NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-19 T17:32:32 PDT
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For refcode 2016MNRAS.458.1199E:
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Copyright by Royal Astronomical Society. 2016MNRAS.458.1199E Halpha kinematics of S^4^G spiral galaxies - III. Inner rotation curves Erroz-Ferrer, Santiago; Knapen, Johan H.; Leaman, Ryan; Diaz-Garcia, Simon; Salo, Heikki; Laurikainen, Eija; Querejeta, Miguel; Munoz-Mateos, Juan Carlos; Athanassoula, E.; Bosma, Albert; Comeron, Sebastien; Elmegreen, Bruce G.; Martinez-Valpuesta, Inma Abstract. 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 Halpha Fabry-Perot observations. In particular, we quantify the steepness of the rotation curve by measuring its slope d_R_v_c_(0). We explore the relationship between the inner slope and several galaxy parameters, such as stellar mass, maximum rotational velocity, central surface brightness (mu_0_), 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 d_R_v_c_(0) and mu_0_ previously reported in the literature. Although we find that the inner slope increases with the Fourier amplitude A_2_ and decreases with the bar torque Q_b_, this may arise from the presence of the bulge implicit in both A_2_ and Q_b_. 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. Key words: galaxies: kinematics and dynamics, galaxies: spiral
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