INTRODUCTION
- (1) the snapshots giving the positions (and velocities) of the DM particles as obtained after the collisionless runs
- (2) the halo catalogues wich list the properties of the haloes constructed with the FOF groupfinding algorithm
- (3) the semi-analytic (photometric and baryonic) properties of the simulated galaxies.
-
Snapshots of Dark Matter: they provide with the positions
and peculiar velocities of the dark matter particles, as dumped by
GADGET. The positions are given in supergalactic coordinates (SG):
[SGX,SGY,SGZ], and are centered on the Milky-Way. They extend in
radius to some 8000 km/s. As emphasized,
we provide only here a randomly sampled subset of the whole distribution.
-
Halo Catalogues: they contain the physical properties of all the
DM haloes. Our groupfinder algorithm (with a linking length
of 0.2 times the mean interparticle separation) has also produced a
"linked list" of particles (which is used to retrieve all the particles belonging
to a halo). However, the linked list is useless without the full particle
distribution, and therefore we do not release it. Recall that the
haloes we consider contain at least 10 particles. Among the
physical properties are the position and velocity of the center of
mass, the position of the most bound particle, the total and virial mass,
virial radius, and circular velocity. Note that the virial
radius is defined as the radius within which the mean DM density is 200
times the critical density of the Universe.
-
Galaxy Catalogues: having constructed a merger tree on the
DM skeletton, the semi-analytic (SA) prescription allows us to graft
galaxy formation on it. The galaxy catalogues, obtained after
running the SA algorithm on the merger trees, are restricted to satellite and
central galaxies (we discarded the field galaxies, which are not
member of any halo at z=0). One will find in these galaxy
catalogues the position and velocity of the DM particle
associated with the galaxy, the identity of the galaxy
(which is by definition the identity of the particle) and its parent
halo (among the haloes given in the halo catalogues), whether it is a
satellite or a central galaxy, and most importantly its
photometric (total and bulge component luminosities) and baryonic properties
(such as stellar mass).
- total number of particles in the halo as found by the groupfinder
- virial radius
- virial mass
- circular velocity
- position of the center of mass
- position of the most bound particle
- velocity of the center of mass
- identity of the galaxy (i.e. that of the DM particle to which it is associated)
- identity of the halo which hosts the galaxy
- total number of particles in that halo (found by the groupfinder)
- whether the galaxy is a satellite or a central galaxy
- the position of the galaxy (i.e. that of its associated DM particle)
- the peculiar velocity of the galaxy (i.e. that of its associated DM particle)
- the total luminosity at z=0 of the galaxy, in four bands: B, V, I, K
- the luminosity at z=0 of the bulge component of the galaxy, in four bands : B, V, I, K
- the mass of cold gas
- the total stellar mass
- the stellar mass of the bulge component
- the total star formation rate, estimated during the most recent redshift interval, including starburst and quiescent star formation
- the redshift when the galaxy was last a central galaxy
- the virial mass of the halo when the galaxy was last a central galaxy
- the disk velocity of the galaxy
The constrained simulations of the Local Universe consist mainly of three types
of data:
Here, we briefly describe the generation and the contents of the files. The formats and units of the data are given in the codes (both F90 and IDL) provided in the reading routines section.
Please note that so far, data are given at z=0 only. Also, for the purpose of speeding up the download of the large files containing the distribution of the dark matter particles, we only provide the DM distribution randomly sampled at a 10% rate.
Finally, all data given here refer to the high resolution
zone of the simulations.
Note that the haloes are given ordered : the first halo read corresponds to the halo with identity # 1.
The units are given in the reading routines.
Note that the galaxies are given fully unordered : if for instance the first galaxy read is the central galaxy of the halo with identity # 26, the second galaxy read can be, e.g., a satellite galaxy of the halo with identity # 219. However, there is of course sufficient information in the galaxy catalogues to reconstruct the full population of a given halo.
The units are given in the reading routines.
SIMULATION PARAMETERS
We define H0=100 h km/s/Mpc. The
other parameters follow standard notation.
| Model | Omega0 | Lambda | h | Gamma | Sigma8 |
| LCDM | 0.3 | 0.7 | 0.7 | 0.21 | 0.9 |
| TCDM | 1.0 | 0.0 | 0.5 | 0.21 | 0.6 |
The subscripts "hr" and "lr" refer to the high and low resolution regions, respectively.
N is the number of (DM) particles, M the mass (units
Msun/h) of one particle, and lsoft is the
physical softening length (units kpc/h).
| Model | Nhr | Mhr (Msun/h) | lsoft,hr (kpc/h) | Nlr | Mlr (Msun/h) | lsoft,lr (kpc/h) |
| LCDM | 50730389 | 0.357 x 1010 | 20 | 20506522 | 14.386 x 1010 | 120 |
| TCDM | 53302154 | 1.18978 x 1010 | 20 | 20442823 | 47.952 x 1010 | 120 |
fbar is the baryon fraction: fbar=Omegabar/Omega0
alpha the star formation efficiency, epsilon the SNe feedback efficiency
fbulge is the ratio of the satellite galaxy mass to the central galaxy mass beyond which a merger is supposed to trigger a starburst and form a bulge component
"Feedback" gives the hypothesis that we made fot eh fate
of the cold gas reheated by the SNe (ejected from the DM halo and
later reincorporated or always retained in the halo)
MB,lum is the luminosity resolution limit of the simulations (in the B band)
MB,morpho the
morphology resolution limit.
| Model | fbar | alpha | epsilon | fbulge | Feedback | MB,lum | MB,morpho |
| LCDM | 0.12 | 0.05 | 0.05 | 0.1 | retention | -16.25 | -18.46 |
| TCDM | 0.2 | 0.15 | 0.03 | 0.1 | ejection | -18.45 | -20.61 |
Milky Way look-alikes are defined as galaxies of type Sb/Sc with a disk circular velocity betwen 200 and 240 km/s.
In the table below, masses are given in units of Msun, disk star
formation rates in units of Msun/year, and we give our zero-point
normalization of the Tully-Fisher realtion.
| Model | Stellar mass | Cold Gas mass | disk SFR | MB- 5 log h | MI- 5 log h | B-V | Number |
| LCDM | 9.32 x 1010 | 1.05 x 1010 | 1.78 | -20.02 | -22.01 | 0.74 | 229 |
| TCDM | 1.58 x 1011 | 1.15 x 1010 | 3.37 | -20.04 | -21.99 | 0.71 | 941 |
READING ROUTINES
-
Note that the units of the fields are given as comments in the routines.
| Type of file | F90 | IDL |
| Full set of routines | ReadAll_F90 | ReadAll_IDL |
| Sampled DM distribution | ReadParts.F | ReadParts.pro |
| Halo catalogue | ReadHaloCat.F | ReadHaloCat.pro |
| Galaxy catalogue | ReadGalCat.F | ReadGalCat.pro |
| Mark III catalogue | ReadMarkIII.F | ReadMarkIII.pro |
| Mock Mark III catalogue | ReadMockMarkIII.F | ReadMockMarkIII.pro |
SAMPLED DARK MATTER DISTRIBUTIONS
| Model | DM distribution sampled at 10% |
| LCDM | DMSampledLCDM.dat (79 MB) |
| TCDM | DMSampledTCDM.dat (92 MB) |
HALO CATALOGUES
| LCDM | TCDM |
| cat.halosLCDM (11 MB) | cat.halosTCDM (11 MB) |
GALAXY CATALOGUES
We that the use of the galaxy catalogues below, and even around the luminosity resolution limit quoted here requires a lot of caution, and is left to the responsibility of the users !
So as to be complete, we provide here two full
catalogues (with and without dust) which are not cut in
resolution. Besides, we also give a catalogue cut at the luminosity resolution
limit, not including dust correction, e.g. to obtain a Tully-Fisher
relation to be compared to that of Giovanelli et al. (1997).
| Model | Full catalogue without dust correction | Full catalogue with dust correction | Catalogue cut at the luminosity resolution without dust correction | Catalogue cut at the luminosity resolution with dust correction | Catalogue cut at the morphology resolution with dust correction |
| LCDM | cat_full.galsLCDM (37 MB) | cat_dust_full.galsLCDM (37 MB) | cat_cutLum.galsLCDM (11 MB) | cat_dust_cutLum.galsLCDM (11 MB) | cat_dust_cutMorpho.galsLCDM (1.8 MB) |
| TCDM | cat_full.galsTCDM (31 MB) | cat_dust_full.galsTCDM (31 MB) | cat_cutLum.galsTCDM (12 MB) | cat_dust_cutLum.galsTCDM (12 MB) | cat_dust_cutMorpho.galsTCDM (1.7 MB) |
MARK III AND MOCK MARK III CATALOGUES
Mock Mark III catalogues of peculiar velocities have been constructed for both cosmologies. They are available as gzipped .tar files (1.2 MB, including the real data).
The reading routines (together with the descriptions of the fields and the units of the data) are given above.
CATALOGUES FOR TEST VOID POPULATIONS
We give in the following table the series of galaxy and halo populations
that we considered for hypothetical void fillers in the LCDM
simulation analysed in
astro-ph/0201193.
For each property, we have separated 7 samples (see preprint). The
samples GL and GC are selected above the luminosity resolution limit
of the simulation; the sample GM is above the morphology resolution
limit. Note that galaxies have been corrected for internal dust
extinction.
The reading routines (together with
the descriptions of the fields and the units of the data) are given
above. For simplicity, the
catalogues of DM haloes selected by their mass
are written in the format of the galaxy catalogues. There, only the
position, mass of the group giving the number of particles and virial
mass are relevant fields.
The disk circular velocity is replaced by the virial circular
velocity of the halo. Other fields have been set to default
values. Alternatively, one can build the samples
described in astro-ph/0201193 directly from the above full dust corrected
galaxy catalogue and from the halo catalogue.
| Property | 1 | 2 | 3 | 4 | 5 | 6 | 7 |
| Halo Mass (HM) | HM1(3.4 MB) | HM2 | HM3 | HM4 | HM5 | HM6 | HM7 |
| Galaxy Luminosity (GL) | GL1(6.5 MB) | GL2(2.9 MB) | GL3(1.3 MB) | GL4 | GL5 | GL6 | GL7 |
| Galaxy Colour (GC) | GC1 | GC2(1.7 MB) | GC3(4.5 MB) | GC4(2.4 MB) | GC5 | GC6(2.2 MB) | GC7 |
| Galaxy Morphology (GM) | GM1 | GM2 | GM3 | GM4 | GM5 | GM6 | GM7 |
Back to the Constrained Realizations Main Page
Back to the Data Download page for other Virgo projects
Back to the Galaxy Formation Group at MPA
Back to NumCos
Last modified: 2006-05-02 14:17:54 CEST