{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:IXWFLB5HLA4KCWKUUJZT7RWLU4","short_pith_number":"pith:IXWFLB5H","schema_version":"1.0","canonical_sha256":"45ec5587a75838a15954a2733fc6cba7062e57b9906a3b2b169206cc2052a5e2","source":{"kind":"arxiv","id":"2306.16228","version":2},"attestation_state":"computed","paper":{"title":"The second data release from the European Pulsar Timing Array: VI. Challenging the ultralight dark matter paradigm","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA","gr-qc","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. Berthereau, A. Chalumeau, A. Franchini, A. G. Lyne, A. Jessner, A. Parthasarathy, A. Petiteau, A. Possenti, A. Samajdar, A.-S. Bak Nielsen, A. Sesana, A. Vecchio, B. B. P. Perera, Boris Goncharov, B. W. Stappers, C. G. Bassa, Clemente Smarra, C. Tiburzi, D. Izquierdo-Villalba, D. J. Champion, D. Perrodin, E. Bortolas, E. F. Keane, E. Graikou, Enrico Barausse, E. van der Wateren, F. Iraci, G. Desvignes, G. H. Janssen, G. Shaifullah, G. Theureau, H. Hu, H. Quelquejay Leclere, I. C. Ni\\c{t}u, I. Cognard, J. Antoniadis, J. Jang, J. Jawor, J.-M. Grie, J. R. Gair, J. Wang, J. W. McKee, K. J. Lee, K. Lackeos, K. Liu, L. Guillemot, L. Speri, L. Wang, M. A. Krishnakumar, M. B. Mickaliger, M. Bonetti, M. Burgay, M. Falxa, M. J. Keith, M. Kramer, N. K. Porayko, P. R. Brook, R. A. Main, R. D. Ferdman, R. Karuppusamy, R. N. Caballero, R. Spiewak, S. A. Sanidas, S. Babak, S. Chanlaridis, S. Chen, S. C. Susarla, V. Venkatraman Krishnan, Y. J. Guo, Y. Liu, Z. Wu","submitted_at":"2023-06-28T13:51:16Z","abstract_excerpt":"Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results show that ultralight particles with masses $10^{-24.0}~\\text{eV} \\lesssim m \\lesssim 10^{-23.3}~\\text{eV}$ cannot constitute $100\\%$ of the measured local dark matter density, but can have at most loca"},"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":"2306.16228","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-06-28T13:51:16Z","cross_cats_sorted":["astro-ph.CO","astro-ph.GA","gr-qc","hep-ph"],"title_canon_sha256":"14bafe48caf697a060256b271b565954c5d13ba72e3abbda8cc32da09f1ac3f9","abstract_canon_sha256":"1b41d7a0b5472f55817d82d4e1974d89a1fcdcbbce00d8fbacf89b80c673b6e5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:04:48.972695Z","signature_b64":"1HRCh02vriMkjrxKFoIdK9J3dqqg7UXHjfBQF7/V7a4i+yGkCevmltPbesFNANIghQws0hrjW9OX6BWY79GeAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"45ec5587a75838a15954a2733fc6cba7062e57b9906a3b2b169206cc2052a5e2","last_reissued_at":"2026-07-05T07:04:48.972265Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:04:48.972265Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The second data release from the European Pulsar Timing Array: VI. Challenging the ultralight dark matter paradigm","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA","gr-qc","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. Berthereau, A. Chalumeau, A. Franchini, A. G. Lyne, A. Jessner, A. Parthasarathy, A. Petiteau, A. Possenti, A. Samajdar, A.-S. Bak Nielsen, A. Sesana, A. Vecchio, B. B. P. Perera, Boris Goncharov, B. W. Stappers, C. G. Bassa, Clemente Smarra, C. Tiburzi, D. Izquierdo-Villalba, D. J. Champion, D. Perrodin, E. Bortolas, E. F. Keane, E. Graikou, Enrico Barausse, E. van der Wateren, F. Iraci, G. Desvignes, G. H. Janssen, G. Shaifullah, G. Theureau, H. Hu, H. Quelquejay Leclere, I. C. Ni\\c{t}u, I. Cognard, J. Antoniadis, J. Jang, J. Jawor, J.-M. Grie, J. R. Gair, J. Wang, J. W. McKee, K. J. Lee, K. Lackeos, K. Liu, L. Guillemot, L. Speri, L. Wang, M. A. Krishnakumar, M. B. Mickaliger, M. Bonetti, M. Burgay, M. Falxa, M. J. Keith, M. Kramer, N. K. Porayko, P. R. Brook, R. A. Main, R. D. Ferdman, R. Karuppusamy, R. N. Caballero, R. Spiewak, S. A. Sanidas, S. Babak, S. Chanlaridis, S. Chen, S. C. Susarla, V. Venkatraman Krishnan, Y. J. Guo, Y. Liu, Z. Wu","submitted_at":"2023-06-28T13:51:16Z","abstract_excerpt":"Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results show that ultralight particles with masses $10^{-24.0}~\\text{eV} \\lesssim m \\lesssim 10^{-23.3}~\\text{eV}$ cannot constitute $100\\%$ of the measured local dark matter density, but can have at most loca"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.16228","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/2306.16228/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":"2306.16228","created_at":"2026-07-05T07:04:48.972321+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.16228v2","created_at":"2026-07-05T07:04:48.972321+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.16228","created_at":"2026-07-05T07:04:48.972321+00:00"},{"alias_kind":"pith_short_12","alias_value":"IXWFLB5HLA4K","created_at":"2026-07-05T07:04:48.972321+00:00"},{"alias_kind":"pith_short_16","alias_value":"IXWFLB5HLA4KCWKU","created_at":"2026-07-05T07:04:48.972321+00:00"},{"alias_kind":"pith_short_8","alias_value":"IXWFLB5H","created_at":"2026-07-05T07:04:48.972321+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.28571","citing_title":"The NANOGrav 15 yr Data Set: Customized Chromatic Noise Models","ref_index":77,"is_internal_anchor":false},{"citing_arxiv_id":"2606.28554","citing_title":"The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave Analyses","ref_index":63,"is_internal_anchor":false},{"citing_arxiv_id":"2506.15496","citing_title":"Thermodynamical uncertainties for primordial black holes from cosmological phase transitions","ref_index":16,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08373","citing_title":"Stochastic problems in pulsar timing","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02172","citing_title":"Constraints on Ultralight Scalar and Dark Photon Dark Matter from PPTA-DR3 and EPTA-DR2","ref_index":32,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4","json":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4.json","graph_json":"https://pith.science/api/pith-number/IXWFLB5HLA4KCWKUUJZT7RWLU4/graph.json","events_json":"https://pith.science/api/pith-number/IXWFLB5HLA4KCWKUUJZT7RWLU4/events.json","paper":"https://pith.science/paper/IXWFLB5H"},"agent_actions":{"view_html":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4","download_json":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4.json","view_paper":"https://pith.science/paper/IXWFLB5H","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.16228&json=true","fetch_graph":"https://pith.science/api/pith-number/IXWFLB5HLA4KCWKUUJZT7RWLU4/graph.json","fetch_events":"https://pith.science/api/pith-number/IXWFLB5HLA4KCWKUUJZT7RWLU4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4/action/storage_attestation","attest_author":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4/action/author_attestation","sign_citation":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4/action/citation_signature","submit_replication":"https://pith.science/pith/IXWFLB5HLA4KCWKUUJZT7RWLU4/action/replication_record"}},"created_at":"2026-07-05T07:04:48.972321+00:00","updated_at":"2026-07-05T07:04:48.972321+00:00"}