{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:DQKAAWLGJ6BUSBXJQS4X2KJ7DK","short_pith_number":"pith:DQKAAWLG","schema_version":"1.0","canonical_sha256":"1c140059664f834906e984b97d293f1aabb450f1a2f5a884651a4beeb5f85e14","source":{"kind":"arxiv","id":"1507.07560","version":1},"attestation_state":"computed","paper":{"title":"Probing the isotropy of cosmic acceleration traced by Type Ia supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Behnam Javanmardi (Bonn), Cristiano Porciani (Bonn), Jan Pflamm-Altenburg (Bonn), Pavel Kroupa (Bonn)","submitted_at":"2015-07-27T20:00:44Z","abstract_excerpt":"We present a method to test the isotropy of the magnitude-redshift relation of Type Ia Supernovae (SNe Ia) and single out the most discrepant direction (in terms of the signal-to-noise ratio) with respect to the all-sky data. Our technique accounts for possible directional variations of the corrections for SNe Ia and yields all-sky maps of the best-fit cosmological parameters with arbitrary angular resolution. To show its potential, we apply our method to the recent Union2.1 compilation, building maps with three different angular resolutions. We use a Monte Carlo method to estimate the statist"},"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":"1507.07560","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2015-07-27T20:00:44Z","cross_cats_sorted":[],"title_canon_sha256":"86d4ddaff9c3f4e02c9541046311c433baaa55f2efab255a1b5a6cf4493be0f1","abstract_canon_sha256":"ac6e6aebda9f1aeb7df5a049fb83f0f5947ed4f7adb994795800d473ea091620"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:34:37.442301Z","signature_b64":"ONap8nd83T6vwapsfJ9+bYOMF5E7c/XgIhBO4EcSomoBNVdGZcdSBbki+lJNucvshuswG4ltUz78zoOFhsByAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1c140059664f834906e984b97d293f1aabb450f1a2f5a884651a4beeb5f85e14","last_reissued_at":"2026-05-18T01:34:37.441563Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:34:37.441563Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing the isotropy of cosmic acceleration traced by Type Ia supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Behnam Javanmardi (Bonn), Cristiano Porciani (Bonn), Jan Pflamm-Altenburg (Bonn), Pavel Kroupa (Bonn)","submitted_at":"2015-07-27T20:00:44Z","abstract_excerpt":"We present a method to test the isotropy of the magnitude-redshift relation of Type Ia Supernovae (SNe Ia) and single out the most discrepant direction (in terms of the signal-to-noise ratio) with respect to the all-sky data. Our technique accounts for possible directional variations of the corrections for SNe Ia and yields all-sky maps of the best-fit cosmological parameters with arbitrary angular resolution. To show its potential, we apply our method to the recent Union2.1 compilation, building maps with three different angular resolutions. We use a Monte Carlo method to estimate the statist"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1507.07560","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":"1507.07560","created_at":"2026-05-18T01:34:37.441700+00:00"},{"alias_kind":"arxiv_version","alias_value":"1507.07560v1","created_at":"2026-05-18T01:34:37.441700+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1507.07560","created_at":"2026-05-18T01:34:37.441700+00:00"},{"alias_kind":"pith_short_12","alias_value":"DQKAAWLGJ6BU","created_at":"2026-05-18T12:29:17.054201+00:00"},{"alias_kind":"pith_short_16","alias_value":"DQKAAWLGJ6BUSBXJ","created_at":"2026-05-18T12:29:17.054201+00:00"},{"alias_kind":"pith_short_8","alias_value":"DQKAAWLG","created_at":"2026-05-18T12:29:17.054201+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":125,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK","json":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK.json","graph_json":"https://pith.science/api/pith-number/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/graph.json","events_json":"https://pith.science/api/pith-number/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/events.json","paper":"https://pith.science/paper/DQKAAWLG"},"agent_actions":{"view_html":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK","download_json":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK.json","view_paper":"https://pith.science/paper/DQKAAWLG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1507.07560&json=true","fetch_graph":"https://pith.science/api/pith-number/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/graph.json","fetch_events":"https://pith.science/api/pith-number/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/action/storage_attestation","attest_author":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/action/author_attestation","sign_citation":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/action/citation_signature","submit_replication":"https://pith.science/pith/DQKAAWLGJ6BUSBXJQS4X2KJ7DK/action/replication_record"}},"created_at":"2026-05-18T01:34:37.441700+00:00","updated_at":"2026-05-18T01:34:37.441700+00:00"}