Space Telescope Science Institute  Part V:  Appendices Camera 1, Filter F095N

Appendix A:
Imaging
Reference Material


In this appendix . . .
Camera 1, Filter F090M
Camera 1, Filter F095N
Camera 1, Filter F097N
Camera 1, Filter F108N
Camera 1, Filter F110M
Camera 1, Filter F110W
Camera 1, Filter F113N
Camera 1, Filter F140W
Camera 1, Filter F145M
Camera 1, Filter F160W
Camera 1, Filter F164N
Camera 1, Filter F165M
Camera 1, Filter F166N
Camera 1, Filter F170M
Camera 1, Filter F187N
Camera 1, Filter F190N
Camera 1, Polarizer POL0S
Camera 2, Filter F110W
Camera 2, Filter F160W
Camera 2, Filter F165M
Camera 2, Filter F171M
Camera 2, Filter F180M
Camera 2, Filter F187N
Camera 2, Filter F187W
Camera 2, Filter F190N
Camera 2, Filter F204M
Camera 2, Filter F205W
Camera 2, Filter F207M
Camera 2, Filter F212N
Camera 2, Filter F215N
Camera 2, Filter F216N
Camera 2, Filter F222M
Camera 2, Filter F237M
Camera 2, Polarizer POL0L
Camera 3, Filter F108N
Camera 3, Filter F110W
Camera 3, Filter F113N
Camera 3, Filter F150W
Camera 3, Filter F160W
Camera 3, Filter F164N
Camera 3, Filter F166N
Camera 3, Filter F175W
Camera 3, Filter F187N
Camera 3, Filter F190N
Camera 3, Filter F196N
Camera 3, Filter F200N
Camera 3, Filter F212N
Camera 3, Filter F215N
Camera 3, Filter F222M
Camera 3, Filter F240M

This chapter provides basic throughput information and plots for the imaging and polarimetric filters. The corresponding information for the grism elements is provided in Chapter 5. The spectral characteristics of the NICMOS flight filters were measured at cryogenic temperature and normal incidence at Ball Aerospace. All filters had their spectral transmission measured from 0.5 to 2.7 microns with a step of 0.001 microns. For each filter, we provide the following information:

All throughput curves and band parameters in this section were built with the DQE curve corrected to 77.1 K. The values for most of these parameters come directly from the synphot task in STSDAS. The graph (grtbl) and component (cmptbl) tables used for these calculations were:

grtbl = "k511557nm_tmg.fits"

cmptbl = "m7t1443mm_tmc.fits"

The above tables used for these calculations are available from CDBS at STScI.

The filter transmission curves and OTA and NICMOS optics reflectivities are the ones listed in these files. The only change made relative to these tables is that the nic?_dqe* table for each camera was modified to reflect changes from the reference temperature of each curve to the nominal NCS operating temperature (77.1 K, at the NDWTMP11 Mounting Cup temperature sensor). Based on the NICMOS standard star photometry, each DQE curve + filter transmission curve is correct for the temperature at which the standard star observations were made (NIC1: 61.3 K, NIC2: 61.3 K, NIC3: 62.0 K)

The correction of the original DQE curves were made based on the ratio of the mean value of lamp-flat images taken at the current operating temperature of 77.1 K to flats taken at the above temperatures. The correction factor as a function of wavelength is then multiplied by the original curve to get the new curve. Note that the DQE can vary by factors of 2-3 across each array. Once the standard star observations from early SMOV are reduced it will be possible to use those to adjust the DQE curves rather than using the lamp flats.

The band parameters correspond to the output of the STSDAS task bandpar where:

Central wavelength = PIVWV

Mean wavelength = AVGWV

Peak wavelength = WPEAK

Maximum throughput = TPEAK

The FWHM is defined as the intersection between the transmission curve and the half-maximum-transmission value. Since the transmission curve shape is strongly affected by the DQE (particularly for the broad filters), the measured FWHM will change with temperature. This is NOT the FWHM value returned by the bandpar task.

The "Wavelength range" values are just measured by-eye from the throughput curves to serve as a rough estimate.

The "central pixel fraction" is the fraction of the total light from a point source that is contained in the central pixel of the point spread function (PSF). This assumes that the source is centered on a pixel, and that the pixel response function is unity across the pixel. All PSFs were made from TinyTim V6.0, using the following parameters, in each of the filters:


Part V:  Appendices Camera 1, Filter F095N
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