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Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 22 > Chapter 7: Feasibility and Detector Performance > 7.4 The MAMA Detectors

7.4
7.4.1 MAMA Properties
There are two MAMA detectors: the STIS/FUV-MAMA provides coverage from 1150 to 1700  and the STIS/NUV-MAMA provides coverage from 1600 to 3100  (with lower response below 1600 ). The STIS MAMA detectors are photon-counting devices that process events serially. They can be used to take data in either an accumulate (ACCUM) mode in which a time-integrated image is produced, or in a time series (TIME-TAG) mode in which the detector location and time of arrival of each photon are recorded as an event stream (see Section 11.1.2 and Section 11.1.3, respectively). The primary benefits afforded by the STIS MAMAs, in comparison with previous HST UV spectroscopic detectors such as those of the GHRS and FOS, are high spatial resolution, two-dimensional imaging over a relatively large field of view, and low background for point sources. The MAMA detector was developed by J. Timothy and R. Bybee for X-ray and UV imaging applications. The properties of the STIS MAMA detectors are summarized in Table 7.7.
Table 7.7: STIS MAMA Detector Performance Characteristics
FUV-MAMA Performance
NUV-MAMA Performance
Cs2Te
1024 1024
1024 1024
25 25 micrometers2
25 25 micrometers2
Image mode
pixel plate scale
0.0245 0.0247 arcsec2 (clear)
0.0246 0.0247 arcsec2 (filtered)
0.0245 0.0248 arcsec2
25.1 25.3 arcsec2 (clear)
25.2 25.3 arcsec2 (filtered)
25.1 25.4 arcsec2
9% @ 2537
5 106 to 6 104 counts/s/pix
8.6 104 to 2.7 103 counts/s/pix
Global count rate
linearity limit1
Local count rate
linearity limita
1
Rate at which counting shows 10% deviation from linearity. These count rates are well above the bright object screening limits.

Figure 7.13 and Figure 7.14 illustrate the design of the FUV and NUV-MAMA, respectively. A photocathode material is deposited on the front surface. The FUV-MAMA has an opaque CsI photocathode deposited directly on the face of the curved microchannel plate (MCP); the NUV-MAMA has a semi-transparent Cs2Te photocathode deposited on the back side of the detector’s entrance window.
Target photons strike the photocathode, liberating single photoelectrons which pass into the microchannel plate (MCP). There they are multiplied to a pulse of ~4  105 electrons. The pulse is recorded by an anode array behind the photocathode and detected by the MAMA electronics which process it, rejecting false pulses and determining the origin of the photon event on the detector.
The FUV-MAMA has a field electrode (repeller wire) which is used to repel electrons emitted away from the microchannel plate back into the channels. This provides an increase in quantum efficiency of the detector at the price of a small increase in the detector PSF halo. The repeller wire is normally on for FUV-MAMA observations (but see Section 7.4.4).
Figure 7.13: Design of the FUV-MAMA
Figure 7.14: Design of the NUV-MAMA
7.4.2 MAMA Spectral Response
The spectral responses of the unfiltered FUV and NUV MAMAs are illustrated in Figure 5.9. The peak photocathode response of the FUV-MAMA occurs at Lyman-α. Its spectral response is defined by the cutoff of the MgF2 window at 1150 at short wavelengths, and by the relatively steep decline of the CsI photocathode at long wavelengths. Out-of-band QE at longer wavelengths (>2000 ) is <10–6 yielding excellent solar-blind performance. The NUV-MAMA spectral response has a relatively flat maximum (~10%) that encompasses 1800–2600 . The photocathode QE declines to ~4% at 3150 , while at longer wavelengths the out-of-band QE is ~10–4. (See also Section 5.3.3.)
7.4.3 MAMA Sensitivity
The STIS MAMA detector modes, similarly to those of the STIS CCD, suffer from changes in sensitivity which depend on both temperature and time. A STIS Sensitivity Monitoring program similar to that aimed at characterizing the CCD behavior has been used to characterize the MAMAs (see Section 7.2). The well-known sensitivity of the FUV-MAMA to temperature for the first-order mode G140L has been confirmed to be 0.30%/C. No significant change with temperature for the NUV-MAMA first-order G230L mode has been registered. Following a correction for the temperature dependence, the sensitivities of the FUV first-order modes decrease linearly with time by wavelength-dependent amounts ranging up to a few percent per year. For the NUV first-order configurations, the sensitivities increased during the 1.5 years of STIS operations and then began to drop, by wavelength-dependent amounts comparable to those in the FUV. There was a significant slow-down in the decline of the time-dependent sensitivity (TDS) of all STIS observational modes beginning in 2002. All detectors continued to decline during the years STIS was inoperative. For STIS Echelle modes, the TDS corrections adopted are taken to be the same as for the corresponding low-order modes. Note, however, that new photometric throughput tables have been created based on Cycle 17 data. TDS corrections for all STIS spectra are implemented in the data reduction pipeline (see Section 15.1). Synphot, pysynphot, and the ETC also include TDS corrections for STIS data. Currently these default to the estimated throughputs for April, 2015.
Figure 7.15: Relative Wavelength-Averaged Sensitivity of STIS MAMA First-Order Low-Resolution Modes G140L and G230L as a Function of Time
7.4.4 Optical Performance
Both MAMAs exhibit low-level extended wings in their detector point spread functions (PSFs), with the NUV-MAMA PSF being considerably worse. Sample MAMA detector PSFs are shown in Figure 7.16. For those wishing to model their effect on absorption or emission line equivalent-width measurements or coronagraphic observations, the LSFs and detector PSFs are maintained on the STScI STIS website. Data for spectral modes can be found at:
http://www.stsci.edu/hst/stis/performance/
spectral_resolution/
and for imaging modes at:
http://www.stsci.edu/hst/stis/performance/image_quality/.
Figure 7.16: MAMA Detector PSFs
 
The FUV-MAMA includes a repeller wire that establishes a field above the microchannel plate and reflects forward-ejected photoelectrons back into the microchannel pores. The repeller wire is normally on for FUV-MAMA observations, but an improvement to the FUV-MAMA PSF (at the expense of a 35% decrease in sensitivity) can be made by disabling the high voltage to this wire. This procedure is only recommended for observations that use the E140H, and perhaps also the E140M, gratings when used with the 0.1X0.03 aperture (sometimes called the “Jenkins slit”) for observations shortward of 1400 . In pre-launch testing, resolutions as high as R ~ 220,000 were obtained in observations of a mono-isotopic emission line lamp in highres mode (see “Highres”), and R ~ 200,000 has been achieved on-orbit (Jenkins 2000, BAAS 32, 731, and Jenkins & Tripp 2001, ApJS, 137, 297). Figure 7.17 shows the effect of disabling the repeller voltage for the case of an observation of a line lamp with the E140H CENWAVE=1234 setting. Note that the main difference is not the FWHM of the central core, but a decrease in the intensity of the line wings.
Figure 7.17: Average Profile of Calibration Lamp Line at 1234 with the Repeller Wire On and Off
Only a small number of proposals per cycle (of the order of one to two) requesting the repeller off mode will be accepted. Note that repeller off observations will require special treatment, so a scientific case will need to be made for why these observations are necessary.
Also note that, due to the large PSF of HST in imaging mode (currently 3.5 low-resolution pixels), there is no advantage in performing FUV-MAMA imaging observations with the repeller wire voltage turned off.

Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 22 > Chapter 7: Feasibility and Detector Performance > 7.4 The MAMA Detectors

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