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On the H i Content of MaNGA Major Merger Pairs

Published online by Cambridge University Press:  09 June 2023

Qingzheng Yu Open the ORCID record for Qingzheng Yu [Opens in a new window] ,
Taotao Fang ,
Shuai Feng ,
Bo Zhang ,
C. Kevin Xu ,
Yunting Wang  and
Lei Hao
Qingzheng Yu
Affiliation:
Department of Astronomy, Xiamen University, Xiamen, Fujian 361005, China; email: fangt@xmu.edu.
Taotao Fang
Affiliation:
Department of Astronomy, Xiamen University, Xiamen, Fujian 361005, China; email: fangt@xmu.edu.
Shuai Feng
Affiliation:
College of Physics, Hebei Normal University, 20 South Erhuan Road, Shijiazhuang, Hebei 050024, China Hebei Key Laboratory of Photophysics Research and Application, Shijiazhuang, Hebei 050024, China
Bo Zhang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences (NAOC), Beijing 100101, China
C. Kevin Xu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences (NAOC), Beijing 100101, China Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, China
Yunting Wang
Affiliation:
Department of Astronomy, Xiamen University, Xiamen, Fujian 361005, China; email: fangt@xmu.edu. Department of Physics and Astronomy, University of British Columbia, 6225 Agricultural Road, Vancouver, V6T 1Z1, Canada
Lei Hao
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China
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Abstract

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To study the role of H i content in galaxy interactions, we select galaxy pairs and control galaxies from the SDSS-IV MaNGA IFU survey, adopting kinematic asymmetry as a new effective indicator to describe the merger stage. With archival data from the HI-MaNGA survey and new observations from the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we investigate the differences in H i gas fraction (fH i), star formation rate (SFR), and H i star formation efficiency (SFEH i) between pairs and controls. Our results suggest that on average the H i gas fraction of major-merger pairs is marginally decreased by ∼ 15% relative to isolated galaxies, and paired galaxies during pericentric passage show weakly decreased fH i (−0.10 ± 0.05 dex), significantly enhanced SFR (0.42 ± 0.11 dex), and SFEH i (0.48 ± 0.12 dex). We propose the marginally detected H i depletion may originate from the gas consumption in fueling the enhanced H2 reservoir of galaxy pairs.

Keywords

Galaxy interactionsGalaxy pairsGalaxy mergersInterstellar atomic gasStar formation
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 186 - 192
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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