{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:ZXJMIUDUEWVLYH4VDFADU7E7XY","short_pith_number":"pith:ZXJMIUDU","schema_version":"1.0","canonical_sha256":"cdd2c4507425aabc1f9519403a7c9fbe1e9b76dcb3b1edb56ced6f5d0b207567","source":{"kind":"arxiv","id":"1210.4540","version":1},"attestation_state":"computed","paper":{"title":"Spectral Energy Distributions of low-luminosity radio galaxies at z~1-3: a high-z view of the host/AGN connection","license":"http://creativecommons.org/licenses/by/3.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"((1) SISSA, 2), (2) Space Telescope Science Institute, 3, (3) INAF-Istituto di Radio Astronomia, 4), (4) Johns Hopkins University, (5) INAF- Osservatorio Astronomico di Torino, 6), (6) Insituto de Astrofisica de Canarias, Alessandro Capetti (5), Baltimore, Bologna, Italy, Javier Rodriguez-Zaurin (2, La Laguna, Marco Chiaberge (2, Ranieri D. Baldi (1, Spain), Susana Deustua (2), Trieste, USA, William B. Sparks (2)","submitted_at":"2012-10-16T19:54:29Z","abstract_excerpt":"We study the Spectral Energy Distributions, SEDs, (from FUV to MIR bands) of the first sizeable sample of 34 low-luminosity radio galaxies at high redshifts, selected in the COSMOS field. To model the SEDs we use two different template-fitting techniques: i) the Hyperz code that only considers single stellar templates and ii) our own developed technique 2SPD that also includes the contribution from a young stellar population and dust emission. The resulting photometric redshifts range from z ~0.7 to 3 and are in substantial agreement with measurements from earlier work, but significantly more "},"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":"1210.4540","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/3.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-10-16T19:54:29Z","cross_cats_sorted":[],"title_canon_sha256":"074726ea72b564f45becc648e3a426f955c6deeb450439045aef5eb331022a24","abstract_canon_sha256":"1682f038187be6b739c5e0336bbcb14c080e0f6f9ab3b1b0d2400590d7a8b6af"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:53:54.070861Z","signature_b64":"eErVsCNukt03kbWLBgND1K1rysDp2BluBAw+7mA/oFU4ZS8+8zNNmV0CL06jCAlG/DKcRrquz1Nim+8UnNcMCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cdd2c4507425aabc1f9519403a7c9fbe1e9b76dcb3b1edb56ced6f5d0b207567","last_reissued_at":"2026-05-18T01:53:54.070199Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:53:54.070199Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spectral Energy Distributions of low-luminosity radio galaxies at z~1-3: a high-z view of the host/AGN connection","license":"http://creativecommons.org/licenses/by/3.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"((1) SISSA, 2), (2) Space Telescope Science Institute, 3, (3) INAF-Istituto di Radio Astronomia, 4), (4) Johns Hopkins University, (5) INAF- Osservatorio Astronomico di Torino, 6), (6) Insituto de Astrofisica de Canarias, Alessandro Capetti (5), Baltimore, Bologna, Italy, Javier Rodriguez-Zaurin (2, La Laguna, Marco Chiaberge (2, Ranieri D. Baldi (1, Spain), Susana Deustua (2), Trieste, USA, William B. Sparks (2)","submitted_at":"2012-10-16T19:54:29Z","abstract_excerpt":"We study the Spectral Energy Distributions, SEDs, (from FUV to MIR bands) of the first sizeable sample of 34 low-luminosity radio galaxies at high redshifts, selected in the COSMOS field. To model the SEDs we use two different template-fitting techniques: i) the Hyperz code that only considers single stellar templates and ii) our own developed technique 2SPD that also includes the contribution from a young stellar population and dust emission. The resulting photometric redshifts range from z ~0.7 to 3 and are in substantial agreement with measurements from earlier work, but significantly more "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1210.4540","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":"1210.4540","created_at":"2026-05-18T01:53:54.070296+00:00"},{"alias_kind":"arxiv_version","alias_value":"1210.4540v1","created_at":"2026-05-18T01:53:54.070296+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1210.4540","created_at":"2026-05-18T01:53:54.070296+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZXJMIUDUEWVL","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZXJMIUDUEWVLYH4V","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZXJMIUDU","created_at":"2026-05-18T12:27:30.460161+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/ZXJMIUDUEWVLYH4VDFADU7E7XY","json":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY.json","graph_json":"https://pith.science/api/pith-number/ZXJMIUDUEWVLYH4VDFADU7E7XY/graph.json","events_json":"https://pith.science/api/pith-number/ZXJMIUDUEWVLYH4VDFADU7E7XY/events.json","paper":"https://pith.science/paper/ZXJMIUDU"},"agent_actions":{"view_html":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY","download_json":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY.json","view_paper":"https://pith.science/paper/ZXJMIUDU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1210.4540&json=true","fetch_graph":"https://pith.science/api/pith-number/ZXJMIUDUEWVLYH4VDFADU7E7XY/graph.json","fetch_events":"https://pith.science/api/pith-number/ZXJMIUDUEWVLYH4VDFADU7E7XY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY/action/storage_attestation","attest_author":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY/action/author_attestation","sign_citation":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY/action/citation_signature","submit_replication":"https://pith.science/pith/ZXJMIUDUEWVLYH4VDFADU7E7XY/action/replication_record"}},"created_at":"2026-05-18T01:53:54.070296+00:00","updated_at":"2026-05-18T01:53:54.070296+00:00"}