STIS Instrument Handbook

The filtered and clear apertures available for UV imaging are summarized in Table 5.1. Although there are only a small number of filters available, the solar-blind and solar-insensitive properties of the FUV-MAMA and NUV-MAMA detectors, respectively, coupled with their 25 × 25 arcsecond field of view, good spatial sampling, and ability to detect rapid variability, give STIS UV imaging capabilities that are complementary to those of ACS. The throughputs of the STIS MAMA imaging modes assumed for this Handbook are mostly based on on-orbit calibration observations.

Most figures and tables were updated for the Cycle 17 version of this handbook, using our best estimates of instrument performance for Cycle 17. Except where otherwise noted, we have not redone these figures and tables to take into account the modest changes expected between those projected values and the estimated Cycle 21 performance. These throughputs are good to within 5% in the FUV and the NUV. The throughputs in the ETC, the calibration reference files, as well as those used by the STSDAS synphot, and the STScI python pysynphot packages will continue to be updated as further analysis of calibration data continues. As of the publication of this handbook, the sensitivities used in those software packages are our best estimates for April 2014.

Figure 5.7 shows an example of MAMA imaging data of a globular cluster taken as part of the Cycle 7 calibration of STIS using the quartz filter and the NUV-MAMA.

The MAMA detectors are subject to absolute bright object limits, above which targets cannot be observed. They are particularly stringent for the MAMA imaging modes (being as faint as V=20.3 for the clear modes), and apply to all sources illuminating the field of view.

We direct MAMA observers to Section 7.7. For summary tables of absolute bright object screening magnitudes for the imaging modes, see Section 14.8.

It is the observers’ responsibility to ensure that their observations do not exceed the MAMA bright object limits.

The MAMA plate scale is ~0.0246 arcsec/pix in imaging mode, providing a good compromise between sampling of the PSF in the UV and field of view. Chapter 14 shows encircled energies as a function of wavelength for MAMA imaging, and provides information on the geometric distortions of the images. The MAMA detector PSFs exhibit broad wings, which are substantially higher in the NUV-MAMA than the FUV-MAMA. Figure 7.16 shows sample detector PSFs for the MAMAs.

Each MAMA can be used with the 25MAMA clear aperture to image a 25×25 arcsecond field of view of the sky, providing the maximum throughput and wavelength coverage in the NUV and FUV as shown in Figure 5.2 and Figure 5.3. However, NUV-MAMA clear direct images will be slightly out of focus, because the corresponding mirror on the MSM optimally focuses for use of a filter. It is recommended that the F25SRF2 longpass filter (see Section 5.3.5) be used instead of 25MAMA (clear) for direct imaging with the NUV-MAMA. The same does not apply to the FUV-MAMA, which has separate MSM mirrors for clear and filtered imaging.

The sky background can be significant for unfiltered FUV-MAMA observations. The strongest contributor is the geocoronal Lyman-α line. Global count rates of several 104 counts/s over the whole detector are not unusual during daytime observations. The same applies to slitless FUV spectroscopy. For observations of large, UV-faint targets, where background subtraction becomes critical, unfiltered imaging may introduce significant noise. In addition, the background may be variable during long exposures. Longpass filtered imaging may be profitable in this case.

Ground measurements of the FUV-MAMA quantum efficiency indicated that it dropped dramatically longward of ~2000 Å, which would have made it effectively solar blind, while the NUV-MAMA also showed a reduced response toward the red, longward of ~3500 Å (see Figure 5.9).

Recently it was realized that the ACS SBC (solar blind channel) detector has a significantly larger sensitivity to optical photons than pre-launch testing had indicated. Since the STIS FUV-MAMA is very similar in design to the ACS SBC, available data was scrutinized to determine whether a similar red leak existed for the STIS detector.

The best available observations for this test appear to be observations of Saturn where G140L, G230L, and FUV-MAMA SFR2 imaging observations were taken in the same visit. Comparison of the flux levels measured in these observations suggest that the optical throughput of the STIS FUV-MAMA detector, although still quite low, is indeed substantially higher than the pre-launch measurement. Based upon these observations and the estimated wavelength dependence of the optical throughput for the SBC, a preliminary revision to the FUV-MAMA imaging throughput curve has been devised (see Figure 5.8), and has been incorporated into the FUV-MAMA imaging throughput curves shown in chapter 14. Note that this revision results in only trivial changes to the formal calculation of bandpass parameters, and should only affect FUV-MAMA imaging observations of very red objects.

There is little STIS data available suitable for confirming the wavelength or time dependence of this extra optical throughput.

Table 5.3 and Table 5.4 give the percentages of detected photons arising in the UV versus optical for observations of different stellar types with the clear MAMA imaging modes. The data for the FUV-MAMA includes the effects of the estimated red leak.

Stellar Type	Teff (K)	Log g	Percentage of All Detected Photons which Have λ<1800 Å	Percentage of All Detected Photons which Have λ<3000 Å
O3	45,000	4.5	99.5	100.0
B0	30,000	4.0	99.4	100.0
A0	9500	4.0	97.2	100.0
A5	8250	4.0	82.6	99.9
F0	7250	4.0	68.3	99.5
G0	6000	4.5	31.2	72.7
K0	5250	4.5	5.1	27.6

Stellar Type	Teff (K)	Log g	Percentage of all Detected Photons which have λ<3000 Å	Percentage of all Detected Photons which have λ<5000 Å
O3	45,000	4.5	97.9	100.0
B0	30,000	4.0	97.6	100.0
A0	9500	4.0	93.0	99.9
A5	8250	4.0	90.0	99.8
F0	7250	4.0	85.0	99.7
G0	6000	4.5	71.3	99.2
K0	5250	4.5	56.9	97.7

The integrated system throughputs of the two UV longpass filters when used with the NUV-MAMA and FUV-MAMA are shown in Figure 5.2 and Figure 5.3 (for sensitivities, signal-to-noise plots, and saturation plots see pages 399 and 428 for F25SRF2, 396 and 424 for F25QTZ). The filter (only) throughputs of these two filters are shown in Figure 5.10. These filters image a 25×25 arcsecond field of view. The cutoff wavelengths of F25SRF2 and F25QTZ were chosen to exclude a) geocoronal Lyman-α 1216 Å and b) [O I] 1302Å+1306Å and O I] 1356 Å, respectively; use of these filters significantly reduces the total sky background in the UV. These filters can be used by themselves in imaging mode, or with the prism or any first-order UV grating in slitless spectroscopic observations, to reduce the background due to geocoronal emission (see Section 4.4 and Section 12.1). F25SRF2 images, combined with images taken in series with the FUV-MAMA/25MAMA clear, can also be used to obtain Lyman-α images (see “Lyman Alpha: F25LYA and Clear-Minus-SRF2”).

The filters for MAMA imaging include:

•	A narrow-band filter (F25MGII) which images the magnesium doublet at 2796–2803 Å, and a matched medium-band continuum filter (F25CN270) centered at 2700 Å (for sensitivities, signal-to-noise plots, and saturation plots, see page 404).

•

A narrow-band filter (F25CIII) which images the semi-forbidden CIII] lines at 1907–1909 Å, among the strongest nebular (low-density) lines in the UV, and a matched medium-band continuum filter (F25CN182) centered at 1800 Å (for sensitivities, signal-to-noise plots, and saturation plots, see page 407 for F25CIII and page 410 for F25CN182).

•

A narrow-band filter (F25LYA) which images Lyman-α; this filter has a relatively low throughput, and we recommend that you consider, instead, obtaining two FUV-MAMA images, one through the 25MAMA unfiltered aperture and a second with the SrF2 longpass filter. The difference of these two images will isolate Lyman-α with much higher throughput than the F25LYA filter. Alternatively, the ACS SBC can be used with the F122M filter (for sensitivities, signal-to-noise plots, and saturation plots of F25LYA, see page 432).

The F25MGII filter images a 25 × 25 arcsecond field of view in the light of the doublet lines of Mg II (2796 and 2803 Å). Figure 5.11 shows the integrated system throughput (see also page 401 for sensitivities, signal-to-noise plots, and saturation plots). There is a substantial red leak in this filter starting at approximately 4200 Å and extending to at least 13,000 Å. For stellar spectral types O and B, less than 2% of the detected counts will be due to red leak. This percentage rises to 7% for an A0 star. For a K0 star, 75% of the counts will be due to red leak. The red leak for this filter is included in the passbands used by the STIS ETC, pysynphot, and synphot. Observers are encouraged to use these tools to predict source and background count rates carefully.

The 2700 Å continuum filter images a 25×25 arcsecond field of view and can be used to measure the continuum for Mg II emission line images. The F25CN270 filter integrated system throughput is shown in Figure 5.11 above (see also page 404 for sensitivities, signal-to-noise plots, and saturation plots). There is a substantial red leak in this filter starting at approximately 4200 Å and extending to at least 12,000 Å. For a K0 star, roughly 40% of the detected counts will be due to red leak. The red leak for this filter is included in the passbands used by the STIS ETC, pysynphot, and synphot. Observers are encouraged to use these tools to predict source and background count rates carefully.

The F25CIII filter images a 25×25 arcsecond field of view in the light of C III] at 1907–1909 Å. The F25CIII integrated system throughput is shown in Figure 5.12 (see also page 407 for sensitivities, signal-to-noise plots, and saturation plots). The out-of-band suppression for this filter is fairly good.

The 1800 Å continuum filter images a 25 × 25 arcsecond field of view, and can be used to measure the continuum for C III] emission line images. The F25CN182 filter integrated system throughput is shown in Figure 5.12 above (see also page 410 for sensitivities, signal-to-noise plots, and saturation plots).

The F25LYA filter images a 25 × 25 arcsecond field of view and can be used to obtain emission line images in the light of Lyman-α. The F25LYA filter integrated system throughput is shown in Figure 5.13 (see also page 432 for sensitivities, signal-to-noise plots, and saturation plots).

At the price of a slightly wider bandpass, and the need to take two exposures, Lyman-α can be isolated by taking one image with the clear (25MAMA) aperture and a second with the longpass (F25SRF2) filter and differencing the two. The integrated system throughput for this imaging sequence is appreciably higher than for the narrowband F25LYA filter, as shown Figure 5.13.