Cosmology and Nongalactic Astrophysics · arXiv:1305.0934 v3 · submitted 4 May 2013
Redshift-space distortions from the cross-correlation of photometric populations
The paper says
“The total improvement of 5 implies that a photometric survey such as the Dark Energy Survey should be able to recover \gamma at the 5-10% from the angular clustering in linear scales of two different tracers.”
from the abstract · picked out as the main claim by a classifier
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The paper
Abstract
Several papers have recently highlighted the possibility of measuring redshift space distortions from angular auto-correlations of galaxies in photometric redshift bins. In this work we extend this idea to include as observables the cross-correlations between redshift bins, as an additional way of measuring radial information. We show that this extra information allows to reduce the recovered error in the growth rate index \gamma by a factor of 2. Although the final error in \gamma depends on the bias and the mean photometric accuracy of the galaxy sample, the improvement from adding cross-correlations is robust in different settings. Another factor of 2-3 improvement in the determination of \gamma can be achieved by considering two galaxy populations over the same photometric sky area but with different biases. This additional gain is shown to be much larger than the one from the same populations when observed over different areas of the sky (with twice the combined area). The total improvement of 5 implies that a photometric survey such as the Dark Energy Survey should be able to recover \gamma at the 5-10% from the angular clustering in linear scales of two different tracers. It can also constrain the evolution of f(z)x\sigma_8(z) in few bins beyond z 0.8-0.9 at the 10-15% level per-bin, compatible with recent constrains from lower-z spectroscopic surveys. We also show how further improvement can be achieved by reducing the photometric redshift error.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: hedged possibility 0.73
What the abstract itself states, as probabilities: claims first 0.06 · states limitation 0.84 · human participants 0.01 · controlled comparison 0.54 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.93 · mentions code or data availability 0.02
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v3). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| Several papers have recently highlighted the possibility of measuring redshift space distortions from angular auto-correlations of galaxies in photometric redshift bins. | background 1.00 | 0.03 | 0.02 | hedged possibility 0.98 |
| In this work we extend this idea to include as observables the cross-correlations between redshift bins, as an additional way of measuring radial information. | contribution 1.00 | 0.82 | 0.09 | asserted 0.97 |
| We show that this extra information allows to reduce the recovered error in the growth rate index \gamma by a factor of ~2. | result 1.00 | 0.94 | 0.39 | asserted 1.00 |
| Although the final error in \gamma depends on the bias and the mean photometric accuracy of the galaxy sample, the improvement from adding cross-correlations is robust in different settings. | result 0.69 | 0.86 | 0.12 | asserted 0.99 |
| Another factor of 2-3 improvement in the determination of \gamma can be achieved by considering two galaxy populations over the same photometric sky area but with different biases. | result 0.97 | 0.86 | 0.11 | hedged possibility 0.61 |
| This additional gain is shown to be much larger than the one from the same populations when observed over different areas of the sky (with twice the combined area). | result 0.98 | 0.90 | 0.06 | asserted 1.00 |
| The total improvement of ~5 implies that a photometric survey such as the Dark Energy Survey should be able to recover \gamma at the 5-10% from the angular clustering in linear scales of two different tracers. | interpretation 0.76 | 0.81 | 0.53 | hedged possibility 0.73 |
| It can also constrain the evolution of f(z)x\sigma_8(z) in few bins beyond z~0.8-0.9 at the 10-15% level per-bin, compatible with recent constrains from lower-z spectroscopic surveys. | result 0.96 | 0.83 | 0.12 | hedged possibility 0.65 |
| We also show how further improvement can be achieved by reducing the photometric redshift error. | result 0.66 | 0.89 | 0.04 | asserted 0.98 |
What kind of paper the classifier reports this is: method or tool 0.86 · evidence from simulation or computation 0.81
What was examined, and what was not
Sources read
- arXiv listing abstract v3
Not examined
- full text
- figures and tables
- references and citing sentences
- relations to other papers
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- P abstract
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- S sections
- T body sentences
- C citations
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How the labels were made
Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,069 input tokens, $0.0003 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 2 Pith papers
Reviewed papers on Pith that cite this one. The full citation record
- The MICE Grand Challenge Lightcone Simulation I: Dark matter clustering astro-ph.CO · Dec 2013
- Cosmological Parameter Estimation with Large Scale Structure Observations astro-ph.CO · Aug 2013
How the literature uses it
2 arXiv papers cite this in 3 sentences
Papers citing it
Compares with it 1 paper
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The novelties of the present analysis is that we marginalize over cosmological parameters which have been fixed in Refs. [ref] and we use a more sophisticated definition of the nonlinearity scale.
Cosmological Parameter Estimation with Large Scale Structure Observations · A DES-like catalog · 0.83
Cites it as background 1 paper
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Although most of these focus mainly on photometric-redshift galaxy surveys ( [ref] , [ref] , [ref] , [ref] , [ref] , [ref] ), this approach has also been applied to spectroscopic-redshift samples ( [ref] , [ref] , [ref] ).
Clustering tomography: measuring cosmological distances through angular clustering in thin redshift shells · Introduction · 0.95
What it cites · 1 sentence without a confident label
Compares with 1 paper
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If we compare our predictions to measurements from spectroscopic surveys like VIPERS [ref] with constrains $fσ_8(z=0.8) = 0.47 ±0.08$ or WiggleZ [ref] where $fσ_8(z=0.76) = 0.38 ±0.04$ we find that DES can achieve the same level of errors ($∼15%$) in determining the growth of structure but extending the constrains beyond redshift of unity.
The VIMOS Public Extragalactic Redshift Survey (VIPERS). Galaxy clustering and redshift-space distortions at z=0.8 in the first data release · Constraining the redshift evolution of the Growth Rate of Structure · 0.92
Cites as background 2 papers
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Redshift space distortions (RSD) [ref] can be used to understand the (linear) growth of structures, which provides a direct path to study the origin of cosmic acceleration.
Linear Redshift Distortions: A Review · Introduction · 0.97
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We now turn to narrow-band photometric surveys such as the ongoing PAU or J-PAS Surveys [ref] .
JPCam: A 1.2Gpixel camera for the J-PAS survey · The case of high-photometric accuracy · 0.81
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