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Article: Kinematic modeling of the milky way using the rave and GCS stellar surveys
Title  Kinematic modeling of the milky way using the rave and GCS stellar surveys 

Authors  Sharma, SanjibBlandHawthorn, Joss BlandBinney, James J.Freeman, Kenneth C.Steinmetz, MatthiasBoeche, CorradoBienaymé, OlivierGibson, Brad K.Gilmore, Gerard F.Grebel, Eva K.Helmi, AminaKordopatis, GeorgesMunari, UlisseNavarro, Julio F.Parker, Quentin A.Reid, Warren A.Seabroke, George M.Siebert, ArnaudWatson, Fred G.Williams, Mary E KWyse, Rosemary F GZwitter, Tomaž 
Keywords  galaxies: fundamental parameters galaxies: kinematics and dynamics methods: data analysis methods: numerical methods: statistical 
Issue Date  2014 
Citation  Astrophysical Journal, 2014, v. 793, n. 1 How to Cite? 
Abstract  © 2014. The American Astronomical Society. All rights reserved.. We investigate the kinematic parameters of the Milky Way disk using the Radial Velocity Experiment (RAVE) and GenevaCopenhagen 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 phasespace 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 agevelocity 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 Besançonstyle 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. 
Persistent Identifier  http://hdl.handle.net/10722/209037 
ISSN  2015 Impact Factor: 5.909 2015 SCImago Journal Rankings: 3.266 
DC Field  Value  Language 

dc.contributor.author  Sharma, Sanjib   
dc.contributor.author  BlandHawthorn, Joss Bland   
dc.contributor.author  Binney, James J.   
dc.contributor.author  Freeman, Kenneth C.   
dc.contributor.author  Steinmetz, Matthias   
dc.contributor.author  Boeche, Corrado   
dc.contributor.author  Bienaymé, Olivier   
dc.contributor.author  Gibson, Brad K.   
dc.contributor.author  Gilmore, Gerard F.   
dc.contributor.author  Grebel, Eva K.   
dc.contributor.author  Helmi, Amina   
dc.contributor.author  Kordopatis, Georges   
dc.contributor.author  Munari, Ulisse   
dc.contributor.author  Navarro, Julio F.   
dc.contributor.author  Parker, Quentin A.   
dc.contributor.author  Reid, Warren A.   
dc.contributor.author  Seabroke, George M.   
dc.contributor.author  Siebert, Arnaud   
dc.contributor.author  Watson, Fred G.   
dc.contributor.author  Williams, Mary E K   
dc.contributor.author  Wyse, Rosemary F G   
dc.contributor.author  Zwitter, Tomaž   
dc.date.accessioned  20150323T02:31:14Z   
dc.date.available  20150323T02:31:14Z   
dc.date.issued  2014   
dc.identifier.citation  Astrophysical Journal, 2014, v. 793, n. 1   
dc.identifier.issn  0004637X   
dc.identifier.uri  http://hdl.handle.net/10722/209037   
dc.description.abstract  © 2014. The American Astronomical Society. All rights reserved.. We investigate the kinematic parameters of the Milky Way disk using the Radial Velocity Experiment (RAVE) and GenevaCopenhagen 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 phasespace 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 agevelocity 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 Besançonstyle 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.language  eng   
dc.relation.ispartof  Astrophysical Journal   
dc.subject  galaxies: fundamental parameters   
dc.subject  galaxies: kinematics and dynamics   
dc.subject  methods: data analysis   
dc.subject  methods: numerical   
dc.subject  methods: statistical   
dc.title  Kinematic modeling of the milky way using the rave and GCS stellar surveys   
dc.type  Article   
dc.description.nature  link_to_subscribed_fulltext   
dc.identifier.doi  10.1088/0004637X/793/1/51   
dc.identifier.scopus  eid_2s2.084906957664   
dc.identifier.volume  793   
dc.identifier.issue  1   
dc.identifier.eissn  15384357   