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Kinematics of our Galaxy from the PMA and TGAS catalogues

Published online by Cambridge University Press:  07 March 2018

Anna B. Velichko ,
Volodymyr S. Akhmetov  and
Peter N. Fedorov
Anna B. Velichko
Affiliation:
Institute of Astronomy, V. N. Karazin Kharkiv National University, 61022, 35 Sumska str., Kharkiv, Ukraine email: Velichko.Anna.B@gmail.com, akhmetovvs@gmail.com, pnfedorov@gmail.com
Volodymyr S. Akhmetov
Affiliation:
Institute of Astronomy, V. N. Karazin Kharkiv National University, 61022, 35 Sumska str., Kharkiv, Ukraine email: Velichko.Anna.B@gmail.com, akhmetovvs@gmail.com, pnfedorov@gmail.com
Peter N. Fedorov
Affiliation:
Institute of Astronomy, V. N. Karazin Kharkiv National University, 61022, 35 Sumska str., Kharkiv, Ukraine email: Velichko.Anna.B@gmail.com, akhmetovvs@gmail.com, pnfedorov@gmail.com
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Abstract

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We derive and compare kinematic parameters of the Galaxy using the PMA and Gaia TGAS data. Two methods are used in calculations: evaluation of the Ogorodnikov-Milne model (OMM) parameters by the least square method (LSM) and a decomposition on a set of vector spherical harmonics (VSH). We trace dependencies on the distance of the derived parameters including the Oort constants A and B and the rotational velocity of the Galaxy Vrot at the Solar distance for the common sample of stars of mixed spectral composition of the PMA and TGAS catalogues. The distances were obtained from the TGAS parallaxes or from reduced proper motions for fainter stars.

The A, B and Vrot parameters derived from proper motions of both catalogues used show identical behaviour but the values are systematically shifted by about 0.5 mas/yr.

The Oort B parameter derived from the PMA sample of red giants shows gradual decrease with increasing the distance while the Oort A has a minimum at about 2 kpc and then gradually increases.

As for models chosen for calculations, first, we confirm conclusions of other authors about the existence of extra-model harmonics in the stellar velocity field. Secondly, not all parameters of the OMM are statistically significant, and the set of parameters depends on the stellar sample used.

Keywords

astrometrystellar kinematicsGalactic structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 100 - 103
Copyright
Copyright © International Astronomical Union 2018 

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