{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:VM4NPFNNO3ZGQSBIDPZNP3ZSBZ","short_pith_number":"pith:VM4NPFNN","schema_version":"1.0","canonical_sha256":"ab38d795ad76f26848281bf2d7ef320e6ecb9ec6d187a3d5e00a972e9e6af574","source":{"kind":"arxiv","id":"1409.8617","version":3},"attestation_state":"computed","paper":{"title":"Baryon effects on the internal structure of LCDM halos in the EAGLE simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"(2) Leiden, (3) Liverpool, (4) Tenerife), Adrian Jenkins (1), Carlos S. Frenk (1), Claudio Dalla Vecchia (3), Durham, I. G. McCarthy (4) ((1) ICC, Joop Schaye (2), Matthieu Schaller (1), Michelle Furlong (1), Richard G. Bower (1), Robert A. Crain (2), Tom Theuns (1)","submitted_at":"2014-09-30T16:24:57Z","abstract_excerpt":"We investigate the internal structure and density profiles of halos of mass $10^{10}-10^{14}~M_\\odot$ in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations. These follow the formation of galaxies in a $\\Lambda$CDM Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time. We find significant differences between the masses of halos in the EAGLE simulations and in simulations that "},"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":"1409.8617","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-09-30T16:24:57Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"984a6da9cea5c7f24b1fdec79483400e5204303eeb907de3917c4fd5460a47b8","abstract_canon_sha256":"d3446ad4e22b355c3bb99bb70f4f64cea33d1a45189f58b79247d632e101a977"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:37:23.382379Z","signature_b64":"iCzYIjRbZyMEsB3jblifWN8//DI0CrCJCJLDRdCxkcibdJcDin/rvKAIC3aRu2R9QImKzpygMUE3tS2zgOT9Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ab38d795ad76f26848281bf2d7ef320e6ecb9ec6d187a3d5e00a972e9e6af574","last_reissued_at":"2026-05-18T01:37:23.381545Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:37:23.381545Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Baryon effects on the internal structure of LCDM halos in the EAGLE simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"(2) Leiden, (3) Liverpool, (4) Tenerife), Adrian Jenkins (1), Carlos S. Frenk (1), Claudio Dalla Vecchia (3), Durham, I. G. McCarthy (4) ((1) ICC, Joop Schaye (2), Matthieu Schaller (1), Michelle Furlong (1), Richard G. Bower (1), Robert A. Crain (2), Tom Theuns (1)","submitted_at":"2014-09-30T16:24:57Z","abstract_excerpt":"We investigate the internal structure and density profiles of halos of mass $10^{10}-10^{14}~M_\\odot$ in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations. These follow the formation of galaxies in a $\\Lambda$CDM Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time. We find significant differences between the masses of halos in the EAGLE simulations and in simulations that "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1409.8617","kind":"arxiv","version":3},"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":"1409.8617","created_at":"2026-05-18T01:37:23.381698+00:00"},{"alias_kind":"arxiv_version","alias_value":"1409.8617v3","created_at":"2026-05-18T01:37:23.381698+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1409.8617","created_at":"2026-05-18T01:37:23.381698+00:00"},{"alias_kind":"pith_short_12","alias_value":"VM4NPFNNO3ZG","created_at":"2026-05-18T12:28:54.890064+00:00"},{"alias_kind":"pith_short_16","alias_value":"VM4NPFNNO3ZGQSBI","created_at":"2026-05-18T12:28:54.890064+00:00"},{"alias_kind":"pith_short_8","alias_value":"VM4NPFNN","created_at":"2026-05-18T12:28:54.890064+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":23,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ","json":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ.json","graph_json":"https://pith.science/api/pith-number/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/graph.json","events_json":"https://pith.science/api/pith-number/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/events.json","paper":"https://pith.science/paper/VM4NPFNN"},"agent_actions":{"view_html":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ","download_json":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ.json","view_paper":"https://pith.science/paper/VM4NPFNN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1409.8617&json=true","fetch_graph":"https://pith.science/api/pith-number/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/graph.json","fetch_events":"https://pith.science/api/pith-number/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/action/storage_attestation","attest_author":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/action/author_attestation","sign_citation":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/action/citation_signature","submit_replication":"https://pith.science/pith/VM4NPFNNO3ZGQSBIDPZNP3ZSBZ/action/replication_record"}},"created_at":"2026-05-18T01:37:23.381698+00:00","updated_at":"2026-05-18T01:37:23.381698+00:00"}