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Swope Operation Manual
Swope Telescope operation manual
This manual describes how to take direct imaging CCD data on the Las Campanas 40-inch Swope telescope with the 4Kx4K E2V CCD231-84 detector. Last updated: December 13, 2023 (Nidia )
Activate telescope and instrument:
- Turn on console (rotate key).
- Turn power on.
- Check that platform is down.
- On TCS display enter COVER (the telescope will move to the COVER position).
- Turn the dome lights on from the LPLC (Local Programable Logic Controller; see below).
- Go upstairs, raise the platform with the hand paddle, and remove the telescope cover. The hand paddle power is enabled by the ON/OFF switch on the paddle, which has three functions allowing movement of the platform, the dome and the wind screen. Move the platform all the way down and disable the hand paddle power. Go back to the control room downstairs.
- On the LPLC push the ‘GO LOCAL’ button and turn the lights off.
- On TCS computer type ZENITH and answer yes to the question about the platform being down.
- Check that the TCS UT is right (compare with http://tycho.usno.navy.mil/what.html or similar). If not, fix it by entering the UT HH MM SS command.
The TCS and the guiders computers share the same monitor and keyboard.You can switch between them using the belkin KVM on the lightblue rack.
We recommend taking sky flats at twilight, which provide better correction (to 1% level) than domeflats. However, domeflats are useful for shutter and linearity tests. The domeflat position is reached by moving the telescope to HA=03:07E and DEC=-25:00 (on TCS type RA hh mm ss –where hh mm ss is the RA needed to reach the required HA– and DEC -25 00 00) and the dome to encoder reading 282 (type DOME 282 on TCS). The quartz lamp is turned on from a box on top of the light-blue rack (do not exceed 935 Volts).
- Turn on the fans from the switch in the next room.
- The dome shutter is controlled from the Local PLC panel. Preferably open the done with the telescope not pointing to Zenith. .
- The LPLC panel also allows control of the dome rotation, dome lights and wind screen, and indicates the status of the platform (DOWN in Figure 3). A member of the day crew will show you how to operate it.
- Start tracking by pushing ASCENCION RECTA on console.
- Lower the wind screen. This can be done either from the LPLC or from the hand paddle upstairs.
- To have the dome follow the telescope enter DOME AUTO on TCS. DOME AUTO needs to be typed again if for any reason a SLEW is aborted (otherwise it will remain in MANUAL and not follow the telescope).
- The pointing model has to be active: the TP indicator should show up in green; if this is not the case, enter TP on the TCS.
The SWOPE-CCD application consists of different controls:
1) Science Camera and Filter wheel control
2) Guiders control
3) Telescope control
In addition to these GUIs there are the image viewer (Quick look tool), the dewar status window, the airmass display and the object list window. A password protect mode allows access to the engineering GUIs.A detailed description of the application can be found here: http://instrumentation.obs.carnegiescience.edu/Software/Swope/
The detector is read out through 4 amplifiers producing four independent files called ccdnnnnc1.fits – ccdnnnnc4.fits. The quadrants as seen in the Quick-Look tool are named counterclockwise beginning from the top right quarter of the image (i.e., top right is c1, top left is c2, bottom left is c3 and bottom right is c4).
Science Camera and Filter wheel control
This window controls the CCD camera and the filter wheel. Exposures are started with the Start button. Macros can be started with the Execute button.
ExpTime is the exposure time in seconds for the next observation. For this parameter and the ones for Loops and File# the entry window will be highlighted red after the number is typed. The value is not recorded by the program until the user hits Enter. The exposure time can be changed at any time during the exposure. Remember to hit Enter to validate the new value.
Loops: Setting up a loop can be a convenient way to take flat fields and bias, or to make a series of observations in order to split the total exposure into shorter individual ones.
ExpType: The exposure type (saved in the fits header) can be set to “Object”, “Focus”, “Bias”, “Dark”, or “Flat”. Selecting “Bias” will automaticaly set the exposure time to 0 seconds. Selecting “Dark” will disable the shutter for the exposure. Selecting “Focus” will enable a focus sequence, automatically setting the loop number to 7 (this can be changed if desired). The focus frame will be saved under a normal filename (e.g. ccd0065.fits). In this frame, the spacing between the first and second images will be larger than for the rest of the sequence, allowing identification of the sequence order.
Binning can be set to 1, 2, 3 or 4 in rows and columns. Note that the readout time given in this manual is for 1 x 1 binning.
Filter: There is room for 10 different filters in the filter wheel. Clicking on the button will present you with the available filters. A ‘combo’ option is also available to allow combination of two filters.
One or more Quadrants can be selected to be read instead of the whole detector (note that this will not save time because each quadrant is read independently). The selection is enabled by clicking the Q checkboxes
Object: Enter here the title you want for the image.
File: File number will be automatically incremented for every new exposure.
Execute: This command is used to start a macro. The macro file name must be specified on the next window to the right. This option is useful when shutter time and/or linearity tests are performed. More details here:http://instrumentation.obs.carnegiescience.edu/Software/Swope/swopegui.html
Speed: only the Turbo readout speed is available at the present time.
Shutter: This is a flag that indicates whether the shutter is open or closed.
Snap will make a 4×4 binned image of the current field without incrementing the file number. The exposure time is as selected in ExpTime.
Subraster Allows to select subrasters on the chip. The regions can be defined giving its central coordinates followed by the width and height of the subraster (XYWH) or by its corners (XXYY). Savemode minimal will save only the selected region while savemode full will keep the original dimension of the quadrant filling with zero the region outside the selected.
Pointing and focus
To point the telescope enter the following command on the TCS computer:
RA hh mm ss.s
DEC dd mm ss.s
<Esc> Immediately abort any dome or telescope move
<F1> Display help screen
A full description of the telescope control system is at this address: https://www.lco.cl/?post_type=epkb_post_type_1&p=4203
To check pointing, move the telescope to a bright star close to Zenith.
There is a list available on puma and mula computers (object lists -→ cset.objects). Make sure that the equinox is right on TCS (MP 2000). Take a short exposure (1-2 s) of the field and compute the required offsets to place the bright star at the center of the image (scale 0.435 “/pixel). The telescope can be offseted from the Offsets section of the Telescope GUI. Take a new exposure and repeat procedure until pointing is right. Then type CSET on the TCS window and write down the ROFF and DOFF values, which will have to be entered manually if the TCS programm needs to be restarted for some reason. Next click on Centerfield on the guider window and check that the bright star ends near the center of the guider display. If it doesn’t, move the guider to place it near the center and then click on SetCenter on the guider window. Do not forget to click ‘Park’ on the guider window after this, to take the guider probe away from the Centerfield.
Focus sequences are allowed by setting Focus as ExpType on the CCD command window. This will allow 7 position sequences (Loops =7). This default can be changed to other number if desired. We recommend taking 10s exposures changing focus by 0.050 units in between. The secondary mirror is moved from the Focus section at the bottom of the telescope GUI (Figure 6). The focus needs to be determined for each filter to be used; a focus value of 23.125 was found for V filter after November 2023 engineering (for that setting, the guider focus was 3700). Focus offsets for the different filters are displayed in the board (a value -0.450 relative to V is good for all the Sloan filters). Once the focus sequence is over the corresponding file can be displayed and examined in the IRAF window. The spacing between focus exposures will be double between the first and second steps to allow identification of the sequence order. Once the approximate focus value is known, it is possible to run new focus sequences using smaller focus steps (such as 0.025 or 0.020). Focus may change along the night depending on temperature and telescope position. Sometimes a new focus sequence will be needed.
If you are using several filters, and already know the focus offsets between them, you may edit the Filter Hardhat (available under the Camera menu) to set the corresponding offsets so the guider will focus automatically each time you switch filters. The filter Hardhat also provides a ‘Combo’ option which allows superposition of two different filters (one from each filter wheel).
Added on January 11, 2019, a new command is available to reset the focus controller without restarting the Swope GUI. If the focus becomes unresponsive, follow the instructions in the picture below:
The main components of the guiding interface are the Skymap, Guider1 and Guider2 windows.
Skymap displays a star catalog and and overlay of the science camera field of view (red box) the patrol area of the guiders (blue boxes) and the area where the guiders vignette the science array (dashed rectangle). By selecting a star the catalog entry will be displayed in the text box in the lower left of the window. The selection will also update the probe relative position on the Guider window. The probe will be moved to that position by pressing the Goto button. The guider probe can be also moved by selecting an offset or by using the keypad (after selecting Enabled in the box next to it). The last section of the Guider window allows to select imaging mode (i.e. the guiding mode) or Shack-Hartman (not yet implemented). The focus of the guiding camera can be changed using the text box in the last row or by moving the slider.
The star catalog in use by Skymap is indicated in the top left box; which can be clicked to see the available options and eventually switch catalogs.
Please note that the Skymap display will only be updated to the current telescope position by taking an image (which can be a snap) or clicking the ‘Get’ button in the Telescope GUI.
Once the probe is at the desired position it should be possible the see the guiding star to appear on one of the guider displays (see fig. 8).
The guider focus can be adjusted by clicking and moving the slide bar button on the guider GUI or just writing the desired focus value next to it. Each time the telescope focus is modified (e.g. to apply focus offsets between filters) the guider foucs has to be modified by the same amount.
To interact with the guiding software the corresponding screen has to be selected on the Belkin KVM which is mounted on the rack next to the observer workstation
At the beginning of the night a software reset of the camera is recommended by typing DSPI. It also recommended to check that the PA and PX parameters are set according the values in Table 4. The cooling system is initiated by entering TEC 1.5. To adjust the range of intensities between black and white displayed the command SPAN is used (e.g. SPAN 1000). In order to guide, the guiding box has to be moved on the star image using the cursors. To change cursor steps use the keys INSERT and DELETE.
Guiding is started with <F3> and it is stopped with <F1>. Usual guider settings are ‘sn’ = 0.5, ‘bx’ between 19 and 23, ‘tf’ = 2, ‘tg’ = 0.60, ‘avf’ = 0, ‘avg’ = 1 or 2. Span around 1000 will work for a 10th mag. guide star; it depends on seeing.
A full detailed description of the guider software (GCAM) can be found at this address: https://www.lco.cl/wp-content/uploads/telescopes/magellan/gcam-usermanual.pdf
Beginning of the night:
- Turn on telescope power (rotate key).
- Check UT on TCS.
- Go upstairs and remove telescope cover.
- Lower wind screen.
- Open dome shutter.
- Turn on the fans in adjacent room.
- Make sure that dome lights are off.
- Turn on tracking (ASCENSION RECTA).
- Turn on guider cooling (TEC 1.5).
- Set the dome to AUTO.
End of night:
- Push ASCENCION RECTA to stop tracking.
- On TCS type DOME PARK and then DOME IDLE, to park the dome to the South.
- Type COVER on TCS
- From the LPLC panel close the dome, rise the wind screen and turn the lights on.
- Go upstairs, raise the platform and replace the telescope cover. Lower the platform all the way again.
- On the LPLC push GO LOCAL and turn off the dome lights.
- Turn the fans off in adjacent room.
- On TCS type ZENITH to park the telescope.
- Set the guider at the PARK position.
- On guider console type SPAN 99999 (or another big number) and TEC 0.0 to stop cooling.
- Turn off instrument power and console (rotate key).
- Activate the screen saver in the LPLC panel.
- Fill out the C40 daily report at HERE (VPN required).
Macros can be used by placing a text file in the DATA directory of the observer’s account on puma.
The file could be something like this:
To run the macro, the file name has to be specified on the window (usually empty) next to Execute on the CCD GUI, for example: /Users/obs1/DATA/macro_test Then the macro is started by clicking on the Execute button.
|Readout Noise (sigma)
|Field of view
|29.7 X 29.8 arcminutes
POWER FAILURE AND OTHER ISSUES
If for some reason the console is turned off, wait at least 15 s before turning it on again.
In case of a power failure the system will be recovered by pressing the RECONNECT yellow/orange button on the lower right of the telescope console.
If the dome becomes fully non- responsive (which happens very seldom), it may need a reset from the dome control box located in the equipment room: