In colour the gas density, in green the stars, in yellow the leaves of DM + core of mother with Dylan’s post treatment.
In grey the metal density, in green the stars, in yellow the leaves of DM + core of mother with Dylan’s post treatment.
The corresponding dark matter adaphop structures are available on the FTP server of the HORIZON collaboration: HORIZON-FTP
3 files are found there
MN-34-adaphop.nod : all clumps in adaphop format
MN-34-leaves-with-stars.nod : all galaxy clumps
MN-34-star.nod : clumps in the star catalog
The second catalog corresponds to a post treatment of the first, following the prescription described in Sort Nodes, and a selection based the fact that each clump contains at least one star. It is our GALAXY reference catalog.
CAVEATS: the dark matter adaphop catalog and its sequels was produced by segments of 1/8th of the simulation. A reordering and overlapping recovery of the full catalog in in progress. It was shown for the FOF catalog that the difference in treatment was minimal (0.2 %).
The corresponding spectra (73k Galaxies) produced with PEGASE2 are available on the FTP server of the HORIZON collaboration: HORIZON-FTP
5 files are found there
MN-34-gal-spectra.dat (500 megas)
the first is in totor format (see below) it contains
|x y z [box fraction]||m [solarM]||age [Myr]||log10 z [mass fraction]||flux [Erg/s/solar M/cm^2 ]|
the second is the beginning of the first in ascii as a check
the third is the corresponding wavelength in Angstrom.
the forth is the table of colours in various filters relevant for high redshift objects
|x y z [box fraction]||m [solarM]||age [Myr]||log10 z [mass fraction]||observed Magnitude in G R I z K IRAC-3.6 IRAC-8.0|
The last is the first 80 lines of the fourth as a check
The following Fortran example shows how to read such files:
As a check we produced the following color diagrams from the above spectra:
Only half of the box is processed. This figure can be reproduced qualitatively from the catalogs given on the ftp server
Quantitativement, la Distribution ci dessous semble en bon accord avec les donnees publiees par Bowens et al. 2006 pour des galaxies à z 6
Once the colours have been computed, it is possible to look at one and two points statistics with the catalogs.
These are computed using the daughters of the adaphop catalogs given above.
For the galaxies above we compute the local maps within a sphere centered on the center of mass of the stars (not the gas) and compute the moment of inertia with respect to the brightest pixel. The Cumulative PDF of ellipticity (the square root of the ratio of the eigenvalues of the inertia tensor weighted by exp(-r/rmax)) is also shown there. An example of ellipsoid fit is also shown
The inner structure of galaxies within the adaphop radii. These X-Y maps correspond to the maximum pixel along the LOS. a dot shows the position of the projection of the densest pixel w.r.t. which the moment of inertia is computed.
Computed from all galaxies within 6 hires cubes near the first few most massive halos.
Mass of metal vz Mass of gas
Eccentricity of gal vz Mass of gas
colour coded in log Mass of metal. The eccentricity is defined as = sqrt(l1/l3)
The metal gas is computed within the ellipse; the stellar mass is computed within the adaphop sphere.
The size and ellipticity are measured as the long axis and sqrt(l3/l1)
catalogs of star/gas/DM
Note that here Yann chose 3 Adaphop radii to make the measurements
Yann’s & Chris’s Mstar vz Mgas
The discrepency arises because of a different choice in outer radius.
Cosmic SFH,Color, metals, density, SFR confrontation with data
Satellite accretion efficiency
Here we compute the fraction of the surface of the (rescaled) adaphop mother radius which is covered by satellites.
Genus (Euler Characteristic)
Two point correlation in redshift-real space for stars as a function
Section of filaments gas/DM;
Spectra and slices with metals species.
Accretion flow maps;
phase space morphology segmentation and NN classification