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Hubble Space Telescope
STIS Instrument Filters

STIS/CCD FILTERS
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.

STIS/NUV MAMA FILTERS
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 Continuum 2700 350 25 x 25
F25CIII [C III] 1909 70 25 x 25
F25CN182 ~1800 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

STIS/FUV MAMA FILTERS
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:

Choosing a filter for imaging observations or slitless spectroscopy: