{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:D23N7XYJHZKUKMNF525JTVVGLI","short_pith_number":"pith:D23N7XYJ","schema_version":"1.0","canonical_sha256":"1eb6dfdf093e554531a5eeba99d6a65a13c587db9840b22ec57eb9f211493f55","source":{"kind":"arxiv","id":"1811.03637","version":2},"attestation_state":"computed","paper":{"title":"How to Measure Galaxy Star Formation Histories II: Nonparametric Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adam C. Carnall, Benjamin D. Johnson, Charlie Conroy, Joel Leja, Joshua S. Speagle","submitted_at":"2018-11-08T19:00:33Z","abstract_excerpt":"Nonparametric star formation histories (SFHs) have long promised to be the `gold standard' for galaxy spectral energy distribution (SED) modeling as they are flexible enough to describe the full diversity of SFH shapes, whereas parametric models rule out a significant fraction of these shapes {\\it a priori}. However, this flexibility is not fully constrained even with high-quality observations, making it critical to choose a well-motivated prior. Here, we use the SED-fitting code \\texttt{Prospector} to explore the effect of different nonparametric priors by fitting SFHs to mock UV-IR photometr"},"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":"1811.03637","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-11-08T19:00:33Z","cross_cats_sorted":[],"title_canon_sha256":"d36f01bfdc1555cbecf83a3d8aa69462482e718ed96f56e38ba1dc268e6bf8bc","abstract_canon_sha256":"bb44ef4dd09d4aad6a4a41503533cebfbedc609a8195425d23e19941611c6a8c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:47:29.646741Z","signature_b64":"EVuzbZLIU4Ll20NFd8ROUKtN3C1kHgP0bLoBpbPDhdum4aPC4pHoA2txDYj6tC/lxwtteGy5N3lKh5T7ON5yBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1eb6dfdf093e554531a5eeba99d6a65a13c587db9840b22ec57eb9f211493f55","last_reissued_at":"2026-05-17T23:47:29.646113Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:47:29.646113Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"How to Measure Galaxy Star Formation Histories II: Nonparametric Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adam C. Carnall, Benjamin D. Johnson, Charlie Conroy, Joel Leja, Joshua S. Speagle","submitted_at":"2018-11-08T19:00:33Z","abstract_excerpt":"Nonparametric star formation histories (SFHs) have long promised to be the `gold standard' for galaxy spectral energy distribution (SED) modeling as they are flexible enough to describe the full diversity of SFH shapes, whereas parametric models rule out a significant fraction of these shapes {\\it a priori}. However, this flexibility is not fully constrained even with high-quality observations, making it critical to choose a well-motivated prior. Here, we use the SED-fitting code \\texttt{Prospector} to explore the effect of different nonparametric priors by fitting SFHs to mock UV-IR photometr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1811.03637","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":"1811.03637","created_at":"2026-05-17T23:47:29.646219+00:00"},{"alias_kind":"arxiv_version","alias_value":"1811.03637v2","created_at":"2026-05-17T23:47:29.646219+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1811.03637","created_at":"2026-05-17T23:47:29.646219+00:00"},{"alias_kind":"pith_short_12","alias_value":"D23N7XYJHZKU","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_16","alias_value":"D23N7XYJHZKUKMNF","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_8","alias_value":"D23N7XYJ","created_at":"2026-05-18T12:32:19.392346+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":23,"internal_anchor_count":9,"sample":[{"citing_arxiv_id":"2605.23049","citing_title":"SDSS+JWST Census of Stellar and Nebular Dust Attenuation at $z \\sim 0$-7: Mass Dependence and Redshift Evolution","ref_index":64,"is_internal_anchor":true},{"citing_arxiv_id":"2509.25577","citing_title":"Characterizing the host galaxies and delay times of Ca-rich gap transients vs 91bg-like SNe and normal Type Ia SNe","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15893","citing_title":"Probing the faint end of simulated galaxy counts at z>3","ref_index":104,"is_internal_anchor":true},{"citing_arxiv_id":"2506.15779","citing_title":"Novel $z\\sim~10$ auroral line measurements extend the gradual offset of the FMR deep into the first Gyr of cosmic time","ref_index":13,"is_internal_anchor":true},{"citing_arxiv_id":"2509.16154","citing_title":"Lensed stars in galaxy-galaxy strong lensing -- a JWST prediction for the Cosmic Horseshoe","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2509.20430","citing_title":"pop-cosmos: Star formation over 12 Gyr from generative modelling of a deep infrared-selected galaxy catalogue","ref_index":140,"is_internal_anchor":true},{"citing_arxiv_id":"2601.02220","citing_title":"The NIRISS PASSAGE Spectroscopic Redshift Catalog in COSMOS","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"1904.02180","citing_title":"dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evidences","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13966","citing_title":"Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\\mathbf{z>3.5}$ from CAPERS","ref_index":119,"is_internal_anchor":true},{"citing_arxiv_id":"2604.01326","citing_title":"Calibrating Photometric Mid-Infrared Star Formation Rates for JWST","ref_index":99,"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":110,"is_internal_anchor":false},{"citing_arxiv_id":"2604.05024","citing_title":"Winding Back the Clock: Recent Star Formation Histories of Massive Quiescent Galaxies Are Consistent With Their Rapid Number Density Evolution Since $\\mathbf{z\\sim7}$","ref_index":70,"is_internal_anchor":false},{"citing_arxiv_id":"2604.07983","citing_title":"A Natural $\\gtrsim 100\\times$ Telescope: Discovery of the Strongly Lensed Type II SN 2025mkn at $z=1.37$","ref_index":52,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13211","citing_title":"Sparks: The Magellan/FIRE survey from starburst to post-starburst","ref_index":61,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13216","citing_title":"Sparks II: Panchromatic SED modeling and galaxy physical properties across the starburst to post-starburst sequence","ref_index":71,"is_internal_anchor":false},{"citing_arxiv_id":"2604.16597","citing_title":"Old Universe, Young SNe Ia: A Statistical Analysis of Type Ia Supernova Progenitor Age from 6,983 TITAN Host Galaxies, and Implications for Cosmology","ref_index":56,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18522","citing_title":"A Census of Na D-traced neutral ISM and outflows at $0.6<z<4$","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21007","citing_title":"DeepDive: Simultaneous Formation of Massive Quiescent Galaxies in High-Redshift Galaxy Proto-clusters","ref_index":73,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21516","citing_title":"SPURS: Bursty Star Formation in an Extremely Luminous Weak Emission Line Galaxy at $z=9.3$","ref_index":223,"is_internal_anchor":false},{"citing_arxiv_id":"2605.00822","citing_title":"PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26195","citing_title":"Resolved Maps of Gas and Dust in a Massive Quiescent Galaxy at z=2 from INQUEST-JWST: Evidence of Accretion and Rejuvenation","ref_index":59,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05548","citing_title":"A Multiwavelength Assessment Disfavoring the X-ray Binary Origin of He III Regions in Metal-Poor Star-Forming Dwarf Galaxies","ref_index":63,"is_internal_anchor":false},{"citing_arxiv_id":"2605.03000","citing_title":"Are Nucleosynthetic Yields Universal? Interpreting the Multi-Elemental Abundances of Quiescent Galaxies over Cosmic Time Using Milky Way Stars","ref_index":79,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI","json":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI.json","graph_json":"https://pith.science/api/pith-number/D23N7XYJHZKUKMNF525JTVVGLI/graph.json","events_json":"https://pith.science/api/pith-number/D23N7XYJHZKUKMNF525JTVVGLI/events.json","paper":"https://pith.science/paper/D23N7XYJ"},"agent_actions":{"view_html":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI","download_json":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI.json","view_paper":"https://pith.science/paper/D23N7XYJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1811.03637&json=true","fetch_graph":"https://pith.science/api/pith-number/D23N7XYJHZKUKMNF525JTVVGLI/graph.json","fetch_events":"https://pith.science/api/pith-number/D23N7XYJHZKUKMNF525JTVVGLI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI/action/storage_attestation","attest_author":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI/action/author_attestation","sign_citation":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI/action/citation_signature","submit_replication":"https://pith.science/pith/D23N7XYJHZKUKMNF525JTVVGLI/action/replication_record"}},"created_at":"2026-05-17T23:47:29.646219+00:00","updated_at":"2026-05-17T23:47:29.646219+00:00"}