# which sets the ORAC_INSTRUMENT environment variable to 'SCUBA2_450' or 'SCUBA2_850'
# else default to 850 band
band = os.getenv("ORAC_INSTRUMENT")
if band == None:
print "ORAC_INSTRUMENT environment variable not set!"
print "This program expects to be run from a shell"
print "prepared with the command: oracdr_scuba2_<band> <observation-date>"
print "where band is: 450 or 850"
print "and observation-date has the form: YYYYMMDD"
sys.exit(0)
# print "band={0}".format(band)
# Get WNFACT value and nFrames from data file
wnfact = float(starutil.get_fits_header(indata, "WNFACT"))
# print "wnfact={0}".format(wnfact)
nFrames = int(starutil.get_fits_header(indata, "MIRSTOP")) + 1
# print "nFrames={0}".format(nFrames)
# Gather statistics on the central region of the input spectrum
# We are interested in the z position of the maximum pixel value (peak)
instats = invoke("$KAPPA_DIR/stats ndf={0} quiet".format(indata))
maxpos = starutil.get_task_par("MAXPOS", "stats")
maxposz = maxpos[2]
# print "maxposz={0}".format(maxposz)
# Calculate the band pass frames centered on the peak
if band == "SCUBA2_850":
wnlbound = 11.2
wnubound = 12.2
# line.
parsys = ParSys( params )
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the template POL2 data files. They should be supplied as the first
# item on the command line, in the form of a Starlink "group expression"
# (i.e.the same way they are supplied to other SMURF commands such as
# makemap). Quote the string so that it can be used as command line
# argument when running an atask from the shell.
indata = parsys["IN"].value
# AZ/EL pointing correction, for pre 20150929 data.
if int(starutil.get_fits_header( indata[0], "UTDATE", True )) < 20150929:
pntfile = os.path.join(NDG.tempdir,"pointing")
fd = open(pntfile,"w")
fd.write("# system=azel\n")
fd.write("# tai dlon dlat\n")
fd.write("54000 32.1 27.4\n")
fd.write("56000 32.1 27.4\n")
fd.close()
else:
pntfile = "!"
# Are we inheriting noise from the input (real) time-streams, rather
# than generating artificial noise?
addon = parsys["ADDON"].value
# Common mode files.
# Get the name of the output NDF. If not supplied, use the name of hte
# input NDF.
outndf = parsys["OUT"].value
if outndf == None:
outndf = inndf
# See how the output NDFs are to be trimmed.
trim = parsys["TRIM"].value
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# See if the supplied NDF holds data from a JCMT instrument by looking at the
# "INSTRUME", "BACKEND" and "FILTER" FITS headers.
instrument = None
cval = starutil.get_fits_header( inndf, "INSTRUME" )
if cval == "SCUBA-2":
cval = starutil.get_fits_header( inndf, "FILTER" )
if cval == "450":
instrument = "SCUBA-2(450)"
elif cval == "850":
instrument = "SCUBA-2(850)"
else:
cval = starutil.get_fits_header( inndf, "BACKEND" )
if cval == "ACSIS":
instrument = "ACSIS"
# Form the polarised intensity map (no de-biassing), and remove the
# spectral axis.
tmp1 = NDG( 1 )
invoke( "$KAPPA_DIR/maths exp=\"'sqrt(ia**2+ib**2)'\" ia={0} ib={1} out={2}"
.format(qmap,umap,tmp1) )
pimap = NDG( 1 )
invoke( "$KAPPA_DIR/ndfcopy in={0} out={1} trim=yes".format(tmp1,pimap) )
# Find the position of the source centre in sky coords within the polarised
# intensity map.
invoke("$KAPPA_DIR/centroid ndf={0} mode=int init=\"'0,0'\"".format(pimap) )
xcen = get_task_par( "xcen", "centroid" )
ycen = get_task_par( "ycen", "centroid" )
# Get the elevation at the middle of the observation.
el1 = float( get_fits_header( qmap, "ELSTART" ) )
el2 = float( get_fits_header( qmap, "ELEND" ) )
el = 0.5*( el1 + el2 )
elist.append( el )
# Get the azimuth at the middle of the observation.
az1 = float( get_fits_header( qmap, "AZSTART" ) )
az2 = float( get_fits_header( qmap, "AZEND" ) )
az = 0.5*( az1 + az2 )
alist.append( az )
# Get the WVM tau at the middle of the observation.
w1 = float( get_fits_header( qmap, "WVMTAUST" ) )
w2 = float( get_fits_header( qmap, "WVMTAUEN" ) )
w = 0.5*( w1 + w2 )
wvmlist.append( w )
fd.write("flagslow=0.01\n")
fd.write("downsampscale=0\n")
fd.close()
# If both QREF and UREF were supplied, we will be rotating the
# polarimetric reference direction. So store the orignal maps in
# intermediate NDFs rather than the final NDFs.
if qref and uref:
tqmap = NDG(1)
tumap = NDG(1)
else:
tqmap = qmap
tumap = umap
# AZ/EL pointing correction, for data between 20150606 and 20150930.
ut = int(starutil.get_fits_header( qts[0], "UTDATE", True ))
if ut >= 20150606 and ut <= 20150929:
pntfile = os.path.join(NDG.tempdir,"pointing")
fd = open(pntfile,"w")
fd.write("# system=azel\n")
fd.write("# tai dlon dlat\n")
fd.write("54000 32.1 27.4\n")
fd.write("56000 32.1 27.4\n")
fd.close()
else:
pntfile = "!"
# Make a map from the Q time series.
msg_out( "Making a map from the Q time series...")
if qref:
ref = qref
os._exit(1)
# To be a group expression, it must contain at least one of the
# following characters: ^,= (NDFs are not allowed any of these).
gexp_chars = set( '^=,' )
if any( (c in gexp_chars) for c in config1 ):
isndf1 = False
else:
isndf1 = True
# If it is an NDF, attempt to get the FILTER or SUBARRAY fits header,
# and determine the waveband. If neither header is found, look for
# "s4a", etc, in the NDF's provenance info.
if isndf1:
try:
subarray = starutil.get_fits_header( config1, "SUBARRAY" )
if subarray is None:
filter = starutil.get_fits_header( config1, "FILTER" )
if filter is not None:
filter = filter.strip()
if filter == "450":
subarray = "s4"
elif filter == "850":
subarray = "s8"
if subarray is None:
text = starutil.invoke( "$KAPPA_DIR/provshow {0}".format(config1) )
if "s4a" in text or "s4b" in text or "s4c" in text or "s4d" in text:
subarray = "s4"
elif "s8a" in text or "s8b" in text or "s8c" in text or "s8d" in text:
subarray = "s8"
fd.write("modelorder=(pca,ext,ast,noi)\n")
fd.write("noisecliphigh=3\n")
fd.write("numiter=-20\n")
fd.write("pca.pcathresh=4\n")
fd.write("spikebox=10\n")
fd.write("spikethresh=5\n")
# Now put in values that are absolutely required by this script. These
# over-write any values in the user-supplied config.
fd.write("noi.usevar=1\n")
fd.write("flagslow=0.01\n")
fd.write("downsampscale=0\n")
fd.close()
# AZ/EL pointing correction, for data between 20150606 and 20150930.
ut = int(starutil.get_fits_header( qts[0], "UTDATE", True ))
if ut >= 20150606 and ut <= 20150929:
pntfile = os.path.join(NDG.tempdir,"pointing")
fd = open(pntfile,"w")
fd.write("# system=azel\n")
fd.write("# tai dlon dlat\n")
fd.write("54000 32.1 27.4\n")
fd.write("56000 32.1 27.4\n")
fd.close()
else:
pntfile = "!"
# If a reference map has been supplied, and parameter ALIGN is TRUE,
# we create an I map and determine any extra pointing corrections
# that are needed to bring the I map into alignment with the reference map.
if ref != "!" and align:
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the input NDFs. They should be supplied as the first item on
# the command line, in the form of a Starlink "group expression" (i.e.
# the same way they are supplied to other SMURF commands such as makemap).
# Quote the string so that it can be used as command line argument when
# running an atask from the shell.
indata = parsys["IN"].value
# See if we can determine a good default for INSTRUMENT by looking at
# the FITS headers of the first input NDF.
try:
cval = starutil.get_fits_header(indata[0], "INSTRUME").strip()
if cval == "SCUBA-2":
cval = starutil.get_fits_header(indata[0], "FILTER").strip()
if cval == "450":
deflt = "SCUBA-2(450)"
elif cval == "850":
deflt = "SCUBA-2(850)"
else:
deflt = None
else:
cval = starutil.get_fits_header(indata[0], "BACKEND")
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# Get any supplied Region defining the required sky region.
region = parsys["REGION"].value
# Get the list of tile NDFs that are available.
tiles = parsys["TILES"].value
# Get the JCMT instrument to which the tiles relate by looking at the
# "INSTRUME" and "FILTER" FITS headers in the first tile. Check all
# tiles have the same value.
instrument0 = None
for tile in tiles:
cval = starutil.get_fits_header( tile, "INSTRUME" )
if cval == "HARP":
instrument = "HARP"
elif cval == "SCUBA-2":
cval = starutil.get_fits_header( tile, "FILTER" )
if cval == "450":
instrument = "SCUBA-2(450)"
elif cval == "850":
instrument = "SCUBA-2(850)"
elif cval != None:
raise starutil.InvalidParameterError("Tile {0} has an unknown "
"value '{1}' for the FILTER header.".format(tile,cval) )
# the mean Q value per bolometer. Astronomical sources will affect this
# mean to a small extent, but its probably the best we can do for now. To
# find the gradient and offset of the linear relationship for each Q image,
# we use kappa:normalize to do a least squares fit between each Q image and
# the mean Q signal.
qnm = NDG(qarray)
qnm.comment = "qnm"
for (qin,qout) in zip( qarray, qnm ):
invoke( "$KAPPA_DIR/normalize in1={0} in2={1} out={2} device={3}".
format(qcom,qin,qout,ndevice), buffer=True )
# If required, store the slope and offset in the diagnostics file.
if diagfd != None:
slope = starutil.get_task_par( "slope", "normalize" )
offset = starutil.get_task_par( "offset", "normalize" )
ichunk = starutil.get_fits_header( qin, "POLCHUNK" )
iblock = starutil.get_fits_header( qin, "POLBLOCK" )
diagfd.write("Q {0} {1} {2} {3} {4}\n".format(iblock,a,ichunk,slope,offset))
# Now substract the normalized mean Q signal from each Q image.
qsub = NDG(qarray)
qsub.comment = "qsub"
invoke( "$KAPPA_DIR/sub in1={0} in2={1} out={2}".
format(qarray,qnm,qsub) )
# And then remove smaller spikes that have now become visible in the
# Q images as a result of subtracting off the bolometer biases.
qffb = NDG(qarray)
qffb.comment = "qffb"
invoke( "$KAPPA_DIR/ffclean in={0} out={1} box=3 clip=\[2,2,2\]".
format(qsub,qffb) )
os._exit(1)
# To be a group expression, it must contain at least one of the
# following characters: ^,= (NDFs are not allowed any of these).
gexp_chars = set( '^=,' )
if any( (c in gexp_chars) for c in config1 ):
isndf1 = False
else:
isndf1 = True
# If it is an NDF, attempt to get the SUBARRAY fits header, and
# determine the waveband. If no SUBARRAY header is found, look for
# "s4a", etc, in the NDF's provenance info.
if isndf1:
try:
subarray = starutil.get_fits_header( config1, "SUBARRAY" )
if subarray is None:
text = starutil.invoke( "$KAPPA_DIR/provshow {0}".format(config1) )
if "s4a" in text or "s4b" in text or "s4c" in text or "s4d" in text:
subarray = "s4"
elif "s8a" in text or "s8b" in text or "s8c" in text or "s8d" in text:
subarray = "s8"
else:
subarray = None
except:
print( "\n!! It looks like NDF '{0}' either does not exist or is "
"corrupt.".format(config1) )
os._exit(1)
if isndf1:
if subarray is None:
ref_units = None
else:
# See if a filtered and scaled v ersion of the referenc emap is to be
# created.
refout = parsys["REFOUT"].value
# If the REF map is in units of mJy/beam, convert it to pW using the FCF
# in the "FCF" FITS header if available, or the standard FCF for the
# wavelength otherwise.
invoke("$KAPPA_DIR/ndftrace ndf={0} quiet".format(ref) )
ref_units = get_task_par( "UNITS", "ndftrace" ).replace(" ", "")
if ref_units != "pW":
try:
filter = int( float( get_fits_header( ref, "FILTER", True )))
except starutil.NoValueError:
filter = 850
msg_out( "No value found for FITS header 'FILTER' in {0} - assuming 850".format(ref))
if filter != 450 and filter != 850:
raise starutil.InvalidParameterError("Invalid FILTER header value "
"'{0} found in {1}.".format( filter, ref ) )
if ref_units == "mJy/beam":
if filter == 450:
fcf = 491000.0
else:
fcf = 537000.0
elif ref_units == "Jy/beam":
# NOTE: This assumes oracdr_scuba2_450 or oracdr_scuba2_850 has been run
# which sets the ORAC_INSTRUMENT environment variable to 'SCUBA2_450' or 'SCUBA2_850'
# else default to 850 band
band = os.getenv('ORAC_INSTRUMENT')
if band is None:
print "ORAC_INSTRUMENT environment variable not set!"
print "This program expects to be run from a shell"
print "prepared with the command: oracdr_scuba2_<band> <observation-date>"
print "where band is: 450 or 850"
print "and observation-date has the form: YYYYMMDD"
sys.exit(0)
# print "band={0}".format(band)
# Get WNFACT value and nFrames from data file
wnfact = float(starutil.get_fits_header(indata, "WNFACT"))
# print "wnfact={0}".format(wnfact)
nFrames = int(starutil.get_fits_header(indata, "MIRSTOP")) + 1
# print "nFrames={0}".format(nFrames)
# Gather statistics on the central region of the input spectrum
# We are interested in the z position of the maximum pixel value (peak)
instats = invoke("$KAPPA_DIR/stats ndf={0} quiet".format(indata))
maxpos = starutil.get_task_par("MAXPOS", "stats")
maxposz = maxpos[2]
# print "maxposz={0}".format(maxposz)
# Calculate the band pass frames centered on the peak
if band == "SCUBA2_850":
wnlbound = 11.2
wnubound = 12.2
parsys = ParSys( params ) # Get the input NDF. indata = parsys["IN"].value # Get the file in which to put the Region. region = parsys["REGION"].value # See if temp files are to be retained. retain = parsys["RETAIN"].value # See if JSA tile indicies are to be displayed. tiles = parsys["TILES"].value # Get the required FITS headers from the NDF. map_hght = float( starutil.get_fits_header( indata, "MAP_HGHT", report=True ) ) map_wdth = float( starutil.get_fits_header( indata, "MAP_WDTH", report=True ) ) basec1 = float( starutil.get_fits_header( indata, "BASEC1", report=True ) ) basec2 = float( starutil.get_fits_header( indata, "BASEC2", report=True ) ) tracksys = starutil.get_fits_header( indata, "TRACKSYS", report=True ) # Convert arc-seconds to degrees. map_hght /= 3600.0 map_wdth /= 3600.0 # Convert degrees to radians. map_hght = math.radians( map_hght ) map_wdth = math.radians( map_wdth ) basec1 = math.radians( basec1 ) basec2 = math.radians( basec2 )
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the input NDFs. They should be supplied as the first item on
# the command line, in the form of a Starlink "group expression" (i.e.
# the same way they are supplied to other SMURF commands such as makemap).
# Quote the string so that it can be used as command line argument when
# running an atask from the shell.
indata = parsys["IN"].value
# See if we can determine a good default for INSTRUMENT by looking at
# the FITS headers of the first input NDF.
try:
instrume = starutil.get_fits_header( indata[0], "INSTRUME" ).strip();
if instrume == "HARP":
deflt = "HARP"
elif instrume == "SCUBA-2":
filter = starutil.get_fits_header( indata[0], "FILTER" ).strip();
if filter == "850":
deflt = "SCUBA-2(850)";
else:
deflt = "SCUBA-2(450)";
else:
deflt = None
except:
deflt = None
# prompted for it.
outcat = parsys["CAT"].value
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# See statistical debiasing is to be performed.
debias = parsys["DEBIAS"].value
# See if we should convert pW to Jy.
jy = parsys["JY"].value
# Determine the waveband and get the corresponding FCF values with and
# without POL2 in the beam.
try:
filter = int( float( starutil.get_fits_header( qin[0], "FILTER", True )))
except NoValueError:
filter = 850
msg_out( "No value found for FITS header 'FILTER' in {0} - assuming 850".format(qin[0]))
if filter == 450:
fcf1 = 962.0
fcf2 = 491.0
elif filter == 850:
fcf1 = 725.0
fcf2 = 537.0
else:
raise starutil.InvalidParameterError("Invalid FILTER header value "
"'{0} found in {1}.".format( filter, qin[0] ) )
# Remove any spectral axes
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the input NDFs. They should be supplied as the first item on
# the command line, in the form of a Starlink "group expression" (i.e.
# the same way they are supplied to other SMURF commands such as makemap).
# Quote the string so that it can be used as command line argument when
# running an atask from the shell.
indata = parsys["IN"].value
# See if we can determine a good default for INSTRUMENT by looking at
# the FITS headers of the first input NDF.
try:
cval = starutil.get_fits_header( indata[0], "INSTRUME" ).strip()
if cval == "SCUBA-2":
cval = starutil.get_fits_header( indata[0], "FILTER" ).strip()
if cval == "450":
deflt = "SCUBA-2(450)"
elif cval == "850":
deflt = "SCUBA-2(850)"
else:
deflt = None
else:
cval = starutil.get_fits_header( indata[0], "BACKEND" )
# prompted for it.
outcat = parsys["CAT"].value
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# See statistical debiasing is to be performed.
debias = parsys["DEBIAS"].value
# See if we should convert pW to Jy/beam.
jy = parsys["JY"].value
# See if the I maps were made from POL2 data.
ipol2 = None
for sdf in iin:
if "pol" in starutil.get_fits_header( sdf, "INBEAM" ):
if ipol2 is None:
ipol2 = True
elif not ipol2:
ipol2 = None
break
else:
if ipol2 is None:
ipol2 = False
elif ipol2:
ipol2 = None
break
if ipol2 is None:
raise starutil.InvalidParameterError("Mixture of POL2 and non-POL2 "
"I maps supplied - all I maps must be the same.")
parsys = ParSys(params)
# Get the input NDF.
indata = parsys["IN"].value
# Get the file in which to put the Region.
region = parsys["REGION"].value
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# See if JSA tile indices are to be displayed.
tiles = parsys["TILES"].value
# Get the required FITS headers from the NDF.
map_hght = float(starutil.get_fits_header(indata, "MAP_HGHT", report=True))
map_wdth = float(starutil.get_fits_header(indata, "MAP_WDTH", report=True))
basec1 = float(starutil.get_fits_header(indata, "BASEC1", report=True))
basec2 = float(starutil.get_fits_header(indata, "BASEC2", report=True))
tracksys = starutil.get_fits_header(indata, "TRACKSYS", report=True)
# Convert arc-seconds to degrees.
map_hght /= 3600.0
map_wdth /= 3600.0
# Convert degrees to radians.
map_hght = math.radians(map_hght)
map_wdth = math.radians(map_wdth)
basec1 = math.radians(basec1)
basec2 = math.radians(basec2)
# line.
parsys = ParSys(params)
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the template POL2 data files. They should be supplied as the first
# item on the command line, in the form of a Starlink "group expression"
# (i.e.the same way they are supplied to other SMURF commands such as
# makemap). Quote the string so that it can be used as command line
# argument when running an atask from the shell.
indata = parsys["IN"].value
# AZ/EL pointing correction, for pre 20150929 data.
if int(starutil.get_fits_header(indata[0], "UTDATE", True)) < 20150929:
pntfile = os.path.join(NDG.tempdir, "pointing")
fd = open(pntfile, "w")
fd.write("# system=azel\n")
fd.write("# tai dlon dlat\n")
fd.write("54000 32.1 27.4\n")
fd.write("56000 32.1 27.4\n")
fd.close()
else:
pntfile = "!"
# Are we inheriting noise from the input (real) time-streams, rather
# than generating artificial noise?
addon = parsys["ADDON"].value
# Common mode files.
# Get the name of the output NDF. If not supplied, use the name of hte
# input NDF.
outndf = parsys["OUT"].value
if outndf is None:
outndf = inndf
# See how the output NDFs are to be trimmed.
trim = parsys["TRIM"].value
# See if temp files are to be retained.
retain = parsys["RETAIN"].value
# See if the supplied NDF holds data from a JCMT instrument by looking at the
# "INSTRUME", "BACKEND" and "FILTER" FITS headers.
instrument = None
cval = starutil.get_fits_header(inndf, "INSTRUME")
if cval == "SCUBA-2":
cval = starutil.get_fits_header(inndf, "FILTER")
if cval == "450":
instrument = "SCUBA-2(450)"
elif cval == "850":
instrument = "SCUBA-2(850)"
else:
cval = starutil.get_fits_header(inndf, "BACKEND")
if cval == "ACSIS":
instrument = "ACSIS"
os._exit(1)
# To be a group expression, it must contain at least one of the
# following characters: ^,= (NDFs are not allowed any of these).
gexp_chars = set( '^=,' )
if any( (c in gexp_chars) for c in config1 ):
isndf1 = False
else:
isndf1 = True
# If it is an NDF, attempt to get the SUBARRAY fits header, and
# determine the waveband. If no SUBARRAY header is found, look for
# "s4a", etc, in the NDF's provenance info.
if isndf1:
try:
subarray = starutil.get_fits_header( config1, "SUBARRAY" )
if subarray == None:
text = starutil.invoke( "$KAPPA_DIR/provshow {0}".format(config1) )
if "s4a" in text or "s4b" in text or "s4c" in text or "s4d" in text:
subarray = "s4"
elif "s8a" in text or "s8b" in text or "s8c" in text or "s8d" in text:
subarray = "s8"
else:
subarray = None
except:
print( "\n!! It looks like NDF '{0}' either does not exist or is "
"corrupt.".format(config1) )
os._exit(1)
if isndf1:
if subarray == None:
retain = parsys["RETAIN"].value
# Get any supplied Region defining the required sky region.
region = parsys["REGION"].value
# Get the list of tile NDFs that are available.
tiles = parsys["TILES"].value
# Get the JCMT instrument to which the tiles relate by looking at the
# "INSTRUME", "BACKEND" and "FILTER" FITS headers in the first tile. Check
# all tiles have the same value.
instrument0 = None
for tile in tiles:
instrument = None
cval = starutil.get_fits_header(tile, "INSTRUME")
if cval == "SCUBA-2":
cval = starutil.get_fits_header(tile, "FILTER")
if cval == "450":
instrument = "SCUBA-2(450)"
elif cval == "850":
instrument = "SCUBA-2(850)"
else:
cval = starutil.get_fits_header(tile, "BACKEND")
if cval == "ACSIS":
instrument = "ACSIS"
retain = parsys["RETAIN"].value
# Get any supplied Region defining the required sky region.
region = parsys["REGION"].value
# Get the list of tile NDFs that are available.
tiles = parsys["TILES"].value
# Get the JCMT instrument to which the tiles relate by looking at the
# "INSTRUME", "BACKEND" and "FILTER" FITS headers in the first tile. Check
# all tiles have the same value.
instrument0 = None
for tile in tiles:
instrument = None
cval = starutil.get_fits_header( tile, "INSTRUME" )
if cval == "SCUBA-2":
cval = starutil.get_fits_header( tile, "FILTER" )
if cval == "450":
instrument = "SCUBA-2(450)"
elif cval == "850":
instrument = "SCUBA-2(850)"
else:
cval = starutil.get_fits_header( tile, "BACKEND" )
if cval == "ACSIS":
instrument = "ACSIS"
# line.
parsys = ParSys( params )
# It's a good idea to get parameter values early if possible, in case
# the user goes off for a coffee whilst the script is running and does not
# see a later parameter propmpt or error...
# Get the template POL2 data files. They should be supplied as the first
# item on the command line, in the form of a Starlink "group expression"
# (i.e.the same way they are supplied to other SMURF commands such as
# makemap). Quote the string so that it can be used as command line
# argument when running an atask from the shell.
indata = parsys["IN"].value
# AZ/EL pointing correction, for pre 20150929 data.
if int(starutil.get_fits_header( indata[0], "UTDATE", True )) < 20150929:
pntfile = os.path.join(NDG.tempdir,"pointing")
fd = open(pntfile,"w")
fd.write("# system=azel\n")
fd.write("# tai dlon dlat\n")
fd.write("54000 32.1 27.4\n")
fd.write("56000 32.1 27.4\n")
fd.close()
else:
pntfile = "!"
# Are we inheriting noise from the input (real) time-streams, rather
# than generating artificial noise?
addon = parsys["ADDON"].value
# Common mode files.
