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The Kinematics and Dynamics of the Globular Clusters and Planetary Nebulae of NGC 5128
View access options below. You previously purchased this article through ReadCube. Institutional Login. Log in to Wiley Online Library. Purchase Instant Access. View Preview. It has a worldwide membership of around 50 comprising physicists from all sectors, as well as those with an interest in physics. It works to advance physics research, application and education; and engages with policy makers and the public to develop awareness and understanding of physics. Its publishing company, IOP Publishing, is a world leader in professional scientific communications.
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Kristin A. Woodley 1 , William E. Harris 1 , Michael A. Beasley 2 , Eric W. Peng 3 , Terry J. Bridges 4 , Duncan A.
Forbes 5 , and Gretchen L. Harris 6. The American Astronomical Society. All rights reserved. Printed in U. The Astronomical Journal , Volume , Number 2.
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Stellar kinematics - Wikipedia
Journal RSS feed. Select your desired journals and corridors below. You will need to select a minimum of one corridor. A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC is presented. From a spectroscopically confirmed sample of globular clusters and planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC There is a indication within kpc that the metal-poor clusters have a lower rotation signal than in the outer regions of the galaxy.
The rotation axis shows an interesting twist at 5 kpc, agreeing with the zero-velocity curve presented by Peng and coworkers. The planetary nebula kinematics are slightly different.
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- IACTalks: Dynamics of galaxies and globular clusters unraveled with two-dimensional kinematics.
The velocity dispersion decreases with galactocentric distance. The total mass of NGC is found using the tracer mass estimator, described by Evans et al. We find a total mass of 1. The similar kinematics of the metal-rich and metal-poor globular clusters allow us to combine the two subpopulations to determine an independent estimate of the total mass, giving 1.
Lastly, we publish a new and homogeneous catalog of known globular clusters in NGC We report the presence of a mild metallicity gradient compatible with those found in other dwarf spheroidals of the same luminosity; we trace the presence of a stellar population gradient also in the spatial distribution of stars in different evolutionary phases in ancillary SuprimeCam photometric data.
There are tentative indications of two chemo-kinematically distinct sub-populations, with the more metal-poor stars showing a hotter kinematics than the metal-richer ones.
Furthermore, the photometric dataset reveals the presence of a foreground population that most likely belongs to the Sagittarius stream. This study represents an important step forward in assessing the internal kinematics of the Cetus dwarf spheroidal galaxy as well as the first wide-area spectroscopic determination of its metallicity properties. With our analysis, Cetus adds to the growing scatter in stellar-dark matter halo properties in low-mass galactic systems.