{"bundle_type":"pith_open_graph_bundle","bundle_version":"1.0","pith_number":"pith:2026:KYT4H77LO4VSI2W5Z7DA3DLI3Q","short_pith_number":"pith:KYT4H77L","canonical_record":{"source":{"id":"2605.13016","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09Z","cross_cats_sorted":[],"title_canon_sha256":"f0d962eb3cec9999ee9a555aa02f431469b37c70544bd8ab89e120596959646d","abstract_canon_sha256":"f0018ba8ff99285b8e7217c3a5fa1571313489a4129f1c928048d47d0610417c"},"schema_version":"1.0"},"canonical_sha256":"5627c3ffeb772b246addcfc60d8d68dc3786b9664a032188a4433d8d4868b448","source":{"kind":"arxiv","id":"2605.13016","version":1},"source_aliases":[{"alias_kind":"arxiv","alias_value":"2605.13016","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"arxiv_version","alias_value":"2605.13016v1","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2605.13016","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"pith_short_12","alias_value":"KYT4H77LO4VS","created_at":"2026-05-18T12:33:37Z"},{"alias_kind":"pith_short_16","alias_value":"KYT4H77LO4VSI2W5","created_at":"2026-05-18T12:33:37Z"},{"alias_kind":"pith_short_8","alias_value":"KYT4H77L","created_at":"2026-05-18T12:33:37Z"}],"events":[{"event_type":"record_created","subject_pith_number":"pith:2026:KYT4H77LO4VSI2W5Z7DA3DLI3Q","target":"record","payload":{"canonical_record":{"source":{"id":"2605.13016","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09Z","cross_cats_sorted":[],"title_canon_sha256":"f0d962eb3cec9999ee9a555aa02f431469b37c70544bd8ab89e120596959646d","abstract_canon_sha256":"f0018ba8ff99285b8e7217c3a5fa1571313489a4129f1c928048d47d0610417c"},"schema_version":"1.0"},"canonical_sha256":"5627c3ffeb772b246addcfc60d8d68dc3786b9664a032188a4433d8d4868b448","receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:09:00.124926Z","signature_b64":"2ErOP3Mfa89kTczfHihWytUUg5075FKPuporU1sIy9fInypcQlVgoaisfuAoXOSH6r2+EeLAackCUViRgQ/eBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5627c3ffeb772b246addcfc60d8d68dc3786b9664a032188a4433d8d4868b448","last_reissued_at":"2026-05-18T03:09:00.124303Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:09:00.124303Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"source_kind":"arxiv","source_id":"2605.13016","source_version":1,"attestation_state":"computed"},"signer":{"signer_id":"pith.science","signer_type":"pith_registry","key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"created_at":"2026-05-18T03:09:00Z","supersedes":[],"prev_event":null,"signature":{"signature_status":"signed_v1","algorithm":"ed25519","key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","signature_b64":"CFpTzahnPDboDiyPYNGwxXORMToKDuI8AxOfdPSJ/ohAGSixCr+QR1G7fiDPbFKTOIvWPlO4wOTxOhnk6iERCg==","signed_message":"open_graph_event_sha256_bytes","signed_at":"2026-05-30T04:13:18.390791Z"},"content_sha256":"8a09201c9d083cc9ad175da21f63719a3073541e11e046611bf2ca0b0435700e","schema_version":"1.0","event_id":"sha256:8a09201c9d083cc9ad175da21f63719a3073541e11e046611bf2ca0b0435700e"},{"event_type":"graph_snapshot","subject_pith_number":"pith:2026:KYT4H77LO4VSI2W5Z7DA3DLI3Q","target":"graph","payload":{"graph_snapshot":{"paper":{"title":"Revisiting constraints on primordial vector modes and implications for sourced magnetic fields and observed $EB$ power spectrum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum.","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Kaito Yura, Kiyotomo Ichiki, Shohei Saga, Shuichiro Yokoyama","submitted_at":"2026-05-13T05:11:09Z","abstract_excerpt":"We revisit regular primordial vector modes sustained by the anisotropic stress of free-streaming neutrinos. We consider two classes of neutrino-sector initial conditions, the neutrino velocity isocurvature mode ($\\nu\\mathrm{VI}$) and the neutrino octupole mode ($\\nu\\mathrm{OCT}$). We update their observational constraints using current cosmological data, and examine the impact of including the BICEP/Keck 2018 $B$-mode polarization data. From an MCMC analysis, we obtain the 95\\% C.L. upper bounds on the vector-to-scalar ratio as $r_\\mathrm{v}<1.55\\times10^{-4}$ and $r_\\mathrm{v}<1.04\\times10^{-"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"From an MCMC analysis, we obtain the 95% C.L. upper bounds on the vector-to-scalar ratio as r_v < 1.55×10^{-4} and r_v < 1.04×10^{-2} for the νVI and νOCT modes at k0 = 0.01 Mpc^{-1}. We show that even a fully helical primordial vector mode cannot reproduce the currently observed EB signal while remaining consistent with parity-even CMB constraints.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The assumption that regular primordial vector modes are sustained by the anisotropic stress of free-streaming neutrinos under the specific neutrino velocity isocurvature (νVI) and octupole (νOCT) initial conditions.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Updated constraints on neutrino-sustained primordial vector modes imply magnetic fields too weak to seed observations and cannot reproduce the EB power spectrum while satisfying parity-even limits.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"0fdefc08848f8d0c00b5d1d40991ca6388eeb8e91af3b48705ed21d5c59a641e"},"source":{"id":"2605.13016","kind":"arxiv","version":1},"verdict":{"id":"ea6ef95c-2c83-4286-9c82-c56d7d16fda3","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-14T18:35:37.725185Z","strongest_claim":"From an MCMC analysis, we obtain the 95% C.L. upper bounds on the vector-to-scalar ratio as r_v < 1.55×10^{-4} and r_v < 1.04×10^{-2} for the νVI and νOCT modes at k0 = 0.01 Mpc^{-1}. We show that even a fully helical primordial vector mode cannot reproduce the currently observed EB signal while remaining consistent with parity-even CMB constraints.","one_line_summary":"Updated constraints on neutrino-sustained primordial vector modes imply magnetic fields too weak to seed observations and cannot reproduce the EB power spectrum while satisfying parity-even limits.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The assumption that regular primordial vector modes are sustained by the anisotropic stress of free-streaming neutrinos under the specific neutrino velocity isocurvature (νVI) and octupole (νOCT) initial conditions.","pith_extraction_headline":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum."},"references":{"count":46,"sample":[{"doi":"","year":2013,"title":"Cosmological Magnetic Fields: Their Generation, Evolution and Observation","work_id":"b101da28-b381-4bc0-9176-e19d6d868643","ref_index":1,"cited_arxiv_id":"1303.7121","is_internal_anchor":true},{"doi":"","year":1992,"title":"Rebhan, Large-Scale Rotational Perturbations of a Friedmann Universe with Collisionless Matter and Pri- mordial Magnetic Fields, ApJ392, 385 (1992)","work_id":"540969b0-f69c-4205-a21e-3c9a78c31511","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2004,"title":"Observable primordial vector modes","work_id":"96128296-ea06-440e-a335-149e2000c5cf","ref_index":3,"cited_arxiv_id":"astro-ph/0403583","is_internal_anchor":true},{"doi":"","year":2012,"title":"Constraint on the primordial vector mode and its magnetic field generation from seven-year Wilkinson Microwave Anisotropy Probe Observations","work_id":"a5a3f9a7-858b-4906-844f-4fb36e0c382c","ref_index":4,"cited_arxiv_id":"1112.4705","is_internal_anchor":true},{"doi":"","year":2014,"title":"Constraining primordial vector mode from B-mode polarization","work_id":"6c4631b0-dfe0-4dd3-8252-5dca98c9d001","ref_index":5,"cited_arxiv_id":"1405.4810","is_internal_anchor":true}],"resolved_work":46,"snapshot_sha256":"3d4d03368b452884f50029cc8bec6bf9a03b65f708f0429480463e50ac550f85","internal_anchors":26},"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"},"verdict_id":"ea6ef95c-2c83-4286-9c82-c56d7d16fda3"},"signer":{"signer_id":"pith.science","signer_type":"pith_registry","key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"created_at":"2026-05-18T03:09:00Z","supersedes":[],"prev_event":null,"signature":{"signature_status":"signed_v1","algorithm":"ed25519","key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","signature_b64":"MHumcJ3nJBbfTGRRz9HUNlMPiz0bQsWkBSHHEqd3bMlXpaRnF9TD13+OxgeFMf8/vnhcMNFFkNKFMW+OJV9AAQ==","signed_message":"open_graph_event_sha256_bytes","signed_at":"2026-05-30T04:13:18.391928Z"},"content_sha256":"842138bd806c8b13002aba458f716e79dd7ccf47c694b3ae51e8e9cb77ea8d4c","schema_version":"1.0","event_id":"sha256:842138bd806c8b13002aba458f716e79dd7ccf47c694b3ae51e8e9cb77ea8d4c"}],"timestamp_proofs":[],"mirror_hints":[{"mirror_type":"https","name":"Pith Resolver","base_url":"https://pith.science","bundle_url":"https://pith.science/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/bundle.json","state_url":"https://pith.science/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/state.json","well_known_bundle_url":"https://pith.science/.well-known/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/bundle.json","status":"primary"}],"public_keys":[{"key_id":"pith-v1-2026-05","algorithm":"ed25519","format":"raw","public_key_b64":"stVStoiQhXFxp4s2pdzPNoqVNBMojDU/fJ2db5S3CbM=","public_key_hex":"b2d552b68890857171a78b36a5dccf368a953413288c353f7c9d9d6f94b709b3","fingerprint_sha256_b32_first128bits":"RVFV5Z2OI2J3ZUO7ERDEBCYNKS","fingerprint_sha256_hex":"8d4b5ee74e4693bcd1df2446408b0d54","rotates_at":null,"url":"https://pith.science/pith-signing-key.json","notes":"Pith uses this Ed25519 key to sign canonical record SHA-256 digests. Verify with: ed25519_verify(public_key, message=canonical_sha256_bytes, signature=base64decode(signature_b64))."}],"merge_version":"pith-open-graph-merge-v1","built_at":"2026-05-30T04:13:18Z","links":{"resolver":"https://pith.science/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q","bundle":"https://pith.science/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/bundle.json","state":"https://pith.science/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/state.json","well_known_bundle":"https://pith.science/.well-known/pith/KYT4H77LO4VSI2W5Z7DA3DLI3Q/bundle.json"},"state":{"state_type":"pith_open_graph_state","state_version":"1.0","pith_number":"pith:2026:KYT4H77LO4VSI2W5Z7DA3DLI3Q","merge_version":"pith-open-graph-merge-v1","event_count":2,"valid_event_count":2,"invalid_event_count":0,"equivocation_count":0,"current":{"canonical_record":{"metadata":{"abstract_canon_sha256":"f0018ba8ff99285b8e7217c3a5fa1571313489a4129f1c928048d47d0610417c","cross_cats_sorted":[],"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09Z","title_canon_sha256":"f0d962eb3cec9999ee9a555aa02f431469b37c70544bd8ab89e120596959646d"},"schema_version":"1.0","source":{"id":"2605.13016","kind":"arxiv","version":1}},"source_aliases":[{"alias_kind":"arxiv","alias_value":"2605.13016","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"arxiv_version","alias_value":"2605.13016v1","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2605.13016","created_at":"2026-05-18T03:09:00Z"},{"alias_kind":"pith_short_12","alias_value":"KYT4H77LO4VS","created_at":"2026-05-18T12:33:37Z"},{"alias_kind":"pith_short_16","alias_value":"KYT4H77LO4VSI2W5","created_at":"2026-05-18T12:33:37Z"},{"alias_kind":"pith_short_8","alias_value":"KYT4H77L","created_at":"2026-05-18T12:33:37Z"}],"graph_snapshots":[{"event_id":"sha256:842138bd806c8b13002aba458f716e79dd7ccf47c694b3ae51e8e9cb77ea8d4c","target":"graph","created_at":"2026-05-18T03:09:00Z","signer":{"key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","signer_id":"pith.science","signer_type":"pith_registry"},"payload":{"graph_snapshot":{"author_claims":{"count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","strong_count":0},"builder_version":"pith-number-builder-2026-05-17-v1","claims":{"count":4,"items":[{"attestation":"unclaimed","claim_id":"C1","kind":"strongest_claim","source":"verdict.strongest_claim","status":"machine_extracted","text":"From an MCMC analysis, we obtain the 95% C.L. upper bounds on the vector-to-scalar ratio as r_v < 1.55×10^{-4} and r_v < 1.04×10^{-2} for the νVI and νOCT modes at k0 = 0.01 Mpc^{-1}. We show that even a fully helical primordial vector mode cannot reproduce the currently observed EB signal while remaining consistent with parity-even CMB constraints."},{"attestation":"unclaimed","claim_id":"C2","kind":"weakest_assumption","source":"verdict.weakest_assumption","status":"machine_extracted","text":"The assumption that regular primordial vector modes are sustained by the anisotropic stress of free-streaming neutrinos under the specific neutrino velocity isocurvature (νVI) and octupole (νOCT) initial conditions."},{"attestation":"unclaimed","claim_id":"C3","kind":"one_line_summary","source":"verdict.one_line_summary","status":"machine_extracted","text":"Updated constraints on neutrino-sustained primordial vector modes imply magnetic fields too weak to seed observations and cannot reproduce the EB power spectrum while satisfying parity-even limits."},{"attestation":"unclaimed","claim_id":"C4","kind":"headline","source":"verdict.pith_extraction.headline","status":"machine_extracted","text":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum."}],"snapshot_sha256":"0fdefc08848f8d0c00b5d1d40991ca6388eeb8e91af3b48705ed21d5c59a641e"},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"paper":{"abstract_excerpt":"We revisit regular primordial vector modes sustained by the anisotropic stress of free-streaming neutrinos. We consider two classes of neutrino-sector initial conditions, the neutrino velocity isocurvature mode ($\\nu\\mathrm{VI}$) and the neutrino octupole mode ($\\nu\\mathrm{OCT}$). We update their observational constraints using current cosmological data, and examine the impact of including the BICEP/Keck 2018 $B$-mode polarization data. From an MCMC analysis, we obtain the 95\\% C.L. upper bounds on the vector-to-scalar ratio as $r_\\mathrm{v}<1.55\\times10^{-4}$ and $r_\\mathrm{v}<1.04\\times10^{-","authors_text":"Kaito Yura, Kiyotomo Ichiki, Shohei Saga, Shuichiro Yokoyama","cross_cats":[],"headline":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum.","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09Z","title":"Revisiting constraints on primordial vector modes and implications for sourced magnetic fields and observed $EB$ power spectrum"},"references":{"count":46,"internal_anchors":26,"resolved_work":46,"sample":[{"cited_arxiv_id":"1303.7121","doi":"","is_internal_anchor":true,"ref_index":1,"title":"Cosmological Magnetic Fields: Their Generation, Evolution and Observation","work_id":"b101da28-b381-4bc0-9176-e19d6d868643","year":2013},{"cited_arxiv_id":"","doi":"","is_internal_anchor":false,"ref_index":2,"title":"Rebhan, Large-Scale Rotational Perturbations of a Friedmann Universe with Collisionless Matter and Pri- mordial Magnetic Fields, ApJ392, 385 (1992)","work_id":"540969b0-f69c-4205-a21e-3c9a78c31511","year":1992},{"cited_arxiv_id":"astro-ph/0403583","doi":"","is_internal_anchor":true,"ref_index":3,"title":"Observable primordial vector modes","work_id":"96128296-ea06-440e-a335-149e2000c5cf","year":2004},{"cited_arxiv_id":"1112.4705","doi":"","is_internal_anchor":true,"ref_index":4,"title":"Constraint on the primordial vector mode and its magnetic field generation from seven-year Wilkinson Microwave Anisotropy Probe Observations","work_id":"a5a3f9a7-858b-4906-844f-4fb36e0c382c","year":2012},{"cited_arxiv_id":"1405.4810","doi":"","is_internal_anchor":true,"ref_index":5,"title":"Constraining primordial vector mode from B-mode polarization","work_id":"6c4631b0-dfe0-4dd3-8252-5dca98c9d001","year":2014}],"snapshot_sha256":"3d4d03368b452884f50029cc8bec6bf9a03b65f708f0429480463e50ac550f85"},"source":{"id":"2605.13016","kind":"arxiv","version":1},"verdict":{"created_at":"2026-05-14T18:35:37.725185Z","id":"ea6ef95c-2c83-4286-9c82-c56d7d16fda3","model_set":{"reader":"grok-4.3"},"one_line_summary":"Updated constraints on neutrino-sustained primordial vector modes imply magnetic fields too weak to seed observations and cannot reproduce the EB power spectrum while satisfying parity-even limits.","pipeline_version":"pith-pipeline@v0.9.0","pith_extraction_headline":"Cosmological data tightly bound neutrino-sustained vector modes, showing they cannot source observed magnetic fields or the EB power spectrum.","strongest_claim":"From an MCMC analysis, we obtain the 95% C.L. upper bounds on the vector-to-scalar ratio as r_v < 1.55×10^{-4} and r_v < 1.04×10^{-2} for the νVI and νOCT modes at k0 = 0.01 Mpc^{-1}. We show that even a fully helical primordial vector mode cannot reproduce the currently observed EB signal while remaining consistent with parity-even CMB constraints.","weakest_assumption":"The assumption that regular primordial vector modes are sustained by the anisotropic stress of free-streaming neutrinos under the specific neutrino velocity isocurvature (νVI) and octupole (νOCT) initial conditions."}},"verdict_id":"ea6ef95c-2c83-4286-9c82-c56d7d16fda3"}}],"author_attestations":[],"timestamp_anchors":[],"storage_attestations":[],"citation_signatures":[],"replication_records":[],"corrections":[],"mirror_hints":[],"record_created":{"event_id":"sha256:8a09201c9d083cc9ad175da21f63719a3073541e11e046611bf2ca0b0435700e","target":"record","created_at":"2026-05-18T03:09:00Z","signer":{"key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","signer_id":"pith.science","signer_type":"pith_registry"},"payload":{"attestation_state":"computed","canonical_record":{"metadata":{"abstract_canon_sha256":"f0018ba8ff99285b8e7217c3a5fa1571313489a4129f1c928048d47d0610417c","cross_cats_sorted":[],"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09Z","title_canon_sha256":"f0d962eb3cec9999ee9a555aa02f431469b37c70544bd8ab89e120596959646d"},"schema_version":"1.0","source":{"id":"2605.13016","kind":"arxiv","version":1}},"canonical_sha256":"5627c3ffeb772b246addcfc60d8d68dc3786b9664a032188a4433d8d4868b448","receipt":{"algorithm":"ed25519","builder_version":"pith-number-builder-2026-05-17-v1","canonical_sha256":"5627c3ffeb772b246addcfc60d8d68dc3786b9664a032188a4433d8d4868b448","first_computed_at":"2026-05-18T03:09:00.124303Z","key_id":"pith-v1-2026-05","kind":"pith_receipt","last_reissued_at":"2026-05-18T03:09:00.124303Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","receipt_version":"0.3","signature_b64":"2ErOP3Mfa89kTczfHihWytUUg5075FKPuporU1sIy9fInypcQlVgoaisfuAoXOSH6r2+EeLAackCUViRgQ/eBA==","signature_status":"signed_v1","signed_at":"2026-05-18T03:09:00.124926Z","signed_message":"canonical_sha256_bytes"},"source_id":"2605.13016","source_kind":"arxiv","source_version":1}}},"equivocations":[],"invalid_events":[],"applied_event_ids":["sha256:8a09201c9d083cc9ad175da21f63719a3073541e11e046611bf2ca0b0435700e","sha256:842138bd806c8b13002aba458f716e79dd7ccf47c694b3ae51e8e9cb77ea8d4c"],"state_sha256":"b5a2ad23118fa251e61175cdd9c0b19a42a33dff80eb94606e9256bfb9bd6a43"},"bundle_signature":{"signature_status":"signed_v1","algorithm":"ed25519","key_id":"pith-v1-2026-05","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54","signature_b64":"ZHD47Jr0xdP5j+jCtUuL97eplxvnIRDy2qtRtb2QPz4nFtMDQkSGF40eR9RcEPUmVL51vL7ivj95N/3asDXFBQ==","signed_message":"bundle_sha256_bytes","signed_at":"2026-05-30T04:13:18.396572Z","bundle_sha256":"d72d58097b1097743b04e40212d3a2ca4ac90f5e443105546be2bd55ea1443d5"}}