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Review of RESIK X-ray spectra database

eHeroes activity. Review of RESIK X-ray spectra database. J. Sylwester, M. Kowaliński, B. Sylwester, A. Kepa Space Research Centre, PAS Wrocław. the XIIth Hvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory .

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Review of RESIK X-ray spectra database

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  1. eHeroesactivity Review of RESIK X-ray spectra database J. Sylwester, M. Kowaliński, B. Sylwester, A. Kepa Space Research Centre, PAS Wrocław the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  2. RESIK operated aboardCORONAS-F Russian satellite Launched 31 July 2001, polar orbit, 95min, ~550 km semi-Sun-synchronous x 10, the XIIth Hvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  3. S/C nights & days polar Sun-synchronous orbit for most of the timenightsinterrupt the observations, but detectorswere on Except the high backgroundparticles regions the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  4. Dispersion planes N S A B 1 2 3 4 II Position on the payload complicated wignietting pattern RESIK the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  5. РентгеновскийСпектрометрсИзогнутымиКристалламиРентгеновскийСпектрометрсИзогнутымиКристаллами Bragg law: kλ=2d sinΘRESIKis the lowestfluorescencespectrometer Measures spectra in the range: ~ 3.3 Å ÷ 6.1 Å, instantaneously in all λ 20 kg Keypeople: Len Culhane, George Doschek V.D. Kuznetsov, Jim Lang, R.D. Bentley

  6. the XIIth Hvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  7. Processing the signal from detectors chan 1 chan 3 chan 2 chan 4 Detector A Detector B (32 μs) Position encoding Amplitude All x = w1/ (w1+w2) is inside the amplitude limits? are both recorded within 1 μs? In-window spectrum each DGI Encoded eachspectral DGI 2-300s the XIIth Hvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  8. Identification of new satellite lines the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  9. The database: http://www.cbk.pan.wroc.pl/experiments/resik/RESIK_Level2/index.html 30 flares, ~4000 spectra, AR: ~300 spectra the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  10. Examplesummaryplots the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  11. Examplesummaryplots the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  12. RESIK average abundances compared with other determinations Aphot. from Asplund et al. Ann. Rev. Astron. Astrophys. 2009. 47:481–522, Acoronalfrom CHIANTI, extendedcoronal, mostly Feldman, U., Mandelbaum, P., Seely, J.L., Doschek, G.A., Gursky H., 1992, ApJSS, 81, 387 * from proxies the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  13. DEM evolutionfor SOL2002-12-26T08:30Barbara, Tomek Mrozek Total & cooler GOES Hot T>9 MK Hot T>9 MK the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  14. Fitting the spectra in DEM the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  15. RHESSI for SOL2002-12-26T08:30 D=4.5 x 108 cm If we consider the total EM of the hot component to be contained in the RHESSI bright kernel, this allows for the estimatation of the densityof hot plasma.

  16. RESIK & RHESSI 26 April 2003, 03:03:12 – 03:05:32 UT Withoutattenuators acceptable agreement the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  17. Diagnostics of non-thermal distributions Elena, Alena The nonthermal analysis of RESIK spectra has shown that the largest deviations of the plasma electron distribution from Maxwellian appeared during the impulsive phase of the flare. The decay phase spectra had an almost isothermal character.. the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  18. The heritage - ADS title:RESIK the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  19. The main effects that contaminate raw spectra: Fluorescence: crystal (Si Kα 1.75 keV),twolonger-wavelenghtchannels Fixed pattern structure (notches) – due to the ADC converter in position encoding (depends on HV and ADS values)‏ Orbital background: Non-solar X-ray illumination Auroral Oval and South Atlantic Anomaly the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  20. Optical and X-ray nights Occultation of X-raysourcestakes place earlier/laterthan in the visiblerange as the absorptioniscompleteatheights~100 -150 km

  21. Processing the signal from detectors chan 1 chan 3 chan 2 chan 4 Detector A Detector B (32 μs) Position encoding Amplitude All x = w1/ (w1+w2) is inside the amplitude limits? are both recorded within 1 μs? In-window spectrum each DGI Encoded eachspectral DGI 2-300s the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  22. Summed PHA - analysis Detector B #0 Wavelength channel No 2 Courtesy: Alena Kulinova

  23. Bcg spectrum 7 Apr 2003, 09417_1, 17.5 – 17.8settings: HV, ADS 1389_1328_110_230_110_230_110_230_140_230 4914 4984 4822 3703 Hiddenbins the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  24. Non-solar X-rays the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  25. Sco-X1 the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  26. Auroras Ambientauroralemission the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  27. How to recognize X-ray aurora Equatorial locations Polar locations the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  28. Understanding amplitude signal F 1.75 keV The statistical uncertainties in the number of ion-electron pairs formed and gas gain result in a pulse amplitude distribution where photons of constant energy are absorbed. Detector resolution, Γ, (in eV) is the full width at half maximum of its pulse amplitude distribution, given empirically b F 1.75 keV silicon S1 3kev S1 3kev Fe55 F 1.75 keV F 1.75 keV S3 6.6keV Quartz SiO2 S1 2.2 S1 2.2 S2 4.4keV S2 4.4keV the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  29. optimum 2% 0.2% 25% 20% Components of the spectral signal early 5% 1% 95% 90% the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  30. eHeroes Whathaschangedrecently • New morepowerfulserverisavailable (128 GB RAM) • Full set of primaryreduced RESIK data can be accessed (30 GB): • ~2 mln DGI for signalpulse-heightanalysis • 0.2-10 keV spectra in 31 bins, • Particlesignal 1 bin • DGI, 10 & 2 s • ~1.3 mln individual spectra, 60 000 with goodsettings the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  31. Dynamic spectra collection the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  32. Dynamic spectra collection 2 the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  33. Optimum settings 60k spectra the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  34. the XIIthHvar Astrophysical ColloqiumSeptember 3 -7, 2012 the 40th anniversary of Hvar Observatory

  35. the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  36. Uninvestigatedareas • Magnetosphericstudies • Distribution of particles on L shells • Study of geomagneticstorms • SAA vriability • Solar studies • Reduction of allgood spectra to Level2 (90%) • Contribution of higherreflectionorders • Non-maxwelliandistribution diagnostics • Impact on electronics • Investigation of allglitches • Temperaturedistributioninside the instrument the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  37. Radiation environment on its circular ~500 km orbit inclined at ~83 deg, polar radiation ovals filled with energetic particles are being crossed 4 times each orbital period SAA is encountered ~ 6 times a day – best seen on PIN sensor the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  38. HigherOrders the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  39. Conclusions • Access to Resikfulldatabasehasstill a lot of newdiscoveries to offer • We arelooking for a talentedpeople to invite to work in ourgroup • We are in a process of converting the data into FITS format and contributethem to the SODA database (SOTERIA) • Right now, we canprovide the IDL *.savlarge file with descriptions (30 GB) • Altitude & attitude, PHA, spectra, Times JD etc

  40. Thankyou ! All interested people, please contact me js@cbk.pan.wroc.pl the XIIthHvar Astrophysical Colloqium September 3 -7, 2012 the 40th anniversary of Hvar Observatory

  41. 2002 8 24 1:12 X3.1 4.6e-004 S02W81 -16.02 + 2002 4 9 0:42 M2.1 1.1e-005 N19E46 -0.36 + super 2002 8 29 12:52 M3.2 1.5e-005 S18E73 15.33 +

  42. Geometry optimization RHESSI location Si XIII 1s2-1s3p 40 flares (+) offset Si XIII 1s2-1s4p z, k x, y w

  43. Double, position sensitive detector: Yohkoh BCS type w2 Anode ~1400 V w&w cathode 256 binów 45  10 w1 w1 Bin No = w1 + w2

  44. Offsets from line positions

  45. 0.16 for Fe55 0.29 for Si Instrumental width: detector position resolution λ/Δλ ~ 1000

  46. We know ADS And HV LUT MAP 255 • Solar spectrum w(k+1).uu(k+1) w(k). uu(k) w(k-1). uu(k-1) Σ=theoretical flat field with Notches -HV | HV + • Si fluor. • Particle b/g PHA Σ= w’s 0 0 255 Due to ADS In order to obtain realistic look-up “relation” we should sum-up over those uu relations which are of interest for a given set of ADS settings used. The relation is dependent on: HV & ADS

  47. FPS: Monte-Carlo model 100 80 60 W1+w2 40 20 „Uniform illumination” q=<const

  48. Removing FPS – dependence on HV & ADS Same HV, different # (ADS) Same channel #1, different HV & ADS #0 1480 V, 96-165 #1 1480 V, 20-160 1450 V, 135-200 #2 #3 1450 V, 70-120

  49. Calibrations • Laboratory • at RAL Yohkoh BCS chamber • at MSSL some detector rests • In-flight • Detector ageing (position of Fe55) 5.9 keV peak against the 32 bit amplitude scale • ADS (amplitude discriminator settings)

  50. RAL vacuum chambers

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