{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:IZJGQYXBVBVN2564HTYDDXBCYC","short_pith_number":"pith:IZJGQYXB","schema_version":"1.0","canonical_sha256":"46526862e1a86add77dc3cf031dc22c0bf4e6b1e477eea0c8389b2ef2b344317","source":{"kind":"arxiv","id":"1611.09023","version":2},"attestation_state":"computed","paper":{"title":"Separation of Stellar Populations by an Evolving Bar: Implications for the Bulge of the Milky Way","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Dante Minniti, K. Freeman, Manuela Zoccali, Melissa Ness, Oscar A. Gonzalez, Victor P. Debattista","submitted_at":"2016-11-28T08:39:04Z","abstract_excerpt":"We present a novel interpretation of the previously puzzling different behaviours of stellar populations of the Milky Way's bulge. We first show, by means of pure N-body simulations, that initially co-spatial stellar populations with different in-plane random motions separate when a bar forms. The radially cooler populations form a strong bar, and are vertically thin and peanut-shaped, while the hotter populations form a weaker bar and become a vertically thicker box. We demonstrate that it is the radial, not the vertical, velocity dispersion that dominates this evolution. Assuming that early "},"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":"1611.09023","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-11-28T08:39:04Z","cross_cats_sorted":[],"title_canon_sha256":"abd525dd652ec1b52b1801afc619d7223591651fc68c0c14ffb37c7da6f081e4","abstract_canon_sha256":"5df60c02fd0b0a5d5bc803e817a71d4fa283af23ad44997320a067621f334f8d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:42:51.444293Z","signature_b64":"yHHqDjQuEmVt84Ylp+MsHsVJH23UQRD51ldErriwdruONpem1MbM8EctLGXd5hFDMeA2pK9cwf4mtrRY+4cZAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"46526862e1a86add77dc3cf031dc22c0bf4e6b1e477eea0c8389b2ef2b344317","last_reissued_at":"2026-05-18T00:42:51.443549Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:42:51.443549Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Separation of Stellar Populations by an Evolving Bar: Implications for the Bulge of the Milky Way","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Dante Minniti, K. Freeman, Manuela Zoccali, Melissa Ness, Oscar A. Gonzalez, Victor P. Debattista","submitted_at":"2016-11-28T08:39:04Z","abstract_excerpt":"We present a novel interpretation of the previously puzzling different behaviours of stellar populations of the Milky Way's bulge. We first show, by means of pure N-body simulations, that initially co-spatial stellar populations with different in-plane random motions separate when a bar forms. The radially cooler populations form a strong bar, and are vertically thin and peanut-shaped, while the hotter populations form a weaker bar and become a vertically thicker box. We demonstrate that it is the radial, not the vertical, velocity dispersion that dominates this evolution. Assuming that early "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1611.09023","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":"1611.09023","created_at":"2026-05-18T00:42:51.443680+00:00"},{"alias_kind":"arxiv_version","alias_value":"1611.09023v2","created_at":"2026-05-18T00:42:51.443680+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1611.09023","created_at":"2026-05-18T00:42:51.443680+00:00"},{"alias_kind":"pith_short_12","alias_value":"IZJGQYXBVBVN","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_16","alias_value":"IZJGQYXBVBVN2564","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_8","alias_value":"IZJGQYXB","created_at":"2026-05-18T12:30:22.444734+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.00077","citing_title":"Hot or Cold? Radial Redistribution of Stars in FIRE Simulations of Milky Way-Mass Galaxies and the Asymmetry of Inward versus Outward Migrators","ref_index":261,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC","json":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC.json","graph_json":"https://pith.science/api/pith-number/IZJGQYXBVBVN2564HTYDDXBCYC/graph.json","events_json":"https://pith.science/api/pith-number/IZJGQYXBVBVN2564HTYDDXBCYC/events.json","paper":"https://pith.science/paper/IZJGQYXB"},"agent_actions":{"view_html":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC","download_json":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC.json","view_paper":"https://pith.science/paper/IZJGQYXB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1611.09023&json=true","fetch_graph":"https://pith.science/api/pith-number/IZJGQYXBVBVN2564HTYDDXBCYC/graph.json","fetch_events":"https://pith.science/api/pith-number/IZJGQYXBVBVN2564HTYDDXBCYC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC/action/storage_attestation","attest_author":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC/action/author_attestation","sign_citation":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC/action/citation_signature","submit_replication":"https://pith.science/pith/IZJGQYXBVBVN2564HTYDDXBCYC/action/replication_record"}},"created_at":"2026-05-18T00:42:51.443680+00:00","updated_at":"2026-05-18T00:42:51.443680+00:00"}