{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:XJIDSOPK3MEFC4QSNKUA7YQCAC","short_pith_number":"pith:XJIDSOPK","schema_version":"1.0","canonical_sha256":"ba503939eadb085172126aa80fe20200b1ce4ddd83a83fa6b30aa47dfeb18e11","source":{"kind":"arxiv","id":"1905.00755","version":1},"attestation_state":"computed","paper":{"title":"Interpreting the distributions of FRB observables","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.HE","authors_text":"Liam Connor","submitted_at":"2019-05-02T14:05:52Z","abstract_excerpt":"Fast radio bursts (FRBs) are short-duration radio transients of unknown origin. Thus far, they have been blindly detected at millisecond timescales with dispersion measures (DMs) between 110--2600\\,pc\\,cm$^{-3}$. However, the observed pulse width, DM, and even brightness distributions depend strongly on the time and frequency resolution of the detection instrument. Spectral and temporal resolution also significantly affect FRB detection rates, similar to beam size and system-equivalent flux density (SEFD). I discuss the interplay between underlying FRB properties and instrumental response, and"},"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":"1905.00755","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-05-02T14:05:52Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"c59875d13abc88da6dc2f77b2d2b439368d82f3c20e70db98fb4c517a2f3d52b","abstract_canon_sha256":"b287b1ba6ea0d696290481c70845ffbc031f3c3383ffb63091975893ac55cd57"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:41:08.820147Z","signature_b64":"WazEu9FbixyindXH7AN0fZAOIRuCUANqPbFvLpHhCg7Q2WQwe43hqcR/K54nbuvZZTD9GCGhEVkdWaLRJ0/4CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ba503939eadb085172126aa80fe20200b1ce4ddd83a83fa6b30aa47dfeb18e11","last_reissued_at":"2026-05-17T23:41:08.819597Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:41:08.819597Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Interpreting the distributions of FRB observables","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.HE","authors_text":"Liam Connor","submitted_at":"2019-05-02T14:05:52Z","abstract_excerpt":"Fast radio bursts (FRBs) are short-duration radio transients of unknown origin. Thus far, they have been blindly detected at millisecond timescales with dispersion measures (DMs) between 110--2600\\,pc\\,cm$^{-3}$. However, the observed pulse width, DM, and even brightness distributions depend strongly on the time and frequency resolution of the detection instrument. Spectral and temporal resolution also significantly affect FRB detection rates, similar to beam size and system-equivalent flux density (SEFD). I discuss the interplay between underlying FRB properties and instrumental response, and"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1905.00755","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":"1905.00755","created_at":"2026-05-17T23:41:08.819693+00:00"},{"alias_kind":"arxiv_version","alias_value":"1905.00755v1","created_at":"2026-05-17T23:41:08.819693+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1905.00755","created_at":"2026-05-17T23:41:08.819693+00:00"},{"alias_kind":"pith_short_12","alias_value":"XJIDSOPK3MEF","created_at":"2026-05-18T12:33:33.725879+00:00"},{"alias_kind":"pith_short_16","alias_value":"XJIDSOPK3MEFC4QS","created_at":"2026-05-18T12:33:33.725879+00:00"},{"alias_kind":"pith_short_8","alias_value":"XJIDSOPK","created_at":"2026-05-18T12:33:33.725879+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.07087","citing_title":"A series of unfortunate events: CHIME/FRB misclassification of a Galactic pulsar as a periodic fast radio burst","ref_index":97,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10538","citing_title":"Updating the PATH framework with FRB host galaxy models","ref_index":243,"is_internal_anchor":true},{"citing_arxiv_id":"1907.07948","citing_title":"Fast Radio Burst Injection Tests","ref_index":5,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC","json":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC.json","graph_json":"https://pith.science/api/pith-number/XJIDSOPK3MEFC4QSNKUA7YQCAC/graph.json","events_json":"https://pith.science/api/pith-number/XJIDSOPK3MEFC4QSNKUA7YQCAC/events.json","paper":"https://pith.science/paper/XJIDSOPK"},"agent_actions":{"view_html":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC","download_json":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC.json","view_paper":"https://pith.science/paper/XJIDSOPK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1905.00755&json=true","fetch_graph":"https://pith.science/api/pith-number/XJIDSOPK3MEFC4QSNKUA7YQCAC/graph.json","fetch_events":"https://pith.science/api/pith-number/XJIDSOPK3MEFC4QSNKUA7YQCAC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC/action/storage_attestation","attest_author":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC/action/author_attestation","sign_citation":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC/action/citation_signature","submit_replication":"https://pith.science/pith/XJIDSOPK3MEFC4QSNKUA7YQCAC/action/replication_record"}},"created_at":"2026-05-17T23:41:08.819693+00:00","updated_at":"2026-05-17T23:41:08.819693+00:00"}