Overview

David Spergel
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Overview Surveys

Nikhil Padmanabhan
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Unbiased Reconstruction of Initial Density Field from Biased Tracers

Houjun Mo
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Measurement of Galaxy Bias from the Three-Point Function

Chi-Ting Chiang
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Chime

Kendrick Smith
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Ellipticity and Substructure of Halos

Bhuvnesh Jain
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Overview - RS

Ravi Sheth
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Orthogonal Polynomials for Bias

Vincent Desjacques
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

(Assembly) Bias from Excursion Sets, Peaks and Other Creatures

Marcello Musso
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.

Halo Formation for CDM Models

Christiano Porciani
September 24, 2015
The interpretation of low-redshift galaxy surveys is more complicated than the interpretation of CMB temperature anisotropies. First, the matter distribution evolves nonlinearly at low redshift, limiting the use of perturbative methods. Secondly, we observe galaxies, rather than the underlying matter field. Fortunately, considerable progress has been made in understanding the large-scale structure of galaxies. A key insight has been that galaxies form in bound structures called halos, whose statistics (e.g.