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, 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


• 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


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


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


• 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


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 “ “


Active Region Slot MovieHe II 256 Å

51

2 a

rc se

c

266 arcsec

266 arc secslot

Fe XV 284 Å

266 arcsec


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


• 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


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


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


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


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


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


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


• 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


• Compile Line List and construct Raster format

EIS_MK_RASTER


• Compile Study

EIS_MK_STUDY


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


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


END OF TALK


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


XRT Movie (Full Sun)

24-OCT-2006

• Evolution of very small structures e.g. Coronal Bright Points, may be followed


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


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


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


XRT and EIS


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


Quiet SunGranules and Magnetic Elements

G-band (photosphere) Ca II H (chromosphere)


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


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


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


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


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

the hinode euv imaging spectrometer: in-orbit performance and early results

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