Astronomy & Astrophysics

All Tables

Table 1: Bulge, disk, and halo parameters used in numerical simulations. The halo mass that is accounted for is the mass of dark matter inside the disk radius.
Table 2: Parameters for the simulations of distant interactions of galaxies. M is the mass ratio (1:2 means that the companion is smaller than the target galaxy, 2:1 that it is more massive). T is the Hubble Type (see Table 1). The orientation of the orbit can be direct (D) or retrograde (R). We also give the relative velocity at an infinite distance V, the impact parameter r, and the inclination of the orbital plane with respect to the galactic plane $\theta$ .
Table 3: Parameters for the simulations of minor mergers. M is the mass ratio. T is the Hubble Type, determining several bulge/halo parameters (see Table 1 for details). The orientation of the orbit can be direct (D) or retrograde (R). We also give the relative velocity at an infinite distance V, the impact parameter r, and the inclination of the orbital plane on the galactic plane $\theta$ . The last column indicates the value of $\langle A_1\rangle$ when the stars of the companion are azimuthally mixed in the galaxy (i.e. when the value of $\langle A_1\rangle$ is unchanged when we include these stars or not, at the instant called t₀ in Fig. 12). Before that, the lopsidedness can be stronger, but the system appears like an ongoing merger, not like an isolated galaxy, as explained in text and shown in Figs. 12 and 13. The value indicated here corresponds to the instant at which the galaxy begins to appear "isolated''.
Table 4: Parameters for simulations of accretion: initial Hubble type of the galaxy, accretion rate (in $M_{\odot }$ yr^-1), and spatial offset of the filament with respect to the disk center. The last column indicates the average value of $\langle A_1\rangle$ between t=2 and t=4 Gyrs.
Table A.1: Inclination and values of $\langle A_1\rangle$ and $\langle A_2\rangle$ for galaxies in our sample.