{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:A3EC3MUZU2FZ2ZCAIDKNSX5KQ5","short_pith_number":"pith:A3EC3MUZ","schema_version":"1.0","canonical_sha256":"06c82db299a68b9d644040d4d95faa874bbedba24716af12fafa01e0667fe07b","source":{"kind":"arxiv","id":"2001.08263","version":1},"attestation_state":"computed","paper":{"title":"X-CIGALE: fitting AGN/galaxy SEDs from X-ray to infrared","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"C. Papovich, D. Burgarella, F. Duras, Guang Yang (Texas A&M), L. Ciesla, M. Boquien, M. Stalevski, V. Buat, W. N. Brandt","submitted_at":"2020-01-22T20:23:25Z","abstract_excerpt":"CIGALE is a powerful multiwavelength spectral energy distribution (SED) fitting code for extragalactic studies. However, the current version of CIGALE is not able to fit X-ray data, which often provide unique insights into AGN intrinsic power. We develop a new X-ray module for CIGALE, allowing it to fit SEDs from the X-ray to infrared (IR). We also improve the AGN fitting of CIGALE from UV-to-IR wavelengths. We implement a modern clumpy two-phase torus model, SKIRTOR. To account for moderately extincted type 1 AGNs, we implement polar-dust extinction. We publicly release the source code (named"},"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":"2001.08263","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2020-01-22T20:23:25Z","cross_cats_sorted":["astro-ph.HE","astro-ph.IM"],"title_canon_sha256":"7bb9d25076d3d16a7c3626eb8ca2355cb8f8de130dfc93c150308b14ba3e9038","abstract_canon_sha256":"3145a96451b593418bb3a4c564e3c4f07cff7d6429f3c54137e48c5bc2af2cbe"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:35:11.394495Z","signature_b64":"TT00eT57lMtlFJNYi/hNyratS9O8x1W6ycIcksFD8FHCuyzLaGjYSibtzhnoShbNNUwNbkmbhKNiy6QQbL4YDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"06c82db299a68b9d644040d4d95faa874bbedba24716af12fafa01e0667fe07b","last_reissued_at":"2026-07-05T00:35:11.393978Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:35:11.393978Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"X-CIGALE: fitting AGN/galaxy SEDs from X-ray to infrared","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"C. Papovich, D. Burgarella, F. Duras, Guang Yang (Texas A&M), L. Ciesla, M. Boquien, M. Stalevski, V. Buat, W. N. Brandt","submitted_at":"2020-01-22T20:23:25Z","abstract_excerpt":"CIGALE is a powerful multiwavelength spectral energy distribution (SED) fitting code for extragalactic studies. However, the current version of CIGALE is not able to fit X-ray data, which often provide unique insights into AGN intrinsic power. We develop a new X-ray module for CIGALE, allowing it to fit SEDs from the X-ray to infrared (IR). We also improve the AGN fitting of CIGALE from UV-to-IR wavelengths. We implement a modern clumpy two-phase torus model, SKIRTOR. To account for moderately extincted type 1 AGNs, we implement polar-dust extinction. We publicly release the source code (named"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2001.08263","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/2001.08263/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":"2001.08263","created_at":"2026-07-05T00:35:11.394037+00:00"},{"alias_kind":"arxiv_version","alias_value":"2001.08263v1","created_at":"2026-07-05T00:35:11.394037+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2001.08263","created_at":"2026-07-05T00:35:11.394037+00:00"},{"alias_kind":"pith_short_12","alias_value":"A3EC3MUZU2FZ","created_at":"2026-07-05T00:35:11.394037+00:00"},{"alias_kind":"pith_short_16","alias_value":"A3EC3MUZU2FZ2ZCA","created_at":"2026-07-05T00:35:11.394037+00:00"},{"alias_kind":"pith_short_8","alias_value":"A3EC3MUZ","created_at":"2026-07-05T00:35:11.394037+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":10,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06844","citing_title":"First detection of ultra-fast outflows in a quiescent galaxy","ref_index":234,"is_internal_anchor":true},{"citing_arxiv_id":"2606.29608","citing_title":"The Lockman-SpReSO Project: A Deep X-ray Spectral View of a FIR-selected AGN Population","ref_index":55,"is_internal_anchor":false},{"citing_arxiv_id":"2606.02699","citing_title":"A New Record Census of Dwarf AGN and a Bimodal $M_{\\rm BH}$-$M_{\\star}$ Scaling Relation with DESI DR1","ref_index":230,"is_internal_anchor":false},{"citing_arxiv_id":"2512.05584","citing_title":"Stellar feedback drives the baryon deficiency in low-mass galaxies","ref_index":41,"is_internal_anchor":false},{"citing_arxiv_id":"2605.17040","citing_title":"PEARLS: JWST Counterparts of Micro-Jy Radio Sources in the NEP Time Domain Field. II. All Four Spokes","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2605.18161","citing_title":"SDSS-V: Revealing a weak accretion state in X-ray selected red quasars","ref_index":158,"is_internal_anchor":false},{"citing_arxiv_id":"2605.00822","citing_title":"PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26743","citing_title":"A Rare Eddington-Limited, Heavily Obscured Low-Mass Active Galactic Nucleus Likely Triggered by a Galaxy Merger","ref_index":119,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04144","citing_title":"The galaxy-halo connection and the dynamical evolution of a giant disc in a massive node of the Cosmic Web at z~3","ref_index":155,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04537","citing_title":"Investigating the Effects of Bars on Star Formation and Nuclear Activity of Galaxies Using DESI Survey Data","ref_index":96,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5","json":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5.json","graph_json":"https://pith.science/api/pith-number/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/graph.json","events_json":"https://pith.science/api/pith-number/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/events.json","paper":"https://pith.science/paper/A3EC3MUZ"},"agent_actions":{"view_html":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5","download_json":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5.json","view_paper":"https://pith.science/paper/A3EC3MUZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2001.08263&json=true","fetch_graph":"https://pith.science/api/pith-number/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/graph.json","fetch_events":"https://pith.science/api/pith-number/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/action/storage_attestation","attest_author":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/action/author_attestation","sign_citation":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/action/citation_signature","submit_replication":"https://pith.science/pith/A3EC3MUZU2FZ2ZCAIDKNSX5KQ5/action/replication_record"}},"created_at":"2026-07-05T00:35:11.394037+00:00","updated_at":"2026-07-05T00:35:11.394037+00:00"}