{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:2W6XHQMAUGQ6XFDWFAR6IS242L","short_pith_number":"pith:2W6XHQMA","schema_version":"1.0","canonical_sha256":"d5bd73c180a1a1eb94762823e44b5cd2f22fc39fbe9c68361b2968da4b25def7","source":{"kind":"arxiv","id":"2309.04526","version":3},"attestation_state":"computed","paper":{"title":"Synchrotron Emission on FIRE: Equipartition Estimators of Magnetic Fields in Simulated Galaxies with Spectrally-Resolved Cosmic Rays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Cameron Hummels, Claude-Andr\\'e Faucher-Gigu\\`ere, Du\\v{s}an Kere\\v{s}, Eliot Quataert, Georgia V. Panopoulou, Iryna S. Butsky, Kung-Yi Su, Philip F. Hopkins, Raphael Skalidis, Sam B. Ponnada","submitted_at":"2023-09-08T18:00:02Z","abstract_excerpt":"Synchrotron emission is one of few observable tracers of galactic magnetic fields (\\textbf{B}) and cosmic rays (CRs). Much of our understanding of \\textbf{B} in galaxies comes from utilizing synchrotron observations in conjunction with several simplifying assumptions of equipartition models, however it remains unclear how well these assumptions hold, and what \\textbf{B} these estimates physically represent. Using FIRE simulations which self consistently evolve CR proton, electron, and positron spectra from MeV to TeV energies, we present the first synthetic synchrotron emission predictions fro"},"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":"2309.04526","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-09-08T18:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"efb1462d6e3183ca8d391696837a317c111b30b335832a3101e9a27cd5d13188","abstract_canon_sha256":"f37711e6bf8479cd5ea32c8c477517315e9072d7421accf870807c507fb84a56"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:31:54.415433Z","signature_b64":"iXJUY3THtEF0LA9G+r81ZikI8iQtZQSMCL9bdpJB8C/ASnI2kpJ5FkhV2oBwJCKH8KPUjCqQ1VRrN82VGcf4BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d5bd73c180a1a1eb94762823e44b5cd2f22fc39fbe9c68361b2968da4b25def7","last_reissued_at":"2026-07-05T07:31:54.414962Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:31:54.414962Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Synchrotron Emission on FIRE: Equipartition Estimators of Magnetic Fields in Simulated Galaxies with Spectrally-Resolved Cosmic Rays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Cameron Hummels, Claude-Andr\\'e Faucher-Gigu\\`ere, Du\\v{s}an Kere\\v{s}, Eliot Quataert, Georgia V. Panopoulou, Iryna S. Butsky, Kung-Yi Su, Philip F. Hopkins, Raphael Skalidis, Sam B. Ponnada","submitted_at":"2023-09-08T18:00:02Z","abstract_excerpt":"Synchrotron emission is one of few observable tracers of galactic magnetic fields (\\textbf{B}) and cosmic rays (CRs). Much of our understanding of \\textbf{B} in galaxies comes from utilizing synchrotron observations in conjunction with several simplifying assumptions of equipartition models, however it remains unclear how well these assumptions hold, and what \\textbf{B} these estimates physically represent. Using FIRE simulations which self consistently evolve CR proton, electron, and positron spectra from MeV to TeV energies, we present the first synthetic synchrotron emission predictions fro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2309.04526","kind":"arxiv","version":3},"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/2309.04526/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":"2309.04526","created_at":"2026-07-05T07:31:54.415017+00:00"},{"alias_kind":"arxiv_version","alias_value":"2309.04526v3","created_at":"2026-07-05T07:31:54.415017+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2309.04526","created_at":"2026-07-05T07:31:54.415017+00:00"},{"alias_kind":"pith_short_12","alias_value":"2W6XHQMAUGQ6","created_at":"2026-07-05T07:31:54.415017+00:00"},{"alias_kind":"pith_short_16","alias_value":"2W6XHQMAUGQ6XFDW","created_at":"2026-07-05T07:31:54.415017+00:00"},{"alias_kind":"pith_short_8","alias_value":"2W6XHQMA","created_at":"2026-07-05T07:31:54.415017+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.00493","citing_title":"Non-linear Dynamical Stability of Magnetic Polytropes","ref_index":59,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L","json":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L.json","graph_json":"https://pith.science/api/pith-number/2W6XHQMAUGQ6XFDWFAR6IS242L/graph.json","events_json":"https://pith.science/api/pith-number/2W6XHQMAUGQ6XFDWFAR6IS242L/events.json","paper":"https://pith.science/paper/2W6XHQMA"},"agent_actions":{"view_html":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L","download_json":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L.json","view_paper":"https://pith.science/paper/2W6XHQMA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2309.04526&json=true","fetch_graph":"https://pith.science/api/pith-number/2W6XHQMAUGQ6XFDWFAR6IS242L/graph.json","fetch_events":"https://pith.science/api/pith-number/2W6XHQMAUGQ6XFDWFAR6IS242L/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L/action/storage_attestation","attest_author":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L/action/author_attestation","sign_citation":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L/action/citation_signature","submit_replication":"https://pith.science/pith/2W6XHQMAUGQ6XFDWFAR6IS242L/action/replication_record"}},"created_at":"2026-07-05T07:31:54.415017+00:00","updated_at":"2026-07-05T07:31:54.415017+00:00"}