Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 1 SPIRE Consortium Meeting La Palma, Oct. 1 – PV Phase and Calibration Plans Sarah Leeks RAL

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 2 When is PV Phase PV= Performance Verification. PV Phase comes after Commissioning. i.e. starts at Launch months Duration 2.5 months Followed by Science Demonstration Phase then Routine Phase

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 3 PV Phase Objectives verification of basic instrument performance population, with initial values, of all calibration files which require in-flight data verification of instrument operating modes validation and optimisation of AOTs generation of data sets required to update instrument sensitivity

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 4 Operations side - 1 The generation of the observations is much like it is for astronomer observations Most CUS scripts have been written to do each type of observation that we what to perform in PV (and commissioning) Expert HSpot provides a simple interface to the CUS scripts to allow observation requests to be produced The Observations are submitted to our SPIRE database They are then released so that they can be scheduled with the mission planning software

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 5 Operations side - 2 Each PV Phase operational day is scheduled with the mission planning software The ODs (and all the files to generate them) are delivered to the HSC for input into their operational system and for scheduling on the spacecraft.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 6 PV Test Flow - Photometer

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 7 PV Test Flow - Spectrometer

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 8 Turnaround of data During PV Phase, we will be usually operating SPIRE two days on, four days ‘off’. We will want to feedback the results from one set of observations into another set of observations. Once we have the data from an operational day, we have to reduce it (running as much as possible through the pipeline to level 0.5 or further) and analyse it. Then we have to update uplink calibration tables and/or CUS scripts and test the updates. These then go into our operational database, then we enter new/updates observations and update the observing day schedules. Then delivering this all to HSC, who in turn enter it into their system and deliver POS files to the MOC.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 9 How to optimise our PV Phase schedule We want to minimise these quick turnaround times to take some pressure off the team. We want to have two streams of observations that don’t depend on each other. A natural split is between the two sub-instruments. Each stream would be done on every other set of SPIRE days, giving us about 8 days turnaround.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 10 PV Test Flow Timeline - Photometer

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 11 SOVT-2 SOVT-1 was an end to end simulation of routine phase The delivery processes of PV Phase observations and schedules have already been verified during tests in May and in July. The first end to end simulation of PV phase on spacecraft is in SOVT-2, this will simulate feeding back data from one OD into another OD which will also be performed on the spacecraft. There will also PV Simulations were a significant fraction of PV days are tested.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 12 Calibration Data Calibration team members are writing their procedures for deriving calibration data. These are to be reviewed along with the data. Calibration data deliveries will need to refer to the procedure and be accompanied by a note saying what data were used to produce this version of the data. The procedure for delivering updated calibration files has been tested with several deliveries from the NHSC, and updated as a result. A meeting was held to access the status of the calibration files and to see what is needed to do to get them to pre-launch status. The actions are being followed up. By the middle of October codefreeze all calibration products (files) will be available for use in the pipeline, some will be at pre-flight status others will contain dummy data. Information on each calibration product is available from m

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 13 Calibration Sources Modelling experts have been working together to refine their models and to determine the best targets for the 3 instruments. We are making sure that we have some common targets between the 3 instruments and will be using the same models provided via a database. We prefer to observe few sources observed regularly. Prime calibrator for the photometer will be Neptune and for the spectrometer will be Uranus To cover the flux scale asteroids and a few stars will also be observed Bright point sources are the only requirement for many observations so a distributed list will be setup ahead of launch Line sources are also required for the spectrometer and suitable sources are under investigation. Also a dark patch of sky is needed, preferably in the continuous viewing zone.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 14 Calibration Observations We will perform observations as much as possible with the AOTs Observations will be multi-purpose as much as possible We will validate all of our AOTs and observing modes in PV Phase Most of PV will be done with the lid open but we will do some tests before it comes of, such as noise checks We want to be the operational instrument as the lid comes off and to perform FTS scans at regular intervals (few days) as the telescope cools down Focal plane geometry and detector angular offsets will of course be done with the lid off but it is formally under commissioning phase time (and the plan is detailed in the Herschel Pointing Calibration plan). A group is being setup to determine how to characterise straylight.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 15 Calibration Observations Some tests like detector noise and responsivity, and determination of the best SCAL settings will be initially be done with the lid on, but will be repeated again, especially once the telescope has reached its stable temperature. Once we have verified the basic instrument performance and populated, with initial values, of all calibration files which require in-flight data from PV, we will verify the operating modes and AOTs determining the best parameters for example scan speed, jiggle offset etc.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 16 PV Phase Plan The plan was updated for the Science Ground Segment Readiness Review. It is being updated further and will be used to generate a model PV phase with the observations entered in Expert HSpot for a delivery to ESA later in the year (the PV simulations and SOVT-2 will also be run from it). We also want to run some PV Phase days on the Flight Spare, to validate the scripts, run the tests in order and get people to analyse the data for feedback into the next days. The updated version will include a list of all the observations needed, the durations of these individual observations (calculated by HSpot) and total duration of ODs needed for SPIRE during PV. The plan will then be iterated on and also be reviewed by the SPIRE team.

Consortium Meeting La Palma October PV-Phase & Calibration Plans Sarah Leeks 17 Routine Calibration Observations Do as much as possible with the AOTs. Regular observations of a few sources. The routine phase calibration plan is in a very draft state at the moment. Final pre-flight plan to be delivered one month before launch