'''Data Pipeline:''' Marco Lam (LJMU; C.Y.Lam@ljmu.ac.uk)
'''Project Scientist for LT:''' Robert Smith '''Local Co-PIs:''' Amanda Sickafoose Nicolas Erasmus (amandanerasmus@saao.ac.za) & Hannah Worters (hannah@saao.ac.za)
'''Local Electronics Engineer:''' Hitesh Gajjar (hitesh@saao.ac.za)
'''Local Mechanical EngineesrEngineers:'''James O'Connor (joc@saao.ac.za) and , Egan Loubser (egan@saao.ac.za), and Kathryn Rosie (krosie@saao.ac.za)
'''Local Software Engineer:''' Carel van Gend (carel@saao.ac.za)
== Documentation ==
* The link to the 2017 October 27 Skype kick-off presentation: https://www.dropbox.com/s/lcr54nkvtusdh69/SAAO-SPRAT-KICKOFF.pptx?dl=0 (includes references to the SPIE paper and Zej's thesis)
== Points to consider (based on 27 Oct. Skype) ==
*(1) Hannah to send Iain telescope optical prescription (done).
*(2) Consideration of mounting, in terms of peripherals and control equipment — basically starting to think about packaging and how much needs to be mounted on the port vs. off to the sides, note that control of moving parts will be pneumatic (James/Egan).
*(3) Question of which coating to buy for the Andor iDus camera -- new option has higher QE over wider range, but higher dark current (Amanda & Hannah)
*(4) Question of whether we want two optimized wavelength settings, like SPRAT, or only one — the former aren’t being well used on SPRAT and the latter saves a moving part. although they say that they have plans to ensure that part is more reliable than the current version (Amanda & Hannah)
*(5) Think about optimal slit size — 1.5” min, could be up to 2”, could also consider stepped slit — these are laser cut, and we could request more than one (Amanda & Hannah)
*(6) Thinking about .fits header information for compatibility with data reduction pipeline, and how to integrate TCS with instrument to allow automated acquisition (Carel)
== Notes from meeting on 1st Feb 2019 ==* [[Media:Mookodi_System_Description_0.4.pdf|Mookodi System Description v0.4]] -- This document is to provide a system description of Mookodi, its sub-assemblies, locations of adjustments and the reasons behind some of the decisions. It does not cover control software, nor procedures for setting up or testing the instrument.
Combined Sprat/SHOC is way <!-- *[[Media:Mookodi_Filter_Change_Instruct_0.2|Mookodi Filter Change Instructions v0.2]] -- This document describes the procedure to gofit/replace filters in the filter assembly.-->
Working out == Notes from Nasmyth:meetings ==* "Inside" Nasymyth is autoguider. This can patrol half of the field of view, and will hopefully have a focus mechanism.* Nasmyth mounting: ** James to provide details of this mounting as used on Wide Field Camera on opposite port.** 1/4 of the field of view will be for a High Resolution Spectrograph (HRS) fibre feed** 1/4 of the field of view with be for SPRAT/SHOC** A cable wrap (copy of that on opposite port) will be provided. James to provide details.** There is possibility of pneumatic supply* Deployable calibration mirror (to feed flat/arc)* Deployable slit* Field Lens* Collimator Lens* FILTER SLIDES (3). Hopefully <50mm thickness. To house maybe 5 filters each. Note one filter will need to be order blocker (4000-8000 Angstroms) for SPRAT. James to design to fit to an interface in SPRAT.* Grism Assembly* Camera Lens and CCD[[ 18 Nov.2019]]
General Design Points* Filter slides need to be in collimated beam to avoid focus shifts* Try and minimise cables on/off mount. So mount control computer with instrument. Note SHOC software requires GPS feed (serial; currently using serial to USB, Amanda to check latest GPS hardware).* USB for camera rather than PCI Card* Use existing SHOC CCD readout (via andor SDK) * Use existing Apache Thrift infrastructure* LJMU responsible for all mechanism control, including filter slides* Use wiki to keep one version of documentation/files etc.[[ 01 Feb 2019]]
Actions:[[ 27 Oct. 2018]]
* IAS: Check/modify optical design to make space for filter slides[[ 24 Jan. 2019]]* James: Provide details of mounting plate/wider field camera (STEP File); provide information on cable wrap being used on other port* Carel: Provide details of SHOC software to Chris Mottram so he can try and built a local copy at LJMU[[ 31 Jan. 2019 Telecon with Iain, plus email communication]]* Amanda: Look at trade off between deep depletion [[ 12 Feb. 2020 Filter requirement meeting (higher red QENic, higher dark currentHannah, Retha, James, (Kathryn) and standard EMCCD)]] [[6 Mar. 2020]] [[20 Mar. 2020]] [[3 Apr 2020]] [[19 June 2020]] [[3 July 2020]] [[17 July 2020]] [[6 Nov 2020]]
== SHOC/SPRAT hybrid ==
== Spreadsheet of pros/cons for proposed mounting options ==
[[File:LesediSpec.Mounting1.jpg||1000 px|center]]
== Project Schedule ==
Proposed: start 01 Jan 2019, delivery 04 May 2020. See timeline in bid. Note that paperwork was not signed until 01 March 2019, so there is an anticipated delay.
[[File:Screen Shot 2019-11-18 at 11.48.27.jpg||500px|center]]
== Lens Coatings and Andor CCD ==
17 July 2020: [[:File:Mookodi_iKon_test.pdf|Mookodi Andor camera test datasheet]]
17 January 2020: Decision was made to go with Andor Ixon 888 UVB and -AB AR coating for lenses. Decision swayed by the off-the-shelf Nikon lens which will be the limiting element for obtaining spectra/photometry below 400nm. -A coating not good > 750nm where other elements still perform well.
[[File:Lens_coatings_update.png||500px|center]]
== Preliminary Exposure Time Calculator ==
[https://livtel.github.io/saao_sprat_etc/ Calculator]
== Imaging Photometry Filters ==
Link below to the SDSS filters for Mookodi's imager:
* [[ Filter Plots and Data]]
== Camera ==
Link below to the Andor CCD spec sheet and manufacturer's performance sheet:
* [[Media:Andor iKon-M 934 Specifications.pdf]]
* [[File:Mookodi iKon test.pdf]]
== Interfaces ==
27 January 2020: Diagram showing overview of system interfaces.
[[File:LJMU_interfaces.png||1250px|center]]
== Software ==
[https://docs.google.com/document/d/1Z9aPGZ-iYJSIZjTwoWAixtsYDBt-WyQUKkqTMmgFrSc/edit Use case 1 - Sidereal Spectroscopy]
The software runs on an instrument PC, which hosts the camera driver software and connects to an Arduino for the moving parts. Additionally a filter mechanism may be controlled from here.
We envisage providing Thrift interfaces to the camera driver, the Arduino driver and the filterwheel driver. These all run as standalone server processes, and are accessed by an instrument controller process, which has clients for each of the server processes. The instrument controller contains logic to coordinate the instrument operations, and also is able to send commands to and receive state from the telescope.
The following diagram illustrates the software layout:
[[File:SpratBlocks.svg|1250px]]
=== Software Interfaces ===
==== Detector ====
==== Moving parts ====
=== Data Files ===
The camera driver software retrieves the observation data from the camera, converted this to FITS format and saves this to disk.
The FITS files are named according to the SAAO file naming convention:
==== FITS header fields ====
The FITS headers include the keywords: