{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:TW53OE3DLWKK5ZF5QBI66I4OSI","short_pith_number":"pith:TW53OE3D","schema_version":"1.0","canonical_sha256":"9dbbb713635d94aee4bd8051ef238e92064e8a5b319ad486f5651d07c4ca0edd","source":{"kind":"arxiv","id":"2506.02748","version":1},"attestation_state":"computed","paper":{"title":"MINDS: The very low-mass star and brown dwarf sample. Detections and trends in the inner disk gas","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"A. Caratti o Garatti, A. D. Sellek, A. M. Arabhavi, B. Tabone, D. Barrado, D. Gasman, E. F. van Dishoeck, F. Lahuis, G. Perotti, H. Jang, I. Kamp, I. Pascucci, J. Kanwar, K. Schwarz, L. B. F. M. Waters, M. G\\\"udel, M. Morales-Calder\\'on, M. Temmink, M. Vlasblom, P.-O. Lagage, P. Patapis, S. L. Grant, Th. Henning, T. Kaeufer, V. Christiaens","submitted_at":"2025-06-03T11:11:27Z","abstract_excerpt":"Planet-forming disks around brown dwarfs and very low-mass stars (VLMS) are on average less massive and are expected to undergo faster radial solid transport than their higher mass counterparts. Spitzer had detected C$_2$H$_2$, CO$_2$ and HCN around these objects. With better sensitivity and spectral resolving power, JWST recently revealed incredibly carbon-rich spectra from such disks. A study of a larger sample of objects is necessary to understand how common such carbon-rich inner disk regions are and to put constraints on their evolution. We present and analyze MIRI observations of 10 disk"},"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":"2506.02748","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2025-06-03T11:11:27Z","cross_cats_sorted":["astro-ph.GA","astro-ph.SR"],"title_canon_sha256":"d5f891e17d6472f11cb42454aeb6b329f1c307400b8d950dd4bd0e8bdf641a64","abstract_canon_sha256":"b773091b7171ba6e0455a482809df2f02627d684b03a83c922bc5a57a61649c7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:33:52.080414Z","signature_b64":"CLy4GtKEkGlQiYIh0jY9/IhZJdrz8kTCLgO8EHvx/Lj8uirt/G9+FJTjT5CaPMYTnEah+nmhGrBSsCYCk4mwAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9dbbb713635d94aee4bd8051ef238e92064e8a5b319ad486f5651d07c4ca0edd","last_reissued_at":"2026-07-05T11:33:52.079908Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:33:52.079908Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"MINDS: The very low-mass star and brown dwarf sample. Detections and trends in the inner disk gas","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"A. Caratti o Garatti, A. D. Sellek, A. M. Arabhavi, B. Tabone, D. Barrado, D. Gasman, E. F. van Dishoeck, F. Lahuis, G. Perotti, H. Jang, I. Kamp, I. Pascucci, J. Kanwar, K. Schwarz, L. B. F. M. Waters, M. G\\\"udel, M. Morales-Calder\\'on, M. Temmink, M. Vlasblom, P.-O. Lagage, P. Patapis, S. L. Grant, Th. Henning, T. Kaeufer, V. Christiaens","submitted_at":"2025-06-03T11:11:27Z","abstract_excerpt":"Planet-forming disks around brown dwarfs and very low-mass stars (VLMS) are on average less massive and are expected to undergo faster radial solid transport than their higher mass counterparts. Spitzer had detected C$_2$H$_2$, CO$_2$ and HCN around these objects. With better sensitivity and spectral resolving power, JWST recently revealed incredibly carbon-rich spectra from such disks. A study of a larger sample of objects is necessary to understand how common such carbon-rich inner disk regions are and to put constraints on their evolution. We present and analyze MIRI observations of 10 disk"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2506.02748","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/2506.02748/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":"2506.02748","created_at":"2026-07-05T11:33:52.079968+00:00"},{"alias_kind":"arxiv_version","alias_value":"2506.02748v1","created_at":"2026-07-05T11:33:52.079968+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2506.02748","created_at":"2026-07-05T11:33:52.079968+00:00"},{"alias_kind":"pith_short_12","alias_value":"TW53OE3DLWKK","created_at":"2026-07-05T11:33:52.079968+00:00"},{"alias_kind":"pith_short_16","alias_value":"TW53OE3DLWKK5ZF5","created_at":"2026-07-05T11:33:52.079968+00:00"},{"alias_kind":"pith_short_8","alias_value":"TW53OE3D","created_at":"2026-07-05T11:33:52.079968+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.21803","citing_title":"MINDS: Intertwined evolution of dust and gas in large planet-forming disks. A diversity driven by halted pebble drift?","ref_index":1,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI","json":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI.json","graph_json":"https://pith.science/api/pith-number/TW53OE3DLWKK5ZF5QBI66I4OSI/graph.json","events_json":"https://pith.science/api/pith-number/TW53OE3DLWKK5ZF5QBI66I4OSI/events.json","paper":"https://pith.science/paper/TW53OE3D"},"agent_actions":{"view_html":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI","download_json":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI.json","view_paper":"https://pith.science/paper/TW53OE3D","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2506.02748&json=true","fetch_graph":"https://pith.science/api/pith-number/TW53OE3DLWKK5ZF5QBI66I4OSI/graph.json","fetch_events":"https://pith.science/api/pith-number/TW53OE3DLWKK5ZF5QBI66I4OSI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI/action/storage_attestation","attest_author":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI/action/author_attestation","sign_citation":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI/action/citation_signature","submit_replication":"https://pith.science/pith/TW53OE3DLWKK5ZF5QBI66I4OSI/action/replication_record"}},"created_at":"2026-07-05T11:33:52.079968+00:00","updated_at":"2026-07-05T11:33:52.079968+00:00"}