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test_disperser_nonsidereal_F250M.yaml
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test_disperser_nonsidereal_F250M.yaml
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Inst:
instrument: NIRCam #Instrument name
mode: moving_target #Observation mode (e.g. imaging, WFSS, moving_target)
nresetlines: 512 #eventially use dictionary w/in code to look this up
Readout:
readpatt: RAPID #Readout pattern (RAPID, BRIGHT2, etc) overrides nframe,nskip unless it is not recognized
nframe: 1 #Number of frames per group
nskip: 0 #Number of skipped frames between groups
ngroup: 5 #Number of groups in integration
nint: 1 #Number of integrations
namp: 4 #Number of amplifiers used in readout (4 for full frame, 1 for subarray)
array_name: NRCA1_FULL #Name of array (FULL, SUB160, SUB64P, etc) overrides subarray_bounds below
subarray_bounds: 0, 0, 159, 159 #Coords of subarray corners. (xstart, ystart, xend, yend) Over-ridden by array_name above. Currently not used. Could be used if output saved in raw format
filter: F250M #Filter of simulated data (F090W, F322W2, etc)
pupil: CLEAR #Pupil element for simulated data (CLEAR, GRISMC, etc)
Reffiles: #Set to None or leave blank if you wish to skip that step
dark: /ifs/jwst/wit/witserv/data4/nrc/hilbert/superbias/cv3/A1/NRCNRCA1-DARK-60091434481_1_481_SE_2016-01-09T15h50m45_uncal.fits #Dark current integration used as the base
hotpixmask: None #Hot pixel mask to go with the dark integration. If none, the script will find hot pixels. Fits file. Ones are hot. Zeros not.
superbias: /ifs/jwst/wit/witserv/data4/nrc/hilbert/superbias/cv3/A1/A1_superbias_from_list_of_biasfiles.list.fits #Superbias file. Set to None or leave blank if not using
subarray_defs: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/NIRCam_subarray_definitions.list #File that contains a list of all possible subarray names and coordinates
readpattdefs: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/nircam_read_pattern_definitions.list #File that contains a list of all possible readout pattern names and associated NFRAME/NSKIP values
linearity: /ifs/jwst/wit/witserv/data7/nrc/reference_files/SSB/CV3/cv3_reffile_conversion/linearity/NRCA1_17004_LinearityCoeff_ADU0_2016-05-14_ssblinearity_v2_DMSorient.fits #linearity correction coefficients
saturation: /ifs/jwst/wit/witserv/data7/nrc/reference_files/SSB/CV3/cv3_reffile_conversion/welldepth/NRCA1_17004_WellDepthADU_2016-03-10_ssbsaturation_DMSorient.fits #well depth reference files
gain: /ifs/jwst/wit/witserv/data7/nrc/reference_files/SSB/CV3/cv3_reffile_conversion/gain/NRCA1_17004_Gain_ISIMCV3_2016-01-23_ssbgain_DMSorient.fits #Gain map
phot: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/nircam_mag15_countrates.list #File with list of all filters and associated quantum yield values and countrates for mag 15 star
pixelflat: None
illumflat: None #Illumination flat field file
astrometric: /ifs/jwst/wit/witserv/data4/nrc/hilbert/distortion_reference_file_testing/reffiles_27Oct2016/NRCA1_FULL_distortion.asdf #Astrometric distortion file (asdf)
distortion_coeffs: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/NIRCam_SIAF_2016-09-29.csv #CSV file containing distortion coefficients
ipc: /ifs/jwst/wit/witserv/data7/nrc/reference_files/SSB/CV3/cv3_reffile_conversion/ipc/NRCA1_17004_IPCDeconvolutionKernel_2016-03-18_ssbipc_DMSorient.fits #File containing IPC kernel to apply
invertIPC: True #Invert the IPC kernel before the convolution. True or False. Use True if the kernel is designed for the removal of IPC effects, like the JWST reference files are.
crosstalk: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/xtalk20150303g0.errorcut.txt #File containing crosstalk coefficients
occult: None #Occulting spots correction image
filtpupilcombo: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/nircam_filter_pupil_pairings.list #File that lists the filter wheel element / pupil wheel element combinations. Used only in writing output file
pixelAreaMap: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/jwst_nircam_area_0001.fits #Pixel area map for the detector. Used to introduce distortion into the output ramp.
flux_cal: NIRCam_zeropoints.list #File that lists flux conversion factor and pivot wavelength for each filter. Only used when making direct image outputs to be fed into the grism disperser code.
nonlin:
limit: 60000.0 #Upper signal limit to which nonlinearity is applied (ADU)
accuracy: 0.000001 #Non-linearity accuracy threshold
maxiter: 10 #Maximum number of iterations to use when applying non-linearity
robberto: False #Use Massimo Robberto type non-linearity coefficients
cosmicRay:
path: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/cosmic_ray_library/ #Path to CR library
library: SUNMIN #Type of cosmic ray environment (SUNMAX, SUNMIN, FLARE)
scale: 1.5 #Cosmic ray scaling factor
suffix: IPC_NIRCam_A1 #Suffix of library file names
seed: 973415286 #Seed for random number generator
simSignals:
pointsource: ptsrc_disperse_test_f250m.list #File containing a list of point sources to add (x,y locations and magnitudes)
psfpath: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/psf_files/ #Path to PSF library
psfbasename: nircam #Basename of the files in the psf library
psfpixfrac: 0.1 #Fraction of a pixel between entries in PSF library (e.g. 0.1 = files for PSF centered at 0.1 pixel intervals within pixel)
psfwfe: 155 #PSF WFE value (0,115,123,132,136,150,155)
psfwfegroup: 0 #WFE realization group (0 to 9)
galaxyListFile: galaxies_disperse_test_f250m.list #File containing a list of positions/ellipticities/magnitudes of galaxies to simulate
extended: None #Extended emission count rate image file name
extendedscale: 2.0 #Scaling factor for extended emission image
extendedCenter: 1024,1024 #x,y pixel location at which to place the extended image if it is smaller than the output array size
PSFConvolveExtended: True #Convolve the extended image with the PSF before adding to the output image (True or False)
movingTargetList: None #Name of file containing a list of point source moving targets (e.g. KBOs, asteroids, satellites) to add. (These objects will move through the fov during the observation)
movingTargetSersic: None #ascii file containing a list of 2D sersic profiles to have moving through the field
movingTargetExtended: None #ascii file containing a list of stamp images to add as moving targets (planets, moons, etc)
movingTargetConvolveExtended: True #convolve the extended moving targets with PSF before adding.
movingTargetToTrack: nonsidereal_target_F250M_disperse_test.list #File containing a single moving target which JWST will track during observation (e.g. a planet, moon, KBO, asteroid) This file will only be used if mode is set to 'moving_target'
zodiacal: None #Zodiacal light count rate image file
zodiscale: 1.0 #Zodi scaling factor
scattered: None #Scattered light count rate image file
scatteredscale: 1.0 #Scattered light scaling factor
bkgdrate: 10.001 #Constant background count rate (electrons/sec/pixel)
poissonseed: 3124580697 #Random number generator seed for Poisson simulation)
photonyield: True #Apply photon yield in simulation
pymethod: True #Use double Poisson simulation for photon yield
Telescope:
ra: "00:00:00.00" #RA of simulated pointing
dec: "00:00:00.00" #Dec of simulated pointing
rotation: 0.0 #y axis rotation (degrees E of N)
newRamp:
combine_method: PROPER
proper_combine: BOTH
proper_signal_limit: 5000
linearized_darkfile: None
dq_configfile: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/dq_init.cfg
sat_configfile: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/saturation.cfg
superbias_configfile: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/superbias.cfg
refpix_configfile: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/refpix.cfg
linear_configfile: /ifs/jwst/wit/witserv/data4/nrc/hilbert/simulated_data/linearity.cfg
Output:
file: test_disperse_f250m.fits #Output filename
format: DMS #Output file format Options: DMS, SSR(not yet implemented)
save_intermediates: False #Save intermediate products separately (point source image, etc)
grism_source_image: True #grism
grism_input_only: True #grism
unsigned: True #Output unsigned integers? (0-65535 if true. -32768 to 32768 if false)
dmsOrient: True #Output in DMS orientation (vs. fitswriter orientation).
program_number: 99999 #Program Number
observation_number: 001 #Obeservation Number
visit_number: 001 #Visit Number
visit_group: 01 #Visit Group
obs_id: 00 #Observation ID
visit_id: 00 #Visit ID
sequence_id: 1 #Sequence ID
activity_id: 01 #activity ID - increment for each dither, keep same for each detector within exposure
exposure_number: 1 #exposure number