LYRA the LargeYield Radiometer onboard PROBA 2 Solar

LYRA the Large-Yield Radiometer onboard PROBA 2 Solar Irradiance Observations with LYRA on PROBA 2 I. E. Dammasch, M. Dominique, J. -F. Hochedez & the LYRA Team Xth Hvar Astrophysical Colloquium Hvar, Croatia, 6 -10 September 2010

LYRA highlights • 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), LPC 2 E (Orléans, F)…

LYRA highlights q 4 spectral channels covering a wide emission temperature range q Redundancy (3 units) gathering three types of detectors q q q Rad-hard, solar-blind diamond UV sensors (PIN and MSM) AXUV Si photodiodes Ly Hz Al Zr Unit 1 MSM PIN MSM Si Unit 2 MSM PIN MSM Unit 3 Si PIN Si Si 2 calibration LEDs per detector (λ = 465 nm and 390 nm) High cadence (up to 100 Hz) Quasi-continuous acquisition during mission lifetime

SWAP and LYRA spectral intervals for solar flares, space weather, and aeronomy LYRA channel 1: the H I 121. 6 nm Lyman-alpha line LYRA channel 2: the 200 -220 nm Herzberg continuum range LYRA channel 3: the 17 -80 nm Aluminium filter range including the He II 30. 4 nm line (+ X-ray) LYRA channel 4: the 6 -20 nm Zirconium filter range where solar variablility is highest (+ X-ray) SWAP: the range around 17. 4 nm including coronal lines like Fe IX and Fe X

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

LYRA data products and manuals… …available at the PROBA 2 Science Center: http: //proba 2. sidc. be/

Summary: FITS File Structure n n n n n lyra_20100609_000000_lev 1_***. fits where: *** = met, std, cal, rej, (bst, bca, bre) generally: header + binary extension table(s) extension = header + data (variable length) Lev 1 met = HK, STATUS, VFC Lev 1 std = uncalibr. irradiance (counts/ms) Lev 2 std = calibr. irradiance (W/m²) Lev 3 std = calibr. aver. irradiance (W/m²) per line: time, ch 1, ch 2, ch 3, ch 4, qual.

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

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

State of the data processing pipeline Telemetry packets LY-TMR: Current state In the future Not distributed Daily basis After each contact Raw data (in counts) LY-EDG fits Lv 1: Engineering data (in Hz) LY-BSDG fits Not available After each contact Lv 2: Calibrated data (in W/m²) Other tools Higher level data products Plots + flare list available irregular systematic

First results (even before opening covers)

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

First Light acquisition (06 Jan 2010)

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

Flares n LYRA observes flares n n down to B 1. 0 LYRA flare list agrees with GOES 14 Flares are visible in the two short-wavelength channels Exceptionally strong and impulsive flares are also visible in the Lyman- alpha channel (precursor) Example: C 4. 0 flare, 06 Feb 2010, 07: 04 UTC

M 2. 0 flare, 08 Feb 2010, 13: 47 UTC

Comparison with GOES flare Example: M 1. 8 flare, 20 Jan 2010, 10: 59 UTC

Comparison with GOES flare Example: C 5. 4 flare, 15 Aug 2010, 18: 30 UTC

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

And we have a fifth channel at 17. 4 nm. . . called SWAP!

SWAP and LYRA observing together 20100607_proba 2_movie. mp 4

Next steps n Cross-calibration (internal/external) n Produce calibrated data automatically n Publish first results n Advertise data products n Get extension from ESA

How to be involved? Scientists are welcome to n use PROBA 2 data n propose special observation campaigns Guest Investigator Program welcomes proposals for dedicated (joint) observations in the frame of a science project: n Funds available for a stay at PROBA 2 Science Center n Scientist can take part in the commanding of the instruments n Will gain expertise in the instrumental effects n Next announcement (for 2011 -12): May 2011 n Proposal deadline and selection: June 2011 n First visits: September 2011 onwards