{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:AJU2Z6GLPGRT6ROYM7IWRHHHLA","short_pith_number":"pith:AJU2Z6GL","schema_version":"1.0","canonical_sha256":"0269acf8cb79a33f45d867d1689ce7580417f895674b3b64f0505292b7b7fbde","source":{"kind":"arxiv","id":"2507.01893","version":2},"attestation_state":"computed","paper":{"title":"Measurement of the diffuse astrophysical neutrino flux over six seasons using cascade events from the Baikal-GVD expanding telescope","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A.A. Doroshenko, A.A. Kulikov, A.A. Petrukhin, A.D. Avrorin, A.E. Sirenko, A.G. Solovjev, A.N. Dmitrieva, A.N. Dyachok, A.P. Koshechkin, A.P. Stromakov, A.R. Gafarov, A.S. Chepurnov, A.S. Nikolaev, A.V. Avrorin, A.V. Korobchenko, A.V. Skurikhin, Baikal-GVD Collaboration: V.A. Allakhverdyan, B.A. Shaybonov, B.B. Ulzutuev, D.N. Zaborov, D.P. Petukhov, D.V. Naumov, D.Y. Zvezdov, E.A. Bondarev, E. Eckerov\\'a, E.N. Pliskovsky, E.V. Khramov, E.V. Ryabov, E.V. Shirokov, F. \\v{S}imkovic, G.B. Safronov, G.V. Domogatsky, I.A. Belolaptikov, I.A. Perevalova, I.V. Borina, I.V. Kharuk, I. \\v{S}tekl, K.G. Kebkal, K.V. Golubkov, K.V. Konischev, M.I. Rozanov, M.M. Kolbin, M.N. Sorokovikov, M.V. Kruglov, M.V. Lisitsin, N.M. Budnev, O.V. Suvorova, R. Dvornick\\'y, R.R. Mirgazov, S.I. Zavjalov, S.O. Koligaev, S.S. Khokhlov, S.V. Lovtsov, T.I. Gress, T.V. Elzhov, V.A. Chadymov, V.A. Kozhin, V.A. Tabolenko, V.F. Kulepov, V.I. Tretjak, V.K. Kebkal, V.M. Aynutdinov, V.N. Fomin, V.Y. Dik, V.Y. Shishkin, Y.E. Lemeshev, Y.V. Yablokova, Z. Be\\v{n}u\\v{s}ov\\'a, Zh.-A.M. Dzhilkibaev","submitted_at":"2025-07-02T17:08:01Z","abstract_excerpt":"We present an updated measurement of the diffuse astrophysical neutrino flux using Baikal-GVD cascade data collected between April 2018 to March 2024. In this period, the detector grew from 15% to 55% of its baseline cubic kilometer configuration. The diffuse astrophysical neutrino flux is detected with a statistical significance of 5.1 $\\sigma$. Assuming a single power law model of the astrophysical neutrino flux with identical contribution from each neutrino flavor, the following best-fit parameter values are found: the spectral index $\\gamma_{astro}$ = 2.64$^{+0.09}_{-0.11}$ and the flux no"},"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":"2507.01893","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-07-02T17:08:01Z","cross_cats_sorted":[],"title_canon_sha256":"89a197ec2774ae4ae8d43116e29abb68c0d7a5c636b9f7efeccff76550e5c386","abstract_canon_sha256":"659a042f94b3a6e13aceeb86009085ad39991559e55300c96749b93580a080d5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:34:10.928817Z","signature_b64":"vsy168hJd9RIMHNpSStjH2nNuP/0vazzRFkhBw3OUDG9ZLdKsdndoBZYCWL7pAdpZyGLkRnlhbmAZy4zb/r1AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0269acf8cb79a33f45d867d1689ce7580417f895674b3b64f0505292b7b7fbde","last_reissued_at":"2026-07-05T11:34:10.928327Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:34:10.928327Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measurement of the diffuse astrophysical neutrino flux over six seasons using cascade events from the Baikal-GVD expanding telescope","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A.A. Doroshenko, A.A. Kulikov, A.A. Petrukhin, A.D. Avrorin, A.E. Sirenko, A.G. Solovjev, A.N. Dmitrieva, A.N. Dyachok, A.P. Koshechkin, A.P. Stromakov, A.R. Gafarov, A.S. Chepurnov, A.S. Nikolaev, A.V. Avrorin, A.V. Korobchenko, A.V. Skurikhin, Baikal-GVD Collaboration: V.A. Allakhverdyan, B.A. Shaybonov, B.B. Ulzutuev, D.N. Zaborov, D.P. Petukhov, D.V. Naumov, D.Y. Zvezdov, E.A. Bondarev, E. Eckerov\\'a, E.N. Pliskovsky, E.V. Khramov, E.V. Ryabov, E.V. Shirokov, F. \\v{S}imkovic, G.B. Safronov, G.V. Domogatsky, I.A. Belolaptikov, I.A. Perevalova, I.V. Borina, I.V. Kharuk, I. \\v{S}tekl, K.G. Kebkal, K.V. Golubkov, K.V. Konischev, M.I. Rozanov, M.M. Kolbin, M.N. Sorokovikov, M.V. Kruglov, M.V. Lisitsin, N.M. Budnev, O.V. Suvorova, R. Dvornick\\'y, R.R. Mirgazov, S.I. Zavjalov, S.O. Koligaev, S.S. Khokhlov, S.V. Lovtsov, T.I. Gress, T.V. Elzhov, V.A. Chadymov, V.A. Kozhin, V.A. Tabolenko, V.F. Kulepov, V.I. Tretjak, V.K. Kebkal, V.M. Aynutdinov, V.N. Fomin, V.Y. Dik, V.Y. Shishkin, Y.E. Lemeshev, Y.V. Yablokova, Z. Be\\v{n}u\\v{s}ov\\'a, Zh.-A.M. Dzhilkibaev","submitted_at":"2025-07-02T17:08:01Z","abstract_excerpt":"We present an updated measurement of the diffuse astrophysical neutrino flux using Baikal-GVD cascade data collected between April 2018 to March 2024. In this period, the detector grew from 15% to 55% of its baseline cubic kilometer configuration. The diffuse astrophysical neutrino flux is detected with a statistical significance of 5.1 $\\sigma$. Assuming a single power law model of the astrophysical neutrino flux with identical contribution from each neutrino flavor, the following best-fit parameter values are found: the spectral index $\\gamma_{astro}$ = 2.64$^{+0.09}_{-0.11}$ and the flux no"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2507.01893","kind":"arxiv","version":2},"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/2507.01893/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":"2507.01893","created_at":"2026-07-05T11:34:10.928390+00:00"},{"alias_kind":"arxiv_version","alias_value":"2507.01893v2","created_at":"2026-07-05T11:34:10.928390+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2507.01893","created_at":"2026-07-05T11:34:10.928390+00:00"},{"alias_kind":"pith_short_12","alias_value":"AJU2Z6GLPGRT","created_at":"2026-07-05T11:34:10.928390+00:00"},{"alias_kind":"pith_short_16","alias_value":"AJU2Z6GLPGRT6ROY","created_at":"2026-07-05T11:34:10.928390+00:00"},{"alias_kind":"pith_short_8","alias_value":"AJU2Z6GL","created_at":"2026-07-05T11:34:10.928390+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.06773","citing_title":"Lepton interactions from GeV to EeV","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2604.06509","citing_title":"Improving Neutrino Point Source Sensitivity with Source-Informed Event Selection","ref_index":7,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA","json":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA.json","graph_json":"https://pith.science/api/pith-number/AJU2Z6GLPGRT6ROYM7IWRHHHLA/graph.json","events_json":"https://pith.science/api/pith-number/AJU2Z6GLPGRT6ROYM7IWRHHHLA/events.json","paper":"https://pith.science/paper/AJU2Z6GL"},"agent_actions":{"view_html":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA","download_json":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA.json","view_paper":"https://pith.science/paper/AJU2Z6GL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2507.01893&json=true","fetch_graph":"https://pith.science/api/pith-number/AJU2Z6GLPGRT6ROYM7IWRHHHLA/graph.json","fetch_events":"https://pith.science/api/pith-number/AJU2Z6GLPGRT6ROYM7IWRHHHLA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA/action/storage_attestation","attest_author":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA/action/author_attestation","sign_citation":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA/action/citation_signature","submit_replication":"https://pith.science/pith/AJU2Z6GLPGRT6ROYM7IWRHHHLA/action/replication_record"}},"created_at":"2026-07-05T11:34:10.928390+00:00","updated_at":"2026-07-05T11:34:10.928390+00:00"}