Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7

By Rachel Mandelbaum, A. Slosar, T. Baldauf, Uros Seljak, C. Hirata, R. Nakajima, R. Reyes, Rowan J. Smith. 2012

242 citations recorded by the source corpus.

Recent studies have shown that the cross-correlation coefficient between galaxies and dark matter is very close to unity on scales outside a few virial radii of galaxy haloes, independent of the details of how galaxies populate dark matter haloes. This finding makes it possible to determine the dark matter clustering from measurements of galaxy–galaxy weak lensing and galaxy clustering. We present new cosmological parameter constraints based on large-scale measurements of spectroscopic galaxy samples from the Sloan Digital Sky Survey (SDSS) data release 7. We generalize the approach of Baldauf et al. to remove small-scale information (below 2 and 4 h^(−1) Mpc for lensing and clustering measurements, respectively), where the cross-correlation coefficient differs from unity. We derive constraints for three galaxy samples covering 7131 deg^2, containing 69 150, 62 150 and 35 088 galaxies with mean redshifts of 0.11, 0.28 and 0.40. We clearly detect scale-dependent galaxy bias for the more luminous galaxy samples, at a level consistent with theoretical expectations. When we vary both σ_8 and Ω_m (and marginalize over non-linear galaxy bias) in a flat Λ cold dark matter model, the best-constrained quantity is σ_8(Ω_m/0.25)^(0.57) = 0.80 ± 0.05 (1σ, stat. + sys.), where statistical and systematic errors (photometric redshift and shear calibration) have comparable contributions, and we have fixed n_s = 0.96 and h = 0.7. These strong constraints on the matter clustering suggest that this method is competitive with cosmic shear in current data, while having very complementary and in some ways less serious systematics. We therefore expect that this method will play a prominent role in future weak lensing surveys. When we combine these data with Wilkinson Microwave Anisotropy Probe 7-year (WMAP7) cosmic microwave background (CMB) data, constraints on σ_8, Ω_m, H_0, w_(de) and ∑m_ν become 30–80 per cent tighter than with CMB data alone, since our data break several parameter degeneracies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b1d5b62d46c450f859a16f658f903a6168034d76

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Citations in the corpus

Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, background): “…2007; van den Bosch et al. 2007; Zheng et al. 2009; Skibba & Sheth 2009; Simon et al. 2009; Ross et al. 2010; Zehavi et al. 2011; Geach et al. 2012; Parejko et al. 2013) as well as cosmology (Tinker et al. 2005; Leauthaud et al. 2011; More et al. 2013; Cacciato et al. 2013; Mandelbaum et al. 2013).”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, methodology): “12 Over the radial range 0.1–70 Mpc h−1, including small-scale information that was not used in the cosmological analysis, the S/N of the Mandelbaum et al. (2013) measurement is S/N = 36.”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, methodology): “An advantage of this method is that it has been applied extensively to Sloan Digital Sky Survey data, and thus the systematics of the method are well understood (Mandelbaum et al. 2005, 2013).”
Target Selection and Validation of DESI Luminous Red Galaxies (2022, methodology): “…gains in constraining powers when the LRG sample is combined with other observations, e.g., using the LRGs (and their massive dark matter halos) as gravitational lenses of background galaxies and the cosmic microwave background (e.g., Mandelbaum et al. 2013; Singh et al. 2020; White et al. 2022).”
KiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing (2016, background): “Similar low values for σ 8 are found in recent studies that make use of a combination of galaxy–galaxy lensing (GGL) and galaxy clustering (Cacciato et al. 2013; Mandelbaum et al. 2013; More et al. 2015).”
Dark Energy Survey Year 1 Results: A Precise H0 Estimate from DES Y1, BAO, and D/H Data (2017, background): “…et al. 2015; Alam et al. 2017); the time delays of multiply imaged quasars (e.g. Bonvin et al. 2017); and weak gravitational lensing measurements (e.g. Mandelbaum et al. 2013; Alsing, Heavens & Jaffe 2017; DES Collaboration 2017; Hildebrandt et al. 2017; Troxel et al. 2017; van Uitert et al.…”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, background): “…both numerical simulations (Kauffmann et al. 1999) and recent results from galaxy-galaxy lensing and galaxy clustering also indicate an increase of the bias with redshift (e.g., Mandelbaum et al. 2013), while Tegmark & Peebles (1998) show that the bias must be close to unity when approaching z = 0.”
Planck2015 results (2015, unknown): “…et al. 2011; Rest et al. 2014), and estimates of the amplitude of the fluctuation spectrum from weak gravitational lensing (Heymans et al. 2013; Mandelbaum et al. 2013) and the abundance of rich clusters of galaxies (Planck Collaboration XX 2014; Benson et al. 2013; Hasselfield et al. 2013b).”
KiDS+GAMA : cosmology constraints from a joint analysis of cosmic shear, galaxy-galaxy lensing, and angular clustering (2017, methodology): “These probes have been used to constrain cosmological parameters (e.g. Cacciato et al. 2013; Mandelbaum et al. 2013; More et al. 2015; Kwan et al. 2017; Nicola, Refregier & Amara 2017).”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, background): “Figure 1 from Mandelbaum et al. (2013) shows that non-linear bias affects the galaxy-dark matter cross-correlation coefficient at the 2% level at a comoving separation of4 h−170 Mpc.”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, methodology): “Based on previous work with this SDSS shape catalogue, we expect this approximation to work well for R < 5 Mpc, outside our upper limits for our fitting range (Mandelbaum et al. 2013).”
The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey (2017, methodology): “…function (or galaxy-galaxy lensing) can be combined with galaxy clustering to provide information about structure growth and dark energy (e.g., Mandelbaum et al. 2013; More et al. 2015; Leauthaud et al. 2017; Kwan et al. 2017) and, when combined with redshift-space distortions, about gravity…”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, background): “, from DES, LSST, Euclid, or CMB-S4) to measure the amplitude of clustering [68, 69].”
Intrinsic alignments of SDSS-III BOSS LOWZ sample galaxies (2014, methodology): “The catalogue of galaxies with measured shapes used in this paper (described in Reyes et al. 2012 and further character- ized in Mandelbaum et al. 2013) was generated using the reGaussianization method (Hirata & Seljak 2003) of correcting for the effects of the point-spread function (PSF) on the…”