The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample

A test for the ACDM cosmology

Sebastián E. Nuza, Ariel G. Sánchez, Francisco Prada, Anatoly Klypin, David J. Schlegel, Stefan Gottlöber, Antonio D. Montero-Dorta, Marc Manera, Cameron K. McBride, Ashley J. Ross, Raul Angulo, Michael Blanton, Adam Bolton, Ginevra Favole, Lado Samushia, Francesco Montesano, Will J. Percival, Nikhil Padmanabhan, Matthias Steinmetz, Jeremy Tinker & 11 others Ramin Skibba, Donald P. Schneider, Hong Guo, Idit Zehavi, Zheng Zheng, Dmitry Bizyaev, Olena Malanushenko, Viktor Malanushenko, Audrey E. Oravetz, Daniel J. Oravetz, Alaina C. Shelden

    Research output: Contribution to journalArticle

    Abstract

    We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.

    Original languageEnglish (US)
    Pages (from-to)743-760
    Number of pages18
    JournalMonthly Notices of the Royal Astronomical Society
    Volume432
    Issue number1
    DOIs
    StatePublished - Jun 2013

    Fingerprint

    cosmology
    dark matter
    galaxies
    halos
    acoustics
    power spectra
    oscillation
    estimates
    Microwave Anisotropy Probe
    oscillations
    damping
    simulation
    test
    cold
    dip
    anisotropy
    catalogs
    probe
    baryons
    statistics

    Keywords

    • General-cosmology
    • Methods
    • Numerical-methods
    • Observational-galaxies
    • Theory-large-scale structure of Universe

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample : A test for the ACDM cosmology. / Nuza, Sebastián E.; Sánchez, Ariel G.; Prada, Francisco; Klypin, Anatoly; Schlegel, David J.; Gottlöber, Stefan; Montero-Dorta, Antonio D.; Manera, Marc; McBride, Cameron K.; Ross, Ashley J.; Angulo, Raul; Blanton, Michael; Bolton, Adam; Favole, Ginevra; Samushia, Lado; Montesano, Francesco; Percival, Will J.; Padmanabhan, Nikhil; Steinmetz, Matthias; Tinker, Jeremy; Skibba, Ramin; Schneider, Donald P.; Guo, Hong; Zehavi, Idit; Zheng, Zheng; Bizyaev, Dmitry; Malanushenko, Olena; Malanushenko, Viktor; Oravetz, Audrey E.; Oravetz, Daniel J.; Shelden, Alaina C.

    In: Monthly Notices of the Royal Astronomical Society, Vol. 432, No. 1, 06.2013, p. 743-760.

    Research output: Contribution to journalArticle

    Nuza, SE, Sánchez, AG, Prada, F, Klypin, A, Schlegel, DJ, Gottlöber, S, Montero-Dorta, AD, Manera, M, McBride, CK, Ross, AJ, Angulo, R, Blanton, M, Bolton, A, Favole, G, Samushia, L, Montesano, F, Percival, WJ, Padmanabhan, N, Steinmetz, M, Tinker, J, Skibba, R, Schneider, DP, Guo, H, Zehavi, I, Zheng, Z, Bizyaev, D, Malanushenko, O, Malanushenko, V, Oravetz, AE, Oravetz, DJ & Shelden, AC 2013, 'The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample: A test for the ACDM cosmology', Monthly Notices of the Royal Astronomical Society, vol. 432, no. 1, pp. 743-760. https://doi.org/10.1093/mnras/stt513
    Nuza, Sebastián E. ; Sánchez, Ariel G. ; Prada, Francisco ; Klypin, Anatoly ; Schlegel, David J. ; Gottlöber, Stefan ; Montero-Dorta, Antonio D. ; Manera, Marc ; McBride, Cameron K. ; Ross, Ashley J. ; Angulo, Raul ; Blanton, Michael ; Bolton, Adam ; Favole, Ginevra ; Samushia, Lado ; Montesano, Francesco ; Percival, Will J. ; Padmanabhan, Nikhil ; Steinmetz, Matthias ; Tinker, Jeremy ; Skibba, Ramin ; Schneider, Donald P. ; Guo, Hong ; Zehavi, Idit ; Zheng, Zheng ; Bizyaev, Dmitry ; Malanushenko, Olena ; Malanushenko, Viktor ; Oravetz, Audrey E. ; Oravetz, Daniel J. ; Shelden, Alaina C. / The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample : A test for the ACDM cosmology. In: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 432, No. 1. pp. 743-760.
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    abstract = "We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.",
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    T1 - The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample

    T2 - A test for the ACDM cosmology

    AU - Nuza, Sebastián E.

    AU - Sánchez, Ariel G.

    AU - Prada, Francisco

    AU - Klypin, Anatoly

    AU - Schlegel, David J.

    AU - Gottlöber, Stefan

    AU - Montero-Dorta, Antonio D.

    AU - Manera, Marc

    AU - McBride, Cameron K.

    AU - Ross, Ashley J.

    AU - Angulo, Raul

    AU - Blanton, Michael

    AU - Bolton, Adam

    AU - Favole, Ginevra

    AU - Samushia, Lado

    AU - Montesano, Francesco

    AU - Percival, Will J.

    AU - Padmanabhan, Nikhil

    AU - Steinmetz, Matthias

    AU - Tinker, Jeremy

    AU - Skibba, Ramin

    AU - Schneider, Donald P.

    AU - Guo, Hong

    AU - Zehavi, Idit

    AU - Zheng, Zheng

    AU - Bizyaev, Dmitry

    AU - Malanushenko, Olena

    AU - Malanushenko, Viktor

    AU - Oravetz, Audrey E.

    AU - Oravetz, Daniel J.

    AU - Shelden, Alaina C.

    PY - 2013/6

    Y1 - 2013/6

    N2 - We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.

    AB - We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.

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    KW - Methods

    KW - Numerical-methods

    KW - Observational-galaxies

    KW - Theory-large-scale structure of Universe

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