{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:ZMCE2AD3RMXGEV6Q6SHQY6WDB6","short_pith_number":"pith:ZMCE2AD3","schema_version":"1.0","canonical_sha256":"cb044d007b8b2e6257d0f48f0c7ac30faa0800dcf5bd5ca69143d78dab15b6ae","source":{"kind":"arxiv","id":"1612.05565","version":1},"attestation_state":"computed","paper":{"title":"Inferring Gravitational Potentials from Mass Densities in Cluster-sized Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alejo Stark, Christopher J. Miller, Daniel Gifford, Nicholas Kern (University of Michigan)","submitted_at":"2016-12-16T17:29:19Z","abstract_excerpt":"We use N-body simulations to quantify how the escape velocity in cluster-sized halos maps to the gravitational potential in a LambdaCDM universe. Using spherical density-potential pairs and the Poisson equation, we find that the matter density inferred gravitational potential profile predicts the escape velocity profile to within a few percent accuracy for group and cluster-sized halos (10^13 < M_200 < 10^15 M_sun, with respect to the critical density). The accuracy holds from just outside the core to beyond the virial radius. We show the importance of explicitly incorporating a cosmological c"},"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":"1612.05565","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-12-16T17:29:19Z","cross_cats_sorted":[],"title_canon_sha256":"f02350db8583b8061c5fdd27e13a775a1fde1975a8d5833b72ca88ec2c9b65fd","abstract_canon_sha256":"c1f9d0306f5266b9ef2ce168ceafff94be4570ec656d067e0125297c863f30e5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:54:51.530956Z","signature_b64":"MDa4B/xN5I0hu6xFSWS/Pk+CWiX+OXtlbc83UjnPSolYwNU89VfAy1ze2CEmgFgeYSR4lky0Lai6isdrhLMpDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cb044d007b8b2e6257d0f48f0c7ac30faa0800dcf5bd5ca69143d78dab15b6ae","last_reissued_at":"2026-05-18T00:54:51.530522Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:54:51.530522Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Inferring Gravitational Potentials from Mass Densities in Cluster-sized Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alejo Stark, Christopher J. Miller, Daniel Gifford, Nicholas Kern (University of Michigan)","submitted_at":"2016-12-16T17:29:19Z","abstract_excerpt":"We use N-body simulations to quantify how the escape velocity in cluster-sized halos maps to the gravitational potential in a LambdaCDM universe. Using spherical density-potential pairs and the Poisson equation, we find that the matter density inferred gravitational potential profile predicts the escape velocity profile to within a few percent accuracy for group and cluster-sized halos (10^13 < M_200 < 10^15 M_sun, with respect to the critical density). The accuracy holds from just outside the core to beyond the virial radius. We show the importance of explicitly incorporating a cosmological c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1612.05565","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":""},"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":"1612.05565","created_at":"2026-05-18T00:54:51.530589+00:00"},{"alias_kind":"arxiv_version","alias_value":"1612.05565v1","created_at":"2026-05-18T00:54:51.530589+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1612.05565","created_at":"2026-05-18T00:54:51.530589+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZMCE2AD3RMXG","created_at":"2026-05-18T12:30:53.716459+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZMCE2AD3RMXGEV6Q","created_at":"2026-05-18T12:30:53.716459+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZMCE2AD3","created_at":"2026-05-18T12:30:53.716459+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21598","citing_title":"Advancing the detection of low surface brightness galaxies. I. ATTILA: multi-tAsking deTecTIon tool for Lsb gAlaxies","ref_index":22,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6","json":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6.json","graph_json":"https://pith.science/api/pith-number/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/graph.json","events_json":"https://pith.science/api/pith-number/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/events.json","paper":"https://pith.science/paper/ZMCE2AD3"},"agent_actions":{"view_html":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6","download_json":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6.json","view_paper":"https://pith.science/paper/ZMCE2AD3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1612.05565&json=true","fetch_graph":"https://pith.science/api/pith-number/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/graph.json","fetch_events":"https://pith.science/api/pith-number/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/action/storage_attestation","attest_author":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/action/author_attestation","sign_citation":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/action/citation_signature","submit_replication":"https://pith.science/pith/ZMCE2AD3RMXGEV6Q6SHQY6WDB6/action/replication_record"}},"created_at":"2026-05-18T00:54:51.530589+00:00","updated_at":"2026-05-18T00:54:51.530589+00:00"}