{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:E4W2DICSWJ6NDAQDJTIZUFBHRE","short_pith_number":"pith:E4W2DICS","schema_version":"1.0","canonical_sha256":"272da1a052b27cd182034cd19a142789036a4c6cf2cd55e8bcc881e457a862d2","source":{"kind":"arxiv","id":"1205.6137","version":2},"attestation_state":"computed","paper":{"title":"Impact of grain size distributions on the dust enrichment in high-redshift quasars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Hiroyuki Hirashita, Tzu-Ming Kuo","submitted_at":"2012-05-28T15:05:20Z","abstract_excerpt":"In high-redshift ($z>5$) quasars, a large amount of dust ($\\textstyle\\sim 10^{8} \\mathrm{M}_{\\sun}$) has been observed. In order to explain the large dust content, we focus on a possibility that grain growth by the accretion of heavy elements is the dominant dust source. We adopt a chemical evolution model applicable to nearby galaxies but utilize parameters adequate to high-$z$ quasars. It is assumed that metals and dust are predominantly ejected by Type II supernovae (SNe). We have found that grain growth strongly depends on the grain size distribution. If we simply use the size distribution"},"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":"1205.6137","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2012-05-28T15:05:20Z","cross_cats_sorted":[],"title_canon_sha256":"221f29620702b6d2b76de59b43bb4b928335c82ab38d2b87bfe05e567bc97fa4","abstract_canon_sha256":"041cb113307f73ca07d04df5fa8eaf9a1075496ad5c4750e778d5eceb00bd15d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:57:16.565629Z","signature_b64":"ekPZZAFqSbygyKuCPKPYyffjRXjwhU/99MoXH/AwpQoYZY3lXwG+R5Y3sMmCAGFiMCQUB/pKbkKQIMTJ7lsOAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"272da1a052b27cd182034cd19a142789036a4c6cf2cd55e8bcc881e457a862d2","last_reissued_at":"2026-05-18T01:57:16.565147Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:57:16.565147Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impact of grain size distributions on the dust enrichment in high-redshift quasars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Hiroyuki Hirashita, Tzu-Ming Kuo","submitted_at":"2012-05-28T15:05:20Z","abstract_excerpt":"In high-redshift ($z>5$) quasars, a large amount of dust ($\\textstyle\\sim 10^{8} \\mathrm{M}_{\\sun}$) has been observed. In order to explain the large dust content, we focus on a possibility that grain growth by the accretion of heavy elements is the dominant dust source. We adopt a chemical evolution model applicable to nearby galaxies but utilize parameters adequate to high-$z$ quasars. It is assumed that metals and dust are predominantly ejected by Type II supernovae (SNe). We have found that grain growth strongly depends on the grain size distribution. If we simply use the size distribution"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1205.6137","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":"1205.6137","created_at":"2026-05-18T01:57:16.565219+00:00"},{"alias_kind":"arxiv_version","alias_value":"1205.6137v2","created_at":"2026-05-18T01:57:16.565219+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1205.6137","created_at":"2026-05-18T01:57:16.565219+00:00"},{"alias_kind":"pith_short_12","alias_value":"E4W2DICSWJ6N","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_16","alias_value":"E4W2DICSWJ6NDAQD","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_8","alias_value":"E4W2DICS","created_at":"2026-05-18T12:27:04.183437+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.13851","citing_title":"Interstellar dust production, destruction and effects of dust depletion in galaxies","ref_index":212,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE","json":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE.json","graph_json":"https://pith.science/api/pith-number/E4W2DICSWJ6NDAQDJTIZUFBHRE/graph.json","events_json":"https://pith.science/api/pith-number/E4W2DICSWJ6NDAQDJTIZUFBHRE/events.json","paper":"https://pith.science/paper/E4W2DICS"},"agent_actions":{"view_html":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE","download_json":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE.json","view_paper":"https://pith.science/paper/E4W2DICS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1205.6137&json=true","fetch_graph":"https://pith.science/api/pith-number/E4W2DICSWJ6NDAQDJTIZUFBHRE/graph.json","fetch_events":"https://pith.science/api/pith-number/E4W2DICSWJ6NDAQDJTIZUFBHRE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE/action/storage_attestation","attest_author":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE/action/author_attestation","sign_citation":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE/action/citation_signature","submit_replication":"https://pith.science/pith/E4W2DICSWJ6NDAQDJTIZUFBHRE/action/replication_record"}},"created_at":"2026-05-18T01:57:16.565219+00:00","updated_at":"2026-05-18T01:57:16.565219+00:00"}