### Abstract

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<inf>*</inf> are antibiased with b < 1 and for these galaxies bias is only weakly dependent on luminosity. In contrast, for galaxies above L<inf>*</inf> 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 to derive new constraints on bias and σ<inf>8</inf>. For the most general parameter space that includes running and neutrino mass, we find σ<inf>8</inf> = 0.88 ± 0.06 and b <inf>*</inf> = 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<inf>v</inf> < 0.6 eV without bias to m<inf>v</inf> < 0.18 eV with bias (95% C.L.), which is weakened to m<inf>v</inf> < 0.24 eV if running is allowed. The corresponding limit for 3 massless + 1 massive neutrino is 1.37 eV.

Original language | English (US) |
---|---|

Article number | 043511 |

Journal | Physical Review D - Particles, Fields, Gravitation and Cosmology |

Volume | 71 |

Issue number | 4 |

DOIs | |

State | Published - 2005 |

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### ASJC Scopus subject areas

- Physics and Astronomy(all)
- Nuclear and High Energy Physics
- Mathematical Physics

### Cite this

*Physical Review D - Particles, Fields, Gravitation and Cosmology*,

*71*(4), [043511]. https://doi.org/10.1103/PhysRevD.71.043511

**SDSS galaxy bias from halo mass-bias relation and its cosmological implications.** / Seljak, Uroš; Makarov, Alexey; Mandelbaum, Rachel; Hirata, Christopher M.; Padmanabhan, Nikhil; McDonald, Patrick; Blanton, Michael R.; Tegmark, Max; Bahcall, Neta A.; Brinkmann, J.

Research output: Contribution to journal › Article

*Physical Review D - Particles, Fields, Gravitation and Cosmology*, vol. 71, no. 4, 043511. https://doi.org/10.1103/PhysRevD.71.043511

}

TY - JOUR

T1 - SDSS galaxy bias from halo mass-bias relation and its cosmological implications

AU - Seljak, Uroš

AU - Makarov, Alexey

AU - Mandelbaum, Rachel

AU - Hirata, Christopher M.

AU - Padmanabhan, Nikhil

AU - McDonald, Patrick

AU - Blanton, Michael R.

AU - Tegmark, Max

AU - Bahcall, Neta A.

AU - Brinkmann, J.

PY - 2005

Y1 - 2005

N2 - 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* are antibiased with b < 1 and for these galaxies bias is only weakly dependent on luminosity. In contrast, for galaxies above L* 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 to derive new constraints on bias and σ8. For the most general parameter space that includes running and neutrino mass, we find σ8 = 0.88 ± 0.06 and b * = 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 mv < 0.6 eV without bias to mv < 0.18 eV with bias (95% C.L.), which is weakened to mv < 0.24 eV if running is allowed. The corresponding limit for 3 massless + 1 massive neutrino is 1.37 eV.

AB - 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* are antibiased with b < 1 and for these galaxies bias is only weakly dependent on luminosity. In contrast, for galaxies above L* 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 to derive new constraints on bias and σ8. For the most general parameter space that includes running and neutrino mass, we find σ8 = 0.88 ± 0.06 and b * = 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 mv < 0.6 eV without bias to mv < 0.18 eV with bias (95% C.L.), which is weakened to mv < 0.24 eV if running is allowed. The corresponding limit for 3 massless + 1 massive neutrino is 1.37 eV.

UR - http://www.scopus.com/inward/record.url?scp=84927714372&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84927714372&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.71.043511

DO - 10.1103/PhysRevD.71.043511

M3 - Article

VL - 71

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 1550-7998

IS - 4

M1 - 043511

ER -