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Acoustic scale from the angular power spectra of SDSS-III DR8 photometric luminous galaxies
Cosmology and Nongalactic Astrophysics · Submitted 10 Jan 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We derive the ratio of the angular diameter distance to the sound horizon scale D_A/r_s= 9.212 + 0.416 -0.404 at z=0.54, and therefore, D_A= 1411+- 65 Mpc at z=0.54; the result is fairly independent of assumptions on the underlying cosmology.
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The abstract, sentence by sentence
We measure the acoustic scale from the angular power spectra of the Sloan Digital Sky Survey III (SDSS-III) Data Release 8 imaging catalog that includes 872,921 galaxies over ~ 10,000 deg^2 between 0.45<z<0.65. The extensive spectroscopic training set of the Baryon Oscillation Spectroscopic Survey (BOSS) luminous galaxies allows precise estimates of the true redshift distributions of galaxies in our imaging catalog. Utilizing the redshift distribution information, we build templates and fit to the power spectra of the data, which are measured in our companion paper, Ho et al. 2011, to derive the location of Baryon acoustic oscillations (BAO) while marginalizing over many free parameters to exclude nearly all of the non-BAO signal. We derive the ratio of the angular diameter distance to the sound horizon scale D_A/r_s= 9.212 + 0.416 -0.404 at z=0.54, and therefore, D_A= 1411+- 65 Mpc at z=0.54; the result is fairly independent of assumptions on the underlying cosmology. Our measurement of angular diameter distance D_A is 1.4 \sigma higher than what is expected for the concordance LCDM (Komatsu et al. 2011), in accordance to the trend of other spectroscopic BAO measurements for z >~ 0.35. We report constraints on cosmological parameters from our measurement in combination with the WMAP7 data and the previous spectroscopic BAO measurements of SDSS (Percival et al. 2010) and WiggleZ (Blake et al. 2011). We refer to our companion papers (Ho et al. 2011; de Putter et al. 2011) for investigations on information of the full power spectrum.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We measure the acoustic scale from the angular power spectra of the Sloan Digital Sky Survey III (SDSS-III) Data Release 8 imaging catalog that includes 872,921 galaxies over ~ 10,000 deg^2 between 0.45<z<0.65. | contribution 0.75 | 0.97 | 0.06 | asserted 1.00 |
| s1 | The extensive spectroscopic training set of the Baryon Oscillation Spectroscopic Survey (BOSS) luminous galaxies allows precise estimates of the true redshift distributions of galaxies in our imaging catalog. | method 0.85 | 0.17 | 0.01 | asserted 0.99 |
| s2 | Utilizing the redshift distribution information, we build templates and fit to the power spectra of the data, which are measured in our companion paper, Ho et al. 2011, to derive the location of Baryon acoustic oscillations (BAO) while marginalizing over many free parameters to exclude nearly all of the non-BAO signal. | method 1.00 | 0.92 | 0.04 | asserted 0.99 |
| s3 | We derive the ratio of the angular diameter distance to the sound horizon scale D_A/r_s= 9.212 + 0.416 -0.404 at z=0.54, and therefore, D_A= 1411+- 65 Mpc at z=0.54; the result is fairly independent of assumptions on the underlying cosmology. | result 1.00 | 0.97 | 0.84 | asserted 1.00 |
| s4 | Our measurement of angular diameter distance D_A is 1.4 \sigma higher than what is expected for the concordance LCDM (Komatsu et al. 2011), in accordance to the trend of other spectroscopic BAO measurements for z >~ 0.35. | interpretation 0.71 | 0.93 | 0.14 | asserted 0.98 |
| s5 | We report constraints on cosmological parameters from our measurement in combination with the WMAP7 data and the previous spectroscopic BAO measurements of SDSS (Percival et al. 2010) and WiggleZ (Blake et al. 2011). | contribution 0.53 | 0.86 | 0.09 | asserted 0.95 |
| s6 | We refer to our companion papers (Ho et al. 2011; de Putter et al. 2011) for investigations on information of the full power spectrum. | future work 0.65 | 0.14 | 0.02 | unclear 0.70 |
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The paper
Original abstract
We measure the acoustic scale from the angular power spectra of the Sloan Digital Sky Survey III (SDSS-III) Data Release 8 imaging catalog that includes 872,921 galaxies over ~ 10,000 deg^2 between 0.45<z<0.65. The extensive spectroscopic training set of the Baryon Oscillation Spectroscopic Survey (BOSS) luminous galaxies allows precise estimates of the true redshift distributions of galaxies in our imaging catalog. Utilizing the redshift distribution information, we build templates and fit to the power spectra of the data, which are measured in our companion paper, Ho et al. 2011, to derive the location of Baryon acoustic oscillations (BAO) while marginalizing over many free parameters to exclude nearly all of the non-BAO signal. We derive the ratio of the angular diameter distance to the sound horizon scale D_A/r_s= 9.212 + 0.416 -0.404 at z=0.54, and therefore, D_A= 1411+- 65 Mpc at z=0.54; the result is fairly independent of assumptions on the underlying cosmology. Our measurement of angular diameter distance D_A is 1.4 \sigma higher than what is expected for the concordance LCDM (Komatsu et al. 2011), in accordance to the trend of other spectroscopic BAO measurements for z >~ 0.35. We report constraints on cosmological parameters from our measurement in combination with the WMAP7 data and the previous spectroscopic BAO measurements of SDSS (Percival et al. 2010) and WiggleZ (Blake et al. 2011). We refer to our companion papers (Ho et al. 2011; de Putter et al. 2011) for investigations on information of the full power spectrum.
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References
How the literature uses it
22 arXiv papers cite this in 29 sentences
Papers citing it · 12 sentences without a confident label
Uses its method or tool 1 paper
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Following previous works [ref] , we model the theoretical galaxy power spectrum as:
Unveiling $\nu$ secrets with cosmological data: neutrino masses and mass hierarchy · Galaxy power spectrum · 0.83
Uses its data or values 11 papers
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In order to constrain the proposed models with recent observational data, we use $N_SN=580$ data points for Type Ia supernovae from Union 2.1 [ref] , $N_H=39$ observed Hubble data points [ref] and $N_BAO=17$ baryon acoustic oscillation data [ref] , and finally the cosmic microwave background radiation (CMB) in the form [ref] .
A model with interaction of dark components and recent observational data · Joint Analysis · 1.00
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We have used a total of 30 data points of various BAO observables from compilation in Table B1 of [ref] , collected therein from many surveys [ref] .
Investigating the accelerated expansion of the Universe through updated constraints on viable $f(R)$ models within the Palatini formalism · CMB data and BAO data · 1.00
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The BAO dataset we are using is a collection of points from different observations [ref] selected not to be correlated by the approach described by [ref] .
Impact of Cosmology on Lorentz Invariance Violation Constraints from GRB Time-Delays · Datasets · 0.97
Cites it as background 4 papers
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The value $r_s(z_d)$ in Eq. ([ref]) is sound horizon size at the end of the drag era $z_d$: [equation] To estimate this important parameter different authors [ref] used theoretical or statistical approaches and suggested different fitting formulas for $r_s$.
Observational constraints on cosmological models with Chaplygin gas and quadratic equation of state · Observational data · 0.82
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Cosmic inflation [ref] persists as the undisputed mechanism explaining the origin of primordial curvature perturbations [ref] necessary to account for the Cosmic Microwave Background (CMB) anisotropies [ref] and the large scale structure of our universe [ref] .
On the importance of heavy fields during inflation · Introduction · 0.97
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Also, while our focus is on analyses of the full shape of angular correlation functions, we note that a number of studies have extracted cosmological information from the study of the baryon acoustic oscillation feature (BAO) in photometric galaxy samples [ref] .
Improving Photometric Galaxy Clustering Constraints With Cross-Bin Correlations · Introduction · 0.96
What it cites · 6 sentences without a confident label
Uses the method or tool of 1 paper
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In this section, however, we use power spectra that were corrected for the systematics using the method introduced in Paper I [ref] and observe the effect of the systematics on the result.
Ameliorating Systematic Uncertainties in the Angular Clustering of Galaxies: A Study using SDSS-III · Effect of systematics · 0.99
Uses data or values from 2 papers
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We use the DR8 imaging catalog of SDSS-III that includes photometric redshifts of luminous galaxies (hereafter, `LGs') between $0.45<z<0.65$ over $∼10,000 deg^2$ [ref] ; the spectroscopy from the SDSS-III Baryon Oscillation Spectroscopic Survey [ref] is used to create a training sample and therefore to estimate the true redshift distribution of photometric galaxies.
Ameliorating Systematic Uncertainties in the Angular Clustering of Galaxies: A Study using SDSS-III · Introduction · 0.99
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For BAO measurements, we use $(z=0.2)/r_s$ and $(z=0.35)/r_s$ from SDSS DR7 [ref] , $(z=0.44)/r_s$, $(z=0.60)/r_s$, and $(z=0.73)/r_s$ from WiggleZ[For COSMOMC, we use the three-redshift slice representation of the WiggleZ data from [ref] , i.e., $0.2<z<0.6$, $0.4<z<0.8$, and $0.6<z<1.0$, accounting for the covariance among them, while in Figure [ref] we show the result for the whole redshift range ($0.2<z<1.0$).
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations · Discussions: Cosmological implications · 0.93
Compares with 2 papers
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We also show the measurements of $(z=0.2)/r_s$ and $(z=0.35)/r_s$ from [ref] for SDSS DR7 [ref] as red lines with magenta shades and $(z=0.6)/r_s$ from [ref] for the WiggleZ data over $0.2 < z < 1$ as a green line with a light green shade.
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations · Discussions: Cosmological implications · 0.91
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The precision of our measurement is much better than that of [ref] , where they measure the BAO location within 9.7%.
Clustering of Photometric Luminous Red Galaxies II: Cosmological Implications from the Baryon Acoustic Scale · Best fit angular location of BAO · 1.00
Cites as support 1 paper
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Also [ref] and [ref] have shown a negligible effect of non-Gaussian errors on the BAO measurement in multi-parameter fitting.
Non-Gaussian errors of baryonic acoustic oscillations · Building the covariance matrix · 1.00
Cites as background 4 papers
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A number of previous works have analyzed and reported the cosmological constraints from the galaxy clustering of the imaging surveys [ref] , but there have been only a few published works on the BAO measurement [ref] .
Angular correlation function of 1.5 million LRGs: clustering evolution and a search for BAO · Introduction · 0.89
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A number of previous works have analyzed and reported the cosmological constraints from the galaxy clustering of the imaging surveys [ref] , but there have been only a few published works on the BAO measurement [ref] .
Clustering of photometric luminous red galaxies I : Growth of Structure and Baryon Acoustic Feature · Introduction · 0.89
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A number of previous works have analyzed and reported the cosmological constraints from the galaxy clustering of the imaging surveys [ref] , but there have been only a few published works on the BAO measurement [ref] .
Clustering of Photometric Luminous Red Galaxies II: Cosmological Implications from the Baryon Acoustic Scale · Introduction · 0.89
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