{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:LO4V2SYZIBJO77QYWBRFBTUQ4E","short_pith_number":"pith:LO4V2SYZ","schema_version":"1.0","canonical_sha256":"5bb95d4b194052effe18b06250ce90e128e01061f22a7babd7ffac68be5a1d48","source":{"kind":"arxiv","id":"1201.0885","version":1},"attestation_state":"computed","paper":{"title":"Simulations of binary galaxy mergers and the link with Fast Rotators, Slow Rotators, and Kinematically Distinct Cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Anne-Marie Weijmans, Davor Krajnovi\\'c, Eric Emsellem, Fr\\'ed\\'eric Bournaud, Harald Kuntschner, Katherine Alatalo, Leo Blitz, Lisa M. Young, Marc Sarzi, Martin Bureau, Maxime Bois, Michele Cappellari, Nicholas Scott, Paolo Serra, Pierre-Alain Duc, Pierre-Yves Lablanche, P. T. de Zeeuw, Raffaella Morganti, Richard M. McDermid, Roger L. Davies, Sadegh Khochfar, Thorsten Naab, Timothy A. Davis, Tom Oosterloo","submitted_at":"2012-01-04T12:51:32Z","abstract_excerpt":"We study the formation of early-type galaxies (ETGs) through mergers with a sample of 70 high-resolution numerical simulations of binary mergers of disc galaxies. These simulations encompass various mass ratios, initial conditions and orbital parameters. We find that binary mergers of disc galaxies with mass ratios of 3:1 and 6:1 are nearly always classified as Fast Rotators according to the Atlas3D criterion: they preserve the structure of the input fast rotating spiral progenitors. Major disc mergers (mass ratios of 2:1 and 1:1) lead to both Fast and Slow Rotators. Most of the Slow Rotators "},"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":"1201.0885","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-01-04T12:51:32Z","cross_cats_sorted":[],"title_canon_sha256":"c6a6305cf63b49d1edffb4c2a4ae4b7ec5a85ae13b2ddd27bfe64f913a1ab914","abstract_canon_sha256":"2646240572a3509584bd5fac22c0288111e3c85eb05b852fd8151fe1bd9ffef1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:05:15.600252Z","signature_b64":"TtrJRsQQ7n4F1KyyErU6eki9Ioh4QQIjjF6sOzZ9qQxj2wqYUA3lpqnBuZHEcLlkIb0MazggIOj2bZTvdtWwCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5bb95d4b194052effe18b06250ce90e128e01061f22a7babd7ffac68be5a1d48","last_reissued_at":"2026-05-18T04:05:15.599641Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:05:15.599641Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulations of binary galaxy mergers and the link with Fast Rotators, Slow Rotators, and Kinematically Distinct Cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Anne-Marie Weijmans, Davor Krajnovi\\'c, Eric Emsellem, Fr\\'ed\\'eric Bournaud, Harald Kuntschner, Katherine Alatalo, Leo Blitz, Lisa M. Young, Marc Sarzi, Martin Bureau, Maxime Bois, Michele Cappellari, Nicholas Scott, Paolo Serra, Pierre-Alain Duc, Pierre-Yves Lablanche, P. T. de Zeeuw, Raffaella Morganti, Richard M. McDermid, Roger L. Davies, Sadegh Khochfar, Thorsten Naab, Timothy A. Davis, Tom Oosterloo","submitted_at":"2012-01-04T12:51:32Z","abstract_excerpt":"We study the formation of early-type galaxies (ETGs) through mergers with a sample of 70 high-resolution numerical simulations of binary mergers of disc galaxies. These simulations encompass various mass ratios, initial conditions and orbital parameters. We find that binary mergers of disc galaxies with mass ratios of 3:1 and 6:1 are nearly always classified as Fast Rotators according to the Atlas3D criterion: they preserve the structure of the input fast rotating spiral progenitors. Major disc mergers (mass ratios of 2:1 and 1:1) lead to both Fast and Slow Rotators. Most of the Slow Rotators "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1201.0885","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":"1201.0885","created_at":"2026-05-18T04:05:15.599769+00:00"},{"alias_kind":"arxiv_version","alias_value":"1201.0885v1","created_at":"2026-05-18T04:05:15.599769+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1201.0885","created_at":"2026-05-18T04:05:15.599769+00:00"},{"alias_kind":"pith_short_12","alias_value":"LO4V2SYZIBJO","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_16","alias_value":"LO4V2SYZIBJO77QY","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_8","alias_value":"LO4V2SYZ","created_at":"2026-05-18T12:27:14.488303+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/LO4V2SYZIBJO77QYWBRFBTUQ4E","json":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E.json","graph_json":"https://pith.science/api/pith-number/LO4V2SYZIBJO77QYWBRFBTUQ4E/graph.json","events_json":"https://pith.science/api/pith-number/LO4V2SYZIBJO77QYWBRFBTUQ4E/events.json","paper":"https://pith.science/paper/LO4V2SYZ"},"agent_actions":{"view_html":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E","download_json":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E.json","view_paper":"https://pith.science/paper/LO4V2SYZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1201.0885&json=true","fetch_graph":"https://pith.science/api/pith-number/LO4V2SYZIBJO77QYWBRFBTUQ4E/graph.json","fetch_events":"https://pith.science/api/pith-number/LO4V2SYZIBJO77QYWBRFBTUQ4E/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E/action/storage_attestation","attest_author":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E/action/author_attestation","sign_citation":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E/action/citation_signature","submit_replication":"https://pith.science/pith/LO4V2SYZIBJO77QYWBRFBTUQ4E/action/replication_record"}},"created_at":"2026-05-18T04:05:15.599769+00:00","updated_at":"2026-05-18T04:05:15.599769+00:00"}