v = ERFA.tpstv(xi, eta, v0)
In the tangent plane projection, given the star's rectangular coordinates and the direction cosines of the tangent point, solve for the direction cosines of the star.
xi,eta double rectangular coordinates of star image (Note 2)
v0 double[3] tangent point's direction cosines
v double[3] star's direction cosines
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The tangent plane projection is also called the "gnomonic projection" and the "central projection".
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The eta axis points due north in the adopted coordinate system. If the direction cosines represent observed (RA,Dec), the tangent plane coordinates (xi,eta) are conventionally called the "standard coordinates". If the direction cosines are with respect to a right-handed triad, (xi,eta) are also right-handed. The units of (xi,eta) are, effectively, radians at the tangent point.
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The method used is to complete the star vector in the (xi,eta) based triad and normalize it, then rotate the triad to put the tangent point at the pole with the x-axis aligned to zero longitude. Writing (a0,b0) for the celestial spherical coordinates of the tangent point, the sequence of rotations is (b-pi/2) around the x-axis followed by (-a-pi/2) around the z-axis.
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If vector v0 is not of unit length, the returned vector v will be wrong.
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If vector v0 points at a pole, the returned vector v will be based on the arbitrary assumption that the longitude coordinate of the tangent point is zero.
spherical vector solve for
eraTpxes eraTpxev xi,eta
eraTpsts > eraTpstv < star
eraTpors eraTporv origin
Calabretta M.R. & Greisen, E.W., 2002, "Representations of celestial coordinates in FITS", Astron.Astrophys. 395, 1077
Green, R.M., "Spherical Astronomy", Cambridge University Press, 1987, Chapter 13.
This revision: 2018 January 2
Copyright (C) 2013-2021, NumFOCUS Foundation. Derived, with permission, from the SOFA library.