{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:JGPSZ5DBRCIGYOEPDV5ZJNQKRI","short_pith_number":"pith:JGPSZ5DB","schema_version":"1.0","canonical_sha256":"499f2cf46188906c388f1d7b94b60a8a02b94d6c78ba421060cc4ccccb80ed8c","source":{"kind":"arxiv","id":"1410.7175","version":1},"attestation_state":"computed","paper":{"title":"Dark matter inner slope and concentration in galaxies: from the Fornax dwarf to M87","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"(2) Dept of Physics & Astronomy, 3), (3) Univ. of California Observatories, (4) Dark Cosmology Centre, 5) ((1) IAP (UMR 7095, (5) KIPAC, A. J. Romanowsky (2, CNRS & UPMC), Copenhagen, G. A. Mamon (1), J. Chevalier (1), R. Wojtak (4, San Jos\\`e State University, Santa Cruz, Stanford University)","submitted_at":"2014-10-27T10:33:44Z","abstract_excerpt":"We apply two new state-of-the-art methods that model the distribution of observed tracers in projected phase space to lift the mass / velocity anisotropy (VA) degeneracy and deduce constraints on the mass profiles of galaxies, as well as their VA. We first show how a distribution function based method applied to the satellite kinematics of otherwise isolated SDSS galaxies shows convincing observational evidence of age matching: red galaxies have more concentrated dark matter (DM) halos than blue galaxies of the same stellar or halo mass. Then, applying the MAMPOSSt technique to M87 (traced by "},"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":"1410.7175","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-10-27T10:33:44Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"d0f916a18f36d97da83eea1d94a746844a347298e3d34b29d7eed7df71ecc24f","abstract_canon_sha256":"63825581f4520afe2c30b49a6912e91c240a14cdf09dcc99f9ca6953d005bebf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:30:35.178802Z","signature_b64":"jZ34hvj2Yj6Lyx9DjokveeQkgQEAlh6B0K35SSJDJVGZQbz0xn9cK+xdGu5/oqQMB+Hn1pKEC/X7rOw5jPokCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"499f2cf46188906c388f1d7b94b60a8a02b94d6c78ba421060cc4ccccb80ed8c","last_reissued_at":"2026-05-18T01:30:35.178062Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:30:35.178062Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dark matter inner slope and concentration in galaxies: from the Fornax dwarf to M87","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"(2) Dept of Physics & Astronomy, 3), (3) Univ. of California Observatories, (4) Dark Cosmology Centre, 5) ((1) IAP (UMR 7095, (5) KIPAC, A. J. Romanowsky (2, CNRS & UPMC), Copenhagen, G. A. Mamon (1), J. Chevalier (1), R. Wojtak (4, San Jos\\`e State University, Santa Cruz, Stanford University)","submitted_at":"2014-10-27T10:33:44Z","abstract_excerpt":"We apply two new state-of-the-art methods that model the distribution of observed tracers in projected phase space to lift the mass / velocity anisotropy (VA) degeneracy and deduce constraints on the mass profiles of galaxies, as well as their VA. We first show how a distribution function based method applied to the satellite kinematics of otherwise isolated SDSS galaxies shows convincing observational evidence of age matching: red galaxies have more concentrated dark matter (DM) halos than blue galaxies of the same stellar or halo mass. Then, applying the MAMPOSSt technique to M87 (traced by "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.7175","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":"1410.7175","created_at":"2026-05-18T01:30:35.178184+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.7175v1","created_at":"2026-05-18T01:30:35.178184+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.7175","created_at":"2026-05-18T01:30:35.178184+00:00"},{"alias_kind":"pith_short_12","alias_value":"JGPSZ5DBRCIG","created_at":"2026-05-18T12:28:33.132498+00:00"},{"alias_kind":"pith_short_16","alias_value":"JGPSZ5DBRCIGYOEP","created_at":"2026-05-18T12:28:33.132498+00:00"},{"alias_kind":"pith_short_8","alias_value":"JGPSZ5DB","created_at":"2026-05-18T12:28:33.132498+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/JGPSZ5DBRCIGYOEPDV5ZJNQKRI","json":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI.json","graph_json":"https://pith.science/api/pith-number/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/graph.json","events_json":"https://pith.science/api/pith-number/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/events.json","paper":"https://pith.science/paper/JGPSZ5DB"},"agent_actions":{"view_html":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI","download_json":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI.json","view_paper":"https://pith.science/paper/JGPSZ5DB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.7175&json=true","fetch_graph":"https://pith.science/api/pith-number/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/graph.json","fetch_events":"https://pith.science/api/pith-number/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/action/storage_attestation","attest_author":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/action/author_attestation","sign_citation":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/action/citation_signature","submit_replication":"https://pith.science/pith/JGPSZ5DBRCIGYOEPDV5ZJNQKRI/action/replication_record"}},"created_at":"2026-05-18T01:30:35.178184+00:00","updated_at":"2026-05-18T01:30:35.178184+00:00"}