Cultural advice

The Australian National University acknowledges, celebrates and pays our respects to the Ngunnawal and Ngambri people of the Canberra region and to all First Nations Australians on whose traditional lands we meet and work, and whose cultures are among the oldest continuing cultures in human history.

Aboriginal and Torres Strait Islander peoples are advised that ANU Library collections may include images, names, voices, and other representations of deceased persons.

Material in the collection may contain terms, language or views that reflect the period in which the item was created and may be considered inappropriate today.

Kinematic Modeling of the Milky Way Using the RAVE and GCS Stellar Surveys

dc.contributor.authorSharma, S
dc.contributor.authorBland-Hawthorn, Joss
dc.contributor.authorBinney, J.
dc.contributor.authorFreeman, Kenneth
dc.contributor.authorSteinmetz, M.
dc.contributor.authorBoeche, C
dc.contributor.authorBienayme, O
dc.contributor.authorGibson, Bradley K
dc.contributor.authorGilmore, G
dc.contributor.authorGrebel, E.
dc.contributor.authorHelmi, Amina
dc.date.accessioned2015-12-07T22:21:48Z
dc.date.issued2014
dc.date.updated2015-12-07T09:02:24Z
dc.description.abstractWe investigate the kinematic parameters of the Milky Way disk using the Radial Velocity Experiment (RAVE) and Geneva-Copenhagen Survey (GCS) stellar surveys. We do this by fitting a kinematic model to the data and taking the selection function of the data into account. For stars in the GCS we use all phase-space coordinates, but for RAVE stars we use only (ℓ, b, v los). Using the Markov Chain Monte Carlo technique, we investigate the full posterior distributions of the parameters given the data. We investigate the age-velocity dispersion relation for the three kinematic components (σR, σφ, σz), the radial dependence of the velocity dispersions, the solar peculiar motion (U O, V O, W O), the circular speed Θ0at the Sun, and the fall of mean azimuthal motion with height above the midplane. We confirm that the Besançon-style Gaussian model accurately fits the GCS data but fails to match the details of the more spatially extended RAVE survey. In particular, the Shu distribution function (DF) handles noncircular orbits more accurately and provides a better fit to the kinematic data. The Gaussian DF not only fits the data poorly but systematically underestimates the fall of velocity dispersion with radius. The radial scale length of the velocity dispersion profile of the thick disk was found to be smaller than that of the thin disk. We find that correlations exist between a number of parameters, which highlights the importance of doing joint fits. The large size of the RAVE survey allows us to get precise values for most parameters. However, large systematic uncertainties remain, especially in V Oand Θ0. We find that, for an extended sample of stars, Θ0is underestimated by as much as 10% if the vertical dependence of the mean azimuthal motion is neglected. Using a simple model for vertical dependence of kinematics, we find that it is possible to match the Sgr A∗ proper motion without any need for V Obeing larger than that estimated locally by surveys like GCS.
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/20215
dc.publisherIOP Publishing
dc.rightsAuthor/s retain copyrighten_AU
dc.sourceAstrophysical Journal, The
dc.titleKinematic Modeling of the Milky Way Using the RAVE and GCS Stellar Surveys
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue51
local.bibliographicCitation.lastpage27
local.bibliographicCitation.startpage1
local.contributor.affiliationSharma, S, University of Sydney
local.contributor.affiliationBland-Hawthorn, Joss, University of Sydney
local.contributor.affiliationBinney, J., Rudolf Peierls Centre for Theoretical Physics
local.contributor.affiliationFreeman, Kenneth, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationSteinmetz, M., Leibniz-Institut fur Astrophysik Potsdam (AIP)
local.contributor.affiliationBoeche, C, Zentrum fur Astronomie der Universitat Heidelberg
local.contributor.affiliationBienayme, O, Observatoire de Strasbourg
local.contributor.affiliationGibson, Bradley K, University of Central Lancashire
local.contributor.affiliationGilmore, G, University of Cambridge
local.contributor.affiliationGrebel, E., Universitat Heidelberg
local.contributor.affiliationHelmi, Amina, University of Groningen
local.contributor.authoruidFreeman, Kenneth, u7000399
local.description.notesImported from ARIES
local.identifier.absfor020100 - ASTRONOMICAL AND SPACE SCIENCES
local.identifier.ariespublicationu4830877xPUB11
local.identifier.citationvolume793
local.identifier.doi10.1088/0004-637X/793/1/51
local.identifier.scopusID2-s2.0-84906957664
local.identifier.thomsonID000341301700051
local.type.statusPublished Version

Downloads

Original bundle

Now showing 1 - 1 of 1
Loading...
Thumbnail Image
Name:
01_Sharma_Kinematic_Modeling_of_the_2014.pdf
Size:
1.77 MB
Format:
Adobe Portable Document Format