{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:75M34HQBJWC6YAH2YK4FNGX2FC","short_pith_number":"pith:75M34HQB","schema_version":"1.0","canonical_sha256":"ff59be1e014d85ec00fac2b8569afa28a0ed6bbc0b0ea4de6656f3fa923e3dc8","source":{"kind":"arxiv","id":"1907.07708","version":1},"attestation_state":"computed","paper":{"title":"Extragalactic megahertz-peaked spectrum radio sources at milliarcsecond scales","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"H. J. A. R\\\"ottgering, J. R. Callingham, M. A. Keim","submitted_at":"2019-07-17T18:25:43Z","abstract_excerpt":"Extragalactic peaked-spectrum radio sources are thought to be the progenitors of larger, radio-loud active galactic nuclei (AGN). Synchrotron self-absorption (SSA) has often been identified as the cause of their spectral peak. The identification of new megahertz-peaked spectrum sources from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey provides an opportunity to test how radio sources with spectral peaks below 1 GHz fit within this evolutionary picture. We observed six peaked-spectrum sources selected from the GLEAM survey, three that have spectral characteris"},"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":"1907.07708","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-07-17T18:25:43Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"6eac94ba5d989b4fc2f69a0022a0edc1ff94675d49eca6c4bd51fb9384abc6b5","abstract_canon_sha256":"0e23c4d7e7eab5013741b50177d948d8ce839bc8dde4fb9292e9f86004859755"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T23:52:00.454287Z","signature_b64":"G81mNgp2Mm7Mstl4jvkFYMHKK164SsbHWzfUKwr8aUe8CUDUFxnYgZwRD6Fs621ZJiwDwUJR1gZOLnd6bge7Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ff59be1e014d85ec00fac2b8569afa28a0ed6bbc0b0ea4de6656f3fa923e3dc8","last_reissued_at":"2026-07-04T23:52:00.453818Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T23:52:00.453818Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Extragalactic megahertz-peaked spectrum radio sources at milliarcsecond scales","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"H. J. A. R\\\"ottgering, J. R. Callingham, M. A. Keim","submitted_at":"2019-07-17T18:25:43Z","abstract_excerpt":"Extragalactic peaked-spectrum radio sources are thought to be the progenitors of larger, radio-loud active galactic nuclei (AGN). Synchrotron self-absorption (SSA) has often been identified as the cause of their spectral peak. The identification of new megahertz-peaked spectrum sources from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey provides an opportunity to test how radio sources with spectral peaks below 1 GHz fit within this evolutionary picture. We observed six peaked-spectrum sources selected from the GLEAM survey, three that have spectral characteris"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.07708","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/1907.07708/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":"1907.07708","created_at":"2026-07-04T23:52:00.453875+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.07708v1","created_at":"2026-07-04T23:52:00.453875+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.07708","created_at":"2026-07-04T23:52:00.453875+00:00"},{"alias_kind":"pith_short_12","alias_value":"75M34HQBJWC6","created_at":"2026-07-04T23:52:00.453875+00:00"},{"alias_kind":"pith_short_16","alias_value":"75M34HQBJWC6YAH2","created_at":"2026-07-04T23:52:00.453875+00:00"},{"alias_kind":"pith_short_8","alias_value":"75M34HQB","created_at":"2026-07-04T23:52:00.453875+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06143","citing_title":"Deep far-UV observations of the ELAIS N1 field using AstroSat: Source catalogue, spectral energy distribution modelling and star formation","ref_index":26,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC","json":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC.json","graph_json":"https://pith.science/api/pith-number/75M34HQBJWC6YAH2YK4FNGX2FC/graph.json","events_json":"https://pith.science/api/pith-number/75M34HQBJWC6YAH2YK4FNGX2FC/events.json","paper":"https://pith.science/paper/75M34HQB"},"agent_actions":{"view_html":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC","download_json":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC.json","view_paper":"https://pith.science/paper/75M34HQB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.07708&json=true","fetch_graph":"https://pith.science/api/pith-number/75M34HQBJWC6YAH2YK4FNGX2FC/graph.json","fetch_events":"https://pith.science/api/pith-number/75M34HQBJWC6YAH2YK4FNGX2FC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC/action/storage_attestation","attest_author":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC/action/author_attestation","sign_citation":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC/action/citation_signature","submit_replication":"https://pith.science/pith/75M34HQBJWC6YAH2YK4FNGX2FC/action/replication_record"}},"created_at":"2026-07-04T23:52:00.453875+00:00","updated_at":"2026-07-04T23:52:00.453875+00:00"}