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Table 4

Kinematic classification.

Objects Velocity υrot υobs,limσint υobs,limσ0,lim Peak ΔPAd < 30° No Class Final
gradienta achievedb > 0.4 > 1 of σc int.e FSf classg
AS1063-1816 X 3 3
AS1063-658 X X X X 1 2
AS1063-1611 X 3 3
AS1063-1670 X X X X X X 1 1
AS1063-1152 X X X X X 1 1
AS1063-1321 X X X X X X X 1 1
AS1063-1331 X 3 3
AS1063-732 X X X X 1 1
AS1063-1904 X X 2 2
AS1063-606_1 X X X 2 2
AS1063-942 X X X X 1 2
AS1063-885 X 4 4
AS1063-1720 X X 2 2
MACS1206-2005 X X X X X 1 1
MACS1206-1123 X 3 3
MACS1206-1409 X 4 4
MACS1206-1235 X 3 3
MACS1206-445 X 4 4
MACS1206-415 X 3 3
MACS1206-1622 X 3 3
MACS1206-2372 X 3 3
MACS1206-1616_1 X X X X 1 1
MACS1206-1472 X X X X 1 2
MACS1206-820 3 3

Notes. The cross (X) indicates that the criterion is satisfied. (a) A velocity gradient is visible in the velocity map of the galaxy. (b) υrot achieved when a flat part is visible in the rotation curve of the observed velocity. (c) A peak in the dispersion is observed in the dispersion map at the center of the galaxy. (d)   Δ PA is defined as |PAkin −PAmorph|. (e) The galaxiesclassified as no interaction (no int.) do not show any evidence of disturbance in their velocity dispersion map obtained from Hα or [OIII] emission lines. A disturbance could be the signature of a system in an on-going merger. (f) Criteria established by Förster Schreiber et al. (2009): galaxies with υobs,limσint > 0.4 are defined as rotation dominated (1) and with υobs,limσint < 0.4 as dispersion dominated (2). Galaxies classified as (3) do not show any evidence of a velocity gradient. Unresolved galaxies are classified as (4). (g) The ratio υobs,limσ0,lim is the criterion we use in this work. Galaxies with υobs,limσ0,lim > 1 are classified as rotation dominated (1) if they also show no sign of interactions in their dispersion map (no int.), otherwise they are classified as irregular (2). The galaxies classified as (3) do not show any evidence of a velocity gradient. Unresolved galaxies are classified as (4).

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