Identifying the progenitor set of present-day early-type galaxies: a view from the standard model

S. Kaviraj; J. E. G. Devriendt; I. Ferreras; S. K. Yi; J. Silk

doi:10.1051/0004-6361/200810483

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Volume 503 / No 2 (August IV 2009)

A&A, 503 2 (2009) 445-458

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Table 1:

Free parameters that affect the evolution of the baryonic Universe, see Sect. 2.3 for more details.
Parameter	Description	Fiducial value	Source of constraints
$\beta$	Inverse of star formation efficiency	50	Kennicutt (1998)
$\epsilon$	Inverse of mass loading for feedback	0.1	Martin et al. (2002)
$\chi$	Galaxy merger power law	3.333	Numerical simulations e.g. Walker et al. (1996)
$\Omega_B$	Baryon fraction	0.02 h^-2	²H abundance in QSO absorption lines (Tytler et al. 1996)
$\psi$	S-S merging normalisation	0.017	Makino & Hut (1997)
$\varsigma$	Recycling efficiency	0.3	Set to fiducial value in Hatton et al. (2003)
$\kappa$	Ratio of burst-to-bulge radius	0.1	Set to fiducial value in Hatton et al. (2003)
Dust	ISM Extinction and emission due to dust	-	Guiderdoni et al. (1987), Desert et al. (1990)
IMF	Initial mass function	-	Kennicutt (1983)

Source LaTeX | All tables | In the text

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