f3/photometry.py
def define_spotsignal(self):
        """
        Identify the "expected" flux value at the time of each observation based on the 
        Kepler long-cadence data, to ensure variations observed are not the effects of a single
        large starspot. Only works if the target star was targeted for long or short cadence
        observations during the primary mission.
        """
        client = kplr.API()
        star = client.star(self.kic)

        lcs = star.get_light_curves(short_cadence=False)
        time, flux, ferr, qual = [], [], [], []
        for lc in lcs:
            with lc.open() as f:
                hdu_data = f[1].data
                time.append(hdu_data["time"])
                flux.append(hdu_data["pdcsap_flux"])
                ferr.append(hdu_data["pdcsap_flux_err"])
                qual.append(hdu_data["sap_quality"])
            tout = np.array([])
            fout = np.array([])
            eout = np.array([])
            for i in range(len(flux)):
                t = time[i][qual[i] == 0]
                f = flux[i][qual[i] == 0]
                e = ferr[i][qual[i] == 0]

                t = t[np.isfinite(f)]
                e = e[np.isfinite(f)]
                f = f[np.isfinite(f)]

                e /= np.median(f)
                f /= np.median(f)
                tout = np.append(tout, t[50:]+54833)
                fout = np.append(fout, f[50:])
                eout = np.append(eout, e[50:])

            self.spot_signal = np.zeros(52)

            for i in range(len(self.times)):
                if self.times[i] < 55000:
                    self.spot_signal[i] = 1.0
                else:
                    self.spot_signal[i] = fout[np.abs(self.times[i] - tout) == np.min(np.abs(self.times[i] - tout))]
def define_spotsignal(self):
        """
        Identify the "expected" flux value at the time of each observation based on the 
        Kepler long-cadence data, to ensure variations observed are not the effects of a single
        large starspot. Only works if the target star was targeted for long or short cadence
        observations during the primary mission.
        """
        client = kplr.API()
        star = client.star(self.kic)

        lcs = star.get_light_curves(short_cadence=False)
        time, flux, ferr, qual = [], [], [], []
        for lc in lcs:
            with lc.open() as f:
                hdu_data = f[1].data
                time.append(hdu_data["time"])
                flux.append(hdu_data["pdcsap_flux"])
                ferr.append(hdu_data["pdcsap_flux_err"])
                qual.append(hdu_data["sap_quality"])
            tout = np.array([])
            fout = np.array([])
            eout = np.array([])
            for i in range(len(flux)):
                t = time[i][qual[i] == 0]
                f = flux[i][qual[i] == 0]
                e = ferr[i][qual[i] == 0]

                t = t[np.isfinite(f)]
                e = e[np.isfinite(f)]
                f = f[np.isfinite(f)]

                e /= np.median(f)
                f /= np.median(f)
                tout = np.append(tout, t[50:]+54833)
                fout = np.append(fout, f[50:])
                eout = np.append(eout, e[50:])

            self.spot_signal = np.zeros(52)

            for i in range(len(self.times)):
                if self.times[i] < 55000:
                    self.spot_signal[i] = 1.0
                else:
                    self.spot_signal[i] = fout[np.abs(self.times[i] - tout) == np.min(np.abs(self.times[i] - tout))]
def define_spotsignal ( self ) : client = kplr . API ( ) star = client . star ( self . kic ) lcs = star . get_light_curves ( short_cadence = False ) time , flux , ferr , qual = [ ] , [ ] , [ ] , [ ] for lc in lcs : with lc . open ( ) as f : hdu_data = f [ 1 ] . data time . append ( hdu_data [ "time" ] ) flux . append ( hdu_data [ "pdcsap_flux" ] ) ferr . append ( hdu_data [ "pdcsap_flux_err" ] ) qual . append ( hdu_data [ "sap_quality" ] ) tout = np . array ( [ ] ) fout = np . array ( [ ] ) eout = np . array ( [ ] ) for i in range ( len ( flux ) ) : t = time [ i ] [ qual [ i ] == 0 ] f = flux [ i ] [ qual [ i ] == 0 ] e = ferr [ i ] [ qual [ i ] == 0 ] t = t [ np . isfinite ( f ) ] e = e [ np . isfinite ( f ) ] f = f [ np . isfinite ( f ) ] e /= np . median ( f ) f /= np . median ( f ) tout = np . append ( tout , t [ 50 : ] + 54833 ) fout = np . append ( fout , f [ 50 : ] ) eout = np . append ( eout , e [ 50 : ] ) self . spot_signal = np . zeros ( 52 ) for i in range ( len ( self . times ) ) : if self . times [ i ] < 55000 : self . spot_signal [ i ] = 1.0 else : self . spot_signal [ i ] = fout [ np . abs ( self . times [ i ] - tout ) == np . min ( np . abs ( self . times [ i ] - tout ) ) ]
Identify the "expected" flux value at the time of each observation based on the 
        Kepler long-cadence data, to ensure variations observed are not the effects of a single
        large starspot. Only works if the target star was targeted for long or short cadence
        observations during the primary mission.
Identify the expected flux value at the time of each observation based on the Kepler long - cadence data to ensure variations observed are not the effects of a single large starspot . Only works if the target star was targeted for long or short cadence observations during the primary mission .