Coverage for python/lsst/sims/utils/m5_flat_sed.py : 19%

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"""Calculate the m5 value, using photometric scaling. Note, does not include shape of the object SED.
Parameters ---------- visitFilter : str One of u,g,r,i,z,y musky : float Surface brightness of the sky in mag/sq arcsec FWHMeff : float The seeing effective FWHM (arcsec) expTime : float Exposure time for the entire visit in seconds airmass : float Airmass of the observation (unitless) tauCloud : float (0.) Any extinction from clouds in magnitudes (positive values = more extinction)
Output ------ m5 : float The five-sigma limiting depth of a point source observed in the given conditions. """
# Set up expected extinction (kAtm) and m5 normalization values (Cm) for each filter. # The Cm values must be changed when telescope and site parameters are updated. # # These values are calculated using $SYSENG_THROUGHPUTS/python/calcM5.py. # This set of values are calculated using v1.2 of the SYSENG_THROUGHPUTS repo.
# Only define the dicts once on initial call if not hasattr(m5_flat_sed, 'Cm'): m5_flat_sed.Cm = {'u': 23.067, 'g': 24.414, 'r': 24.439, 'i': 24.325, 'z': 24.157, 'y': 23.730} m5_flat_sed.dCm_infinity = {'u': 0.631, 'g': 0.179, 'r': 0.097, 'i': 0.071, 'z': 0.048, 'y': 0.037} m5_flat_sed.kAtm = {'u': 0.492, 'g': 0.213, 'r': 0.126, 'i': 0.096, 'z': 0.069, 'y': 0.170} m5_flat_sed.msky = {'u': 22.989, 'g': 22.256, 'r': 21.196, 'i': 20.478, 'z': 19.600, 'y': 18.612} # Calculate adjustment if readnoise is significant for exposure time # (see overview paper, equation 7) Tscale = expTime / 30.0 * np.power(10.0, -0.4 * (musky - m5_flat_sed.msky[visitFilter])) dCm = 0. dCm += m5_flat_sed.dCm_infinity[visitFilter] dCm -= 1.25 * np.log10(1 + (10**(0.8 * m5_flat_sed.dCm_infinity[visitFilter]) - 1)/Tscale) # Calculate fiducial m5 m5 = (m5_flat_sed.Cm[visitFilter] + dCm + 0.50 * (musky - 21.0) + 2.5 * np.log10(0.7 / FWHMeff) + 1.25 * np.log10(expTime / 30.0) - m5_flat_sed.kAtm[visitFilter] * (airmass - 1.0) - 1.1 * tauCloud)
return m5 |