| Name | Filter | Central Wavelength (Å) | FWHM (Å) | Field of View (arcsec2) |
|---|---|---|---|---|
| plate scale 0.05071 ± 0.00007 arcseconds per pixel | ||||
| 50CCD1 | Clear | 5850 | 4410 | 52 x 52 |
| F28X50LP1 | longpass > 5500 Å | 7230 | 2720 | 28 x 52 |
| F28X50OIII2 | [O III] | 5007 | 5 | 28 x 52 |
| F28X50OII | [O II] | 3740 | 80 | 28 x 52 |
| 50CORON3 | Clear + Coronagraphic fingers | 5850 | 4410 | Special |
1red halo 2red leak 3The 50CORON aperture is an unfiltered aperture with a number of occulting bars and wedges which functions as a coronagraphic mask. A number of separate aperture positions have been defined for use within 50CORON, ad may be individually specified in Phase 2 proposals.
| Aperture Name | Filter | Central Wavelength (Å) | FWHM (Å) | Field of View (arcsec2) |
|---|---|---|---|---|
| plate scale ~0.0248 arcseconds per pixel | ||||
| 25MAMA 4 | Clear | 2220 | 1200 | 25 x 25 |
| F25QTZ 5 | longpass > 1475 Å | 2320 | 1010 | 25 x 25 |
| F25SRF26 | longpass > 1275 Å | 2270 | 1110 | 25 x 25 |
| F25MGII | Mg II | 2800 | 70 | 25 x 25 |
| F25CN270 | ~2700 е Continuum | 2700 | 350 | 25 x 25 |
| F25CIII | [C III] | 1909 | 70 | 25 x 25 |
| F25CN182 | ~1800 е Continuum | 1820 | 350 | 25 x 25 |
| F25ND3 | ND=10-3 | 2344 | 1345 | 25 x 25 |
| F25ND5 | ND=5 x 10-6 | 2621 | 1515 | 25 x 25 |
|
F25NDQ1 F25NDQ2 F25NDQ3 F25NDQ4 |
ND=10-1 ND=10-2 ND=10-3 ND=10-4 |
2277 2318 2417 2450 |
1126 1036 756 607 |
~12 x 12 ~12 x 12 ~12 x 12 ~12 x 12 |
| Aperture Name | Filter | Central Wavelength (Å) | FWHM (Å) | Field of View (arcsec2) |
|---|---|---|---|---|
| plate scale ~0.0248 arcseconds per pixel | ||||
| 25MAMA 7 | Clear | 1370 | 320 | 25 x 25 |
| F25QTZ 5 | longpass > 1475 Å | 1590 | 220 | 25 x 25 |
| F25SRF2 6 | longpass > 1275 Å | 1480 | 280 | 25 x 25 |
| F25LYA 8 | Ly-alpha | 1216 | 85 | 25 x 25 |
| F25ND3 | ND=10-3 | 1376 | 316 | 25 x 25 |
| F25ND5 | ND=7 x 10-7 | 1385 | 336 | 25 x 25> |
|
F25NDQ1 F25NDQ2 F25NDQ3 F25NDQ4 |
ND=10-1 ND=10-2 ND=10-3 ND=10-4 |
1416 1404 1407 1437 |
384 384 401 391 |
~12 x 12 ~12 x 12 ~12 x 12 ~12 x 12 |
4not well focused, 5excludes O I 1302, 6excludes Ly-alpha, 7high airglow, 8low throughput
Note that MAMA imaging observations are subject to especially strict bright object limits, and will not be performed unless ALL objects in or near the aperture can be shown to be below these limits.
As STIS filters are located in the STIS slit wheel they must be listed as apertures in Phase II proposals and cannot be used in combination with other apertures. The STIS filters can, however, be used together with a grating to do filtered slitless first order spectroscopy. This can be especially useful when it is necessary to exclude contamination due to geocoronal lines.
STIS has a relatively limited set of filters. However its imaging capabilities do include some unique advantages that make it worth considering as an alternative to ACS for some UV and optical imaging projects.
Comparisons of Imaging Mode Throughputs:
- CCD, FUV-MAMA and NUV-MAMA Clear and Filtered Throughputs
- Color Corrections from Johnson V to AB Magnitude
Choosing a filter for imaging observations or slitless spectroscopy: