{"paper":{"title":"Exploring the Transitional Parameter Space of Blazars using Gamma-ray and X-ray Population Diagnostics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Changing-look blazars occupy intermediate gamma-ray and X-ray spaces but lie closer to flat-spectrum radio quasars.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Sikandar Akbar, Zahir Shah, Zahoor Malik","submitted_at":"2026-05-17T11:30:10Z","abstract_excerpt":"We investigate the $\\gamma$-ray and X-ray population properties of changing-look blazars (CLBs) using sources from the Fourth \\textit{Fermi} LAT Source Catalog Data Release 4 (4FGL-DR4) together with X-ray information from the Living \\textit{Swift} XRT Point Source (LSXPS) catalog. The CLB sample is compared with large populations of confirmed BL Lac objects (BLLs) and flat-spectrum radio quasars (FSRQs) using spectral, variability, and broadband properties. In the $\\gamma$-ray parameter space, CLBs mainly occupy intermediate and overlap regions between the BLL and FSRQ populations. However, t"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"Overall, the results suggest that CLBs form a transitional population between the two main blazar subclasses while retaining characteristics closer to the FSRQ population.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The gamma-ray and X-ray parameters drawn from the 4FGL-DR4 and LSXPS catalogs are assumed to be free of major selection biases and to faithfully represent the intrinsic properties of the three populations being compared.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Changing-look blazars occupy intermediate regions in gamma-ray and X-ray parameter spaces but lie statistically closer to flat-spectrum radio quasars than to BL Lac objects according to centroids, PCA, UMAP, and random-forest classification.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Changing-look blazars occupy intermediate gamma-ray and X-ray spaces but lie closer to flat-spectrum radio quasars.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"e576d8caf9defe8b0b3d7a398608b7e584fae0d04d1bc41998946f1e30a76650"},"source":{"id":"2605.17397","kind":"arxiv","version":1},"verdict":{"id":"a0711461-4245-4f87-9b05-a9b507cc9ca7","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T22:52:18.067771Z","strongest_claim":"Overall, the results suggest that CLBs form a transitional population between the two main blazar subclasses while retaining characteristics closer to the FSRQ population.","one_line_summary":"Changing-look blazars occupy intermediate regions in gamma-ray and X-ray parameter spaces but lie statistically closer to flat-spectrum radio quasars than to BL Lac objects according to centroids, PCA, UMAP, and random-forest classification.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The gamma-ray and X-ray parameters drawn from the 4FGL-DR4 and LSXPS catalogs are assumed to be free of major selection biases and to faithfully represent the intrinsic properties of the three populations being compared.","pith_extraction_headline":"Changing-look blazars occupy intermediate gamma-ray and X-ray spaces but lie closer to flat-spectrum radio quasars."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2605.17397/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"doi_compliance","ran_at":"2026-05-19T23:01:51.242545Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_title_agreement","ran_at":"2026-05-19T23:01:19.656627Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"claim_evidence","ran_at":"2026-05-19T21:41:57.757043Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"ai_meta_artifact","ran_at":"2026-05-19T21:33:23.698999Z","status":"skipped","version":"1.0.0","findings_count":0}],"snapshot_sha256":"88c77b5c79ed4c232fe3d1d1c9a9ae09b249da70cc3fc2b0d85b08a07a7d7cd0"},"references":{"count":54,"sample":[{"doi":"","year":null,"title":"AM Wolfe, Ed , volume=","work_id":"876ed35f-98b3-4b87-8a33-0b4032cd25ef","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1086/133630","year":null,"title":"M., & Padovani, P","work_id":"bab421bb-cbb0-428a-b65e-28d457db4fed","ref_index":2,"cited_arxiv_id":"astro-ph/9506063","is_internal_anchor":true},{"doi":"10.1146/annurev-astro-081913-040044","year":2016,"title":", year = 2016, month = sep, volume =","work_id":"ff7466e2-7676-4523-ac48-6eefadc82889","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1146/annurev-astro-081817-051948","year":null,"title":"2019, ARA&A, 57, 467, doi: 10.1146/annurev-astro-081817-051948","work_id":"10f156a4-078f-4b56-a11d-ee32f3b98d84","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1007/s10509-007-9404-0","year":null,"title":"Modeling the Emission Processes in Blazars","work_id":"ddb31383-3df1-4915-84c7-a7419513f08b","ref_index":5,"cited_arxiv_id":"astro-ph/0608713","is_internal_anchor":true}],"resolved_work":54,"snapshot_sha256":"7124436cb3b9d24fe40f8c815fdfcbb20a55d0ffb24c27b476a087ddc88ce61d","internal_anchors":20},"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"}