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ISIS Blue Arm

The default CCD on the blue arm of ISIS is a thinned, blue-sensitive EEV12 array of 4096×2048 (13.5 micron) pixels.

  1. General information on the device
  2. Wavelength coverage and spectral resolution
  3. Spatial scale
  4. Fringing and cosmetic defects
  5. Linearity measurements
  6. Shutter effect
  7. Charge spreading and its effect on resolution
  8. Flux standard data and empirical through-puts
  9. Quality control history
  10. Bad pixel masks
  11. Atlas of arc lines in the blue arm

Wavelength coverage and spectral resolution

The table below gives the dispersion provided by each grating when mounted blaze to collimator (see the ISIS manual for more detailed information on gratings and their properties), and the spectral range covered by the EEV12 CCD. The EEV12 is mounted on the blue arm with its 4096 pixel axis along the dispersion direction, giving maximum utility of the beam width leaving the camera. However, the camera optics vignette the outer regions of the dispersed light beam such that approximately 600 pixels at either end of the CCD are vignetted. A plot of the CCD vignetting function across the chip is shown below to illustrate this effect. This function was measured in May 2011 from a flat-field exposure corrected by CCD quantum efficiency, grating efficiency and tungsten lamp spectral emissivity functions. The unvignetted region is from (spectral) pixel 665 to 3485, which is essentially the central 2820 pixels, and both the unvignetted and 50% vignetted spectral ranges in Å are given in the table below.

The dispersions of the blue-arm gratings in Å/mm are 120 (R158B), 64 (R300B), 33 (R600B), 17 (R1200B) and 8 (H2400B). The pixel size of the EEV12 detector is 13.5 microns, and the corresponding grating dispersions in Å/pixel are listed in the table, as are the slit widths that project to four pixels (54 microns) with the gratings set at blaze. The spectral resolution elements, Δλ, in Å for a 1-arcsec slit are also listed. The corresponding nominal spectral resolutions, λ/Δλ, at 4000Å with a 1-arcec slit are approximately 512 (R158B), 976 (R300B), 1980 (R600B), 4706 (R1200B) and 11429 (H2400B). These values exclude the impact of diffusion of charge between pixels, which will degrade resolution by at least 10% for wavelengths ≲6000Å. Resolutions for other slit widths and wavelengths can be computed with the SLITTOOLS calculator.

Note in the table that the slit width projecting to four pixels increases with grating resolution. This is due to grating anamorphic de-magnification, which is parameterised by cos(θ+φ/2)/cos(θ-φ/2), where θ is the grating tilt with respect to zero order and φ is the camera-collimator angle. This relation demonstrates why the slit size projecting to four pixels is larger for the higher resolution gratings; they are set to larger tilt angles for a given central wavelength, and so their de-magnification is greater. See here for a discussion of this effect.

ISIS wavelength coverage and resolution with EEV12
Grating
Blaze
Total Spectral range (Å)
Unvignetted range 2820 pixels (Å)
50% unvignetted range 3670 pixels (Å)
Dispersion (Å/pix)
Slit-width for 54 mu at detector (in arcsecs)
Resol. element with a 1" slit (Å)
R158B
3600
6635
4568
5944
1.62
0.83
7.81
R300B
4000
3539
2436
3170
0.86
0.84
4.10
R600B
3900
1825
1256
1636
0.45
0.89
2.02
R1200B
4000
940
646
842
0.23
1.08
0.85
H2400B
Holo
442
304
396
0.11
1.24
0.35

According to sampling theory a line as recorded on the detector is fully sampled if it has at least two dispersion elements across its FWHM, and so the detector oversamples the resolution element when the slit width is set to 1-arcsec (e.g. to approximately match seeing). In this configuration the detector can be binned ×2 spectrally to increase the signal-to-noise in each wavelength bin, without loss of spectral resolution. This can also be done at the reduction stage, but binning on-chip reduces the readout noise contribution to the resolution element.

It is also possible of course to improve spectral resolution by reducing the slit width. This increases slit losses especially in moderate seeing, and in any case the slit should project to at least two pixels so that the resolution element remains fully sampled by the detector.

Spatial scale

The blue (and red) camera is a folded Schmidt design of focal length 500mm and gives a scale of 14.9 arcsec/mm along the slit. Hence a spatial scale of 0.2 arcsec/pixel is achieved with the EEV12. It is possible to bin in the spatial direction if one is not concerned with high spatial resolution observations, indeed the seeing conditions need to be excellent to allow full advantage to be taken of using an unbinned chip with this pixel scale. The maximum unvignetted slit-length usable with ISIS is 3.7 arcmin (corresponding to 1100 spatial detector pixels, spanning ~[400:1500, 1:4096]).

Fringing and cosmetic defects

These thinned chips suffer severely from fringing in the red part of the spectrum, which limits their usefulness in this region despite their continued good QE down to 8000 Å. Click here to see an illustrative flat field spectra.  The following figures are illustrative:
 
Wavelength     Peak-to-Peak Amplitude
6500Å                 5%
7000Å                 15%
7500Å                 30%
8000Å                 50%   
8500Å                 60%
9000Å                 60-70%
There are a few cosmetic defects on the surface of the chip, but nothing particularly severe.

Linearity measurements

A linearity test in standard readout mode with no binning showed the chip to be linear to better than 1% up to just over 60,000 ADU.

Shutter effect

The Prontor shutter opens the aperture radially symmetrically. The count levels on a series of exposures with requested integration times 2, 1, 0.5, 0.25, 0.13, 0.06, and 0.03 sec suggest that the overhead for opening and closing the shutter is ~ 0.04 - 0.05 sec. An exposure of 0.03 s yields fewer counts, probably due to the shutter not being fully opened. If an exposure time of 0.01 sec is requested, the exposure fails. To clear the error state, type in the instrument control system

    SYS@taurus> dasreset blue

Remember to check the CCD readout-speed and binning after the dasreset. For observations of spectrophotometric standards we recommend a minimum exposure of 2 sec.

Charge spreading and its effect on resolution

The diffusion of charge between pixels during integrations degrades both the spatial and spectral resolutions. For a back illuminated CCD this charge diffusion becomes progressively worse for shorter-wavelength incident light; as wavelength decreases, absorption of photons occurs closer to the surface of the CCD where the pixel potential wells are less-well defined. Photoelectrons generated closer to the surfave have a greater tendency to diffuse into the wells of neighbouring pixels, thereby degrading resolution in both the spectral and spatial directions.

In the spectral direction, using a slit-width projecting to 2 pixels on the detector results in a measured FWHM of 2.4 pixels at wavelength λ~4000Å when the spectrograph is at best focus. Similarly a slit-width projecting to 4 detector pixels will produce a FWHM of ~4.4 pixels, again at λ~4000Å. This effect becomes less severe towards redder wavelengths and is negligible at around 6000Å.

The FWHM of the spatial profile in median seeing is similarly broadened from ~4 to ~4.4 pixels by charge diffusion. Note that the combination of charge diffusion and the λ-0.2 dependence of seeing means the spatial profile in the blue arm can be broader than in the red arm by several tenths of an arcsec at widely-spaced wavelengths, at optimum telescope focus.

Flux standard data and empirical throughput

The figure below shows the results from throughput measurements of flux standards. The Y-axis is the apparent AB magnitude of star observed at zenith which gives one detected photon per second per Angstrom. The lowest resolution grating was used (R158B) in the blue arm (without a dichroic) with a wide slit (10 arcsec). The conditions were photometric, with negligible dust levels present. This figure shows the response of the whole ISIS blue channel (i.e. WHT primary + secondary + ISIS blue optics + detector response) from ~3200 to ~8300Å.

Note that the H2400 grating vignettes significantly at ''redder'' central wavelengths because of its high inclination to the collimator in longer-wavelength settings, e.g., by ~20% at 5000Å, ~45% at 6000Å and ~100% at 7000Å.

Quality control history

The figure below shows the results from several throughput measurements of flux standards in both the blue and the red arms and with different detectors. The Y-axis is the apparent AB magnitude of star observed at zenith which gives one detected photon per second per Angstrom. In each case the lowest resolution grating was used (R158B) in the blue arm (without a dichroic) with a wide slit (10 arcsec). In each case, the conditions were photometric, with negligible dust levels present.

Bad pixel masks

Bad pixel masks for EEV12 with different binning were created using noao.imred.ccdred task in IRAF. All masks are created for the default CCD window [585:1550,1:4200].

bad pixel mask bin 1 1           bad pixel mask bin 1 2           bad pixel mask bin 2 1

bad pixel mask bin 2 2           bad pixel mask bin 3 1           bad pixel mask bin 3 2

bad pixel mask bin 4 1           bad pixel mask bin 4 2

Atlas of arc lines in the blue arm

An atlas of arc lines for a range of central wavelengths of the blue arm gratings is available here.


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Contact:  (ISIS Instrument Specialist)
Last modified: 20 September 2016