{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:63BGB63EKGLDEWOY7WKPDN65LR","short_pith_number":"pith:63BGB63E","schema_version":"1.0","canonical_sha256":"f6c260fb6451963259d8fd94f1b7dd5c5591405ab80d1636b35239c2f42c9c94","source":{"kind":"arxiv","id":"2502.03529","version":1},"attestation_state":"computed","paper":{"title":"Stellar population synthesis models with a physically varying IMF","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Akram Hasani Zonoozi, Hosein Haghi, Pavel Kroupa","submitted_at":"2025-02-05T19:00:02Z","abstract_excerpt":"Interpreting galactic luminosity requires assumptions about the galaxy-wide initial mass function (gwIMF), often assumed invariant in most stellar population synthesis (SPS) models. If stars form in clusters with metallicity- and density-dependent \\textit{stellar IMFs}, the integrated galaxy-wide IMF (IGIMF) can be calculated, with its shape depending on the star formation rate (SFR) and metallicity. The shape of the IGIMF thus depends on the star formation rate (SFR) and metallicity. We develop the \\texttt{SPS-VarIMF} code which enables us for the first time to compute the spectra, luminositi"},"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":"2502.03529","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2025-02-05T19:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"42fceca264dd023c6e44e9f155310b9dd73b2ff1967046e3d1888412d69756f6","abstract_canon_sha256":"466c45b0c06ea517822d4df54bd6c09a7883ccd28fef37eebb0ab86c55ce285b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:10:11.716897Z","signature_b64":"I/XFBxgXt5D+X+mSLQ9R3Tt7/1GnjB+yscNdPm+SFipByh3jqwvpFZ0xAh6bioz9yr9qJshmd5n0OCernIMcDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f6c260fb6451963259d8fd94f1b7dd5c5591405ab80d1636b35239c2f42c9c94","last_reissued_at":"2026-07-05T10:10:11.716405Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:10:11.716405Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stellar population synthesis models with a physically varying IMF","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Akram Hasani Zonoozi, Hosein Haghi, Pavel Kroupa","submitted_at":"2025-02-05T19:00:02Z","abstract_excerpt":"Interpreting galactic luminosity requires assumptions about the galaxy-wide initial mass function (gwIMF), often assumed invariant in most stellar population synthesis (SPS) models. If stars form in clusters with metallicity- and density-dependent \\textit{stellar IMFs}, the integrated galaxy-wide IMF (IGIMF) can be calculated, with its shape depending on the star formation rate (SFR) and metallicity. The shape of the IGIMF thus depends on the star formation rate (SFR) and metallicity. We develop the \\texttt{SPS-VarIMF} code which enables us for the first time to compute the spectra, luminositi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2502.03529","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2502.03529/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":"2502.03529","created_at":"2026-07-05T10:10:11.716465+00:00"},{"alias_kind":"arxiv_version","alias_value":"2502.03529v1","created_at":"2026-07-05T10:10:11.716465+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2502.03529","created_at":"2026-07-05T10:10:11.716465+00:00"},{"alias_kind":"pith_short_12","alias_value":"63BGB63EKGLD","created_at":"2026-07-05T10:10:11.716465+00:00"},{"alias_kind":"pith_short_16","alias_value":"63BGB63EKGLDEWOY","created_at":"2026-07-05T10:10:11.716465+00:00"},{"alias_kind":"pith_short_8","alias_value":"63BGB63E","created_at":"2026-07-05T10:10:11.716465+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.19454","citing_title":"Baryonic mass budgets in the central regions of the Bullet Cluster and their consistency with strong lensing in MOND","ref_index":47,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR","json":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR.json","graph_json":"https://pith.science/api/pith-number/63BGB63EKGLDEWOY7WKPDN65LR/graph.json","events_json":"https://pith.science/api/pith-number/63BGB63EKGLDEWOY7WKPDN65LR/events.json","paper":"https://pith.science/paper/63BGB63E"},"agent_actions":{"view_html":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR","download_json":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR.json","view_paper":"https://pith.science/paper/63BGB63E","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2502.03529&json=true","fetch_graph":"https://pith.science/api/pith-number/63BGB63EKGLDEWOY7WKPDN65LR/graph.json","fetch_events":"https://pith.science/api/pith-number/63BGB63EKGLDEWOY7WKPDN65LR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR/action/storage_attestation","attest_author":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR/action/author_attestation","sign_citation":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR/action/citation_signature","submit_replication":"https://pith.science/pith/63BGB63EKGLDEWOY7WKPDN65LR/action/replication_record"}},"created_at":"2026-07-05T10:10:11.716465+00:00","updated_at":"2026-07-05T10:10:11.716465+00:00"}