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The observability of galaxy merger signatures in nearby gas-rich spirals

McElroy, Rebecca and Bottrell, Connor and Hani, Maan H. and Moreno, Jorge and Croom, Scott M. and Hayward, Christopher C. and Twum, Angela and Feldmann, Robert and Hopkins, Philip F. and Hernquist, Lars and Husemann, Bernd (2022) The observability of galaxy merger signatures in nearby gas-rich spirals. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20220818-003825154

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Abstract

Galaxy mergers are crucial to understanding galaxy evolution, therefore we must determine their observational signatures to select them from large IFU galaxy samples such as MUSE and SAMI. We employ 24 high-resolution idealised hydrodynamical galaxy merger simulations based on the "Feedback In Realistic Environment" (FIRE-2) model to determine the observability of mergers to various configurations and stages using synthetic images and velocity maps. Our mergers cover a range of orbital configurations at fixed 1:2.5 stellar mass ratio for two gas rich spirals at low redshift. Morphological and kinematic asymmetries are computed for synthetic images and velocity maps spanning each interaction. We divide the interaction sequence into three: (1) the pair phase; (2) the merging phase; and (3) the post-coalescence phase. We correctly identify mergers between first pericentre passage and 500 Myr after coalescence using kinematic asymmetry with 66% completeness, depending upon merger phase and the field-of-view of the observation. We detect fewer mergers in the pair phase (40%) and many more in the merging and post-coalescence phases (97%). We find that merger detectability decreases with field-of-view, except in retrograde mergers, where centrally concentrated asymmetric kinematic features enhances their detectability. Using a cut-off derived from a combination of photometric and kinematic asymmetry, we increase these detections to 89% overall, 79% in pairs, and close to 100% in the merging and post-coalescent phases. By using this combined asymmetry cut-off we mitigate some of the effects caused by smaller fields-of-view subtended by massively multiplexed integral field spectroscopy programmes.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/2206.07545arXivDiscussion Paper
https://resolver.caltech.edu/CaltechAUTHORS:20220825-833695900Related ItemJournal Article
ORCID:
AuthorORCID
McElroy, Rebecca0000-0003-2290-7060
Bottrell, Connor0000-0003-4758-4501
Hani, Maan H.0000-0002-5351-2291
Moreno, Jorge0000-0002-3430-3232
Croom, Scott M.0000-0003-2880-9197
Hayward, Christopher C.0000-0003-4073-3236
Feldmann, Robert0000-0002-1109-1919
Hopkins, Philip F.0000-0003-3729-1684
Hernquist, Lars0000-0001-6950-1629
Husemann, Bernd0000-0003-2901-6842
Additional Information:RM acknowledges and pays respect to the Gadigal people of the Eora Nation, upon whose unceded, sovereign, ancestral lands the University of Sydney is built; and the traditional owners of the land on which the University of Queensland is situated, the Turrbal and Jagera people. We pay respects to their Ancestors and descendants, who continue cultural and spiritual connections to Country. RM and SC acknowledge the support of the Australian Research Council [Grant ID: DP190102714]. RM also acknowledges the support of a UQ Postdoctoral Fellowship. The computations in this paper were partly run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. CB acknowledges support from the Natural Science and Engineering Council of Canada (NSERC) [funding reference number PDF-546234-2020]. MHH gratefully acknowledges support from the William and Caroline Herschel Postdoctoral Fellowship fund. Support for JM is provided by the NSF (AST Award Number 1516374), and by the Harvard Institute for Theory and Computation, through their Visiting Scholars Program. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. Support for JM is provided by the NSF (AST Award Number 1516374), the Grace Steele Foundation, and Downing College. RF acknowledges financial support from the Swiss National Science Foundation (grant no 194814). BH greatly appreciates financial support from the DFG via grant GE625/17-1. CCH acknowledges that the Flatiron Institute is supported by the Simons Foundation. DATA AVAILABILITY. The data underlying this article will be shared on reasonable request to the corresponding author.
Funders:
Funding AgencyGrant Number
Australian Research CouncilDP190102714
University of QueenslandUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)PDF-546234-2020
William and Caroline Herschel Postdoctoral FellowshipUNSPECIFIED
NSFAST-1516374
Harvard UniversityUNSPECIFIED
Grace C. Steele FoundationUNSPECIFIED
Downing CollegeUNSPECIFIED
Swiss National Science Foundation (SNSF)194814
Deutsche Forschungsgemeinschaft (DFG)GE625/17-1
Simons FoundationUNSPECIFIED
Subject Keywords:galaxies:formation – galaxies:evolution – galaxies: interactions – galaxies: kinematics and dynamics
Record Number:CaltechAUTHORS:20220818-003825154
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220818-003825154
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116357
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:18 Aug 2022 23:04
Last Modified:29 Aug 2022 22:45

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