{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:2Y3B3JJDSFBNNUBLE7SMIRCZHS","short_pith_number":"pith:2Y3B3JJD","schema_version":"1.0","canonical_sha256":"d6361da5239142d6d02b27e4c444593cbfa2745db2294f171ebe0c836b4a86b5","source":{"kind":"arxiv","id":"1809.08239","version":2},"attestation_state":"computed","paper":{"title":"The optical morphologies of galaxies in the IllustrisTNG simulation: a comparison to Pan-STARRS observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Annalisa Pillepich, David A. Thilker, Dylan Nelson, Federico Marinacci, Gregory F. Snyder, Jennifer M. Lotz, Lars Hernquist, Mark Vogelsberger, Paul Torrey, Rainer Weinberger, Ruediger Pakmor, Sandro Tacchella, Shy Genel, Vicente Rodriguez-Gomez, Volker Springel","submitted_at":"2018-09-21T18:00:00Z","abstract_excerpt":"We have generated synthetic images of $\\sim$27,000 galaxies from the IllustrisTNG and the original Illustris hydrodynamic cosmological simulations, designed to match Pan-STARRS observations of $\\log_{10}(M_{\\ast}/{\\rm M}_{\\odot}) \\approx 9.8$-$11.3$ galaxies at $z \\approx 0.05$. Most of our synthetic images were created with the SKIRT radiative transfer code, including the effects of dust attenuation and scattering, and performing the radiative transfer directly on the Voronoi mesh used by the simulations themselves. We have analysed both our synthetic and real Pan-STARRS images with the newly"},"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":"1809.08239","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-09-21T18:00:00Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"1e1016877c90798304c49451de7ea1be8f14a48365c330ac4a255655aacd8078","abstract_canon_sha256":"64ea454bd67ba887dbac17ee056c6144b35ecfddbf2873518ec33cb626a03016"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:56:47.124643Z","signature_b64":"iKAbCyHCxWtsvLjrm5OmxSmgPqWlie3v8oQ5oqj8+gZRwdzy2FGAuRkupEdZwuVcNIqF8HCAQWw8Q6b4FhFmAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d6361da5239142d6d02b27e4c444593cbfa2745db2294f171ebe0c836b4a86b5","last_reissued_at":"2026-05-17T23:56:47.124242Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:56:47.124242Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The optical morphologies of galaxies in the IllustrisTNG simulation: a comparison to Pan-STARRS observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Annalisa Pillepich, David A. Thilker, Dylan Nelson, Federico Marinacci, Gregory F. Snyder, Jennifer M. Lotz, Lars Hernquist, Mark Vogelsberger, Paul Torrey, Rainer Weinberger, Ruediger Pakmor, Sandro Tacchella, Shy Genel, Vicente Rodriguez-Gomez, Volker Springel","submitted_at":"2018-09-21T18:00:00Z","abstract_excerpt":"We have generated synthetic images of $\\sim$27,000 galaxies from the IllustrisTNG and the original Illustris hydrodynamic cosmological simulations, designed to match Pan-STARRS observations of $\\log_{10}(M_{\\ast}/{\\rm M}_{\\odot}) \\approx 9.8$-$11.3$ galaxies at $z \\approx 0.05$. Most of our synthetic images were created with the SKIRT radiative transfer code, including the effects of dust attenuation and scattering, and performing the radiative transfer directly on the Voronoi mesh used by the simulations themselves. We have analysed both our synthetic and real Pan-STARRS images with the newly"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1809.08239","kind":"arxiv","version":2},"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":"1809.08239","created_at":"2026-05-17T23:56:47.124309+00:00"},{"alias_kind":"arxiv_version","alias_value":"1809.08239v2","created_at":"2026-05-17T23:56:47.124309+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1809.08239","created_at":"2026-05-17T23:56:47.124309+00:00"},{"alias_kind":"pith_short_12","alias_value":"2Y3B3JJDSFBN","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_16","alias_value":"2Y3B3JJDSFBNNUBL","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_8","alias_value":"2Y3B3JJD","created_at":"2026-05-18T12:32:02.567920+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":10,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2511.09644","citing_title":"statmorph-lsst: Quantifying and correcting morphological biases in galaxy surveys","ref_index":104,"is_internal_anchor":false},{"citing_arxiv_id":"2603.05287","citing_title":"The Local Tremaine-Weinberg Method for Galactic Pattern Speed: Theory and its Application to IllustrisTNG","ref_index":35,"is_internal_anchor":false},{"citing_arxiv_id":"2605.06782","citing_title":"The galaxy ultraviolet luminosity function from $z=7$ to $15$ in the COLIBRE simulations","ref_index":165,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08682","citing_title":"The Hubble sequence in JWST CEERS from unbiased galaxy morphologies","ref_index":98,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13408","citing_title":"ALESS--JWST: Dust-driven Morphologies and Hidden Stellar Mass in $z\\sim3$ Sub-millimeter Galaxies","ref_index":84,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18209","citing_title":"Galaxy Populations in the IllustrisTNG Caustic Skeleton","ref_index":161,"is_internal_anchor":false},{"citing_arxiv_id":"2605.00349","citing_title":"A Universal Dance of Galactic Disks: Ubiquitous Precession and Its Implications","ref_index":48,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26743","citing_title":"A Rare Eddington-Limited, Heavily Obscured Low-Mass Active Galactic Nucleus Likely Triggered by a Galaxy Merger","ref_index":91,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01981","citing_title":"A Comprehensive Study of Morphology and Kinematics in Extended Nebulae Around UV Luminous Quasars at $z\\approx1$","ref_index":80,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02493","citing_title":"Morphological and Star Formation Properties of Cosmic Noon Massive Quiescent Galaxies","ref_index":82,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS","json":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS.json","graph_json":"https://pith.science/api/pith-number/2Y3B3JJDSFBNNUBLE7SMIRCZHS/graph.json","events_json":"https://pith.science/api/pith-number/2Y3B3JJDSFBNNUBLE7SMIRCZHS/events.json","paper":"https://pith.science/paper/2Y3B3JJD"},"agent_actions":{"view_html":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS","download_json":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS.json","view_paper":"https://pith.science/paper/2Y3B3JJD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1809.08239&json=true","fetch_graph":"https://pith.science/api/pith-number/2Y3B3JJDSFBNNUBLE7SMIRCZHS/graph.json","fetch_events":"https://pith.science/api/pith-number/2Y3B3JJDSFBNNUBLE7SMIRCZHS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS/action/storage_attestation","attest_author":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS/action/author_attestation","sign_citation":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS/action/citation_signature","submit_replication":"https://pith.science/pith/2Y3B3JJDSFBNNUBLE7SMIRCZHS/action/replication_record"}},"created_at":"2026-05-17T23:56:47.124309+00:00","updated_at":"2026-05-17T23:56:47.124309+00:00"}