{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:ZWTKKA3YKDDTKVIP52PMSOYNJK","short_pith_number":"pith:ZWTKKA3Y","schema_version":"1.0","canonical_sha256":"cda6a5037850c735550fee9ec93b0d4a960c11ef554e1384e32a6dd904263617","source":{"kind":"arxiv","id":"0909.5439","version":1},"attestation_state":"computed","paper":{"title":"Analysis of galaxy SEDs from far-UV to far-IR with CIGALE: Studying a SINGS test sample","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"D. Burgarella, D. Marcillac, E. Giovannoli, J. C. Munoz-Mateos, S. Noll, V. Buat","submitted_at":"2009-09-29T21:05:30Z","abstract_excerpt":"Photometric data of galaxies covering the rest-frame wavelength range from far-UV to far-IR make it possible to derive galaxy properties with a high reliability by fitting the attenuated stellar emission and the related dust emission at the same time. For this purpose we wrote the code CIGALE (Code Investigating GALaxy Emission) that uses model spectra composed of the Maraston (or PEGASE) stellar population models, synthetic attenuation functions based on a modified Calzetti law, spectral line templates, the Dale & Helou dust emission models, and optional spectral templates of obscured AGN. De"},"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":"0909.5439","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-09-29T21:05:30Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"3dfd9cbeeb0402d9424d9d7eff052d44da7e2b10b10c77c25cefaa590b6d8a69","abstract_canon_sha256":"80fca281e6775795de68deab1e082724abae9aa6305b824731b2cc39a0e406eb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:11:36.301145Z","signature_b64":"6g86ASylU3UHj1SzoyH1ydnV8pOWyiTqMtI7ybWSmeLGaAJHSHU+V0UMNSBkYqZ8IbWTbag+QuOSr2BurqrGDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cda6a5037850c735550fee9ec93b0d4a960c11ef554e1384e32a6dd904263617","last_reissued_at":"2026-05-18T02:11:36.299618Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:11:36.299618Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Analysis of galaxy SEDs from far-UV to far-IR with CIGALE: Studying a SINGS test sample","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"D. Burgarella, D. Marcillac, E. Giovannoli, J. C. Munoz-Mateos, S. Noll, V. Buat","submitted_at":"2009-09-29T21:05:30Z","abstract_excerpt":"Photometric data of galaxies covering the rest-frame wavelength range from far-UV to far-IR make it possible to derive galaxy properties with a high reliability by fitting the attenuated stellar emission and the related dust emission at the same time. For this purpose we wrote the code CIGALE (Code Investigating GALaxy Emission) that uses model spectra composed of the Maraston (or PEGASE) stellar population models, synthetic attenuation functions based on a modified Calzetti law, spectral line templates, the Dale & Helou dust emission models, and optional spectral templates of obscured AGN. De"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0909.5439","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":"0909.5439","created_at":"2026-05-18T02:11:36.299712+00:00"},{"alias_kind":"arxiv_version","alias_value":"0909.5439v1","created_at":"2026-05-18T02:11:36.299712+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0909.5439","created_at":"2026-05-18T02:11:36.299712+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZWTKKA3YKDDT","created_at":"2026-05-18T12:26:03.138858+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZWTKKA3YKDDTKVIP","created_at":"2026-05-18T12:26:03.138858+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZWTKKA3Y","created_at":"2026-05-18T12:26:03.138858+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":12,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.20590","citing_title":"Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\\beta$ narrow-band imaging","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2508.15899","citing_title":"CIGaRS I: Combined simulation-based inference from type Ia supernovae and host photometry","ref_index":84,"is_internal_anchor":true},{"citing_arxiv_id":"2601.07345","citing_title":"New $H(z)$ measurement at Redshift = 0.12 with DESI Data Release 1","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13966","citing_title":"Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\\mathbf{z>3.5}$ from CAPERS","ref_index":83,"is_internal_anchor":true},{"citing_arxiv_id":"2604.01326","citing_title":"Calibrating Photometric Mid-Infrared Star Formation Rates for JWST","ref_index":126,"is_internal_anchor":false},{"citing_arxiv_id":"2604.05024","citing_title":"Winding Back the Clock: Recent Star Formation Histories of Massive Quiescent Galaxies Are Consistent With Their Rapid Number Density Evolution Since $\\mathbf{z\\sim7}$","ref_index":80,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13216","citing_title":"Sparks II: Panchromatic SED modeling and galaxy physical properties across the starburst to post-starburst sequence","ref_index":90,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18522","citing_title":"A Census of Na D-traced neutral ISM and outflows at $0.6<z<4$","ref_index":273,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20411","citing_title":"The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies","ref_index":12,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05548","citing_title":"A Multiwavelength Assessment Disfavoring the X-ray Binary Origin of He III Regions in Metal-Poor Star-Forming Dwarf Galaxies","ref_index":76,"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":119,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02999","citing_title":"Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas","ref_index":50,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK","json":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK.json","graph_json":"https://pith.science/api/pith-number/ZWTKKA3YKDDTKVIP52PMSOYNJK/graph.json","events_json":"https://pith.science/api/pith-number/ZWTKKA3YKDDTKVIP52PMSOYNJK/events.json","paper":"https://pith.science/paper/ZWTKKA3Y"},"agent_actions":{"view_html":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK","download_json":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK.json","view_paper":"https://pith.science/paper/ZWTKKA3Y","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0909.5439&json=true","fetch_graph":"https://pith.science/api/pith-number/ZWTKKA3YKDDTKVIP52PMSOYNJK/graph.json","fetch_events":"https://pith.science/api/pith-number/ZWTKKA3YKDDTKVIP52PMSOYNJK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK/action/storage_attestation","attest_author":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK/action/author_attestation","sign_citation":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK/action/citation_signature","submit_replication":"https://pith.science/pith/ZWTKKA3YKDDTKVIP52PMSOYNJK/action/replication_record"}},"created_at":"2026-05-18T02:11:36.299712+00:00","updated_at":"2026-05-18T02:11:36.299712+00:00"}