{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:HIXV2M7MYJQBXWQ3DKKIJPJSAI","short_pith_number":"pith:HIXV2M7M","schema_version":"1.0","canonical_sha256":"3a2f5d33ecc2601bda1b1a9484bd3202381b63747c7d7b248ea37b97e27ecdc3","source":{"kind":"arxiv","id":"astro-ph/0212214","version":2},"attestation_state":"computed","paper":{"title":"A radial mass profile analysis of the lensing cluster MS2137-23","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"B. Fort (IAP), M. Dantel-Fort (Obs. de Paris/LERMA), R. Gavazzi (IAP), R. Pello (OMP Toulouse), Y. Mellier (IAP; Obs. de Paris/LERMA)","submitted_at":"2002-12-09T20:39:31Z","abstract_excerpt":"We reanalyze the strong lens modeling of the cluster of galaxies MS2137-23 using a new data set obtained with the ESO VLT. We found the photometric redshifts of the two main arc systems are both at z=1.6. After subtraction of the central cD star light of the HST image we found that only one object lying underneath has the expected properties of the fifth image associated to the tangential arc. We improve the previous lens modelings of the central dark matter distribution of the cluster, using an isothermal model with a core (IS) and the NFW-like model with a cusp. Without the fifth image, the "},"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":"astro-ph/0212214","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-12-09T20:39:31Z","cross_cats_sorted":[],"title_canon_sha256":"c97fc8d20c7a1501bad95e5420dc637e2975ee0e7b1a92d094ae7e16e80fcf93","abstract_canon_sha256":"28f96082d7484616d5068e580611b3cf3c0b521d40ccc04591fc969b3f6cd175"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:31:23.069840Z","signature_b64":"yci/VPc/q7YBhqc0f5OSxwr5hZKRgx4s4fYJPO9IGoFYTcuQ3ISj8fuuO55Lm++lxfA8l+2HNTZbldif/vkOCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3a2f5d33ecc2601bda1b1a9484bd3202381b63747c7d7b248ea37b97e27ecdc3","last_reissued_at":"2026-07-04T16:31:23.069441Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:31:23.069441Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A radial mass profile analysis of the lensing cluster MS2137-23","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"B. Fort (IAP), M. Dantel-Fort (Obs. de Paris/LERMA), R. Gavazzi (IAP), R. Pello (OMP Toulouse), Y. Mellier (IAP; Obs. de Paris/LERMA)","submitted_at":"2002-12-09T20:39:31Z","abstract_excerpt":"We reanalyze the strong lens modeling of the cluster of galaxies MS2137-23 using a new data set obtained with the ESO VLT. We found the photometric redshifts of the two main arc systems are both at z=1.6. After subtraction of the central cD star light of the HST image we found that only one object lying underneath has the expected properties of the fifth image associated to the tangential arc. We improve the previous lens modelings of the central dark matter distribution of the cluster, using an isothermal model with a core (IS) and the NFW-like model with a cusp. Without the fifth image, the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0212214","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/astro-ph/0212214/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":"astro-ph/0212214","created_at":"2026-07-04T16:31:23.069498+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0212214v2","created_at":"2026-07-04T16:31:23.069498+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0212214","created_at":"2026-07-04T16:31:23.069498+00:00"},{"alias_kind":"pith_short_12","alias_value":"HIXV2M7MYJQB","created_at":"2026-07-04T16:31:23.069498+00:00"},{"alias_kind":"pith_short_16","alias_value":"HIXV2M7MYJQBXWQ3","created_at":"2026-07-04T16:31:23.069498+00:00"},{"alias_kind":"pith_short_8","alias_value":"HIXV2M7M","created_at":"2026-07-04T16:31:23.069498+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07750","citing_title":"Multi-Wavelength Signatures of a Giant Cometary Radio Halo in MACSJ0417-1154","ref_index":54,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI","json":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI.json","graph_json":"https://pith.science/api/pith-number/HIXV2M7MYJQBXWQ3DKKIJPJSAI/graph.json","events_json":"https://pith.science/api/pith-number/HIXV2M7MYJQBXWQ3DKKIJPJSAI/events.json","paper":"https://pith.science/paper/HIXV2M7M"},"agent_actions":{"view_html":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI","download_json":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI.json","view_paper":"https://pith.science/paper/HIXV2M7M","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0212214&json=true","fetch_graph":"https://pith.science/api/pith-number/HIXV2M7MYJQBXWQ3DKKIJPJSAI/graph.json","fetch_events":"https://pith.science/api/pith-number/HIXV2M7MYJQBXWQ3DKKIJPJSAI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI/action/storage_attestation","attest_author":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI/action/author_attestation","sign_citation":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI/action/citation_signature","submit_replication":"https://pith.science/pith/HIXV2M7MYJQBXWQ3DKKIJPJSAI/action/replication_record"}},"created_at":"2026-07-04T16:31:23.069498+00:00","updated_at":"2026-07-04T16:31:23.069498+00:00"}