Source code for lightcurvelynx.astro_utils.obs_utils

import numpy as np


[docs] def phot_eff_function(snr): """ Photometric detection efficiency as a simple step function of snr. Parameters ---------- snr: list or numpy.ndarray Signal to noise ratio of a list of observations. Returns ------- eff: list or numpy.ndarray The photometric detection efficiency given snr. """ snr = np.array(snr) eff = np.where(snr > 5, 1.0, 0.0) return eff
[docs] def spec_eff_function(peak_imag): """ Spectroscopic follow-up efficiency as a function of peak i band magnitude. Parameters ---------- peak_imag: list or numpy.ndarray Peak magnitude in i band. Returns ------- eff: list or numpy.ndarray The spectroscopic efficiency given peak i band magnitude. Based on Equation (17) in Kessler et al. 2019 s0, s1, s2 are fitted using data from Figure 4 in Kessler et al. 2019 """ s0 = 1.0 s1 = 2.36 s2 = 51.9 peak_imag = np.array(peak_imag) eff = s0 * np.power((1.0 + np.exp(s1 * peak_imag - s2)), -1) return eff