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[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
%%(color:red;)__This page is still under construction. All of the information should be accurate, but some of the links are broken.__%%
!!!A guide to accessing and analyzing EIS data
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This guide describes how to access, calibrate and derive scientific results from the EIS instrument on Hinode. For a description of EIS and its observing modes please consult the instrument paper, [Culhane et al. (2007)|http://adsabs.harvard.edu/abs/2007SoPh..243...19C], and the [MSSL Science Centre webpage|http://msslxr.mssl.ucl.ac.uk:8080/SolarB/].
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!!!EIS data analysis guide
!!Tutorial
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This guide describes how to access, calibrate and derive scientific results from the EIS instrument on Hinode. For a description of EIS and its observing modes please consult the instrument paper, [Culhane et al. (2007)|http://adsabs.harvard.edu/abs/2007SoPh..243...19C], and the [MSSL Science Centre webpage|https://vsolar.mssl.ucl.ac.uk/SolarB/].
!!Tutorials
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Each country contributing to the Hinode mission provides access to the data through web portals. Each one offers different capabilities and so it is recommended that you try each to familiarize yourself with the methods for searching for data. The four data access points are given below and we also list an IDL-based tool for accessing data.
There are several methods for searching and downloading EIS data and these are summarized below. Follow the links to find more details.
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[Hinode Science Data Centre (Europe)|http://elnath.uio.no/search/API] \\
[Hinode Science Data Centre Europe|SDCEurope] \\
Contains all of the Hinode data and has very flexible search tools.
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[MSSL Science Centre (UK)|https://vsolar.mssl.ucl.ac.uk/SolarB/]\\
[MSSL Science Centre|MSSLArchive]\\
EIS/XRT/SOT data all available. View thumbnails/movies for EIS data set; uses SQL for flexible searches.
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[Hinode Data Centre, DARTS (Japan)|http://darts.isas.jaxa.jp/hinode]\\
[Virtual Solar Observatory|VSOArchive]
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[Virtual Solar Observatory (US)|http://virtualsolar.org]
[EIS_CAT|EISCAT]
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[EIS_CAT (IDL tool)|EISCAT]
The large quantity of EIS data coupled with the large number of free parameters (raster size, wavelength windows, slit choice) means that it can be quite difficult to find the perfect data-set if you don't already know which study you want. Check out [Tips for finding the perfect data-set|TipsPerfect] to get some hints on searching for data.
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The standard call for eis_prep is:
[eis_prep options|Eis_prep_call]
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{{{
IDL> eis_prep, filename, /quiet, /retain, /default, /save
}}}
[Detailed description of eis_prep processing steps|Eis_prep]
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an explanation of these keywords and a description of the calibration steps performed by eis_prep are available in [EIS Software Note No. 1|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/01_EIS_PREP/eis_swnote_01.pdf].
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{{{
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}}}
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[Control|QuicklookControl] - find basic info on your data, run eis_prep, access QL tools.
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A complete data-set is read into IDL as an object as follows:
After you have calibrated your data with eis_prep and had a quick-look at the contents you will be ready to do more detailed analysis from the IDL command line. There are two options:
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{{{
IDL> data=obj_new('eis_data',filename)
}}}
# Read all EIS data into an IDL object
# Read an individual wavelength window into an IDL structure ([EIS_GETWINDATA|EISGetWindata])
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where 'filename' is the name of the level-1 file (a level-0 file can be read in the same way). The contents of the object can be read and manipulated through a large number of methods and an overview of some of the most useful methods is given below.
Many of the EIS analysis routines make use of the EIS_GETWINDATA structures, and so this is generally recommended.
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[EIS object methods|EISmethods]
The routine [EIS_GETWINDATA|EISGetWindata] is also available if you want to extract a single EIS data window into an IDL structure. Some routines (e.g., EIS_AUTO_FIT) require as input the structures produced by EIS_GETWINDATA.
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The 1" and 2" slits return emission line spectra and a basic task for such data-sets is to fit Gaussians to the emission lines to return intensity, centroid and width information. Gaussian fitting routines available to EIS users are described below. The routines correct for most instrumental effects, but users should familiarize themselves with some of these effects through the software notes listed below:
The 1" and 2" slits return emission line spectra and a basic task for such data-sets is to fit Gaussians to the emission lines to return intensity, centroid and width information. Gaussian fitting routines available to EIS users are described below. Interpretation of centroids and widths is hampered by certain instrumental effects and these are dealt with in the sections below.
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* Warm and hot pixels (Software Notes 6 and 13)
* Orbital drift of line centroids (Software Note 5)
* EIS slit tilts (Software Note 4)
* EIS grating tilt (Software Note 3)
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Fitting a Gaussian function to an emission line yields measures of the line intensity, centroid (velocity) and width. Single Gaussian fits to individual lines are possible using [EIS object methods|EISmethods], while more sophisticated fitting options are available through the EIS_AUTO_FIT and SPEC_GAUSS_EIS routines available in Solarsoft. Documents describing these routines and giving examples are listed below.
!Intensity maps
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[Gaussian fitting for the Hinode/EIS mission|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/fitting/eis_auto_fit.pdf]\\
[Gaussian fitting examples using eis_auto_fit|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/fitting/eis_auto_fit_examples.pdf]
!Velocity maps
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!Line width maps
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Users should be aware that EIS line profiles can often take on non-Gaussian shapes which may contain valuable scientific information (e.g., [Chifor et al. 2008|http://adsabs.harvard.edu/abs/2008A%26A...481L..57C,], [De Pontieu et al. 2009|http://adsabs.harvard.edu/abs/2009ApJ...701L...1D,]).
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Some emission line ratios are sensitive to the electron density, and software is available to take the line fit structures output by EIS_AUTO_FIT and convert them to electron density maps. The density then allows the emitting column depth of the plasma to be determined which in turn allows the filling factor of the plasma to be estimated. The document below describes how this done, making use of atomic data from the [CHIANTI database|http://www.chiantidatabase.org].
Deriving densities from Hinode/EIS data
!Emission measure
When line intensities are available from several different ions, then an emission measure (EM) or differential emission measure (DEM) distribution can be constructed. No specific EIS software is available for doing this and so users are referred to software in the CHIANTI database, in particular:
integral_calc.pro: computes an EM value from a single line intensity\\
chianti_dem.pro: computes a DEM distribution from multiple line intensities
Another popular DEM code is available within the [PINTofALE|http://hea-www.harvard.edu/PINTofALE/] software package.
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Most EIS users will be analyzing data-sets from multiple instruments and so it is necessary to determine where an EIS raster is positioned relative to the other instruments. Usually the pointing information within an EIS file will not be good enough to accurately co-align data-sets and so cross-correlation will be necessary.
Most EIS users will be analyzing data-sets from multiple instruments and so it is necessary where an EIS raster is positioned relative to the other instruments. Usually the pointing information within an EIS file will not be good enough to accurately co-align data-sets and so cross-correlation will be necessary.
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* [Obtaining pointing information from EIS data|EISPointing]
* [Creating an IDL map from EIS data|EISMaps]
* [Cross-correlating EIS and SOT images|EISSOTcoalign]
* [Cross-correlating EIS and XRT images|EISXRTcoaling]
!How to get the most accurate EIS coordinates
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!!EIS Software Notes
!EIS and IDL maps
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A series of Software Notes have been written that give details about various technical aspects related to the EIS mission.
!Cross-correlation with SOT and XRT
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[Software Note No. 1|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/01_EIS_PREP/eis_swnote_01.pdf] - eis_prep\\
[Software Note No. 2|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/02_RADIOMETRIC_CALIBRATION/eis_swnote_02.pdf] - Radiometric calibration\\
Software Note No. 3 - Grating/Detector tilt\\
[Software Note No. 4|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/04_SLIT_TILT/eis_swnote_04.pdf] - Slit tilts\\
Software Note No. 5 - Orbital variation of EIS wavelength scale\\
[Software Note No. 6|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/06_HOT_WARM_PIXELS/eis_swnote_06.pdf] - Hot and Warm pixels\\
Software Note No. 7 - Variation of line width with slit position\\
Software Note No. 8 - EIS Point Spread function (coma)\\
[Software Note No. 9|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/09_POINTING/eis_swnote_09.pdf] - EIS Pointing\\
[Software Note No. 10|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/10_DARK_CURRENT/eis_swnote_10.pdf] - Dark Current\\
[Software Note No. 11|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/11_JPEG_COMPRESSION/eis_swnote_11.pdf] - JPEG Compression\\
[Software Note No. 12|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/12_STRAY_LIGHT/eis_swnote_12.pdf] - Stray Light \\
[Software Note No. 13|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/13_INTERPOLATION/eis_swnote_13.pdf] - Interpolation of missing EIS data\\
[Software Note No. 14|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/eis_notes/14_BP_TRIGGER/eis_swnote_14.pdf] - The EIS Bright Point Trigger\\
!Cross-correlation with EIT and TRACE
This page (revision-28) was last changed on 18-Apr-2021 19:17 by PeterYoungTop