EDP Sciences
Free Access
Issue
A&A
Volume 582, October 2015
Article Number A21
Number of page(s) 50
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201424935
Published online 30 September 2015

Online material

Appendix A: Table of kinematic properties

Table A.1

Morphological parameters of the sample of interacting CALIFA galaxies used in this study.

Table A.2

Stellar kinematic properties of the interacting sample selected for this study included in the CALIFA survey.

Table A.3

Ionized gas kinematic properties of the interacting sample selected for this study included in the CALIFA survey.

Table A.4

Kinematic (mis)alignment between the stellar and the ionised gas components for the galaxies included in this study.

Appendix B: Velocity fields

In this appendix we present the stellar and ionized gas kinematic maps of the sample used in this study. We group from Figs. B.1 to B.4 the galaxies in the different interaction stages described in Sect. 2.1. For each interacting galaxy (system) we show from left to right: SDSS r-band image. For post-merger and merger remnants we enhance the contrast of the images to highlight their morphological features. The white hexagon represents the area covered by the CALIFA FoV. The white line in the bottom left corner represents a 10 kpc scale. In systems where both objects are observed, two hexagons are plotted. The next panel shows the SDSS r-band image at the same area for which the kinematic velocity distributions has been observed. The white line represents the morphological PA. The next two

panels show the stellar and the ionized gas velocity fields. The green dots in each of these panels represent the position of maximum velocity for that galactocentric distance. The black lines represent the mean kinematic PA derived from these points (see details in Sect. 2.5). The last panel shows the velocity curve derived directly from the velocity field (see details in Sect. 2.5); the blue and red curves represent the stellar and the ionized gas components, respectively. The thickness of the lines represents the uncertainty in the determination of the maximum velocity for each galactocentric distance by means of Monte Carlo simulations (see details in Sect. 2.5). For galaxies where the kinematic PA was not possible to determine in a given component, neither the velocity curves nor the positions are plotted in the velocity fields.

thumbnail Fig. B.1

Objects in the pre-merger stage. Top: UGC 312 and UGC 312NOTES01. Middle: NGC 192 and NGC 197. Bottom: NGC 444.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: NGC 477 and CGCG536-030. Middle: NGC 499 and NGC 495. Bottom: NGC 2449.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 432. Middle: IC 2247. Bottom: IC 540.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: NGC 4003. Middle: UGC 7012. Bottom: IC 944.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: NGC 5378. Middle: NGC 5682. Bottom: NGC 5730 and NGC 5731.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 9476. Middle: NGC 5797 and NGC 5794. Bottom: IC 1079 and IC 1078.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 9873. Middle: NGC 5957. Bottom: NGC 5966.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: IC 4566, Middle: NGC 6021, Bottom: NGC 6146.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 10650. Middle: NGC 6278. Bottom: NGC 6314.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 10796. Middle: NGC 6427. Bottom: NGC 6978 and NGC 6977.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: UGC 11717. Middle: NGC 7562 Bottom: UGC 12494.

Open with DEXTER

thumbnail Fig. B.1

continued. Top: NGC 7608. Middle: NGC 7653. Bottom: NGC 7671.

Open with DEXTER

thumbnail Fig. B.1

continued. Top panel: UGC 5498NED01. Middle: UGC 9711. Bottom: UGC 10331.

Open with DEXTER

thumbnail Fig. B.1

continued. VV488NED02.

Open with DEXTER

thumbnail Fig. B.2

Pairs of Galaxies with signatures of interactions. Top: pair UGC 335NED02 and NED01. Middle: pair of galaxies NGC 169 and NGC 169A. Bottom: UGC 3995.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: pair NGC 3303 and NGC 3303NED01. Middle: NGC 3406NED01 and NGC 3406NED02. Bottom: companion NGC 3991.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: NGC 4211NED02 and NGC 4211NED01. Middle: NGC 4676A and NGC 4676B. Bottom: NGC 5216 and NGC 5218.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: NGC 5394. Middle: NGC 5614. Bottom: NGC 5930 and NGC 5929.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: NGC 5934 and NGC 5935. Middle: NGC 5953 and NGC 5954. Bottom: UGC 10695.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: NGC 7236 and UGC 11958. Middle: UGC 11680 NED01 and NED02. Bottom: NGC 7549 and NGC 7550.

Open with DEXTER

thumbnail Fig. B.2

continued. Top: UGC 12688. Middle: NGC 7783NED01. Bottom: NGC 4841 A and NGC 4841 B.

Open with DEXTER

thumbnail Fig. B.3

Post-merger galaxies. Top: NGC 2623. Middle: UGC 8107. Bottom: Arp 220.

Open with DEXTER

thumbnail Fig. B.3

continued. Post-merger galaxies. Top: UGC 10205. Middle: NGC 7025. Bottom: NGC 7625.

Open with DEXTER

thumbnail Fig. B.3

continued. Top: NGC 7722. Bottom: UGC 12864.

Open with DEXTER

thumbnail Fig. B.4

Late merger remnants galaxies. Top: NGC 1167. Middle: NGC 1349. Bottom: NGC 3106.

Open with DEXTER

thumbnail Fig. B.4

continued. Late merger remnants galaxies. Top: NGC 5623. Middle: NGC 5739. Bottom: NGC 5784.

Open with DEXTER

thumbnail Fig. B.4

continued. Late merger remnants galaxies. Top: NGC 6154. Middle: UGC 10905. Bottom: NGC 7711.

Open with DEXTER

thumbnail Fig. B.4

continued. NGC 7738.

Open with DEXTER


© ESO, 2015

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.