{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:YDAZDPZJMCXJGH32LWBND5R6H6","short_pith_number":"pith:YDAZDPZJ","schema_version":"1.0","canonical_sha256":"c0c191bf2960ae931f7a5d82d1f63e3f9120a5ab6b185bde45981bdd5eccbeff","source":{"kind":"arxiv","id":"astro-ph/0106324","version":1},"attestation_state":"computed","paper":{"title":"Theoretical Modeling of Starburst Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"C. A. Heisler, J. Trevena, L. J. Kewley, M. A. Dopita, R. S. Sutherland","submitted_at":"2001-06-19T08:15:46Z","abstract_excerpt":"We have modeled a large sample of infrared starburst galaxies using both the PEGASE v2.0 and STARBURST99 codes to generate the spectral energy distribution of the young star clusters. PEGASE utilizes the Padova group tracks while STARBURST99 uses the Geneva group tracks, allowing comparison between the two. We used our MAPPINGS III code to compute photoionization models which include a self-consistent treatment of dust physics and chemical depletion. We use the standard optical diagnostic diagrams as indicators of the hardness of the EUV radiation field in these galaxies. These diagnostic diag"},"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":"astro-ph/0106324","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-06-19T08:15:46Z","cross_cats_sorted":[],"title_canon_sha256":"e78b3910e94223e94a93f539e3054af21d911f09abebe2678f47adb1c5a94a93","abstract_canon_sha256":"7bd55a8a2727e698d8a62afac66ded12a5140474103f4c9263151f745519d31a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T21:19:03.630138Z","signature_b64":"4TI+rajO6xYODecYjV5431kURVUJpVH0cwGsh4zIoMtAL+P2C4RRwRP1i5FygLAelUc5eva1fZ5VkzHA+wLqAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c0c191bf2960ae931f7a5d82d1f63e3f9120a5ab6b185bde45981bdd5eccbeff","last_reissued_at":"2026-07-04T21:19:03.629560Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T21:19:03.629560Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Theoretical Modeling of Starburst Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"C. A. Heisler, J. Trevena, L. J. Kewley, M. A. Dopita, R. S. Sutherland","submitted_at":"2001-06-19T08:15:46Z","abstract_excerpt":"We have modeled a large sample of infrared starburst galaxies using both the PEGASE v2.0 and STARBURST99 codes to generate the spectral energy distribution of the young star clusters. PEGASE utilizes the Padova group tracks while STARBURST99 uses the Geneva group tracks, allowing comparison between the two. We used our MAPPINGS III code to compute photoionization models which include a self-consistent treatment of dust physics and chemical depletion. We use the standard optical diagnostic diagrams as indicators of the hardness of the EUV radiation field in these galaxies. These diagnostic diag"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0106324","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/astro-ph/0106324/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":"astro-ph/0106324","created_at":"2026-07-04T21:19:03.629622+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0106324v1","created_at":"2026-07-04T21:19:03.629622+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0106324","created_at":"2026-07-04T21:19:03.629622+00:00"},{"alias_kind":"pith_short_12","alias_value":"YDAZDPZJMCXJ","created_at":"2026-07-04T21:19:03.629622+00:00"},{"alias_kind":"pith_short_16","alias_value":"YDAZDPZJMCXJGH32","created_at":"2026-07-04T21:19:03.629622+00:00"},{"alias_kind":"pith_short_8","alias_value":"YDAZDPZJ","created_at":"2026-07-04T21:19:03.629622+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":51,"internal_anchor_count":42,"sample":[{"citing_arxiv_id":"2607.07329","citing_title":"Beyond traditional emission-line diagnostics: using autoencoders to uncover active galactic nuclei in DESI spectra","ref_index":135,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01832","citing_title":"Post-starburst Galaxies with Active Galactic Nucleus: Properties and Evolutionary Sequences","ref_index":49,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00921","citing_title":"Spatially resolved optical and mid-infrared spectroscopy of SDSS1335+0728: implications for the origin of the Ansky event","ref_index":252,"is_internal_anchor":true},{"citing_arxiv_id":"2606.31960","citing_title":"Caught in the act: interaction-driven evolution in the nearby compact galaxy group Roberts Quartet (SCG0018-4854)","ref_index":91,"is_internal_anchor":true},{"citing_arxiv_id":"2606.31926","citing_title":"A Suppressed Volumetric Rate of High-Luminosity Mid-Infrared Selected Tidal Disruption Events","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2606.30715","citing_title":"Hunting Wandering 3<z<8 Black Holes: Spatial Offsets in Ionization Ratio and Continuum Emission","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09992","citing_title":"EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined Supernova","ref_index":110,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28489","citing_title":"pop-cosmos: Galaxy size evolution across structural and star-formation classifications in COSMOS-Web","ref_index":41,"is_internal_anchor":true},{"citing_arxiv_id":"2605.29616","citing_title":"An Obscured Tidal Disruption Event Uncovered by Its Mid- and Near-Infrared Dust Echo in a Star-Forming Galaxy","ref_index":75,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27675","citing_title":"OzSSy1: The Australian Southern Seyfert-1 Spectroscopic Atlas and Catalogue at z < 0.1","ref_index":78,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02699","citing_title":"A New Record Census of Dwarf AGN and a Bimodal $M_{\\rm BH}$-$M_{\\star}$ Scaling Relation with DESI DR1","ref_index":129,"is_internal_anchor":true},{"citing_arxiv_id":"2606.08987","citing_title":"The origin of WHAM Point Source~46","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10160","citing_title":"Aether-SHELLQs: JWST integral-field spectroscopy of candidate obscured quasars at z ~ 6","ref_index":75,"is_internal_anchor":true},{"citing_arxiv_id":"2606.11308","citing_title":"pop-cosmos: Disentangling galaxy properties from observables using data-driven approaches","ref_index":39,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10558","citing_title":"Hector Galaxy Survey: Linking the low- and high-mass ends of the initial mass function in star-forming galaxies","ref_index":206,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12541","citing_title":"DESI as sparse Integral Field Spectrograph I: Spatially resolved chemical enrichment in star-forming galaxies at $z\\leq0.1$","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25995","citing_title":"The evolution of the galaxy gas-phase mass-metallicity relation from $z=15$ to $z=0$ in the COLIBRE cosmological simulations","ref_index":204,"is_internal_anchor":true},{"citing_arxiv_id":"2606.17152","citing_title":"Hector Galaxy Survey: Optical IFU and Chandra Reveal a Low-Luminosity AGN Behind Extended LINER Emission","ref_index":58,"is_internal_anchor":true},{"citing_arxiv_id":"2606.17144","citing_title":"Decoupled Kinematics and Excitation in the Compton-thick AGN NGC 6552: Spatially Resolved KOOLS-IFU Observations","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2606.17444","citing_title":"GRB 250424A: A Case Study of Energy Injection with Multiwavelength Observations","ref_index":114,"is_internal_anchor":true},{"citing_arxiv_id":"2606.21007","citing_title":"Clumpy Disk, Interloper, or Merger? Nature of a Distant Galaxy Pair at 5 kpc Projected Separation","ref_index":35,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23649","citing_title":"The EDGE-CALIFA Survey: Star Formation Efficiency and Galaxy Quenching across 62 Main Sequence, Green Valley, and Red Galaxies","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27057","citing_title":"Unveiling a cosmic tango: Integral field spectroscopy and numerical simulations of Arp 143's interaction","ref_index":66,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26355","citing_title":"Probing the Nature of Lyman Continuum Emitting and Low-metallicity Galaxies Using the SKA","ref_index":215,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24211","citing_title":"Jet-ISM Interaction and Multi-channel AGN Feedback in the Post-merger Galaxy 4C+29.30","ref_index":49,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6","json":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6.json","graph_json":"https://pith.science/api/pith-number/YDAZDPZJMCXJGH32LWBND5R6H6/graph.json","events_json":"https://pith.science/api/pith-number/YDAZDPZJMCXJGH32LWBND5R6H6/events.json","paper":"https://pith.science/paper/YDAZDPZJ"},"agent_actions":{"view_html":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6","download_json":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6.json","view_paper":"https://pith.science/paper/YDAZDPZJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0106324&json=true","fetch_graph":"https://pith.science/api/pith-number/YDAZDPZJMCXJGH32LWBND5R6H6/graph.json","fetch_events":"https://pith.science/api/pith-number/YDAZDPZJMCXJGH32LWBND5R6H6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6/action/storage_attestation","attest_author":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6/action/author_attestation","sign_citation":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6/action/citation_signature","submit_replication":"https://pith.science/pith/YDAZDPZJMCXJGH32LWBND5R6H6/action/replication_record"}},"created_at":"2026-07-04T21:19:03.629622+00:00","updated_at":"2026-07-04T21:19:03.629622+00:00"}