{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:E3MPIAWTQCYUB6ZKMAOOKCOC27","short_pith_number":"pith:E3MPIAWT","schema_version":"1.0","canonical_sha256":"26d8f402d380b140fb2a601ce509c2d7faeb919e18185e1b0781528a1d071009","source":{"kind":"arxiv","id":"1408.0731","version":2},"attestation_state":"computed","paper":{"title":"The Type IIb SN 2011dh - Two years of observations and modelling of the lightcurves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Jerkstrand, A. Pastorello, C. Fransson, G. Helou, J. Maund, J. Sollerman, J. Spyromilio, L. Tomasella, M. Ergon, M. Fraser, M.M. Kasliwal, N. Elias-Rosa, R. Kotak, S. Benetti, S.J. Smartt, S. Taubenberger, S. Valenti","submitted_at":"2014-08-04T16:10:51Z","abstract_excerpt":"We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models and a bolometric correction determined with steady-state NLTE modelling. Using this method we find a helium core mass of 3.1 (+0.7-0.4) solar masses for SN 2011dh, consistent within"},"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":"1408.0731","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-08-04T16:10:51Z","cross_cats_sorted":[],"title_canon_sha256":"044b9bed3eae9f799e2926684abeaa2db60ae686fe4dd7d37e6fea1698fe4d98","abstract_canon_sha256":"5f1a902252eca28fa673389c5bcd6e17276226a5b506abd2ffbf2e482a92b4ef"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:33:49.167060Z","signature_b64":"cfiOaFRL6Qb6OOPfql0mwlSYpFc4k8DbIRlSNMm2Hjvr4aKymseoh/SbAGRT+8+HzCn5m5UkFLYYo2fsCZU8DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"26d8f402d380b140fb2a601ce509c2d7faeb919e18185e1b0781528a1d071009","last_reissued_at":"2026-05-18T01:33:49.166450Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:33:49.166450Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Type IIb SN 2011dh - Two years of observations and modelling of the lightcurves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Jerkstrand, A. Pastorello, C. Fransson, G. Helou, J. Maund, J. Sollerman, J. Spyromilio, L. Tomasella, M. Ergon, M. Fraser, M.M. Kasliwal, N. Elias-Rosa, R. Kotak, S. Benetti, S.J. Smartt, S. Taubenberger, S. Valenti","submitted_at":"2014-08-04T16:10:51Z","abstract_excerpt":"We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models and a bolometric correction determined with steady-state NLTE modelling. Using this method we find a helium core mass of 3.1 (+0.7-0.4) solar masses for SN 2011dh, consistent within"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1408.0731","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":"1408.0731","created_at":"2026-05-18T01:33:49.166540+00:00"},{"alias_kind":"arxiv_version","alias_value":"1408.0731v2","created_at":"2026-05-18T01:33:49.166540+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1408.0731","created_at":"2026-05-18T01:33:49.166540+00:00"},{"alias_kind":"pith_short_12","alias_value":"E3MPIAWTQCYU","created_at":"2026-05-18T12:28:25.294606+00:00"},{"alias_kind":"pith_short_16","alias_value":"E3MPIAWTQCYUB6ZK","created_at":"2026-05-18T12:28:25.294606+00:00"},{"alias_kind":"pith_short_8","alias_value":"E3MPIAWT","created_at":"2026-05-18T12:28:25.294606+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21062","citing_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","ref_index":135,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27","json":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27.json","graph_json":"https://pith.science/api/pith-number/E3MPIAWTQCYUB6ZKMAOOKCOC27/graph.json","events_json":"https://pith.science/api/pith-number/E3MPIAWTQCYUB6ZKMAOOKCOC27/events.json","paper":"https://pith.science/paper/E3MPIAWT"},"agent_actions":{"view_html":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27","download_json":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27.json","view_paper":"https://pith.science/paper/E3MPIAWT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1408.0731&json=true","fetch_graph":"https://pith.science/api/pith-number/E3MPIAWTQCYUB6ZKMAOOKCOC27/graph.json","fetch_events":"https://pith.science/api/pith-number/E3MPIAWTQCYUB6ZKMAOOKCOC27/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27/action/timestamp_anchor","attest_storage":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27/action/storage_attestation","attest_author":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27/action/author_attestation","sign_citation":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27/action/citation_signature","submit_replication":"https://pith.science/pith/E3MPIAWTQCYUB6ZKMAOOKCOC27/action/replication_record"}},"created_at":"2026-05-18T01:33:49.166540+00:00","updated_at":"2026-05-18T01:33:49.166540+00:00"}