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The 6dF Galaxy Survey: baryon acoustic oscillations and the local Hubble constant: 6dFGS: BAOs and the local Hubble constant
Open accessAbstract
We analyse the large-scale correlation function of the 6dF Galaxy Survey (6dFGS) and detect a baryon acoustic oscillation (BAO) signal at 105 h−1 Mpc. The 6dFGS BAO detection allows us to constrain the distance–redshift relation at zeff= 0.106. We achieve a distance measure of DV(zeff) = 457 ± 27 Mpc and a measurement of the distance ratio, rs(zd)/DV(zeff) = 0.336 ± 0.015 (4.5 per cent precision), where rs(zd) is the sound horizon at the drag epoch zd. The low-effective redshift of 6dFGS makes it a competitive and independent alternative to Cepheids and low-z supernovae in constraining the Hubble constant. We find a Hubble constant of H0= 67 ± 3.2 km s−1 Mpc−1 (4.8 per cent precision) that depends only on the Wilkinson Microwave Anisotropy Probe-7 (WMAP-7) calibration of the sound horizon and on the galaxy clustering in 6dFGS. Compared to earlier BAO studies at higher redshift, our analysis is less dependent on other cosmological parameters. The sensitivity to H0 can be used to break the degeneracy between the dark energy equation of state parameter w and H0 in the cosmic microwave background data. We determine that w=−0.97 ± 0.13, using only WMAP-7 and BAO data from both 6dFGS and Percival et al. (2010). We also discuss predictions for the large-scale correlation function of two future wide-angle surveys: the Wide field ASKAP L-band Legacy All-sky Blind surveY (WALLABY) blind H i survey (with the Australian Square Kilometre Array Pathfinder, ASKAP) and the proposed Transforming Astronomical Imaging surveys through Polychromatic Analysis of Nebulae (TAIPAN) all-southern-sky optical galaxy survey with the UK Schmidt Telescope. We find that both surveys are very likely to yield detections of the BAO peak, making WALLABY the first radio galaxy survey to do so. We also predict that TAIPAN has the potential to constrain the Hubble constant with 3 per cent precision.
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Cites
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
Komatsu, E., Smith, K. M., Dunkley, J., Bennett, C. L., Gold, B., Hinshaw, G., Jarosik, N., Larson, D., Nolta, M. R., Page, L., et al. (2011) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/192/2/18 · Cited by 8,802
The Sloan Digital Sky Survey: Technical Summary
York, D., Adelman, J., Anderson, J., Anderson, S., Annis, J., Bahcall, N., Bakken, J., Barkhouser, R., Bastian, S., Berman, E., et al. (2000) · The Astronomical Journal · doi:10.1086/301513 · Cited by 8,368 · cited 1×
“The Sloan Digital Sky Survey (SDSS; York et al. 2000), and the 2dF Galaxy Redshift Survey (2dFGRS; Colless et al. 2001) were the first redshift surveys which have directly detected the BAO signal.”
MethodFIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION
Komatsu, E., Dunkley, J., Nolta, M. R., Bennett, C. L., Gold, B., Hinshaw, G., Jarosik, N., Larson, D., Limon, M., Page, L., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/180/2/330 · Cited by 5,786
THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
Abazajian, K. N., Adelman-McCarthy, J. K., Agüeros, M. A., Allam, S. S., Prieto, C. A., An, D., Anderson, K. S. J., Anderson, S. F., Annis, J., Bahcall, N. A., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/182/2/543 · Cited by 5,341 · cited 1×
“The volume of the 6dF Galaxy Survey is approximately as large as the volume covered by the 2dF Galaxy Redshift Survey, with a sample density similar to SDSSDR7 (Abazajian et al. 2009).”
MethodThe Design and Implementation of FFTW3
Frigo, M., & Johnson, S. G. (2005) · Proceedings of the IEEE · doi:10.1109/jproc.2004.840301 · Cited by 5,086
Lewis, A., Challinor, A., & Lasenby, A. (2000) · The Astrophysical Journal · doi:10.1086/309179 · Cited by 4,920
Eisenstein, D. J., Zehavi, I., Hogg, D. W., Scoccimarro, R., Blanton, M. R., Nichol, R. C., Scranton, R., Seo, H., Tegmark, M., Zheng, Z., et al. (2005) · The Astrophysical Journal · doi:10.1086/466512 · Cited by 4,641 · cited 9×
“We derive the parameter (Eisenstein et al. 2005) A(zeff) = 100DV (zeff) √ Ωmh2 czeff , (27) which has no dependence on the Hubble constant since DV ∝ h−1.”
BackgroundMethodInfluentialFinal Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant
Freedman, W. L., Madore, B. F., Gibson, B. K., Ferrarese, L., Kelson, D. D., Sakai, S., Mould, J. R., Robert C. Kennicutt, Jr., Ford, H. C., Graham, J. A., et al. (2001) · The Astrophysical Journal · doi:10.1086/320638 · Cited by 3,543
Clustering in real space and in redshift space
Kaiser, N. (1987) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/227.1.1 · Cited by 2,762 · cited 1×
“The model of linear redshift space distortions introduced by Kaiser (1987) is based on the plane parallel approximation.”
MethodEisenstein, D. J., Zehavi, I., Hogg, D. W., Scoccimarro, R., Blanton, M. R., Nichol, R. C., Scranton, R., Seo, H., Tegmark, M., Zheng, Z., et al. (2005) · Cited by 2,568
The 2dF Galaxy Redshift Survey: spectra and redshifts
Colless, M., Dalton, G., Maddox, S., Sutherland, W. J., Norberg, P., Cole, S., Bland‐Hawthorn, J., Bridges, T. J., Cannon, R., Collins, C. A., et al. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04902.x · Cited by 2,368 · cited 2×
“The Sloan Digital Sky Survey (SDSS; York et al. 2000), and the 2dF Galaxy Redshift Survey (2dFGRS; Colless et al. 2001) were the first redshift surveys which have directly detected the BAO signal.”
MethodSelf-citationBaryonic Features in the Matter Transfer Function
Eisenstein, D. J., & Hu, W. (1998) · The Astrophysical Journal · doi:10.1086/305424 · Cited by 2,250 · cited 3×
“During the fit we calculate rs(zd) using the fitting formula of Eisenstein & Hu (1998).”
BackgroundMethodInfluentialCole, S., Percival, W. J., Peacock, J. A., Norberg, P., Baugh, C. M., Frenk, C. S., Baldry, I. K., Bland‐Hawthorn, J., Bridges, T., Cannon, R., et al. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09318.x · Cited by 2,100 · cited 2×
“…function ξ(s) (Martinez 2009; Gaztanaga, Cabre & Hui 2009; Labini et al. 2009; Sanchez et al. 2009; Kazin et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples…”
BackgroundMethodSelf-citationStable clustering, the halo model and non-linear cosmological power spectra
Smith, R. E., Peacock, J. A., Jenkins, A., White, S. D. M., Frenk, C. S., Pearce, F. R., Thomas, P. A., Efstathiou, G., & Couchman, H. M. P. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06503.x · Cited by 2,054 · cited 1×
“The nonlinear evolution of the power spectrum in CAMB is calculated using the halofit code (Smith et al. 2003).”
MethodBias and variance of angular correlation functions
Landy, S. D., & Szalay, A. S. (1993) · The Astrophysical Journal · doi:10.1086/172900 · Cited by 1,969 · cited 1×
“The redshift correlation function itself is given by Landy & Szalay (1993): ξ′data(s) = 1 + DD(s) RR(s) ( nr nd )2 − 2DR(s) RR(s) ( nr nd ) , (4) where the ratio nr/nd is given by nr nd = ∑Nr i wi(~x) ∑Nd j wj(~x) (5) and the sums go over all random (Nr) and data (Nd) galaxies.”
MethodBaryon acoustic oscillations in the Sloan Digital Sky Survey Data Release 7 galaxy sample
Percival, W. J., Reid, B. A., Eisenstein, D. J., Bahcall, N. A., Budavari, T., Frieman, J. A., Fukugita, M., Gunn, J. E., Ivezić, Ž., Knapp, G. R., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15812.x · Cited by 1,846 · cited 6×
“Subsequent studies using the final SDSS-LRG sample and combining it with the SDSS-main and the 2dFGRS sample were able to improve on this measurement and constrain the distance-redshift relation at zeff = 0.2 and zeff = 0.35 with 3% accuracy (Percival et al. 2010).”
MethodResultInfluentialRiess, A. G., Macri, L. M., Casertano, S., Lampeitl, H., Ferguson, H. C., Filippenko, A. V., Jha, S. W., Li, W., & Chornock, R. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/730/2/119 · Cited by 1,513 · cited 2×
“The SH0ES program (Riess et al. 2011) determined the Hubble constant using the distance ladder method.”
MethodCosmological constraints from the SDSS luminous red galaxies
Tegmark, M., Eisenstein, D. J., Strauss, M. A., Weinberg, D. H., Blanton, M. R., Frieman, J. A., Fukugita, M., Gunn, J. E., Hamilton, A. J. S., Knapp, G. R., et al. (2006) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.74.123507 · Cited by 1,479 · cited 1×
“…(Martinez 2009; Gaztanaga, Cabre & Hui 2009; Labini et al. 2009; Sanchez et al. 2009; Kazin et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples (Padmanabhan et al.…”
BackgroundPrimeval Adiabatic Perturbation in an Expanding Universe
Peebles, P. J. E., & Yu, J. T. (1970) · The Astrophysical Journal · doi:10.1086/150713 · Cited by 1,230 · cited 1×
“The radiation pressure drives sound-waves originating from overdensities in the matter distribution (Peebles & Yu 1970; ⋆ E-mail: florian.beutler@icrar.org Sunyaev & Zeldovich 1970; Bond & Efstathiou 1987).”
BackgroundA Cosmology Calculator for the World Wide Web
WRIGHT, E. L. (2006) · Publications of the Astronomical Society of the Pacific · doi:10.1086/510102 · Cited by 1,172 · cited 1×
“Our fiducial model gives DfidV (zeff) = 440.5 Mpc, where we have followed the distance definitions of Wright (2006) throughout.”
BackgroundInfluentialSmall-scale fluctuations of relic radiation
Sunyaev, R. A., & Zel’dovich, Y. B. (1970) · Astrophysics and Space Science · doi:10.1007/bf00653471 · Cited by 1,114
The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures
Jones, D. H. P., Read, M., Saunders, W., Colless, M., Jarrett, T. H., Parker, Q. A., Fairall, A. P., Mauch, T., Sadler, E. M., Watson, F. G., et al. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15338.x · Cited by 1,052 · cited 2×
“Papers by Jones et al. (2004, 2006, 2009) describe 6dFGS in full detail, including comparisons between 6dFGS, 2dFGRS and SDSS. Galaxies were excluded from our sample if they resided in sky regions with completeness lower than 60 percent.”
MethodInfluentialSelf-citation2MASS Extended Source Catalog: Overview and Algorithms
Jarrett, T. H., Chester, T. J., Cutri, R. M., Schneider, S. E., Skrutskie, M. F., & Huchra, J. P. (2000) · The Astronomical Journal · doi:10.1086/301330 · Cited by 989 · cited 1×
“The galaxies used in this analysis were selected to K 6 12.9 from the 2MASS Extended Source Catalog (2MASS XSC; Jarrett et al. 2000) and combined with redshift data from the 6dF Galaxy Survey (6dFGS; Jones et al. 2009).”
MethodInfluentialPower-spectrum analysis of three-dimensional redshift surveys
Feldman, H. A., Kaiser, N., & Peacock, J. A. (1994) · The Astrophysical Journal · doi:10.1086/174036 · Cited by 931
Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys
Seo, H., & Eisenstein, D. J. (2003) · The Astrophysical Journal · doi:10.1086/379122 · Cited by 797 · cited 1×
“Very interesting for cosmology is the idea of using the sound horizon scale as a standard ruler (Eisenstein, Hu & Tegmark 1998; Cooray et al. 2001; Seo & Eisenstein 2003; Blake & Glazebrook 2003).”
BackgroundGAZTAÑAGA, E., Cabré, A., & Hui, L. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15405.x · Cited by 635
The statistics of cosmic background radiation fluctuations
Bond, J. R., & Efstathiou, G. (1987) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/226.3.655 · Cited by 629 · cited 1×
“The radiation pressure drives sound-waves originating from overdensities in the matter distribution (Peebles & Yu 1970; ⋆ E-mail: florian.beutler@icrar.org Sunyaev & Zeldovich 1970; Bond & Efstathiou 1987).”
BackgroundA lognormal model for the cosmological mass distribution
Coles, P., & Jones, B. J. T. (1991) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/248.1.1 · Cited by 605 · cited 1×
“To obtain reliable error-bars for the correlation function we use log-normal realisations (Coles & Jones 1991; Cole et al. 2005; Kitaura et al. 2009).”
MethodThe 6dF Galaxy Survey: samples, observational techniques and the first data release
Jones, D. H., Saunders, W., Colless, M., Read, M. A., Parker, Q. A., Watson, F. G., Campbell, L., Burkey, D., Mauch, T., Moore, L., et al. (2004) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2004.08353.x · Cited by 561 · cited 1×
“Papers by Jones et al. (2004, 2006, 2009) describe 6dFGS in full detail, including comparisons between 6dFGS, 2dFGRS and SDSS. Galaxies were excluded from our sample if they resided in sky regions with completeness lower than 60 percent.”
Self-citationPOWER SPECTRUM ANALYSIS OF THREE-DIMENSIONAL REDSHIFT SURVEYSPreprint
Feldman, H. A., Kaiser, N., & Peacock, J. A. (1993) · Cited by 537
Renormalized cosmological perturbation theory
Crocce, M., & Scoccimarro, R. (2006) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.73.063519 · Cited by 536 · cited 1×
“c© 0000 RAS, MNRAS 000, 000–000 ory (Crocce & Scoccimarro 2006; Matsubara 2008) by k∗ = [ 1 6π2 ∫ ∞ 0 dk Plin(k) ]−1/2 , (19) where Plin(k) is again the linear power spectrum.”
Probing Dark Energy Using Baryonic Oscillations in the Galaxy Power Spectrum as a Cosmological Ruler
Blake, C., & Glazebrook, K. (2003) · The Astrophysical Journal · doi:10.1086/376983 · Cited by 535
Self-citationMatsubara, T. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.063530 · Cited by 491 · cited 1×
“c© 0000 RAS, MNRAS 000, 000–000 ory (Crocce & Scoccimarro 2006; Matsubara 2008) by k∗ = [ 1 6π2 ∫ ∞ 0 dk Plin(k) ]−1/2 , (19) where Plin(k) is again the linear power spectrum.”
Reid, B., Percival, W. J., Eisenstein, D. J., Verde, L., Spergel, D. N., Skibba, R., Bahcall, N. A., Budavári, T., Frieman, J. A., Fukugita, M., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16276.x · Cited by 489 · cited 2×
“…Hui 2009; Labini et al. 2009; Sanchez et al. 2009; Kazin et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples (Padmanabhan et al. 2007; Blake et al. 2007) and a…”
BackgroundMethodInfluentialNonlinear evolution of baryon acoustic oscillations
Crocce, M., & Scoccimarro, R. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.023533 · Cited by 467 · cited 5×
“Crocce & Scoccimarro (2008) used renormalised perturbation theory (RPT) and found percentlevel shifts in the BAO peak.”
BackgroundMethodInfluentialOn the Robustness of the Acoustic Scale in the Low‐Redshift Clustering of Matter
Eisenstein, D. J., Seo, H., & White, M. J. (2007) · The Astrophysical Journal · doi:10.1086/518755 · Cited by 460 · cited 1×
“All non-linear effects influencing the correlation function can be approximated by a convolution with a Gaussian damping factor exp[−(rk∗/2)2] (Eisenstein et al. 2007; Eisenstein, Seo & White 2007), where k∗ is the damping scale.”
MethodImproving Cosmological Distance Measurements by Reconstruction of the Baryon Acoustic Peak
Eisenstein, D., Seo, H., Sirko, E., & Spergel, D. (2006) · The Astrophysical Journal · doi:10.1086/518712 · Cited by 456 · cited 1×
“All non-linear effects influencing the correlation function can be approximated by a convolution with a Gaussian damping factor exp[−(rk∗/2)2] (Eisenstein et al. 2007; Eisenstein, Seo & White 2007), where k∗ is the damping scale.”
MethodEfstathiou, G., & Bond, J. R. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02274.x · Cited by 402 · cited 1×
“Measurements of other cosmological parameters often show degeneracies in the CMB data alone (Efstathiou & Bond 1999), especially in models with extra parameters beyond flat ΛCDM.”
BackgroundThick gas discs in faint dwarf galaxies
Roychowdhury, S., Chengalur, J. N., Begum, A., & Karachentsev, I. D. (2010) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2010.00835.x · Cited by 394
The clustering of luminous red galaxies in the Sloan Digital Sky Survey imaging data
Padmanabhan, N., Schlegel, D. J., Seljak, U., Makarov, A., Bahcall, N. A., Blanton, M. R., Brinkmann, J. V., Eisenstein, D. J., Finkbeiner, D. P., Gunn, J. E., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11593.x · Cited by 360 · cited 1×
“…et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples (Padmanabhan et al. 2007; Blake et al. 2007) and a cluster sample based on the SDSS photometric data (Huetsi 2009).”
MethodMeasuring Cosmological Parameters with Galaxy Surveys
Tegmark, M. (1997) · Physical Review Letters · doi:10.1103/physrevlett.79.3806 · Cited by 353 · cited 2×
“We calculated the effective volume of the survey using the estimate of Tegmark (1997) Veff = ∫ d3~x [ n(~x)P0 1 + n(~x)P0 ]2 (1) where n(~x) is the mean galaxy density at position ~x, determined from the data, and P0 is the characteristic power spectrum amplitude of the BAO signal.”
BackgroundMethodTHE COYOTE UNIVERSE. I. PRECISION DETERMINATION OF THE NONLINEAR MATTER POWER SPECTRUM
Heitmann, K., White, M. J., Wagner, C., Habib, S., & Higdon, D. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/715/1/104 · Cited by 321 · cited 1×
“This code is calibrated by n-body simulations and can describe non-linear effects in the shape of the matter power spectrum for pure CDM models to an accuracy of around 5 − 10% (Heitmann et al. 2010).”
MethodNorberg, P., Baugh, C., Gaztañaga, E., & Croton, D. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14389.x · Cited by 291
The Stromlo-APM redshift survey. 2: Variation of galaxy clustering with morphology and luminosity
Loveday, J., Maddox, S., Efstathiou, G., & Peterson, B. A. (1995) · The Astrophysical Journal · doi:10.1086/175453 · Cited by 275 · cited 1×
“Other authors have used the so called J3-weighting which optimises the error over all scales by weighting each scale differently (e.g. Efstathiou 1988; Loveday et al. 1995).”
MethodImproving Cosmological Distance Measurements by Reconstruction of the Baryon Acoustic Peak
Eisenstein, D. J., Seo, H., Sirko, E., & Spergel, D. N. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 275
Efstathiou, G. P., & Bond, J. R. (1998) · CERN Document Server (European Organization for Nuclear Research) · Cited by 255
Eisenstein, D. J., Hu, W., & Tegmark, M. (1998) · The Astrophysical Journal · doi:10.1086/311582 · Cited by 252
Scale dependence of halo and galaxy bias: Effects in real space
Smith, R. C., Scoccimarro, R., & Sheth, R. K. (2007) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.75.063512 · Cited by 251 · cited 1×
“However, several authors report possible shifts of up to 1% (Guzik & Bernstein 2007; Smith et al. 2008, 2007; Angulo et al. 2008).”
BackgroundKazin, E. A., Blanton, M. R., Scoccimarro, R., McBride, C. K., Berlind, A. A., Bahcall, N. A., Brinkmann, J., Czarapata, P. C., Frieman, J. A., Kent, S., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/710/2/1444 · Cited by 234 · cited 3×
“Another motivation for our study is that the SDSS data after data release 3 (DR3) show more correlation on large scales than expected by ΛCDM and have no sign of a crossover to negative ξ up to 200h−1 Mpc (the ΛCDM prediction is 140h−1 Mpc) (Kazin et al. 2010).”
BackgroundMethodResultThe detectability of baryonic acoustic oscillations in future galaxy surveys
Angulo, R. E., Baugh, C. M., Frenk, C. S., & Lacey, C. G. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12587.x · Cited by 212
The Intermediate‐Scale Clustering of Luminous Red Galaxies
Zehavi, I., Eisenstein, D. J., Nichol, R. C., Blanton, M. R., Hogg, D. W., Brinkmann, J., Loveday, J., Meiksin, A. A., Schneider, D. P., & Tegmark, M. (2005) · The Astrophysical Journal · doi:10.1086/427495 · Cited by 209 · cited 1×
“In a magnitude limited sample there is a correlation between luminosity and redshift, which establishes a correlation between bias and redshift (Zehavi et al. 2005).”
BackgroundBlake, C., Collister, A., Bridle, S., & Lahav, O. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11263.x · Cited by 162 · cited 1×
“…et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples (Padmanabhan et al. 2007; Blake et al. 2007) and a cluster sample based on the SDSS photometric data (Huetsi 2009).”
MethodSelf-citationCorrelation Function in Deep Redshift Space as a Cosmological Probe
Matsubara, T. (2004) · The Astrophysical Journal · doi:10.1086/424561 · Cited by 161 · cited 3×
“The wide angle description of redshift space distortions has been laid out in several papers (Szalay et al. 1997; Szapudi 2004; Matsubara 2004; Papai & Szapudi 2008; Raccanelli et al. 2010), which we summarise in Appendix C.”
BackgroundBlake, C., Davis, T. M., Poole, G. B., Parkinson, D., Brough, S., Colless, M., Contreras, C., Couch, W. J., Croom, S. M., Drinkwater, M. J., et al. (2024) · doi:10.25916/sut.26215247.v1 · Cited by 155
Self-citationMotion of the acoustic peak in the correlation function
Smith, R. C., Scoccimarro, R., & Sheth, R. K. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.043525 · Cited by 152 · cited 1×
“However, several authors report possible shifts of up to 1% (Guzik & Bernstein 2007; Smith et al. 2008, 2007; Angulo et al. 2008).”
BackgroundNear-infrared and optical luminosity functions from the 6dF Galaxy Survey
Jones, D. H. P., Peterson, B. A., Colless, M., & Saunders, W. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10291.x · Cited by 150 · cited 2×
“Papers by Jones et al. (2004, 2006, 2009) describe 6dFGS in full detail, including comparisons between 6dFGS, 2dFGRS and SDSS. Galaxies were excluded from our sample if they resided in sky regions with completeness lower than 60 percent.”
MethodSelf-citationChuang, C.-H., & Wang, Y. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21565.x · Cited by 140 · cited 1×
“While there are studies that report a successful (but very low signal-to-noise) detection in the 2D correlation function using the SDSS-LRG data (e.g. Gaztanaga, Cabre & Hui 2009; Chuang & Wang 2011, but see also Kazin et al. 2010), our sample does not allow this kind of analysis.”
MethodThe detectability of baryonic acoustic oscillations in future galaxy surveys
Angulo, R. E., Baugh, C. M., Frenk, C. S., & Lacey, C. G. (2007) · CERN Document Server (European Organization for Nuclear Research) · Cited by 138
Constraining anisotropic baryon oscillations
Padmanabhan, N., & White, M. J. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.123540 · Cited by 122 · cited 2×
“It is defined as (Eisenstein et al. 2005; Padmanabhan & White 2008) α = DV (zeff) DfidV (zeff) .”
BackgroundMethodSánchez, A. G., Crocce, M., Cabre, A., Baugh, C. M., & GAZTAÑAGA, E. (2009) · Max Planck Digital Library · Cited by 113
Correlation Function in Deep Redshift Space as a Cosmological Probe
Matsubara, T. (2004) · CERN Document Server (European Organization for Nuclear Research) · Cited by 105
Fourier analysis of luminosity-dependent galaxy clustering
Percival, W. J., Verde, L., & Peacock, J. A. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2004.07245.x · Cited by 93
Non-perturbative effects of geometry in wide-angle redshift distortions
Pápai, P., & Szapudi, I. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13572.x · Cited by 93 · cited 1×
“The wide angle description of redshift space distortions has been laid out in several papers (Szalay et al. 1997; Szapudi 2004; Matsubara 2004; Papai & Szapudi 2008; Raccanelli et al. 2010), which we summarise in Appendix C.”
BackgroundWide‐Angle Redshift Distortions Revisited
Szapudi, I. (2004) · The Astrophysical Journal · doi:10.1086/423168 · Cited by 93 · cited 1×
“The wide angle description of redshift space distortions has been laid out in several papers (Szalay et al. 1997; Szapudi 2004; Matsubara 2004; Papai & Szapudi 2008; Raccanelli et al. 2010), which we summarise in Appendix C.”
BackgroundWhat is the best way to measure baryonic acoustic oscillations?
Sánchez, A. G., Baugh, C. M., & Angulo, R. E. (2008) · Max Planck Digital Library · Cited by 93
Non-Gaussian fluctuations and the statistics of galaxy clustering
Weinberg, D. H., & Cole, S. (1992) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/259.4.652 · Cited by 88
Theoretical uncertainty in baryon oscillations
Eisenstein, D. J., & White, M. J. (2004) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.70.103523 · Cited by 78 · cited 1×
“Beside the fact that the Hubble constant H0 cancels out in the determination of R, this ratio is also more robust against effects caused by possible extra relativistic species (Eisenstein & White 2004).”
BackgroundMeasuring Angular Diameter Distances through Halo Clustering
Cooray, A. R., Hu, W., Dragan Huterer, A., & Joffre, M. (2001) · The Astrophysical Journal · doi:10.1086/323323 · Cited by 74 · cited 1×
“Very interesting for cosmology is the idea of using the sound horizon scale as a standard ruler (Eisenstein, Hu & Tegmark 1998; Cooray et al. 2001; Seo & Eisenstein 2003; Blake & Glazebrook 2003).”
BackgroundRecovering the non-linear density field from the galaxy distribution with a Poisson-lognormal filter
Kitaura, F.-S., Jasche, J., & Metcalf, R. B. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.16163.x · Cited by 73 · cited 1×
“To obtain reliable error-bars for the correlation function we use log-normal realisations (Coles & Jones 1991; Cole et al. 2005; Kitaura et al. 2009).”
MethodFourier analysis of luminosity-dependent galaxy clusteringPreprint
Percival, W. J., Verde, L., & Peacock, J. A. (2003) · Cited by 67
Power spectrum of the maxBCG sample: detection of acoustic oscillations using galaxy clusters
Hütsi, G. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15824.x · Cited by 65
RELIABILITY OF THE DETECTION OF THE BARYON ACOUSTIC PEAK
Martı́nez, V. J., Arnalte-Mur, P., Saar, E., de la Cruz, P., Pons-Bordería, M. J., Paredes, S., Fernández-Soto, A., & Tempel, E. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/696/1/l93 · Cited by 61
Wide Angle Redshift Distortions Revisited
Szapudi, I. (2004) · CERN Document Server (European Organization for Nuclear Research) · Cited by 57
Systematic effects in the sound horizon scale measurements
Guzik, J., Bernstein, G. M., & Smith, R. C. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11385.x · Cited by 51
Labini, F. S., Vasilyev, N. L., Baryshev, Y. V., & López-Corredoira, M. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200911987 · Cited by 49 · cited 1×
“Other studies of the same data found similar results using the correlation function ξ(s) (Martinez 2009; Gaztanaga, Cabre & Hui 2009; Labini et al. 2009; Sanchez et al. 2009; Kazin et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the…”
ResultMeasuring Angular Diameter Distances through Halo Clustering
Cooray, A. R., Hu, W., Dragan Huterer, A., & Joffre, M. (2001) · CERN Document Server (European Organization for Nuclear Research) · Cited by 47
Possible Detection of Baryonic Fluctuations in the Large‐Scale Structure Power Spectrum
Miller, C. J., Nichol, R. C., & Batuski, D. J. (2001) · The Astrophysical Journal · doi:10.1086/321468 · Cited by 46
Power spectrum of the SDSS luminous red galaxies: constraints on cosmological parameters
Hütsi, G. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20065377 · Cited by 45
Large-scale structure in the H I Parkes All-Sky Survey: filling the voids with H I galaxies?
Basilakos, S., Plionis, M., Kovač, K., & Voglis, N. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11781.x · Cited by 44 · cited 1×
“For WALLABY we used a bias of 0.7 (based on the results found in the HIPASS survey; Basilakos et al. 2007).”
MethodInfluentialKazin, E. A., Blanton, M. R., Scoccimarro, R., McBride, C. K., & Berlind, A. A. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/719/2/1032 · Cited by 42 · cited 3×
“Another motivation for our study is that the SDSS data after data release 3 (DR3) show more correlation on large scales than expected by ΛCDM and have no sign of a crossover to negative ξ up to 200h−1 Mpc (the ΛCDM prediction is 140h−1 Mpc) (Kazin et al. 2010).”
BackgroundMethodResultLabini, F. S., Vasilyev, N. L., Baryshev, Y. V., & López-Corredoira, M. (2009) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/200911987/pdf · Cited by 41
Dynamics of cosmological perturbations in position space
Bashinsky, S., & Bertschinger, E. (2002) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.65.123008 · Cited by 39 · cited 1×
“Through this process each over-density of the original density perturbation field has evolved to become a centrally peaked perturbation surrounded by a spherical shell (Bashinsky & Bertschinger 2001, 2002; Eisenstein, Seo & White 2007).”
BackgroundDetermination of the Baryon Density from Large‐Scale Galaxy Redshift Surveys
Goldberg, D. M., & Strauss, M. A. (1998) · The Astrophysical Journal · doi:10.1086/305284 · Cited by 39 · cited 1×
“Since the signal appears at very large scales, it is necessary to probe a large volume of the universe to decrease sample variance, which dominates the error on these scales (Tegmark 1997; Goldberg & Strauss 1998; Eisenstein, Hu & Tegmark 1998).”
BackgroundBashinsky, S., & Bertschinger, E. (2001) · Physical Review Letters · doi:10.1103/physrevlett.87.081301 · Cited by 37 · cited 1×
“Through this process each over-density of the original density perturbation field has evolved to become a centrally peaked perturbation surrounded by a spherical shell (Bashinsky & Bertschinger 2001, 2002; Eisenstein, Seo & White 2007).”
BackgroundBaryon Acoustic OscillationsPreprint
Bassett, B. A., & Hložek, R. (2009) · arXiv (Cornell University) · doi:10.48550/arxiv.0910.5224 · Cited by 19
Galaxies as tracers of the mass distribution
Efstathiou, G. (2008) · Springer eBooks · doi:10.1007/bfb0118824 · Cited by 10 · cited 1×
“Other authors have used the so called J3-weighting which optimises the error over all scales by weighting each scale differently (e.g. Efstathiou 1988; Loveday et al. 1995).”
MethodAorta Fluorescence Imaging by Using Confocal Microscopy
Wang, C., Tsai, J.-C., Chuang, C., Hsieh, Y., & Sun, C. (2011) · ISRN Cardiology · doi:10.5402/2011/215627 · Cited by 2
Research works printed but not linked: 2
- Arnalte-Mur, 2011, MNRAS
- Sanchez, 2008, MNRAS, 390, 1470
Cited by
Sorted by citations
Planck 2018 results: VI. Cosmological parameters
Planck Collaboration, Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., et al. (2020) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201833910 · Cited by 14,258
Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201525830 · Cited by 10,685
“XIII. shows DV/rdrag from the analysis of Anderson et al. (2014), updating the BOSS-DR9 analysis of Anderson et al. (2012) used in PCP13.”
InfluentialPlanck 2013 results. XVI. Cosmological parameters
Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321591 · Cited by 8,459
Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., et al. (2016) · Research at the University of Copenhagen (University of Copenhagen) · doi:10.17863/cam.32861 · Cited by 5,299
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE ( WMAP ) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS
Hinshaw, G., Larson, D., Komatsu, E., Spergel, D. N., Bennett, C. L., Dunkley, J., Nolta, M. R., Halpern, M., Hill, R. S., Odegard, N., et al. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/208/2/19 · Cited by 5,121
“At lower redshift, z = 0.1, a detection of the BAO scale has been made using the 6dFGS survey (Beutler et al. 2011).”
BackgroundMethodInfluential
Metadata
- Authors
- Beutler, F., Blake, C., Colless, M., Jones, D. H., Staveley-Smith, L., Campbell, L., Parker, Q., Saunders, W., & Watson, F.
- Affiliations
- The University of Western Australia (AU)
- Swinburne University of Technology (AU)
- Australian Astronomical Observatory (AU)
- Monash University (AU)
- Western Kentucky University (US)
- Corresponding author
- Beutler, Florian
- ORCID
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2011-07-25
- Volume
- 416
- Issue
- 4
- Pages
- 3017-3032
- ISSN
- 0035-8711 (ISSN-L)
- OpenAlex
- W2121951791
- Cited by
- 2,590
- References
- 87
- Citations by year
- 2026: 90 · 2025: 191 · 2024: 228 · 2023: 207 · 2022: 210 · 2021: 236 · 2020: 241 · 2019: 207 · 2018: 176 · 2017: 178 · 2016: 167 · 2015: 131 · 2014: 147 · 2013: 113 · 2012: 61
- FWCI
- 54.71
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- UWA Profiles and Research Repository (UWA) (publishedVersion, other-oa)
- arXiv (Cornell University) (submittedVersion)
- Figshare (submittedVersion, cc-by)
- The HKU Scholars Hub (University of Hong Kong) (submittedVersion)
- ANU Open Research (Australian National University) (submittedVersion)
- Swinburne figshare (Swinburne University of Technology) (submittedVersion)
- arXiv (Cornell University)
- American Astronomical Society Meeting Abstracts #219
- Swinburne figshare (Swinburne University of Technology)
- Funders
- Australian Government
- Australian National University
- Australian Research Council (DP0208876)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- baryon acoustic oscillations, 6dF Galaxy Survey, local Hubble constant, sound horizon, distance-redshift relation, dark energy equation of state, wallabies, taipan, radio galaxy surveys, cosmological constraints
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