{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:72TDCFZXBBCLNFF2LPBYRHGOIZ","short_pith_number":"pith:72TDCFZX","schema_version":"1.0","canonical_sha256":"fea63117370844b694ba5bc3889cce466b1a7a54aaf797bbd385d5cd0def8dc8","source":{"kind":"arxiv","id":"1306.5235","version":3},"attestation_state":"computed","paper":{"title":"Polycyclic Aromatic Hydrocarbon and Mid-Infrared Continuum Emission in a z>4 Submillimeter Galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(10) NOAO, (11) Vienna), 2), (2) Caltech, (3) UMASS, (4) CEA, (5) SSC, (6) NRAO, (7) MPIA, (8) CFHT, 9), (9) IfA Hawaii, Alexandra Pope (3), Christopher L. Carilli (6), David Elbaz (4) ((1) Cornell, Dominik A. Riechers (1, Emanuele Daddi (4), Fabian Walter (7), Glenn E. Morrison (8, Helmut Dannerbauer (11), Jacqueline Hodge (7), Lee Armus (5), Mark Dickinson (10), Ranga-Ram Chary (5)","submitted_at":"2013-06-21T20:00:00Z","abstract_excerpt":"We report the detection of 6.2um polycyclic aromatic hydrocarbon (PAH) and rest-frame 4-7um continuum emission in the z=4.055 submillimeter galaxy GN20, using the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. This represents the first detection of PAH emission at z>4. The strength of the PAH emission feature is consistent with a very high star formation rate of ~1600Msun/yr. We find that this intense starburst powers at least ~1/3 of the faint underlying 6um continuum emission, with an additional, significant (and perhaps dominant) contribution due to a power-law-like hot d"},"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":"1306.5235","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-06-21T20:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"3d4c34cde4f2965f1d873baeb715cde63a07b865d34f59d27a52ceacb586ef2b","abstract_canon_sha256":"151e7c35b58c8dc8829c8aa2872b9e1536906a0bd697610f1ce29a1bd1ebdf83"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:49:13.845256Z","signature_b64":"kn2gM+jfK7y/IA6Fo70eJtk9lfMgh1ekeUJC/w7ytFpDZutEy50YUbp2akbiRuUGa1DyaR6hRRPqmXHqARxqCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fea63117370844b694ba5bc3889cce466b1a7a54aaf797bbd385d5cd0def8dc8","last_reissued_at":"2026-05-18T01:49:13.844647Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:49:13.844647Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Polycyclic Aromatic Hydrocarbon and Mid-Infrared Continuum Emission in a z>4 Submillimeter Galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(10) NOAO, (11) Vienna), 2), (2) Caltech, (3) UMASS, (4) CEA, (5) SSC, (6) NRAO, (7) MPIA, (8) CFHT, 9), (9) IfA Hawaii, Alexandra Pope (3), Christopher L. Carilli (6), David Elbaz (4) ((1) Cornell, Dominik A. Riechers (1, Emanuele Daddi (4), Fabian Walter (7), Glenn E. Morrison (8, Helmut Dannerbauer (11), Jacqueline Hodge (7), Lee Armus (5), Mark Dickinson (10), Ranga-Ram Chary (5)","submitted_at":"2013-06-21T20:00:00Z","abstract_excerpt":"We report the detection of 6.2um polycyclic aromatic hydrocarbon (PAH) and rest-frame 4-7um continuum emission in the z=4.055 submillimeter galaxy GN20, using the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. This represents the first detection of PAH emission at z>4. The strength of the PAH emission feature is consistent with a very high star formation rate of ~1600Msun/yr. We find that this intense starburst powers at least ~1/3 of the faint underlying 6um continuum emission, with an additional, significant (and perhaps dominant) contribution due to a power-law-like hot d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1306.5235","kind":"arxiv","version":3},"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":"1306.5235","created_at":"2026-05-18T01:49:13.844739+00:00"},{"alias_kind":"arxiv_version","alias_value":"1306.5235v3","created_at":"2026-05-18T01:49:13.844739+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1306.5235","created_at":"2026-05-18T01:49:13.844739+00:00"},{"alias_kind":"pith_short_12","alias_value":"72TDCFZXBBCL","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_16","alias_value":"72TDCFZXBBCLNFF2","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_8","alias_value":"72TDCFZX","created_at":"2026-05-18T12:27:36.564083+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/72TDCFZXBBCLNFF2LPBYRHGOIZ","json":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ.json","graph_json":"https://pith.science/api/pith-number/72TDCFZXBBCLNFF2LPBYRHGOIZ/graph.json","events_json":"https://pith.science/api/pith-number/72TDCFZXBBCLNFF2LPBYRHGOIZ/events.json","paper":"https://pith.science/paper/72TDCFZX"},"agent_actions":{"view_html":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ","download_json":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ.json","view_paper":"https://pith.science/paper/72TDCFZX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1306.5235&json=true","fetch_graph":"https://pith.science/api/pith-number/72TDCFZXBBCLNFF2LPBYRHGOIZ/graph.json","fetch_events":"https://pith.science/api/pith-number/72TDCFZXBBCLNFF2LPBYRHGOIZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ/action/storage_attestation","attest_author":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ/action/author_attestation","sign_citation":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ/action/citation_signature","submit_replication":"https://pith.science/pith/72TDCFZXBBCLNFF2LPBYRHGOIZ/action/replication_record"}},"created_at":"2026-05-18T01:49:13.844739+00:00","updated_at":"2026-05-18T01:49:13.844739+00:00"}