{"arxiv_id":"1001.1737","incoming":{"papers":16,"sentences":21,"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":8,"sentences":11,"quotes":[{"arxiv_id":"2512.23157","title":"The GLASS-JWST Early Release Science Program. V. H$\\alpha$ luminosity functions at $z\\sim1.3$ and $z\\sim2.0$","url":"/paper/2512.23157","section":"LF results","sentence":"When calculating the errors, we consider Poisson noise for the small number statistics [ref] and also include the uncertainty caused by cosmic variance following the methods in [ref] , which estimates large-scale density fluctuations as the product of the galaxy bias [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"2604.05022","title":"PANORAMIC: The Dawn of Massive Quiescent Galaxies I. Number Density and Cosmic Variance from 1000 arcmin$^2$ NIRCam Imaging","url":"/paper/2604.05022","section":"Method","sentence":"To estimate $σ̃_CV$, we use the code developed by [ref] , which is based on the [ref] cosmic-variance calculator, combined with constraints from the UniverseMachine simulations [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"2512.14212","title":"Exploring Cosmic Dawn with PANORAMIC II: Cosmic Variance and Galaxy Clustering at $z\\sim10$","url":"/paper/2512.14212","section":"Bootstrapping","sentence":"following e.g. [ref] and [ref] where N stands for the completeness corrected galaxy number counts per field, $μ=⟨N⟩$ is the mean number count, and we make use of the fact that the Poisson contribution to the variance is $σ_Poisson^2=⟨N⟩$.","intent_p":0.97,"contests_p":null},{"arxiv_id":"1009.0269","title":"The Most Massive Galaxies at 3.0<z<4.0 in the NEWFIRM Medium-Band Survey: Properties and Improved Constraints on the Stellar Mass Function","url":"/paper/1009.0269","section":"Uncertainties on the Stellar Mass Function","sentence":"We have derived the cosmic variance following the cosmic variance cookbook presented by [ref] and using the parameters for our survey and for a population of massive galaxies with $M_star>10^11$ M$_$, resulting in an uncertainty due to cosmic variance of 0.18 dex, in very good agreement with our empirical estimate.","intent_p":0.98,"contests_p":null},{"arxiv_id":"2608.08203","title":"A New Window on the H{\\alpha} Luminosity Function and Star Formation Rate Density from 1.2 < z < 6.6 from JWST Medium-Band Photometry","url":"/paper/2608.08203","section":"Redshift Evolution","sentence":"Uncertainties from cosmic variance are incorporated directly in the Monte Carlo by perturbing each realization with a field-combined fractional cosmic variance term estimated from the [ref] calculator, combining the CANUCS pointings as independent volumes following [ref] .","intent_p":0.98,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites it as support","papers":1,"sentences":1,"quotes":[{"arxiv_id":"2605.11077","title":"The Impact of Cosmic Variance and Satellites on JWST Clustering Measurements at Redshift around 6","url":"/paper/2605.11077","section":"Introduction","sentence":"The narrow pencil-beam fields of JWST/WFSS ($≈2' ×2'$ each) make cosmic variance the dominant source of uncertainty [ref] , and the highly biased tracers at $z > 5$ further amplify the effect.","intent_p":0.98,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":3,"sentences":3,"quotes":[{"arxiv_id":"2512.14212","title":"Exploring Cosmic Dawn with PANORAMIC II: Cosmic Variance and Galaxy Clustering at $z\\sim10$","url":"/paper/2512.14212","section":"Introduction","sentence":"They are therefore subject to significant cosmic variance, which describes fluctuations in the number density of galaxies because of their clustering in the cosmic web [ref] .","intent_p":0.95,"contests_p":null},{"arxiv_id":"2604.05022","title":"PANORAMIC: The Dawn of Massive Quiescent Galaxies I. Number Density and Cosmic Variance from 1000 arcmin$^2$ NIRCam Imaging","url":"/paper/2604.05022","section":"Cosmic variance of massive quiescent galaxies at redshift $z∼3$–8","sentence":"In pencil-beam surveys, these fluctuations are often dominated by cosmic variance, i.e., the clustering-driven excess (relative to Poisson) variance obtained by integrating the power spectrum weighted by the survey window function [ref] .","intent_p":0.92,"contests_p":null},{"arxiv_id":"2305.04520","title":"Minkowski Functionals of Large-Scale Structure as a Probe of Modified Gravity","url":"/paper/2305.04520","section":"Cosmic variance","sentence":"It is important for both cosmological parameter estimation and future survey design, and it has been extensively studied for various LSS statistics [ref] .","intent_p":0.98,"contests_p":null}]}],"unlabelled_sentences":6},"outgoing":{"papers":1,"sentences":5,"groups":[{"kind":"data_used","label":"Uses data or values from","papers":1,"sentences":2,"quotes":[{"arxiv_id":"0903.4682","title":"Constraints on the relationship between stellar mass and halo mass at low and high redshift","url":"/paper/0903.4682","section":"Conclusions","sentence":"We have used the galaxy bias predictions by [ref] (for six stellar mass bins and six thresholds) and the dark matter cosmic variance to compute the cosmic variance for galaxies.","intent_p":0.83,"contests_p":null}]}],"unlabelled_sentences":3},"claims":[],"thresholds":{"intent_p":0.8,"supports_p":0.95,"contests_p":0.7},"method":"Citing sentences come from each paper's LaTeX source; every \\cite marks the sentence and the works it cites. Pith's classifier typed each sentence. A label is shown at intent probability 0.8 or more (0.95 for support), a contest at 0.7 or more. Measured accuracy against two blind model families is at https://pith.science/accuracy. The quoted sentences are the citing authors' own.","held_up":{"arxiv_id":"1001.1737","kind":"model","paper_version":1,"prompt_version":"held-up-v3.5","generated_at":"2026-10-27T17:06:56+00:00","loaded_at":"2026-10-28T01:02:53.618414+00:00","evidence":"substantial","account":[],"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":15,"entries":[{"p":1.0,"quote":{"text":"To estimate $σ̃_CV$, we use the code developed by [ref] , which is based on the [ref] cosmic-variance calculator, combined with constraints from the UniverseMachine simulations [ref] .","citing":"2604.05022","section":"Method"},"citing":[{"self":false,"year":2026,"title":"PANORAMIC: The Dawn of Massive Quiescent Galaxies I. Number Density and Cosmic Variance from 1000 arcmin$^2$ NIRCam Imaging","arxiv_id":"2604.05022"}],"verified":true,"paraphrase":"Used a code based on this paper's cosmic-variance calculator, combined with constraints from the UniverseMachine simulations, to estimate cosmic variance."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2021,"title":"Evolution of the galaxy stellar mass function: evidence for an increasing $M^*$ from $z=2$ to the present day","arxiv_id":"2101.07182"}],"verified":true,"paraphrase":"Used this paper's treatment, which estimates cosmic variance as a function of both stellar mass and redshift, to model the effects of cosmic variance on its measurements."},{"p":0.97,"quote":null,"citing":[{"self":false,"year":2025,"title":"Exploring Cosmic Dawn with PANORAMIC II: Cosmic Variance and Galaxy Clustering at $z\\sim10$","arxiv_id":"2512.14212"}],"verified":true,"paraphrase":"Followed this paper and another work in using the Poisson contribution to the variance as the mean number count."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2020,"title":"The Number Densities and Stellar Populations of Massive Galaxies at 3 < z < 6: A Diverse, Rapidly Forming Population in the Early Universe","arxiv_id":"2010.04725"}],"verified":true,"paraphrase":"Estimated the contribution of cosmic variance to its total error budget using this paper's prescription."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2023,"title":"Modeling the JWST high-redshift galaxies with a general formation scenario and the consistency with the $\\Lambda$CDM model","arxiv_id":"2307.12487"}],"verified":true,"paraphrase":"Followed this paper in calculating cosmic variance."},{"p":0.98,"quote":null,"citing":[{"self":false,"year":2010,"title":"The Most Massive Galaxies at 3.0<z<4.0 in the NEWFIRM Medium-Band Survey: Properties and Improved Constraints on the Stellar Mass Function","arxiv_id":"1009.0269"}],"verified":true,"paraphrase":"Derived the cosmic variance following this paper's cosmic variance cookbook with its survey parameters and a population of massive galaxies with M_star>10^11 M_sun, obtaining 0.18 dex."},{"p":0.99,"quote":null,"citing":[{"self":false,"year":2024,"title":"SCUBADive I: JWST+ALMA Analysis of 289 sub-millimeter galaxies in COSMOS-Web","arxiv_id":"2408.08346"}],"verified":true,"paraphrase":"Outlined its method for calculating the volume density uncertainty from cosmic variance, which follows the formalism developed by this paper."},{"p":0.97,"quote":null,"citing":[{"self":false,"year":2020,"title":"On the (Lack of) Evolution of the Stellar Mass Function of Massive Galaxies from $z$=1.5 to 0.4","arxiv_id":"2002.07189"}],"verified":true,"paraphrase":"Used the formalism set by this paper to estimate the relative cosmic variance of galaxies more massive than 10^11 M_sun at z=0.35 for COSMOS and SHELA."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2022,"title":"Galaxy luminosity functions at redshifts 0.6 to 1.2 in the Chandra Deep Field South","arxiv_id":"2203.03563"}],"verified":true,"paraphrase":"Obtained average fractional cosmic variance from this paper's method for its average stellar masses in two redshift bins."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2023,"title":"MIGHTEE-HI: The first MeerKAT HI mass function from an untargeted interferometric survey","arxiv_id":"2304.13051"}],"verified":true,"paraphrase":"Evaluated the uncertainty due to sample variance for MIGHTEE following the prescriptions from this paper's cosmic variance cookbook."},{"p":0.9,"quote":null,"citing":[{"self":false,"year":2020,"title":"The Synthetic Emission Line COSMOS catalog: H$\\alpha$ and [OII] galaxy luminosity functions and counts at $0.3<z<2.5$","arxiv_id":"2003.06394"}],"verified":true,"paraphrase":"Estimated the sample variance contribution in each redshift interval using this paper's method, assuming a Planck 2015 matter power spectrum and galaxy linear biases given in another work."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2023,"title":"The Impact of Black Hole Scaling Relation Assumptions on the Mass Density of Black Holes","arxiv_id":"2307.04878"}],"verified":true,"paraphrase":"Obtained cosmic variance estimates following the methods outlined in this paper."},{"p":1.0,"quote":{"text":"We have estimated the effect of the cosmic variance using the method implemented following [ref] .","citing":"2305.16141","section":"Cosmic variance"},"citing":[{"self":false,"year":2023,"title":"Constraints on the Faint End of the Galaxy Stellar Mass Function at z ~ 4-8 from Deep JWST Data","arxiv_id":"2305.16141"}],"verified":true,"paraphrase":"Estimated the effect of cosmic variance using the method implemented following this paper."},{"p":0.97,"quote":{"text":"The uncertainty of our luminosity function measurements include the standard deviation from MC simulation, Poisson error (following [ref] ) and cosmic variance ($∼$ 0.03 dex, negligible; following [ref] prescription), respectively.","citing":"2412.06894","section":"Spectroscopically Complete Infrared Luminosity Function"},"citing":[{"self":false,"year":2024,"title":"A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$","arxiv_id":"2412.06894"}],"verified":true,"paraphrase":"Included cosmic variance of about 0.03 dex, negligible, following this paper's prescription among the uncertainties of its luminosity function measurements."}],"papers_all":44,"self_papers":1,"self_entries":[{"p":0.91,"quote":null,"citing":[{"self":true,"year":2017,"title":"Major Merging History in CANDELS. I. Evolution of the Incidence of Massive Galaxy-Galaxy Pairs from z=3 to z~0","arxiv_id":"1712.06611"}],"verified":true,"paraphrase":"Referred to this paper for additional details."}]},{"kind":"data_used","label":"Uses its data or values","papers":1,"entries":[{"p":0.87,"quote":null,"citing":[{"self":false,"year":2024,"title":"SCUBADive I: JWST+ALMA Analysis of 289 sub-millimeter galaxies in COSMOS-Web","arxiv_id":"2408.08346"}],"verified":true,"paraphrase":"Started with the dark matter root cosmic variance reported by this paper for the COSMOS field."}],"papers_all":3,"self_papers":0,"self_entries":[]}],"counts":{"by_kind":{"contests":2,"data_used":3,"comparison":3,"method_or_tool":44,"supports_this_paper":5},"dropped":{"relied_on":0,"unknown_ids":0,"account_lines":0,"contest_vetoed":0,"below_threshold":0,"contest_drawback":0,"contest_without_basis":0,"contest_not_one_sentence":0,"contest_on_group_citation":0},"papers_read":24,"self_papers":9,"citing_papers":99,"sentences_read":31,"citing_sentences":159,"unambiguous_read":31,"typed_independent":51,"independent_papers":90,"by_kind_independent":{"contests":1,"data_used":3,"comparison":3,"method_or_tool":42,"supports_this_paper":5}},"input_sha256":"47f698cab6d14eb1b29c29b0d0186b48af8bed5f68db9f62e025e74a0fd01e0b","method":"For a paper with five or more citing arXiv papers, Pith selected up to 40 citing sentences its citation classifier typed, read those whose citation markers point at this paper alone, and wrote one paraphrase for each later paper in each group, each resting on one sentence. A later paper is listed under a label only when the classifier gives one of its sentences that label at intent probability 0.8 or more (0.95 for support), Pith's reading of the sentence finds that the citing paper itself did it, and a second check of the paraphrase against the sentence passes. The section lists uses only: building on the paper, using its method, tool, data or values, comparing with it and citing it as support. It does not list criticism or disagreement, so their absence says nothing about how the paper has been received. Code counted the papers, wrote the summary from the listed entries, set the evidence level and linked each entry to its citing paper. Quotes are copied from the citing sentence and shown only when the citing paper's licence is CC BY, CC BY-SA or CC0; otherwise the paraphrase is shown. Papers that share an author with this one are listed apart. A paper with fewer citing papers gets a line counted by code, which names uses only: a later paper whose only label is a contest is counted as not described.","line":null,"summary":"14 later papers by other authors are listed below: 14 used its method or tool and 1 used its data or values. 1 of them appears under more than one label. 1 more paper by the same authors is listed: 1 used its method or tool."},"_links":{"html":"https://pith.science/paper/1001.1737"}}