Changes
SPUPNIC
,/* Change Log */
= SpUpNIC User Manual =
<!--<span style="color:red">'''NOTE: ''' There is a memory leak in the Quick-Look software, which causes the software's memory consumption to grow larger each time a new spectrum is loaded. We are working to fix this. In the meantime, the work-around is to restart the Quick-Look GUI at least daily, or more often if required. See instructions below for how to do this.</span>-->*'' If you have found find this webpage already loaded in the browser, please refresh the page to ensure that it is current!'' == SpUpNIC Pointing Restrictions == Please note that SpUpNIC extends far enough from the bottom of the telescope that the instrument could potentially collide with the north pier when pointing east between declinations of -60 and -80. The situation is aggravated by the fact that the telescope can only be used on the east side of the pier. The result is quite severe pointing restrictions in the east, unfortunately for a declination range that includes the Magellanic Clouds! One is able to auto-slew into that dec range up to an hour angle of -2, and extremely careful manual pointing done from the console on the telescope floor can gain an additional half an hour. The absolute pointing limits are thus -2.5 hours for declinations between -65 and -75. '''When pointing automatically from the control room, please take note of where the cyan star appears on the TCS crash-limits plot when you start the slew. If the telescope would need to move through that problem region, abort the auto-slew and rather point manually, using the console on the dome floor.''' [[File:pointing_limits.jpg|thumbnail]] == SpUpNIC Call list == [[File:SpUpNIC.jpg|thumbnail]] '''SpUpNIC Instrument software:''' Carel van Gend - 076 818 1312 '''Rear-slit-viewer camera & images:''' Steve Potter - 072 246 7368 '''Commissioning/general issues:''' Lisa Crause - 082 498 4780 '''Telescope software issues:''' standby **113 (021 201 5178) or 9118 '''Electronics Issues:''' standby **103 (021 201 5179 ) or 9117 '''Mechanical Issues:''' standby **104 (021 201 5180 )
== Introduction ==
This is the current user manual for SpUpNIC (Spectrograph Upgrade - Newly Improved Cassegrain), the newly recently upgraded spectrograph at the Cassegrain focus of the 1.9 metre -m telescope's Cassegrain focus. Most of See the mechanical components have been rebuilt, [https://topswiki.saao.ac.za/images_topswiki.saao.ac.za/3/3e/SpUpNIC_2016.pdf '''SpUpNIC paper'''] presented at the optics have been significantly improved, 2016 SPIE Astronomical Telescopes and Instrumentation conference in Edinburgh for more information about the instrument has a new detector, and please cite the [https://topswiki.saao.ac.za/index.php/File:SpUpNIC_JATIS.pdf '''SpUpNIC refereed science paper'''] published in the SPIE Journal of Astronomical Telescopes, Instruments and Systems. [[File:annotated. We hope you enjoy using it!jpg|thumbnail]]
The spectrograph's collimator and camera optics have been replaced, the instrument has two subsystemsa new detector, all of the mechanisms are now under PLC subsystem (controlling the things that move) control and the detector subsystem software (controlling the both for instrument control + quick-look data acquisitionreduction)has been completely re-written. There is also a rear-of-slit camera that makes it easier to acquire targets and focus the telescope properly.
The instrument software has been built using two sub-systems, the new SAAO software frameworkPLC sub-system (controlling everything that moves) and the detector sub-system (controlling the data acquisition process). The drivers for the detector and PLC subsystems now these sub-systems run as stand-alone processes, and the user interface runs as a separate process on top of these. Typically, users will connect to the graphical user interface (GUI), although certain diagnostic functions may be accessed using the command line interfaces.
== Change Log Recent Updates ==*'''October 2023:''' The new autoguider that forms part of the instrument selector to accommodate both SpUpNIC and SHOC has been commissioned. There are slight changes to the operation of the autoguider, and <span style="color:red">observers now needs to connect to a new TCS PC (tcs74v4.suth) to use the telescope with SpUpNIC.</span>
== Quick Start ==
This is an a basic overview of taking data; if you're unsure about anything, the Advanced User Guide has much section contains more information.
* Log into the SpUpNIC PC. If observing remotely, connect to spupnic.suth.saao.ac.za by VNC. Username & password available from support staff.* If the main user interface instrument Control and quickQuick-look Look interfaces are not running, they may be started from the panel on the left edge of the left screen. The main user interface SpUpNIC Control GUI is started with the icon of an absorption spectrumicon [[File:control_GUI.jpg|20px]], and the quickQuick-look interface Look GUI from the icon of an emission spectrumicon [[File:quicklook_GUI.jpg|20px]].* Fill in target information Ensure that the grating you require has been installed by a technician - '''observers must not handle the gratings''' (optionalsee the grating change instructions in the Start of Run Section), and then set the grating to the required angle.* Set Check that the focus required filter is in the beam (or use the left open if required). * Run a Hartmann routine; (see the Advanced User Guide)to establish the best focus for the spectrograph.* The required spectrograph camera focus should be set automatically after a Hartmann run - check that this is the case.
* Set the slit width.
* If appropriate, set the exposure time and number of exposures.
* Load your target catalogue file.* Select a target from the target catalogue file so that the object name and coordinates will go into the fits header, and can be read by the TCS.* If taking a science image, acquire the target, and ensure that it is visible through the slitand in focus.* If taking an arc, ensure that the arc mirror is in-beam, and the chosen required arc lamp is on (remember to .* Select the SCIENCE exposure type after taking an arc, this will turn off the arc lamp and move remove the arc mirror out of beam when done).* Start the exposure with the ''Expose '' button.
* The countdown timer will show the time remaining, and the progress bar will first show the exposure completion state, and then the readout state.
* The software remembers settings used previously for given exposure types (e.g. 3 x 600 sec for a SCIENCE observation, or 25 x 30 sec for FLAT) so keep an eye out for this before you hit ''Expose'' for a new setup.
== PLC Subsystem SpUpNIC User Interfaces==
SpUpNIC's displays are labelled "Monitor 1" and "Monitor 2", and are located to the right of the TCS monitor in the warm room. To launch the SpUpNIC Control GUI, click on the absorption spectrum icon in the menu bar on the left-hand-side of Monitor 1. All of the spectrograph sub-systems (e.g. grating angle, slit width, arcs, exposures, guide mirror) are controlled from this GUI. There's an accompanying SpUpNIC Quick-Look GUI https://topswiki.saao.ac.za/index.php/Quick_Look_Tool , which displays each spectrum after readout and allows basic extraction and wavelength calibration. To launch the SpUpNIC Quick-Look, click on the emission line icon below the absorption spectrum icon on the left-hand edge of Monitor 1. == Detector Subsystem The Instrument Schematic== Normal operations are performed in the ''Main View'' tab of the SpUpNIC Control interface. [[File:Control_Arc.png|thumbnail]] [[File:Control_Science.png|thumbnail]] On the right-hand-side is a graphical representation of the instrument, which shows the light path through the various components controlled by the GUI. You can click on the guide mirror, arc mirror, rear-of-slit mirror and Hartmann shutters to move them in and out of the beam, and on the arc lamps and slit illumination to switch them on and off. A blue border surrounding the graphic indicates that the spectrograph is configured for acquisition or calibration, i.e. some component is in the beam that would obstruct its path to the science detector. If the system is correctly set up for a science exposure, there will be no coloured frame and the red light-path will reach the detector. == Advanced Detailed Users Guide ==
* The SpUpNIC Control interface has a number of tabs:
** The ''Main View '' tab, in which you'll spend most of your time.** The ''RoScam'' tab, which will later include the rear-of-slit GUI.** The ''Advanced '' tab, used at the start of the run, and which may be used if things go wrong(e.g. to reset or initialise mechanisms).** The ''Engineering View '' tab, which displays various diagnostic settingsand allows one to check the CCD and cold finger temperatures.** The ''Config '' tab, which you should not need for the most part, although this is where the temporary software lock for the grating is now.
* The panel on the right is an interactive schematic representation of the instrument. Components with in/out or on/off states can be toggled by clicking on the relevant part of the image. The light path is shown in red so that one can easily verify the instrument configuration.
==SpUpNIC User Interfaces=Start Of Run===
* At the start of your run, click Click on the "Advanced" tab. In the "Observer Info" boxfollowing links for '''Arc Maps''' for '''[[G4]]''', enter your name '''[[G5]]''', '''[[G6]]''' and run number'''[[G7]]'''. You can determine your run number from the triplicate "CCD and Unit Spectrograph" log bookOtherwise, stored in the "Log Books" section here are additional sets of the bookcase, on top of the chest of drawers beside the door to the observing floor maps for [[CuNe]] (behind you, if you're sitting at the SpUpNIC interfacefor G5). Your run number will be one greater than and [[CuAr]] (for all the previous observer's run number, listed in the log bookother gratings) with many more lines identified.
{| class="wikitable" border="1"
|-
! Grating
! OrderLines/mm
! Blaze (A)
! Res 2-Pix (A)
! Range (A)
! Star Filter
! Arc Lamp
! Arc Filter
! ~ Angle
! Arc Map
|-
| 4
| 11200| 46005100| 1.3| 8001250
| None
| CuAr
| None
| 3
| [[File:G4wc.jpg|thumbnail]]
|-
| 5
| 11200| 68006200| 1.1| 8001130
| GG495
| CuNe
| GG495
|-4| 5| 2| 3400| 0[[File:G5wc.5| 350| BG39| CuArjpg| BG39thumbnail]]
|-
| 6
| 1600| 46005100| 2.7| 16002780
| None
| CuAr
| Nonefor angle=13, but BG38 for angle<12 (wavelength range beyond ~6800A)| 13| [[File:G6wc.jpg|thumbnail]]
|-
| 7
| 1300| 46005000| 5.4| 42005550
| None
| CuAr
| BG38
| 16
| [[File:G7wc.jpg|thumbnail]]
|-
| 8
| 1400| 78008500| 4.4| 23004130
| GG495
| CuAr
| GG495
|-12| 8| 2| 3900| 2| 1150| BG39| CuAr[[File:G8wc.jpg| BG39thumbnail]]
|-
| 9
| 1830
| 7800
| 1.57| 9601750
| GG495
| CuAr
| GG495
|-0| 9| 2| 3900| 0[[File:G9wc.7| 480| BG39| CuArjpg| BG39thumbnail]]
|-
| 10
| 11200
| 10000
| 10.95| 800960
| GG495
| CuAr
| GG495
| -9
| [[File:G10wc.jpg|thumbnail]]
|-
| 11
| 1600
| 10000
| 2.5| 16002600
| GG495
| CuAr
| GG495
| 7
| [[File:G11wc.jpg|thumbnail]]
|-
| 12
| 1300
| 10000
| 5.5| 32005630
| GG495
| CuAr
| GG495
| 14
| [[File:G12wc.jpg|thumbnail]]
|-
| 13
| 2160
| 5000
| 0.54
| 580
| None
| CuAr
| None
| -8
| [[File:G13wc.jpg|thumbnail]]
|}
* If a grating is mounted in the spectrograph, it will be indicated toward at the bottom of the "''Instrument Setup" section'' pane, e.g. "''gr8" '' in the ''Grating '' field indicates shows that grating Grating 8 is mountedinstalled. Below this Above that is the grating ''Grating angle '' field. * '''If you need to mount a different grating, rotate you must ask the standby technician to change it for you.''' <!-- GRATING CHANGE INSTRUCTIONS: - follow the steps below - being EXTREMELY careful not to touch, or even breathe on, the optical surface! - set the grating angle to 0 degrees by entering 0 deg in the "SpUpNIC control GUI - set the telescope vertical - position the ladder on the north side (so that you ascend from the south) - undo the two quarter-turn fasteners on the grating hatch - hold the grating handle at all times while undoing the 3 orange knobs that secure the grating - the bolts are captive so they will unscrew and slide back, but not fall out - carefully retract the grating, keeping it level as you do so (you may need to wriggle it slightly if it seems tight) - take the grating that was in the instrument to the grating room on the NW side of the dome and replace it in its box - select the desired grating from its box and take it out to the telescope - at the telescope, ensure the grating's orientated correctly (2 bolts on 1 side, 1 on the other) before trying to insert it - keep the grating level to insert it, applying firm upward pressure until it's flush with the edges of the grating holder frame - keep hold of the handle and apply gentle upward pressure while you tighten the bolts - if any of the bolts feel stiff or awkward during tightening, gently wiggle the grating a bit (the bolts should turn easily) - continue tightening until all 3 bolts are fully secure (and can turn no further) - with all 3 bolts screwed in fully, close the hatch and lock the quarter-turn fasteners - remove the ladder - go to the ''Advanced'' tab on the control GUI and click the ''grating angle initialise'' button (in the bank of buttons on the left) --> * Once you have the correct grating in the spectrograph, enter an approximate starting angle (see the grating table above) in the ''Grating angle" '' box and pressing "click ''Go"''. You can also move * Take an arc and check the grating wavelength range on the Quick-Look extraction that will appear shortly after the image is read out. Note that it is advisable to double check the arc by entering displaying the number spectrum in e.g. pyRAF, as the Quick-Look plot doesn't always display the arc lines at the end of the wavelength range. * If the spectrum is too blue (red), decrease (increase) the grating angle and repeat the arc to check the new wavelength range - iterate until happy with the range. * Note that angle changes <0.05 degrees you wish are too small, so make a larger change and then go back the other way to move it achieve very small shifts (the software takes care of backlash in the system by ensuring that the desired value is always approached from the appropriate direction). * The software knows which order-blocking filters should be used with each grating, but it is still a good idea to check that the correct filter is selected (refer to the table above). If necessary, select the required filter from the drop-down menu at the bottom of the ''Instrument Setup'' pane and click ''Go''. * Please note that '''grating 13''' was a late addition and '''has not yet been incorporated into the software'''. This means that the SpUpNIC control software will not report that grating 13 is mounted, and will not know which science filter or arc lamp should be used - users will have to select these themselves based on the table above. The Quicklook software will not be able to identify the arc lines, nor necessarily plot them on a sensible scale - it may be necessary to zoom in on the "Grating spectrum in the Quicklook software to see the lines. * Note that '''grating 6''' does not require an arc filter when centred on 5100A (grating angle increment" box of 13), which extends to ~6500A. If you need to include redder wavelengths than this (angles ~12 and below), you will encounter very bright arc lines from ~6800A and will need a '''BG38 filter''' in the arc beam to avoid saturation. ====Arc lamp and filter selection==== * Two arc lamps are permanently mounted in the spectrograph - you no longer need to swap out a lamp - but the arc lamp filters are still changed manually. These will be changed for you by the duty technician when you submit your google form requesting your grating/arc lamp/filter setup. Filter requirements are listed in the table above.<!-- On the spectrograph, the CuNe lamp (Lamp 1) is in the horizontal housing, with two slots for filters in the light path. The vertically housed CuAr lamp (Lamp 2) is above it, similarly with slots for two filters at the bottom. Filter requirements are listed in the table above and the filters are stored in a small, labelled wooden box on the bench in the grating room (on the NW side of the dome). --> * The software now decides, based on which grating is in use, which lamp to switch on once ARC is selected from the ''Exposure type'' drop-down list on the ''Exposure/CCD info'' pane. * Alternatively, click on the appropriate lamp icon in the instrument schematic, where 1=CuNe and 2=CuAr. This will switch on the lamp and insert the arc mirror into the beam. Having taken the arc, simply click on the arc mirror icon in the schematic to remove the arc mirror and switch the lamp off. One can also control the lamps using the ''Lamp/Mirror Settings'' pane of the SpUpNIC Control GUI. Click the appropriate ''Change'' state button to switch the desired lamp on/off, and to move the arc mirror into the beam to take an arc exposure. ===Daily Daytime Tasks===
===Arc lamp and filter selection=Dome flat recipe====
====Focusing the spectrographThe Spectrograph - running a Hartmann sequence====
Before each night's observations, you should focus the spectrograph. This is done using a scripted Hartmann sequence, which run from the SpUpNIC Control GUI. The process moves a shutter halfway into the beam, takes an arc exposure; then blocks the other half of the beam and takes a second arc exposure. The arc lines are then cross-correlated to measure the shift between the two. The procedure is repeated at a range of camera focus positions until the line shifts are minimised, indicating best focus. This procedure can may be performed manually or , but it is typically run automatically. For an auto focus run, as follows:# Above Take an arc to check that the grating setupangle is appropriate for your desired wavelength range, select slit width 7: 1.05" (or smaller) from the dropdown meny and click "Go".# In to get an idea of the "Exposure/CCD info" "Advanced" subtab, select CCD modes "Faint" and "Slow" from required exposure time (aim for at least ~1000 counts in the dropdown menus, and CCD Binning "1x2".# In weaker lines): in the "''Exposure/CCD info" "'' pane on the ''Main" subtabView'' tab, select "Exposure type" = ARC from the dropdown drop-down menu, and enter e.g. 20 10 seconds in the "Exposure time" box.# Move If satisfied with the arc mirror into obtained, locate the beam and switch on ''Hartmann focus sequence'' panel in the appropriate arc lamp for your grating setup.# In the "''Instrument Setup" section '' pane on the ''Main View'' tab of the SpUpNIC Control GUI(if not, select adjust the "Auto" tabexposure time and grating angle as required before proceeding).# Enter an "Select the ''Auto'' tab and enter the parameters for the Hartmann sequence: 3.7 for the ''initial focus position" (e.g. 3.80)'', a "focus increment" (0.05 is recommended) for the ''focus increment'' and a 9 for the number of "''steps" '' - with the system still set up as it was for the test arc (try 7 iterationslamp on, arc mirror in beam) and . A bug in the software causes the Hartmann routine to fail if the camera focus isn't first set to the "initial focus pos", so enter 3.7 in the Camera focus "REQUESTED" box above, then click "RunGo". Once the focus has changed, click ''Run'' to start the Hartmann sequence. # The slit width will automatically be set to 1.05" and the exposure type will switch to HARTMANN, then the GUI will grey out and not be available during the Hartmann focus sequence, but (although you will see the current "''Current Camera focus" Focus'' field changing and the Hartmann shutters indicate "''Moving"''.# On completion, of the sequence: in the SpUpNIC Quick-Look GUI, in the log box to the left right of the spectrum display window, you will see a list of focus positions and their corresponding pixel shifts. Best focus corresponds to a shift of zero.# Enter The camera focus should automatically be set to the best focus value, but if it isn't, enter the best focus into the "requested''Requested" Camera focus Focus box on the SpUpNIC ControlGUI's "''Instrument Setup" window '' pane and click "''Go"''.# Switch off the arc lamp and move * The Hartmann sequence ends with the arc mirror shutter out of the beam by clicking , but be sure to select the desired slit width in the ''Instrument Setup'' pane and click ''Go''. Check that it goes to the required position, click ''Go'' again if it does not do it the first time.* Select "Exposure type" = ARC and take an arc to confirm that the focus looks good.* Click on the arc mirror in the schematic.# The Hartmann test ends with to switch off the shutter arc lamp and move the arc mirror out of the beam.
==Observing Setup==
* Do Open a terminal on the SpUpNIC PC and use your favourite text editor to produce a simple text file (e.g. Run007.txt) with the format shown below: Target_1_name HH:MM:SS -DD:MM:SS J2000 Target_2_name HH:MM:SS -DD:MM:SS J2000 Target_3_name HH:MM:SS -DD:MM:SS J2000(Note: do not include spaces in the target names.* Use and use single spaces between the object name, RA, Dec and Equinox.* Select the appropriate target name from the list that appears in the Target Info box after the catalogue file has been loaded.)
==Recipe for setting =Setting up the slit position on the TCS - using the SpUpNIC Control GUI===
The purpose of this step is to figure out where on the acquisition image you need to place your star, in order for it to land pretty close to the ideal spot on the slit. Very bright stars can be seen reflected on the slit jaws, and can be placed on the slit directly, but this is not the case for fainter stars, which need the superior reflectivity of the guide mirror in order to be seen on the acquisition camera. This position should be approximately stable throughout your run, but you can fine-tune the target location using the rear-of-slit camera.
# Move the guide mirror into the beam, either by setting the "''Acquisition" '' state in the "''Lamp/Mirror Settings" section '' pane of the SpUpNic SpUpNIC control GUI (if it says Guide Mirror "''Science"'', click "''Change"''), or by clicking on the guide mirror in the graphical viewinstrument schematic.# Acquire a bright star (e.g. ~4 4th mag from the Bright Stars chapter of the Sutherland Almanac, available in the warm room), roughly centre it on in the acquisition camera field and continue exposing.# Move the guide mirror out of the beam(i.e. centre the mirror so that light can go down the central hole).# Move the rear-of-slit mirror into the beam ("''Lamp/Mirror Settings" section'' pane, "RoS mirror" change from "''Out of beam" '' to "''In beam"'').# Turn on the slit illumination (in "the ''Instrument Setup" move the Slit illumination slider to .... and click "'' pane, ''Change" '' to turn on the lamp). Tune the exposure time/LUT sliders on the TCS until you can clearly see the slit running horizontally across the acquisition image, approximately halfway up.# Using the hand paddle, move the telescope to place the star on the slit, approximately one third quarter of the image width away from the right-hand edge.# Turn off slit illumination.# Open a terminal Click on Monitor 1, and run the following commands * ssh -Y tcs@tcstest * password ******* icon [[File:Potcamicon.jpg|40px]] for the rear of slit camera (you should have been supplied with on the passwordleft-hand side of Monitor 1) * sudo ./1X1_thread_forms * password *******# .....description of pottercam when functioning sensibly.......# An image window for the rear-of-slit camera will pop up. This looks up at the slit from behindbelow, to enable you to check that your star is centred on the slit. Move the telescope such that the star falls on the centre of the slit image in both x and y.[[File:slit_view.png|thumbnail]]# Move the rear -of -slit mirror out of the beam and take a test spectrum (e.g. 20 seconds) of the bright star (in "the ''Exposure/CCD info" '' pane, select "''Exposure type" "Science" '' = SCIENCE from the dropdown drop-down menu, enter "''20" '' in "''Exposure time" '' and click "''Expose"'').# The resulting image will be displayed on the Quick-Look GUI, on Monitor 2. You are aiming for the spectrum to fall on approximately the central row of pixelswithin the image area (note that this is a roughly central band that only covers about half the vertical extent of the CCD). If the spectrum is too highor low, move the telescope slightly ...east?west? ; if too lowin RA (the RA- button moves the spectrum downwards in the image), move iterate until the telescope slightly west/east....star is well positioned.? ?# When Once you are happy with the position of the spectrum on the image, on go back to the TCS, and add a red marker over the position of the star on the slit (TCS "''Pointer" '' pane: "''Markers"'', "''Add a red marker"'').
# Finally, move the guide mirror into the beam, and add a second red marker at the position of the star. This marker will be used to approximately position stars on the slit that are too faint to be seen reflected off the slit jaws.
* The red markers are lost if the TCS software gets restarted, so it is a good idea to note down their coordinates!
===Focusing the telescope===# * Acquire a ..... ~11th mag star (e.g. one of the spectrophotometric standards) with the guide mirror in the beam* Position the star on the appropriate red box on the acquisition image* On the instrument schematic, set the guide mirror to Science (so that light reaches the slit)* Also insert the rear-of-slit mirror into the beam to direct the light to the Lodestar (rear-of-slit) camera* View the stand-alone rear-of-slit software window * Click on the "continuous" button for an ongoing series of 2 second exposures* Open the slit wide, to about 4"* Adjust the slider bar to the right of the image to adjust the scaling, or hold down the mouse button while mousing over the image, as in ds9 * Using GUIDE speed, use the RA & Dec arrow buttons on the bottom-right of the TCS GUI (or the hand paddle if in the dome) to position the star near the centre of the slit (in both X and Y)* Adjust the telescope focus on the TCS (or the hand paddle if in the dome) in steps of 3-5 units and assess how the star image changes* The star will move around due to the translation of the secondary mirror, so adjust it back into view if necessary* Astigmatism in the system extends the star image diagonally and the orientation indicates whether the focus value is too high or too low: Star extended from upper-left to lower-right: focus value is too high Star extended from lower-left to upper-right: focus value is too low* Best focus is where the star is as round and sharp as possible* Optimum focus varies with temperature, typical summer values are ~2200 while cold winter nights may be closer to 2270 units
== User's Troubleshooting Guide =Focusing the acquisition camera===* Having focused the telescope as described above, one needs to focus the acquisition camera.* The star used to focus the telescope may be too bright, so aim for something fainter (e.g. a guide star that needs a ~1 sec exposure).* Adjust the acquisition camera focus with the up/down buttons in the lower right corner of the TCS GUI to get the stars as sharp as possible.* With the new autoguider (installed Oct 2023), a focus value of 5300 is a good starting point.
= Technician=User's Troubleshooting Guide ==