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Using 1.4 GHz FIRST, 1.4 GHz NVSS, 327 MHz WENNS, and 150 MHz TGSS catalogues we find the radio-detection of merely $\\sim$ 4.5 per cent (498/11101) NLS1s, with majority (407/498 $\\sim$ 81.7 pe"},"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":"1807.01945","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-07-05T11:28:48Z","cross_cats_sorted":[],"title_canon_sha256":"3169b43e822f255b95bac3ebc57f76711015a0a02cadeb2335084750137a081e","abstract_canon_sha256":"7de2cafee54573621bd4f313f13c7381d02525fd314c56a7b0b4b222ea92852b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:11:23.069753Z","signature_b64":"g6njXhnkX/m38/JCdaOSJRatcQpeN4pyU2JD5YHLdUXqCv9k67HibuLPK2JujYmnIQ8JaVuSalzWjTjMq8R7Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"58dc4287eb45635e43f0ce33ea351049d1125fe176a313ad6406fdeb162b6edb","last_reissued_at":"2026-05-18T00:11:23.069208Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:11:23.069208Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Investigating kpc-scale radio emission properties of narrow-line Seyfert 1 galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Hum Chand, Veeresh Singh","submitted_at":"2018-07-05T11:28:48Z","abstract_excerpt":"In recent years, several Radio-Loud Narrow-Line Seyfert 1 galaxies (RL-NLS1) possessing relativistic jets have come into attention with their detections in Very Large Baseline Array (VLBA) and in $\\gamma$-ray observations. 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