{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:XV5H257FW55MGNFYG3656MNP3A","short_pith_number":"pith:XV5H257F","schema_version":"1.0","canonical_sha256":"bd7a7d77e5b77ac334b836fddf31afd83a2a051e0c40a558f44ff14d1e875ad6","source":{"kind":"arxiv","id":"2012.01426","version":1},"attestation_state":"computed","paper":{"title":"Stellar Population Inference with Prospector","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Prospector infers stellar population parameters from UV-to-IR photometry and spectroscopy by forward modeling and Monte Carlo sampling of the posterior.","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"Benjamin D. Johnson, Charlie Conroy, Joel Leja, Joshua S. Speagle","submitted_at":"2020-12-02T19:00:00Z","abstract_excerpt":"Inference of the physical properties of stellar populations from observed photometry and spectroscopy is a key goal in the study of galaxy evolution. In recent years the quality and quantity of the available data has increased, and there have been corresponding efforts to increase the realism of the stellar population models used to interpret these observations. Describing the observed galaxy spectral energy distributions in detail now requires physical models with a large number of highly correlated parameters. These models do not fit easily on grids and necessitate a full exploration of the "},"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":true,"formal_links_present":true},"canonical_record":{"source":{"id":"2012.01426","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2020-12-02T19:00:00Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"11a6aaf42ae85fc87ef1ae570fec30e92bee9424b9bb28292ddfafa03d9aa8b2","abstract_canon_sha256":"69d7e353048a147d3b96d7838ce61918f0e8cf4874551991c3cc81626b3f4397"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:42:45.699385Z","signature_b64":"AQubUc83zMGF4UEOBjj15e+dcMQosCB1s6JDirk87EptxzFcO/z61TEPq9wjX6uYJAz+fX0+ejcnYtXUNArrAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd7a7d77e5b77ac334b836fddf31afd83a2a051e0c40a558f44ff14d1e875ad6","last_reissued_at":"2026-07-05T02:42:45.698330Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:42:45.698330Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stellar Population Inference with Prospector","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Prospector infers stellar population parameters from UV-to-IR photometry and spectroscopy by forward modeling and Monte Carlo sampling of the posterior.","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"Benjamin D. Johnson, Charlie Conroy, Joel Leja, Joshua S. Speagle","submitted_at":"2020-12-02T19:00:00Z","abstract_excerpt":"Inference of the physical properties of stellar populations from observed photometry and spectroscopy is a key goal in the study of galaxy evolution. In recent years the quality and quantity of the available data has increased, and there have been corresponding efforts to increase the realism of the stellar population models used to interpret these observations. Describing the observed galaxy spectral energy distributions in detail now requires physical models with a large number of highly correlated parameters. These models do not fit easily on grids and necessitate a full exploration of the "},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We present prospector, a flexible code for inferring stellar population parameters from photometry and spectroscopy spanning UV through IR wavelengths. This code is based on forward modeling the data and Monte Carlo sampling the posterior parameter distribution, enabling complex models and exploration of moderate dimensional parameter spaces.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the underlying stellar population synthesis models (including star-formation histories, dust, and nebular emission) are sufficiently realistic and that Monte Carlo sampling can efficiently explore the correlated parameter space without prohibitive computational cost or convergence issues.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Prospector is a flexible code for Bayesian inference of stellar population parameters from multi-wavelength photometry and spectroscopy via forward modeling and posterior sampling.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Prospector infers stellar population parameters from UV-to-IR photometry and spectroscopy by forward modeling and Monte Carlo sampling of the posterior.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"df111871aea409f128ac90a1a9b15c121b58fd3177fde024111d03a672af103c"},"source":{"id":"2012.01426","kind":"arxiv","version":1},"verdict":{"id":"16be4651-0f69-4354-85d1-9ed84e8ccf4e","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T22:08:08.265004Z","strongest_claim":"We present prospector, a flexible code for inferring stellar population parameters from photometry and spectroscopy spanning UV through IR wavelengths. This code is based on forward modeling the data and Monte Carlo sampling the posterior parameter distribution, enabling complex models and exploration of moderate dimensional parameter spaces.","one_line_summary":"Prospector is a flexible code for Bayesian inference of stellar population parameters from multi-wavelength photometry and spectroscopy via forward modeling and posterior sampling.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the underlying stellar population synthesis models (including star-formation histories, dust, and nebular emission) are sufficiently realistic and that Monte Carlo sampling can efficiently explore the correlated parameter space without prohibitive computational cost or convergence issues.","pith_extraction_headline":"Prospector infers stellar population parameters from UV-to-IR photometry and spectroscopy by forward modeling and Monte Carlo sampling of the posterior."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2012.01426/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":97,"sample":[{"doi":"","year":2011,"title":"2011, ApJ, 737, 47","work_id":"a5d265a1-2464-4fe5-8c42-b4f37396676d","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2020,"title":"2020, ApJS, 249, 3","work_id":"742e9e4e-a4ac-47c9-9246-3000749769b6","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2020,"title":"2020, ApJS, 249, 5 Astropy Collaboration, Robitaille, T","work_id":"66f3d450-090a-444e-be1d-db2c04cd801d","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2015,"title":"Becker, J. C., Johnson, J. A., Vand erburg, A., & Morton, T. D. 2015, ApJS, 217, 29","work_id":"1815946d-4610-48a3-b63f-b563f5224962","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2001,"title":"F., & de Jong, R","work_id":"b8b996ba-6019-4ccb-ba40-c3ed2501ae54","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":97,"snapshot_sha256":"1f029ec1fddcdc39a52eba30b79d3c7abb020d6471b4ba5138afc5de08292e56","internal_anchors":1},"formal_canon":{"evidence_count":2,"snapshot_sha256":"ab03afb6692e01b4becc02cf6a708c2b18243faf1e755c70c6708d19ea863a8c"},"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":"2012.01426","created_at":"2026-07-05T02:42:45.698416+00:00"},{"alias_kind":"arxiv_version","alias_value":"2012.01426v1","created_at":"2026-07-05T02:42:45.698416+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2012.01426","created_at":"2026-07-05T02:42:45.698416+00:00"},{"alias_kind":"pith_short_12","alias_value":"XV5H257FW55M","created_at":"2026-07-05T02:42:45.698416+00:00"},{"alias_kind":"pith_short_16","alias_value":"XV5H257FW55MGNFY","created_at":"2026-07-05T02:42:45.698416+00:00"},{"alias_kind":"pith_short_8","alias_value":"XV5H257F","created_at":"2026-07-05T02:42:45.698416+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":52,"internal_anchor_count":52,"sample":[{"citing_arxiv_id":"2607.07818","citing_title":"The DESI View of the Faint Radio Source Population in LoTSS DR2","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2607.07819","citing_title":"Compact Objects Merging with Stars as an Origin of Ultra-Long Gamma-Ray Bursts and Luminous Fast Blue Optical Transients","ref_index":111,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10009","citing_title":"Decadal pre-explosion activity and circumstellar interaction in a supernova","ref_index":150,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00982","citing_title":"Bar-driven secular evolution largely complete in a disk galaxy 7.6 billion years ago","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2607.00505","citing_title":"FRB20250613A: a remarkable repeating FRB with apparent millisecond-timescale scattering variations","ref_index":87,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01053","citing_title":"Bridging the gap between SLSNe and SE-SNe. Multi-wavelength analysis of the SLSN-Ib SN 2024jlc","ref_index":106,"is_internal_anchor":true},{"citing_arxiv_id":"2606.30787","citing_title":"JWST spectroscopy of galaxies at $z>10$: Damped Ly$\\alpha$ absorbers reveal efficient star formation and hidden redshift biases","ref_index":166,"is_internal_anchor":true},{"citing_arxiv_id":"2605.24088","citing_title":"Discovery and Analysis of a Type II Supernova Candidate at z = 3.19 from JWST's COSMOS-Web Survey","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28918","citing_title":"Late-time evolution of the interacting stripped-envelope supernova 2017dio","ref_index":127,"is_internal_anchor":true},{"citing_arxiv_id":"2605.25130","citing_title":"Exploring biases in derived stellar parameters and the ionizing photon production efficiency","ref_index":65,"is_internal_anchor":true},{"citing_arxiv_id":"2605.30410","citing_title":"RUBIES: The Evolution of the Ionization Parameter from 0 < z < 9","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2605.30513","citing_title":"The JADES Mass-Metallicity and Fundamental Metallicity Relations at $z\\gtrsim2$ Using New High-Redshift Metallicity Calibrations","ref_index":36,"is_internal_anchor":true},{"citing_arxiv_id":"2606.13351","citing_title":"Stellar Population Spectra Incorporating Detailed Binary Evolution using POSYDON","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02738","citing_title":"Signature of Bursty Star Formation in the High-Redshift Galaxies Detected with JWST","ref_index":187,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02698","citing_title":"Towards Unbreaking the Universe: MINERVA Measurements of Color Gradients in Massive Quiescent Galaxies Can Help Ease Too-Early Star Formation Tensions","ref_index":58,"is_internal_anchor":true},{"citing_arxiv_id":"2606.02685","citing_title":"A Steep-Extinction QSO at z=4.6: JWST Evidence for Abundant Small Dust Grains","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2606.03652","citing_title":"Systematically Measuring Ultra-Diffuse Galaxies. IX. A Gyr in the Life of Nearby Low Surface Brightness Galaxies","ref_index":48,"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":93,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10648","citing_title":"Star-formation variability on the star-forming main sequence during the Epoch of Reionization","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2606.11345","citing_title":"JADES: the mass-metallicity relation at $z=1-10$. New calibrations, extremely metal-poor galaxies, and chemical diversity","ref_index":92,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12249","citing_title":"Spatially Resolved Nebular-Stellar Reddening with JWST/NIRISS","ref_index":192,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18353","citing_title":"Late-time JWST/NIRCam Observations of the Extremely Long-duration GRB 250702B/EP 250702a and Its Host Galaxy","ref_index":45,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20804","citing_title":"LEGGOS II: A Strong Lens Model and Source-Plane Projection of the Clumpy Star-Forming Galaxy SGASJ111020.0+645950.8 at z=2.48","ref_index":11,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23869","citing_title":"A Strongly Lensed Ultra-faint Arc at $z \\approx 10$ with an F200W excess in Abell S1063","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23793","citing_title":"Discovery of a Barred-Spiral Galaxy at $z_{spec}$ = 3.16 II. The Star Formation History","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":2,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A","json":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A.json","graph_json":"https://pith.science/api/pith-number/XV5H257FW55MGNFYG3656MNP3A/graph.json","events_json":"https://pith.science/api/pith-number/XV5H257FW55MGNFYG3656MNP3A/events.json","paper":"https://pith.science/paper/XV5H257F"},"agent_actions":{"view_html":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A","download_json":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A.json","view_paper":"https://pith.science/paper/XV5H257F","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2012.01426&json=true","fetch_graph":"https://pith.science/api/pith-number/XV5H257FW55MGNFYG3656MNP3A/graph.json","fetch_events":"https://pith.science/api/pith-number/XV5H257FW55MGNFYG3656MNP3A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A/action/storage_attestation","attest_author":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A/action/author_attestation","sign_citation":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A/action/citation_signature","submit_replication":"https://pith.science/pith/XV5H257FW55MGNFYG3656MNP3A/action/replication_record"}},"created_at":"2026-07-05T02:42:45.698416+00:00","updated_at":"2026-07-05T02:42:45.698416+00:00"}