Volume 642, October 2020
|Number of page(s)||29|
|Section||Interstellar and circumstellar matter|
|Published online||20 October 2020|
Spectroscopic study of the HII regions in the NGC 1232 galaxy
NAT – Universidade Cidade de São Paulo/Universidade Cruzeiro do Sul,
Rua Galvão Bueno 868,
2 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, Itajubá-MG 37530-000, Brazil
Accepted: 19 August 2020
Context. NGC 1232 is a face-on spiral galaxy that serves as an excellent laboratory for the study of star formation due to its proximity. Recent studies have revealed interesting features about this galaxy: X-ray observations suggest that it recently collided with a dwarf galaxy, however, no apparent remnant is observed.
Aims. In this study, we search for evidence of this possible collision.
Methods. We used long-slit optical spectra of the galaxy in two different positions obtained with the Goodman spectrograph at the SOAR telescope.
Results. We detected 18 HII regions in the north-south direction and 22 HII regions in the east-west direction and a background galaxy, NGC 1232B, for which we present the first redshift measurement and spectral analysis. We used the stellar population fitting technique to study the underlying stellar population of NGC 1232 and NGC 1232B and to subtract it from the spectra to measure the emission lines. The emission lines were used to determine the extinction, electron density, chemical abundance, and the star-formation rate gradient of NGC 1232.
Conclusions. As is common in spiral galaxies, we found a stellar population gradient with older populations at the central regions and younger ones towards the outskirts, along with a negative oxygen abundance gradient of −0.16 dex/re. Due to the difficulty of measuring important emission lines, the number of objects for the abundance gradient is small, but there is a hint that this galaxy has a broken gradient profile, with a drop towards the center. Some authors have explained this effect as the result of a satellite collision, but observations of a large sample of spiral galaxies shows evidence that goes against such a mechanism. If the collision caused any disturbance in the galaxy, we believe it would be small and hard to detect with a limited number of objects. From all the other measurements, we found no deviations from a typical spiral galaxy and no significant difference between different directions in the galaxy. The stellar population and emission line analysis of NGC 1232B suggest that it is a starburst galaxy.
Key words: ISM: abundances / HII regions / galaxies: individual: NGC 1232 / galaxies: individual: NGC 1232B / galaxies: star formation
© ESO 2020
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