{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:7KHRZ666IQU2N6BGRAPPWK6VCV","short_pith_number":"pith:7KHRZ666","schema_version":"1.0","canonical_sha256":"fa8f1cfbde4429a6f826881efb2bd51563e8ad0e7a9329a17a7c835fe36aa155","source":{"kind":"arxiv","id":"1708.07125","version":1},"attestation_state":"computed","paper":{"title":"Observations of the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"A. Melis, C. Ferrari, E. Carretti, E. Orr\\`u, F. De Gasperin, F. Gastaldello, F. Govoni, F. Loi, F. Vazza, G.B Taylor, G. Giovannini, G. Valente, H. Junklewitz, L. Feretti, L. Gregorini, M. Girardi, M. Johnston-Hollitt, M. Murgia, P. Parma, R. Concu, R. Paladino, R. Perley, S. Colafrancesco, S. Poppi, T.E. Clarke, T. En{\\ss}lin, V. Vacca, W. Boschin","submitted_at":"2017-08-23T18:00:00Z","abstract_excerpt":"We observed the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope to provide new constraints on its spectral properties at high frequency. We conducted observations in three frequency bands centred at 1.4 GHz, 6.6 GHz and 19 GHz, resulting in beam resolutions of 14$^{\\prime}$, 2.9$^{\\prime}$ and 1$^{\\prime}$ respectively. These single-dish data were also combined with archival interferometric observations at 1.4 and 1.7 GHz. From the combined images, we measured a flux density of ${\\rm S_{1.4GHz}=(158.3\\pm9.6)\\,mJy}$ for the central radio halo and ${\\rm S_{1.4GHz}=(126\\pm8)\\,m"},"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":"1708.07125","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-08-23T18:00:00Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"a3a2ec767ba2cb8ffa267be6568e0f677cbfa558a455ff7835322998fdf8166f","abstract_canon_sha256":"49ba577923850c680fecf7b0e977a4600775148e8a689c2eaf61df133afa1ed2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:31:11.938711Z","signature_b64":"7DmLUQrNlw1TNDqMcJ2NrNHN/uyjZFz0K8a6Ws1itXdNYBu8l3iyTogSR5nSUpGLowfY04Jdob55re7xDvEiCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fa8f1cfbde4429a6f826881efb2bd51563e8ad0e7a9329a17a7c835fe36aa155","last_reissued_at":"2026-05-18T00:31:11.938097Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:31:11.938097Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observations of the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"A. Melis, C. Ferrari, E. Carretti, E. Orr\\`u, F. De Gasperin, F. Gastaldello, F. Govoni, F. Loi, F. Vazza, G.B Taylor, G. Giovannini, G. Valente, H. Junklewitz, L. Feretti, L. Gregorini, M. Girardi, M. Johnston-Hollitt, M. Murgia, P. Parma, R. Concu, R. Paladino, R. Perley, S. Colafrancesco, S. Poppi, T.E. Clarke, T. En{\\ss}lin, V. Vacca, W. Boschin","submitted_at":"2017-08-23T18:00:00Z","abstract_excerpt":"We observed the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope to provide new constraints on its spectral properties at high frequency. We conducted observations in three frequency bands centred at 1.4 GHz, 6.6 GHz and 19 GHz, resulting in beam resolutions of 14$^{\\prime}$, 2.9$^{\\prime}$ and 1$^{\\prime}$ respectively. These single-dish data were also combined with archival interferometric observations at 1.4 and 1.7 GHz. From the combined images, we measured a flux density of ${\\rm S_{1.4GHz}=(158.3\\pm9.6)\\,mJy}$ for the central radio halo and ${\\rm S_{1.4GHz}=(126\\pm8)\\,m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1708.07125","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":"1708.07125","created_at":"2026-05-18T00:31:11.938197+00:00"},{"alias_kind":"arxiv_version","alias_value":"1708.07125v1","created_at":"2026-05-18T00:31:11.938197+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1708.07125","created_at":"2026-05-18T00:31:11.938197+00:00"},{"alias_kind":"pith_short_12","alias_value":"7KHRZ666IQU2","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_16","alias_value":"7KHRZ666IQU2N6BG","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_8","alias_value":"7KHRZ666","created_at":"2026-05-18T12:31:05.417338+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15264","citing_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","ref_index":194,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV","json":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV.json","graph_json":"https://pith.science/api/pith-number/7KHRZ666IQU2N6BGRAPPWK6VCV/graph.json","events_json":"https://pith.science/api/pith-number/7KHRZ666IQU2N6BGRAPPWK6VCV/events.json","paper":"https://pith.science/paper/7KHRZ666"},"agent_actions":{"view_html":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV","download_json":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV.json","view_paper":"https://pith.science/paper/7KHRZ666","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1708.07125&json=true","fetch_graph":"https://pith.science/api/pith-number/7KHRZ666IQU2N6BGRAPPWK6VCV/graph.json","fetch_events":"https://pith.science/api/pith-number/7KHRZ666IQU2N6BGRAPPWK6VCV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV/action/storage_attestation","attest_author":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV/action/author_attestation","sign_citation":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV/action/citation_signature","submit_replication":"https://pith.science/pith/7KHRZ666IQU2N6BGRAPPWK6VCV/action/replication_record"}},"created_at":"2026-05-18T00:31:11.938197+00:00","updated_at":"2026-05-18T00:31:11.938197+00:00"}