{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:BM3J5AXLVD2AQDCKPFNG23IYEP","short_pith_number":"pith:BM3J5AXL","schema_version":"1.0","canonical_sha256":"0b369e82eba8f4080c4a795a6d6d1823d5e7fbf992e5b0a9335e9b507be5242f","source":{"kind":"arxiv","id":"2603.04505","version":2},"attestation_state":"computed","paper":{"title":"The Drivers of Cosmic Dust Temperature Evolution","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Chiara Feruglio, Desika Narayanan, Fabrizio Fiore, Francesco Salvestrini, Gian Luigi Granato, Laura Silva, Manuela Bischetti, Massimiliano Parente, Roberta Tripodi, Simone Bianchi","submitted_at":"2026-03-04T19:00:05Z","abstract_excerpt":"Observations of the rest-frame far-infrared (far-IR) emission of galaxies suggest a mild increase of dust temperature $T_{\\rm dust}$ with redshift, although constraining $T_{\\rm dust}$ in high-redshift systems remains challenging due to limited sampling of the far-IR spectral energy distribution (SED). We present and discuss the redshift evolution of $T_{\\rm dust}$ predicted by a cosmological galaxy evolution simulation with dust treatment, and interpret its dependence on other galaxy physical properties. We use a semi-analytic model of galaxy formation that includes an explicit treatment of 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":"2603.04505","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2026-03-04T19:00:05Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"ebedddb46464bee923f39beb75ee1f37e9b2a4707899be9dbbdc338599095159","abstract_canon_sha256":"825c817d618e5365c07bae0daa9063da7a84aacd0225ac5c9a006e9575a47365"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-17T01:21:46.853661Z","signature_b64":"JdTzpdL54iidjXohQF05I5NA508V163LgazteLajJuTPYhIMaO27eF90tq77jdz9SwKwSR41X4RimadwVo7dDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0b369e82eba8f4080c4a795a6d6d1823d5e7fbf992e5b0a9335e9b507be5242f","last_reissued_at":"2026-07-17T01:21:46.852730Z","signature_status":"signed_v1","first_computed_at":"2026-07-17T01:21:46.852730Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Drivers of Cosmic Dust Temperature Evolution","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Chiara Feruglio, Desika Narayanan, Fabrizio Fiore, Francesco Salvestrini, Gian Luigi Granato, Laura Silva, Manuela Bischetti, Massimiliano Parente, Roberta Tripodi, Simone Bianchi","submitted_at":"2026-03-04T19:00:05Z","abstract_excerpt":"Observations of the rest-frame far-infrared (far-IR) emission of galaxies suggest a mild increase of dust temperature $T_{\\rm dust}$ with redshift, although constraining $T_{\\rm dust}$ in high-redshift systems remains challenging due to limited sampling of the far-IR spectral energy distribution (SED). We present and discuss the redshift evolution of $T_{\\rm dust}$ predicted by a cosmological galaxy evolution simulation with dust treatment, and interpret its dependence on other galaxy physical properties. We use a semi-analytic model of galaxy formation that includes an explicit treatment of d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2603.04505","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2603.04505/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":"2603.04505","created_at":"2026-07-17T01:21:46.853171+00:00"},{"alias_kind":"arxiv_version","alias_value":"2603.04505v2","created_at":"2026-07-17T01:21:46.853171+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2603.04505","created_at":"2026-07-17T01:21:46.853171+00:00"},{"alias_kind":"pith_short_12","alias_value":"BM3J5AXLVD2A","created_at":"2026-07-17T01:21:46.853171+00:00"},{"alias_kind":"pith_short_16","alias_value":"BM3J5AXLVD2AQDCK","created_at":"2026-07-17T01:21:46.853171+00:00"},{"alias_kind":"pith_short_8","alias_value":"BM3J5AXL","created_at":"2026-07-17T01:21:46.853171+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2604.09347","citing_title":"A first [CII] view of high-z quiescent galaxies","ref_index":52,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP","json":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP.json","graph_json":"https://pith.science/api/pith-number/BM3J5AXLVD2AQDCKPFNG23IYEP/graph.json","events_json":"https://pith.science/api/pith-number/BM3J5AXLVD2AQDCKPFNG23IYEP/events.json","paper":"https://pith.science/paper/BM3J5AXL"},"agent_actions":{"view_html":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP","download_json":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP.json","view_paper":"https://pith.science/paper/BM3J5AXL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2603.04505&json=true","fetch_graph":"https://pith.science/api/pith-number/BM3J5AXLVD2AQDCKPFNG23IYEP/graph.json","fetch_events":"https://pith.science/api/pith-number/BM3J5AXLVD2AQDCKPFNG23IYEP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP/action/storage_attestation","attest_author":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP/action/author_attestation","sign_citation":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP/action/citation_signature","submit_replication":"https://pith.science/pith/BM3J5AXLVD2AQDCKPFNG23IYEP/action/replication_record"}},"created_at":"2026-07-17T01:21:46.853171+00:00","updated_at":"2026-07-17T01:21:46.853171+00:00"}