Issue |
A&A
Volume 401, Number 3, April III 2003
|
|
---|---|---|
Page(s) | 951 - 958 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361:20030152 | |
Published online | 01 April 2003 |
A method for deriving stellar space densities
Instituto Argentino de Nivología y Glaciología (IANIGLA), C.C. 330, 5500 Mendoza, Argentina
Corresponding author: rlb@lanet.com.ar
Received:
16
July
2002
Accepted:
28
January
2003
The fundamental integral equation of stellar statistics
represents a direct, model-independent approach to calculating stellar
densities. Many techniques exist for its solution, but some of these require
assumptions, such as a Gaussian luminosity function or a specific form for
the density function, that may be unrealistic. To solve the equation as an
undeterdetermined total least squares system with Tikhanov regularization
recognizes that the problem is ill-posed and generally ill-conditioned as
well and offers decided advantages: it is unnecessary to assume a Gaussian
luminosity function nor a specific form for the density function;
discretization error in the kernel of the integral equation as well as the
Poisson error in the star counts are accounted for; mean errors for the
densities are calculated; the densities are constrained to be both
continuous and positive. The greatest drawback to the method comes from the
selection of the ridge parameter, but the drawback becomes surmountable. The
method is first applied to three examples, general star counts, the
distribution of K0 giants, and the distribution of M 2–M 4 dwarfs, and
compared with densities calculated from methods such as Malmquist's and the
(m, log table. Regularized total least squares competes well with
these methods. Then the method is applied to a new data set from the
AC2000.2 catalog to calculate the densities of M giants and supergiants in
the directions of the north and south galactic poles. The densities decrease
exponentially to near zero at 2000 pc, with half-density points near 550 pc
No evidence for asymmetry between the two hemispheres can be seen.
Key words: galactic structure / methods / data reduction
© ESO, 2003
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