While a direct image is required for identifying the full complex of overlapping orders in spectral images, wavelength assignments for sources with known coordinates can be derived using the offsets from the zero order grism images (see WFC3 ISR 2015-10
). The inaccuracy caused by any non-linearity in the dispersion is estimated at ~0.1 pixel or ~2.5 Å for G102 and ~5 Å for G141. The rms precision of the assigned wavelengths for individual spectra is better than 0.2 pixel. For the same or very similar POSTARGs, the separation from direct image to zero order varies by up to 0.5 pixels in both x and y directions, corresponding to an uncertainty of about ~12Å (G102) and ~23Å (G141).
The GRISM apertures (Table 7.1
) are designed to be used for both the grism exposure and the associated direct image. At a given telescope pointing, the first order spectrum and the location of the target in the direct image are roughly aligned in the x direction. The G102 spectrum starts at about 55 pixels to the right of the target image location and extends about 155 pixels; the G141 spectrum starts at about 35 pixels to the right of the target image location and extends about 135 pixels. For either grism, the same pointing can thus be used to place the target image and the first order spectrum on an array with dimensions greater than about 210 pixels. The apertures GRISM1024, GRISM512, and GRISM256 have been designed to take advantage of this, with the placement of the target optimized for the dimensions of the array, which is indicated by the number in the aperture name. For the smaller apertures, GRISM128 and GRISM64, different pointings are automatically used for the direct image and the grism exposure so that the target is within the aperture in the direct image and the target’s spectrum is also inside the aperture in the grism image. See http://www.stsci.edu/hst/wfc3/analysis/grism_obs/wfc3-grism-faq.html
for details on selecting GRISM apertures and using combinations of these apertures.
The performance of the IR grisms was analyzed during SMOV (WFC3 ISR 2009-17
, WFC3 ISR 2009-18
). The flux calibration was revised based on calibration observations made in cycle 17 (WFC3 ISR 2011-05
). Analysis of monitoring observations made from SMOV through cycle 20 has shown that the flux calibrations of the +1st order spectra have excellent temporal stability, varying by less than 1%, and that the calibration of the large-scale throughput variations over the detector are good to 4% (WFC3 ISR 2012-06
and WFC3 ISR 2014-01)
. Point source aperture corrections measured in cycle 20 (WFC3 ISR 2014-01
) are generally consistent with those derived in cycle 17 (WFC3 ISR 2011-05
) to 1%. Sky images for the IR grisms have been constructed using publicly available data; the average sky brightness measured in the G102 and G141 images is 0.8 e-
/s and 1.3 e-
/s, respectively (WFC3 ISR 2011-01
The wavelength calibration of the +1, -1, and +2 G102 and G141 orders were re-derived using all of the available multi-cycle calibration data (WFC3 ISR 2016-15
). The accuracy of this new calibration is estimated to be better than 0.1 pixel for the trace description and better than 0.5 pixel (~10A and 20A for the G102 and G141 grisms, respectively) for the wavelength calibration. Previous calibration assumed that grism observations would be paired with F098M and F140W direct images for the G102 and G141 grisms, respectively. New calibration solutions that include the effect of the filter wedge offset (WFC3 ISR 2010-12
) are now also available. See the calibration web pages for G102
shows the disposition of the zeroth-order image and +1st-order spectrum (which has much higher sensitivity than the –1st order due to the grating blaze) for the G102 grism. The location of the direct image (superposed from an F098M undispersed exposure) is indicated in the figure.
The trace of the first-order spectrum is well described by a first-order polynomial, however the offset and slope are a function of source position in the field. The tilt of the spectrum is 0.7°
with respect to the detector x-
axis. The total throughput (including HST
optics) of the G102 grism has a maximum of 41% at 1100 nm in the positive first order and is above 10% between 805 and 1150 nm. The zeroth order and other negative and positive orders show much lower throughput (see Figure 8.5
). The dispersion in the +1st order varies over the field from 2.36 to 2.51 nm/pixel; this variation was calibrated from both ground and on-orbit data to allow absolute wavelength calibration to better than one pixel. The absolute throughput of the G102 orders –1 to +3, including the instrument and the detector, is shown in Figure 8.5
. Suitable filters for the accompanying direct images for source selection and wavelength zero-point determination are F098M or F105W (see Section 7.9.5
for discussion of the IR background), but any of the narrower filters can also be used to prevent bright sources from saturating.
For the lower-dispersion G141 grism, the 0th-, 1st-, 2nd-, and 3rd-order spectra all lie within the field of view when the positive first-order is roughly centered. Figure 8.6
shows the appearance of the spectra on the detector, with the superposed direct image, for the G141 grism. The useful spectral range is from 1075 nm to about 1700 nm, limited in the red by the grism bandpass. Over most of the spectral range, more than 80% of the throughput is in the +1st-order spectrum. The trace of the first-order spectrum is well described by a first-order polynomial. The average tilt of the spectrum is 0.5 degrees with respect to the detector x-
axis. The dispersion in the +1st-order varies over the field from 4.47 to 4.78 nm/pixel; this variation has been measured from both ground and on-orbit data to allow absolute wavelength calibration to better than one pixel. The total throughput (including HST
optics) of the G141 grism reaches a maximum of 48% at ~1450 nm in the positive first order and is above 10% between 1080 and 1690 nm (see Figure 8.7