Veltz, L.; Bienaymé, O.; Freeman, K. C.; Binney, J.; Bland-Hawthorn, J.; Gibson, B. K.; Gilmore, G.; Grebel, G. K.; Helmi, A.; Munari, U.; Navarro, J. F.; Parker, Q. A.; Seabroke, G. M.; Siebert, A.; Steinmetz, M.; Watson, F. G.; Williams, M.; Wyse, R. F. G. and Zwitter, T.
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|DOI (Digital Object Identifier) Link:||https://doi.org/10.1051/0004-6361:20066948|
|Google Scholar:||Look up in Google Scholar|
We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics.
We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.
|Item Type:||Journal Article|
|Copyright Holders:||2008 ESO|
|Keywords:||stellar kinematics; disk galaxies; galactic fundamental parameters; galactic kinematics and dynamics; galactic structure|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||George Seabroke|
|Date Deposited:||29 Jan 2009 08:50|
|Last Modified:||06 Oct 2016 09:18|
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