{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:CM3HLP6ULHGKGIEGZH25M2SZH7","short_pith_number":"pith:CM3HLP6U","schema_version":"1.0","canonical_sha256":"133675bfd459cca32086c9f5d66a593ff2a5e82d6818657314382afa26b52ef2","source":{"kind":"arxiv","id":"0705.2266","version":1},"attestation_state":"computed","paper":{"title":"Evolution of the Frequency of Luminous (\\geq L_V*) Close Galaxy Pairs at z < 1.2 in the COSMOS Field","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Koekemoer, B. Mobasher, D. B. Sanders, D. Calzetti, J. S. Kartaltepe, M. Salvato, N. Z. Scoville, P. Capak, S. S. Sasaki, T. Murayama, Y. Taniguchi","submitted_at":"2007-05-16T01:26:39Z","abstract_excerpt":"We measure the fraction of luminous galaxies in pairs at projected separations of 5-20 kpc out to z=1.2 in the COSMOS field using ACS images and photometric redshifts derived from an extensive multiwavelength dataset. Analysis of a complete sample of 106,188 galaxies more luminous than M_V=-19.8 (~ L_V*) in the redshift range 0.1 < z < 1.2 yields 1,749 galaxy pairs. These data are supplemented by a local z=0-0.1 value for the galaxy pair fraction derived from the Sloan Digital Sky Survey (SDSS). After statistically correcting the COSMOS pair sample for chance line-of-sight superpositions, 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":"0705.2266","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-05-16T01:26:39Z","cross_cats_sorted":[],"title_canon_sha256":"144f37e0b7281d7e7cb776805cba5307df0450ace8fe69af311fdd40d898d18d","abstract_canon_sha256":"2a80514d475e3c1f32a1cfc75472bcd38433d6ca7ddecc87330acefbc0b6a1cc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:03:51.370807Z","signature_b64":"MTR5r4BO0YeeYBp1Xr2dQD+FzDgqn0uZWK8EvejhbEKWpWfyKQz7tV+bWa165r0zs6Q0iftLpusNNlbiONEaBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"133675bfd459cca32086c9f5d66a593ff2a5e82d6818657314382afa26b52ef2","last_reissued_at":"2026-07-04T17:03:51.370458Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:03:51.370458Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evolution of the Frequency of Luminous (\\geq L_V*) Close Galaxy Pairs at z < 1.2 in the COSMOS Field","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Koekemoer, B. Mobasher, D. B. Sanders, D. Calzetti, J. S. Kartaltepe, M. Salvato, N. Z. Scoville, P. Capak, S. S. Sasaki, T. Murayama, Y. Taniguchi","submitted_at":"2007-05-16T01:26:39Z","abstract_excerpt":"We measure the fraction of luminous galaxies in pairs at projected separations of 5-20 kpc out to z=1.2 in the COSMOS field using ACS images and photometric redshifts derived from an extensive multiwavelength dataset. Analysis of a complete sample of 106,188 galaxies more luminous than M_V=-19.8 (~ L_V*) in the redshift range 0.1 < z < 1.2 yields 1,749 galaxy pairs. These data are supplemented by a local z=0-0.1 value for the galaxy pair fraction derived from the Sloan Digital Sky Survey (SDSS). After statistically correcting the COSMOS pair sample for chance line-of-sight superpositions, the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0705.2266","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0705.2266/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":"0705.2266","created_at":"2026-07-04T17:03:51.370515+00:00"},{"alias_kind":"arxiv_version","alias_value":"0705.2266v1","created_at":"2026-07-04T17:03:51.370515+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0705.2266","created_at":"2026-07-04T17:03:51.370515+00:00"},{"alias_kind":"pith_short_12","alias_value":"CM3HLP6ULHGK","created_at":"2026-07-04T17:03:51.370515+00:00"},{"alias_kind":"pith_short_16","alias_value":"CM3HLP6ULHGKGIEG","created_at":"2026-07-04T17:03:51.370515+00:00"},{"alias_kind":"pith_short_8","alias_value":"CM3HLP6U","created_at":"2026-07-04T17:03:51.370515+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.31140","citing_title":"Deep Extragalactic VIsible Legacy Survey (DEVILS): Morphologically-selected galaxy merger fractions and their direct comparison to close-pair samples","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7","json":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7.json","graph_json":"https://pith.science/api/pith-number/CM3HLP6ULHGKGIEGZH25M2SZH7/graph.json","events_json":"https://pith.science/api/pith-number/CM3HLP6ULHGKGIEGZH25M2SZH7/events.json","paper":"https://pith.science/paper/CM3HLP6U"},"agent_actions":{"view_html":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7","download_json":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7.json","view_paper":"https://pith.science/paper/CM3HLP6U","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0705.2266&json=true","fetch_graph":"https://pith.science/api/pith-number/CM3HLP6ULHGKGIEGZH25M2SZH7/graph.json","fetch_events":"https://pith.science/api/pith-number/CM3HLP6ULHGKGIEGZH25M2SZH7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7/action/storage_attestation","attest_author":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7/action/author_attestation","sign_citation":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7/action/citation_signature","submit_replication":"https://pith.science/pith/CM3HLP6ULHGKGIEGZH25M2SZH7/action/replication_record"}},"created_at":"2026-07-04T17:03:51.370515+00:00","updated_at":"2026-07-04T17:03:51.370515+00:00"}