Application of Vector Spherical Harmonics and Kernel Regression to the Computations of OMM Parameters
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Otros documentos de la autoría: Marco Castillo, Francisco José; Martínez, M. J.; López Ortí, José Antonio
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Título
Application of Vector Spherical Harmonics and Kernel Regression to the Computations of OMM ParametersFecha de publicación
2015-04Editor
The American Astronomical SocietyISSN
0004-6256Cita bibliográfica
MARCO, F. J.; MARTÍNEZ, M. J.; LÓPEZ, J. A. Application of Vector Spherical Harmonics and Kernel Regression to the Computations of OMM Parameters. The Astronomical Journal, 2015, vol. 149, no 4, p. 129.Tipo de documento
info:eu-repo/semantics/articleVersión de la editorial
http://iopscience.iop.org/article/10.1088/0004-6256/149/4/129/metaVersión
info:eu-repo/semantics/publishedVersionPalabras clave / Materias
Resumen
The high quality of Hipparcos data in position, proper motion, and parallax has allowed for studies about stellar
kinematics with the aim of achieving a better physical understanding of our galaxy, based on accurate ... [+]
The high quality of Hipparcos data in position, proper motion, and parallax has allowed for studies about stellar
kinematics with the aim of achieving a better physical understanding of our galaxy, based on accurate calculus of
the Ogorodnikov–Milne model (OMM) parameters. The use of discrete least squares is the most common
adjustment method, but it may lead to errors mainly because of the inhomogeneous spatial distribution of the data.
We present an example of the instability of this method using the case of a function given by a linear combination
of Legendre polynomials. These polynomials are basic in the use of vector spherical harmonics, which have been
used to compute the OMM parameters by several authors, such as Makarov & Murphy, Mignard & Klioner, and
Vityazev & Tsvetkov. To overcome the former problem, we propose the use of a mixed method (see Marco et al.)
that includes the extension of the functions of residuals to any point on the celestial sphere. The goal is to be able to
work with continuous variables in the calculation of the coefficients of the vector spherical harmonic developments
with stability and efficiency. We apply this mixed procedure to the study of the kinematics of the stars in our
Galaxy, employing the Hipparcos velocity field data to obtain the OMM parameters. Previously, we tested the
method by perturbing the Vectorial Spherical Harmonics model as well as the velocity vector field. [-]
Publicado en
The Astronomical Journal, 2015, vol. 149, no 4Derechos de acceso
© 2015. The American Astronomical Society. All rights reserved.
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