{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:3TG752NXD5P5JUEE4YXXK6IGYV","short_pith_number":"pith:3TG752NX","schema_version":"1.0","canonical_sha256":"dccdfee9b71f5fd4d084e62f757906c540ba1558354f72362e9dd775783bc325","source":{"kind":"arxiv","id":"2101.04045","version":2},"attestation_state":"computed","paper":{"title":"A population of heavily reddened, optically missed novae from Palomar Gattini-IR: Constraints on the Galactic nova rate","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Alexandre Delacroix, Aliya-Nur Babul, Anastasios Tzanidakis, Anna M. Moore, Ashish Mahabal, Ashot Bagdasaryan, Daniel McKenna, David Hale, Eran O. Ofek, Gokul Srinivasaragavan, Jacob E. Jencson, Jamie Soon, Jennifer L. Sokoloski, Kishalay De, Manasi Sharma, Mansi M. Kasliwal, Matthew J. Hankins, Michael C. B. Ashley, Richard Dekany, Roberto Soria, Roger M. Smith, Ryan M. Lau, Samaporn Tinyanont, Scott M. Adams, Timothee Greffe, Tony Travouillon, Viraj R. Karambelkar, Yuhan Yao","submitted_at":"2021-01-11T17:32:34Z","abstract_excerpt":"The nova rate in the Milky Way remains largely uncertain, despite its vital importance in constraining models of Galactic chemical evolution as well as understanding progenitor channels for Type Ia supernovae. The rate has been previously estimated in the range of $\\approx10-300$ yr$^{-1}$, either based on extrapolations from a handful of very bright optical novae or the nova rates in nearby galaxies; both methods are subject to debatable assumptions. The total discovery rate of optical novae remains much smaller ($\\approx5-10$ yr$^{-1}$) than these estimates, even with the advent of all-sky o"},"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":"2101.04045","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-01-11T17:32:34Z","cross_cats_sorted":["astro-ph.GA","astro-ph.SR"],"title_canon_sha256":"50420766641480702593395e39ad436737d106dac03350ec50aa30f883d4bdd0","abstract_canon_sha256":"dba634ab8bc034d0555d1fb7b34a31b880153b891da6c196f55cccdbeca44edb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:39:10.942204Z","signature_b64":"2FjFtF5tfAKlCvzy3l1QuEH61T18ETc2XZY0+KXmewb0xNtCVzHF22bWVd5BeYBExm9zglZM/y0b6J+FtrOACw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dccdfee9b71f5fd4d084e62f757906c540ba1558354f72362e9dd775783bc325","last_reissued_at":"2026-07-05T02:39:10.941678Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:39:10.941678Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A population of heavily reddened, optically missed novae from Palomar Gattini-IR: Constraints on the Galactic nova rate","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Alexandre Delacroix, Aliya-Nur Babul, Anastasios Tzanidakis, Anna M. Moore, Ashish Mahabal, Ashot Bagdasaryan, Daniel McKenna, David Hale, Eran O. Ofek, Gokul Srinivasaragavan, Jacob E. Jencson, Jamie Soon, Jennifer L. Sokoloski, Kishalay De, Manasi Sharma, Mansi M. Kasliwal, Matthew J. Hankins, Michael C. B. Ashley, Richard Dekany, Roberto Soria, Roger M. Smith, Ryan M. Lau, Samaporn Tinyanont, Scott M. Adams, Timothee Greffe, Tony Travouillon, Viraj R. Karambelkar, Yuhan Yao","submitted_at":"2021-01-11T17:32:34Z","abstract_excerpt":"The nova rate in the Milky Way remains largely uncertain, despite its vital importance in constraining models of Galactic chemical evolution as well as understanding progenitor channels for Type Ia supernovae. The rate has been previously estimated in the range of $\\approx10-300$ yr$^{-1}$, either based on extrapolations from a handful of very bright optical novae or the nova rates in nearby galaxies; both methods are subject to debatable assumptions. The total discovery rate of optical novae remains much smaller ($\\approx5-10$ yr$^{-1}$) than these estimates, even with the advent of all-sky o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2101.04045","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2101.04045/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":"2101.04045","created_at":"2026-07-05T02:39:10.941749+00:00"},{"alias_kind":"arxiv_version","alias_value":"2101.04045v2","created_at":"2026-07-05T02:39:10.941749+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2101.04045","created_at":"2026-07-05T02:39:10.941749+00:00"},{"alias_kind":"pith_short_12","alias_value":"3TG752NXD5P5","created_at":"2026-07-05T02:39:10.941749+00:00"},{"alias_kind":"pith_short_16","alias_value":"3TG752NXD5P5JUEE","created_at":"2026-07-05T02:39:10.941749+00:00"},{"alias_kind":"pith_short_8","alias_value":"3TG752NX","created_at":"2026-07-05T02:39:10.941749+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/3TG752NXD5P5JUEE4YXXK6IGYV","json":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV.json","graph_json":"https://pith.science/api/pith-number/3TG752NXD5P5JUEE4YXXK6IGYV/graph.json","events_json":"https://pith.science/api/pith-number/3TG752NXD5P5JUEE4YXXK6IGYV/events.json","paper":"https://pith.science/paper/3TG752NX"},"agent_actions":{"view_html":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV","download_json":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV.json","view_paper":"https://pith.science/paper/3TG752NX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2101.04045&json=true","fetch_graph":"https://pith.science/api/pith-number/3TG752NXD5P5JUEE4YXXK6IGYV/graph.json","fetch_events":"https://pith.science/api/pith-number/3TG752NXD5P5JUEE4YXXK6IGYV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV/action/storage_attestation","attest_author":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV/action/author_attestation","sign_citation":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV/action/citation_signature","submit_replication":"https://pith.science/pith/3TG752NXD5P5JUEE4YXXK6IGYV/action/replication_record"}},"created_at":"2026-07-05T02:39:10.941749+00:00","updated_at":"2026-07-05T02:39:10.941749+00:00"}