Space Telescope Science Institute   1.2.2 Comparison of WFPC2 and NICMOS  1.3 History of WFPC2

1.2.3 Comparison of WFPC2 and STIS


Both WFPC2 and STIS are capable of imaging over the same wavelength ranges between ~1150Å and ~11000Å. At much longer wavelengths NICMOS must be used.

Advantages of each instrument may be summarized as follows.

WFPC2 advantages are:

STIS advantages are:

In general, WFPC2 has a much greater selection of filters and wider field-of-view than STIS, but STIS has greater detective efficiency in the UV and for its long-pass and unfiltered modes. Table 1.4 compares the detective efficiency for WFPC2 and STIS filters with similar bandpasses. For UV imaging STIS is greatly superior due to higher throughput and insensitivity to filter red-leak; only if some detail of a WFPC2 filter bandpass were needed, would it be a viable choice.

For both [OII] 3727Å and [OIII] 5007Å imaging STIS has much higher QE and is preferred, unless the larger WFPC2 field-of-view is an important factor. The WFPC2 [OIII] filter is wider than its STIS counter-part, which may also be useful for redshifted lines. For broad-band imaging the unfiltered and 5500Å long-pass modes of STIS again have higher efficiency than WFPC2, though with reduced field-of-view.

Table 1.4: Comparison of WFPC2 and STIS Detector Efficiencies.
Instrument
Filter
Mean
Wavelength
(Å)
Bandpass
FWHM
(Å)1
Peak QE2
WFPC2
F122M
1420
100
0.11%
STIS
F25LYA
1216
85
0.32%
WFPC2
F160BW
1492
500
0.07%
STIS
25MAMA (FUV)
1370
320
4.5%
WFPC2
F255W
2586
393
0.5%
STIS
25MAMA (NUV)
2220
1200
3.1%
WFPC2
F375N
3738
42
0.9%
STIS
F28X50OII
3740
80
3.7%
WFPC2
F502N
5013
37
5.8%
STIS
F28X50OIII
5007
5
11%
WFPC2
F606W
5935
2200
14%
STIS
F28X50LP
~73003
2720
12%
STIS
50CCD
~5800
4410
15%
1Note that definition of FWHM is different from "effective width" elsewhere herein.
2Includes instrument and OTA.
35500Å long pass filter.


 1.2.2 Comparison of WFPC2 and NICMOS  1.3 History of WFPC2
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