{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:O3XOFLEEVIWOBINSP764FFYXQJ","short_pith_number":"pith:O3XOFLEE","schema_version":"1.0","canonical_sha256":"76eee2ac84aa2ce0a1b27ffdc29717826fa821b8947d2e88a2a98cfb128d847e","source":{"kind":"arxiv","id":"0803.2706","version":1},"attestation_state":"computed","paper":{"title":"Toward a halo mass function for precision cosmology: the limits of universality","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anatoly Klypin, Andrey V Kravtsov, Daniel E Holz, Gustavo Yepes, Jeremy L Tinker, Kevork Abazajian, Michael S Warren, Stefan Gottlober","submitted_at":"2008-03-18T22:17:55Z","abstract_excerpt":"We measure the mass function of dark matter halos in a large set of collisionless cosmological simulations of flat LCDM cosmology and investigate its evolution at z<~2. Halos are identified as isolated density peaks, and their masses are measured within a series of radii enclosing specific overdensities. We argue that these spherical overdensity masses are more directly linked to cluster observables than masses measured using the friends-of-friends algorithm (FOF), and are therefore preferable for accurate forecasts of halo abundances. Our simulation set allows us to calibrate the mass functio"},"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":"0803.2706","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-03-18T22:17:55Z","cross_cats_sorted":[],"title_canon_sha256":"5a9d1895aea62c034c1b77225f41b8310fefcf072df997e1add8ee7fab62fc58","abstract_canon_sha256":"a3abcd47403e76192d9acc2079ac3b2dbeb19baf1e6b964064402983eb0a6b5c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:29:33.731612Z","signature_b64":"2wEccrCRZDIGIF7ZxjINT8ylX1YFBygpJmBYILHqqqcKpb5FoSH1mza6/etuFTxB8bCEItoMjoz9ynKKoHKoAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"76eee2ac84aa2ce0a1b27ffdc29717826fa821b8947d2e88a2a98cfb128d847e","last_reissued_at":"2026-05-18T04:29:33.731197Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:29:33.731197Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Toward a halo mass function for precision cosmology: the limits of universality","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anatoly Klypin, Andrey V Kravtsov, Daniel E Holz, Gustavo Yepes, Jeremy L Tinker, Kevork Abazajian, Michael S Warren, Stefan Gottlober","submitted_at":"2008-03-18T22:17:55Z","abstract_excerpt":"We measure the mass function of dark matter halos in a large set of collisionless cosmological simulations of flat LCDM cosmology and investigate its evolution at z<~2. Halos are identified as isolated density peaks, and their masses are measured within a series of radii enclosing specific overdensities. We argue that these spherical overdensity masses are more directly linked to cluster observables than masses measured using the friends-of-friends algorithm (FOF), and are therefore preferable for accurate forecasts of halo abundances. Our simulation set allows us to calibrate the mass functio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0803.2706","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":""},"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":"0803.2706","created_at":"2026-05-18T04:29:33.731263+00:00"},{"alias_kind":"arxiv_version","alias_value":"0803.2706v1","created_at":"2026-05-18T04:29:33.731263+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0803.2706","created_at":"2026-05-18T04:29:33.731263+00:00"},{"alias_kind":"pith_short_12","alias_value":"O3XOFLEEVIWO","created_at":"2026-05-18T12:25:57.157939+00:00"},{"alias_kind":"pith_short_16","alias_value":"O3XOFLEEVIWOBINS","created_at":"2026-05-18T12:25:57.157939+00:00"},{"alias_kind":"pith_short_8","alias_value":"O3XOFLEE","created_at":"2026-05-18T12:25:57.157939+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":20,"internal_anchor_count":10,"sample":[{"citing_arxiv_id":"1906.08174","citing_title":"Optical follow-up study of 32 high-redshift galaxy cluster candidates from Planck with the William Herschel Telescope","ref_index":54,"is_internal_anchor":true},{"citing_arxiv_id":"2503.16355","citing_title":"DEMNUni: the Sunyaev-Zel'dovich effect in the presence of massive neutrinos and dynamical dark energy","ref_index":63,"is_internal_anchor":true},{"citing_arxiv_id":"2509.03458","citing_title":"Comparison of Halo Model and Simulation Predictions for Projected-Field Kinematic Sunyaev-Zel'dovich Cross-Correlations","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20393","citing_title":"The Splashback Mass Function of Galaxy Clusters from Photometric Data","ref_index":68,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15264","citing_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","ref_index":161,"is_internal_anchor":true},{"citing_arxiv_id":"2509.07097","citing_title":"Constraining Gas Mass Fractions in Galaxy Groups and Clusters with the First CHIME/FRB Outrigger","ref_index":90,"is_internal_anchor":true},{"citing_arxiv_id":"2509.07960","citing_title":"The evolution of the galaxy stellar mass function and star formation rates in the COLIBRE simulations from redshift 17 to 0","ref_index":150,"is_internal_anchor":true},{"citing_arxiv_id":"2511.13708","citing_title":"Statistics Meet Systematics: Resolution of the Massive Early JWST Galaxy Tension","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2602.02778","citing_title":"Probing The Dark Matter Halo of High-redshift Quasar from Wide-Field Clustering Analysis","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2605.11083","citing_title":"FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2605.11083","citing_title":"FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26015","citing_title":"Kinematic Lensing Ratio: Reviving Weak Lensing Cosmography as a Geometric Dark Energy Probe","ref_index":101,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13866","citing_title":"Dark energy, spatial curvature, and star formation efficiency from JWST photometric and spectroscopic high-redshift galaxies","ref_index":145,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17162","citing_title":"Signatures of Suppressed Matter Clustering revealed by Fast Radio Bursts","ref_index":58,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18801","citing_title":"Preserving Clusters in Error-Bounded Lossy Compression of Particle Data","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17981","citing_title":"Efficiently emulating distribution functions in gigaparsec volumes for varying cosmological parameters","ref_index":61,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19865","citing_title":"A population-based approach to understanding radio AGN feedback with LOFAR: The LoTSS Deep Fields","ref_index":105,"is_internal_anchor":false},{"citing_arxiv_id":"2604.23236","citing_title":"The functional form of galaxy and halo luminosity and mass functions","ref_index":71,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22105","citing_title":"Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers","ref_index":106,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02723","citing_title":"Euclid preparation. CosmoPostProcess: A simulation calibrated framework for weak lensing selection bias in richness-selected galaxy clusters","ref_index":17,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ","json":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ.json","graph_json":"https://pith.science/api/pith-number/O3XOFLEEVIWOBINSP764FFYXQJ/graph.json","events_json":"https://pith.science/api/pith-number/O3XOFLEEVIWOBINSP764FFYXQJ/events.json","paper":"https://pith.science/paper/O3XOFLEE"},"agent_actions":{"view_html":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ","download_json":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ.json","view_paper":"https://pith.science/paper/O3XOFLEE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0803.2706&json=true","fetch_graph":"https://pith.science/api/pith-number/O3XOFLEEVIWOBINSP764FFYXQJ/graph.json","fetch_events":"https://pith.science/api/pith-number/O3XOFLEEVIWOBINSP764FFYXQJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ/action/storage_attestation","attest_author":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ/action/author_attestation","sign_citation":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ/action/citation_signature","submit_replication":"https://pith.science/pith/O3XOFLEEVIWOBINSP764FFYXQJ/action/replication_record"}},"created_at":"2026-05-18T04:29:33.731263+00:00","updated_at":"2026-05-18T04:29:33.731263+00:00"}