{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:MMATH73UNOQXG7H7UBKWAWZQML","short_pith_number":"pith:MMATH73U","schema_version":"1.0","canonical_sha256":"630133ff746ba1737cffa055605b3062e9c32a6473d67cd762b3c26dc637b223","source":{"kind":"arxiv","id":"1207.6105","version":2},"attestation_state":"computed","paper":{"title":"The Average Star Formation Histories of Galaxies in Dark Matter Halos from z=0-8","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) UC Santa Cruz), Charlie Conroy (2) ((1) KIPAC, Peter S. Behroozi (1), Risa H. Wechsler (1), Stanford University","submitted_at":"2012-07-25T20:00:00Z","abstract_excerpt":"We present a robust method to constrain average galaxy star formation rates, star formation histories, and the intracluster light as a function of halo mass. Our results are consistent with observed galaxy stellar mass functions, specific star formation rates, and cosmic star formation rates from z=0 to z=8. We consider the effects of a wide range of uncertainties on our results, including those affecting stellar masses, star formation rates, and the halo mass function at the heart of our analysis. As they are relevant to our method, we also present new calibrations of the dark matter halo mas"},"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":"1207.6105","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-07-25T20:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"51e03ab998219df548bbd612e462d442ac2e2942d202b2cb7c10cec0b0fece02","abstract_canon_sha256":"b529d8f5a181bfe1d750d9b25ffa16a8ec5e9a46284b1fa3557af13d0027f5c5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:22:18.858522Z","signature_b64":"KyuIABn/bNbUNrmpomZwY9lGEJgsc+NaLJuaaNnUduglg5UyHJc0O2ehEKL40xTd5ohRXUej7Fo1+pDCLJvbCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"630133ff746ba1737cffa055605b3062e9c32a6473d67cd762b3c26dc637b223","last_reissued_at":"2026-05-18T03:22:18.857802Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:22:18.857802Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Average Star Formation Histories of Galaxies in Dark Matter Halos from z=0-8","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) UC Santa Cruz), Charlie Conroy (2) ((1) KIPAC, Peter S. Behroozi (1), Risa H. Wechsler (1), Stanford University","submitted_at":"2012-07-25T20:00:00Z","abstract_excerpt":"We present a robust method to constrain average galaxy star formation rates, star formation histories, and the intracluster light as a function of halo mass. Our results are consistent with observed galaxy stellar mass functions, specific star formation rates, and cosmic star formation rates from z=0 to z=8. We consider the effects of a wide range of uncertainties on our results, including those affecting stellar masses, star formation rates, and the halo mass function at the heart of our analysis. As they are relevant to our method, we also present new calibrations of the dark matter halo mas"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.6105","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":"1207.6105","created_at":"2026-05-18T03:22:18.857918+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.6105v2","created_at":"2026-05-18T03:22:18.857918+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.6105","created_at":"2026-05-18T03:22:18.857918+00:00"},{"alias_kind":"pith_short_12","alias_value":"MMATH73UNOQX","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_16","alias_value":"MMATH73UNOQXG7H7","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_8","alias_value":"MMATH73U","created_at":"2026-05-18T12:27:14.488303+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":24,"internal_anchor_count":11,"sample":[{"citing_arxiv_id":"2605.23554","citing_title":"Inferring the role of binary neutron star mergers in r-process nucleosynthesis with multi-messenger observations using Cosmic Explorer and Einstein Telescope","ref_index":192,"is_internal_anchor":true},{"citing_arxiv_id":"1907.02977","citing_title":"Realistic simulations of galaxy formation in f(R) modified gravity","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20590","citing_title":"Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\\beta$ narrow-band imaging","ref_index":163,"is_internal_anchor":true},{"citing_arxiv_id":"2605.16485","citing_title":"Halo-driven Origin and Suppression of Over-massive Black Holes and Little Red Dots","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17253","citing_title":"HI Observations of Baryon-Dominated Dwarf Galaxy Candidates","ref_index":35,"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":93,"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":13,"is_internal_anchor":true},{"citing_arxiv_id":"2512.04362","citing_title":"ELG$\\times$LRG distribution through dark matter halo dynamics","ref_index":12,"is_internal_anchor":true},{"citing_arxiv_id":"2601.22213","citing_title":"Little Red Dots on FIRE: The Ability of Bursty Galaxies to Host an Abundant Population of High-Redshift AGN","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"1712.04452","citing_title":"Inferring the star-formation histories of massive quiescent galaxies with BAGPIPES: Evidence for multiple quenching mechanisms","ref_index":8,"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":27,"is_internal_anchor":true},{"citing_arxiv_id":"2605.08342","citing_title":"Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters","ref_index":4,"is_internal_anchor":false},{"citing_arxiv_id":"2605.08342","citing_title":"Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters","ref_index":4,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":89,"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":11,"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":2,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17963","citing_title":"BEACON: JWST NIRCam Pure-parallel Imaging Survey. III. Constraints on the UV LF and the Clustering of z~7-14 Galaxies","ref_index":286,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19449","citing_title":"Cosmological constraints from the small scale clustering of Emission Line Galaxies","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2604.27477","citing_title":"The Critical Mass in Galaxy Evolution","ref_index":3,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25560","citing_title":"Massive black holes and their galaxies","ref_index":24,"is_internal_anchor":false},{"citing_arxiv_id":"2604.23236","citing_title":"The functional form of galaxy and halo luminosity and mass functions","ref_index":7,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04776","citing_title":"Redshift Evolution of the Ratio of Supermassive Black Hole Mass to Stellar Mass","ref_index":7,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04144","citing_title":"The galaxy-halo connection and the dynamical evolution of a giant disc in a massive node of the Cosmic Web at z~3","ref_index":77,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02999","citing_title":"Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas","ref_index":80,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML","json":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML.json","graph_json":"https://pith.science/api/pith-number/MMATH73UNOQXG7H7UBKWAWZQML/graph.json","events_json":"https://pith.science/api/pith-number/MMATH73UNOQXG7H7UBKWAWZQML/events.json","paper":"https://pith.science/paper/MMATH73U"},"agent_actions":{"view_html":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML","download_json":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML.json","view_paper":"https://pith.science/paper/MMATH73U","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.6105&json=true","fetch_graph":"https://pith.science/api/pith-number/MMATH73UNOQXG7H7UBKWAWZQML/graph.json","fetch_events":"https://pith.science/api/pith-number/MMATH73UNOQXG7H7UBKWAWZQML/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML/action/storage_attestation","attest_author":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML/action/author_attestation","sign_citation":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML/action/citation_signature","submit_replication":"https://pith.science/pith/MMATH73UNOQXG7H7UBKWAWZQML/action/replication_record"}},"created_at":"2026-05-18T03:22:18.857918+00:00","updated_at":"2026-05-18T03:22:18.857918+00:00"}