Commit 3351be22 authored by Wei Chengliang's avatar Wei Chengliang
Browse files

update codestyle-PEP8

parent 8fd9723d
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+1 −1
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@@ -98,7 +98,7 @@ class Quasar(MockObject):
        del self.sed

    def getGSObj(self, psf, g1=0, g2=0, flux=None, filt=None, tel=None, exptime=150.):
        if flux == None:
        if flux is None:
            flux = self.getElectronFluxFilt(filt, tel, exptime)
        qso = galsim.Gaussian(sigma=1.e-8, flux=1.)
        qso = qso.withFlux(flux)
+1 −1
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@@ -21,7 +21,7 @@ class Stamp(MockObject):
        del self.sed

    def drawObj_multiband(self, tel, pos_img, psf_model, bandpass_list, filt, chip, nphotons_tot=None, g1=0, g2=0, exptime=150., fd_shear=None):
        if nphotons_tot == None:
        if nphotons_tot is None:
            nphotons_tot = self.getElectronFluxFilt(filt, tel, exptime)

        try:
+2 −2
Original line number Diff line number Diff line
@@ -22,7 +22,7 @@ class Star(MockObject):
        del self.sed

    def getGSObj(self, psf, g1=0, g2=0, flux=None, filt=None, tel=None, exptime=150.):
        if flux == None:
        if flux is None:
            flux = self.getElectronFluxFilt(filt, tel, exptime)
        # star = galsim.Gaussian(sigma=1.e-8, flux=1.)
        star = galsim.DeltaFunction()
@@ -35,7 +35,7 @@ class Star(MockObject):
            raise ValueError(
                "!!!The number of PSF profiles and the number of bandpasses must be equal.")
        objs = []
        if nphotons_tot == None:
        if nphotons_tot is None:
            nphotons_tot = self.getElectronFluxFilt(filt, tel, exptime)

        try:
+2 −2
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@@ -428,8 +428,8 @@ class TestSpecDisperse(unittest.TestCase):
        plt.xlim(6200, 10000)
        plt.ylim(1, 4)
        plt.yscale('log')
        plt.xlabel('$\lambda$')
        plt.ylabel('$F\lambda$')
        plt.xlabel(r'$\lambda$')
        plt.ylabel(r'$F\lambda$')
        plt.legend(['one spec', 'split in 8000 A'])
        plt.show()

+1 −1
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@@ -192,7 +192,7 @@ class TestStraylight(unittest.TestCase):
        plt.figure()
        plt.plot(spec['WAVELENGTH'], spec['FLUX'], 'r')
        plt.xlabel('WAVELENGTH')
        plt.ylabel('F$\lambda$(erg/s/cm2/A/arcsec2)')
        plt.ylabel(r'F$\lambda$(erg/s/cm2/A/arcsec2)')
        plt.xlim(2000, 10000)
        plt.show()
        median = np.median(sl_e_pix[0:tnum])
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