{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:OP2HFXPZXJ2FBYPHJ37EY57SSG","short_pith_number":"pith:OP2HFXPZ","schema_version":"1.0","canonical_sha256":"73f472ddf9ba7450e1e74efe4c77f2918df8fddd5c5f1a88b5cacaf6d8fd0045","source":{"kind":"arxiv","id":"0811.2484","version":1},"attestation_state":"computed","paper":{"title":"Observation and modelling of dusty, low gravity L, and M dwarfs","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Adam J. Burgasser, Andreas Seifahrt, Christiane Helling, Dagny L. Looper, Katelyn N. Allers, Kelle L. Cruz, Michael C. Cushing, S\\\"oren Witte, Ulrike Heiter","submitted_at":"2008-11-15T12:25:14Z","abstract_excerpt":"Observational facilities allow now the detection of optical and IR spectra of young M- and L-dwarfs. This enables empirical comparisons with old M- and L- dwarfs, and detailed studies in comparison with synthetic spectra. While classical stellar atmosphere physics seems perfectly appropriate for old M-dwarfs, more physical and chemical processes, cloud formation in particular, needs to be modelled in the substellar regime to allow a detailed spectral interpretation.\n  Not much is known so far about the details of the inset of cloud formation at the spectral transition region between M and L dw"},"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":"0811.2484","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-11-15T12:25:14Z","cross_cats_sorted":[],"title_canon_sha256":"424655b03c395bf7530e766b3b59bd6532aa556889e5fc6d2b7e5f4b572d355c","abstract_canon_sha256":"41355f308036d5e4c0c9894fab6d5c045c9cc1e62b4244f2a8e3ed208cebb878"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:13:39.508766Z","signature_b64":"nf0LbHeDWXJmcXwQPauWs4cZoHNqGjuMDRrBIg2TLXSe8GEj+sSMwmAuOAIE1fAdcJ2LHJs+vOueasDh+Mf2CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"73f472ddf9ba7450e1e74efe4c77f2918df8fddd5c5f1a88b5cacaf6d8fd0045","last_reissued_at":"2026-07-04T17:13:39.508376Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:13:39.508376Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observation and modelling of dusty, low gravity L, and M dwarfs","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Adam J. Burgasser, Andreas Seifahrt, Christiane Helling, Dagny L. Looper, Katelyn N. Allers, Kelle L. Cruz, Michael C. Cushing, S\\\"oren Witte, Ulrike Heiter","submitted_at":"2008-11-15T12:25:14Z","abstract_excerpt":"Observational facilities allow now the detection of optical and IR spectra of young M- and L-dwarfs. This enables empirical comparisons with old M- and L- dwarfs, and detailed studies in comparison with synthetic spectra. While classical stellar atmosphere physics seems perfectly appropriate for old M-dwarfs, more physical and chemical processes, cloud formation in particular, needs to be modelled in the substellar regime to allow a detailed spectral interpretation.\n  Not much is known so far about the details of the inset of cloud formation at the spectral transition region between M and L dw"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0811.2484","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0811.2484/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":"0811.2484","created_at":"2026-07-04T17:13:39.508429+00:00"},{"alias_kind":"arxiv_version","alias_value":"0811.2484v1","created_at":"2026-07-04T17:13:39.508429+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0811.2484","created_at":"2026-07-04T17:13:39.508429+00:00"},{"alias_kind":"pith_short_12","alias_value":"OP2HFXPZXJ2F","created_at":"2026-07-04T17:13:39.508429+00:00"},{"alias_kind":"pith_short_16","alias_value":"OP2HFXPZXJ2FBYPH","created_at":"2026-07-04T17:13:39.508429+00:00"},{"alias_kind":"pith_short_8","alias_value":"OP2HFXPZ","created_at":"2026-07-04T17:13:39.508429+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG","json":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG.json","graph_json":"https://pith.science/api/pith-number/OP2HFXPZXJ2FBYPHJ37EY57SSG/graph.json","events_json":"https://pith.science/api/pith-number/OP2HFXPZXJ2FBYPHJ37EY57SSG/events.json","paper":"https://pith.science/paper/OP2HFXPZ"},"agent_actions":{"view_html":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG","download_json":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG.json","view_paper":"https://pith.science/paper/OP2HFXPZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0811.2484&json=true","fetch_graph":"https://pith.science/api/pith-number/OP2HFXPZXJ2FBYPHJ37EY57SSG/graph.json","fetch_events":"https://pith.science/api/pith-number/OP2HFXPZXJ2FBYPHJ37EY57SSG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG/action/storage_attestation","attest_author":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG/action/author_attestation","sign_citation":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG/action/citation_signature","submit_replication":"https://pith.science/pith/OP2HFXPZXJ2FBYPHJ37EY57SSG/action/replication_record"}},"created_at":"2026-07-04T17:13:39.508429+00:00","updated_at":"2026-07-04T17:13:39.508429+00:00"}