Astrophysics · arXiv:astro-ph/9708121 v2 · submitted 13 Aug 1997
Light-cone effect on higher-order clustering in redshift surveys
The paper says
“Therefore at present, the effect has to be taken into account for high precision measurements at very small scales only, while in future deep surveys it amounts to a significant correction.”
from the abstract · picked out as the main claim by a classifier
Reviews
Reviews by people
No person has reviewed this paper on Pith yet. A scientist listed on Pith can review it for a fee, and their review is published here whatever it concludes.
The paper
Abstract
We have evaluated a systematic effect on counts-in-cells analysis of deep, wide-field galaxy catalogues induced by the evolution of clustering within the survey volume. A multiplicative correction factor is explicitly presented, which can be applied after the higher order correlation functions have been extracted in the usual way, without taking into account the evolution. The general theory of this effect combined with the ansatz describing the non-linear evolution of clustering in simulations enables us to estimate the magnitude of the correction factor in different cosmologies. In a series of numerical calculations assuming an array of cold dark matter models, it is found that, as long as galaxies are unbiased tracers of underlying density field, the effect is relatively small ($ \simeq 10%$) for the shallow surveys (z < 0.2), while it becomes significant (order of unity) in deep surveys (z ∼ 1). Depending on the scales of interest, the required correction is comparable to or smaller than the expected errors of on-going wide-field galaxy surveys such as the SDSS and 2dF. Therefore at present, the effect has to be taken into account for high precision measurements at very small scales only, while in future deep surveys it amounts to a significant correction.
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. No sentence in this record was written by a model.
abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 0.98
What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.66 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.27 · mentions code or data availability 0.02
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v2). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| We have evaluated a systematic effect on counts-in-cells analysis of deep, wide-field galaxy catalogues induced by the evolution of clustering within the survey volume. | contribution 0.98 | 0.94 | 0.08 | asserted 1.00 |
| A multiplicative correction factor is explicitly presented, which can be applied after the higher order correlation functions have been extracted in the usual way, without taking into account the evolution. | method 0.50 | 0.83 | 0.12 | asserted 1.00 |
| The general theory of this effect combined with the ansatz describing the non-linear evolution of clustering in simulations enables us to estimate the magnitude of the correction factor in different cosmologies. | method 0.89 | 0.72 | 0.07 | asserted 0.96 |
| In a series of numerical calculations assuming an array of cold dark matter models, it is found that, as long as galaxies are unbiased tracers of underlying density field, the effect is relatively small ($ \simeq 10%$) for the shallow surveys ($z <0.2$), while it becomes significant (order of unity) in deep surveys ($z \sim1$). | result 1.00 | 0.94 | 0.47 | asserted 1.00 |
| Depending on the scales of interest, the required correction is comparable to or smaller than the expected errors of on-going wide-field galaxy surveys such as the SDSS and 2dF. | result 0.53 | 0.76 | 0.12 | asserted 0.90 |
| Therefore at present, the effect has to be taken into account for high precision measurements at very small scales only, while in future deep surveys it amounts to a significant correction. | interpretation 1.00 | 0.74 | 0.68 | asserted 0.98 |
What kind of paper the classifier reports this is: theoretical result 0.61 · evidence from simulation or computation 0.97
What was examined, and what was not
Sources read
- arXiv listing abstract v2
Not examined
- full text
- figures and tables
- references and citing sentences
- relations to other papers
Levels run
- P abstract
Not run
- S sections
- T body sentences
- C citations
- R cross-paper relations
How the labels were made
Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,120 input tokens, $0.0002 reported.
Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON
Cited by 3 Pith papers
Reviewed papers on Pith that cite this one. The full citation record
- Relativistic wide-angle galaxy bispectrum on the light-cone astro-ph.CO · May 2017
- Cosmological Measurements with General Relativistic Galaxy Correlations astro-ph.CO · May 2015
- Lensing and time-delay contributions to galaxy correlations astro-ph.CO · Nov 2013
How the literature uses it
4 arXiv papers cite this in 4 sentences
Papers citing it · 3 sentences without a confident label
Cites it as background 1 paper
-
Galaxy clustering has been extensively studied (see, e.g., [ref] ); here we briefly review the theoretical tools used in the analysis presented in this chapter.
Using SKAO to Understand the Clustering of Gravitational Wave Sources · Brief overview of clustering theory · 1.00
Challenges and discussion
Know something about this paper? Leave a comment.
Come back by email
A short list of the week's newly reviewed papers. Nothing is sent until you confirm from your inbox, and every email has a link that stops it. No account.
No comments yet.
Sign in to comment