Hα Kinematics of the Isolated Interacting Galaxy Pair KPG486 (NGC6090)
ABSTRACT In optical images, the barely studied isolated interacting galaxy pair KPG486 (NGC 6090) displays similar features to the Antennae (NGC 4038/39) galaxy pair. To compare the distribution of ionized hydrogen gas, morphology and kinematic and dynamic behaviour of both galaxy pairs, we present observations in the Hα emission line of NGC6090 acquired with the scanning Fabry-Perot interferometer, PUMA. For each galaxy in NGC6090 we obtained several kinematic parameters, its velocity field and its rotation curve. We also analysed some of the perturbation induced by their encounter. We verified the consistency of our results by comparing them with kinematic results from the literature. The comparison of our results on NGC6090 with those obtained in a previous similar kinematic analysis of the Antennae highlighted great differences between these galaxy pairs.
| Main Authors: | , , |
|---|---|
| Format: | Digital revista |
| Language: | English |
| Published: |
Universidad Nacional Autónoma de México, Instituto de Astronomía
2020
|
| Online Access: | http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012020000100071 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| Summary: | ABSTRACT In optical images, the barely studied isolated interacting galaxy pair KPG486 (NGC 6090) displays similar features to the Antennae (NGC 4038/39) galaxy pair. To compare the distribution of ionized hydrogen gas, morphology and kinematic and dynamic behaviour of both galaxy pairs, we present observations in the Hα emission line of NGC6090 acquired with the scanning Fabry-Perot interferometer, PUMA. For each galaxy in NGC6090 we obtained several kinematic parameters, its velocity field and its rotation curve. We also analysed some of the perturbation induced by their encounter. We verified the consistency of our results by comparing them with kinematic results from the literature. The comparison of our results on NGC6090 with those obtained in a previous similar kinematic analysis of the Antennae highlighted great differences between these galaxy pairs. |
|---|