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ISIS Setup

Overview

Roughly one month before the observations take place you should have read the observer's proposal which you can access on the schedules page from within the ING network by selecting the programme reference. The proposal should contain all the details of the required configuration (CCDs, dichroic, gratings, blocking filters and central wavelengths). You should ask the PI to confirm the setup in your pre-run contact email. You should be able to advise on the use of a blocking filter (more details here). You should also check that the required configuration is met by the engineering schedules. If this is not the case contact the WHT manager.

Starting the observing system

A detailed procedure describing how to start and shut down the observing system can be found here.

Physical setup: dichroic, dekker and gratings

Note 1: When LIRIS is mounted the ISIS polarisation filters (MF-POL-PAR and MF-POL-PER), located in the main colour filter slide in the A&G box, are replaced by the LIRIS polarimetry half-wave plates along with the instrument change. The SA rostered on the first night following a change from LIRIS back to ISIS should check on the mimic that the ISIS polarisation filters have been replaced. Be aware that on occasions other instruments such as Ultracam can be scheduled between LIRIS and ISIS runs. If the ISIS polarisation filters aren't summarised in the mimic send an email to the ISIS specialists.

Note 2: If you're switching from an ISIS polarisation or image-slicer run back to a long-slit spectroscopy run, remember to move or change the relevant components before starting the new setup:

When switching from spectro-polarimetry mode you'll need to change to the observing dekker, and move the calcite, half- or quarter- waveplates, and probably mainfiltc out of the optical path, and also bring the blue and/or red collimator values to the non-polarimetry anastigmatic range (ISIS Setup for Spectropolarimetry).

When switching from imaging polarimetry you should swap the mirror in the imaging-polarimetry arm to the required grating irrespective of what is indicated in the ISIS MIMIC (Image Polarimetry with ISIS).

After imaging-polarimetry or image-slicer runs switch back to long slit mode with the longslit command:

SYS@taurus> longslit

You can now proceed to physically change the dichroic, dekker and gratings as needed (note that even if these components as needed are indicated on the mimic you should check that they are actually deployed).

To change the dekker, dichroic or below-slit filters first move the dichroic out of the beam for easy access:

SYS@taurus> bfold 0

Then move the dekker out:

SYS@taurus> dekker 1

Then unlock the slit door:

SYS@taurus> slit_door open

You can now open the slit door located on top of the red cryostat. Inside you will have access to the dichroic, filters and dekker. Remove the filter slide (RFILTA) to protect filters from being accidentally damaged. Pull the pin that holds the dichroic and carefully slide the dichroic out. Put the dichroic back in its sealed box at the bottom of the WHT observing floor cabinet. Take the new dichroic out of its box and carefully slide it in and lock its pin holder.

Proceed in a similar way with the dekker unit. Just pull it out, put the dekker back in its box and introduce the other one in the unit. Be careful to arrive to the end and make sure that the dekker is locked.

Close the slit door securely by snapping the locks. Finally lock the slit door in the control window:

SYS@taurus> slit_door close

put the dekker in clear position:

SYS@taurus> dekker 8

and update the mimic:

SYS@taurus> setdichroic <dichroic name>

SYS@taurus> setdekkerset <dekker name>

The dekker name can be either observing, standard or polarisation. Here are images of the available dekkers. The Prot dekker is used to protect the slit when ISIS is off the telescope. For the standard ISIS runs the observing dekker should be used. It has the same clear parts as the dekker standard but also eliminates ghosts in the blue arm caused by a dichroic.

If you have changed a dekker click on the "Update filters" button in both the "ISIS Observer" and "ISIS Eng." tabs of the Instrument Control Console so that the dekker drop-down menus are updated.

Now you can proceed to change the gratings, e.g.:

SYS@taurus> setgrating red R1200R

to change the red grating to R1200R. Then answer yes to access the grating door. The doors are then unlocked and can be opened manually. To release a grating hold it by its handles, push the "open" switch and gently pull it out from its holder. Place it back in its box and insert the new one.

You must ensure when you load a grating in the grating cell that the blaze arrow on the back of the grating points towards the left for the red arm, and towards the right for the blue arm, i.e. gratings should be inserted blaze-to-collimator. If the grating is inserted in the opposite sense, i.e. blaze-to-camera, then throughput is reduced by up to an order-of-magnitude.

Never touch the surface of a grating. Inspect visually all gratings that you put in and out and compare with a list of known scratches on the gratings. Report any unusual findings to the ISIS instrument specialist.

Once a grating is in place hold it by its handles and push the "close" button (place your fingers away from the three grating clamps!). Finally, securely close the grating doors by snapping the door locks.

Set the slit width to ~0.5-0.7 arcsec; don't close the slit more than this since the intrinsic line-width will not be fully sampled on the CCD.

SYS@taurus>  slitarc 0.7

Set the red and blue central wavelengths to the values requested by the observers, e.g.:

SYS@taurus> cenwave red 7500

The red fold mechanism should always be left in the mirror position ("rfold 0", or "rfold mirror") to direct light to the red arm. Set the blue fold mechanism to position the dichroic to the required position:

SYS@taurus> bfold 2

to observe in both red and blue arms simultaneously,

SYS@taurus> bfold 1

to observe in the blue arm only.

SYS@taurus> bfold 0

to observe in the red arm only. Note that arc lines falling in the attenuated wavelength range of the dichroic will appear stronger in single-arm configurations.

Insert the order sorting filter GG495 if needed:

SYS@taurus> rfilta 3

Deploy the comparison mirror and turn on calibration lamps:

SYS@taurus> agcomp

SYS@taurus> complamps cune+cuar

Set the correct CCD window:

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

(should be OK for red arm + REDPLUS)

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

(should be OK for blue arm + EEV12)

SYS@taurus> window red 1 "[1:1072,440:739]"

(should be OK for red arm + QUCAM)

SYS@taurus> window blue 1 "[1:1072,440:739]"

(should be OK for blue arm + QUCAM)

Do not bin the CCD. Use fast readout speed to quicken the process:

SYS@taurus> rspeed red fast

SYS@taurus> rspeed blue fast

Cryostat alignment


You are now ready to align the cryostat, that is, align the spatial axis with the detector rows, ensure that the CCD is not tilted with respect to the focal plane, focus the spectrograph, and finally check that the collimator position for the best spectral focus also produces a good spatial focus. Complementary information on this procedure is available.

Note that the spectral and spatial directions are not orthogonal in either arm of ISIS. By default the spatial direction is aligned with the detector rows since this simplifies sky subtraction. It is of course possible to align the dispersion direction with the detector columns instead, but in this case precise alignment won't be maintained on-sky because ISIS does not have an ADC.

In order to check for the rotation, it is good practice to first check that the CCD focus and CCD tilt are broadly OK. The reason for this is that lines used by setup script need to be reasonably and uniformly sharp across the CCD. If you are going to use a dichroic, check the rotation with the dichroic deployed since the dichroics can introduce some image rotation, especially in the blue arm. Also, if you notice an unexpectedly large rotation between two gratings it's wise to check the grating is firmly seated before embarking on rotating the cryostat.

Be aware that configuring the setup is an iterative process, and that there is "cross-talk" between e.g. rotating the cryostat and adjusting the cryostat tilt. Therefore if you need to modify the tilt after setting the rotation, re-check the rotation again. After the final mechanical intervention for rotation and tilt, tighten rotation bolts, Allen-bolt locks and capstan clamps, and make a final check that rotation and tilt remain acceptable. Finally, with the spectrograph anastigmatic (see below) fine-tune the focus by adjusting the collimator (this process does not involve mechanical intervention with the cryostat).

CCD rotation

Start IRAF and load the isis package: in a shell on whticsdisplay type iraf, and at the ecl prompt in the iraf window type

ecl> ing

ecl> isis

Start by moving the collimators to the approximate centre of the anastigmatic range taking into account the focus offsets of the optical components deployed, in order to avoid spectrograph astigmatism. Next check that the CCD focus and tilt are more or less OK. Take a test exposure:

SYS@taurus> glance red 3

SYS@taurus> glance blue 60

Check that you get reasonably intense arc lines; it's important that arc lines aren't saturated, and those used in the setup scripts should have signal-to-noise of at least ∼15 to obtain consistent results when using the calibration scripts. Now take an arc exposure:

SYS@taurus> arc red 2 "Rotation test"

In IRAF, run the isis_rotation script with mode 1=arc lamp. Mode 2 is used when aligning the spectral direction with the CCD columns by using a narrow dekker, the 0.3-arcsec dekker in position 2 of the standard dekker slide, illuminated with a continuum lamp.

isis> isis_rotation r2345678

The IRAF script isis_rotation.cl extracts the spectra of an arc image in two windows separated spatially and cross-correlates them to determine any pixel shift due to rotation. The shift is then converted into a detector rotation offset in micrometer units (mm). The pixel shifts are measured directly on the arc image and are the fundamental numbers; the detector rotation and micrometer offset are calculations from a scale conversion and may be occasionally wrong (e.g. if the cryostat is rotated with respect to the nominal position).

For a well-aligned cryostat you should aim to have the pixel shifts between top and bottom as reported by the rotation script <0.5 pixel, preferably <0.25 pixel. If the rotation is larger than this limit, loosen the cryostat rotation bolts which attach the cryostat mounting ring to the spectrograph mounting ring, with an Allen key. Never loosen the two recessed bolts, which fix the spectrograph mounting ring to the spectrograph. Apply the recommended micrometer offset to the cryostat, clockwise (+) or anti-clockwise (-) as required. For anti-clockwise rotation of the cryostat you should lower the value on the micrometer, and for clockwise rotation you should increase the value on the micrometer. Re-tighten ~3 of these bolts which are the closest to the three capstans A, B and C.

Iterate this procedure until the rotation is within limit, then re-tighten all rotation bolts with the Allen key. In order not to over-tighten them, engage the long end of the Allen key in each bolt, and rotate the short end until it is reasonably "finger tight". Finally, back-off the rotation micrometer by a few complete turns, e.g. four, so it is not in contact with the stop even with flexure, to ensure pick-up noise is never transmitted through it to the cryostat.

Note that for 1200 gratings and H2400B grating, arc lines are slightly curved by approximately 2 pixels from centre-to-edge of the standard window.

CCD tilt

Take two exposures, one with the left Hartmann shutter closed and one with the right Hartmann shutter closed. Do not move the Hartmann shutter until the frame has been read out. The order in which the exposures are taken is not important. Make sure that spectral lines are not saturated and that the collimator is in the anastigmatic range (see CCD focus below).

You can use one of the following scripts:
1- this script to take the necessary images in both arms
2- this script to take the necessary images with the red arm only
3- this script to take the necessary images with the blue arm only

This is basically what the scripts do:

SYS@taurus> rhart l

(left Hartmann shutter closed)

SYS@taurus> arc red 4 "test hart l"

SYS@taurus> rhart r

(right Hartmann shutter closed)

SYS@taurus> arc red 4 "test hart r"

SYS@taurus> rhart 0

(Both Hartmann shutters open)

Now analyze the data with IRAF. First display one of the spectra taken and note the y-coordinates of three well-spaced spectral lines, i.e. near the bottom, centre and top of the detector. The positions need to be accurate only to within 10 pixels. They must not be saturated, so check red-arm spectra carefully, and choose lines that are strong (signal-to-noise at least ∼15; the arm lamps are faint in the blue arm), that are not doublets or blends, that are not too close to other lines and that are not located in the vignetted part of the CCD. Run the isis_tilt task, e.g.

isis> isis_tilt r2345678 r2345679 y1 y2 y3

where y1, y2 and y3 are the y-coordinates of the three fiducial lines, e.g. 600, 2000 and 3400, respectively. Apply the recommended capstan turns, if any, in order A, B, C. The capstan micrometers should be backed-off when turning the capstans.

When adjusting the capstans their Allen-bolt locks should first be loosened with an Allen key (3mm, stored in the torque screwdriver's box), and locked again after final adjustment. Never forcibly turn a capstan which is locked, and don't overtighten the Allen bolt (finger tight with the long arm of the Allen key engaged is good), in both cases to avoid wearing the threads on the capstan and/or faceplate. To adjust capstan A, loosen its M5 bolt using the torque screwdriver, and loosen slightly the M5 bolts of capstans B and C to prevent buildup of mechanical tension if applying large adjustments to capstan A (small adjustments to a capstan can be effected by loosening only its M5 bolt), while supporting the cryostat with your other hand. Then proceed similarly with capstans B and C. Never completely loosen all three capstan clamps simultaneously; this would cause the cryostat to fall. Ensure the M5 bolts of each capstan are tightened to a torque of 3Nm using the torque screwdriver after each adjustment cycle, in the order A, B and C; this constrains the most degrees of freedom soonest.

You should aim to have the top-bottom and left-right tilts restricted to <0.5 pixel, and preferably to <0.25 pixel of Hartmann shift. This means each capstan offset - overall, top-bottom and left-right tilt for A, B and C - would be less than about 0.1 turn (but the important numbers in judging the alignment are of course the Hartmann shifts). In this way degradation of optimal spectral focus will be negligible.

When you're happy with the capstan settings, back-off their associated micrometers again if you've used them to measure the capstan positions, to avoid transmission of pick-up noise to the cryostat. It's good practice at this stage to take another arc to check that there's been no induced change in rotation caused by the tilt adjustments.

Proceed similarly for the blue arm.

CCD focus

The nominal collimator values with no extra refractive components (dichroics, filters, polarisation module) between the slit and the collimators are 5100μ for the blue arm, and 9300μ for the red arm. The spectrograph should be focused with the collimators within ± 1500μ of these nominal values, otherwise it will be astigmatic due to de-collimation of the beam incident on the grating.

If the optimum spectral focus set by moving the collimator would move the collimator beyond this nominal range, then instead the spectrograph should be coarse-focused by moving the cryostat using the capstans so that the collimator remains within the anastigmatic range. So, conceptually the focus procedure involves setting the red and blue collimators to 9300 and 5100 respectively with no additional optics in the beam, reducing the Hartmann shifts as reported by the focus script to <1 pixel by adjusting the respective cryostat capstans, and then fine-tuning the focus to its optimum value by adjusting the respective collimator values.

If you subsequently deploy e.g. a filter then the appropriate focus offset must be applied manually by adjusting the collimator. The recommended values can be found here for D5300 and GG495 and here for remaining dichroics and filters.

Therefore, the focus procedure is:

SYS@taurus> rcoll 9300

SYS@taurus> bcoll 5100

Take two exposures, one with the left Hartmann shutter closed and one with the right Hartmann shutter closed. Use the same procedure as for CCD tilt above. Now run the isis_focus task:

isis> isis_focus r2345678 r2345679

If the Hartmann shift reported is >1 pixel turn each cryostat capstan by the recommended amount. Alternatively, if the Hartmann shift reported is <1 pixel apply the recommended collimator shift, i.e.

SYS@taurus> rcoll "value"

SYS@taurus> bcoll "value"

where value=original_value+shift.

Repeat this sequence until the recommended collimator shift is 200μ or less and the collimator value is in the anastigmatic range.

Don't forget to note the A, B, C, & D micrometer values down in the CCD capstan settings folder.

Finally, you can make a "sanity check" of the spectrograph setup by measuring the position and FWHM of three lines (top, centre and bottom of CCD) in three different positions (left, centre and right to ensure there's no significant rotation or focus change across the detector.

You should also check that the final central wavelength is correct, comparing with an atlas of cuar+cune lines. This is especially important for the higher resolution gratings, which have a correspondingly small spectral range.

Update the ISIS setup database when you are finished. The entries in this database are a useful complement to the nightlogs to identify specific setups when troubleshooting.

Blocking filters

Ideally the dichroics would block light at wavelengths below the cross-over from entering the red arm, making a blocking filter in the red arm unnecessary. In reality, the dichroic response is not perfect and some blue light can enter the red arm. ISIS is sensitive to light from ∼3000Å to ∼10000Å, and so second order blue light can contaminate red-arm observations at wavelengths redder than ∼6000Å, especially for targets which have strong blue continuum or line emission. If second-order contamination would be a problem a GG495 blocking filter, which blocks wavelengths below ∼4950Å and has ∼95% throughput at the remaining wavelengths, should be deployed. If the spectrograph is focused with the GG495 blocking filter in the light path the collimator offset is about +800 microns.

Second-order contamination can also affect blue-arm observations when the D7500 dichroic is used, with the second-order contamination being caused by wavelengths bluer than ∼3750Å. This can be prevented by using a BG395 blocking filter above-slit, but when this is used of course the blue arm is no longer sensitive to first-order light with wavelengths below ∼3950Å.

In the case of red-arm-only observations at wavelengths beyond ∼6000Å, i.e without a dichroic deployed, the use of a blocking filter is usually mandatory to avoid second-order contamination. Even if the science targets are very red the flux and telluric standards may not be.

The observer must ultimately confirm whether a blocking filter is to be used or not, but ought to be aware of the potential effects of not doing so.

This z-scaled image shows an integration with the R1200R grating centred on 8384Å of a bright, A0 star at zenith distance 52-degrees with no dichroic or blocking filter deployed, and with the slit oriented vertically. The fainter "ghost" upper spectrum is the second-order spectrum of the blue wavelength region centred on 4191Å. It is displaced spatially from the first-order spectrum due to cross-dispersion by atmospheric differential refraction along the vertical slit, and the separation of the two orders ranges from ~1.6-arcsec at the blue end to ~1.3-arcsec at the red end because of the wavelength dependence of differential refraction. The broad absorption features at ~8200Å and ~8680Å in the upper spectrum are second order H-delta and H-gamma respectively.

Re-focusing when changing dichroics or gratings

When the spectrograph is focused there are fixed offsets for the red collimator in case the dichroic is changed (see useful information).

When the spectrograph is focused with a different grating, check the focus offset caused by gratings.

Setup for spectropolarimetry

For spectropolarimetry, set up the spectrograph as described here.

Here is the procedure describing a change of ISIS polarimetry filters MF-POL-PAR and MF-POL-PER to the LIRIS half-wave plates in the Main Colour Filter Tray. For ISIS spectropolarimetry, you will need to replace the LIRIS half-wave plates with ISIS polarimetry filters. Follow the same procedure as above but the other way around.

Setup for imaging polarimetry

For imaging polarimetry set up the spectrograph as described here.

Setup for fast and faint-object spectroscopy

The scripts isis_rotation, isis_tilt and isis_focus recognize QUCAM CCDs from the image headers, and the setup procedure is the same as for normal CCDs.

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Contact:  (ISIS Instrument Specialist)
Last modified: 11 September 2017