# Presentation: 560418

## Overview of EIS Performance

**Overview of EIS Performance**

**H. Hara**
**National Astronomical Observatory of Japan**
**2007 Aug 21**
**Hinode Sci. Meeting, Trinity College in Dublin, Ireland**

## HINODE Telescopes 

- <date/time>

*HINODE* Telescopes

- X-ray Telescope
- (XRT)

- Solar Optical Telescope
- (SOT)

- EUV Imaging Spectrometer
- (EIS)

- EIS

- XRT

- SOT

## Solar Atmosphere

- <date/time>

- TR/Corona (EUV)

- Height from Photosphere (km)

**SOT**

**EIS**

- Corona

**XRT**

- Photosphere

- Chromosphere

**Corona**

**Transition**
**Region**

- Temperature (K)

## EIS Optical Layout

- Slit exchanger

- Primary mirror (offset parabola)

- Entrance filter

- Concave grating

- Filter

- CCD

- Shutter

- 1939 mm

- 1440mm

- 1000mm

**S**

**L**

**L**

**S**

## References for Instrumentation

- Overall
-     Culhane et al. 2007, Solar Phys. in press
-             (On-line version is available in the Journal page.)
- Optics and mechanisms
-     Korendyke et al. 2006, Appl. Opt., 45, No.34, 8674
- Calibration issues
-     Lang et al. 2006, Appl. Opt., 45, No.34, 8689

## Performance

- Large Effective Area in EUV band:     170-210 A & 250-290 A
-        Mo/Si **multi-layer coated** Mirror and Grating
-         High QE CCD: Two 2048×1024 back illuminated CCD
- Spatial resolution: 2 arcsec resolution over raster-scan area
-                                    (1 arcsec pixel sampling)
- Line spectroscopy of 20-30 km/s pixel sampling
- Instrumental width in emission lines for 1 arcsec slit observation:
-                                    short- band: 47 mA,  long- band: 58 mA  at ground CAL
- Raster-scan area (EW×NS): 576×512  arcsec2 max. for 1” width slit
-                                        FOV center can move in East-West direction
-                                        by 890 arcsec.
- Wide temperature coverage: log T = 4.7, 5.4, 6.0-7.3
- Simultaneous observation of multiple lines up to **25**

**short-******** band     long-******** band**

## Observables

- <date/time>

**Information from a single emission line**
- Line intensity
- Line shift by Doppler motion
- Line width:    temperature,  non-thermal motion
**Information from selected two line ratio**
- Temperature
- Density

## Field of View

- <date/time>

*E*

*S*

**        ****EIS **(576”x512”)

**XRT**
- (2048”x2048”)

*W*

**SOT:**NFI/SP
- (328”x164”)

**SOT:** BFI
- (205”x102”)

*N*

## Four slit selections available
Direction of slit length: north-south direction
EUV line spectroscopy
     - 1 arcsec  L arcsec slit for the best quality of image/spectrum quality
      - 2 arcsec  L arcsec slit for a higher throughput

EUV Imaging (Velocity information is convolved.)
     - 40 arcsec  L arcsec slot for imaging with little overlap
     -266 arcsec  L arcsec slot for hunting transient events  

- <date/time>

- Four slit selections available
- Direction of slit length: north-south direction
**EUV line spectroscopy**
-      - 1 arcsec  L arcsec slit for the best quality of image/spectrum quality
-       - 2 arcsec  L arcsec slit for a higher throughput
**EUV Imaging** (Velocity information is convolved.)
-      - 40 arcsec  L arcsec slot for imaging with little overlap
-      -266 arcsec  L arcsec slot for hunting transient events

- EIS Slit/Slot

**L > 1024 arcsec (=CCD height)**

**By the update of control software in Aug 2007,**
**the exchange of slit is possible at any time.  **

## EIS Slit Observation- Slit of 1arcsec width -

**AR**

- 2006 Nov 04  11:50 UT: 160 sec exposure

- 1024
- arcsec

- Fe XIII

- Fe XIV

- Fe XI

- Fe XII

- Fe X/XI

- Fe X

- Fe XV

- Si X

- Fe XIV

- Fe XIII

- He II

- Fe XVI

## Wavelength Calibration

|  | λ0
Å | A
Å/pixel | B
Å/pixel2 |
| --- | --- | --- | --- |
| SW CCD | 166.1435 | 0.0223 | -6.53E-09 |
| σ coeff | 0.0014 | 2.77E-06 | 1.19E-09 |
| σ fit | 0.0015 |  |  |
| LW CCD | 199.9719 | 0.0223 | -1.112E-08 |
| σ coeff | 0.0013 | 9.50E-06 | 1.625E-09 |
| σ fit | 0.0015 |  |  |

- Brown et al. (2007)

## Sit & Stare Observation

- Mariska et al. (2007)

- Fe XII 195

- Fe XV 284

- Intensity

- Doppler

## EIS Observations

**40****"**** slit raster**

**2****"**** slit raster**

**1****"**** slit raster**

**266****"**** slit raster**
- (no mirror motion)

**Examples of 240" ********240" Raster Scan**

- 240 "

- 240 "

- Contribution of
- other emission lines

- Wider instrumental width

- EUV imaging  of
- less contamination
- by other lines

- Discontinuous
- raster

## EIS Raster Scan Observation

- <date/time>

- 2006 Dec 03  15:32 – 17:46 UT

- 1”-width slit, 1” scan step

- SOT FG Magnetic-Field Index

- White:N polarity
- Black:S polarity

- He II 256 / log T=4.7

- Fe VIII 185/ log T=5.8

- Fe X 184 / log T=6.0

- Fe XI 188 / log T=6.1

- Fe XII 195 /log T=6.2

- Fe XIII 202 / log T=6.2

- Fe XIV 274 / log T=6.3

- Fe XV 284/log T=6.4

## Raster scan movie

- SOHO EIT

- Systematic jitter is mostly due to thermal distortion of S/C and EIS components.

## Fast raster by coarse stepping(2.6 min cadence)

- Fe XVI

- Fe XII

- Fe XXIII

- Fe XVII + Fe XXIV

- He II

- Fe XI+Ca XVII

- Fe XI +Fe XXIV

- Fe VIII

- Fe X

- Fe XI

- Si VII

## Slot Observation

**EIS Fe XV 284**** **
**( log T = 6.3  ****)**

## Density sensitive line ratio

- From  P. Young

- 10.0

- 9.0

- Position long the slit (pixel)

- log10( Ne [cm-3] )

- 9.5

- 8.5

- 10.5

- Fe XIII 203.8/Fe XIII 202.0

- Fe XIII 196.5/Fe XIII 202.0

- Fe XIII density sensitive line ratio

## 2006 Dec 17 Flare

- <date/time>

- 

- Y

- Y

- X

- Scanning direction ( time )

- 8x104 K

- 1x106 K

- 2x106 K

- 6x106 K

- Hara et al. (2007)

## 2006 Dec 17 Flare Flare observation in Ca XVII

- 2006 Dec 17 Flare Flare observation in Ca XVII

- Ca XVII

- Fe XI

- Fe XI

- O V

- 3240 ph/pixel
- at peak

- 127 ph/pixel
- at peak

- Cusp above limb

- Disk

- Hara et al. (2007)

- Good example of line blending

## 2006 Dec 17 Flare Flare observation in Ca XVII

- 2006 Dec 17 Flare Flare observation in Ca XVII

- Intensity

- Fe XI contribution is largely reduced by its subtraction.
- Instrumental line width is not subtracted.

**Ca XVII & O V 192**

- Intensity line ratio for temperature diagnosis

- log *I * [DN]

-  FWHM [ km/s ]

**Ca XVII, Fe XI & O V 192**

**Fe XV284 / Fe XIV274**

- Far side

- Hara et al. (2007)

## Intensity, Doppler, and FWHM 

- Intensity, Doppler, and FWHM

- Intensity

- Doppler

- FWHM

- Fe XII 195

- km/s

- km/s

- (contains instrumental width)

- log N (photons)

- scanning direction (=time)

- Hara et al. (2007)

## Blueshift in Fe XXIII and Fe XXIV

- -400 km/s

- -400 km/s

**Fe X VII+Fe XXIV**

- Watanabe et al. (2007)

## Orbital variation of line centers

- Line center (Data point in the slit direction are averaged)

- Orbital period

## Line center drift

- Fe XII 195 line center

- Brown et al. (2007)

- West limb

- East limb

## Spacecraft Doppler Motion

- S/C Doppler motion to the Sun needs to be corrected. This information is not contained in the FITS image header at the moment.
- This component needs to be removed from Doppler maps.

## Instrumental Width- Very Preliminary -

**HOP10 observation**

- W211

- W274

- W5303

- W5303

- W: observed FWHM of emission lines
- W*I*: instrumental line width

- Green line: Norikura

- EUV lines: EIS

**Under investigation**

- Unit: [km/s]

## Summary

- EIS is working with no major problems.
- Instrument performance is very good.
- Tutorial for simple analysis: see EIS web page at MSSL.
-     Some software is still under development.
- Keywords for careful data analysis
-     - Line blending
-     - line center drift
-     - solar image drift perpendicular to/along the slit
-     - uncertainty in instrumental line width
-     - uncertainty in effective area when line-ratio technique is   used.

## END

## Slide 30

## EIS Science

- <date/time>

***Yohkoh******, SOHO, and TRACE***:
-    reveal dynamic solar corona (flare, plasmoid, jet, coronal expansion ...)
- → Necessity of higher-cadence coronal velocity-field measurements
-      with SOT and XRT

- Photospheric motions

- Energy injection to corona
- Energy dissipation in corona

- Observation with
**EUV imaging spectrometer (EIS)**
- in emission-line spectroscopy and
- high-cadence imaging with **XRT**

- Observation with **SOT**

**Photosphere-corona connections**

***Coronal heating***

***Flare/CME physics***

- Reconnection physics, Site of large non-thermal line broadening, ...

## History (1)

- Starting point:
- 1993: T. Watanabe has proposed an EUV spectrometer of 4m long to SOLAR-B mission.
- 1994 Feb: Length of Spectrometer was reduced to 3.5 m to match the size of available volume in rocket fairing.

- wavelength range: 250-290 A
- Three reflection optics
- Multilayer coated optics
- Scanning mirror is an option.

## History (2)

- 1994:
-    H. Hara has started the feasibility
-    study and a system design of EIS.

**1994 Oct**

- 1995 Mar (in revised SOLAR-B mission proposal)

- Two reflection optics for high throughput.
- Need of back-illuminated CCD
- Scanning with primary mirror for raster scan
- wavelength range: 250-290 A
- Ray-tracing for spectrometer design
- 1.6” spatial sampling

## History (3)

- NRL and MSSL have proposed to join the development of EUV spectrometer.
- In the proposal to AO (1998):
-     Leading institute: NRL
-     Electronics and CCD camera: MSSL
-     S/C interface and S/C-level testing: ISAS+NAOJ
- After AO selection (affected by FPP development cost)
-     Leading institute: MSSL
-     Optics and mechanism: NRL
-     S/C interface and S/C-level testing: ISAS+NAOJ

## History (4)

- SOLAR-B Spectrometer in AO proposal by NRL to NASA (1998)
-              Three reflection spectrometer
-       wavelength range:170-210 A
-       1” spatial sampling

## EIS Sensitivity

| Ion | Wavelength
(A) | logT | Nphotons |  |
| --- | --- | --- | --- | --- |
|  |  |  | AR | M2-Flare |
| Fe X | 184.54 | 6.00 | 15 | 36 |
| Fe XII | 186.85 / 186.88 | 6.11 | 13/21 | 105/130 |
| Fe XXI | 187.89 | 7.00 | - | 346 |
| Fe XI | 188.23 / 188.30 | 6.11 | 41 / 15 | 110/47 |
| Fe XXIV | 192.04 | 7.30 | - | 4.0104 |
| Fe XII | 192.39 | 6.11 | 46 | 120 |
| Ca XVII | 192.82 | 6.70 | 31 | 1.8103 |
| Fe XII | 193.52 | 6.11 | 135 | 305 |
| Fe XII | 195.12 / 195.13 | 6.11 | 241/16 | 538/133 |
| Fe XIII | 200.02 | 6.20 | 20 | 113 |
| Fe XIII | 202.04 | 6.20 | 35 | 82 |
| Fe XIII | 203.80 / 203.83 | 6.20 | 7/20 | 38/114 |

- Detected photons per 11 area of the sun per 1 sec exposure.

| Ion | Wavelength
(A) | logT | Nphotons |  |
| --- | --- | --- | --- | --- |
|  |  |  | AR | M2-Flare |
| Fe XVI | 251.07 | 6.40 | - | 108 |
| Fe XXII | 253.16 | 7.11 | - | 71 |
| Fe XVII | 254.87 | 6.60 | - | 109 |
| Fe XXVI | 255.10 | 7.30 | - | 3.3103 |
| He II | 256.32 | 4.70 | 16 | 3.6103 |
| Si X | 258.37 | 6.11 | 14 | 62 |
| Fe XVI | 262.98 | 6.40 | 15 | 437 |
| Fe XXIII | 263.76 | 7.20 | - | 1.2103 |
| Fe XIV | 264.78 | 6.30 | 20 | 217 |
| Fe XIV | 270.51 | 6.30 | 17 | 104 |
| Fe XIV | 274.20 | 6.30 | 14 | 76 |
| Fe XV | 284.16 | 6.35 | 111 | 1.5103 |

- AR: active region

## Line Center Variation in Slit direction

- CCD1

- CCD0

- Line center c, OBS(y), c, MODEL(y)

- 1” width slit

##     Expected Accuracy of Velocity 

**Doppler **
**Velocity**

**Line **
**Width**

- FL-line (GOES-M2)

**Number of detected photons**
**(1****"********1****"**** area)****-1**** **

- AR-line

- AR-line

**Fe XII 195**

**Fe XII 195**

**Fe XV 284**

**Fe XV 284**

**Fe XXIV 255**

**Fe XXIV 255**

## Functionality not yet verified

- Response of XRT flare trigger
- Internal EIS flare trigger
- Internal EIS event trigger
- Automatic exposure control
- Anti-rotation compensation
- CCD bakeout heater operationy

## Comparison between FWHMOBS and FWHMRAL at CCDY=700

- Fe X 184:
-      FWHMOBS= sqrt(  (FWHMRAL+0.90)2+ (FWHMTH)2 +(FWHMNT)2
-         FWHMRAL: = 1.97 pixel
-         FWHMTH : estimated from Fe XI 188/FeX184 line ratio temperature
-       FWHMNT: 15 km/s assumed.
- Fe XV284
-       FWHMOBS= sqrt(  (FWHMRAL+0.43)2+ (FWHMTH)2 +(FWHMNT)2
-         FWHMRAL: = 2.71 pixel
-         FWHMTH : estimated from Fe XV 284/FeXIV274 line ratio temperature
-       FWHMNT: 15 km/s assumed.
**      ****GRA focus set point has not been adjusted after launch.**

- ~46% wider than FWHMRAL

- ~16% wider than FWHMRAL

## Data CompressionDPCM vs JPEG(Q=95)

- DPCM (loss-less compression)

- 12-bit  JPEG (Q=95)

- Error bar: 1-level

## Data CompressionDPCM vs JPEG (Q=95)

- DPCM: 2007/01/04 11:54:43 -11:57:19
- JPEG:   2007/01/0411:57:22 -11:59:58

- JPEG (Q=95)

- DPCM
- (loss less compression)

- Marks: 1 error

- shift due to
- orbital variation

## SLOT movie: Jet in a polar region

- relative CCD offset between two CCDs

- Jet

- South limb

- Kamio et al. (2007)