Determination of resonance locations in NGC 613 from morphological arguments

Marc Seigar, Amber Harrington, Patrick Treuthardt

Research output: Contribution to journalArticlepeer-review

2 Scopus citations

Abstract

In this paper, we present BVRI imaging data of NGC 613. We use these data to determine the corotation radius of the bar, using the photometric phase crossing method. This method uses the phase angle of the spiral structure in several wavebands, and looks for a crossing between the blue (B) light and the redder wavebands (e.g. R or I). For NGC 613, we find two phase crossings, an outer phase crossing at 136 ± 8 arcsec and an inner phase crossing at 16 ± 8 arcsec. We argue that the outer phase crossing is due to the bar corotation radius, and from the bar length of Rbar = 90.0 ± 4.0 arcsec we go on to calculate a relative bar pattern speed of R = 1.5 ± 0.1, which is consistent with the results of previous methods described in the literature. For a better understanding of the inner phase crossing, we have created structure maps in all four wavebands and a B - R colour map. All of our structure maps and our colour map highlight a nuclear ring of star formation at a radius of ~4 arcsec, which had also been observed recently using Atacama Large Millimeter Array. Furthermore, the radius of our inner phase crossing appears to be consistent with the size of a nuclear disc of star formation that has been recently detected and described in the literature. We therefore suggest that the phase crossing method can be used to detect the size of nuclear star formation regions as well as the location of corotation resonances in spiral galaxies.

Original languageEnglish (US)
Pages (from-to)5394-5400
Number of pages7
JournalMonthly Notices of the Royal Astronomical Society
Volume481
Issue number4
DOIs
StatePublished - Dec 1 2018

Bibliographical note

Funding Information:
MSS wishes to thank the University of Minnesota Duluth for their support and the Fund for Astrophysical Research. The data presented in this paper were collected as part of the Carnegie–Irvine Galaxy Survey (CGS), using facilities at Las Campanas Observatory, Carnegie Institution for Science. The optical data were reduced independently from those presented in Ho et al. (2011). The authors wish to thank the anonymous referee for comments that significantly improved the content of this paper.

Funding Information:
MSS wishes to thank the University of Minnesota Duluth for their support and the Fund for Astrophysical Research. The data presented in this paper were collected as part of the Carnegie-Irvine Galaxy Survey (CGS), using facilities at Las Campanas Observatory, Carnegie Institution for Science. The optical data were reduced independently from those presented in Ho et al. (2011). The authors wish to thank the anonymous referee for comments that significantly improved the content of this paper

Publisher Copyright:
© 2018 The Author(s).

Keywords

  • Galaxies: fundamental parameters
  • Galaxies: individual: NGC 613
  • Galaxies: kinematics and dynamics
  • Galaxies: spiral
  • Galaxies: structure

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