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Cycle 23 STIS Instrument Handbook
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Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 23 > Chapter 12: Special Uses of STIS > 12.1 Slitless First-Order Spectroscopy

12.1
The vast majority of STIS first-order grating mode observations use a long slit. The use of a long slit ensures a clean separation of emission lines arising from different spatial features. However, all of STIS’ first-order gratings as well as the NUV PRISM (see Table 4.1, STIS Spectroscopic Capabilities) can also be used slitless or with a wide slit to obtain emission line images. Figure 12.1 below shows a schematic example of a slitless spectrogram. Figure 4.8, STIS G750M 6581 52 2 Spectral Image of SN1987A shows an image of SN1987A observed using the 52X2 aperture, and as the source is smaller than the slit, this is effectively a slitless image.
Figure 12.1: A Schematic Slitless Spectrogram of a Planetary Nebula
When STIS is used slitless (or with a wide slit), the image obtained will be the sum of a series of shifted monochromatic images of the field of view. The range of wavelengths covered in the series of monochromatic images is dictated by the spectral range of the grating. The result is that there is not a one-to-one mapping of pixel location to wavelength in your image or of pixel location to spatial location on the sky. Depending on the structure of your source and the grating you use, it may be easy to deconvolve the spatial and spectral information, or it may be very difficult.
Slitless spectroscopy can be employed either for prime or parallel STIS observing, (although MAMA pure parallels are not allowed). If you are designing a slitless spectroscopic observation there are a few important points to keep in mind:
Since each point in the sky emits geocoronal light, the background due to the geocoronal emission lines (Lyman-α λ1216, [O I] λλ1302,1306, and occasionally on the day side [O I] λ1356 and [O II] λ2471; see “Geocoronal Emission and Shadow” ) will be observed at all pixels in the image when a slitless spectrum is obtained which covers these wavelengths. This background must be taken into account in your signal-to-noise calculations. For this reason, you may wish to consider using one of the two longpass ultraviolet (UV) blocking filters (see Section 5.3.5), instead of a clear aperture when performing UV slitless spectroscopy. Note that when a spectroscopic exposure is obtained with a slit, these sky emission lines are localized in the resulting image to the pixels at the corresponding wavelengths.
In order to properly calibrate slitless data it is necessary to know the position of each source along the dispersion direction. This usually requires a STIS, ACS, WFC3, or archival image at comparable spatial resolution and imaged with a comparable bandpass to the emission line structure that is being imaged with the slitless STIS spectroscopy. Obtaining the image during the same visit and at the same position angle as the slitless spectroscopy simplifies the image registration and analysis. Variations in the positioning of the Mode Select Mechanism (MSM), which contains the mirrors and gratings, can result in an uncertainty of the position of an image or spectrum on the detector by as much as five pixels, and an additional special calibration may be needed in order to fix the absolute offset between the images and the spectrograms. The standard STIS ACQ procedure automatically measures the offset between the location of a star and a reference aperture on the CCD detector and uses this to place the target accurately in the desired slit. So if the ACQ target appears in the field of view, there is no need for an additional image to calibrate the MSM offset, although a separate full field image may still be needed to measure the relative positions of other sources with respect to the ACQ target. In cases where no STIS ACQ exposure is done, an image of the field should be taken either immediately following or immediately preceding a lamp image taken through a narrow slit. For the CCD, a 1 second tungsten lamp exposure with the 52X0.1 slit will do nicely. This will allow the MSM offset for that image to be determined. It is important that no MSM motion (mirror or grating change) occur between the sky image and the lamp image of the slit. The MSM offset for the spectrographic exposure itself can usually be measured from the standard wavecal exposure. If extremely precise alignment between the spectrum and the field image in the cross dispersion direction is also required for source identification, this procedure may require some modifications, and observers should consult their contact scientist or the STScI Help Desk.
Finally, we note that to achieve an accurate wavelength calibration for targets observed in slitless mode, when those targets are well displaced from the nominal AXIS1 center, the dispersion coefficients at the off-nominal centerings must be well known. Currently, the incidence-angle offset corrections are based on ground calibration data and are somewhat less accurate than the on-axis dispersion solutions. We recommend that observers consult the Help Desk if they are concerned about the calibration of observations taken of targets which are expected to be off-center by more than 1 arcsecond in the dispersion direction.

Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 23 > Chapter 12: Special Uses of STIS > 12.1 Slitless First-Order Spectroscopy

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