This database stores lightcones derived from the Millennium Run galaxy catalogue in the Guo2010a database.
This link contains
a description of the "virtual observation" algorithm, as presented in
Henriques et al. (2012).
The lightcones were created using an updated version of the MoMaF code
(see Blaizot et al. (2005))
and the semi-analytic model presented in
Guo et al. (2011).
If you use the data from this dataset, please cite
Henriques et al. (2012) and
Guo et al. (2011)
as well as the relevant papers mentioned in the general
G. Lemson & the Virgo Consortium (2006) and
V. Springel et al. (2005).
The database stores cones for galaxy catalogues created with the same physics, but using two different
stellar population synthesis algorithms, Bruzual & Charlot (2003) and Maraston (2005).
For each stellar population, the first set of cones contains: 24 pencil-beam lightcones (1.4 times 1.4 square degrees)
for different lines-of-sight with observer-frame apparent magnitudes in 40 bands; the same 24 pencil-beam lightcones
with rest-frame absolute magnitudes for SDSS and VISTA/2MASS bands; one allsky lightcone with SDSS and VISTA/2MASS
observer-frame apparent magnitudes [NB as of 2012-01-17 only a BC03 allsky map is available, an M05 version will be added soon].
All magnitudes are in the AB system.
(This link fully describes
the photometric properties available, including filter curves). All physical properties of galaxies can be obtained by
joining the lightcone tables with the Guo2010a catalog.
These catalogues still assume the WMAP 1 cosmology of the Millennium simulations. A second set will be published
soon based on the WMAP 7 cosmology, produced with the scaling algorithm of Angulo & White (2010).
No flux limits are imposed, except for the all sky maps (i<21.0). Nonetheless, due to the resolution of the dark matter
simulation used to construct the semi-analytic model
(Millennium Run, see Springel et al. (2005)),
objects with stellar mass bellow 109 Msun should not be used.
In this link, we present all
the queries used to produce the plots in
Henriques et al. (2012)
(number counts, redshift distributions, B-band luminosity function, K-band luminosity function and colour distributions)
and some other useful examples.