Remarks on General Perturbative Bias Expansion, and Precision Measurements of b_1, b_2, b_3

Fabian Schmidt
September 25, 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.

Perturbative Interaction Approach to Large-Scale Structure Formation

Yacine Ali Haimoud
September 25, 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 Bias Beyond CDM

Marilena LoVerde
September 25, 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.

Tracing Mass, Light, and Stars on Large Scales

Neta Bahcall
September 25, 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.

Ramsey numbers of degenerate graphs

Choongbum Lee
Massachusetts Institute of Technology
September 28, 2015
The Ramsey number of a graph $G$ is the minimum integer $n$ for which every edge-coloring of the complete graph on $n$ vertices with two colors contains a monochromatic copy of $G$. A graph is $d$-degenerate if all its subgraphs have a vertex of degree at most $d$. In this talk, we prove that for all $d$, there exists a constant $c$ such that every $d$-degenerate graph $G$ has Ramsey number at most $c|V(G)|$. This solves a conjecture of Burr and Erdős from 1973.