Split intlclock out into its own package

svn path=/; revision=27

3 files changed, 562 insertions, 0 deletions

diff --git a/gnome-extra/intlclock-applet/Manifest b/gnome-extra/intlclock-applet/Manifest
new file mode 100644
index 0000000..d4b47d4
--- /dev/null
+++ b/gnome-extra/intlclock-applet/Manifest
@@ -0,0 +1,12 @@
+AUX intlclock-sunpos-gpl.patch 16071 RMD160 76a00b20a18a7b0d4dacf28bbfdf4f8ca00ffe7c SHA1 e69cd3cfc03a1d2d291e10f16450e7a466a0b892 SHA256 680a55ecd34ad2021c085d45f8255c514ef80a22d77bda2e6075141678c1d419
+MD5 2066ccd2e7bffad1203f2abbe7648888 files/intlclock-sunpos-gpl.patch 16071
+RMD160 76a00b20a18a7b0d4dacf28bbfdf4f8ca00ffe7c files/intlclock-sunpos-gpl.patch 16071
+SHA256 680a55ecd34ad2021c085d45f8255c514ef80a22d77bda2e6075141678c1d419 files/intlclock-sunpos-gpl.patch 16071
+DIST intlclock-1.0.tar.gz 605354 RMD160 d463895c794c2dc19f1bd6169903984063369f4b SHA1 29b61d0108a49b2e415aaeb2b71b58ef7804a47f SHA256 8848af9c052c45c5b6304143a22b9ef01d1249db66b30bf0cfdea499a13c7f3a
+EBUILD intlclock-applet-1.0.ebuild 993 RMD160 673891b1366c84c4a18d2cca0114a0c6144dfe44 SHA1 ef6b0fa8df7effdae5b95b710d349ec8d5770805 SHA256 42c4061d1f062d3339e1910e7443b79585de24eeb7e75b79c7aa9057a6d6990f
+MD5 8bc352f3075ac9fc64ac1dcabda384d2 intlclock-applet-1.0.ebuild 993
+RMD160 673891b1366c84c4a18d2cca0114a0c6144dfe44 intlclock-applet-1.0.ebuild 993
+SHA256 42c4061d1f062d3339e1910e7443b79585de24eeb7e75b79c7aa9057a6d6990f intlclock-applet-1.0.ebuild 993
+MD5 023771a1f08e7b1cfe6320a7496d9cb6 files/digest-intlclock-applet-1.0 241
+RMD160 3e6ac668649d3ee94e2a9b2e302c255b8590815e files/digest-intlclock-applet-1.0 241
+SHA256 9cffc1a24561f00c8181459d53b0153f76790d84fdc811a5f383354c7fc8f62d files/digest-intlclock-applet-1.0 241
diff --git a/gnome-extra/intlclock-applet/files/intlclock-sunpos-gpl.patch b/gnome-extra/intlclock-applet/files/intlclock-sunpos-gpl.patch
new file mode 100644
index 0000000..7e8178b
--- /dev/null
+++ b/gnome-extra/intlclock-applet/files/intlclock-sunpos-gpl.patch
@@ -0,0 +1,508 @@
+--- src/intlclock-map.c
++++ src/intlclock-map.c
+@@ -516,7 +516,7 @@
+         width = gdk_pixbuf_get_width (pixbuf);
+         height = gdk_pixbuf_get_height (pixbuf);
+ 
+-        sun_position (now, &sun_lat, &sun_lon);
++        get_sun_position (now, &sun_lat, &sun_lon);
+ 
+         for (y = 0; y < height; y++) {
+                 gdouble lat = (height / 2.0 - y) / (height / 2.0) * 90.0;
+--- src/intlclock-sunpos.c
++++ src/intlclock-sunpos.c
+@@ -1,348 +1,189 @@
+ /*
+- * sunpos.c
+- * kirk johnson
+- * july 1993
++ *  Copyright (C) 2007 Red Hat, Inc.
+  *
+- * includes revisions from Frank T. Solensky, february 1999
++ *  This program is free software; you can redistribute it and/or modify
++ *  it under the terms of the GNU General Public License as published by
++ *  the Free Software Foundation; either version 2, or (at your option)
++ *  any later version.
++ *
++ *  This program is distributed in the hope that it will be useful,
++ *  but WITHOUT ANY WARRANTY; without even the implied warranty of
++ *  MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE.  See the
++ *  GNU General Public License for more details.
++ *
++ *  You should have received a copy of the GNU General Public License
++ *  along with this program; if not, write to the Free Software
++ *  Foundation, Inc., 59 Temple Place - Suite 330, Boston, MA 02111-1307, USA.
+  *
+- * code for calculating the position on the earth's surface for which
+- * the sun is directly overhead (adapted from _practical astronomy
+- * with your calculator, third edition_, peter duffett-smith,
+- * cambridge university press, 1988.)
+- *
+- * Copyright (C) 1989, 1990, 1993-1995, 1999 Kirk Lauritz Johnson
+- *
+- * Parts of the source code (as marked) are:
+- *   Copyright (C) 1989, 1990, 1991 by Jim Frost
+- *   Copyright (C) 1992 by Jamie Zawinski <jwz@lucid.com>
+- *
+- * Permission to use, copy, modify and freely distribute xearth for
+- * non-commercial and not-for-profit purposes is hereby granted
+- * without fee, provided that both the above copyright notice and this
+- * permission notice appear in all copies and in supporting
+- * documentation.
+- *
+- * Unisys Corporation holds worldwide patent rights on the Lempel Zev
+- * Welch (LZW) compression technique employed in the CompuServe GIF
+- * image file format as well as in other formats. Unisys has made it
+- * clear, however, that it does not require licensing or fees to be
+- * paid for freely distributed, non-commercial applications (such as
+- * xearth) that employ LZW/GIF technology. Those wishing further
+- * information about licensing the LZW patent should contact Unisys
+- * directly at (lzw_info@unisys.com) or by writing to
+- *
+- *   Unisys Corporation
+- *   Welch Licensing Department
+- *   M/S-C1SW19
+- *   P.O. Box 500
+- *   Blue Bell, PA 19424
+- *
+- * The author makes no representations about the suitability of this
+- * software for any purpose. It is provided "as is" without express or
+- * implied warranty.
+- *
+- * THE AUTHOR DISCLAIMS ALL WARRANTIES WITH REGARD TO THIS SOFTWARE,
+- * INCLUDING ALL IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS,
+- * IN NO EVENT SHALL THE AUTHOR BE LIABLE FOR ANY SPECIAL, INDIRECT
+- * OR CONSEQUENTIAL DAMAGES OR ANY DAMAGES WHATSOEVER RESULTING FROM
+- * LOSS OF USE, DATA OR PROFITS, WHETHER IN AN ACTION OF CONTRACT,
+- * NEGLIGENCE OR OTHER TORTIOUS ACTION, ARISING OUT OF OR IN
+- * CONNECTION WITH THE USE OR PERFORMANCE OF THIS SOFTWARE.
+- */
+-
+-#include <assert.h>
+-#include <math.h>
+-#include <time.h>
+-
+-#include "intlclock-sunpos.h"
+-
+-#define TWOPI         (2*M_PI)
+-#define DegsToRads(x) ((x)*(TWOPI/360))
+-
+-/*
+- * the epoch upon which these astronomical calculations are based is
+- * 1990 january 0.0, 631065600 seconds since the beginning of the
+- * "unix epoch" (00:00:00 GMT, Jan. 1, 1970)
+- *
+- * given a number of seconds since the start of the unix epoch,
+- * DaysSinceEpoch() computes the number of days since the start of the
+- * astronomical epoch (1990 january 0.0)
++ * AUTHORS: Jonathan Blandford <jrb@redhat.com>, Matthias Clasen <mclasen@redhat.com>
+  */
+ 
+-#define EpochStart           (631065600)
+-#define DaysSinceEpoch(secs) (((secs)-EpochStart)*(1.0/(24*3600)))
+ 
+-/*
+- * assuming the apparent orbit of the sun about the earth is circular,
+- * the rate at which the orbit progresses is given by RadsPerDay --
+- * TWOPI radians per orbit divided by 365.242191 days per year:
+- */
+-
+-#define RadsPerDay (TWOPI/365.242191)
++#include <time.h>
++#include <gtk/gtk.h>
++#include <math.h>
+ 
+-/*
+- * details of sun's apparent orbit at epoch 1990.0 (after
+- * duffett-smith, table 6, section 46)
+- *
+- * Epsilon_g    (ecliptic longitude at epoch 1990.0) 279.403303 degrees
+- * OmegaBar_g   (ecliptic longitude of perigee)      282.768422 degrees
+- * Eccentricity (eccentricity of orbit)                0.016713
++/* Calculated with the methods and figures from "Practical Astronomy With Your
++ * Calculator, version 3" by Peter Duffet-Smith.
+  */
++/* Table 6.  Details of the Sun's apparent orbit at epoch 1990.0 */
+ 
+-#define Epsilon_g    (DegsToRads(279.403303))
+-#define OmegaBar_g   (DegsToRads(282.768422))
+-#define Eccentricity (0.016713)
++#define EPOCH          2447891.5  /* days */    /* epoch 1990 */
++#define UNIX_EPOCH     2440586.5  /* days */    /* epoch 1970 */
++#define EPSILON_G      279.403303 /* degrees */ /* ecliptic longitude at epoch 1990.0 */
++#define PI_G           282.768422 /* degrees */ /* ecliptic longitude at perigree */
++#define ECCENTRICITY   0.016713                 /* eccentricity of orbit */
++#define R_0            149598500  /* km */      /* semi-major access */
++#define THETA_0        0.533128   /* degrees */ /* angular diameter at r = r_0 */
++#define MEAN_OBLIQUITY 23.440592  /* degrees */ /* mean obliquity of earths axis at epoch 1990.0 */
+ 
+-/*
+- * MeanObliquity gives the mean obliquity of the earth's axis at epoch
+- * 1990.0 (computed as 23.440592 degrees according to the method given
+- * in duffett-smith, section 27)
+- */
+-#define MeanObliquity (23.440592*(TWOPI/360))
++/* Constrain x to 0-360 degrees */
++#define NORMALIZE(x) \
++  while (x>360) x-=360; while (x<0) x+= 360;
+ 
+-/*
+- * Lunar parameters, epoch January 0, 1990.0
+- */
+-#define MoonMeanLongitude        DegsToRads(318.351648)
+-#define MoonMeanLongitudePerigee DegsToRads( 36.340410)
+-#define MoonMeanLongitudeNode    DegsToRads(318.510107)
+-#define MoonInclination          DegsToRads(  5.145396)
++#define DEG_TO_RADS(x) \
++  (x * G_PI/180.0)
+ 
+-#define SideralMonth (27.3217)
++#define RADS_TO_DEG(x) \
++  (x * 180.0/G_PI)
+ 
+-/*
+- * Force an angular value into the range [-PI, +PI]
+- */
+-#define Normalize(x)                        \
+-  do {                                      \
+-    if ((x) < -M_PI)                        \
+-      do (x) += TWOPI; while ((x) < -M_PI); \
+-    else if ((x) > M_PI)                    \
+-      do (x) -= TWOPI; while ((x) > M_PI);  \
+-  } while (0)
+-
+-static double solve_keplers_equation (double);
+-static double mean_sun (double);
+-static double sun_ecliptic_longitude (time_t);
+-static void   ecliptic_to_equatorial (double, double, double *, double *);
+-static double julian_date (int, int, int);
+-static double GST (time_t);
+-
+-/*
+- * solve Kepler's equation via Newton's method
+- * (after duffett-smith, section 47)
++/* Calculate number of days since 4713BC.
+  */
+-static double solve_keplers_equation(M)
+-     double M;
++static gdouble
++unix_time_to_julian_date (gint unix_time)
+ {
+-  double E;
+-  double delta;
+-
+-  E = M;
+-  while (1)
+-  {
+-    delta = E - Eccentricity*sin(E) - M;
+-    if (fabs(delta) <= 1e-10) break;
+-    E -= delta / (1 - Eccentricity*cos(E));
+-  }
+-
+-  return E;
++  return UNIX_EPOCH + (double) unix_time / (60 * 60 * 24);
+ }
+ 
++/* Finds an iterative solution for [ E - e sin (E) = M ] for values of e less
++   than 0.1.  Page 90  */
+ 
+-/*
+- * Calculate the position of the mean sun: where the sun would
+- * be if the earth's orbit were circular instead of ellipictal.
+- */
++#define ERROR_ACCURACY 1e-6 /* radians */
+ 
+-static double mean_sun (D)
+-     double D;                  /* days since ephemeris epoch */
++static gdouble
++solve_keplers_equation (gdouble e,
++			gdouble M)
+ {
+-  double N, M;
++  gdouble d, E;
+ 
+-  N = RadsPerDay * D;
+-  N = fmod(N, TWOPI);
+-  if (N < 0) N += TWOPI;
+-
+-  M = N + Epsilon_g - OmegaBar_g;
+-  if (M < 0) M += TWOPI;
+-  return M;
+-}
+-
+-/*
+- * compute ecliptic longitude of sun (in radians)
+- * (after duffett-smith, section 47)
+- */
+-static double sun_ecliptic_longitude(ssue)
+-     time_t ssue;               /* seconds since unix epoch */
+-{
+-  double D;
+-  double M_sun, E;
+-  double v;
+-
+-  D = DaysSinceEpoch(ssue);
+-  M_sun = mean_sun(D);
++  /* start with an initial estimate */
++  E = M;
++  
++  d = E - e * sin (E) - M;
+ 
+-  E = solve_keplers_equation(M_sun);
+-  v = 2 * atan(sqrt((1+Eccentricity)/(1-Eccentricity)) * tan(E/2));
++  while (ABS (d) > ERROR_ACCURACY)
++    {
++      E = E - (d / (1 - e * cos (E)));
++      d = E - e * sin (E) - M;
++    }
+ 
+-  return (v + OmegaBar_g);
++  return E;
+ }
+ 
++  /* convert the ecliptic longitude to right ascension and declination.  Section 27.  */
++static void
++ecliptic_to_equatorial (gdouble  lambda,
++			gdouble  beta,
++			gdouble *ra,
++			gdouble *dec)
++{
++  gdouble cos_mo;
++  gdouble sin_mo;
++
++  g_assert (ra != NULL);
++  g_assert (dec != NULL);
++
++  sin_mo = sin (DEG_TO_RADS (MEAN_OBLIQUITY));
++  cos_mo = cos (DEG_TO_RADS (MEAN_OBLIQUITY));
++
++  *ra = atan2 (sin (lambda) * cos_mo - tan (beta) * sin_mo, cos (lambda));
++  *dec = asin (sin (beta) * cos_mo + cos (beta) * sin_mo * sin (lambda));
++}
++
++/* calculate GST.  Section 12  */
++static gdouble
++greenwich_sidereal_time (gdouble unix_time)
++{
++  gdouble u, JD, T, T0, UT;
++
++  u = fmod (unix_time, 24 * 60 * 60);
++  JD = unix_time_to_julian_date (unix_time - u);
++  T = (JD - 2451545) / 36525;
++  T0 = 6.697374558 + (2400.051336 * T) + (0.000025862 * T * T);
++  T0 = fmod (T0, 24);
++  UT = u / (60 * 60);
++  T0 = T0 + UT * 1.002737909;
++  T0 = fmod (T0, 24);
+ 
+-/*
+- * convert from ecliptic to equatorial coordinates
+- * (after duffett-smith, section 27)
+- */
+-static void ecliptic_to_equatorial(lambda, beta, alpha, delta)
+-     double  lambda;            /* ecliptic longitude       */
+-     double  beta;              /* ecliptic latitude        */
+-     double *alpha;             /* (return) right ascension */
+-     double *delta;             /* (return) declination     */
+-{
+-  double sin_e, cos_e;
+-
+-  sin_e = sin(MeanObliquity);
+-  cos_e = cos(MeanObliquity);
+-
+-  *alpha = atan2(sin(lambda)*cos_e - tan(beta)*sin_e, cos(lambda));
+-  *delta = asin(sin(beta)*cos_e + cos(beta)*sin_e*sin(lambda));
++  return T0;
+ }
+ 
+-
+-/*
+- * computing julian dates (assuming gregorian calendar, thus this is
+- * only valid for dates of 1582 oct 15 or later)
+- * (after duffett-smith, section 4)
+- */
+-static double julian_date(y, m, d)
+-     int y;                     /* year (e.g. 19xx)          */
+-     int m;                     /* month (jan=1, feb=2, ...) */
+-     int d;                     /* day of month              */
++/* Calulate the position of the sun at a given time.  pages 89-91 */
++void
++get_sun_position (gint unix_time, gdouble *latitude, gdouble *longitude)
+ {
+-  int    A, B, C, D;
+-  double JD;
++  gdouble jd, D, N, M, E, x, v, lambda;
++  gdouble ra, dec, lat, lon;
++  jd = unix_time_to_julian_date (unix_time);
+ 
+-  /* lazy test to ensure gregorian calendar */
+-  assert(y >= 1583);
++  /* Calculate number of days since the epoch */
++  D = jd - EPOCH;
+ 
+-  if ((m == 1) || (m == 2))
+-  {
+-    y -= 1;
+-    m += 12;
+-  }
+-
+-  A = y / 100;
+-  B = 2 - A + (A / 4);
+-  C = 365.25 * y;
+-  D = 30.6001 * (m + 1);
++  N = D*360/365.242191;
+ 
+-  JD = B + C + D + d + 1720994.5;
++  /* noramlize to 0 - 360 degrees */
++  NORMALIZE (N);
+ 
+-  return JD;
+-}
++  /* Step 4: */
++  M = N + EPSILON_G - PI_G;
++  NORMALIZE (M);
+ 
++  /* Step 5: convert to radians */
++  M = DEG_TO_RADS (M);
+ 
+-/*
+- * compute greenwich mean sidereal time (GST) corresponding to a given
+- * number of seconds since the unix epoch
+- * (after duffett-smith, section 12)
+- */
+-static double GST(ssue)
+-     time_t ssue;               /* seconds since unix epoch */
+-{
+-  double     JD;
+-  double     T, T0;
+-  double     UT;
+-  struct tm *tm;
+-
+-  tm = gmtime(&ssue);
++  /* Step 6: */
++  E = solve_keplers_equation (ECCENTRICITY, M);
+ 
+-  JD = julian_date(tm->tm_year+1900, tm->tm_mon+1, tm->tm_mday);
+-  T  = (JD - 2451545) / 36525;
++  /* Step 7: */
++  x = sqrt ((1 + ECCENTRICITY)/(1 - ECCENTRICITY)) * tan (E/2);
+ 
+-  T0 = ((T + 2.5862e-5) * T + 2400.051336) * T + 6.697374558;
++  /* Step 8, 9 */
++  v = 2 * RADS_TO_DEG (atan (x));
++  NORMALIZE (v);
+ 
+-  T0 = fmod(T0, 24.0);
+-  if (T0 < 0) T0 += 24;
++  /* Step 10 */
++  lambda = v + PI_G;
++  NORMALIZE (lambda);
+ 
+-  UT = tm->tm_hour + (tm->tm_min + tm->tm_sec / 60.0) / 60.0;
++  /* convert the ecliptic longitude to right ascension and declination */
++  ecliptic_to_equatorial (DEG_TO_RADS (lambda), 0.0, &ra, &dec);
+ 
+-  T0 += UT * 1.002737909;
+-  T0 = fmod(T0, 24.0);
+-  if (T0 < 0) T0 += 24;
++  ra = ra - (G_PI/12) * greenwich_sidereal_time (unix_time);
+ 
+-  return T0;
++  *longitude = RADS_TO_DEG (ra);
++  *latitude = RADS_TO_DEG (dec);
++/*
++  NORMALIZE (ra);
++  NORMALIZE (dec);
++*/
+ }
+ 
+-
+ /*
+- * given a particular time (expressed in seconds since the unix
+- * epoch), compute position on the earth (lat, lon) such that sun is
+- * directly overhead.
+- */
+-void sun_position(ssue, lat, lon)
+-     time_t  ssue;              /* seconds since unix epoch */
+-     double *lat;               /* (return) latitude        */
+-     double *lon;               /* (return) longitude       */
++int
++main (int argc, char *argv[])
+ {
+-  double lambda;
+-  double alpha, delta;
+-  double tmp;
+-
+-  lambda = sun_ecliptic_longitude(ssue);
+-  ecliptic_to_equatorial(lambda, 0.0, &alpha, &delta);
+-
+-  tmp = alpha - (TWOPI/24)*GST(ssue);
+-  Normalize(tmp);
+-  *lon = tmp * (360/TWOPI);
+-  *lat = delta * (360/TWOPI);
+-}
++  gint i;
++  gint now;
++  GTimeVal timeval;
+ 
++  gtk_init (&argc, &argv);
+ 
+-/*
+- * given a particular time (expressed in seconds since the unix
+- * epoch), compute position on the earth (lat, lon) such that the
+- * moon is directly overhead.
+- *
+- * Based on duffett-smith **2nd ed** section 61; combines some steps
+- * into single expressions to reduce the number of extra variables.
+- */
+-void moon_position(ssue, lat, lon)
+-     time_t  ssue;              /* seconds since unix epoch */
+-     double *lat;               /* (return) latitude        */
+-     double *lon;               /* (return) longitude       */
+-{
+-  double lambda, beta;
+-  double D, L, Ms, Mm, N, Ev, Ae, Ec, alpha, delta;
++  g_get_current_time (&timeval);
++  now = timeval.tv_sec;
++
++  for (i = 0; i < now; i += 15 * 60)
++    get_sun_position (i);
+ 
+-  D      = DaysSinceEpoch(ssue);
+-  lambda = sun_ecliptic_longitude(ssue);
+-  Ms     = mean_sun(D);
+-
+-  L = fmod(D/SideralMonth, 1.0)*TWOPI + MoonMeanLongitude;
+-  Normalize(L);
+-  Mm = L - DegsToRads(0.1114041*D) - MoonMeanLongitudePerigee;
+-  Normalize(Mm);
+-  N = MoonMeanLongitudeNode - DegsToRads(0.0529539*D);
+-  Normalize(N);
+-  Ev  = DegsToRads(1.2739) * sin(2.0*(L-lambda)-Mm);
+-  Ae  = DegsToRads(0.1858) * sin(Ms);
+-  Mm += Ev - Ae - DegsToRads(0.37)*sin(Ms);
+-  Ec  = DegsToRads(6.2886) * sin(Mm);
+-  L  += Ev + Ec - Ae + DegsToRads(0.214) * sin(2.0*Mm);
+-  L  += DegsToRads(0.6583) * sin(2.0*(L-lambda));
+-  N  -= DegsToRads(0.16) * sin(Ms);
+-
+-  L -= N;
+-  lambda =(fabs(cos(L)) < 1e-12) ?
+-    (N + sin(L) * cos(MoonInclination) * M_PI/2) :
+-    (N + atan2(sin(L) * cos(MoonInclination), cos(L)));
+-  Normalize(lambda);
+-  beta = asin(sin(L) * sin(MoonInclination));
+-  ecliptic_to_equatorial(lambda, beta, &alpha, &delta);
+-  alpha -= (TWOPI/24)*GST(ssue);
+-  Normalize(alpha);
+-  *lon = alpha * (360/TWOPI);
+-  *lat = delta * (360/TWOPI);
++  return 0;
+ }
++*/
+--- src/intlclock-sunpos.h
++++ src/intlclock-sunpos.h
+@@ -1 +1,2 @@
+-void sun_position(time_t ssue, double *lat, double *lon);
++void
++get_sun_position (gint unix_time, gdouble *latitude, gdouble *longitude);
diff --git a/gnome-extra/intlclock-applet/intlclock-applet-1.0.ebuild b/gnome-extra/intlclock-applet/intlclock-applet-1.0.ebuild
new file mode 100644
index 0000000..123bf4c
--- /dev/null
+++ b/gnome-extra/intlclock-applet/intlclock-applet-1.0.ebuild
@@ -0,0 +1,42 @@
+# Copyright 1999-2007 Gentoo Foundation
+# Distributed under the terms of the GNU General Public License v2
+# $Header: /var/cvsroot/gentoo-x86/gnome-extra/fast-user-switch-applet/fast-user-switch-applet-2.18.0.ebuild,v 1.8 2007/08/28 19:34:07 jer Exp $
+
+inherit eutils gnome2
+
+DESCRIPTION="Enhanced international Clock for the GNOME Panel"
+HOMEPAGE="http://www.gnome.org/"
+MY_PN="intlclock"
+MY_P="${MY_PN}-${PV}"
+SRC_URI="http://dev.gentoo.org/~suka/files/${MY_P}.tar.gz"
+S="${WORKDIR}/${MY_P}"
+
+LICENSE="GPL-2"
+SLOT="0"
+KEYWORDS="~x86"
+IUSE="eds"
+
+RDEPEND=">=dev-libs/glib-2
+	>=x11-libs/gtk+-2
+	>=gnome-base/librsvg-2
+	>=gnome-base/gconf-2
+	>=gnome-base/gnome-panel-2.0
+	>=gnome-base/libgnome-2
+	eds? ( >=gnome-extra/evolution-data-server-1.6 )"
+
+DEPEND="${RDEPEND}"
+
+DOCS="AUTHORS ChangeLog NEWS README"
+USE_DESTDIR="1"
+
+pkg_setup() {
+	GG2CONF="--disable-scrollkeeper $(use_enable eds)"
+}
+
+src_unpack() {
+	unpack ${A}
+	cd ${S}
+	epatch ${FILESDIR}/${MY_PN}-sunpos-gpl.patch
+
+	gnome2_omf_fix
+}