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Differences in star formation activity between tidally triggered and isolated bars : a case study of NGC 4303 and NGC 3627

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Mon. Not. Roy. Astron. Soc.510-3_3899–3916.pdf11.49 MBPDFView/Open
Please use this identifier to cite or link to this item:http://hdl.handle.net/2115/84582

Title: Differences in star formation activity between tidally triggered and isolated bars : a case study of NGC 4303 and NGC 3627
Authors: Iles, Elizabeth J. Browse this author
Pettitt, Alex R. Browse this author
Okamoto, Takashi Browse this author →KAKEN DB
Keywords: methods: numerical
stars: formation
ISM: structure
galaxies: interactions
galaxies: kinematics and dynamics
Issue Date: Mar-2022
Publisher: Oxford University Press
Journal Title: Monthly notices of the royal astronomical society
Volume: 510
Issue: 3
Start Page: 3899
End Page: 3916
Publisher DOI: 10.1093/mnras/stab3330
Abstract: Galactic bars are important drivers of galactic evolution, and yet how they impact the interstellar medium and correspondingly star formation, remains unclear. We present simulation results for two barred galaxies with different formation mechanisms, bars formed in isolation or via a tidal interaction, to consider the spatially and temporally varying trends of star formation. We focus on the early (<1 Gyr) epoch of bar formation so that the interaction is clearly identifiable. The nearby NGC 4303 (isolated) and NGC 3627 (interaction history) are selected as observational analogues to tailor these simulations. Regardless of formation mechanism, both models show similar internal dynamical features, although the interaction appears to promote bar-arm disconnection in the outer disc velocity structure. Both bars trigger similar boosts in star formation (79 per cent; 66 per cent), while the interaction also triggers an earlier 31 per cent burst. Significant morphological dependence is observed in the relation between surface gas and star formation rate. In both cases, the bar component is notably steepest; the arm is similar to the overall disc average; and the interarm clearly the shallowest. A distinguishable feature of the tidal disc is the presence of moderately dense, inefficiently star-forming gas mostly confined to tidal debris outside the optical disc. The tidal disc also exhibits a unique trend of radially increasing star formation efficiency and a clear dearth of star formation which persists along the bar between the centre and bar ends. These are potential signatures for identifying a barred system post-interaction.
Rights: This article has been accepted for publication in Monthly notices of the royal astronomical society ©: 2021 Elizabeth J Iles, Alex R Pettitt, Takashi Okamoto Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved.
Type: article
URI: http://hdl.handle.net/2115/84582
Appears in Collections:理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)

Submitter: 岡本 崇

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