Histograms of the specific AM, l (in units of 100 kpc km s^-1), and the radial (v_r) and tangential (v_t) velocities (in units of 100 km s^-1) of stars between radii of 2–3 R_d in a number of minor merger remnants. The top three rows show direct minor mergers, with disk gas mass fractions increasing from 0 to 0.2. Indicated in each panel are the entire old stellar population (gray), new stars (blue) and old stars with |z|    ≤ 1 kpc (red). The vertical dashed lines show the average values of l, v_r and v_t for each of these three components. The three lowest rows are similar, but for retrograde mergers.

Same as Fig. 9, but for two consecutive minor mergers.

Same as Fig. 9, but for galaxies that were evolved in isolation for 3 Gyr: a gSa (upper panels) with a gas mass fraction f_gas = 0.1 and a gSb (middle panels) with f_gas = 0.2, as well as a galaxy with a much higher gas fraction of 0.5 which went through an unstable clumpy phase (bottom panels). In the latter case the parameters are also shown after 3 Gyr, when the clumps have dissolved through tidal effects or spiraled into the galaxy center through dynamical friction and interaction.

Distribution of tangential velocities v_t (in units of 100 km s^-1) of old stars for six minor mergers. For each encounter a pair of panels is shown, with stars originally in the primary disk (left) and those accreted from the satellite (right). In each panel the histograms correspond to different heights above and below the galaxy midplane: |z|    ≤ 1 kpc (black), 1    <    |z|    ≤    3 kpc (blue), 3    <    |z|    ≤    5 kpc (green) and 5    <    |z|    ≤    10 kpc (orange). The average values of v_t in the different regions is also indicated.

Same as Fig. 12 but for an isolated, very gas-rich galaxy (f_gas = 0.5), after an unstable, clumpy phase. Note that in this case the fourth and highest region is missing, due to a lack of stars above/below 5 kpc from the galaxy midplane.

Specific AM, l, as a function of scaled radius for old stars in three direct merger remnants. For each encounter a pair of plots is shown, where stars are selected on their heights above (or below) the galaxy midplane: |z|    ≤ 1 kpc (upper panels) and |z|    > 1 kpc (lower panels). In each panel stars originally in the primary galaxy are shown as black points, stars originally in the satellite as blue points, and satellite stars with |z|    > 5 kpc as red points. The specific AM is in units of 100 kpc km s^-1.

Same as Fig. 14, but for three retrograde mergers.

Fraction of counter-rotating stars (shown in blue) for four dissipationless retrograde mergers. Stars are divided into four regions, according to their height above (or below) the galaxy midplane: (1) at |z|    ≤    1 kpc; (2) at 1 kpc  ≤    |z|    ≤ 3 kpc; (3) at 3 kpc  ≤    |z|    ≤ 5 kpc; and (4) at 5 kpc ≤ |z|    ≤ 10 kpc. For each region the fraction of satellite stars to the total number of stars is also shown (gray).

Same as Fig. 16, but for four dissipative retrograde mergers.

Same as Fig. 16, but for a gS0 galaxy after a single retrograde merger (left panel) and after two consecutive retrograde mergers (right panel) with a dE0 satellite.