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
2Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
SUMMARY OF TALK
• Outline of Hinode/EIS features and in-orbit performance
• Some early EIS observations
• Observation planning with Hinode/EIS
• Conclusions
3Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• Large Effective Area in two EUV bands: 170-210 Å and 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
EIS - Instrument Features
4Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
EIS Optical Layout
Slit exchanger
Primary mirror (offset parabola)
Entrance filter
Concave grating
Filter
CCDs
Shutter
1939mm
1440mm1000mm
Grating
Front Baffle
Entrance Filter
Primary Mirror
CCD Camera
SL
LS
• EIS first light: 28th October, 2006
Four positions:1 and 2 arc sec slits40 and 266 arc sec slots- all with 1024 pixels/ 17 arc min height
5Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Wavelength = 195.12 Å (Fe XII)(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 Resolution
Wavelength = 256.32 Å (He II)(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/orlarger non-thermal component?
• First-light spectra from a small emerging AR on 28-OCT-2006
6Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• EIS and CDS Rasters of AR 10926 on 01-DEC-2006
HinodeEIS →
Nominal 2.1 arc sec
SOHOCDS →
Nominal 5 arc sec
Spatial Resolution - EIS and CDS
7Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Spatial Resolution – EIT, EIS and TRACE
EIT 195 Å Image23-JAN-0711:12:09 UT
TRACE 195 Å Image23-JAN-0711:12:18 UT
EIS 195 Å Raster- 1 arc sec slit23-JAN-0710:47:09 to 11:37:02 UT
Resolution → 5.0 arc sec 2.1 arc sec 1.0 arc sec Pixel size → 2.6 “ “ 1.0 “ “ 0.5 “ “
8Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Active Region Slot MovieHe II 256 Å
51
2 a
rc se
c
266 arcsec
266 arc secslot
Fe XV 284 Å
266 arcsec
9Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Active Region Slot Raster Image
EIS Fe XV 284
Image assembled from 266 arc sec x 512 arc sec slot exposures
512 arc sec
850 arc sec
10Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• SOT B-Field index gives polarity• Stokes V signal - White: +ve - Black: -ve
Active Region Raster
He II 256 Fe VIII 185 Fe X 184 Fe XI 188
Fe XII 195 Fe XIII 202 Fe XIV 274 Fe XV 284
• 03-Dec-2006; 15:32 – 17:46 UT - 1 arc sec slit with 1 arc sec scan step
11Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Electron Density–sensitive Line Ratios
10.0
9.0
Log ne [cm-3]
9.5
8.5
10.5
Fe XIII 203.8/Fe XIII 202.0Fe XIII 196.5/Fe XIII 202.0
• 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
EIT 171 Å
13:00 UT
Slit
12Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Fe XIII 202.2 Å Fe XIII 203.8 Å
ne (cm-3) Log ne
Electron Density Mapping
• 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
13Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Active Region, Quiet Sun and Coronal Hole Raster
SOHO EIT
• Part of a 17 line observation on 28-DEC-2006 – location and coverage of raster indicated on EIT image
• Raster has 2" slit, 2"steps and covers 240" x 240" with 5s exposure/13 m cadence
14Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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
15Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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
Ca XVII & O V 192 (Fe XI subtracted)
Log DN
Intensity
km/s
FWHM
16Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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 jet temperature and plasma flow
17Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• 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: “[email protected]”
Observing with Hinode/EIS EIS Observer
Science Summary& Study Plan
Science Schedule Coordinators (SSCs)
Select Standard Study Formulate New Study
Validate on HardwareSimulatorEIS SSCs
Hinode SSCsMonthly Telecon
Hinode MontllyStrategy & Planning
Meeting/Telecon
Hinode Weekly Meeting
Hinode Daily Meeting OBSERVATION
OBSERVER
EIS
HINODE
18Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• Compile Line List and construct Raster format
EIS_MK_RASTER
19Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
• Compile Study
EIS_MK_STUDY
20Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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 ( ~ 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
21Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Access to Hinode data• Chief Coordinators:
– John Davis ([email protected])– Tetsuya Watanabe ([email protected])
• Science Schedule Coordinators (in U.S.):– SOT: T. Berger ([email protected])– XRT: L. Golub ([email protected])– EIS: J. Mariska ([email protected])
L. Culhane ([email protected]) in Europe
• XRT Observing (XOB) Proposals: http://solar.physics.montana.edu/HINODE/XRT
22Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
END OF TALK
23Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
ラスタースキャン観測: LDE フレア
Intensity FWHMCa XVII 192
Fe XV284 / Fe XIV274
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
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 XXIFe XXII
Ca XVII
24Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
XRT Movie (Full Sun)
24-OCT-2006
• Evolution of very small structures e.g. Coronal Bright Points, may be followed
25Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
JAXA/ISAS Hinode SpacecraftPayload 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.
All participants are involved in Post-launch Mission Operations and Data Analysis
SOT
FPP
EIS
XRT
SOT/FPP: NAOJ, ISAS/Lockheed Martin, HAO
XRT: Harvard CfA, NAOJ, ISAS
EIS: MSSL, Birmingham, RAL, US NRL withintegration on spacecraft by NAOJ and ISAS
26Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Three Solar-B Instrumentsbefore installation in thespacecraft
MV LaunchLaunch of Solar-B, now Hinode, at 06:36 JST on Saturday 23rd Nov. 2006
Launch Readiness
Orbit680 km Sun-synchronous
27Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Solar images at identical respective points in the solar cycle, seen by Hinode/XRT and Yohkoh/SXT
Hinode XRTOctober 28, 2006
Yohkoh SXTNovember 28, 1995
28Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
XRT and EIS
29Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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.
30,000 Km
15
0,0
00
k
m
30,000 Km
15
0,0
00
k
m
30Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
Quiet SunGranules and Magnetic Elements
G-band (photosphere) Ca II H (chromosphere)
31Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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 images at 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
32Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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
33Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
He II 256 Fe XII 195
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
34Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
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
35Len Culhane, 8th March, 2007 Hinode/EIS: Performance and Early Observations STEREO/SECCHI, Paris
EIS Observer
Science Summary& Study Plan
Science Schedule Coordinators (SSCs)
Select Standard Study Formulate New Study
Validate on HardwareSimulatorEIS SSCs
Hinode SSCsMonthly Telecon
Hinode MontllyStrategy & Planning
Meeting/Telecon
Hinode Weekly Meeting
Hinode Daily Meeting OBSERVATION
OBSERVER
EIS
HINODE