Galaxy formation physics behind bar formation: A view from cosmological hydrodynamical simulations

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Table 3.

Median galaxy properties at z = 0 for the different models.

Sim name	$\log_{10} (\frac{M_{crit 200}}{M_{⊙}})$ $\mathrm{log_{10}}\left(\frac{M_{\mathrm{crit200}}}{M_{\odot}}\right)$	$\log_{10} (\frac{M_{}}{M_{⊙}})$ $\mathrm{log_{10}}\left(\frac{M_{}}{M_{\odot}}\right)$	D/T ((D/T)_fit)	B/T ((B/T)_fit)	R_bulge	h_disc	$h_{z, disc}$ $h_{z, \rm disc}$	r_bar	$A_{2, \max}$ $A_{2,\rm max}$
					kpc	kpc	kpc	kpc
NW (no winds)	11.98	11.06	0.48 (0.45)	0.21 (0.55)	0.44 ^(a)	1.33	0.55	–	–
WW (weaker winds)	11.91	10.70	0.51 (0.59)	0.23 (0.35)	0.33	3.01	1.58	2.35	0.62
TNG50-like	11.95	10.72	0.74 (0.70)	0.10 (0.18)	0.64	2.98	2.01	2.45	0.50
MW (medium winds)	11.94	10.53	0.74 (0.88)	0.08 (0.11)	1.03	5.19	1.71	–	–
SW (strong winds)	11.93	10.43	0.67 (0.86)	0.09 (0.10)	1.04	4.47	2.00	–	–
NBH (no black holes)	11.94	10.62	0.72 (0.74)	0.10 (0.20)	0.55	3.41	1.66	2.70	0.57
BHlowEff	11.92	10.58	0.63 (0.78)	0.12 (0.16)	0.79	4.28	1.80	2.95	0.53

Notes.

^(a)

From left to right: Variation Model, the logarithm of halo mass, disc (thin and thick components) to total mass fraction from kinematic decomposition (from fitting the total surface density stellar profiles), bulge (classical component) to total mass fraction from kinematic decomposition (from fitting surface density stellar profiles), the effective radius from the bulge calculated from a Sersic profile, disc scale length from kinematic decomposition, disc thickness fitting the edge-on surface density with a square arc secant function in the z-direction, bar length and strength using Fourier decomposing face-on stellar surface density. The disc-scale length of galaxies in the no wind model is calculated using the stellar half-mass radius of the disc and assuming an exponential profile. We use this alternative because fitting an exponential profile of the disc stellar surface density fails due to the high density presented in the centre of these discs.

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