def process(infile, coords, method, inner_radius, outer_radius, cen_method,
window_size, output, zmag, avg):
"""
Entry point function to process science image.
Parameters
----------
infile : string
Science image or list of science images
coords : string
Input text file with coordinates of stars
method : string
FWHM of the stelar psf in pixels
inner_radius : float
Sky background sigma
outer_radius : int
Inner sky annulus radius in pixels
cen_method : string
Centroid method
window_size : int
Centroid finding window size in pixels
output : string
Output file name
zmag : float
Photometric zero point
Returns
-------
None
"""
print("FASTPHOT: CHIMERA Fast Aperture Photometry Routine")
inner_radius = float(inner_radius)
outer_radius = float(outer_radius)
# Check if input is a string of FITS images or a text file with file names
if infile[0] == "@":
infile = infile[1:]
if not os.path.exists(infile):
print("REGISTER: Not able to locate file %s" % infile)
image_cubes = []
with open(infile, "r") as fd:
for line in fd.readlines():
if len(line) > 1:
image_cubes.append(line.replace("\n", ""))
else:
image_cubes = infile.split(",")
# Number of images
ncubes = len(image_cubes)
pos = np.loadtxt(coords, ndmin=2)
nstars = len(pos)
total_phot_data = []
for i in range(ncubes):
sci_file = image_cubes[i]
print(" Processing science image %s" % sci_file)
# Read FITS image and star coordinate
image = chimera.fitsread(sci_file)
if avg != "":
image = time_average(image, avg)
avg = int(avg)
else:
avg = 1
# Instantiate an Aperphot object
ap = chimera.Aperphot(sci_file, coords)
# Set fwhmpsf, sigma, annulus, dannulus and zmag
ap.method = method
ap.inner_radius = inner_radius
ap.outer_radius = outer_radius
if zmag != "":
ap.zmag = float(zmag)
# Determine nominal aperture radius for photometry
if i == 0:
nom_aper = ap.cog(window_size, cen_method)
#nom_aper = 3
print(" Nominal aperture radius : %4.1f pixels" % nom_aper)
# Perform aperture photometry on all the frames
dtype = [("DATETIME", "S25"), ("XCEN", "f4"), ("YCEN", "f4"),
("MSKY", "f8"), ("NSKY", "f8"), ("AREA", "f8"),
("FLUX_ADU", "f8"), ("FLUX_ELEC", "f8"), ("FERR", "f8"),
("MAG", "f8")]
phot_data = np.zeros([nstars, ap.nframes / avg], dtype=dtype)
for j in range(ap.nframes / avg):
print(" Processing frame number : %d" % (j + 1))
objpos = chimera.recenter(image[j, :, :], pos, window_size,
cen_method)
aperphot_data = ap.phot(image[j, :, :], objpos, nom_aper)
pos = np.copy(objpos)
phot_data[:, j]['DATETIME'] = ap.addtime(j * avg *
ap.kintime).isoformat()
phot_data[:, j]['XCEN'] = aperphot_data["xcenter_raw"]
phot_data[:, j]['YCEN'] = aperphot_data["ycenter_raw"]
phot_data[:, j]['MSKY'] = aperphot_data["msky"]
phot_data[:, j]['NSKY'] = aperphot_data["nsky"]
phot_data[:, j]['AREA'] = aperphot_data["area"]
phot_data[:, j]['FLUX_ADU'] = aperphot_data["flux"]
phot_data[:,
j]['FLUX_ELEC'] = phot_data[:, j]['FLUX_ADU'] * ap.epadu
phot_data[:, j]['MAG'] = ap.zmag - 2.5 * np.log10(
phot_data[:, j]['FLUX_ELEC'] / (ap.exptime))
# Calculate error in flux - using the formula
# err = sqrt(flux * gain + npix * (1 + (npix/nsky)) * (flux_sky * gain + R**2))
phot_data[:, j]['FERR'] = np.sqrt(
phot_data[:, j]['FLUX_ELEC'] + phot_data[:, j]['AREA'] *
(1 + phot_data[:, j]['AREA'] / phot_data[:, j]['NSKY']) *
(phot_data[:, j]['MSKY'] * ap.epadu + ap.readnoise**2))
total_phot_data.append(phot_data)
# Save photometry data in numpy binary format
print(" Saving photometry data as numpy binary")
if output != "":
npy_outfile = output + ".npy"
else:
npy_outfile = sci_file.replace(".fits", ".phot.npy")
if os.path.exists(npy_outfile):
os.remove(npy_outfile)
#np.save(npy_outfile, phot_data)
'''
# Plot first pass light curve
if plot_flag:
print " Plotting normalized light curve"
if output != "":
plt_outfile = output + ".png"
else:
plt_outfile = sci_file.replace(".fits", ".lc.png")
plotter(phot_data, ap.nframes, ap.kintime, plt_outfile)
'''
# Convert the total_phot_data to array and reshape it
print(' Saving consolidated photometry data...')
total_phot_data_arr = np.concatenate(total_phot_data, axis=1)
# Save the array as npy file
if output != "":
np.save(output + "phot_total.npy", total_phot_data_arr)
else:
np.save("phot_total.npy", total_phot_data_arr)
return
def process(infile, coords, fwhmpsf, sigma, aperture, annulus, dannulus,
output, zmag, debug):
"""
Entry point function to process science image.
Parameters
----------
infile : string
Science image or list of science images
coords : string
Input text file with coordinates of stars
fwhmpsf : float
FWHM of the stelar psf in pixels
sigma : float
Sky background sigma
annulus : int
Inner sky annulus radius in pixels
dannulus : int
Radius of sky annulus in pixels
output : string
Output file name
zmag : string
Photometric zero point
Returns
-------
None
"""
print("PHOTOMETRY: CHIMERA Aperture Photometry Routine")
fwhmpsf = float(fwhmpsf)
sigma = float(sigma)
annulus = int(annulus)
dannulus = int(dannulus)
# Check if input is a string of FITS images or a text file with file names
if infile[0] == "@":
infile = infile[1:]
if not os.path.exists(infile):
raise IOError("PHOTOMETRY: Not able to locate file %s. Stopping." %
infile)
image_cubes = []
with open(infile, "r") as fd:
for line in fd.readlines():
if len(line) > 1:
image_cubes.append(line.replace("\n", ""))
else:
image_cubes = infile.split(",")
# Number of images
ncubes = len(image_cubes)
# Check if the input coordinates file exists. Take a tmp copy of the input
# file and use that. Delete at the end of processing.
if not os.path.exists(coords):
raise IOError("Input coordinate file %s does not exist. Stopping." %
coords)
else:
tmp_coords = coords + ".tmp"
iraf.copy(coords, tmp_coords)
# Fields to extract from phot file
fields = "XCEN,YCEN,CIER,MSKY,STDEV,NSKY,SIER,SUM,AREA,FLUX,MERR,PIER"
total_phot_data = []
img_sec = []
for i in range(ncubes):
sci_file = image_cubes[i]
if not os.path.exists(sci_file):
raise IOError("FITS image %s does not exist. Stopping." % sci_file)
fpath, fname = os.path.split(sci_file)
print("\n Processing science image %s" % fname)
# Instantiate an Aperphot object
ap = chimera.Aperphot(sci_file, coords)
# Set fwhmpsf, sigma, annulus. dannulus and zero point
ap.fwhmpsf = fwhmpsf
ap.sigma = sigma
ap.annulus = annulus
ap.dannulus = dannulus
if zmag != "":
ap.zmag = float(zmag)
# Read the input FITS image
if i == 0:
img, imghdr = chimera.fitsread(ap.sci_file, header=True)
else:
img = chimera.fitsread(ap.sci_file)
# Determine nominal aperture radius for photometry
if i == 0:
if aperture:
nom_aper = float(aperture)
else:
nom_aper = ap.daocog()
print(" Nominal aperture radius : %4.1f pixels" % nom_aper)
# Perform aperture photometry on all the frames
dtype = [
("DATETIME", "S25"),
("XCEN", "f4"),
("YCEN", "f4"),
("CIER", "i4"),
("MSKY", "f4"),
("STDEV", "f4"),
("NSKY", "i4"),
("SIER", "i4"),
("SUM", "f4"),
("AREA", "f4"),
("FLUX_ADU", "f4"),
("FLUX_ELEC", "f4"),
("FERR", "f4"),
("MAG", "f4"),
("MERR", "f4"),
("PIER", "i4"),
]
phot_data = np.zeros([ap.nframes], dtype=dtype)
for j in range(ap.nframes):
print(" Processing frame number : %d" % (j + 1))
outfile = sci_file.replace(".fits", "_" + str(j) + ".phot.1")
ap.daophot(j + 1, tmp_coords, outfile, nom_aper)
objcen = dump(outfile, "XCEN,YCEN")
with open(tmp_coords, "w") as fd:
fd.write(objcen + '\n')
aperphot_data = dump(outfile, fields).split()
phot_data[j]['DATETIME'] = ap.addtime(j * ap.kintime).isoformat()
phot_data[j]['XCEN'] = float(aperphot_data[0])
phot_data[j]['YCEN'] = float(aperphot_data[1])
phot_data[j]['CIER'] = int(aperphot_data[2])
phot_data[j]['MSKY'] = float(aperphot_data[3])
phot_data[j]['STDEV'] = float(aperphot_data[4])
phot_data[j]['NSKY'] = int(aperphot_data[5])
phot_data[j]['SIER'] = int(aperphot_data[6])
phot_data[j]['SUM'] = float(aperphot_data[7])
phot_data[j]['AREA'] = float(aperphot_data[8])
phot_data[j]['FLUX_ADU'] = float(aperphot_data[9])
phot_data[j]['FLUX_ELEC'] = float(aperphot_data[9]) * ap.epadu
phot_data[j]['MAG'] = ap.zmag - 2.5 * np.log10(
phot_data[j]['FLUX_ELEC'] / ap.exptime)
if aperphot_data[10] == 'INDEF':
phot_data[j]['MERR'] = -10
else:
phot_data[j]['MERR'] = float(aperphot_data[10])
phot_data[j]['PIER'] = int(aperphot_data[11])
# Calculate error in flux - using the formula
# err = sqrt(flux * gain + npix * (1 + (npix/nsky)) * (flux_sky * gain + R**2))
phot_data[j]['FERR'] = np.sqrt(
phot_data[j]['FLUX_ELEC'] + phot_data[j]['AREA'] *
(1 + phot_data[j]['AREA'] / phot_data[j]['NSKY']) *
(phot_data[j]['MSKY'] * ap.epadu + ap.readnoise**2))
# Save a 51x51 image section of the object
xmin, xmax = int(phot_data[j]['XCEN']) - 25, int(
phot_data[j]['XCEN']) + 25
ymin, ymax = int(phot_data[j]['YCEN']) - 25, int(
phot_data[j]['YCEN']) + 25
img_sec.append(img[j, ymin:ymax, xmin:xmax])
# Save photometry of all the image cubes in a single file
total_phot_data.append(phot_data)
# If debug mode -
# 1. save DAOPHOT phot files
# 2. save individual phot data as npy file
# 3. Plot light cuve for each data cube separatly
if debug:
# Save photometry data in numpy binary format
print(" Saving photometry data as numpy binary")
if output != "":
npy_outfile = output + ".npy"
else:
npy_outfile = coords + "_phot.npy"
if os.path.exists(npy_outfile):
os.remove(npy_outfile)
np.save(npy_outfile, phot_data)
# Plot first pass light curve
if plot_flag:
print(" Plotting normalized light curve")
if output != "":
plt_outfile = output + ".png"
else:
plt_outfile = coords + "_lc.png"
plotter(phot_data, ap.nframes, ap.kintime, plt_outfile)
else:
# Delete intermediate files is not debug mode
iraf.delete(os.path.join(fpath, '*.phot.1'))
# Convert the total_phot_data to array and reshape it
print(' Saving consolidated photometry data...')
total_phot_data_arr = np.concatenate(total_phot_data)
# Save the array as npy file
np.save(coords + "_total.phot.npy", total_phot_data_arr)
# Save the image section with object as FITS file
print(' Saving image section with object as FITS image...')
img_sec_arr = np.asarray(img_sec)
img_fname = coords + "_obj.fits"
if os.path.exists(img_fname):
os.remove(img_fname)
chimera.fitswrite(img_sec_arr, coords + "_obj.fits", header=imghdr)
# Delete temporary coordinate file
if os.path.exists(tmp_coords):
os.remove(tmp_coords)
return