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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731671.0, MPI für Astronomie / Publikationen_mpia
Hα Kinematics of S4G spiral galaxies - III. Inner rotation curves
Authors:Erroz-Ferrer, S.; Knapen, J. H.; Leaman, R.; Díaz-García, S.; Salo, H.; Laurikainen, E.; Querejeta, M.; Mu noz-Mateos, J. C.; Athanassoula, E.; Bosma, A.; Comerón, S.; Elmegreen, B. G.; Martínez-Valpuesta, I.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:2
Start Page:1199
End Page:1213
Audience:Not Specified
Abstract / Description:We present a detailed study of the shape of the innermost part of the rotation curves of a sample of 29 nearby spiral galaxies, based on high angular and spectral resolution kinematic Hα Fabry-Perot observations. In particular, we quantify the steepness of the rotation curve by measuring its slope dRvc(0). We explore the relationship between the inner slope and several galaxy parameters, such as stellar mass, maximum rotational velocity, central surface brightness (μ0), bar strength and bulge-to-total ratio. Even with our limited dynamical range, we find a trend for low-mass galaxies to exhibit shallower rotation curve inner slopes than high-mass galaxies, whereas steep inner slopes are found exclusively in high-mass galaxies. This trend may arise from the relationship between the total stellar mass and the mass of the bulge, which are correlated among them. We find a correlation between the inner slope of the rotation curve and the morphological T-type, complementary to the scaling relation between dRvc(0) and μ0 previously reported in the literature. Although we find that the inner slope increases with the Fourier amplitude A2 and decreases with the bar torque Qb, this may arise from the presence of the bulge implicit in both A2 and Qb. As previously noted in the literature, the more compact the mass in the central parts of a galaxy (more concretely, the presence of a bulge), the steeper the inner slopes. We conclude that the baryonic matter dominates the dynamics in the central parts of our sample galaxies.
Free Keywords:galaxies: kinematics and dynamics; galaxies: spiral
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/stw300
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