{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:C3TCK35E7HSUO4SITBLDRZHHBM","short_pith_number":"pith:C3TCK35E","schema_version":"1.0","canonical_sha256":"16e6256fa4f9e5477248985638e4e70b022987d49f8804b809ca5b27ccb97086","source":{"kind":"arxiv","id":"1809.04088","version":2},"attestation_state":"computed","paper":{"title":"Comprehensive comparison of models for spectral energy distributions from 0.1 micron to 1 mm of nearby star-forming galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Rossi, B. A. Groves, B. Brandl, B. T. Draine, C. D. Wilson, D. A. Dale, D. Calzetti, G. Helou, G. L. Granato, I. De Looze, J. D. Smith, J. Koda, J. L. Hinz, K. D. Gordon, K. M. Sandstrom, K. V. Croxall, L. Ciesla, L.K. Hunt, L. Silva, M. Boquien, M. Galametz, M. Relano, R. C. Kennicutt, R. Herrera-Camus, R. Nikutta, S. Bianchi, S. Salim, S. Viaene, S. Zibetti","submitted_at":"2018-09-11T18:00:06Z","abstract_excerpt":"We have fit the far-ultraviolet (FUV) to sub-millimeter (850 micron) spectral energy distributions (SEDs) of the 61 galaxies from the \"Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel\" (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multi-wavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple \"recipes\" for stellar mass (Mstar)"},"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":"1809.04088","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-09-11T18:00:06Z","cross_cats_sorted":[],"title_canon_sha256":"d24c231570516c436d146a9a33fc663512643b814f39f2524dc54334f5b9f595","abstract_canon_sha256":"20746b82b889df1cbaea7496359bfdbb4c2a44d866b7d865be3661179284f0ec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:56:47.253008Z","signature_b64":"WK38CiB6VzbcpCmL4UTDW5Tnf3S9EOW0JuoEpe9jsFkZEAWSRIUeYQyeRuXat0BvCZDxZVmIaBF8Be4GVyRSBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"16e6256fa4f9e5477248985638e4e70b022987d49f8804b809ca5b27ccb97086","last_reissued_at":"2026-05-17T23:56:47.252469Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:56:47.252469Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Comprehensive comparison of models for spectral energy distributions from 0.1 micron to 1 mm of nearby star-forming galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Rossi, B. A. Groves, B. Brandl, B. T. Draine, C. D. Wilson, D. A. Dale, D. Calzetti, G. Helou, G. L. Granato, I. De Looze, J. D. Smith, J. Koda, J. L. Hinz, K. D. Gordon, K. M. Sandstrom, K. V. Croxall, L. Ciesla, L.K. Hunt, L. Silva, M. Boquien, M. Galametz, M. Relano, R. C. Kennicutt, R. Herrera-Camus, R. Nikutta, S. Bianchi, S. Salim, S. Viaene, S. Zibetti","submitted_at":"2018-09-11T18:00:06Z","abstract_excerpt":"We have fit the far-ultraviolet (FUV) to sub-millimeter (850 micron) spectral energy distributions (SEDs) of the 61 galaxies from the \"Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel\" (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multi-wavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple \"recipes\" for stellar mass (Mstar)"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1809.04088","kind":"arxiv","version":2},"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":"1809.04088","created_at":"2026-05-17T23:56:47.252552+00:00"},{"alias_kind":"arxiv_version","alias_value":"1809.04088v2","created_at":"2026-05-17T23:56:47.252552+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1809.04088","created_at":"2026-05-17T23:56:47.252552+00:00"},{"alias_kind":"pith_short_12","alias_value":"C3TCK35E7HSU","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_16","alias_value":"C3TCK35E7HSUO4SI","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_8","alias_value":"C3TCK35E","created_at":"2026-05-18T12:32:16.446611+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.12254","citing_title":"Investigating the young stellar populations and hierarchies in nearby galaxies with the UVIT. II. Presenting the properties of ~25,000 UV-detected star-forming clumps","ref_index":138,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM","json":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM.json","graph_json":"https://pith.science/api/pith-number/C3TCK35E7HSUO4SITBLDRZHHBM/graph.json","events_json":"https://pith.science/api/pith-number/C3TCK35E7HSUO4SITBLDRZHHBM/events.json","paper":"https://pith.science/paper/C3TCK35E"},"agent_actions":{"view_html":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM","download_json":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM.json","view_paper":"https://pith.science/paper/C3TCK35E","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1809.04088&json=true","fetch_graph":"https://pith.science/api/pith-number/C3TCK35E7HSUO4SITBLDRZHHBM/graph.json","fetch_events":"https://pith.science/api/pith-number/C3TCK35E7HSUO4SITBLDRZHHBM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM/action/storage_attestation","attest_author":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM/action/author_attestation","sign_citation":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM/action/citation_signature","submit_replication":"https://pith.science/pith/C3TCK35E7HSUO4SITBLDRZHHBM/action/replication_record"}},"created_at":"2026-05-17T23:56:47.252552+00:00","updated_at":"2026-05-17T23:56:47.252552+00:00"}