ING Banner
Home > Astronomy > ISIS > Imaging-polarimetry SA notes


ISIS imaging-polarimetry SA notes

  1. Before a run
  2. Configuring the spectrograph for imaging polarimetry
  3. Configuring the telescope
  4. Useful information

Before a run

  • Ask the optical engineer to change LIRIS halfwave plates for ISIS polarizers MF-POL-PAR and MF-POL-PER, if before the run they are not mounted in the main colour-filter slide in the WHT A&G box.

  • Check well in advance which filter(s) are requested by observers, so that there is enough time if some filter slides modifications are necessary.

Back to the top

Configuring the spectrograph for imaging polarimetry

  1. Mount the calcite analyser

    The calcite analyser (Fig. 1) should be mounted in the multi-slit position of the ISIS slit carriage. You may have to remove the image slicer first which is there by default. Note that the below-slit calcite (Savart plate) is NOT used for imaging-polarimetry but only for spectropolarimetry observations.

    First put the dichroic out of the beam for easy access:

    SYS@taurus> bfold 0

    Then protect the slit unit with the dekker (note that the dekker out, that is in position 1, is necessary to be able to open the slit door):

    SYS@taurus> dekker 1

    Now we will move the multi-slit unit to the light path. In order to have a correct information in the ISIS Mimic, Instrument Control Console and image headers, locate ISIS Observer tab of the Instrument Control Console, and in the Slit Unit section choose "Imaging polarimetry" option. This will move the multi-slit unit to the light path, and the image-header keyword ISISLITU will show IMAGE_POL.

    Then unlock the slit door:

    SYS@taurus> slit_door open

    You can open the slit door located on top of the red cryostat. Inside you will have access to the slit unit, dichroic, filters and dekker. Carefully slide out the image slicer (if it was deployed in the multi-slit unit), put it in it's box and store it in the WHT observing-floor cabinet. Take the analyser unit, also stored in the WHT observing-floor cabinet, out of it's box, carefully slide it in and tighten the bolt by screwing it in (see Fig. 2).

    If you want to change filters (see next section) proceed in a similar way with filter units, just pull them out, put them back to their boxes and introduce new ones in the unit. Be careful to arrive to the end and make sure they are properly in.

    Close the slit door and lock it:

    SYS@taurus> slit_door close

    You can leave the dekker in position 1 because in the imaging polarimetry mode the dekker position does not matter - the dekker is always above the long slit which moves away from the light path.

    For observations with the blue arm the dichroic should be preferably D5300 and the bfold in a mirror position:

    SYS@taurus> bfold 1

    For observations with the red arm the dichroic should be out of the beam:

    SYS@taurus> bfold 0


    calcite unit

    Fig. 1 -  The analyser unit for imaging polarimetry. The unit should be mounted in the ISIS multi-slit position. The calcite is below the dekker field mask (in yellow).

    analyser unit

    Fig. 2 -  The position of the analyser unit inside the ISIS slit area. The analyser unit should be fixed in its position tightening the bolt.

  2. Mount the filters

    Colour and/or neutral density filters have to be mounted in filter holders that were specially adapted for imaging-polarimetry observations (Fig. 3). These filter holders are designed to deploy 50x50-mm square filters, and can cater for some 50-mm circular filters too. Check in advance which filters are requested by the observer and if they fit in the available filter holders or wheter some modification has to be done (the filter thickness has to be taken into account too).

    The filter slides are then mounted in their position below the ISIS slit unit following the same procedure used to mount the analyser unit (it is a good idea to change the analyser and filters at the same time). Two filters can be mounted on each arm. Remember that it is recommended to use only one arm at a time.


    filter unit

    filter

    Fig. 3 - Top: one of the two filter holders used for the red arm. Similar can be mounted in the blue arm. Bottom: R filter mounted in the filter holder. Notice that black tape at sides of 50x50-mm square filters is needed to avoid a stray light.

    Normal filter slides hold two filters, while the slides modified for imaging polarimetry hold only one. For imaging polarimetry observations, filter position 4 should be used. Therefore, to use a filter mounted in BFILTA (or BFILTB) slide type:

    SYS@taurus> bfilta 4 (or bfiltb 4)

    Similarly, to use a filter mounted in RFILTA (or RFILTB) slide type:

    SYS@taurus> rfilta 4 (or rfiltb 4)

    Inside ISIS note that slots to place the RFILTA and RFILTB filter holders are located below the dichroic while the ones for the BFILTA and BFILTB are located to the right side of the dichroic (see Fig. 2).

    When you are finished with filter changes, remember to update the filter database and choose the position number 4 for all filter slides.

  3. Mount the mirror

    The mirror should be mounted in place of the grating in the arm which is going to be used for observations. Just replace a grating with the flat mirror unit in a same way as changing a grating. Any valid name of a grating works fine with the mirror as it will be used in order 0. So, for example, to change the red grating to the mirror you can type:

    SYS@taurus> setgrating red R1200R

    Then answer "yes" to access the grating door. The doors are then unlocked and can be opened manually. In the dome, release the grating as usual with the "open" button, deploy the mirror, use the "close" button and lock the grating door.

    Then set the central wavelength to 0:

    SYS@taurus> cenwave red  0

    Follow the same procedure if you need to put the mirror in the blue arm.

    If both arms of ISIS are going to be used, it is recommended to use the old mirror in the blue arm and the new mirror in the red arm (see here).

  4. Put the retarder plate in the beam

    Deploy the halfwave plate (for linear polarimetry) or the quarterwave plate (for circular polarimetry) in the light path:

    SYS@taurus> hwin (for linear) or qwin (for circular)

    To take halfwave or quaterwave plate out of the beam, type:

    SYS@taurus> hwout or qwout

  5. Setup the detector

    Setup ISIS to take a flat-field exposure:

    SYS@taurus> agcomp

    SYS@taurus> complamps w

    SYS@taurus> compnd 4

    In the red arm, a 1 sec exposure with this ND filter produced a flat-field like the one presented in Fig. 4, with enough counts to check the focus in a next step. In the blue arm, a 1 sec exposure with compnd 3 will produce similar flat field.

    Set the appropriate window and readout speed of the detector as usual.

    The windows below can be used as a reference. They cover the whole field of view and include an overscan region on the right side (see Fig. 4)

    For a linear polarimetry:

    SYS@taurus> window red 1 "[680:2148,1700:2470]"

    SYS@taurus> window blue 1 "[695:2148,1580:2440]"

    For a circular polarimetry:

    SYS@taurus> window red 1 "[770:2148,1820:2300]"

    SYS@taurus> window blue 1 "[800:2148,1750:2280]"

    flat

    Fig. 4 - This window includes the field and overscan columns of the CCD (right end of the image). The double pattern of slits corresponds to the ordinary and extra-ordinary image of the comb mask as produced by the calcite analyser.

  6. Focus the spectrograph

    Set the collimator to a rough "nominal" focus using the commands:

    SYS@taurus> rcoll 9300 (for the red arm)

    SYS@taurus> bcoll 5100 (for the blue arm)

    Then make steps of r/bcoll values of 500 microns (the collimator units) around the nominal focus and take a flat-field exposure at each collimator value until the edges of the dekker are at their sharpest (as determined e.g. with IRAF-imexamine task), which will be the final collimator value. Use the same exposure time and ND filter as in the previous step. An example of flat fields taken at different spectrograph focuses (collimator values) is shown in Fig. 5.

  7. spectrograph_focus

    Fig. 5 -  Flat-field exposures at different collimator positions where spectrograph defocus can be seen. Top panels show images with a spectrograph in focus (rcoll 9300), middle panels show out-of-focus image (rcoll 11000) and bottom panels show even more out-of-focus image (rcoll 15000).

  8. Find the instrumental zero angles

    Zero angles are the angles of the retarder plate for which the contrast between the ordinary (o-) and extraordinary (e-) beams is maximized. The theoretical zero angles should be around 0 deg for a linear polarimetry and 90 deg for a circular polarimetry. However, zero angles in ISIS are known to have an offset. The table below summarizes the expected ISIS wave plate angles when doing linear and circular imaging-polarimetry observations.


    ISIS arm
    Polarimetry mode
    Retarder
    Angles (deg)
    Red
    Linear
    Halfwave plate
    8, 53, 30.5, 75.5
    Red
    Circular
    Quarterwave plate
    97, 187
    Blue
    Linear
    Halfwave plate
    11, 56, 33.5, 78.5
    Blue
    Circular
    Quarterwave plate
    97, 187

    To find the instrumental zero angles insert the MF-POL-PAR filter in the beam:

    SYS@taurus> mainfiltc MF-POL-PAR

    If this filter is not mounted in the A&G box (it can happen after a LIRIS run), proceed in a similar way as described in the LIRIS Setting-up web page, but other way around. MF-POL-PAR has a serial number 1000 and MF-POL-PER has a serial number 1001 in the ING filter database.

    Now you should take flat-field images around the expected zero angle:

    SYS@taurus> complamps w

    SYS@taurus> hwp <angle> or qwp <angle>, to move the required plate to a requested angle between 0-360 deg

    SYS@taurus> flat red 2 "angle"

    To measure the average brightness use the central o- and e- rays. You can use the iraf imstat command on two rectangular regions, which must have the same size. For example:

    cl> imstat r123456.fit[1][326:340,130:630]. For the o- ray.

    cl> imstat r123456.fit[1][359:373,130:630]. For the e- ray.

    Always use a fairly long region for good statistics on both rays. Take a note of the average count values and compute the difference. Do the same at remaining angles and record the angle of the maximum difference between both rays which will be the zero angle.

    Linear polarisation (using the hwp plate)
    Theoretically, for linear-polarisation observations, the target should be observed at the halfwave-plate angles 0, 45, 22.5, and 67.5 degrees. Hence, you should add +0, +45, +22.5, and +67.5 degrees to the zero angle you have found and use these angles for science observations by introducing them in the linear-polarimetry script at /home/whtobs/linimpolscript [1].

    It is a good practice to check that other plate angles (+22.5, +45, and +67.5) make sense. With the half-wave plate at 22.5 and 67.5 deg away from the zero angle the difference in the intensity between the ordinary and extraordinary beams should be minimal, at 45 deg maximal.

    Circular polarisation (using the qwp plate)
    We were feeding the spectrograph with linearly polarised light when we measured a zero angle (we used the MF-POL-PAR), and therefore a final zero angle is obtained by adding 45 degrees to the measured angle. That is, if 52 degrees was the zero angle with the MF-POL-PAR, then the angle in the script for circular polarimetry should be 52+45=97 degrees. We will use this angle and +90 degrees in the circular-polarimetry script at /home/whtobs/cirimpolscript [1].

    When you are finished, remember to remove the MF-POL-PAR filter out of the beam:

    SYS@taurus> mainfiltc out

Back to the top

Configuring the telescope

At the start of the first night when ISIS is used for imaging polarimetry, the telescope operator will determine the rotator centre on the direct-view camera (switching to agcomp) and will make a mark on the DS9 display (it is recommended to also write down the TV coordinates of this point in case the marks are erased). The telescope operator will also perform a seven-star calibration about this point in the direct-view camera.

Afterwards, follow steps described in imaging-polarimetry user guide.

Back to the top

Useful information

  • For an imaging-polarimetry user guide, click here.

  • If you want to configure ISIS from an imaging polarization into a longslit mode, proceed as following:

    • Replace a mirror by a grating using the standard procedure.

    • Remove polarization optics from a light path:

      SYS@taurus> hwout (qwout), moves halfwave (quarterwave) plate out

      SYS@taurus> longslit, moves the calcite analyser out of beam and moves to a long slit

      SYS@taurus> mainfiltc 1, removes polariser in the main colour-filter unit

      SYS@taurus> bfilta 1 (or bfiltb 1, rfilta 1, rfiltb 1), removes filters from a light path.

    • Set the appropriate window, e.g.:

      SYS@taurus> window red 1 "[555:1520,1:4200]"

      SYS@taurus> window blue 1 "[585:1550,1:4200]"

  • For the linear imaging polarimetry observations, it is usually not necessary to measure an accurate value of the zero angle. On the other hand, for the circular imaging polarimetry observations, the zero angle should be determined accurately.

  • Measurements (in millimetres) of the four filter slides:

    Filter slide
    Width (outer)
    Width (inner)
    depth to end-stop
    Height (thickness)
    Bfilt A
    90.7
    85.3
    77.2
    6 (slot is 3 mm high)
    Bfilt B
    92.0
    85.3
    77.2
    10 (slot in middle, not measured)
    Rfilt A
    95.4
    86.2
    109.8
    6 (slot is 3 mm high)
    Rfilt B
    89.9
    83.9
    109.8
    10 (slot in middle, not measured)

[1] These scripts are the same as for ISIS spectropolarimetry observations, except that for imaging polarimetry a waveplate does not move out of a beam during an acquisition.




Top | Back

Contact:  (ISIS Polarisation Specialist)
Last modified: 31 March 2017