SDSS galaxy bias from halo mass-bias relation and its cosmological implications

By Uros Seljak, A. Makarov, Rachel Mandelbaum, C. Hirata, Nikhil Padmanabhan, P. Mcdonald, M. Blanton, Max Tegmark, N. Bahcall, J. Brinkmann. 2004

133 citations recorded by the source corpus.

We combine the measurements of luminosity dependence of bias with the luminosity dependent weak lensing analysis of dark matter around galaxies to derive the galaxy bias and constrain amplitude of mass fluctuations. We take advantage of theoretical and simulation predictions that predict that, while halo bias is rapidly increasing with mass for high masses, it is nearly constant in low mass halos. We use a new weak lensing analysis around the same Sloan Digital Sky Survey (SDSS) galaxies to determine their halo mass probability distribution. We use these halo mass probability distributions to predict the bias for each luminosity subsample. Galaxies below L{sub *} are antibiased with b<1 and for these galaxies bias is only weakly dependent on luminosity. In contrast, for galaxies above L{sub *} bias is rapidly increasing with luminosity. These observations are in an excellent agreement with theoretical predictions based on weak lensing halo mass determination combined with halo bias-mass relations. We find that for standard cosmological parameters theoretical predictions are able to explain the observed luminosity dependence of bias over six magnitudes in absolute luminosity. We combine the bias constraints with those from the Wilkinson Microwave Anisotropy Probe (WMAP) and the SDSS power spectrum analysis tomore » derive new constraints on bias and {sigma}{sub 8}. For the most general parameter space that includes running and neutrino mass, we find {sigma}{sub 8}=0.88{+-}0.06 and b{sub *}=0.99{+-}0.07. In the context of spatially flat models we improve the limit on the neutrino mass for the case of three degenerate families from m{sub {nu}}<0.6 eV without bias to m{sub {nu}}<0.18 eV with bias (95% C.L.), which is weakened to m{sub {nu}}<0.24 eV if running is allowed. The corresponding limit for 3 massless+1 massive neutrino is 1.37 eV.« less

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/dbea1c90ced4c7317dc38dcfd35f3238cbf46a58

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

The CFHTLS strong lensing legacy survey - I. Survey overview and T0002 release sample (2006, methodology): “It complements the galaxy-galaxy lensing methods that explore galaxy haloes on much larger scales (Hoekstra et al. 2004; Seljak et al. 2005).”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “This results in the ‘linear’ halo model, which has been used previously by numerous authors (e.g., Ma & Fry 2000; Seljak 2000; Scoccimarro et al. 2001; Guzik & Seljak 2002; Mandelbaum et al. 2005; Seljak et al. 2005; see also Cooray & Sheth 2002 and Mo et al. 2010).”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “Clustering of galaxies and Lyα forest observations have been used to obtain some of the strongest limits on neutrino masses (Seljak et al. 2005b; Seljak et al. 2006; Viel et al. 2006).”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, methodology): “A first application of this idea by Seljak et al. (2005), when combined with WMAP constraints, yielded a relative high value for σ8 of 0.88± 0.06 (for Ωm ≃ 0.25).”
Physical properties and environments of nearby galaxies (2009, background): “Interestingly, such a trend is exactly what is required for the ΛCDM mass function, with its slow cutoff at high mass and steep faint-end slope, to successfully produce the observed luminosity function (§2.3; Tasitsiomi et al. 2004; Seljak et al. 2005).”
Cosmological Parameters from the 2003 Flight of BOOMERANG (2005, methodology): “The LSS Data For our final data combination we also include LSS observations from 2dFGRS and the SDSS.”
Systematic errors in weak lensing: application to SDSS galaxy-galaxy weak lensing (2005, background): “Points have a slight horizontal offset so that error bars on all three signals are visible. source samples for all six luminosity bins, with statistical error bars only, and the results of halo model fits to the signal as described in Seljak et al. (2005) and Mandelbaum et al. (2004).”
The DEEP2 Galaxy Redshift Survey: Color and Luminosity Dependence of Galaxy Clustering at z ∼ 1 (2007, methodology): “Cosmological parameters consistent with those measured from the first year WMAP data (Spergel et al. 2003; Seljak et al. 2005) were used.”
Simultaneous measurement of cosmology and intrinsic alignments using joint cosmic shear and galaxy number density correlations (2009, background): “…Zhan 2006; Blake et al. 2007; Padmanabhan et al. 2007) galaxygalaxy lensing (e.g. Schneider & Rix 1997; Guzik & Seljak 2001, 2002; Seljak 2002; Seljak et al. 2005; Yoo et al. 2006; Johnston et al. 2007; Cacciato et al. 2009) and lensing magnification (Broadhurst et al. 1995; Zhang & Pen 2005,…”
Galaxy halo masses and satellite fractions from galaxy–galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies (2005, methodology): “In the latest Sloan Digital Sky Survey (SDSS) analyses (Sheldon et al. 2004; Seljak et al. 2005), 20–30σ detections of the signal as a function of physical separation have been obtained.”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, methodology): “…con- tains no useful information on small scales, the galaxy-dark matter correlation does contain information on halo mass, which in combination with the galaxy auto-correlation on large scales can provide independent cosmological information using the method of Seljak et al. (2005).”
KiDS+GAMA : cosmology constraints from a joint analysis of cosmic shear, galaxy-galaxy lensing, and angular clustering (2017, background): “…by the displacement of the posteriors in the m–σ 8 plane between PE and Pgm + Pgg. Finally, it is interesting to note that PE and Pgm + Pgg have similar statistical power, even though the latter is measured on less than half the survey area (see also Seljak et al. 2005; Mandelbaum et al. 2013).”