pith. sign in

arxiv: 2606.12405 · v1 · pith:YFY463GYnew · submitted 2026-06-10 · 🌌 astro-ph.CO

Bounding the Effect of HOD Assumptions on Small-Scale Clustering Constraints

Nick Magnelli , Zachery Brown , Lado Samushia This is my paper

Pith reviewed 2026-06-27 08:40 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords small-scale clusteringhalo occupation distributioncosmological constraintsgalaxy-halo connectiontwo-point correlation functionAbacusSummit
0
0 comments X

The pith

Small-scale galaxy clustering excludes far fewer cosmologies when halo occupation parameters are allowed to vary than when fixed.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper measures how strongly small-scale galaxy clustering can constrain cosmology once uncertainty in the galaxy-halo connection is taken into account. It compares two limiting cases on the same set of mock data vectors: one that profiles over a five-parameter HOD model with only broad initial bounds, and one that assumes those parameters are known exactly. A reader cares because the two cases produce very different numbers of excluded cosmologies, showing that the amount of prior information on how galaxies occupy halos directly sets how much cosmological information the data can deliver. The analysis uses two-point correlation function multipoles from LRG-like mocks built on 81 AbacusSummit cosmologies.

Core claim

When the HOD parameters are profiled over with broad bounds, only 25 percent of the tested AbacusSummit cosmologies are excluded at 3 sigma by the Planck LCDM data vector; when the same parameters are fixed exactly, 81 percent are excluded.

What carries the argument

The floor treatment, which minimizes chi-squared over the five HOD parameters after imposing only broad initial bounds, versus the ceiling treatment that holds those parameters fixed.

If this is right

  • Under conservative HOD assumptions many more cosmologies remain consistent with the data than under optimistic assumptions.
  • The difference persists across variations in scale cuts, multipole inclusion, and mock phase.
  • Strong small-scale clustering constraints require informative priors on the galaxy-halo connection.
  • The same data vector can produce chi-squared values that differ by multiple orders of magnitude depending on the HOD treatment.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Analyses that aim to use small scales for cosmology will need independent constraints on HOD parameters or joint modeling that marginalizes them properly.
  • If the true galaxy-halo relation varies with cosmology, even the floor case may overestimate the available constraining power.
  • Combining small-scale clustering with other observables that help pin down HOD parameters could close the gap between the floor and ceiling results.

Load-bearing premise

The standard five-parameter HOD model with broad initial bounds is flexible enough to represent the true minimum information extractable from the clustering data.

What would settle it

Direct evidence that the galaxy-halo connection requires more than five parameters or depends on cosmology would mean the floor case no longer gives the actual minimum constraining power.

Figures

Figures reproduced from arXiv: 2606.12405 by Lado Samushia, Nick Magnelli, Zachery Brown.

Figure 1
Figure 1. Figure 1: — Two instances of DD(r, µ) for c000 ph000+5pAHOD-set-A ( [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: — 2PCF multipoles for several values of µmax2 produced from c000 ph000+5pAHOD-set-A. The uncertainties shown have been recomputed for the corresponding values of µmax2. In our methodology we only consider µmax2 ∈ {0.9, 1.0}. The source causing the strong effect of µmax2 in the small-scale quadrupole is the excess of extreme-angle galaxy pairs that can be seen in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: — 2PCF multipoles for fixed ph000, but varying 5pAHOD and cosmological parameters about c000+5pAHOD-set-A. The top panel shows the monopole and quadrupole for c000 ph000+5pAHOD-set-A versus c125 ph000+5pAHOD-set-A. The latter is chosen because it represents a +0.5% change in σ8, an important parameter in small-scale clustering (e.g. Leauthaud et al. 2017; Yuan et al. 2022a; Amon et al. 2023). Note that whi… view at source ↗
Figure 4
Figure 4. Figure 4: — 2PCF multipoles for fixed c000+5pAHOD-set-A, but different phases. ph000 is shown in black. The 24 remaining cubic box phases, ph[001--024], are shown in red. The blue lines denote the small box phases. These are nominally listed as ph[3000--4999], but only 1830 of these are considered in our anal￾ysis (see Section 2.4). The uncertainties shown on ph000 are taken from the covariance matrix produced from … view at source ↗
Figure 5
Figure 5. Figure 5: — 2PCF multipoles for fixed c000+5pAHOD-set-A, vary￾ing phase (blue, 25 phases) and the AbacusHOD seed for pseudoran￾dom galaxy population (red, 25 seeds). The spread due to seed is smaller than the spread due to phase, but the seed spread is not negligible. We treat the seed as part of the model (fixed at the default value) and construct covariance matrices from phase variation alone (Section 2.4). to the… view at source ↗
Figure 6
Figure 6. Figure 6: — Sampling density of the filtered interpolation data vectors for c000 ph000. The nontrivial shapes arise from the filters on ¯n and fsat; in the unfiltered case the distribution against the 5pAHOD parameters would be approximately uniform. The 500 unfiltered sampling vectors are omitted. Note that some ¯n and fsat values fall outside the nominal cuts because our filtration acts on a far quicker but slight… view at source ↗
Figure 7
Figure 7. Figure 7: — Accuracy of the 2PCF multipole interpolator (5pIHOD) relative to AbacusHOD (5pAHOD) for c000 ph000, where for each case, 5pAHOD-set = 5pIHOD-set. These pseudorandom 5pAHOD-sets were generated approximately within our bounds on HOD parameters, n¯, and fsat (see comment on [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: — Validation results for each cosmology tested in the suite. For each cosmology, the best minimum χ 2 ν values from HODmin-S1 and HODmin-S2 out of the 1000 independent values for all 5 validation cases are shown, such that there are 10 points per cosmology, 405 unique validation mocks across the suite, and 810 data points shown in total. “Index” represents the 81 cosmologies tested, but these are not order… view at source ↗
Figure 9
Figure 9. Figure 9: — Distribution of minimum χ 2 ν from the 1000 independent runs of HODmin for the c000 ph000+5pAHOD interpolator against the c000 ph000+5pAHOD-set-A mock data vector (rmin2 = 5, µmax2 = 0.9, monopole+quadrupole). The two histograms cor￾respond to the outputs of HODmin-S1 and HODmin-S2. HODmin-S2 consistently converges well within χ 2 ν ≪ 1. χ 2 is a useful measure of goodness of fit, but the best￾fit HOD pa… view at source ↗
Figure 10
Figure 10. Figure 10: — Scatter corner plot of the 1000 best-fit 5pIHOD-sets from the HODmin-S2 outputs of the runs described in [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: — Two sets of 1000 2PCF multipoles correspond￾ing to the HODmin-S2 best-fit 5pIHOD-sets in comparison to the c000 ph000+5pAHOD-set-A mock data vector (black): c000 ph000+5pIHOD (red; corresponds to Figures 9–10, along with the mock data vector) and c180 ph000+5pIHOD (blue). Despite the wide spread in best-fit 5pIHOD-space ( [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: — The effect on suite constraints from varying the available inputs one at a time from the default test configuration of rmin2 = 5, µmax2 = 0.9, monopole+quadrupole, and a mock data vector produced from c000 ph000+5pAHOD-set-A (red). The first panel shows the effect of varying to rmin2 = 20 (blue). The second panel shows the effect of varying to µmax2 = 1.0 (blue). The third panel shows the effect of cons… view at source ↗
Figure 13
Figure 13. Figure 13: — Floor versus ceiling constraints across the AbacusSummit suite. In the ceiling case (blue), computations are made directly from AbacusHOD rather than through an interpolator, and no minimization is performed; 5pAHOD parameters are fixed to those of the mock data vector. The floor case (red), as well as the indexing of this plot, corresponds to the same default configuration shown in [PITH_FULL_IMAGE:fi… view at source ↗
Figure 14
Figure 14. Figure 14: — Baseline-configuration χ 2 ν as a function of the cosmological parameters of the AbacusSummit-based models. The 81-cosmology sampling is too sparse for clear contours. With more data points, we might plausibly expect to uncover reliable contours in the w0 − wa and h − ωcdm projections. variance matrices derived from the Planck ΛCDM phases suffice for all interpolation and data vectors, whether or not th… view at source ↗
Figure 15
Figure 15. Figure 15: — Distribution of minimum χ 2 ν from HODmin runs of the c000 ph000+5pAHOD interpolator against 24 mock data vectors from c000 ph[001-024]+5pAHOD-set-A. The 5pAHOD flexibility is generally insufficient to compensate phase differences within an otherwise￾identical cosmology. small-scale 2PCF multipoles can strongly discriminate between cosmologies in the AbacusSummit grid. If, in￾stead, HOD parameters are a… view at source ↗
read the original abstract

Small-scale galaxy clustering is expected to contain substantial cosmological information, but the extent to which this information constrains halo-based cosmologies independent of an assumed galaxy--halo connection remains unclear. We quantify this dependence using LRG-like mock galaxy catalogs built from 81 cosmologies in the {\tt \textsc{AbacusSummit}} suite. We analyze two-point correlation function multipoles on scales ranging from $5$--$80$ Mpc/$h$ and compare two limiting treatments, the \enquote{floor} and \enquote{ceiling}, of the standard five-parameter HOD model. In the conservative floor case, we impose only broad initial HOD bounds and profile over HOD parameters to determine the minimum constraining power available; we accomplish this with {\tt HODmin}, a two-stage global optimization algorithm written for minimizing $\chi^2$ in HOD space. In the optimistic ceiling case, we assume the HOD parameters are known exactly. We find a significant difference between the floor and ceiling when comparing against the same Planck $\Lambda$CDM mock data vector with identical modeling assumptions: for the floor, $25\%$ of the discrete {\tt \textsc{AbacusSummit}} cosmologies tested are excluded at $3\sigma$, whereas for the ceiling, $\sim81\%$ are excluded. Many cosmologies agree well with data in the floor, and yet in the ceiling are excluded by multiple orders of magnitude in $\chi^2$. We therefore observe the strength of small-scale clustering constraints depends heavily on the amount of prior HOD information assumed. We compare the sensitivity of this effect to various choices like scale cut, angle cut, multipole inclusion, mock phase, and mock HOD model. Our wide floor--ceiling bracket indicates that informative galaxy--halo priors are necessary for extracting strong small-scale clustering constraints.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The paper analyzes small-scale galaxy clustering using LRG-like mocks from 81 AbacusSummit cosmologies. It compares two-point correlation function multipoles (5--80 Mpc/h) against a fixed Planck ΛCDM data vector under two limiting treatments of the standard five-parameter HOD model: a conservative 'floor' case that profiles over HOD parameters with broad initial bounds via a new two-stage optimizer (HODmin) to find minimum χ², and an optimistic 'ceiling' case that fixes the HOD parameters exactly. The central result is that 25% of the tested cosmologies are excluded at 3σ in the floor case versus ∼81% in the ceiling case, with many cosmologies fitting well under the floor but excluded by orders of magnitude under the ceiling. Sensitivity tests to scale cuts, multipoles, and mock choices are reported, leading to the conclusion that small-scale clustering constraints depend strongly on the amount of prior HOD information assumed.

Significance. If the central result holds, the work provides a concrete, quantitative demonstration that the cosmological information extractable from small-scale clustering is highly sensitive to galaxy--halo connection assumptions, using independent external mocks and a fixed reference data vector for a clean floor--ceiling bracket. The explicit exclusion fractions (25% vs. ∼81%) and reported sensitivity tests supply falsifiable benchmarks for future analyses. This highlights the practical necessity of informative HOD priors and supplies a methodological template (HODmin) for profiling over nuisance parameters in similar settings.

major comments (2)
  1. [Methods, HODmin optimizer] Methods, HODmin optimizer: The two-stage global optimization algorithm is load-bearing for the floor case χ² values that determine the 25% exclusion fraction, yet no validation (e.g., recovery of known minima on test functions, multiple random starts, or comparison to alternative minimizers) is described; without this, it is unclear whether the reported minima are reliably global or whether local minima inflate the floor χ² and thereby understate the exclusion rate.
  2. [HOD model description and floor definition] HOD model description and floor definition: The claim that the five-parameter HOD with broad initial bounds implements the 'minimum constraining power available' assumes this functional form spans all relevant galaxy--halo degrees of freedom. If the true connection requires additional parameters (assembly bias, velocity bias, or cosmology dependence) outside the five-parameter family, the profiled floor χ² values would be higher than the true minimum, so the reported 25% exclusion fraction would overstate the conservative limit and the floor--ceiling difference would not fully bracket the dependence on prior information.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which help clarify the scope and robustness of our results. We respond to each major comment below.

read point-by-point responses

  1. Referee: [Methods, HODmin optimizer] The two-stage global optimization algorithm is load-bearing for the floor case χ² values that determine the 25% exclusion fraction, yet no validation (e.g., recovery of known minima on test functions, multiple random starts, or comparison to alternative minimizers) is described; without this, it is unclear whether the reported minima are reliably global or whether local minima inflate the floor χ² and thereby understate the exclusion rate.

    Authors: We agree that validation of HODmin is essential to establish that the reported minima are global. In the revised manuscript we will add a dedicated subsection on optimizer validation. This will include: (i) recovery of known analytic minima on standard test functions, (ii) results from 50 independent random initializations per cosmology showing convergence to the same minimum within numerical tolerance, and (iii) direct comparison of HODmin results against scipy.optimize.differential_evolution on a subset of cosmologies. These tests will confirm that local minima do not inflate the floor χ² values. revision: yes

  2. Referee: [HOD model description and floor definition] The claim that the five-parameter HOD with broad initial bounds implements the 'minimum constraining power available' assumes this functional form spans all relevant galaxy--halo degrees of freedom. If the true connection requires additional parameters (assembly bias, velocity bias, or cosmology dependence) outside the five-parameter family, the profiled floor χ² values would be higher than the true minimum, so the reported 25% exclusion fraction would overstate the conservative limit and the floor--ceiling difference would not fully bracket the dependence on prior information.

    Authors: We thank the referee for this important qualification. Our floor is defined strictly as the minimum χ² attainable by profiling over the standard five-parameter HOD with broad initial bounds; it is therefore the minimum within that model family. We agree that if the true galaxy-halo connection requires additional parameters (assembly bias, velocity bias, or explicit cosmology dependence), the true minimum could be lower still. We will revise the text to state explicitly that the reported 25% exclusion fraction is the conservative limit within the five-parameter HOD, and we will add a short discussion of how extra degrees of freedom would further reduce the exclusion rate. This framing preserves the floor-ceiling bracket as a demonstration of sensitivity to HOD prior information while acknowledging the model limitation. revision: partial

Circularity Check

0 steps flagged

No circularity; central result from direct comparison on independent mocks

full rationale

The paper computes exclusion fractions (25% floor vs ~81% ceiling at 3σ) by comparing each of 81 AbacusSummit cosmologies to a fixed Planck ΛCDM mock data vector, profiling HOD parameters in the floor case via the HODmin optimizer to obtain minimum χ² values. These fractions are measured outputs of the χ² comparisons on external realizations rather than quantities defined by the HOD fits themselves. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citations appear in the derivation chain; the floor/ceiling bracket is a direct empirical measurement under stated modeling assumptions.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The paper relies on the standard five-parameter HOD model and the AbacusSummit N-body suite as background infrastructure; the only new element is the HODmin optimizer whose internal details are not specified in the abstract.

free parameters (1)
  • five HOD parameters
    Profiled over with broad bounds in the floor case; their specific values are not reported as they are marginalized.
axioms (2)
  • domain assumption The five-parameter HOD model is an adequate description of the galaxy-halo connection across the tested cosmologies
    Invoked when defining the floor case as the conservative minimum constraining power.
  • domain assumption AbacusSummit mocks accurately represent the clustering signal for LRG-like galaxies in each cosmology
    Required for the exclusion fractions to be meaningful.

pith-pipeline@v0.9.1-grok · 5876 in / 1513 out tokens · 22513 ms · 2026-06-27T08:40:24.566856+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

101 extracted references · 100 canonical work pages · 50 internal anchors

  1. [1]

    Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies

    Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies. , keywords =. doi:10.1086/466512 , archivePrefix =. astro-ph/0501171 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/466512

  2. [2]

    DESI DR2 results. II. Measurements of baryon acoustic oscillations and cosmological constraints. , keywords =. doi:10.1103/tr6y-kpc6 , archivePrefix =. 2503.14738 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/tr6y-kpc6

  3. [3]

    , keywords =

    Stringent _ 8 constraints from small-scale galaxy clustering using a hybrid MCMC + emulator framework. , keywords =. doi:10.1093/mnras/stac1830 , archivePrefix =. 2203.11963 , primaryClass =

    work page doi:10.1093/mnras/stac1830

  4. [4]

    Modeling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity

    Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity. , keywords =. doi:10.1093/mnras/stw2602 , archivePrefix =. 1606.08054 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2602

  5. [5]

    DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars

    DESI 2024 V: Full-Shape galaxy clustering from galaxies and quasars. , keywords =. doi:10.1088/1475-7516/2025/09/008 , archivePrefix =. 2411.12021 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/09/008 2024

  6. [6]

    , keywords =

    Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument. , keywords =. doi:10.3847/1538-3881/ad0b08 , archivePrefix =. 2306.06307 , primaryClass =

    work page doi:10.3847/1538-3881/ad0b08

  7. [7]

    , keywords =

    Cosmological Fisher forecasts for next-generation spectroscopic surveys. , keywords =. doi:10.1093/mnras/stad611 , archivePrefix =. 2301.02289 , primaryClass =

    work page doi:10.1093/mnras/stad611

  8. [8]

    DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

    DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements. , keywords =. doi:10.1088/1475-7516/2025/07/028 , archivePrefix =. 2411.12022 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/07/028 2024

  9. [9]

    DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

    DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations. , keywords =. doi:10.1088/1475-7516/2025/02/021 , archivePrefix =. 2404.03002 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/02/021 2024

  10. [10]

    , keywords =

    Selecting samples of galaxies with fewer Fingers-of-God. , keywords =. doi:10.1088/1475-7516/2025/07/014 , archivePrefix =. 2501.10587 , primaryClass =

    work page doi:10.1088/1475-7516/2025/07/014 2025

  11. [11]

    , keywords =

    ABACUSHOD: a highly efficient extended multitracer HOD framework and its application to BOSS and eBOSS data. , keywords =. doi:10.1093/mnras/stab3355 , archivePrefix =. 2110.11412 , primaryClass =

    work page doi:10.1093/mnras/stab3355

  12. [12]

    , keywords =

    Five per cent measurements of the growth rate from simulation-based modelling of redshift-space clustering in BOSS LOWZ. , keywords =. doi:10.1093/mnras/stab3111 , archivePrefix =. 2101.12261 , primaryClass =

    work page doi:10.1093/mnras/stab3111

  13. [13]

    arXiv e-prints , keywords =

    The MegaMapper: A Stage-5 Spectroscopic Instrument Concept for the Study of Inflation and Dark Energy. arXiv e-prints , keywords =. doi:10.48550/arXiv.2209.04322 , archivePrefix =. 2209.04322 , primaryClass =

    work page doi:10.48550/arxiv.2209.04322

  14. [14]

    MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys

    MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys. arXiv e-prints , keywords =. doi:10.48550/arXiv.2411.07970 , archivePrefix =. 2411.07970 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2411.07970

  15. [15]

    Astronomische Nachrichten , keywords =

    The Maunakea Spectroscopic Explorer: Thousands of fibers, infinite possibilities. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20230108 , archivePrefix =. 2307.07667 , primaryClass =

    work page doi:10.1002/asna.20230108

  16. [16]

    arXiv e-prints , keywords =

    WST -- Widefield Spectroscopic Telescope: Motivation, science drivers and top-level requirements for a new dedicated facility. arXiv e-prints , keywords =. doi:10.48550/arXiv.2405.12518 , archivePrefix =. 2405.12518 , primaryClass =

    work page doi:10.48550/arxiv.2405.12518

  17. [17]

    Optimizing Roman survey design for CMB cross-correlation science

    Cosmology from weak lensing, galaxy clustering, CMB lensing and tSZ: II. Optimizing Roman survey design for CMB cross-correlation science. arXiv e-prints , keywords =. doi:10.48550/arXiv.2411.04088 , archivePrefix =. 2411.04088 , primaryClass =

    work page doi:10.48550/arxiv.2411.04088

  18. [18]

    , keywords =

    Euclid: The importance of galaxy clustering and weak lensing cross-correlations within the photometric Euclid survey. , keywords =. doi:10.1051/0004-6361/202038313 , archivePrefix =. 2005.00055 , primaryClass =

    work page doi:10.1051/0004-6361/202038313 2005

  19. [19]

    arXiv e-prints , keywords =

    The Spectroscopic Stage-5 Experiment. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.07923 , archivePrefix =. 2503.07923 , primaryClass =

    work page doi:10.48550/arxiv.2503.07923

  20. [20]

    , author =

    Interpreting large-scale redshift-space distortion measurements. , keywords =. doi:10.1111/j.1365-2966.2011.20169.x , archivePrefix =. 1102.1014 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.20169.x 2011

  21. [21]

    arXiv e-prints , keywords =

    Effective Field Theory for Large Scale Structure. arXiv e-prints , keywords =. doi:10.48550/arXiv.2212.08488 , archivePrefix =. 2212.08488 , primaryClass =

    work page doi:10.48550/arxiv.2212.08488

  22. [22]

    Inhomogeneous cosmology and backreaction: Current status and future prospects

    Inhomogeneous cosmology and backreaction: Current status and future prospects. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271817300117 , archivePrefix =. 1612.08222 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271817300117

  23. [23]

    Is there proof that backreaction of inhomogeneities is irrelevant in cosmology?

    Is there proof that backreaction of inhomogeneities is irrelevant in cosmology?. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/32/21/215021 , archivePrefix =. 1505.07800 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/32/21/215021

  24. [24]

    Frontiers in Astronomy and Space Sciences , keywords =

    Backreaction in Cosmology. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2021.692198 , archivePrefix =. 2106.06043 , primaryClass =

    work page doi:10.3389/fspas.2021.692198 2021

  25. [25]

    , keywords =

    ABACUSSUMMIT: a massive set of high-accuracy, high-resolution N-body simulations. , keywords =. doi:10.1093/mnras/stab2484 , archivePrefix =. 2110.11398 , primaryClass =

    work page doi:10.1093/mnras/stab2484

  26. [26]

    The AEMULUS Project. I. Numerical Simulations for Precision Cosmology. , keywords =. doi:10.3847/1538-4357/ab1085 , archivePrefix =. 1804.05865 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1085

  27. [27]

    Tests of redshift-space distortions models in configuration space for the analysis of the BOSS final data release

    Tests of redshift-space distortions models in configuration space for the analysis of the BOSS final data release. , keywords =. doi:10.1093/mnras/stu2460 , archivePrefix =. 1408.5435 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2460

  28. [28]

    A rigorous EFT-based forward model for large-scale structure

    A rigorous EFT-based forward model for large-scale structure. , keywords =. doi:10.1088/1475-7516/2019/01/042 , archivePrefix =. 1808.02002 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2019/01/042 2019

  29. [29]

    , keywords =

    Bayesian and frequentist investigation of prior effects in EFT of LSS analyses of full-shape BOSS and eBOSS data. , keywords =. doi:10.1103/PhysRevD.108.123514 , archivePrefix =. 2309.04468 , primaryClass =

    work page doi:10.1103/physrevd.108.123514

  30. [30]

    arXiv e-prints , keywords =

    Frequentist Cosmological Constraints from Full-Shape Clustering Measurements in DESI DR1. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.11811 , archivePrefix =. 2508.11811 , primaryClass =

    work page doi:10.48550/arxiv.2508.11811

  31. [31]

    Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering

    Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering. , keywords =. doi:10.1086/521074 , archivePrefix =. astro-ph/0703457 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521074

  32. [32]

    , keywords =

    Multitracer extension of the halo model: probing quenching and conformity in eBOSS. , keywords =. doi:10.1093/mnras/staa1956 , archivePrefix =. 1910.05095 , primaryClass =

    work page doi:10.1093/mnras/staa1956 1910

  33. [33]

    , keywords =

    Evidence for galaxy assembly bias in BOSS CMASS redshift-space galaxy correlation function. , keywords =. doi:10.1093/mnras/stab235 , archivePrefix =. 2010.04182 , primaryClass =

    work page doi:10.1093/mnras/stab235 2010

  34. [34]

    , keywords =

    The DESI one-per cent survey: exploring the halo occupation distribution of luminous red galaxies and quasi-stellar objects with ABACUSSUMMIT. , keywords =. doi:10.1093/mnras/stae359 , archivePrefix =. 2306.06314 , primaryClass =

    work page doi:10.1093/mnras/stae359

  35. [35]

    , keywords =

    DESI luminous red galaxy samples for cross-correlations. , keywords =. doi:10.1088/1475-7516/2023/11/097 , archivePrefix =. 2309.06443 , primaryClass =

    work page doi:10.1088/1475-7516/2023/11/097 2023

  36. [36]

    Annals of Physics , keywords =

    Comparing <mml:math><mml:mrow><mml:mi> </mml:mi><mml:mi>CDM</mml:mi></mml:mrow></mml:math>, <mml:math><mml:mrow><mml:mi> </mml:mi><mml:mi>CDM</mml:mi></mml:mrow></mml:math>, and <mml:math><mml:mrow><mml:msub><mml:mrow><mml:mi> </mml:mi></mml:mrow><mml:mrow><mml:mn>0</mml:mn></mml:mrow></mml:msub><mml:msub><mml:mrow><mml:mi> </mml:mi></mml:mrow><mml:mrow><...

    work page doi:10.1016/j.aop.2026.170453 2026

  37. [37]

    Planck 2018 results. VI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  38. [38]

    , keywords =

    The High Latitude Spectroscopic Survey on the Nancy Grace Roman Space Telescope. , keywords =. doi:10.3847/1538-4357/ac4973 , archivePrefix =. 2110.01829 , primaryClass =

    work page doi:10.3847/1538-4357/ac4973

  39. [39]

    Euclid Definition Study Report

    Euclid Definition Study Report. arXiv e-prints , keywords =. doi:10.48550/arXiv.1110.3193 , archivePrefix =. 1110.3193 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1110.3193

  40. [40]

    Overview of the Euclid mission

    Euclid: I. Overview of the Euclid mission. , keywords =. doi:10.1051/0004-6361/202450810 , archivePrefix =. 2405.13491 , primaryClass =

    work page doi:10.1051/0004-6361/202450810

  41. [41]

    , keywords =

    Clustering in real space and in redshift space. , keywords =. doi:10.1093/mnras/227.1.1 , adsurl =

    work page doi:10.1093/mnras/227.1.1

  42. [42]

    Linear Redshift Distortions: A Review

    Linear Redshift Distortions: a Review. The Evolving Universe , year = 1998, editor =. doi:10.1007/978-94-011-4960-0_17 , archivePrefix =. astro-ph/9708102 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/978-94-011-4960-0_17 1998

  43. [43]

    Redshift-Space Distortions, Pairwise Velocities and Nonlinearities

    Redshift-space distortions, pairwise velocities, and nonlinearities. , keywords =. doi:10.1103/PhysRevD.70.083007 , archivePrefix =. astro-ph/0407214 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.70.083007

  44. [44]

    , author =

    Testing cosmological structure formation using redshift-space distortions. , keywords =. doi:10.1111/j.1365-2966.2008.14211.x , archivePrefix =. 0808.0003 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.14211.x 2008

  45. [45]

    On average properties of inhomogeneous fluids in general relativity I: dust cosmologies

    On Average Properties of Inhomogeneous Fluids in General Relativity: Dust Cosmologies. General Relativity and Gravitation , keywords =. doi:10.1023/A:1001800617177 , archivePrefix =. gr-qc/9906015 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1023/a:1001800617177

  46. [46]

    Backreaction of inhomogeneities on the expansion: the evolution of cosmological parameters

    Back reaction of inhomogeneities on the expansion: The evolution of cosmological parameters. , keywords =. doi:10.1103/PhysRevD.62.043525 , archivePrefix =. astro-ph/9912347 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.62.043525

  47. [47]

    Dark energy from backreaction

    Dark energy from back-reaction. , keywords =. doi:10.1088/1475-7516/2004/02/003 , archivePrefix =. astro-ph/0311257 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2004/02/003 2004

  48. [48]

    Accelerated expansion from structure formation

    Accelerated expansion from structure formation. , keywords =. doi:10.1088/1475-7516/2006/11/003 , archivePrefix =. astro-ph/0607626 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2006/11/003 2006

  49. [49]

    On cosmic acceleration without dark energy

    On cosmic acceleration without dark energy. New Journal of Physics , keywords =. doi:10.1088/1367-2630/8/12/322 , archivePrefix =. astro-ph/0506534 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1367-2630/8/12/322

  50. [50]

    Exact solution to the averaging problem in cosmology

    Exact Solution to the Averaging Problem in Cosmology. , keywords =. doi:10.1103/PhysRevLett.99.251101 , archivePrefix =. 0709.0732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.99.251101

  51. [51]

    Does the growth of structure affect our dynamical models of the universe? The averaging, backreaction and fitting problems in cosmology

    Does the growth of structure affect our dynamical models of the Universe? The averaging, backreaction, and fitting problems in cosmology. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/74/11/112901 , archivePrefix =. 1109.2314 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0034-4885/74/11/112901

  52. [52]

    Annual Review of Nuclear and Particle Science , keywords =

    Backreaction in Late-Time Cosmology. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev.nucl.012809.104435 , archivePrefix =. 1112.5335 , primaryClass =

    work page doi:10.1146/annurev.nucl.012809.104435

  53. [53]

    Dark Energy from structure: a status report

    Dark Energy from structure: a status report. General Relativity and Gravitation , keywords =. doi:10.1007/s10714-007-0554-8 , archivePrefix =. 0707.2153 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s10714-007-0554-8

  54. [54]

    Can the Acceleration of Our Universe Be Explained by the Effects of Inhomogeneities?

    Can the acceleration of our universe be explained by the effects of inhomogeneities?. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/23/1/012 , archivePrefix =. gr-qc/0509108 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/23/1/012

  55. [55]

    A new framework for analyzing the effects of small scale inhomogeneities in cosmology

    New framework for analyzing the effects of small scale inhomogeneities in cosmology. , keywords =. doi:10.1103/PhysRevD.83.084020 , archivePrefix =. 1011.4920 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.83.084020

  56. [56]

    Examples of backreaction of small scale inhomogeneities in cosmology

    Examples of backreaction of small-scale inhomogeneities in cosmology. , keywords =. doi:10.1103/PhysRevD.87.124037 , archivePrefix =. 1304.2318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.87.124037

  57. [57]

    How well is our universe described by an FLRW model?

    How well is our Universe described by an FLRW model?. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/31/23/234003 , archivePrefix =. 1407.8084 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/31/23/234003

  58. [58]

    , keywords =

    Cosmology with the EFTofLSS and BOSS: dark energy constraints and a note on priors. , keywords =. doi:10.1088/1475-7516/2023/01/028 , archivePrefix =. 2207.14784 , primaryClass =

    work page doi:10.1088/1475-7516/2023/01/028 2023

  59. [59]

    , keywords =

    Consistency of effective field theory analyses of the BOSS power spectrum. , keywords =. doi:10.1103/PhysRevD.107.123530 , archivePrefix =. 2208.05929 , primaryClass =

    work page doi:10.1103/physrevd.107.123530

  60. [60]

    arXiv e-prints , keywords =

    Mapping the galaxy-halo connection to the galaxy bias: implication to the HOD-informed prior. arXiv e-prints , keywords =. doi:10.48550/arXiv.2410.08998 , archivePrefix =. 2410.08998 , primaryClass =

    work page doi:10.48550/arxiv.2410.08998

  61. [61]

    , keywords =

    Fast test to assess the impact of marginalization in Monte Carlo analyses and its application to cosmology. , keywords =. doi:10.1103/PhysRevD.106.063506 , archivePrefix =. 2203.16285 , primaryClass =

    work page doi:10.1103/physrevd.106.063506

  62. [62]

    , keywords =

    Analysis of unified galaxy power spectrum multipole measurements. , keywords =. doi:10.1093/mnras/stad2957 , archivePrefix =. 2307.07475 , primaryClass =

    work page doi:10.1093/mnras/stad2957

  63. [63]

    The Open Journal of Astrophysics , keywords =

    Cosmology with 6 parameters in the Stage-IV era: efficient marginalisation over nuisance parameters. The Open Journal of Astrophysics , keywords =. doi:10.21105/astro.2301.11895 , archivePrefix =. 2301.11895 , primaryClass =

    work page doi:10.21105/astro.2301.11895

  64. [64]

    , keywords =

    Cosmological constraints on early dark energy from the full shape analysis of eBOSS DR16. , keywords =. doi:10.1093/mnras/stae992 , archivePrefix =. 2312.01977 , primaryClass =

    work page doi:10.1093/mnras/stae992

  65. [65]

    , keywords =

    Full-shape analysis with simulation-based priors: Constraints on single field inflation from BOSS. , keywords =. doi:10.1103/PhysRevD.110.063538 , archivePrefix =. 2402.13310 , primaryClass =

    work page doi:10.1103/physrevd.110.063538

  66. [66]

    , keywords =

    HOD-informed prior for EFT-based full-shape analyses of LSS. , keywords =. doi:10.1088/1475-7516/2025/04/041 , archivePrefix =. 2409.12937 , primaryClass =

    work page doi:10.1088/1475-7516/2025/04/041 2025

  67. [67]

    Accelerating Universes with Scaling Dark Matter

    Accelerating Universes with Scaling Dark Matter. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271801000822 , archivePrefix =. gr-qc/0009008 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271801000822

  68. [68]

    Exploring the Expansion History of the Universe

    Exploring the Expansion History of the Universe. , keywords =. doi:10.1103/PhysRevLett.90.091301 , archivePrefix =. astro-ph/0208512 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.90.091301

  69. [69]

    Report of the Dark Energy Task Force

    Report of the Dark Energy Task Force. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0609591 , archivePrefix =. astro-ph/0609591 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0609591

  70. [70]

    The Limits of Quintessence

    Limits of Quintessence. , keywords =. doi:10.1103/PhysRevLett.95.141301 , archivePrefix =. astro-ph/0505494 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.95.141301

  71. [71]

    Mapping the Chevallier-Polarski-Linder parametrization onto Physical Dark Energy Models

    Mapping the Chevallier-Polarski-Linder parametrization onto physical dark energy Models. , keywords =. doi:10.1103/PhysRevD.92.043001 , archivePrefix =. 1505.05781 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.92.043001

  72. [72]

    Figure of Merit for Dark Energy Constraints from Current Observational Data

    Figure of merit for dark energy constraints from current observational data. , keywords =. doi:10.1103/PhysRevD.77.123525 , archivePrefix =. 0803.4295 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.77.123525

  73. [73]

    Velocity Bias from the Small Scale Clustering of SDSS-III BOSS Galaxies

    Velocity bias from the small-scale clustering of SDSS-III BOSS galaxies. , keywords =. doi:10.1093/mnras/stu2120 , archivePrefix =. 1407.4811 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2120

  74. [74]

    Exploring the squeezed three-point galaxy correlation function with generalized halo occupation distribution models

    Exploring the squeezed three-point galaxy correlation function with generalized halo occupation distribution models. , keywords =. doi:10.1093/mnras/sty1089 , archivePrefix =. 1802.10115 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1089

  75. [75]

    , keywords =

    CORRFUNC - a suite of blazing fast correlation functions on the CPU. , keywords =. doi:10.1093/mnras/stz3157 , archivePrefix =. 1911.03545 , primaryClass =

    work page doi:10.1093/mnras/stz3157 1911

  76. [76]

    A New Method to Correct for Fiber Collisions in Galaxy Two-Point Statistics

    A New Method to Correct for Fiber Collisions in Galaxy Two-point Statistics. , keywords =. doi:10.1088/0004-637X/756/2/127 , archivePrefix =. 1111.6598 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/756/2/127

  77. [77]

    The Effect of Fiber Collisions on the Galaxy Power Spectrum Multipole

    The Effect of Fiber Collisions on the Galaxy Power Spectrum Multipoles. , keywords =. doi:10.1093/mnras/stx185 , archivePrefix =. 1609.01714 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx185

  78. [78]

    Unbiased clustering estimation in the presence of missing observations

    Unbiased clustering estimation in the presence of missing observations. , keywords =. doi:10.1093/mnras/stx2053 , archivePrefix =. 1703.02070 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2053

  79. [79]

    , keywords =

    The completed SDSS-IV extended baryon oscillation spectroscopic survey: pairwise-inverse probability and angular correction for fibre collisions in clustering measurements. , keywords =. doi:10.1093/mnras/staa2344 , archivePrefix =. 2007.09005 , primaryClass =

    work page doi:10.1093/mnras/staa2344 2007

  80. [80]

    , keywords =

    The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe. , keywords =. doi:10.1046/j.1365-2966.2003.07063.x , archivePrefix =. astro-ph/0212375 , primaryClass =

    work page doi:10.1046/j.1365-2966.2003.07063.x 2003

Showing first 80 references.