   // 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;

  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;

  return (DST);
}

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 */
