schoenfelder","submitted_at":"2005-09-12T13:04:50Z","abstract_excerpt":"The diffuse continuum emission from the Galactic plane in the energy range 18-1000 keV has been studied using 16 Ms of data from the SPI instrument on INTEGRAL. With such an exposure we can exploit the imaging properties of SPI to achieve a good separation of point sources from the various diffuse components. Using a candidate-source catalogue derived with IBIS on INTEGRAL and a number of sky distribution models we obtained spectra resolved in Galactic longitude. We can identify spectral components of a diffuse continuum of power law shape with index about 1.7, a positron annihilation componen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0509290","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/astro-ph/0509290/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":"astro-ph/0509290","created_at":"2026-07-04T14:48:24.541107+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0509290v1","created_at":"2026-07-04T14:48:24.541107+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0509290","created_at":"2026-07-04T14:48:24.541107+00:00"},{"alias_kind":"pith_short_12","alias_value":"MMKMCBRVJSQH","created_at":"2026-07-04T14:48:24.541107+00:00"},{"alias_kind":"pith_short_16","alias_value":"MMKMCBRVJSQHUXJZ","created_at":"2026-07-04T14:48:24.541107+00:00"},{"alias_kind":"pith_short_8","alias_value":"MMKMCBRV","created_at":"2026-07-04T14:48:24.541107+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2503.15630","citing_title":"Supernova production of axion-like particles coupling to electrons, reloaded","ref_index":69,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX","json":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX.json","graph_json":"https://pith.science/api/pith-number/MMKMCBRVJSQHUXJZL7WQM2OQQX/graph.json","events_json":"https://pith.science/api/pith-number/MMKMCBRVJSQHUXJZL7WQM2OQQX/events.json","paper":"https://pith.science/paper/MMKMCBRV"},"agent_actions":{"view_html":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX","download_json":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX.json","view_paper":"https://pith.science/paper/MMKMCBRV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0509290&json=true","fetch_graph":"https://pith.science/api/pith-number/MMKMCBRVJSQHUXJZL7WQM2OQQX/graph.json","fetch_events":"https://pith.science/api/pith-number/MMKMCBRVJSQHUXJZL7WQM2OQQX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX/action/storage_attestation","attest_author":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX/action/author_attestation","sign_citation":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX/action/citation_signature","submit_replication":"https://pith.science/pith/MMKMCBRVJSQHUXJZL7WQM2OQQX/action/replication_record"}},"created_at":"2026-07-04T14:48:24.541107+00:00","updated_at":"2026-07-04T14:48:24.541107+00:00"}