Mathematics – Logic
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.3203k&link_type=abstract
American Astronomical Society Meeting 210, #32.03; Bulletin of the American Astronomical Society, Vol. 39, p.144
Mathematics
Logic
Scientific paper
We study properties of gas accreted by galaxies that form and evolve in the cosmological SPH simulations using entropy and energy conserving code Gadget-2. Similar to our previous findings we find that at early times and in lower mass halos galaxies grow through cold accretion mode where gas streams into a central galaxy on a free fall times scale, in filamentary flows, without experiencing strong shock in the halo.
However, our new simulations show that, although hot virialized gas does develop in massive halos, the accretion from this hot atmosphere almost stops for the wide range of halo masses and redshifts. The typical accretion rates in massive halos are much lower that in the SAMs of galaxy formation making classical "hot mode accretion" only a minor supply channel for the global growth of galaxy population.
We also compare the properties of the population of simulated galaxies with the observed galaxy population and find that simulated galaxies are too massive and have specific star formation substantially different from the observed galaxies. Such comparison enables us to discuss what kind of feedback mechanisms are needed to bring the properties of simulated galaxies in agreement with observations. For example, even without significant late time accretion of central galaxies in the massive halos, the high mass end of the simulated galaxy mass function is much higher than the observed one.
The reason for this is that the most massive galaxies formed in the sequence of mergers and their progenitors accumulated their mass at high redshifts. Therefore to enable properties of the simulated massive galaxies to agree with observations one has to have very efficient feedback in smaller objects especially at high redhists, which could also help bridging the differences at the low mass end of the mass function.
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