NGC 1300 dynamics – II. The response models

We study the stellar response in a spectrum of potentials describing the barred spiral galaxy NGC 1300. These potentials have been presented in a previous paper and correspond to three different assumptions as regards the geometry of the galaxy. For each potential we consider a wide range of Ωp patt...

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Bibliographic Details
Published inMonthly notices of the Royal Astronomical Society Vol. 408; no. 1; pp. 9 - 21
Main Authors Kalapotharakos, C., Patsis, P. A., Grosbøl, P.
Format Journal Article
LanguageEnglish
Published Oxford, UK Blackwell Publishing Ltd 11.10.2010
Wiley-Blackwell
Subjects
Astronomy
Earth, ocean, space
Exact sciences and technology
galaxies: kinematics and dynamics
galaxies: spiral
galaxies: structure
ISM: kinematics and dynamics
galaxies: structure
galaxies: kinematics and dynamics
galaxies: spiral
ISM: kinematics and dynamics
Barred spiral galaxies
Galaxy structure
Dynamics
Kinematics
Models
Spiral galaxies
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Summary:We study the stellar response in a spectrum of potentials describing the barred spiral galaxy NGC 1300. These potentials have been presented in a previous paper and correspond to three different assumptions as regards the geometry of the galaxy. For each potential we consider a wide range of Ωp pattern speed values. Our goal is to discover the geometries and the Ωp supporting specific morphological features of NGC 1300. For this purpose we use the method of response models. In order to compare the images of NGC 1300 with the density maps of our models, we define a new index which is a generalization of the Hausdorff distance. This index helps us to find out quantitatively which cases reproduce specific features of NGC 1300 in an objective way. Furthermore, we construct alternative models following a Schwarzschild-type technique. By this method we vary the weights of the various energy levels, and thus the orbital contribution of each energy, in order to minimize the differences between the response density and that deduced from the surface density of the galaxy, under certain assumptions. We find that the models corresponding to Ωp≈ 16 and 22 km s−1 kpc−1 are able to reproduce efficiently certain morphological features of NGC 1300, with each one having its advantages and drawbacks.
Bibliography:Based on observations collected at the European Southern Observatory, Chile: programme ESO 69.A-0021.
istex:20F36B10E2CEA4153184A60194CF4AA8B6CF8766
ark:/67375/HXZ-Z8PLCN55-J
Based on observations collected at the European Southern Observatory, Chile: programme ESO 69.A‐0021.
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2010.17061.x