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The Hinode EUV Imaging Spectrometer: In-Orbit Performance and Early Results

The Hinode EUV Imaging Spectrometer: In-Orbit Performance and Early Results STEREO-SECCHI Consortium Meeting Paris, 5 th – 8 th March, 2007 L. Culhane , L. Harra, D. Williams G. Doschek, J. Mariska H. Hara Mullard Space Science Laboratory D. Brooks T. Watanabe

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The Hinode EUV Imaging Spectrometer: In-Orbit Performance and Early Results

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  1. The Hinode EUV Imaging Spectrometer: In-Orbit Performance and Early Results STEREO-SECCHI Consortium Meeting Paris, 5th – 8th March, 2007 L. Culhane, L. Harra, D. Williams G. Doschek, J. Mariska H. Hara Mullard Space Science Laboratory D. Brooks T. Watanabe University College London US Naval Research Lab NAOJ

  2. SUMMARY OF TALK • Outline of Hinode/EIS features and in-orbit performance • Some early EIS observations • Observation planning with Hinode/EIS • Conclusions

  3. EIS - Instrument Features • Large Effective Area in two EUV bands:170-210Åand 250-290 Å • Multi-layer Mirror (15 cm dia ) and Grating; both with optimized Mo/Si Coatings • CCD camera; Two 2048 x 1024 high QE back illuminated CCDs • Spatial resolution: 1 arc sec pixels/2 arc sec resolution • Line spectroscopy with ~ 25 km/s per pixel velocity sampling • Field of View： • Raster: 6 arc min × 8.5 arc min (max height: 17 arc min) • FOV centre moveable E – W by ± 15 arc min • Wide temperature coverage: log T = 4.7, 5.4 - 7.3 K • Simultaneous observation of up to 25 lines/spectral windows

  4. Primary Mirror Four positions: 1 and 2 arc sec slits 40 and 266 arc sec slots - all with 1024 pixels/ 17 arc min height Entrance Filter CCD Camera Front Baffle Grating • EIS first light: 28th October, 2006 EIS Optical Layout Primary mirror (offset parabola) S L 1939mm Slit exchanger Shutter Entrance filter CCDs Filter L S 1440mm 1000mm Concave grating

  5. Wavelength Resolution • First-light spectra from a small emerging AR on 28-OCT-2006 Wavelength = 195.12 Å (Fe XII) Dl (FWHM) = 52 mÅ (pre-launch calibration) = 55 mÅ (AR observation) – TD (Fe XII) ~ 1.3 MK – vnt ~ 20 km/s Agreement after allowance for TD and vnt Wavelength = 256.32 Å (He II) Dl (FWHM) = 65 mÅ (pre-launch calibration) = 115 mÅ (AR observation) – TD (He II) ~ 0.08 MK – vnt ~ 20 km/s Additional line broadening due to opacity and/or larger non-thermal component?

  6. Spatial Resolution - EIS and CDS • EIS and CDS Rasters of AR 10926 on 01-DEC-2006 Hinode EIS → Nominal Dq 2.1 arc sec SOHO CDS → Nominal Dq 5 arc sec

  7. Spatial Resolution – EIT, EIS and TRACE EIT 195 Å Image 23-JAN-07 11:12:09 UT EIS 195 Å Raster - 1 arc sec slit 23-JAN-07 10:47:09 to 11:37:02 UT TRACE 195 Å Image 23-JAN-07 11:12:18 UT Resolution → 5.0 arc sec 2.1 arc sec 1.0 arc sec Pixel size → 2.6 “ “ 1.0 “ “ 0.5 “ “

  8. 266 arc sec slot Active Region Slot Movie He II 256 Å Fe XV 284 Å 512 arc sec 266 arcsec 266 arcsec

  9. Active Region Slot Raster Image 850 arc sec EIS Fe XV 284 512 arc sec Image assembled from 266 arc sec x 512 arc sec slot exposures

  10. He II 256 Fe VIII 185 Fe X 184 Fe XI 188 Fe XII 195 Fe XIII 202 Fe XIV 274 Fe XV 284 • SOT B-Field • index gives polarity • Stokes V signal • - White: +ve • - Black: -ve Active Region Raster • 03-Dec-2006; 15:32 – 17:46 UT • - 1 arc sec slit with 1 arc sec scan step

  11. Logne [cm-3] 10.5 Fe XIII 196.5/Fe XIII 202.0 Fe XIII 203.8/Fe XIII 202.0 10.0 9.5 EIT 171 Å Slit 9.0 8.5 13:00 UT Electron Density–sensitive Line Ratios • Fe XIII line ratios from an along-slit observation (150 arc sec) on 03-NOV-2006 • -includes part of an AR (data from Peter Young, RAL) • - intensity ratio vs ne plots from Chianti

  12. Electron Density Mapping Fe XIII 202.2 Å Fe XIII 203.8 Å • EIS 1 arc sec slit raster at • 11:25 UT on 01-DEC-2006 • 2-D density map derived from the • ratio of the Fe XIII line intensities • (data from P. Young, RAL) • 8.2 < log ne < 10.0 ne (cm-3) Log ne

  13. SOHO EIT • Part of a 17 line observation on 28-DEC-2006 • – location and coverage of raster indicated on EIT image Active Region, Quiet Sun and Coronal Hole Raster • Raster has 2" slit, 2"steps and covers 240" x 240" with 5s exposure/13 m cadence

  14. Flare of 17-DEC-2006 • EIS 256“ x 256“ raster - 1“ slit • is scanned right to left • He II (log T = 4.9) and ions for • 6.0 < log T < 6.7 • Ratio of Fe XV to Fe XIV • intensity will give Te map

  15. Ca XVII & O V 192 (Fe XI subtracted) Intensity FWHM Log DN km/s Flare of 17-DEC-2006 • GOES plot shows a LDE • Spectra show bi-directional Doppler flows • from loop-top - also flows at footpoints • RHESSI missed event start but shows • soft spectrum through the event

  16. EIS and XRT Observation of Jets in Polar Region • EIS 40 arc sec slot images 20-JAN-2007;12:13 UT to 17:12 UT • Analysis will focus on time variation of jettemperature and plasma flow

  17. EIS Observer OBSERVER Science Summary & Study Plan Science Schedule Coordinators (SSCs) EIS Select Standard Study Formulate New Study Validate on Hardware Simulator EIS SSCs Hinode SSCs Monthly Telecon Hinode Montlly Strategy & Planning Meeting/Telecon HINODE Hinode Weekly Meeting Hinode Daily Meeting OBSERVATION Observing with Hinode/EIS • Planning requires installation of EIS SolarSoft tree • Study Preparation • Line Lists • Raster Definition • Study Definition • Users export studies to ASCII format • Include science case and summary then e-mail to: • “eis_obs@mssl.ucl.ac.uk”

  18. EIS_MK_RASTER • Compile Line List and construct Raster format

  19. EIS_MK_STUDY • Compile Study

  20. Conclusions • Following the Hinode launch (23-SEP-2006) and instrument first light (28-OCT-2006), EIS is now performing well in orbit • There is no evidence of contamination on optics or CCDs • Performance parameters: • wavelength resolution is nominal (Dl ~ 55 mÅ at 200 Å) • spatial resolution is close to the design goal of 2 arc min • throughput appears nominal and stable with time after five months in orbit • EIS 90 day science plan has been essentially completed • Active Region, Quiet Sun and Flare observations have been carried out • Major joint observing campaign with SUMER will be undertaken in April • We look forward to fruitful collaboration with STEREO for Sun-Earth studies

  21. Access to Hinode data • Chief Coordinators: • John Davis (john.m.davis@nasa.gov) • Tetsuya Watanabe (watanabe@uvlab.mtk.nao.ac.jp) • Science Schedule Coordinators (in U.S.): • SOT: T. Berger (berger@lmsal.com) • XRT: L. Golub (golub@cfa.harvard.edu) • EIS: J. Mariska (mariska@nrl.navy.mil) L. Culhane (jlc@mssl.ucl.ac.uk) in Europe • XRT Observing (XOB) Proposals: http://solar.physics.montana.edu/HINODE/XRT

  22. END OF TALK

  23. ラスタースキャン観測：LDEフレア Intensity FWHM Ca XVII 192 足元に幅広い輝線？ O Vのブレンドによる カスプループの周り に幅広い輝線 周囲にはFe XXI等の 高温輝線も確認 Ca XVII Fe XV284 / Fe XIV274 Fe XV284 / Fe XIV274 輝線強度比： 外側ほど温度が 高くなっている ことを示している Fe XXI Fe XXII

  24. 24-OCT-2006 XRT Movie (Full Sun) • Evolution of very small • structures e.g. Coronal • Bright Points, may be • followed

  25. SOT EIS FPP XRT Payload includes: - 0.5m optical telescope (SOT) with a focal plane package (FPP) for 0.25 arc sec images and vector magnetograms - EUV Imaging Spectrometer (EIS) with 2 arc sec resolution - Imaging X-ray Telescope (XRT) with 2 arc sec resolution Science goals: - Determine how the corona is heated in active regions and in the quiet Sun - Establish the mechanisms that give rise to transient phenomena, such as flares and CMEs - Investigate the processes responsible for energy transfer in the quiet Sun. JAXA/ISAS Hinode Spacecraft SOT/FPP: NAOJ, ISAS/Lockheed Martin, HAO EIS: MSSL, Birmingham, RAL, US NRL with integration on spacecraft by NAOJ and ISAS XRT: Harvard CfA, NAOJ, ISAS All participants are involved in Post-launch Mission Operations and Data Analysis

  26. Launch Readiness Three Solar-B Instruments before installation in the spacecraft MV Launch Launch of Solar-B, now Hinode, at 06:36 JST on Saturday 23rd Nov. 2006 Orbit 680 km Sun-synchronous

  27. Solar images at identical respective points in the solar cycle, seen by Hinode/XRT and Yohkoh/SXT Hinode XRT October 28, 2006 Yohkoh SXT November 28, 1995

  28. XRT and EIS

  29. 30,000 Km 30,000 Km 150,000 km 150,000 km Images (40 arc sec slot) of part of a newly emerging active region (AR 10919) observed on 29-OCT-2006 Theoretical fits to line profiles, like those shown in blue, permit the determination of physical parameters of the gas such as temperature, density and velocity to be measured by EIS on a spatial scale of 1500 km.

  30. Quiet SunGranules and Magnetic Elements Ca II H (chromosphere) G-band (photosphere)

  31. SDO and Hinode Missions • Hinode • Three main science goals: • - Determine how the corona is heated in active regions and in the quiet Sun • - Establish mechanisms that give rise to transient phenomena e.g. flares, CMEs • - Investigate quiet Sun energy transfer processes • Three instruments • - Solar Optical Telescope (SOT): Precision velocity, LOS and vector B fields at 0.2” • - EUV Imaging Spectrometer (EIS): High wavelength resolution EUV spectral imagesat 2” • - X-ray Telescope (XRT): X-ray filter images at 2” • SDO gives full-Sun coverage at very high cadence • Hinode emphasises limited spatial coverage (≈ 4 x 4 arc min2) at very high resolution

  32. XRT Movie (Active Region) • 11-NOV-2006 with thin Al filter •  response range 6 – 60 Å or • 0.2 – 2.0 keV • Many complex brightenings •  transient AR loop brightenings? • Cusp and sigmoid formation •  signatures of magnetic • reconnection and eruption? • Important to make detailed study • of AR magnetic configuration

  33. Fe XII 195 He II 256 Fe XV 284 Ca XVII/Fe XI 192 Flare of 17-DEC-2006 • Raster images of flare • GOES plot shows a LDE • RHESSI missed start but shows • soft spectrum through the event

  34. Flare of 17-DEC-2006 • EIS 256“ x 256“ raster - 1“ slit • is scanned right to left • He II (log T = 4.9) and ions for • 6.0 < log T < 6.7 • Bi-directional Doppler shifts • seen in the loop-top source

  35. EIS Observer OBSERVER Science Summary & Study Plan Science Schedule Coordinators (SSCs) EIS Select Standard Study Formulate New Study Validate on Hardware Simulator EIS SSCs Hinode SSCs Monthly Telecon Hinode Montlly Strategy & Planning Meeting/Telecon HINODE Hinode Weekly Meeting Hinode Daily Meeting OBSERVATION

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