Large Scale Structure
Density field, Cosmic Web environment, and galaxy type measurements
Measurements from Darvish et al. (2017) ApJ 837:16
The density field (local density), the cosmic web environment (cluster, filament, field) and galaxy type (central, satellite, isolated) are derived for a mass complete sample of galaxies out to z=1.2 from the COSMOS15 catalog (Laigle et al. 2016). The local density estimation is based on the weighted adaptive kernel smoothing algorithm (Darvish et al. 2015). The cosmic web extraction relies on the density field Hessian matrix and breaks the density field into clusters, filaments, and the field.
Two tables are currently provided and can be downloaded here.
Table 1: All galaxies used for environmental measurements are given. They are located in the range 149.33 < RA(deg) < 150.8, 1.6 < Dec(deg) < 2.83, are in the redshift range 0.1 < z < 1.2, and have stellar masses log(M/Msun)>=9.6 (Chabrier IMF). This table is also presented in Darvish et al. (2017).
Table 2: All galaxies in the redshift range 0.1 < z < 1.2 are interpolated to the environmental measurements. No mass and coordinate cuts are applied.
Density Fields
The environmental densities are from Scoville et al (2013) ApJS 206:3
The density fields for z < 3 were derived using Voronoi tesselation and adaptive smoothing of a sample of 155,954 galaxies from the K-band selected photometric redshift catalog of Ilbert et al 2013. The available files include LSS images in pdf, mpeg and 3d-fits files.
Download the density field files
Group Catalogue
This is a COSMOS X-ray group membership catalog, combining X-ray group properties from Finoguenov et al. in prep. (also 2007) with estimates for masses and radii calibrated from weak lensing (Leauthaud et al. 2010), and member galaxy information (George et al. 2011). Group redshifts have been determined by searching for red sequence overdensities within 500 kpc of the X-ray centers and are refined by using spectroscopic redshifts when available. We use groups with z<1 to ensure good optical identifications and small photoz uncertainties.
