{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:5F5NTIMSARSMLWHYKBKECH6AGD","short_pith_number":"pith:5F5NTIMS","schema_version":"1.0","canonical_sha256":"e97ad9a1920464c5d8f85054411fc030edaa5947a7811867e8d86b0bec9f15da","source":{"kind":"arxiv","id":"1506.01533","version":1},"attestation_state":"computed","paper":{"title":"Dust evolution in the transition towards the denser ISM: impact on dust temperature, opacity, and spectral index","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Anthony P. Jones, Melanie K\\\"ohler, Nathalie Ysard","submitted_at":"2015-06-04T10:06:44Z","abstract_excerpt":"Variations in the observed dust emission and extinction indicate a systematic evolution of grain properties in the transition from the diffuse interstellar medium (ISM) to denser molecular clouds. The differences in the dust spectral energy distribution (SED) observed from the diffuse ISM to denser regions, namely an increase in the spectral index at long wavelengths, an increase in the FIR opacity, and a decrease in temperature, are usually assumed to be the result of changes in dust properties. We investigate if evolutionary processes, such as coagulation and accretion, are able to change th"},"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":"1506.01533","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2015-06-04T10:06:44Z","cross_cats_sorted":[],"title_canon_sha256":"344afb286a8a7ab44a630c1986aaa3e19f7b1720d51f118a9207d185636e118c","abstract_canon_sha256":"38ded455cc7a5b1cb36446e8b6fb04f57d1e4dcc9579db56090adeca5f6a3dce"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:57:18.614988Z","signature_b64":"eifxY393eQtL4b1Ld/L9rhiycovIGok7EfvsaMA580TpHv/wWFhnair+qG+DnIsz4sY0QCAqvgWL4qvXQcYVCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e97ad9a1920464c5d8f85054411fc030edaa5947a7811867e8d86b0bec9f15da","last_reissued_at":"2026-05-18T01:57:18.614355Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:57:18.614355Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dust evolution in the transition towards the denser ISM: impact on dust temperature, opacity, and spectral index","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Anthony P. Jones, Melanie K\\\"ohler, Nathalie Ysard","submitted_at":"2015-06-04T10:06:44Z","abstract_excerpt":"Variations in the observed dust emission and extinction indicate a systematic evolution of grain properties in the transition from the diffuse interstellar medium (ISM) to denser molecular clouds. The differences in the dust spectral energy distribution (SED) observed from the diffuse ISM to denser regions, namely an increase in the spectral index at long wavelengths, an increase in the FIR opacity, and a decrease in temperature, are usually assumed to be the result of changes in dust properties. We investigate if evolutionary processes, such as coagulation and accretion, are able to change th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1506.01533","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":"1506.01533","created_at":"2026-05-18T01:57:18.614457+00:00"},{"alias_kind":"arxiv_version","alias_value":"1506.01533v1","created_at":"2026-05-18T01:57:18.614457+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1506.01533","created_at":"2026-05-18T01:57:18.614457+00:00"},{"alias_kind":"pith_short_12","alias_value":"5F5NTIMSARSM","created_at":"2026-05-18T12:29:05.191682+00:00"},{"alias_kind":"pith_short_16","alias_value":"5F5NTIMSARSMLWHY","created_at":"2026-05-18T12:29:05.191682+00:00"},{"alias_kind":"pith_short_8","alias_value":"5F5NTIMS","created_at":"2026-05-18T12:29:05.191682+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.05325","citing_title":"Scylla: Observational Evidence for an Order of Magnitude in Dust Mass Opacity Evolution with ISM Density in the Large Magellanic Cloud","ref_index":42,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD","json":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD.json","graph_json":"https://pith.science/api/pith-number/5F5NTIMSARSMLWHYKBKECH6AGD/graph.json","events_json":"https://pith.science/api/pith-number/5F5NTIMSARSMLWHYKBKECH6AGD/events.json","paper":"https://pith.science/paper/5F5NTIMS"},"agent_actions":{"view_html":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD","download_json":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD.json","view_paper":"https://pith.science/paper/5F5NTIMS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1506.01533&json=true","fetch_graph":"https://pith.science/api/pith-number/5F5NTIMSARSMLWHYKBKECH6AGD/graph.json","fetch_events":"https://pith.science/api/pith-number/5F5NTIMSARSMLWHYKBKECH6AGD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD/action/storage_attestation","attest_author":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD/action/author_attestation","sign_citation":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD/action/citation_signature","submit_replication":"https://pith.science/pith/5F5NTIMSARSMLWHYKBKECH6AGD/action/replication_record"}},"created_at":"2026-05-18T01:57:18.614457+00:00","updated_at":"2026-05-18T01:57:18.614457+00:00"}