1. Solar Irradiance Observations with LYRA on PROBA2 (An Introduction) I. E. Dammasch, M. Dominique & the LYRA Team Royal Observatory of Belgium LYRA the Large-Yield Radiometer onboard PROBA2

6. LYRA: the Large-Yield RAdiometer 3 instrument units (redundancy) 4 spectral channels per head 3 types of detectors, Silicon + 2 types of diamond detectors (MSM, PIN): - radiation resistant - insensitive to visible light compared to Si detectors High cadence up to 100 Hz

7. Royal Observatory of Belgium (Brussels, B) Principal Investigator, overall design, onboard software specification, science operations PMOD/WRC (Davos, CH) Lead Co-Investigator, overall design and manufacturing Centre Spatial de Liège (B) Lead institute, project management, filters IMOMEC (Hasselt, B) Diamond detectors Max-Planck-Institut für Sonnensystemforschung (Lindau, D) calibration science Co-Is: BISA (Brussels, B), LPC2E (Orléans, F)… LYRA highlights

8.  4 spectral channels covering a wide emission temperature range  Redundancy (3 units) gathering three types of detectors  Rad-hard, solar-blind diamond UV sensors (PIN and MSM)  AXUV Si photodiodes  2 calibration LEDs per detector (λ = 465 nm and 390 nm)  High cadence (up to 100Hz)  Quasi-continuous acquisition during mission lifetime LyHzAlZr Unit1MSMPINMSMSi Unit2MSMPINMSM Unit3SiPINSi

9. SWAP and LYRA spectral intervals for solar flares, space weather, and aeronomy LYRA channel 1: the H I 121.6 nm Lyman-alpha line (120-123 nm) LYRA channel 2: the 200-220 nm Herzberg continuum range (now 190-222 nm) LYRA channel 3: the 17-80 nm Aluminium filter range incl the He II 30.4 nm line (+ <5nm X-ray) LYRA channel 4: the 6-20 nm Zirconium filter range with highest solar variablility (+ <2nm X-ray) SWAP: the range around 17.4 nm including coronal lines like Fe IX and Fe X

10. LYRA pre-flight spectral responsivity (filter + detector, twelve combinations)

11. LYRA data products and manuals… …available at the PROBA2 Science Center: http://proba2.sidc.be/

14. Summary: FITS File Structure lyra_20100609_000000_lev1_***.fits where: *** = met, std, cal, rej, (bst, bca, bre) generally: header + binary extension table(s) extension = header + data (variable length) Lev1 met = HK, STATUS, VFC Lev1 std = uncalibr. irradiance (counts/ms) Lev2 std = calibr. irradiance (W/m²) Lev3 std = calibr. aver. irradiance (W/m²) per line: time, ch1, ch2, ch3, ch4, qual.

15. Product Definition Level 1 = full raw data (LY-EDG output) Level 2 = calibrated physical data (LY-BSDG output) Caution: preliminary status. Require versioning. Level 3 = processed products (e.g. averages) Level 4 = plots of products Level 5 = event lists (optionally with plots)

16. Further Data Products… …“Level 4”, “Level 5” (still preliminary):

20. LY-TMR: State of the data processing pipeline LY-EDG LY-BSDG Telemetry packets “Lev0”: Raw data (in counts) Lev1: Engineering data (in kHz) fits Lev2,Lev3: Calibrated data (in W/m²) Other tools Higher level data products Current stateIn the future Not distributed After each contact After each contact Testing After each contact Plots + flare list available irregular systematic

21. First results (even before opening covers)

22. Aurora Oval  Perturbations appearing around 75° latitude  2-3 days after a CME, flare...  Associated to geomagnetic perturbations Spacecraft maneuvers SAA

23. First Light acquisition (06 Jan 2010)

24. Aeronomy  Occultations: Study atmospheric absorption; high temporal resolution needed  Input for atmospheric models: NRT and calibrated data needed

25. Flares LYRA observes flares down to B1.0 LYRA flare list agrees with GOES14 Flares are visible in the two short-wavelength channels Exceptionally strong and impulsive flares are also visible in the Lyman- alpha channel (precursor) Example: C4.0 flare, 06 Feb 2010, 07:04 UTC

26. M2.0 flare, 08 Feb 2010, 13:47 UTC

27. Comparison with GOES flare Example: M1.8 flare, 20 Jan 2010, 10:59 UTC

28. Comparison with GOES flare Example: C5.4 flare, 15 Aug 2010, 18:30 UTC

29. LYRA flare size LYRA background-subtracted flux in Zr (channel 2-4) LYRA observes all GOES flares in both Al and Zr channels Initially also Lyman-alpha contribution for impulsive flares Different onset and peak times in different pass bands Good correlation to GOES, better temporal resolution

30. Sun-Moon eclipse …demonstrating the inhomogeneous distribution of EUV radiation across the solar surface

31. Eclipses as seen with SWAP swap_eclipse_15Jan2010.mp4 swap_eclipse_11Jul2010.mp4

32. And we have a fifth channel at 17.4nm...... called SWAP (using “SWAVINT”)

33. Jan - Sep 2010 SWAVINT and LYRA look quite similar LYRA shows flares in addition to EUV

34. SWAP and LYRA observing together 20100607_proba2_movie.mp4

35. Next steps Cross-calibration (internal/external) Produce calibrated data automatically Publish first results Advertise data products Get extension from ESA (2012: OK)

36. How to be involved? Scientists are welcome to use PROBA2 data propose special observation campaigns Guest Investigator Program welcomes proposals for dedicated (joint) observations in the frame of a science project: Funds available for a stay at PROBA2 Science Center Scientist can take part in the commanding of the instruments Will gain expertise in the instrumental effects Next announcement (for 2011-12): May 2011 Proposal deadline and selection: June 2011 First visits: September 2011 onwards

37. Calibration 2010 according to TIMED/SEE

38. Calibration – Problem: 2010 according to LYRA

39. Solution – Start with “First Light”

40. … fit the degradation …

41. … and add it Plausibility: Artifacts in channels 1 and 2 Non-degenerated SXR in channels 3 and 4

42. To be continued