Properties of molecular gas in galaxies in early and mid stages of Interaction. III. Resolved Kennicutt–Schmidt law. (22nd February 2022)

• Record Type: Journal Article
• Authors: Kaneko, Hiroyuki; Kuno, Nario; Iono, Daisuke; Tamura, Yoichi; Tosaki, Tomoka; Nakanishi, Kouichiro; Sawada, Tsuyoshi
• Is Part Of: Publications of the Astronomical Society of Japan. Volume 74:Number 2(2022)
• Page Start: 343
• Page End: 363
• Publication Date: 2022-02-22
• Subjects: galaxies: individual (Arp 84, VV 219, VV 254, the Antennae galaxies) -- galaxies: interactions -- galaxies: ISM -- ISM: molecules; Astronomy -- Periodicals; 520.5
• DOI: 10.1093/pasj/psab129
• Languages: English
• ISSNs: 0004-6264

Abstract

Abstract: We study properties of the interstellar medium, an ingredient of stars, and star formation activity, in four nearby galaxy pairs in the early and mid stages of interaction for both a galaxy scale and a kpc scale. The galaxy-scale Kennicutt–Schmidt law shows that seven of eight interacting galaxies have a star formation rate within a factor of three compared with the best fit of the isolated galaxies, although we have shown that molecular hydrogen gas is efficiently produced from atomic hydrogen during the interaction in the previous paper (Kaneko et al. 2017 PASJ, 69, 66). The galaxy-scale specific star formation rate (sSFR) and star formation efficiency (SFE) in interacting galaxies are comparable to those in isolated galaxies. We also investigate SFE and the Kennicutt–Schmidt law on a kpc scale. The spatial distributions of SFE reveal that SFE is locally enhanced, and the enhanced regions take place asymmetrically or at off-centre regions. The local enhancement of SFE could be induced by shock. We find that the index of the Kennicutt–Schmidt law for the interacting galaxies in the early stage is 1.30 ± 0.04, which is consistent with that of the isolated galaxies. Since CO emission, which is used in the Kennicutt–Schmidt law, is a tracer of the amount of molecular gas, this fact suggests that dense gas, which is more directly connected to star formation, is not changed at the early stage of interaction.