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The hierarchical build-up of the Tully-Fisher relation | | Chiara Tonini
; Claudia Maraston
; Bodo Ziegler
; Asmus Böhm
; Daniel Thomas
; Julien Devriendt
; Joseph Silk
; | | Date: |
1 Jun 2010 | | Abstract: | We use the semi-analytic model GalICS to predict the Tully-Fisher relation in
the B, I and for the first time, in the K band, and its evolution with
redshift, up to z sim 1. We refined the determination of the disk galaxies
rotation velocity, with a dynamical recipe for the rotation curve, rather than
a simple conversion from the total mass to maximum velocity. The new recipe
takes into account the disk shape factor, and the angular momentum transfer
occurring during secular evolution leading to the formation of bulges. This
produces model rotation velocities that are lower by sim 40-50 km/s in case of
Milky Way-like objects, up to ~50-60 km/s at the high-mass end, and up to
~20-30 km/s for the majority of the spirals, amounting to an average effect of
~20-25 %. We implemented stellar population models with a complete treatment of
the TP-AGB branch, which leads to a revision of the mass-to-light ratio in the
near-IR. Due to this effect, K band luminosities increase by sim 0.5 mags at
redshift z=0 and by ~1 mags at z=3, while in the I band at the same redshifts
the increase amounts to sim 0.3 and sim 0.5 mags. With these two new recipes
in place, the comparison between the predicted Tully-Fisher relation with a
series of datasets in the optical and near-IR, at redshifts between 0 and 1, is
used as a diagnostics of the assembly and evolution of spiral galaxies in the
model. The new model shows a net improvement over its original version of 2003.
However, the z=0 predicted Tully-Fisher is too bright in all bands, although
the model is able to reproduce the morphological differentiation observed in
the K band. At z>0.4 the match between the model and data improves
dramatically. We argue that this behavior is caused by inadequate star
formation histories in the model galaxies at low redshifts. The SFR declines
too slowly, due to continuous gas infall that is not efficiently suppressed. | | Source: | arXiv, 1006.0229 | | Services: | Forum | Review | PDF | Favorites | |
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