Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Introduction to the EIS instrument on Introduction to the EIS instrument on HinodeHinode
Dr Peter YoungDr Peter YoungRutherford Appleton Laboratory, UKRutherford Appleton Laboratory, UK
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Basic factsBasic facts
• EIS – EUV Imaging SpectrometerEIS – EUV Imaging Spectrometer• Successor to CDS on SOHOSuccessor to CDS on SOHO• Covers two wavelength bands: 170-211 Covers two wavelength bands: 170-211 Å, 246-292 ÅÅ, 246-292 Å• Principally for coronal spectroscopyPrincipally for coronal spectroscopy
• PI institutes: MSSL (UK), NRL (USA), NAOJ (Japan)PI institutes: MSSL (UK), NRL (USA), NAOJ (Japan)• PI: Prof Louise Harra (MSSL)PI: Prof Louise Harra (MSSL)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Instrument layoutInstrument layout
Single mirror for focussing – improves throughput of telescope
Multilayer coating – gives high reflectivity in EUV
Back-thinned CCDs – directly sensitive to EUV radiation
Aluminium filters – block out visible light
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Field of viewField of view
E
EIS (576”x512”)
XRT(2048”x2048”)
W
SOT:NFI/SP(328”x164”)SOT: BFI
(205”x102”)
N
A coarse offset can A coarse offset can also be applied to also be applied to offset EIS from the offset EIS from the other instrumentsother instruments
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
CCD imageCCD image
CCD-BShort wavelength170-211 Å
CCD-ALong wavelength246-292 Å
2048 pixels
1024
pix
els
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Slit optionsSlit options
• Four slits available, defined by their widthFour slits available, defined by their width• 1” and 2” slits are for spectroscopy1” and 2” slits are for spectroscopy• 40” and 266” slits for imaging40” and 266” slits for imaging
1”
266”
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Using wide slits: context imagesUsing wide slits: context images
Context slot raster, Fe XII 195Duration: 3min 20s
2” slit raster, Fe XII 195Duration: 22min
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Using wide slits: moviesUsing wide slits: movies
• The most ‘clean’ emission line for the 266” slit is Fe XV 284.16 (2 The most ‘clean’ emission line for the 266” slit is Fe XV 284.16 (2 million K)million K)
EIS wide slot movieFe XV 284.2 (logT=6.3)Courtesy H. Warren (NRL)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
The EIS spectrumThe EIS spectrum
• Spectrum dominated Spectrum dominated by coronal ions (iron, by coronal ions (iron, particularly)particularly)
• Few useful transition Few useful transition region lines, but not region lines, but not strongstrong
Young et al. (2007, PASJ, in press)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Telemetry limitationsTelemetry limitations
• The EIS data rate is limited to around 50 kbits/sThe EIS data rate is limited to around 50 kbits/s• Data are routinely compressed using DPCM (lossless) by a factor of Data are routinely compressed using DPCM (lossless) by a factor of
around 3around 3– JPEG (lossy) compression is also allowedJPEG (lossy) compression is also allowed
• Despite this, complete CCD data can not be obtained routinelyDespite this, complete CCD data can not be obtained routinely– Specific wavelengths (emission lines) must be chosenSpecific wavelengths (emission lines) must be chosen– reduced spatial coverage along slit (solar-Y)reduced spatial coverage along slit (solar-Y)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Science capabilityScience capability
• Transition region linesTransition region lines• Coronal iron linesCoronal iron lines• Flare linesFlare lines• Density diagnosticsDensity diagnostics• Line width and velocity mapsLine width and velocity maps
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Transition region linesTransition region lines
• EIS spectra are dominated by coronal iron lines, but there are a EIS spectra are dominated by coronal iron lines, but there are a number of useful transition region linesnumber of useful transition region lines
Density in loop footpointsDensity in loop footpoints
Young et al. (2007, PASJ)Young et al. (2007, PASJ)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Coronal iron linesCoronal iron lines
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Flaring loop (17 Dec)Flaring loop (17 Dec)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
SpectroscopySpectroscopy
• Emission line diagnostics come in two typesEmission line diagnostics come in two types
• Study of shape and position of emission linesStudy of shape and position of emission lines– yields plasma velocity, broadening parametersyields plasma velocity, broadening parameters
• Study of emission line strengthsStudy of emission line strengths– yields temperatures, densities, abundances, emission measureyields temperatures, densities, abundances, emission measure– requires detailed atomic datarequires detailed atomic data
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Doppler shiftsDoppler shifts
• Each emission line has a standard position (the Each emission line has a standard position (the rest wavelengthrest wavelength))• Shifts from this position imply motion of the plasmaShifts from this position imply motion of the plasma
– blueshiftsblueshifts: towards the observer: towards the observer– redshiftsredshifts: away from the observer: away from the observer
Blueshift Redshift
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Line width diagnosticsLine width diagnostics
• The width of emission lines can be written in velocity units as The width of emission lines can be written in velocity units as
• The components of The components of ΔΔvv are written as are written as
• where where
– ΔΔvvII is the instrumental width is the instrumental width
– 22kT/MkT/M is the thermal width is the thermal width– ξξ is the non-thermal velocity is the non-thermal velocity
22I
2 2 M
kTvv
c
v
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Line width and velocity mapsLine width and velocity maps
• Active region mapActive region map– Fe XII 195.12 Fe XII 195.12 ÅÅ– 2006 Dec 22006 Dec 2
Intensity
Velocity
Width
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Close-up of loop: line widthClose-up of loop: line width
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Close-up of loop: velocityClose-up of loop: velocity
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Caution: non-Gaussian profilesCaution: non-Gaussian profiles
• Line profiles are not always GaussianLine profiles are not always Gaussian
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Density diagnosticsDensity diagnostics
• Certain emission lines from particular ions have ratios that are Certain emission lines from particular ions have ratios that are sensitive to the plasma densitysensitive to the plasma density
• EIS is the first solar UV instrument to EIS is the first solar UV instrument to routinelyroutinely allow high precision allow high precision density measurements density measurements – high effective areahigh effective area– access to best coronal density diagnosticsaccess to best coronal density diagnostics
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Density mapsDensity maps
• The high quality of the EIS data make density maps easy to generateThe high quality of the EIS data make density maps easy to generate• Big improvement over SOHO/CDS density mapsBig improvement over SOHO/CDS density maps
Density map from SOHO/CDS
(Tripathi et al. 2006)
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Best density diagnosticsBest density diagnostics
IonIon RatiosRatios
Fe XIIFe XII
(logT=6.1)(logT=6.1)λλ186.88 / 186.88 / λλ195.12195.12
λ196λ196.64 / .64 / λλ195.12195.12
Fe XIIIFe XIII
(logT=6.2)(logT=6.2)λ196λ196.54 / .54 / λλ202.04202.04
λ203λ203.82 / .82 / λλ202.04202.04
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
Instrumental effects to be wary ofInstrumental effects to be wary of
• There is a spatial offset in both X and Y between the two EIS CCDsThere is a spatial offset in both X and Y between the two EIS CCDs– X: 2 pixels, Y: 15-20 pixelsX: 2 pixels, Y: 15-20 pixels
• The line centroids vary by around 60-70 km sThe line centroids vary by around 60-70 km s-1-1 through an orbit through an orbit• Line centroids and widths vary along the EIS slitLine centroids and widths vary along the EIS slit• The EIS slits are slightly tilted relative to CCDThe EIS slits are slightly tilted relative to CCD• There are a number of warm and hot pixels on the detectorThere are a number of warm and hot pixels on the detector• There are a few dust particles on the CCDsThere are a few dust particles on the CCDs
– affects Fe XI 188.23 and Fe XII 193.51affects Fe XI 188.23 and Fe XII 193.51• Image wobble (satellite & instrument) leads to strange effect in raster Image wobble (satellite & instrument) leads to strange effect in raster
moviesmovies
Dr Peter Young, Rutherford Appleton LaboratoryDr Peter Young, Rutherford Appleton LaboratoryHin
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Hin
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Hinode Data Analysis Workshop, Paris, Nov 2007Hinode Data Analysis Workshop, Paris, Nov 2007
EIS observationsEIS observations
• Basic observation units for EIS are called Basic observation units for EIS are called studiesstudies• Different studies have unique acronyms; there are over 220Different studies have unique acronyms; there are over 220
– e.g., COMSCI_AR3, PRY_footpoints_v2, SYNOP001e.g., COMSCI_AR3, PRY_footpoints_v2, SYNOP001
• Studies actually comprise one or more Studies actually comprise one or more rastersrasters• A raster can be, e.g.,A raster can be, e.g.,
– a scan of a region with the narrow slita scan of a region with the narrow slit– sit-and-stare with narrow slit or wide slitsit-and-stare with narrow slit or wide slit
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