   return (DST);
 }
 
-/*
-  SUNRISET.C - Computes Sun rise/set times, start/end of twilight, and
-             the length of the day at any date and latitude
-
-  Written as DAYLEN.C, 1989-08-16
-
-  Modified to SUNRISET.C, 1992-12-01
-
-  (c) Paul Schlyter, 1989, 1992
-
-  Released to the public domain by Paul Schlyter, December 1992
-
-  http://stjarnhimlen.se/comp/sunriset.c
-
-*/
-
-/* The "workhorse" function for sun rise/set times */
-int __sunriset__( int year, int month, int day, double lon, double lat,
-                  double altit, int upper_limb, double *trise, double *tset )
-/***************************************************************************/
-/* Note: year,month,date = calendar date, 1801-2099 only.             */
-/*       Eastern longitude positive, Western longitude negative       */
-/*       Northern latitude positive, Southern latitude negative       */
-/*       The longitude value IS critical in this function!            */
-/*       altit = the altitude which the Sun should cross              */
-/*               Set to -35/60 degrees for rise/set, -6 degrees       */
-/*               for civil, -12 degrees for nautical and -18          */
-/*               degrees for astronomical twilight.                   */
-/*         upper_limb: non-zero -> upper limb, zero -> center         */
-/*               Set to non-zero (e.g. 1) when computing rise/set     */
-/*               times, and to zero when computing start/end of       */
-/*               twilight.                                            */
-/*        *rise = where to store the rise time                        */
-/*        *set  = where to store the set  time                        */
-/*                Both times are relative to the specified altitude,  */
-/*                and thus this function can be used to compute       */
-/*                various twilight times, as well as rise/set times   */
-/* Return value:  0 = sun rises/sets this day, times stored at        */
-/*                    *trise and *tset.                               */
-/*               +1 = sun above the specified "horizon" 24 hours.     */
-/*                    *trise set to time when the sun is at south,    */
-/*                    minus 12 hours while *tset is set to the south  */
-/*                    time plus 12 hours. "Day" length = 24 hours     */
-/*               -1 = sun is below the specified "horizon" 24 hours   */
-/*                    "Day" length = 0 hours, *trise and *tset are    */
-/*                    both set to the time when the sun is at south.  */
-/*                                                                    */
-/**********************************************************************/
-{
-  double  d,  /* Days since 2000 Jan 0.0 (negative before) */
-          sr,         /* Solar distance, astronomical units */
-          sRA,        /* Sun's Right Ascension */
-          sdec,       /* Sun's declination */
-          sradius,    /* Sun's apparent radius */
-          t,          /* Diurnal arc */
-          tsouth,     /* Time when Sun is at south */
-          sidtime;    /* Local sidereal time */
-
-  int rc = 0; /* Return cde from function - usually 0 */
-
-  /* Compute d of 12h local mean solar time */
-  d = days_since_2000_Jan_0(year, month, day) + 0.5 - lon / 360.0;
-
-  /* Compute the local sidereal time of this moment */
-  sidtime = revolution( GMST0(d) + 180.0 + lon );
-
-  /* Compute Sun's RA, Decl and distance at this moment */
-  sun_RA_dec( d, &sRA, &sdec, &sr );
-
-  /* Compute time when Sun is at south - in hours UT */
-  tsouth = 12.0 - rev180(sidtime - sRA) / 15.0;
-
-  /* Compute the Sun's apparent radius in degrees */
-  sradius = 0.2666 / sr;
-
-  /* Do correction to upper limb, if necessary */
-  if ( upper_limb )
-    altit -= sradius;
-
-  /* Compute the diurnal arc that the Sun traverses to reach */
-  /* the specified altitude altit: */
-  {
-    double cost;
-    cost = ( sind(altit) - sind(lat) * sind(sdec) ) /
-           ( cosd(lat) * cosd(sdec) );
-    if ( cost >= 1.0 )
-      rc = -1, t = 0.0;       /* Sun always below altit */
-    else if ( cost <= -1.0 )
-      rc = +1, t = 12.0;      /* Sun always above altit */
-    else
-      t = acosd(cost) / 15.0; /* The diurnal arc, hours */
-  }
-
-  /* Store rise and set times - in hours UT */
-  *trise = tsouth - t;
-  *tset  = tsouth + t;
-
-  return rc;
-}  /* __sunriset__ */
-
-/* The "workhorse" function */
-double __daylen__( int year, int month, int day, double lon, double lat,
-                   double altit, int upper_limb )
-/**********************************************************************/
-/* Note: year,month,date = calendar date, 1801-2099 only.             */
-/*       Eastern longitude positive, Western longitude negative       */
-/*       Northern latitude positive, Southern latitude negative       */
-/*       The longitude value is not critical. Set it to the correct   */
-/*       longitude if you're picky, otherwise set to to, say, 0.0     */
-/*       The latitude however IS critical - be sure to get it correct */
-/*       altit = the altitude which the Sun should cross              */
-/*               Set to -35/60 degrees for rise/set, -6 degrees       */
-/*               for civil, -12 degrees for nautical and -18          */
-/*               degrees for astronomical twilight.                   */
-/*         upper_limb: non-zero -> upper limb, zero -> center         */
-/*               Set to non-zero (e.g. 1) when computing day length   */
-/*               and to zero when computing day+twilight length.      */
-/**********************************************************************/
-{
-  double  d,  /* Days since 2000 Jan 0.0 (negative before) */
-          obl_ecl,    /* Obliquity (inclination) of Earth's axis */
-          sr,         /* Solar distance, astronomical units */
-          slon,       /* True solar longitude */
-          sin_sdecl,  /* Sine of Sun's declination */
-          cos_sdecl,  /* Cosine of Sun's declination */
-          sradius,    /* Sun's apparent radius */
-          t;          /* Diurnal arc */
-
-  /* Compute d of 12h local mean solar time */
-  d = days_since_2000_Jan_0(year, month, day) + 0.5 - lon / 360.0;
-
-  /* Compute obliquity of ecliptic (inclination of Earth's axis) */
-  obl_ecl = 23.4393 - 3.563E-7 * d;
-
-  /* Compute Sun's ecliptic longitude and distance */
-  sunpos( d, &slon, &sr );
-
-  /* Compute sine and cosine of Sun's declination */
-  sin_sdecl = sind(obl_ecl) * sind(slon);
-  cos_sdecl = sqrt( 1.0 - sin_sdecl * sin_sdecl );
-
-  /* Compute the Sun's apparent radius, degrees */
-  sradius = 0.2666 / sr;
-
-  /* Do correction to upper limb, if necessary */
-  if ( upper_limb )
-    altit -= sradius;
-
-  /* Compute the diurnal arc that the Sun traverses to reach */
-  /* the specified altitude altit: */
-  {
-    double cost;
-    cost = ( sind(altit) - sind(lat) * sin_sdecl ) /
-           ( cosd(lat) * cos_sdecl );
-    if ( cost >= 1.0 )
-      t = 0.0;                      /* Sun always below altit */
-    else if ( cost <= -1.0 )
-      t = 24.0;                     /* Sun always above altit */
-    else  t = (2.0 / 15.0) * acosd(cost); /* The diurnal arc, hours */
-  }
-  return t;
-}  /* __daylen__ */
-
-/* This function computes the Sun's position at any instant */
-void sunpos( double d, double *lon, double *r )
-/******************************************************/
-/* Computes the Sun's ecliptic longitude and distance */
-/* at an instant given in d, number of days since     */
-/* 2000 Jan 0.0.  The Sun's ecliptic latitude is not  */
-/* computed, since it's always very near 0.           */
-/******************************************************/
-{
-  double M,         /* Mean anomaly of the Sun */
-         w,         /* Mean longitude of perihelion */
-         /* Note: Sun's mean longitude = M + w */
-         e,         /* Eccentricity of Earth's orbit */
-         E,         /* Eccentric anomaly */
-         x, y,      /* x, y coordinates in orbit */
-         v;         /* True anomaly */
-
-  /* Compute mean elements */
-  M = revolution( 356.0470 + 0.9856002585 * d );
-  w = 282.9404 + 4.70935E-5 * d;
-  e = 0.016709 - 1.151E-9 * d;
-
-  /* Compute true longitude and radius vector */
-  E = M + e * RADEG * sind(M) * ( 1.0 + e * cosd(M) );
-  x = cosd(E) - e;
-  y = sqrt( 1.0 - e * e ) * sind(E);
-  *r = sqrt( x * x + y * y );          /* Solar distance */
-  v = atan2d( y, x );                  /* True anomaly */
-  *lon = v + w;                        /* True solar longitude */
-  if ( *lon >= 360.0 )
-    *lon -= 360.0;                   /* Make it 0..360 degrees */
-}
-
-void sun_RA_dec( double d, double *RA, double *dec, double *r )
-/******************************************************/
-/* Computes the Sun's equatorial coordinates RA, Decl */
-/* and also its distance, at an instant given in d,   */
-/* the number of days since 2000 Jan 0.0.             */
-/******************************************************/
-{
-  double lon, obl_ecl, x, y, z;
-
-  /* Compute Sun's ecliptical coordinates */
-  sunpos( d, &lon, r );
-
-  /* Compute ecliptic rectangular coordinates (z=0) */
-  x = *r * cosd(lon);
-  y = *r * sind(lon);
-
-  /* Compute obliquity of ecliptic (inclination of Earth's axis) */
-  obl_ecl = 23.4393 - 3.563E-7 * d;
-
-  /* Convert to equatorial rectangular coordinates - x is unchanged */
-  z = y * sind(obl_ecl);
-  y = y * cosd(obl_ecl);
-
-  /* Convert to spherical coordinates */
-  *RA = atan2d( y, x );
-  *dec = atan2d( z, sqrt(x * x + y * y) );
-
-}  /* sun_RA_dec */
-
-/******************************************************************/
-/* This function reduces any angle to within the first revolution */
-/* by subtracting or adding even multiples of 360.0 until the     */
-/* result is >= 0.0 and < 360.0                                   */
-/******************************************************************/
+void convertDate(int hour, int* year, int* month, int* day) {
+
+  uint8_t DaysAMonth[] = {31, 28, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31};
+
+  if (*year % 4 == 0) DaysAMonth[1] = 29; //leap year check (the simple method)
+  if (hour < 24) {
+    *day -= 1;
+    if (*day < 1) {
+      if (*month == 1) {
+        *month = 12;
+        *year -= 1;
+      } // if (*month == 1)
+      else {
+        *month -= 1;
+      }
+      *day = DaysAMonth[*month - 1];
+    } // if (*day < 1)
+  } // if (*hour < 24)
+  else if (hour >= 24) {
+    *day += 1;
+    if (*day > DaysAMonth[*month - 1]) {
+      *day = 1;
+      *month += 1;
+      if (*month > 12) *year += 1;
+    } // if (*day > DaysAMonth[*month - 1])
+  }
+}
+
+  /*
+    SUNRISET.C - Computes Sun rise/set times, start/end of twilight, and
+               the length of the day at any date and latitude
+
+    Written as DAYLEN.C, 1989-08-16
+
+    Modified to SUNRISET.C, 1992-12-01
+
+    (c) Paul Schlyter, 1989, 1992
+
+    Released to the public domain by Paul Schlyter, December 1992
+
+    http://stjarnhimlen.se/comp/sunriset.c
+
+  */
+
+  /* The "workhorse" function for sun rise/set times */
+  int __sunriset__( int year, int month, int day, double lon, double lat,
+                    double altit, int upper_limb, double * trise, double * tset )
+  /***************************************************************************/
+  /* Note: year,month,date = calendar date, 1801-2099 only.             */
+  /*       Eastern longitude positive, Western longitude negative       */
+  /*       Northern latitude positive, Southern latitude negative       */
+  /*       The longitude value IS critical in this function!            */
+  /*       altit = the altitude which the Sun should cross              */
+  /*               Set to -35/60 degrees for rise/set, -6 degrees       */
+  /*               for civil, -12 degrees for nautical and -18          */
+  /*               degrees for astronomical twilight.                   */
+  /*         upper_limb: non-zero -> upper limb, zero -> center         */
+  /*               Set to non-zero (e.g. 1) when computing rise/set     */
+  /*               times, and to zero when computing start/end of       */
+  /*               twilight.                                            */
+  /*        *rise = where to store the rise time                        */
+  /*        *set  = where to store the set  time                        */
+  /*                Both times are relative to the specified altitude,  */
+  /*                and thus this function can be used to compute       */
+  /*                various twilight times, as well as rise/set times   */
+  /* Return value:  0 = sun rises/sets this day, times stored at        */
+  /*                    *trise and *tset.                               */
+  /*               +1 = sun above the specified "horizon" 24 hours.     */
+  /*                    *trise set to time when the sun is at south,    */
+  /*                    minus 12 hours while *tset is set to the south  */
+  /*                    time plus 12 hours. "Day" length = 24 hours     */
+  /*               -1 = sun is below the specified "horizon" 24 hours   */
+  /*                    "Day" length = 0 hours, *trise and *tset are    */
+  /*                    both set to the time when the sun is at south.  */
+  /*                                                                    */
+  /**********************************************************************/
+  {
+    double  d,  /* Days since 2000 Jan 0.0 (negative before) */
+            sr,         /* Solar distance, astronomical units */
+            sRA,        /* Sun's Right Ascension */
+            sdec,       /* Sun's declination */
+            sradius,    /* Sun's apparent radius */
+            t,          /* Diurnal arc */
+            tsouth,     /* Time when Sun is at south */
+            sidtime;    /* Local sidereal time */
+
+    int rc = 0; /* Return cde from function - usually 0 */
+
+    /* Compute d of 12h local mean solar time */
+    d = days_since_2000_Jan_0(year, month, day) + 0.5 - lon / 360.0;
+
+    /* Compute the local sidereal time of this moment */
+    sidtime = revolution( GMST0(d) + 180.0 + lon );
+
+    /* Compute Sun's RA, Decl and distance at this moment */
+    sun_RA_dec( d, &sRA, &sdec, &sr );
+
+    /* Compute time when Sun is at south - in hours UT */
+    tsouth = 12.0 - rev180(sidtime - sRA) / 15.0;
+
+    /* Compute the Sun's apparent radius in degrees */
+    sradius = 0.2666 / sr;
+
+    /* Do correction to upper limb, if necessary */
+    if ( upper_limb )
+      altit -= sradius;
+
+    /* Compute the diurnal arc that the Sun traverses to reach */
+    /* the specified altitude altit: */
+    {
+      double cost;
+      cost = ( sind(altit) - sind(lat) * sind(sdec) ) /
+             ( cosd(lat) * cosd(sdec) );
+      if ( cost >= 1.0 )
+        rc = -1, t = 0.0;       /* Sun always below altit */
+      else if ( cost <= -1.0 )
+        rc = +1, t = 12.0;      /* Sun always above altit */
+      else
+        t = acosd(cost) / 15.0; /* The diurnal arc, hours */
+    }
+
+    /* Store rise and set times - in hours UT */
+    *trise = tsouth - t;
+    *tset  = tsouth + t;
+
+    return rc;
+  }  /* __sunriset__ */
+
+  /* The "workhorse" function */
+  double __daylen__( int year, int month, int day, double lon, double lat,
+                     double altit, int upper_limb )
+  /**********************************************************************/
+  /* Note: year,month,date = calendar date, 1801-2099 only.             */
+  /*       Eastern longitude positive, Western longitude negative       */
+  /*       Northern latitude positive, Southern latitude negative       */
+  /*       The longitude value is not critical. Set it to the correct   */
+  /*       longitude if you're picky, otherwise set to to, say, 0.0     */
+  /*       The latitude however IS critical - be sure to get it correct */
+  /*       altit = the altitude which the Sun should cross              */
+  /*               Set to -35/60 degrees for rise/set, -6 degrees       */
+  /*               for civil, -12 degrees for nautical and -18          */
+  /*               degrees for astronomical twilight.                   */
+  /*         upper_limb: non-zero -> upper limb, zero -> center         */
+  /*               Set to non-zero (e.g. 1) when computing day length   */
+  /*               and to zero when computing day+twilight length.      */
+  /**********************************************************************/
+  {
+    double  d,  /* Days since 2000 Jan 0.0 (negative before) */
+            obl_ecl,    /* Obliquity (inclination) of Earth's axis */
+            sr,         /* Solar distance, astronomical units */
+            slon,       /* True solar longitude */
+            sin_sdecl,  /* Sine of Sun's declination */
+            cos_sdecl,  /* Cosine of Sun's declination */
+            sradius,    /* Sun's apparent radius */
+            t;          /* Diurnal arc */
+
+    /* Compute d of 12h local mean solar time */
+    d = days_since_2000_Jan_0(year, month, day) + 0.5 - lon / 360.0;
+
+    /* Compute obliquity of ecliptic (inclination of Earth's axis) */
+    obl_ecl = 23.4393 - 3.563E-7 * d;
+
+    /* Compute Sun's ecliptic longitude and distance */
+    sunpos( d, &slon, &sr );
+
+    /* Compute sine and cosine of Sun's declination */
+    sin_sdecl = sind(obl_ecl) * sind(slon);
+    cos_sdecl = sqrt( 1.0 - sin_sdecl * sin_sdecl );
+
+    /* Compute the Sun's apparent radius, degrees */
+    sradius = 0.2666 / sr;
+
+    /* Do correction to upper limb, if necessary */
+    if ( upper_limb )
+      altit -= sradius;
+
+    /* Compute the diurnal arc that the Sun traverses to reach */
+    /* the specified altitude altit: */
+    {
+      double cost;
+      cost = ( sind(altit) - sind(lat) * sin_sdecl ) /
+             ( cosd(lat) * cos_sdecl );
+      if ( cost >= 1.0 )
+        t = 0.0;                      /* Sun always below altit */
+      else if ( cost <= -1.0 )
+        t = 24.0;                     /* Sun always above altit */
+      else  t = (2.0 / 15.0) * acosd(cost); /* The diurnal arc, hours */
+    }
+    return t;
+  }  /* __daylen__ */
+
+  /* This function computes the Sun's position at any instant */
+  void sunpos( double d, double * lon, double * r )
+  /******************************************************/
+  /* Computes the Sun's ecliptic longitude and distance */
+  /* at an instant given in d, number of days since     */
+  /* 2000 Jan 0.0.  The Sun's ecliptic latitude is not  */
+  /* computed, since it's always very near 0.           */
+  /******************************************************/
+  {
+    double M,         /* Mean anomaly of the Sun */
+           w,         /* Mean longitude of perihelion */
+           /* Note: Sun's mean longitude = M + w */
+           e,         /* Eccentricity of Earth's orbit */
+           E,         /* Eccentric anomaly */
+           x, y,      /* x, y coordinates in orbit */
+           v;         /* True anomaly */
+
+    /* Compute mean elements */
+    M = revolution( 356.0470 + 0.9856002585 * d );
+    w = 282.9404 + 4.70935E-5 * d;
+    e = 0.016709 - 1.151E-9 * d;
+
+    /* Compute true longitude and radius vector */
+    E = M + e * RADEG * sind(M) * ( 1.0 + e * cosd(M) );
+    x = cosd(E) - e;
+    y = sqrt( 1.0 - e * e ) * sind(E);
+    *r = sqrt( x * x + y * y );          /* Solar distance */
+    v = atan2d( y, x );                  /* True anomaly */
+    *lon = v + w;                        /* True solar longitude */
+    if ( *lon >= 360.0 )
+      *lon -= 360.0;                   /* Make it 0..360 degrees */
+  }
+
+  void sun_RA_dec( double d, double * RA, double * dec, double * r )
+  /******************************************************/
+  /* Computes the Sun's equatorial coordinates RA, Decl */
+  /* and also its distance, at an instant given in d,   */
+  /* the number of days since 2000 Jan 0.0.             */
+  /******************************************************/
+  {
+    double lon, obl_ecl, x, y, z;
+
+    /* Compute Sun's ecliptical coordinates */
+    sunpos( d, &lon, r );
+
+    /* Compute ecliptic rectangular coordinates (z=0) */
+    x = *r * cosd(lon);
+    y = *r * sind(lon);
+
+    /* Compute obliquity of ecliptic (inclination of Earth's axis) */
+    obl_ecl = 23.4393 - 3.563E-7 * d;
+
+    /* Convert to equatorial rectangular coordinates - x is unchanged */
+    z = y * sind(obl_ecl);
+    y = y * cosd(obl_ecl);
+
+    /* Convert to spherical coordinates */
+    *RA = atan2d( y, x );
+    *dec = atan2d( z, sqrt(x * x + y * y) );
+
+  }  /* sun_RA_dec */
+
+  /******************************************************************/
+  /* This function reduces any angle to within the first revolution */
+  /* by subtracting or adding even multiples of 360.0 until the     */
+  /* result is >= 0.0 and < 360.0                                   */
+  /******************************************************************/
 #define INV360    ( 1.0 / 360.0 )
 
-double revolution( double x )
-/*****************************************/
-/* Reduce angle to within 0..360 degrees */
-/*****************************************/
-{
-  return ( x - 360.0 * floor( x * INV360 ) );
-}  /* revolution */
-
-double rev180( double x )
-/*********************************************/
-/* Reduce angle to within +180..+180 degrees */
-/*********************************************/
-{
-  return ( x - 360.0 * floor( x * INV360 + 0.5 ) );
-}  /* revolution */
-
-
-/*******************************************************************/
-/* This function computes GMST0, the Greenwich Mean Sidereal Time  */
-/* at 0h UT (i.e. the sidereal time at the Greenwhich meridian at  */
-/* 0h UT).  GMST is then the sidereal time at Greenwich at any     */
-/* time of the day.  I've generalized GMST0 as well, and define it */
-/* as:  GMST0 = GMST - UT  --  this allows GMST0 to be computed at */
-/* other times than 0h UT as well.  While this sounds somewhat     */
-/* contradictory, it is very practical:  instead of computing      */
-/* GMST like:                                                      */
-/*                                                                 */
-/*  GMST = (GMST0) + UT * (366.2422/365.2422)                      */
-/*                                                                 */
-/* where (GMST0) is the GMST last time UT was 0 hours, one simply  */
-/* computes:                                                       */
-/*                                                                 */
-/*  GMST = GMST0 + UT                                              */
-/*                                                                 */
-/* where GMST0 is the GMST "at 0h UT" but at the current moment!   */
-/* Defined in this way, GMST0 will increase with about 4 min a     */
-/* day.  It also happens that GMST0 (in degrees, 1 hr = 15 degr)   */
-/* is equal to the Sun's mean longitude plus/minus 180 degrees!    */
-/* (if we neglect aberration, which amounts to 20 seconds of arc   */
-/* or 1.33 seconds of time)                                        */
-/*                                                                 */
-/*******************************************************************/
-
-double GMST0( double d )
-{
-  double sidtim0;
-  /* Sidtime at 0h UT = L (Sun's mean longitude) + 180.0 degr  */
-  /* L = M + w, as defined in sunpos().  Since I'm too lazy to */
-  /* add these numbers, I'll let the C compiler do it for me.  */
-  /* Any decent C compiler will add the constants at compile   */
-  /* time, imposing no runtime or code overhead.               */
-  sidtim0 = revolution( ( 180.0 + 356.0470 + 282.9404 ) +
-                        ( 0.9856002585 + 4.70935E-5 ) * d );
-  return sidtim0;
-}  /* GMST0 */
+  double revolution( double x )
+  /*****************************************/
+  /* Reduce angle to within 0..360 degrees */
+  /*****************************************/
+  {
+    return ( x - 360.0 * floor( x * INV360 ) );
+  }  /* revolution */
+
+  double rev180( double x )
+  /*********************************************/
+  /* Reduce angle to within +180..+180 degrees */
+  /*********************************************/
+  {
+    return ( x - 360.0 * floor( x * INV360 + 0.5 ) );
+  }  /* revolution */
+
+
+  /*******************************************************************/
+  /* This function computes GMST0, the Greenwich Mean Sidereal Time  */
+  /* at 0h UT (i.e. the sidereal time at the Greenwhich meridian at  */
+  /* 0h UT).  GMST is then the sidereal time at Greenwich at any     */
+  /* time of the day.  I've generalized GMST0 as well, and define it */
+  /* as:  GMST0 = GMST - UT  --  this allows GMST0 to be computed at */
+  /* other times than 0h UT as well.  While this sounds somewhat     */
+  /* contradictory, it is very practical:  instead of computing      */
+  /* GMST like:                                                      */
+  /*                                                                 */
+  /*  GMST = (GMST0) + UT * (366.2422/365.2422)                      */
+  /*                                                                 */
+  /* where (GMST0) is the GMST last time UT was 0 hours, one simply  */
+  /* computes:                                                       */
+  /*                                                                 */
+  /*  GMST = GMST0 + UT                                              */
+  /*                                                                 */
+  /* where GMST0 is the GMST "at 0h UT" but at the current moment!   */
+  /* Defined in this way, GMST0 will increase with about 4 min a     */
+  /* day.  It also happens that GMST0 (in degrees, 1 hr = 15 degr)   */
+  /* is equal to the Sun's mean longitude plus/minus 180 degrees!    */
+  /* (if we neglect aberration, which amounts to 20 seconds of arc   */
+  /* or 1.33 seconds of time)                                        */
+  /*                                                                 */
+  /*******************************************************************/
+
+  double GMST0( double d )
+  {
+    double sidtim0;
+    /* Sidtime at 0h UT = L (Sun's mean longitude) + 180.0 degr  */
+    /* L = M + w, as defined in sunpos().  Since I'm too lazy to */
+    /* add these numbers, I'll let the C compiler do it for me.  */
+    /* Any decent C compiler will add the constants at compile   */
+    /* time, imposing no runtime or code overhead.               */
+    sidtim0 = revolution( ( 180.0 + 356.0470 + 282.9404 ) +
+                          ( 0.9856002585 + 4.70935E-5 ) * d );
+    return sidtim0;
+  }  /* GMST0 */

  int month = monthS.toInt();
  String dayS = timeS.substring(8, 10);
  int day = dayS.toInt();
  
  timeS = timeS.substring(length - 8, length - 6); // Strip out the hours
  int time = timeS.toInt();

#ifdef CONVERTTIMETOLOCAL
  // For some reason, time is off by some (???) hours from UTC. Need to compensate
  int TimeErrorOffset = -3;
  if (((time > 18) && (time < 21)) ||
      (time == 12) ||
      (time == 15)) {
    time += (TimeErrorOffset + 2);
  }
  else if (time == 0) {
    time += (TimeErrorOffset + 0);
  }
  else {
    time += TimeErrorOffset;

  // Convert UTC time & date to local time & date
  bool DST = convertToLocal(&time, &year, &month,
                            &day, (double)longitude.toFloat(), true); // true means date and DST conversion

#endif

  *monthI = month;
