   return (DOW);
 }
 
-  /*
-    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                                   */
-  /******************************************************************/
+/*
+ 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 */

String result;
bool night = false;
bool toggleDisplay = HIGH;
bool pastToggleDisplay = toggleDisplay;

Adafruit_ST7735 tft(TFT_CS, TFT_DC, TFT_RST);


    return;
  }

  // Not sure why this is needed.  It works fine without it
  // while (client.connected() && !client.available()) delay(1); //waits for data

#ifdef DEBUG
  Serial.println("Waiting for data");
#endif

  while (client.connected() && client.available()) { // While connected
    char c = client.read(); // Gets byte from WIFI buffer
    result = result + c;
  }

