2016
DOI: 10.1093/mnras/stw2113
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Abstract: We present a disc-halo N-body model of the low surface brightness galaxy UGC 628, one of the few systems that harbours a "slow" bar with a ratio of corotation radius to bar length of R ≡ R c /a b ∼ 2. We select our initial conditions using SDSS DR10 photometry, a physically motivated radially variable mass-to-light ratio profile, and rotation curve data from the literature. A global bar instability grows in our submaximal disc model, and the disc morphology and dynamics agree broadly with the photometry and ki… Show more

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Cited by 6 publications
(13 citation statements)
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“…Our bar strength values found for UGC 628, 0.26 and 0.22, are roughly consistent with those found by Chequers et al (2016) at late simulation time, ∼0.30, although our values are somewhat weaker. Based on the behaviour of the relative Fourier amplitudes, our bar strengths are likely indicative of the true strength.…”
Section: Bar Strengthssupporting
confidence: 92%
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“…Our bar strength values found for UGC 628, 0.26 and 0.22, are roughly consistent with those found by Chequers et al (2016) at late simulation time, ∼0.30, although our values are somewhat weaker. Based on the behaviour of the relative Fourier amplitudes, our bar strengths are likely indicative of the true strength.…”
Section: Bar Strengthssupporting
confidence: 92%
“…Finally, we also have selected UGC 628, which has had its bar pattern speed measured via Fabry-Perot kinematics (Chemin & Hernandez 2009) and numerical modeling (Chequers et al 2016).…”
Section: Samplementioning
confidence: 99%
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“…Miwa & Noguchi (1998). However, slow bars can be created spontaneously if the disk is dark matter dominated and there is little or no gas (Debattista & Sellwood 2000;Saha & Naab 2013;Athanassoula 2014;Lokas et al 2016;Chequers et al 2016;Pettitt & Wadsley 2018). Our dwarfs were also dominated by dark matter.…”
Section: Discussionmentioning
confidence: 83%