- Gemini Home
- Telescopes and Sites
- Science Visitors at Gemini
- Observing With Gemini
- Visiting Instrument Policy
- DSSI Speckle Camera (North)
- TEXES (North)
- Integration Time Calculators
- Adaptive Optics
- Magnitudes and Fluxes
- Near-IR Resources
- Mid-IR Resources
- Observing Condition Constraints
- Performance Monitoring
- SV/Demo Science
- Future Instrumentation
- Queue and Schedules
- Data and Results
Change page style:
Detector Properties Summary
The table below summarises the NIFS detector properties. Additional important information on the detector array is given below.
|NIFS Detector Basic Parameters|
|Type||Rockwell HAWAII-2RG HgCdTe|
|Array Size||2048×2048 pixels (2040×2040 active)|
|Pysical Pixel Size||18μm|
|Pixel Scale||0.043" along slit|
|NIFS Detector Read-out Modes|
|Mode Name||No. of Samples||Read-Out Time/
|Bright Object||1||5.3 sec||∼5.8||15.0||Medium Object||4||21.2 sec||∼3.1||8.1||Faint Object||16||84.8 sec||∼1.8||4.7|
The NIFS spectrograph detector is a Rockwell HAWAII-2RG (H2RG) device with 2048x2048 18μm pixels. The outer four pixels on each side are not illuminated, and so act as reference pixels. This leaves an active area of 2040x2040 pixels.
The HAWAII-2RG detector is sensitive to light out to 2.6μm, and uses a HgCdTe detector layer. It uses four output amplifiers that simultaneously read out 512x2048 pixels in around 5 seconds. Rather than using a shutter to control the duration of a given exposure, the recorded image is actually the difference in signal between two read-outs of the detector: one at the start of the integration, and one at the end. For this reason, the minimum permitted exposure time is determined by the read-out time.
There are several settings used to read the NIFS detector, depending on the source brightness and noise characteristics. Unlike charge-coupled devices (CCDs) commonly used at optical wavelengths, the charge stored on a particular pixel can be read multiple times without destroying the charge. Each read of the detector has some uncertainty (read noise), which can be reduced by averaging over several reads (a technique known as 'Fowler sampling', Fowler & Gatley 1990, ApJL, 353, L33). The reduction in read noise comes at the cost of larger overheads. Details of the three read-out modes currently implimented for NIFS (Bright, Medium and Faint Object) are given in the table above.
the NIFS detector is sensitive to cosmic rays, which appear as diffuse patterns that can extend over tens of pixels. They typically do not saturate the detector, adding only a few hundred electrons to the pixel signal. However their diffuse nature makes them rather destructive to the data signal. For this reason, multiple shorter exposures are preferred over few longer exposures, as far as signal-to-noise requirements will allow. Exposures longer than 20 minutes should be avoided, which is in any case a similar timescale to the variations in the night-sky background.
Dark Current and Bad Pixels
The dark current level in the NIFS detector is very low and stable, and has been measured as less than 0.01e-/s/pix. Hot pixels and 'debonded' cool pixels affect a few percent of detector pixels. Hot pixels have a characteristic 'plus sign' shape due to capacitance coupling of neighbouring pixels, causing a leakage of the hot pixel charge to its neighbours.
Bad pixels in science data can be corrected by subtracting an exposure of equal integration time, either in the form of an associated sky observation, or a combined stack of daytime dark frames, each having the same integration time as the science exposure. Daytime darks are particularly recommended if the sky emission lines are to be used for wavelength calibration. Daytime darks should be requested by the PI in their Phase II submission.
The NIFS detector suffers from image persistence, which causes saturated images to appear as faint artifacts in subsequent exposures. These ghost images can persist for several hours. This is particularly noticeable when the NIFS grating setting is changed, since bright sky emission lines from the previous setting can remain as artifacts in subsequent exposures.
Care should be taken to avoid saturation of the detector, and to plan observing strategies in ways that reduce the frequency with which the grating position is changed.
Saturation of the NIFS detector occurs at about 48,000 ADU, which will also result in strong persistence effects, affecting subsequent images for up to several hours. Keep the counts below ∼40,000 ADU per coadd! Furthermore, the detector response becomes >6% nonlinear at ∼38,000 ADU.