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Absolute Magnitudes by Statistical Parallaxes

Published online by Cambridge University Press:  14 August 2015

André Heck
André Heck*
Affiliation:
Liége Institute of Astrophysics (Belgium)

Extract

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Our algorithm for stellar luminosity calibrations (based on the principle of maximum likelihood) allows the calibration of relations of the type:

Where n is the size of the sample at hand,

  • Mi, are the individual absolute magnitudes,

  • Cij are observational quantities (j = 1, …, N), and

  • qj are the coefficients to be determined.

If we put N = 1 and CiN = 1, we have the mean absolute magnitude of the sample. As additional output, the algorithm provides us also with the dispersion in magnitude of the sample σM, the mean solar motion (U, V, W) and the corresponding velocity ellipsoid (σu, σV, σw).

Type
Part I: Fundamentals of the HR Diagram
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 49 - 52
Copyright
Copyright © Reidel 1978 

References

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