The PolCor "Lucky" Polarimeter/coronagraph
PolCor is a combined "Lucky" imager, polarimeter, and coronagraph
built for NOT by Göran Olofsson and Hans-Gustav Florén, Stockholm.
Compared to a general purpose instrument like ALFOSC, PolCor has the following
1. Sharper images (typically 0.7 -> 0.4 arcsec without wasting frames and -> 0.2-0.3
arcsec with frame selection)
2. Much higher time resolution (milliseconds, if needed)
3. Much better PSF (higher image contrast)
4. Much better coronagraphic performance
5. Much less interference fringes
6. More accurate sky subtraction
7. More accurate colour index measurements
8. No time loss for reading out
The disadvantage is a small field (1 arcmin) and no spectroscopic mode. The data volume is
also much larger and the data reduction more time consuming.
The all-mirror re-imaging optics is (with good margin) diffraction limited and the reflectivity
of the 4 mirrors in the light path is 99.5% each (over the sensitivity range of the detector)
resulting in only 2% losses. The relay optics has a 1:1 imaging which results in a pixel scale
of 0.12 arcsec/pixel. Only shift-and-add (i.e. correcting for image motion) typically improves
the seeing from 0.7” in staring mode to 0.4”. If one uses frame selection (“Lucky imaging”)
and deconvolution, the resolution will improve to 0.2 – 0.3 “, but at the expense of the
limiting magnitude. Barlow lenses with x2 and x3 are available, which would be needed for
speckle interferometry. The all-mirror optics (except for filter and cryostat window)
minimizes the risk for ghosts (we have so far not detected any ghosts). In order to limit the
extent of diffraction stripes, PolCor has a computer controlled Lyot stop that masks the
secondary mirror support blades. This mask is slightly undersized to block the diffraction
rings caused by the coronagraphic disks (and thereby lower the PSF wings by 1-2 orders of
The EMCCD camera (Andor IXON) uses a thinned 512x512 CCD array with 16 micron
pixels, giving a full field of 1 arcminute. It can be used both in classical mode (with a read-out
noise of 6 e- rms) and EM mode with an on-chip gain up to 1000. For low light levels it can
be used in a photon counting mode (fastest full-frame readout rate 33 Hz), which is in
principle noise-less, but in practice limited by clock induced pulses, which occur typically
once for 200 readouts. With broad band filters the sky emission is too high for photon
counting, but it has been found that the EM mode is linear over a wide range and this is the
normal mode of operation. In practice, all frames are stored, so the mode of operation is a
Th QE is not particularily high (around 30%) in the UV, but on the other hand, the AR
coating is efficient at longer wavelengths and we have seen no interference fringes caused by
the OH sky emission.
Very high time resolution can be achieved by limiting the readout area of the chip, making
namspeckle interferomerty possible.
There is a choice of 3 sizes (1.5, 3 and 6 arcseconds in diameter) coronagraphic disks each
size with a choice of 3 different optical densities (2, 3.5 and 5 equivalent to 5, 8.75 and 12.5
magnitudes). The reason for not using totally opaque disks is to allow centering
and monitoring the star. The Lyot mask is rotating in the same sense (but opposite direction)
as the field rotator in order to cancel the effect of spider deffraction.
The polarizing element is a high-quality polarizer which is designed for the 410 – 750 nm
region). It is rapidly turned to the 4 positions (0, 45, 90 and 135 degrees) and “dark”
repeatedly many cycles to average atmospheric variations.
PolCor is equipped with Bessel U, B, V, R and I filters. In addition very narrow-band filters
(0.3-0.5 nm) are also available for the lines FeI 386 nm, CaII 393, NaI 589, KI 767, and CaII
854. The purpose of these filters is observations of circumstellar resonance scattering. The
filter holder can take 2 filters at a time and in order to cancel sky variation in filter ratio
measurements, Polcor has a mode of operation that repeatedly change between the two
filters. It is a relatively simple matter to change filter holder, and other filters out of the NOT
list with diameter 50 or 60 mm can be used.
A beam switching mode is being prepared in order to make it possible to measure low surface
brightness objects without the usual difficulties in determining the sky level.