{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:LRW6BIX7C67DLTJVW3PKZEDSY3","short_pith_number":"pith:LRW6BIX7","schema_version":"1.0","canonical_sha256":"5c6de0a2ff17be35cd35b6deac9072c6c4c499a9c7990beb7ff60f07c2634218","source":{"kind":"arxiv","id":"2206.07069","version":2},"attestation_state":"computed","paper":{"title":"The Response of Dark Matter Haloes to Gas Ejection: CuspCore II","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Avishai Dekel, Jonathan Freundlich, Nir Mandelker, Thibaut Fran\\c{c}ois, Zhaozhou Li","submitted_at":"2022-06-14T18:00:07Z","abstract_excerpt":"We propose an analytic model, CuspCore II, for the response of dark matter (DM) haloes to central gas ejection, as a mechanism for generating DM-deficient cores in dwarfs and high-z massive galaxies. We test this model and three other methods using idealized N-body simulations. The current model is physically justified and provides more accurate predictions than the earlier version, CuspCore I (Freundlich et al. 2020). The CuspCore model assumes an instantaneous change of potential, followed by a relaxation to a new Jeans equilibrium. The relaxation turns out to be violent relaxation during 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":"2206.07069","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-06-14T18:00:07Z","cross_cats_sorted":["astro-ph.CO","astro-ph.HE"],"title_canon_sha256":"965ab43d5d7f74775cf5cbefafd32b8f84f3630ef4d5e6e9490a7ef15daf86c8","abstract_canon_sha256":"288f60cc4009e3a11dba8140565e9fb7035c740839df20f0519ee326671a1be0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:58:51.021416Z","signature_b64":"+vg7lN7uJN3I4nVPCvebGNppBlckmFdJTetX4AIQ+LILx1ULmrA8Ss/AZZCtNoyH3wgoC0t0VygD31cd+kc5Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5c6de0a2ff17be35cd35b6deac9072c6c4c499a9c7990beb7ff60f07c2634218","last_reissued_at":"2026-07-05T05:58:51.020901Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:58:51.020901Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Response of Dark Matter Haloes to Gas Ejection: CuspCore II","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Avishai Dekel, Jonathan Freundlich, Nir Mandelker, Thibaut Fran\\c{c}ois, Zhaozhou Li","submitted_at":"2022-06-14T18:00:07Z","abstract_excerpt":"We propose an analytic model, CuspCore II, for the response of dark matter (DM) haloes to central gas ejection, as a mechanism for generating DM-deficient cores in dwarfs and high-z massive galaxies. We test this model and three other methods using idealized N-body simulations. The current model is physically justified and provides more accurate predictions than the earlier version, CuspCore I (Freundlich et al. 2020). The CuspCore model assumes an instantaneous change of potential, followed by a relaxation to a new Jeans equilibrium. The relaxation turns out to be violent relaxation during th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2206.07069","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2206.07069/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":"2206.07069","created_at":"2026-07-05T05:58:51.020961+00:00"},{"alias_kind":"arxiv_version","alias_value":"2206.07069v2","created_at":"2026-07-05T05:58:51.020961+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2206.07069","created_at":"2026-07-05T05:58:51.020961+00:00"},{"alias_kind":"pith_short_12","alias_value":"LRW6BIX7C67D","created_at":"2026-07-05T05:58:51.020961+00:00"},{"alias_kind":"pith_short_16","alias_value":"LRW6BIX7C67DLTJV","created_at":"2026-07-05T05:58:51.020961+00:00"},{"alias_kind":"pith_short_8","alias_value":"LRW6BIX7","created_at":"2026-07-05T05:58:51.020961+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.07470","citing_title":"Cosmological simulations of the same spiral galaxy: satellite properties, the role of baryonic physics and star formation history in shaping dark matter cores/cusps","ref_index":93,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3","json":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3.json","graph_json":"https://pith.science/api/pith-number/LRW6BIX7C67DLTJVW3PKZEDSY3/graph.json","events_json":"https://pith.science/api/pith-number/LRW6BIX7C67DLTJVW3PKZEDSY3/events.json","paper":"https://pith.science/paper/LRW6BIX7"},"agent_actions":{"view_html":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3","download_json":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3.json","view_paper":"https://pith.science/paper/LRW6BIX7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2206.07069&json=true","fetch_graph":"https://pith.science/api/pith-number/LRW6BIX7C67DLTJVW3PKZEDSY3/graph.json","fetch_events":"https://pith.science/api/pith-number/LRW6BIX7C67DLTJVW3PKZEDSY3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3/action/storage_attestation","attest_author":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3/action/author_attestation","sign_citation":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3/action/citation_signature","submit_replication":"https://pith.science/pith/LRW6BIX7C67DLTJVW3PKZEDSY3/action/replication_record"}},"created_at":"2026-07-05T05:58:51.020961+00:00","updated_at":"2026-07-05T05:58:51.020961+00:00"}