{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:V4B6J6WARIUPLX6VGIBM5W7FEN","short_pith_number":"pith:V4B6J6WA","schema_version":"1.0","canonical_sha256":"af03e4fac08a28f5dfd53202cedbe5237de1a0ff54edaf684e70296851c22bee","source":{"kind":"arxiv","id":"1306.0898","version":2},"attestation_state":"computed","paper":{"title":"The dependence of dark matter profiles on the stellar to halo mass ratio: a prediction for cusps vs cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Aaron A. Dutton, Alexander Knebe, Andrea V. Maccio, Arianna Di Cintio, Chris B. Brook, Greg S. Stinson, James Wadsley","submitted_at":"2013-06-04T20:00:01Z","abstract_excerpt":"We use 31 simulated galaxies from the MaGICC project to investigate the effects of baryonic feedback on the density profiles of dark matter (DM) haloes. The sample covers a wide mass range: 9.4e9<Mhalo/Msun<7.8e11, hosting galaxies with stellar masses: 5.0e5<M*/Msun<8.3e10, i.e. from dwarf to L*. The galaxies are simulated with several baryonic prescriptions, including a range of stellar feedbacks. The main result is a clear dependence of the inner slope of the DM density profile, \\alpha\\ in \\rho r^\\alpha, on the ratio between stellar-to-halo mass (M*/Mhalo). This relation is independent of th"},"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":"1306.0898","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-06-04T20:00:01Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"8769fc66e7f095a9482874bb6f31858033739c1c6c3140e8c79d6c0b23aa921d","abstract_canon_sha256":"087ed6554d4bb23f39e5e3434f54998ccce0ff6f30e8396c28784953d0391657"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:49:32.912646Z","signature_b64":"NKyJh+rZEEExgB/8CBb/66ggD6UXPGducN8xrJvl3eKjLBHpP/M13RL2iPnNyck/xmRzPXa11V65JkIefBvpBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"af03e4fac08a28f5dfd53202cedbe5237de1a0ff54edaf684e70296851c22bee","last_reissued_at":"2026-05-18T01:49:32.912239Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:49:32.912239Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The dependence of dark matter profiles on the stellar to halo mass ratio: a prediction for cusps vs cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Aaron A. Dutton, Alexander Knebe, Andrea V. Maccio, Arianna Di Cintio, Chris B. Brook, Greg S. Stinson, James Wadsley","submitted_at":"2013-06-04T20:00:01Z","abstract_excerpt":"We use 31 simulated galaxies from the MaGICC project to investigate the effects of baryonic feedback on the density profiles of dark matter (DM) haloes. The sample covers a wide mass range: 9.4e9<Mhalo/Msun<7.8e11, hosting galaxies with stellar masses: 5.0e5<M*/Msun<8.3e10, i.e. from dwarf to L*. The galaxies are simulated with several baryonic prescriptions, including a range of stellar feedbacks. The main result is a clear dependence of the inner slope of the DM density profile, \\alpha\\ in \\rho r^\\alpha, on the ratio between stellar-to-halo mass (M*/Mhalo). This relation is independent of th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1306.0898","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":"1306.0898","created_at":"2026-05-18T01:49:32.912305+00:00"},{"alias_kind":"arxiv_version","alias_value":"1306.0898v2","created_at":"2026-05-18T01:49:32.912305+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1306.0898","created_at":"2026-05-18T01:49:32.912305+00:00"},{"alias_kind":"pith_short_12","alias_value":"V4B6J6WARIUP","created_at":"2026-05-18T12:28:02.375192+00:00"},{"alias_kind":"pith_short_16","alias_value":"V4B6J6WARIUPLX6V","created_at":"2026-05-18T12:28:02.375192+00:00"},{"alias_kind":"pith_short_8","alias_value":"V4B6J6WA","created_at":"2026-05-18T12:28:02.375192+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/V4B6J6WARIUPLX6VGIBM5W7FEN","json":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN.json","graph_json":"https://pith.science/api/pith-number/V4B6J6WARIUPLX6VGIBM5W7FEN/graph.json","events_json":"https://pith.science/api/pith-number/V4B6J6WARIUPLX6VGIBM5W7FEN/events.json","paper":"https://pith.science/paper/V4B6J6WA"},"agent_actions":{"view_html":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN","download_json":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN.json","view_paper":"https://pith.science/paper/V4B6J6WA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1306.0898&json=true","fetch_graph":"https://pith.science/api/pith-number/V4B6J6WARIUPLX6VGIBM5W7FEN/graph.json","fetch_events":"https://pith.science/api/pith-number/V4B6J6WARIUPLX6VGIBM5W7FEN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN/action/storage_attestation","attest_author":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN/action/author_attestation","sign_citation":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN/action/citation_signature","submit_replication":"https://pith.science/pith/V4B6J6WARIUPLX6VGIBM5W7FEN/action/replication_record"}},"created_at":"2026-05-18T01:49:32.912305+00:00","updated_at":"2026-05-18T01:49:32.912305+00:00"}