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Measuring mass
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Text
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Title
Measuring mass
SubTitle
non-circular motions of gas in disk galaxies and radial velocities of stars in a global cluster
TitleInfo
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Title
Non-circular motions of gas in disk galaxies and radial velocities of stars in a global cluster
Identifier
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ETD_2115
Identifier
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http://hdl.rutgers.edu/1782.2/rucore10001600001.ETD.000051901
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eng
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theses
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Topic
Physics and Astronomy
Subject
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(authority = ETD-LCSH)
Topic
Disks (Astrophysics)
Subject
(ID = SBJ-3);
(authority = ETD-LCSH)
Topic
Galaxies
Subject
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(authority = ETD-LCSH)
Topic
Stars--Global clusters
Abstract
This thesis is concerned with the motions of gas in disk galaxies and with the motions of stars in a globular cluster to learn about their mass content.
First we study non-circular streaming motions of HI gas in five representative disk galaxies with a bisymmetric model. We show that this physically motivated method can represent a wide range of bar-like distortions and that its model parameters can be related to useful physical parameters of galaxies like the amplitude of the forced non-circular speed, the bar angle, and the halo ellipticity.
We also model the non-circular gas flow in the strongly barred galaxy NGC~1365. The gravitational potential is based on new observations that include photometric imaging, Fabry-Perot emission line imaging spectroscopy and a detailed re-analysis of archival HI data from the VLA. We use our 2-dimensional velocity map to constrain the strength and positions of the shocks in hydrodynamical simulations and find that better agreement is found with a massive, but not fully maximal disk $(m{M/L}simeq 2.0pm 1.0)$ and a fast bar (corotation at 1.2$m{R_{bar}}$). The analysis was complicated by the discovery of an asymmetric distribution of dust and kinematics in the bar region despite the remarkably bisymmetric distribution of the I-band light.
We have measured 543 radial velocities of stars in the direction of the Galactic globular cluster M80 with Fabry-Perot absorption-line imaging spectroscopy. The data is used to derive the total mean velocity of $7.39 pm 0.54$ kms, the total velocity dispersion of $10.1 pm 0.4$ kms, a declining dispersion profile, and the rotation of the cluster. M80 is rotating with an amplitude of $2.42 pm 0.81$ kms along an axis with a position angle of $246.1degr pm 17.1$ (measured from North through East), which is perpendicular to the major axis of the cluster flattening. We have fitted single- and multi-mass Michie-King models to our velocity data and to surface-brightness profiles taken from the literature.
Only when we increase the expected present-day number of white dwarfs are we able to match the expected $M/L_V$ of the stellar population with the
dynamically-derived value of $3.0pm0.3$. We tentatively interpret this as evidence of tidal stripping given that M80 is on an orbit that keeps it in the inner regions of the Galaxy and therefore has probably experienced significant tidal mass loss.
First we study non-circular streaming motions of HI gas in five representative disk galaxies with a bisymmetric model. We show that this physically motivated method can represent a wide range of bar-like distortions and that its model parameters can be related to useful physical parameters of galaxies like the amplitude of the forced non-circular speed, the bar angle, and the halo ellipticity.
We also model the non-circular gas flow in the strongly barred galaxy NGC~1365. The gravitational potential is based on new observations that include photometric imaging, Fabry-Perot emission line imaging spectroscopy and a detailed re-analysis of archival HI data from the VLA. We use our 2-dimensional velocity map to constrain the strength and positions of the shocks in hydrodynamical simulations and find that better agreement is found with a massive, but not fully maximal disk $(m{M/L}simeq 2.0pm 1.0)$ and a fast bar (corotation at 1.2$m{R_{bar}}$). The analysis was complicated by the discovery of an asymmetric distribution of dust and kinematics in the bar region despite the remarkably bisymmetric distribution of the I-band light.
We have measured 543 radial velocities of stars in the direction of the Galactic globular cluster M80 with Fabry-Perot absorption-line imaging spectroscopy. The data is used to derive the total mean velocity of $7.39 pm 0.54$ kms, the total velocity dispersion of $10.1 pm 0.4$ kms, a declining dispersion profile, and the rotation of the cluster. M80 is rotating with an amplitude of $2.42 pm 0.81$ kms along an axis with a position angle of $246.1degr pm 17.1$ (measured from North through East), which is perpendicular to the major axis of the cluster flattening. We have fitted single- and multi-mass Michie-King models to our velocity data and to surface-brightness profiles taken from the literature.
Only when we increase the expected present-day number of white dwarfs are we able to match the expected $M/L_V$ of the stellar population with the
dynamically-derived value of $3.0pm0.3$. We tentatively interpret this as evidence of tidal stripping given that M80 is on an orbit that keeps it in the inner regions of the Galaxy and therefore has probably experienced significant tidal mass loss.
PhysicalDescription
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electronic resource
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xv, 127 p. : ill.
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application/pdf
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Note
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Ph.D.
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Includes bibliographical references
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by Ricardo Zánmar Sánchez
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Sánchez
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Ricardo Zánmar
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1978-
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Ricardo Zánmar Sánchez
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Sellwood
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Jerry
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Jerry Sellwood
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Zamick
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Larry
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Larry Zamick
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Keeton
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Charles
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Charles R Keeton
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Hughes
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John
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John P Hughes
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Spekkens
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Kristine
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Kristine Spekkens
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Rutgers University
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Graduate School - New Brunswick
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2009
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2009-10
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xx
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Rutgers University Electronic Theses and Dissertations
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ETD
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Graduate School - New Brunswick Electronic Theses and Dissertations
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rucore19991600001
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doi:10.7282/T300028H
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ETD doctoral
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Rights
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The author owns the copyright to this work
Copyright
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Copyright protected
Notice
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Open
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Sánchez
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Ricardo
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Ricardo Sánchez
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Rutgers University. Graduate School - New Brunswick
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Author Agreement License
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I hereby grant to the Rutgers University Libraries and to my school the non-exclusive right to archive, reproduce and distribute my thesis or dissertation, in whole or in part, and/or my abstract, in whole or in part, in and from an electronic format, subject to the release date subsequently stipulated in this submittal form and approved by my school. I represent and stipulate that the thesis or dissertation and its abstract are my original work, that they do not infringe or violate any rights of others, and that I make these grants as the sole owner of the rights to my thesis or dissertation and its abstract. I represent that I have obtained written permissions, when necessary, from the owner(s) of each third party copyrighted matter to be included in my thesis or dissertation and will supply copies of such upon request by my school. I acknowledge that RU ETD and my school will not distribute my thesis or dissertation or its abstract if, in their reasonable judgment, they believe all such rights have not been secured. I acknowledge that I retain ownership rights to the copyright of my work. I also retain the right to use all or part of this thesis or dissertation in future works, such as articles or books.
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