SMOS L1 Sun BT Valida0on against on-ground radio-telescope network
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1 SMOS L1 Sun BT Valida0on against on-ground radio-telescope network Daniele Casella 1, Raffaele Crapolicchio 1;2, Nicola Compare7 1, Christophe Marqué 3 1 Serco 2 ESA-ESRIN 3 Royal Observatory of Belgium
2 Content SMOS mission - How SMOS can sense the Sun Establish a Sun L-band reference measurements from on-ground radiotelescope SMOS Sun L-band observa0ons verifica0on (quite Sun). Case studies Long term SMOS Sun L-band observa0ons verifica0on (erup0ve / Sun microwave burst). Conclusion.
3 How SMOS can sense the Sun
4 How SMOS can sense the Sun The MIRAS instrument antenna array is formed by three arms 120 apart, with 23 equally spaced LICEF (Lightweight Cost-Effec0ve Front-end) receivers each. Due to antenna size (diameter equal to 16.5 cm) and frequency wavelength (21 cm at Lband) the instrument s field of view (FoV) is large and includes full Earth-disk and part of the surrounding Sky. The brightness temperature image is retrieved from the cross correla0ons measured by pair of elements in the array (Fourier synthesis in case of ideal instrument).
5 How SMOS can sense the Sun DFT Basic Period Alias-free FOV Replicas Earth sky Horizon Direct Sun The Y-array configura0on leads to an hexagonal sampling of the spa0al frequency domain. Antenna spacing is wavelengths. Part of the FoV is affected by aliasing. Replicas The alias-free FoV can be suitably extended over regions where the Sky alias is present to obtain an extended alias-free FoV (EAF-FoV) Extended Alias-free FOV Replicas Direct Sun appears as a replica in the image extended FoV
6 How SMOS can sense the Sun X-pol Y-pol The Sun signal appears superimposed to earth scene, as a bright spots over the SMOS EAF-FoV image and it contaminates the radiometer measurement. It appears nearly 97% of images regardless if Sun posi0on is in front or in the back of the antenna plane. Sun s tails signal contaminate also the AF-FoV. The Sun signal is estmated and removed during the image reconstruc0on processing. The removed Sun brightness temperature (in X and Y polariza0on) is annotated in the SMOS L1b user product.
7 Establish a Sun L-band reference measurements from on-ground radiotelescope
8 Ground based radio telescopes available measurements Humain spectrometer ( MHz) RSTN 245, 410, 610, 1415, 2695 MHz 4.995, 8.800, 15.4 GHz Nobeyama Radio Polarimeter 1, 2, 3.75, 9.4, 17, 35, 80 GHz L-band L-band interpolated L-band proxy Penticton Observatory 2.8 GHz
9 Ground based radio telescopes available measurements n L-band daily Solar flux from Humain spectrometer (from July 2015 onwards) access to be agreed with Royal Observatory of Belgium n L-band daily Solar flux from RSTN radio-telescope 0ll beginning 2011 free access n L-band daily Solar flux can be retrieved from RSTN radio-telescope 1s dataset (from 2010, free access several months delay) RSTN is inaccurate, not always inter-calibrated, RFI Flare 1s Solar Flux RFI Solar Flux 1s [SFU]
10 Ground based radio telescopes reference measurements n Shimojo et al Recently described by Shimojo et al In this approach the monthly mean of the daily flux at different frequency has been fiied with an exponen0al func0on log10flux=a+b*ν Where ν is the frequency a, b linear fit coefficients a, b are not constant and are func0on of Solar minimum and Solar maximum periods
11 Ground based radio telescopes reference measurements n Casella et al. (2018, SMOS Sun BT verifica0on study TN IDEAS+-SER-EVO-REP-2978 ) 1s L-band Flux inter-calibrated Solar Flux 1s [SFU] Solar Flux 1s [SFU] Raw Data: RSTN 1s, NoRP 1s and daily flux Calibrated data Solar Flux 1s [SFU] Reference 1s solar flux
12 Ground based radio telescopes measurements comparison n RSTN 1s data (Casella) compared with Tanaka daily flux 2 days in July, 22 December Daily Flux Noon Time Daily Flux Mean 1s 22/12/ ±0.96 8/7/ ±1.64
13 SMOS SUN L-band observa0ons verifica0on (quite SUN case studies).
14 SMOS observa0on comparison: linear polariza0on (quite Sun) SMOS Sun BT (X+Y)/2 normalized with inter-calibrated radio-telescope 1s daily Solar Flux converted in BT (including Sun-Earth distance) Two days SMOS observa0ons (winter/summer) to cover different antenna paiern areas 8 Jul 2016 Flux= B λ Ω Sun = 2 K b BT/ λ 2 Ω Sun D=UA ( /2 cos( N day )) 22 Dec 2016 Scalefactor= SMOS Sun BT/ Radiotelescope Sun BT
15 SMOS observa0on comparison: linear polariza0on (quite Sun) Scale factor (SMOS Sun BT divided by the reference value) as func0on of the eleva0on angle for all data with Sun in the front of the antenna. Front v Dec 2016
16 SMOS observa0on comparison: linear polariza0on (quite Sun) scale factors V720/eleveTon (corrected by the Sun Earth distance) 08/07/ D 22/12/ A 8 Jul Dec 2016
17 SMOS SUN L-band observa0ons verifica0on (quite SUN Long term).
18 First aiempt for SMOS Sun Flux long term verifica0on v620 The full reprocessing of SMOS with new L1OP is imminent We started the development of an algorithm for the calibra0on and correc0on of SMOS Sun BT
19 Verifica0on with Pen0cion Monthly Flux Pen0cion: 2.8 GHz SMOS: 1.4 GHz
20 SMOS SUN L-band observa0ons verifica0on (erup0ve SUN).
21 SMOS observa0on comparison: linear polariza0on (erup0ve Sun) Solar flare (M-class) on May The Coronal Mass Ejec0ons (CME) occurred between utc. Expected Solar Microwave Burst peak Sun L-band brightness temperature SMOS V620 SMOS V720 Reference
22 SMOS observa0on comparison: linear polariza0on (erup0ve Sun) SMOS Sun BT (X+Y) v720 normalized by Sun eleva0on angle and correlated with 1s solar flux measurement from RSTN (inter-calibrated) and Humain radio telescopes Similar and very good correla0on performance between v620 and v720, very good correla0on also for Sun in antenna back plane. Date and Time of Event X-ray Solar Flare Class ground based* Front Back Corr 620 Corr 720 Corr /02/2011 ~01:45 X 2.2 RSTN /08/2011 ~08:05 X6.9 RSTN /09/2011 ~13:15 M7.1 RSTN /01/2012 ~04:00 M8.7 RSTN /05/2012 ~01:47 M5.1 RSTN /07/2012 ~16:50 X1.4 RSTN /09/2017 ~12:00 X9.3 Humain /09/2017 ~09:30 C2.3/M1.4 Humain /09/2017 ~14:30 X1.3 Humain /11/2015 ~14:00 M3.7 RSTN Sun in the Back plane SMOS v720/elev RSTN
23 SMOS observa0on comparison: circular polariza0on (erup0ve Sun) SMOS Sun BT 4 th Stokes divided by 2 and sign changed to make it comparable with Nobeyama let hand (LH) and right hand (RH) polariza0on observa0on 9 Aug 2011 X 6.9 flare event SMOS v720 Nobeyama 1GHz Nobeyama 2 GHz Front Change in 4 th Stokes sign well captured by SMOS Back
24 Conclusions.
25 Conclusions Radiotelescope mul0frequency 1s dataset has been intercalibrated to derive a reference Sun L- band brightness temperature. SMOS Sun L-band brightness temperature observa0on have been compared with that inter-calibrated radiotelescope measurements. Results show a very good correla0on in case of Sun microwave burst (for Sun posi0on in front and back of the sensor antenna plane). For quite Sun SMOS Sun L-band brightness temperature compare very well if a mul0plica0ve calibra0on factor is used. SMOS Sun L-band brightness temperature can be very useful for different users community: Earth Observa0on community for the retrieval of geophysical parameters at L-band (e.g. sea surface salinity): to correct for Sun effects at L-band (direct and glint); Solar microwave community to complement ground based data (only available for few hours, not in real 0me, not inter-calibrated) for solar microwave burst analysis and impacts on onground services (e.g. flight radar); Space weather community: SMOS Sun L-band polarimetry observa0on is a unique asset to study or analyze GPS circular signal anomaly poten0ally due to erup0ve Sun that might impact several services based on GPS.
26 SMOS L1 Sun BT Valida0on against on-ground radio-telescope network Many thanks for your aien0on
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