This page (revision-28) was last changed on 18-Apr-2021 19:17 by PeterYoung

This page was created on 16-Nov-2009 21:50 by PeterYoung

Only authorized users are allowed to rename pages.

Only authorized users are allowed to delete pages.

Page revision history

Version Date Modified Size Author Changes ... Change note
28 18-Apr-2021 19:17 9 KB PeterYoung to previous
27 08-Jul-2010 16:40 9 KB PeterYoung to previous | to last
26 08-Jul-2010 16:17 10 KB PeterYoung to previous | to last
25 08-Jul-2010 15:36 10 KB PeterYoung to previous | to last
24 08-Jul-2010 01:47 10 KB PeterYoung to previous | to last
23 09-Jun-2010 22:14 10 KB PeterYoung to previous | to last
22 09-Jun-2010 18:20 8 KB PeterYoung to previous | to last
21 07-Jun-2010 21:47 8 KB PeterYoung to previous | to last

Page References

Incoming links Outgoing links
NRLtest...nobody
NRLtest

Version management

Difference between version and

At line 1 changed 3 lines
[{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
At line 3 added one line
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/].
At line 6 removed 4 lines
!!!EIS data analysis guide
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/].
At line 20 changed one line
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.
At line 22 changed one line
[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.
At line 24 changed one line
[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.
At line 26 changed one line
[Hinode Data Centre, DARTS (Japan)|http://darts.isas.jaxa.jp/hinode]\\
[Virtual Solar Observatory|VSOArchive]
At line 28 changed one line
[Virtual Solar Observatory (US)|http://virtualsolar.org]
[EIS_CAT|EISCAT]
At line 30 removed 2 lines
[EIS_CAT (IDL tool)|EISCAT]
At line 40 removed one line
{{{
At line 42 removed one line
}}}
At line 44 changed one line
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].
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/eis_swnote_01.pdf].
At line 50 removed one line
{{{
At line 52 removed one line
}}}
At line 70 changed one line
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:
At line 72 changed 3 lines
{{{
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])
At line 76 changed one line
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.
At line 78 removed 5 lines
[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.
At line 85 changed one line
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.
At line 87 removed 5 lines
* 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)
At line 94 changed one line
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
At line 96 changed 2 lines
[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
At line 78 added one line
!Line width maps
At line 100 removed 2 lines
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,]).
At line 104 removed 15 lines
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.
At line 133 changed 4 lines
* [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
At line 98 added 16 lines
!EIS and IDL maps
The set of [IDL map software|http://beauty.nascom.nasa.gov/~zarro/idl/maps/maps.html] of D. Zarro is a popular means for handling solar image data. The situation is more complicated for EIS than imaging instruments as an image can be an intensity, velocity or line width map. EIS maps are generated from EIS data objects as follows (in the case of a velocity map from Fe XII 195.12):
IDL> obj=obj_new('eis_data', filename)\\
IDL> m=obj_new('eis_moment',obj,iwin=195.12)\\
IDL> mmap=m->mk_eis_map(195.12,/vel)
The output mmap is in the standard format accepted by the map software.
To generate an intensity map use keyword /int and for a line width map use /wid. When the 'eis_moment' object is created (step 2) a widget will pop up allowing you to define the spectral region containing the emission line. Moments are used to generate the velocity and line widths which ensures quick results. You can use Gaussian fitting by giving the additional keyword fit='gauss' in step 2 for the eis_moment call.
!Cross-correlation with SOT and XRT
!Cross-correlation with EIT and TRACE
This page (revision-28) was last changed on 18-Apr-2021 19:17 by PeterYoungTop