{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:Q4DIQHECNETMNL4THEHFKCSPIT","short_pith_number":"pith:Q4DIQHEC","schema_version":"1.0","canonical_sha256":"8706881c826926c6af93390e550a4f44d3a5cb026881e6756ad8af82961b2001","source":{"kind":"arxiv","id":"1103.2324","version":1},"attestation_state":"computed","paper":{"title":"Keck Observations of the Young Metal-Poor Host Galaxy of the Super-Chandrasekhar-Mass Type Ia Supernova SN 2007if","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Canto, B. A. Weaver, C. Aragon, C. Baltay, C. Buton, C. Tao, C. Wu, D. Rabinowitz, E. Gangler, E. Pecontal, E. Y. Hsiao, G. Aldering, G. Smadja, H. K. Fakhouri, K. Paech, K. Runge, M. Childress, M. Kerschhaggl, M. Kowalski, N. Chotard, P. Antilogus, P. Nugent, R. C. Thomas, R. Pain, R. Pereira, R. Scalzo, S. Bailey, S. Bongard, S. Loken, S. Perlmutter, Y. Copin","submitted_at":"2011-03-11T17:55:28Z","abstract_excerpt":"We present Keck LRIS spectroscopy and $g$-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be $m_g=23.15\\pm0.06$, which at the spectroscopically-measured redshift of $z_{helio}=0.07450\\pm0.00015$ corresponds to an absolute magnitude of $M_g=-14.45\\pm0.06$. Galaxy $g-r$ color constrains the mass-to-light ratio, giving a host stellar mass estimate of $\\log(M_*/M_\\odot)=7.32\\pm0.17$. Balmer absorption in the stellar continuum, along with the strength of the 4000\\AA\\"},"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":"1103.2324","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-03-11T17:55:28Z","cross_cats_sorted":[],"title_canon_sha256":"1bd87c6b10d377aa953f08bb56c773573d31ea9d9b24c4b9cdf479658352fdf4","abstract_canon_sha256":"d57d9d81e3d726fb50888af2f203c802ec8c20f1098d0cce2a721fe14503838d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:02:54.501583Z","signature_b64":"Iov1NRP0pt1DtopTXLH8SPR5hneiZQinA0ZDizplWMm6o8iBngZcGntZBkoFuoX56lJhu2UMSKERTw7+Y9rlCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8706881c826926c6af93390e550a4f44d3a5cb026881e6756ad8af82961b2001","last_reissued_at":"2026-05-18T02:02:54.500862Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:02:54.500862Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Keck Observations of the Young Metal-Poor Host Galaxy of the Super-Chandrasekhar-Mass Type Ia Supernova SN 2007if","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Canto, B. A. Weaver, C. Aragon, C. Baltay, C. Buton, C. Tao, C. Wu, D. Rabinowitz, E. Gangler, E. Pecontal, E. Y. Hsiao, G. Aldering, G. Smadja, H. K. Fakhouri, K. Paech, K. Runge, M. Childress, M. Kerschhaggl, M. Kowalski, N. Chotard, P. Antilogus, P. Nugent, R. C. Thomas, R. Pain, R. Pereira, R. Scalzo, S. Bailey, S. Bongard, S. Loken, S. Perlmutter, Y. Copin","submitted_at":"2011-03-11T17:55:28Z","abstract_excerpt":"We present Keck LRIS spectroscopy and $g$-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be $m_g=23.15\\pm0.06$, which at the spectroscopically-measured redshift of $z_{helio}=0.07450\\pm0.00015$ corresponds to an absolute magnitude of $M_g=-14.45\\pm0.06$. Galaxy $g-r$ color constrains the mass-to-light ratio, giving a host stellar mass estimate of $\\log(M_*/M_\\odot)=7.32\\pm0.17$. Balmer absorption in the stellar continuum, along with the strength of the 4000\\AA\\"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1103.2324","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":"1103.2324","created_at":"2026-05-18T02:02:54.500982+00:00"},{"alias_kind":"arxiv_version","alias_value":"1103.2324v1","created_at":"2026-05-18T02:02:54.500982+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1103.2324","created_at":"2026-05-18T02:02:54.500982+00:00"},{"alias_kind":"pith_short_12","alias_value":"Q4DIQHECNETM","created_at":"2026-05-18T12:26:39.201973+00:00"},{"alias_kind":"pith_short_16","alias_value":"Q4DIQHECNETMNL4T","created_at":"2026-05-18T12:26:39.201973+00:00"},{"alias_kind":"pith_short_8","alias_value":"Q4DIQHEC","created_at":"2026-05-18T12:26:39.201973+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT","json":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT.json","graph_json":"https://pith.science/api/pith-number/Q4DIQHECNETMNL4THEHFKCSPIT/graph.json","events_json":"https://pith.science/api/pith-number/Q4DIQHECNETMNL4THEHFKCSPIT/events.json","paper":"https://pith.science/paper/Q4DIQHEC"},"agent_actions":{"view_html":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT","download_json":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT.json","view_paper":"https://pith.science/paper/Q4DIQHEC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1103.2324&json=true","fetch_graph":"https://pith.science/api/pith-number/Q4DIQHECNETMNL4THEHFKCSPIT/graph.json","fetch_events":"https://pith.science/api/pith-number/Q4DIQHECNETMNL4THEHFKCSPIT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT/action/storage_attestation","attest_author":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT/action/author_attestation","sign_citation":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT/action/citation_signature","submit_replication":"https://pith.science/pith/Q4DIQHECNETMNL4THEHFKCSPIT/action/replication_record"}},"created_at":"2026-05-18T02:02:54.500982+00:00","updated_at":"2026-05-18T02:02:54.500982+00:00"}