{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:AMAFBYKC2NEORIEBW4EAZQGN5U","short_pith_number":"pith:AMAFBYKC","schema_version":"1.0","canonical_sha256":"030050e142d348e8a081b7080cc0cded0f07ad56db98b1f0d9841106e03eda93","source":{"kind":"arxiv","id":"2501.14868","version":1},"attestation_state":"computed","paper":{"title":"Theoretical Predictions for the Inner Dark Matter Distribution in the Milky Way Informed by Simulations","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"hep-ph","authors_text":"Abdelaziz Hussein, Andrew Wetzel, Justin I. Read, Lina Necib, Manoj Kaplinghat, Martin P. Rey, Oscar Agertz, Stacy Y. Kim","submitted_at":"2025-01-24T19:00:01Z","abstract_excerpt":"We build a theoretical range for the Milky Way's (MW) inner dark matter (DM) distribution informed by the FIRE-2, Auriga, VINTERGATAN-GM, and TNG50 simulation suites assuming the canonical cold dark matter (CDM) model. The DM density profiles in Auriga, VINTERGATAN-GM, and TNG50 can be approximately modeled using the adiabatic contraction prescription of Gnedin et al. 2004, while FIRE-2 has stronger baryonic feedback, leading to a departure from the adiabatic contraction model. The simulated halos that are adiabatically contracted are close to spherical (axis ratio $q \\in [0.75-0.9]$ at $5^\\ci"},"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":"2501.14868","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"hep-ph","submitted_at":"2025-01-24T19:00:01Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"d1d2d6b56065552f3382be4eb855f454087df0eb8440b902baec39cfbe1ca73c","abstract_canon_sha256":"e1397bd79aa4615ee64202655766fcb8f5ee2c52a1db81d09db4d1c1f7fdbd4e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:05:20.041285Z","signature_b64":"hxAtXiUUMyZkfS+xpICWvVRwKnjt4VGDT7EUTLXk5FBza3Dmcesi9ZknL+12AzuPjk+eFVU5k91kFp3oeJB2Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"030050e142d348e8a081b7080cc0cded0f07ad56db98b1f0d9841106e03eda93","last_reissued_at":"2026-07-05T10:05:20.040799Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:05:20.040799Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Theoretical Predictions for the Inner Dark Matter Distribution in the Milky Way Informed by Simulations","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"hep-ph","authors_text":"Abdelaziz Hussein, Andrew Wetzel, Justin I. Read, Lina Necib, Manoj Kaplinghat, Martin P. Rey, Oscar Agertz, Stacy Y. Kim","submitted_at":"2025-01-24T19:00:01Z","abstract_excerpt":"We build a theoretical range for the Milky Way's (MW) inner dark matter (DM) distribution informed by the FIRE-2, Auriga, VINTERGATAN-GM, and TNG50 simulation suites assuming the canonical cold dark matter (CDM) model. The DM density profiles in Auriga, VINTERGATAN-GM, and TNG50 can be approximately modeled using the adiabatic contraction prescription of Gnedin et al. 2004, while FIRE-2 has stronger baryonic feedback, leading to a departure from the adiabatic contraction model. The simulated halos that are adiabatically contracted are close to spherical (axis ratio $q \\in [0.75-0.9]$ at $5^\\ci"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2501.14868","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2501.14868/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":"2501.14868","created_at":"2026-07-05T10:05:20.040856+00:00"},{"alias_kind":"arxiv_version","alias_value":"2501.14868v1","created_at":"2026-07-05T10:05:20.040856+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2501.14868","created_at":"2026-07-05T10:05:20.040856+00:00"},{"alias_kind":"pith_short_12","alias_value":"AMAFBYKC2NEO","created_at":"2026-07-05T10:05:20.040856+00:00"},{"alias_kind":"pith_short_16","alias_value":"AMAFBYKC2NEORIEB","created_at":"2026-07-05T10:05:20.040856+00:00"},{"alias_kind":"pith_short_8","alias_value":"AMAFBYKC","created_at":"2026-07-05T10:05:20.040856+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.04633","citing_title":"A spectroscopic map of the Galactic centre: Integrated light and dynamical modelling","ref_index":42,"is_internal_anchor":false},{"citing_arxiv_id":"2509.08043","citing_title":"Testing Viability of Benchmark Dark Matter Models for the Galactic Center Excess","ref_index":26,"is_internal_anchor":false},{"citing_arxiv_id":"2512.03132","citing_title":"The DREAMS Project: Disentangling the Impact of Halo-to-Halo Variance and Baryonic Feedback on Milky Way Dark Matter Density Profiles","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04633","citing_title":"A spectroscopic map of the Galactic centre: Integrated light and dynamical modelling","ref_index":42,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04138","citing_title":"Galactic Amnesia: The Information Washout of the Milky Way Merger History","ref_index":75,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U","json":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U.json","graph_json":"https://pith.science/api/pith-number/AMAFBYKC2NEORIEBW4EAZQGN5U/graph.json","events_json":"https://pith.science/api/pith-number/AMAFBYKC2NEORIEBW4EAZQGN5U/events.json","paper":"https://pith.science/paper/AMAFBYKC"},"agent_actions":{"view_html":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U","download_json":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U.json","view_paper":"https://pith.science/paper/AMAFBYKC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2501.14868&json=true","fetch_graph":"https://pith.science/api/pith-number/AMAFBYKC2NEORIEBW4EAZQGN5U/graph.json","fetch_events":"https://pith.science/api/pith-number/AMAFBYKC2NEORIEBW4EAZQGN5U/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U/action/storage_attestation","attest_author":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U/action/author_attestation","sign_citation":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U/action/citation_signature","submit_replication":"https://pith.science/pith/AMAFBYKC2NEORIEBW4EAZQGN5U/action/replication_record"}},"created_at":"2026-07-05T10:05:20.040856+00:00","updated_at":"2026-07-05T10:05:20.040856+00:00"}