{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:JAV5I2YBDLJUPVDUOSZWKE4EZC","short_pith_number":"pith:JAV5I2YB","schema_version":"1.0","canonical_sha256":"482bd46b011ad347d47474b3651384c890b2e85446022e5d303f68d0e6f461a3","source":{"kind":"arxiv","id":"1606.02714","version":2},"attestation_state":"computed","paper":{"title":"Simulating the dust content of galaxies: successes and failures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), (2) Caltech, 3), (3) Harvard), Christopher C. Hayward (2, Federico Marinacci (1) ((1) MIT, Mark Vogelsberger (1), Paul Torrey (1, Ryan McKinnon (1)","submitted_at":"2016-06-08T20:00:01Z","abstract_excerpt":"We present full volume cosmological simulations using the moving-mesh code AREPO to study the coevolution of dust and galaxies. We extend the dust model in AREPO to include thermal sputtering of grains and investigate the evolution of the dust mass function, the cosmic distribution of dust beyond the interstellar medium, and the dependence of dust-to-stellar mass ratio on galactic properties. The simulated dust mass function is well-described by a Schechter fit and lies closest to observations at $z = 0$. The radial scaling of projected dust surface density out to distances of $10 \\, \\text{Mpc"},"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":"1606.02714","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-06-08T20:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"776cceb59c089c064fcebdbb0053cff896e1a7d0bc3531a9294cdfcd6f006355","abstract_canon_sha256":"1aa91bdebdbf3f3b8264c9a1d3e5108ed771d9b100c73fb47cf8c358c9024fff"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:43:45.414287Z","signature_b64":"CN/9bw9dAIA2SSZPMkAOKMkYPKy7ydHDTuVosGSTbbggyFyeBl+B+SU9DQlW9zQg4GbMa14FTiwzvGJc1npgAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"482bd46b011ad347d47474b3651384c890b2e85446022e5d303f68d0e6f461a3","last_reissued_at":"2026-05-18T00:43:45.413793Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:43:45.413793Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulating the dust content of galaxies: successes and failures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), (2) Caltech, 3), (3) Harvard), Christopher C. Hayward (2, Federico Marinacci (1) ((1) MIT, Mark Vogelsberger (1), Paul Torrey (1, Ryan McKinnon (1)","submitted_at":"2016-06-08T20:00:01Z","abstract_excerpt":"We present full volume cosmological simulations using the moving-mesh code AREPO to study the coevolution of dust and galaxies. We extend the dust model in AREPO to include thermal sputtering of grains and investigate the evolution of the dust mass function, the cosmic distribution of dust beyond the interstellar medium, and the dependence of dust-to-stellar mass ratio on galactic properties. The simulated dust mass function is well-described by a Schechter fit and lies closest to observations at $z = 0$. The radial scaling of projected dust surface density out to distances of $10 \\, \\text{Mpc"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.02714","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":"1606.02714","created_at":"2026-05-18T00:43:45.413874+00:00"},{"alias_kind":"arxiv_version","alias_value":"1606.02714v2","created_at":"2026-05-18T00:43:45.413874+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1606.02714","created_at":"2026-05-18T00:43:45.413874+00:00"},{"alias_kind":"pith_short_12","alias_value":"JAV5I2YBDLJU","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_16","alias_value":"JAV5I2YBDLJUPVDU","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_8","alias_value":"JAV5I2YB","created_at":"2026-05-18T12:30:22.444734+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2605.19661","citing_title":"COSMOS-Web: Star formation along the early Hubble sequence and the evolution of dust over the redshift range 0