Repatch (from linux) of OSX IRAF

1 files changed, 117 insertions, 0 deletions

diff --git a/noao/astutil/asttools/astprecess.x b/noao/astutil/asttools/astprecess.x
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+include	<math.h>
+
+# AST_PRECESS -- Precess coordinates from epoch1 to epoch2.
+#
+# The method used here is based on the new IAU system described in the
+# supplement to the 1984 Astronomical Almanac.  The precession is
+# done in two steps; precess epoch1 to the standard epoch J2000.0 and then
+# precess from the standard epoch to epoch2.  The precession between
+# any two dates is done this way because the rotation matrix coefficients
+# are given relative to the standard epoch.
+
+procedure ast_precess (ra1, dec1, epoch1, ra2, dec2, epoch2)
+
+double	ra1, dec1, epoch1		# First coordinates
+double	ra2, dec2, epoch2		# Second coordinates
+
+double	r0[3], r1[3], p[3, 3]
+bool	fp_equald()
+
+begin
+	# If the input epoch is 0 or undefined then assume the input epoch
+	# is the same as the output epoch.  If the two epochs are the same
+	# then return the coordinates from epoch1.
+
+	if ((epoch1 == 0.) || IS_INDEFD (epoch1) || fp_equald(epoch1, epoch2)) {
+	    ra2 = ra1
+	    dec2 = dec1
+	    return
+	}
+
+	# Rectangular equitorial coordinates (direction cosines).
+	ra2 = DEGTORAD (ra1 * 15.)
+	dec2 = DEGTORAD (dec1)
+
+	r0[1] = cos (ra2) * cos (dec2)
+	r0[2] = sin (ra2) * cos (dec2)
+	r0[3] = sin (dec2)
+
+	# If epoch1 is not the standard epoch then precess to the standard
+	# epoch.
+
+	if (epoch1 != 2000.) {
+	    call ast_rotmatrix (epoch1, p)
+
+	    # Note that we multiply by the inverse of p which is the
+	    # transpose of p.
+
+	    r1[1] = p[1, 1] * r0[1] + p[1, 2] * r0[2] + p[1, 3] * r0[3]
+	    r1[2] = p[2, 1] * r0[1] + p[2, 2] * r0[2] + p[2, 3] * r0[3]
+	    r1[3] = p[3, 1] * r0[1] + p[3, 2] * r0[2] + p[3, 3] * r0[3]
+	    r0[1] = r1[1]
+	    r0[2] = r1[2]
+	    r0[3] = r1[3]
+	}
+
+	# If epoch2 is not the standard epoch then precess from the standard
+	# epoch to the desired epoch.
+
+	if (epoch2 != 2000.) {
+	    call ast_rotmatrix (epoch2, p)
+	    r1[1] = p[1, 1] * r0[1] + p[2, 1] * r0[2] + p[3, 1] * r0[3]
+	    r1[2] = p[1, 2] * r0[1] + p[2, 2] * r0[2] + p[3, 2] * r0[3]
+	    r1[3] = p[1, 3] * r0[1] + p[2, 3] * r0[2] + p[3, 3] * r0[3]
+	    r0[1] = r1[1]
+	    r0[2] = r1[2]
+	    r0[3] = r1[3]
+	}
+
+	# Convert from radians to hours and degrees.
+	ra2 = RADTODEG (atan2 (r0[2], r0[1]) / 15.)
+	dec2 = RADTODEG (asin (r0[3]))
+	if (ra2 < 0.)
+	    ra2 = ra2 + 24
+end
+
+
+# ROTMATRIX -- Compute the precession rotation matrix from the standard epoch
+# J2000.0 to the specified epoch.
+
+procedure ast_rotmatrix (epoch, p)
+
+double	epoch		# Epoch of date
+double	p[3, 3]		# Rotation matrix
+
+double	t, a, b, c, ca, cb, cc, sa, sb, sc
+double	ast_julday()
+
+begin
+	# The rotation matrix coefficients are polynomials in time measured
+	# in Julian centuries from the standard epoch.  The coefficients are
+	# in degrees.
+
+	t = (ast_julday (epoch) - 2451545.0d0) / 36525d0
+
+	a = t * (0.6406161d0 + t * (0.0000839d0 + t * 0.0000050d0))
+	b = t * (0.6406161d0 + t * (0.0003041d0 + t * 0.0000051d0))
+	c = t * (0.5567530d0 - t * (0.0001185d0 + t * 0.0000116d0))
+
+	# Compute the cosines and sines once for efficiency.
+	ca = cos (DEGTORAD (a))
+	sa = sin (DEGTORAD (a))
+	cb = cos (DEGTORAD (b))
+	sb = sin (DEGTORAD (b))
+	cc = cos (DEGTORAD (c))
+	sc = sin (DEGTORAD (c))
+
+	# Compute the rotation matrix from the sines and cosines.
+	p[1, 1] = ca * cb * cc - sa * sb
+	p[2, 1] = -sa * cb * cc - ca * sb
+	p[3, 1] = -cb * sc
+	p[1, 2] = ca * sb * cc + sa * cb
+	p[2, 2] = -sa * sb * cc + ca * cb
+	p[3, 2] = -sb * sc
+	p[1, 3] = ca * sc
+	p[2, 3] = -sa * sc
+	p[3, 3] = cc
+end