{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:GHHBY27EW4I7AVT2IYXJ6P4TVN","short_pith_number":"pith:GHHBY27E","schema_version":"1.0","canonical_sha256":"31ce1c6be4b711f0567a462e9f3f93ab77454f2979df3dcb3117ef2b1c3dc4bd","source":{"kind":"arxiv","id":"0709.1950","version":1},"attestation_state":"computed","paper":{"title":"The XMM-LSS survey: the Class 1 cluster sample over the initial 5 square degrees and its cosmological modelling","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Detal, A. Gueguen, A. Mazure, A. Refregier, B. Altieri, C. Adami, C. Jean, C. Libbrecht, D. Alloin, D. Maccagni, D. Proust, F. Pacaud, G. Galaz, G. Hertling, G. Trinchieri, H. J. A. R\\\"ottgering, H. Quintana, I. Valtchanov, J.-B. Melin, J.-P. Le F\\`evre, J. P. Willis, J. Surdej, L. Chiappetti, L. R. Jones, M. Birkinshaw, M. N. Bremer, M. Pierre, O. Garcet, O. Le F\\`evre, P.-A. Duc, P.-G. Sprimont, S. Andreon, T. J. Ponman","submitted_at":"2007-09-13T13:40:15Z","abstract_excerpt":"We present a sample of 29 galaxy clusters from the XMM-LSS survey over an area of some 5deg2 out to a redshift of z=1.05. The sample clusters, which represent about half of the X-ray clusters identified in the region, follow well defined X-ray selection criteria and are all spectroscopically confirmed. For all clusters, we provide X-ray luminosities and temperatures as well as masses. The cluster distribution peaks around z=0.3 and T =1.5 keV, half of the objects being groups with a temperature below 2 keV. Our L-T(z) relation points toward self-similar evolution, but does not exclude other ph"},"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":"0709.1950","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-09-13T13:40:15Z","cross_cats_sorted":[],"title_canon_sha256":"65939bdce4694653640ab7f8263350d18c8d26b71e2fe5b3f16c6dfd559b4464","abstract_canon_sha256":"2d899d779a689e69d5ff877284ad82103ec5846839d99522c03b640a4431c5d7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:35:30.411208Z","signature_b64":"IpDKaOFTN1AG0e7kuP4J+2ZxJXNRXoTd+bEmaCHQkT0M3O+r+7dZD4+c+BHSvy8VC0huVnhMY3EbcJJwg3p6BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"31ce1c6be4b711f0567a462e9f3f93ab77454f2979df3dcb3117ef2b1c3dc4bd","last_reissued_at":"2026-05-18T02:35:30.410619Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:35:30.410619Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The XMM-LSS survey: the Class 1 cluster sample over the initial 5 square degrees and its cosmological modelling","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Detal, A. Gueguen, A. Mazure, A. Refregier, B. Altieri, C. Adami, C. Jean, C. Libbrecht, D. Alloin, D. Maccagni, D. Proust, F. Pacaud, G. Galaz, G. Hertling, G. Trinchieri, H. J. A. R\\\"ottgering, H. Quintana, I. Valtchanov, J.-B. Melin, J.-P. Le F\\`evre, J. P. Willis, J. Surdej, L. Chiappetti, L. R. Jones, M. Birkinshaw, M. N. Bremer, M. Pierre, O. Garcet, O. Le F\\`evre, P.-A. Duc, P.-G. Sprimont, S. Andreon, T. J. Ponman","submitted_at":"2007-09-13T13:40:15Z","abstract_excerpt":"We present a sample of 29 galaxy clusters from the XMM-LSS survey over an area of some 5deg2 out to a redshift of z=1.05. The sample clusters, which represent about half of the X-ray clusters identified in the region, follow well defined X-ray selection criteria and are all spectroscopically confirmed. For all clusters, we provide X-ray luminosities and temperatures as well as masses. The cluster distribution peaks around z=0.3 and T =1.5 keV, half of the objects being groups with a temperature below 2 keV. Our L-T(z) relation points toward self-similar evolution, but does not exclude other ph"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0709.1950","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":"0709.1950","created_at":"2026-05-18T02:35:30.410713+00:00"},{"alias_kind":"arxiv_version","alias_value":"0709.1950v1","created_at":"2026-05-18T02:35:30.410713+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0709.1950","created_at":"2026-05-18T02:35:30.410713+00:00"},{"alias_kind":"pith_short_12","alias_value":"GHHBY27EW4I7","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_16","alias_value":"GHHBY27EW4I7AVT2","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_8","alias_value":"GHHBY27E","created_at":"2026-05-18T12:25:55.427421+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":174,"is_internal_anchor":true},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":76,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN","json":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN.json","graph_json":"https://pith.science/api/pith-number/GHHBY27EW4I7AVT2IYXJ6P4TVN/graph.json","events_json":"https://pith.science/api/pith-number/GHHBY27EW4I7AVT2IYXJ6P4TVN/events.json","paper":"https://pith.science/paper/GHHBY27E"},"agent_actions":{"view_html":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN","download_json":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN.json","view_paper":"https://pith.science/paper/GHHBY27E","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0709.1950&json=true","fetch_graph":"https://pith.science/api/pith-number/GHHBY27EW4I7AVT2IYXJ6P4TVN/graph.json","fetch_events":"https://pith.science/api/pith-number/GHHBY27EW4I7AVT2IYXJ6P4TVN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN/action/storage_attestation","attest_author":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN/action/author_attestation","sign_citation":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN/action/citation_signature","submit_replication":"https://pith.science/pith/GHHBY27EW4I7AVT2IYXJ6P4TVN/action/replication_record"}},"created_at":"2026-05-18T02:35:30.410713+00:00","updated_at":"2026-05-18T02:35:30.410713+00:00"}