def recv(self):
if self.mode == SCUMode.SendMode:
raise Exception
key, length = self.file_received.get()
return utils.fold_data(self.received_files_data[key], length)
def get_cutout_phased_df(self,t0=None,P=None,dur=0.2,sigma=None,plot=True,use_median_filter=True):
"""
A function to get both transit cutout data, and also the final folded transit.
INPUT:
- t0
- P
- dur is the total duration of the data (i.e. if 0.2, then goes from -0.1 to 0.1)
- sigma
OUTPUT:
df with columns:
- x the phased folded time
- y flux value
- time original time value before folding
- index index of the original value before folding
EXAMPLE:
df = EP.get_cutout_phased_df(dur=0.4,sigma=3)
_, mm = k2help.savgol_sigma_clip(df.y,win=21,sigma_upper=3)
plt.plot(df.x, df.y,"r.")
dfmm = df[~mm]
t_fold_final = dfmm.x
f_fold_final = dfmm.y
plt.plot(t_fold_final,f_fold_final)
dfmm_s = dfmm.sort_index()
plt.plot(dfmm_s.x,dfmm_s.y,"r.")
plt.plot(dfmm.x,dfmm.y,"k.")
"""
if t0 is None and P is None:
t0 = self.planet._pl_tranmid - k2help.KEPLER_JD_OFFSET
P = self.planet._pl_orbper
print("Using planet with t0=",t0,"and P=",P)
if use_median_filter:
print("Using median filtered data -- assumes you have run that from beginning!")
t, f = self.t, self.f
else:
print("Using whitened flux")
t, f = self.star.get_whitened_flux()
m = np.isnan(f)
t, f = t[~m],f[~m]
ind = self.star.get_masked_indices_in_transit(t,t0,P,dur=dur)
t_unfolded, f_unfolded = t[ind], f[ind]
df = utils.fold_data(t_unfolded,f_unfolded,t0,P,dur=dur,sort=True)
if sigma is not None:
S=astropy.stats.sigma_clipping.sigma_clip(df.y.values)
dfm = df[~S.mask]
if plot:
fig, ax = plt.subplots()
ax.plot(df.x,df.y,"r.",label="folded data")
if sigma is not None:
ax.plot(dfm.x,dfm.y,"k.",label="sigma clipped")
ax.legend(loc="upper right",fontsize=12)
if sigma is not None:
return dfm
else:
return df