Mock Catalogues

This is a brief overview of the different aspects of the synthetic catalogues produced for ECO RESOLVE-A and RESOLVE-B surveys

For a more comprehensive discussion on how the synthetic mocks were created, you can read the ECO and Resolve Synthetic Catalogue guide.

ECO and RESOLVE

We construct a set of synthethic (mock) catalogues that have the same geometries as the Environmental COntext (ECO), RESOLVE-A, and RESOLVE-B galaxy surveys.

REsolved Spectroscopy Of a Local VolumE (RESOLVE) is a volume-limited census of stellar, gas, and dynamical mass as well as star formation and merging within >50,000 cubic Mpc of the nearby cosmic web, reaching down to the dwarf galaxy regime and up to structures on tens of Mpc scales such as filaments, walls, and voids.

The Environmental COntext (ECO) catalog around RESOLVE is a much larger, purely archival data set with pipelines and methods matched to RESOLVE, enabling statistically robust analyses of environmental trends and calibration of cosmic variance.

Full size survey of RESOLVE

This shows the right-ascension (RA) and declination (DEC) of galaxies in RESOLVE-A and RESOLVE-B galaxy redshift surveys.

RESOLVE-A (footprint demarcated by red dashed lines) embedded within ECO (entire plot showing current footprint, with ECO-B in preparation)

For more information on how the data for the different galaxy surveys were taken, go to the Main ECO and RESOLVE website.

Constructing catalogues

We design the synthetic catalogues to have the exact same geometries and redshift limits as those of the ECO, RESOLVE-A, and RESOLVE-B galaxy surveys.

This is a summary of the values used to create the synthetic galaxy catalogues. These catalogues are taking a buffer regions, which is an extra buffer region along the cz (velocity) direction in redshift-space.

Survey RA (deg) RA range DEC (deg) DEC range zmin zmax Vmin (km/s) Vmax (km/s) Dist (Mpc)
A (131.25, 236.25) 105.0 (0 ,+5) 5 0.00844 0.0249 2532
(25.32,70.02)
B (330.0 , 45.0 ) 75.0 (-1.25,+1.25) 2.5 0.01416 0.024166 4250
(42.5 , 72.5)
ECO (130.05, 237.45) 107.4 (-1, +49.85) 50.85 0.00844 0.0249 2532
(25.32,70.02)

The next table provides the number of synthetic catalogues per cubic box of L = 180 Mpc/h, where h = 1.

Survey Number Mocks
A 59
B 104
ECO 8

In order to run the Friends-of-Friends (FoF) algorithm and put galaxies into galaxy groups, we have to choose a set of linking lengths. The set of linking lengths used for this analyses are

FoF Group-finding parameters
l_perp l_para
0.07 1.1

Note

The units for the linking lengths are in terms of the mean inter-galaxy separation of the simulation.

Distribution of catalogues in simulation box

In order to maximize the number of catalogues per simulation, we have to fit as many catalogues as we can, while keeping a distance of ~10 Mpc/h between catalogues. We chose this distance of 10 Mpc/h in order to avoid using the same galaxy for different catalogues, and also to make the catalogues as independent from each other as possible.

Distribution of mock catalogues within simulation box

This figure shows how the catalogues for ECO surveys are organized within the simulation box used for this analysis.

Distribution of RESOLVE-A mock catalogues within simulation box

And this fugre shows the distribution of synthetic RESOLVE-A catalogues in the simulation box!

Downloading and reading in data from catalogues

The mock catalogues are located at http://lss.phy.vanderbilt.edu/groups/data_eco_vc/Mock_Catalogues/.

These catalogues can be downloaded as tar files, and be read by the Python package Pandas.

After having downloaded your file, you can read them in the following way:

#! /usr/bin/env python

import pandas as pd
import os

def reading_catls(filename, catl_format='.hdf5'):
    """
    Function to read ECO/RESOLVE catalogues.

    Parameters
    ----------
    filename: string
        path and name of the ECO/RESOLVE catalogue to read

    catl_format: string, optional (default = '.hdf5')
        type of file to read.
        Options:
            - '.hdf5': Reads in a catalogue in HDF5 format

    Returns
    -------
    mock_pd: pandas DataFrame
        DataFrame with galaxy/group information

    Examples
    --------
    # Specifying `filename`
    >>> filename = 'ECO_catl.hdf5'

    # Reading in Catalogue
    >>> mock_pd = reading_catls(filename, format='.hdf5')

    >>> mock_pd.head()
               x          y         z          vx          vy          vz  \
    0  10.225435  24.778214  3.148386  356.112457 -318.894409  366.721832
    1  20.945772  14.500367 -0.237940  168.731766   37.558834  447.436951
    2  21.335835  14.808488  0.004653  967.204407 -701.556763 -388.055115
    3  11.102760  21.782235  2.947002  611.646484 -179.032089  113.388794
    4  13.217764  21.214905  2.113904  120.689598  -63.448833  400.766541

       loghalom  cs_flag  haloid  halo_ngal    ...        cz_nodist      vel_tot  \
    0    12.170        1  196005          1    ...      2704.599189   602.490355
    1    11.079        1  197110          1    ...      2552.681697   479.667489
    2    11.339        1  197131          1    ...      2602.377466  1256.285409
    3    11.529        1  199056          1    ...      2467.277182   647.318259
    4    10.642        1  199118          1    ...      2513.381124   423.326770

           vel_tan     vel_pec     ra_orig  groupid    M_group g_ngal  g_galtype  \
    0   591.399858 -115.068833  215.025116        0  11.702527      1          1
    1   453.617221  155.924074  182.144134        1  11.524787      4          0
    2  1192.742240  394.485714  182.213220        1  11.524787      4          0
    3   633.928896  130.977416  210.441320        2  11.502205      1          1
    4   421.064495   43.706352  205.525386        3  10.899680      1          1

       halo_rvir
    0   0.184839
    1   0.079997
    2   0.097636
    3   0.113011
    4   0.057210
    """
    ## Checking if file exists
    if not os.path.exists(filename):
        msg = '`filename`: {0} NOT FOUND! Exiting..'.format(filename)
        raise ValueError(msg)
    ## Reading file
    if catl_format=='.hdf5':
        mock_pd = pd.read_hdf(filename)
	else:
		msg = '`catl_format` ({0}) not supported! Exiting...'.format(catl_format)
		raise ValueError(msg)

    return mock_pd

def main():
    # Specifying filename
    filename = 'ECO_catl.hdf5'
    # Reading in ECO/RESOLVE catalogue
    mock_pd = reading_catls(filename)


if __name__=='__main__':
    main()

Description of the fields in the catalogues

Each mock catalogues contains information about the galaxy, group galaxy, host halo, and more. We will denote *dark matter* as DM.

Note

The descriptions for the variables are somewhat long, so don’t forget to scroll to the right to see more.

Main Galaxy Properties

List of Parameters
Field Description Units
ra Right Ascension degrees
dec Declination degrees
cz Velocity of the galaxy (**with redshift-space distortions) km/s
M_r r-band absolute magnitude of the galaxy magnitudes
haloid Dark matter halo ID, as taking from the simulation None
loghalom logarithmic value of the DM’s mass log(Msun/h) where h=1
halo_ngal Total number of galaxies in DM halo. Number of galaxies in the mock may differ from this value None
cs_flag Type of galaxy. Halo central = 1, Halo satellite = 0 None
cz_nodist Velocity of the galaxy (without redshift-space distortions) km/s
dist_c Real distance between halo’s central galaxy and the galaxy. Mpc/h with h=1
vel_tot Total velu for peculiar velocity km/s
vel_tan Tangential component of the peculiar velocity km/s
morph Galaxy’s morphology. ‘LT’: Late Type; ‘ET’: Early type. Used either goodmorph (ECO) or MORPH (RESOLVE) keys. ‘-9999’ if no matched galaxy None
logmstar Log value of galaxy’s stellar mass. Used either ‘rpgoodmstarsnew’ (ECO) or ‘MSTARS’ (RESOLVE) keys in the files log(Msun)
rmag r-band apparent magnitude. Used either ‘rpsmoothrestrmagnew’ (ECO) or ‘SMOOTHRESTRMAG’ (RESOLVE) keys in the files. magnitudes
umag u-band apparent magnitude. Used either ‘rpsmoothrestumagnew’ (ECO) or ‘SMOOTHRESTUMAG’ (RESOLVE) keys in the files. magnitudes
fsmgr Stellar mass produced over last Gyr divided by pre-existing stellar mass from new model set. Used ‘rpmeanssfr’ (ECO) or ‘MODELFSMGR’ (RESOLVE) keys. (1/Gyr)
survey_flag Survey name, from which the properties of the real matched galaxy were extracted. None
u_r Color of the matched galaxy, i.e. (umag - rmag) magnitudes
mhi HI mass in galaxy. Used the predicted HI massed (matched to the ECO file, i.e. eco_wresa_050815.dat) and the key “MHI” (RESOLVE). To compute MHI masses using ECO, we used the formula: 10^(MHI + logmstar) Msun
groupid Group ID, to which the galaxy belongs after running Berlind2006 FoF group finder. None
g_ngal Number of galaxies in a group of galaxies None
halo_rvir Virial radius of the DM halo, to which the galaxy belongs. Mpc/h with h = 1.
M_group Abundance matched mass of the galaxy group. This was calculated by assuming a monotonic relation between DM halo mass logM_halo and the group total luminosity. For RESOLVE-B, we used a modified version of the ECO group luminosity function. Msun/h with h = 1
g_galtype Type of galaxy. Group central = 1, Group satellite = 0 None

Note

The relationship between velocities (cz’s’) is the following: (cz - cz_nodist)^2 + (vel_tan)^2 = (vel_tot)^2.

Halos Filaments

Author: Roberto Gonzales [regonzar@astro.puc.cl or regonzar@oddjob.uchicago.edu]

Affiliation: The University of Chicago, Universidad Católica de Chile

This file includes data about the filaments found in the simulation box used for these synthetic catalogues.

The catalogue can be found at http://lss.phy.vanderbilt.edu/groups/data_eco_vc/Halo_Filaments/.

List of Parameters - Halo Filaments
Field Description Units
Halo ID Halo ID number for the given DM halo in the simulation box.  
log(MHalo) Logarithmic value of the DM halo’s mass, as log(Msun/h) with h = 1
ID/Type ID of the DM halo’s environment. ‘0’: Not in a filament; ‘1’: filament node; ‘2’: part of a filament skeleton; ‘3’: within a clode radius of a filament.  
Fil ID of the halo’s filament. (-1 if not in a filament)  
Fil. Quality Quality of the filament, i.e. probability that the filament is real