{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:DHGVJF5Q5V3GKCP2PMJHN266EP","short_pith_number":"pith:DHGVJF5Q","schema_version":"1.0","canonical_sha256":"19cd5497b0ed766509fa7b1276ebde23f597689c6cb50ab4b6ff07faf5cdb812","source":{"kind":"arxiv","id":"1001.1223","version":3},"attestation_state":"computed","paper":{"title":"Stellar atmosphere parameters with MAx, a MAssive compression of x^2 for spectral fitting","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"Achim Weiss, Ben Panter, Camilla Juul Hansen, Paula Jofr\\'e","submitted_at":"2010-01-08T14:49:08Z","abstract_excerpt":"MAx is a new tool to estimate parameters from stellar spectra. It is based on the maximum likelihood method, with the likelihood compressed in a way that the information stored in the spectral fluxes is conserved. The compressed data are given by the size of the number of parameters, rather than by the number of flux points. The optimum speed-up reached by the compression is the ratio of the data set to the number of parameters. The method has been tested on a sample of low-resolution spectra from the Sloan Extension for Galactic Understanding and Exploration (SEGUE) survey for the estimate of"},"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":"1001.1223","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2010-01-08T14:49:08Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"0669e4d7f3a5ca79a2d19a7b49b62aa04e387afa00f752d46d871d846f63bbc2","abstract_canon_sha256":"3d4e75acee5566ed8f7511a53ff25287ed6a0fa93ff3706aed11d9fcca0955bf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:10:03.845810Z","signature_b64":"v+cHSQ+e/Q2G7uNlW6wVMFrVT+oMlQurlanvBaAhHqPfCJ/PE4TnHBehzGs4OU8mrCb9mtXRfhP3q8nT+x7gAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"19cd5497b0ed766509fa7b1276ebde23f597689c6cb50ab4b6ff07faf5cdb812","last_reissued_at":"2026-05-18T02:10:03.845381Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:10:03.845381Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stellar atmosphere parameters with MAx, a MAssive compression of x^2 for spectral fitting","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"Achim Weiss, Ben Panter, Camilla Juul Hansen, Paula Jofr\\'e","submitted_at":"2010-01-08T14:49:08Z","abstract_excerpt":"MAx is a new tool to estimate parameters from stellar spectra. It is based on the maximum likelihood method, with the likelihood compressed in a way that the information stored in the spectral fluxes is conserved. The compressed data are given by the size of the number of parameters, rather than by the number of flux points. The optimum speed-up reached by the compression is the ratio of the data set to the number of parameters. The method has been tested on a sample of low-resolution spectra from the Sloan Extension for Galactic Understanding and Exploration (SEGUE) survey for the estimate of"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1001.1223","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":""},"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":"1001.1223","created_at":"2026-05-18T02:10:03.845448+00:00"},{"alias_kind":"arxiv_version","alias_value":"1001.1223v3","created_at":"2026-05-18T02:10:03.845448+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1001.1223","created_at":"2026-05-18T02:10:03.845448+00:00"},{"alias_kind":"pith_short_12","alias_value":"DHGVJF5Q5V3G","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_16","alias_value":"DHGVJF5Q5V3GKCP2","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_8","alias_value":"DHGVJF5Q","created_at":"2026-05-18T12:26:06.534383+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/DHGVJF5Q5V3GKCP2PMJHN266EP","json":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP.json","graph_json":"https://pith.science/api/pith-number/DHGVJF5Q5V3GKCP2PMJHN266EP/graph.json","events_json":"https://pith.science/api/pith-number/DHGVJF5Q5V3GKCP2PMJHN266EP/events.json","paper":"https://pith.science/paper/DHGVJF5Q"},"agent_actions":{"view_html":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP","download_json":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP.json","view_paper":"https://pith.science/paper/DHGVJF5Q","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1001.1223&json=true","fetch_graph":"https://pith.science/api/pith-number/DHGVJF5Q5V3GKCP2PMJHN266EP/graph.json","fetch_events":"https://pith.science/api/pith-number/DHGVJF5Q5V3GKCP2PMJHN266EP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP/action/storage_attestation","attest_author":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP/action/author_attestation","sign_citation":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP/action/citation_signature","submit_replication":"https://pith.science/pith/DHGVJF5Q5V3GKCP2PMJHN266EP/action/replication_record"}},"created_at":"2026-05-18T02:10:03.845448+00:00","updated_at":"2026-05-18T02:10:03.845448+00:00"}