data:data_analysis_manual
Differences
This shows you the differences between two versions of the page.
| Both sides previous revision Previous revision Next revision | Previous revision | ||
|
data:data_analysis_manual [2024/11/11 20:28] Peter Young [Line fitting] |
data:data_analysis_manual [2026/08/24 16:48] (current) Peter Young [Find data] added event list links |
||
|---|---|---|---|
| Line 22: | Line 22: | ||
| The data levels, FITS files, and headers are described in | The data levels, FITS files, and headers are described in | ||
| - | * The [[https://spice-wiki.ias.u-psud.fr/lib/exe/fetch.php/public:spice-uio-dpdd-0002-2.1-data_product_description_document_spicefits_.pdf|Data Products Description Document]] (DPDD) | + | * The {{ :public:spice-uio-dpdd-0002-2.2-data_product_description_document_spicefits_all_accepted.pdf |Data Product Description Document (DPDD) version 2.2}} |
| * The LLDPDD for the Low-Latency (LL) files | * The LLDPDD for the Low-Latency (LL) files | ||
| Line 88: | Line 88: | ||
| * Accessible through IDL/SSW and Python/Fido | * Accessible through IDL/SSW and Python/Fido | ||
| * FIXME As of 2024-03-29, the SPICE files on VSO are old files from release 3.0 only | * FIXME As of 2024-03-29, the SPICE files on VSO are old files from release 3.0 only | ||
| + | |||
| + | Event lists: | ||
| + | * [[public:eventlists:flares|Flares]] | ||
| + | * [[public:eventlists:prominences|Prominences]] | ||
| ===== Tips and Advice on Analyzing SPICE Data ===== | ===== Tips and Advice on Analyzing SPICE Data ===== | ||
| Line 236: | Line 240: | ||
| Links: | Links: | ||
| + | * Python quicklook tool: [[https://pypi.org/project/spiceitup/|SPICE-IT-UP]]. | ||
| * Example with [[:data:data_analysis_manual:sunraster|with sunraster]]. | * Example with [[:data:data_analysis_manual:sunraster|with sunraster]]. | ||
| * Tutorial about [[https://git.ias.u-psud.fr/spice/data-analysis-club/-/blob/main/20230516-coordinates/coordinates.ipynb|plotting and coordinates transforms]] | * Tutorial about [[https://git.ias.u-psud.fr/spice/data-analysis-club/-/blob/main/20230516-coordinates/coordinates.ipynb|plotting and coordinates transforms]] | ||
| Line 263: | Line 268: | ||
| ==== Line fitting ==== | ==== Line fitting ==== | ||
| + | For IDL Gaussian fitting software, please check: **[[data:line_fitting_idl|IDL software for emission line fitting]]**. | ||
| - | === Fitting a Gaussian at each spatial pixel in a raster (IDL) === | + | Fitting in Python can be done with any fitting library, including [[https://docs.astropy.org/en/stable/modeling/|astropy.modelling]]. From astropy 7.0, there is a user-friendly way of doing the fitting in parallel ([[https://github.com/aperiosoftware/parallel-modeling-examples/blob/main/spice/Final_Tutorial.ipynb|tutorial]] by Stuart Mumford). |
| - | + | ||
| - | Spectra at each spatial pixel in a raster can be fit with Gaussians using the eis\_auto\_fit IDL routine developed for the Hinode/EIS mission (you must have the EIS branch in your Solarsoft distribution). The key step is to format a SPICE wavelength window into a "windata" structure using the routine spice\_getwindata. An example call is: | + | |
| - | + | ||
| - | '' | + | |
| - | IDL> wd=spice\_getwindata(file) ; choose a wavelength window \\ | + | |
| - | IDL> eis\_fit\_template,wd,template ; create a template for the fit\\ | + | |
| - | IDL> eis\_auto\_fit,wd,fit,template=template\\ | + | |
| - | IDL> eis\_fit\_viewer,wd,fit | + | |
| - | '' | + | |
| - | + | ||
| - | The routine eis\_fit\_viewer is a GUI-based routine for browsing the fit results. More details on the eis\_auto\_fit suite of routines are available in [[https://doi.org/10.5281/zenodo.6339584 | + | |
| - | |EIS Software Note 15]]. | + | |
| - | + | ||
| - | + | ||
| - | The EIS software enable a number of operations to be performed on windata structures, as described in [[https://sohoftp.nascom.nasa.gov/solarsoft/hinode/eis/doc/eis_notes/21_WINDATA/eis_swnote_21.pdf|EIS Software Note 21]]. For example, eis\_bin\_windata allows spatial binning of the rasters. | + | |
| - | + | ||
| - | If you have problems running the EIS software on SPICE data, please contact [[https://science.gsfc.nasa.gov/sed/bio/peter.r.young|Dr. Peter Young]]. | + | |
| - | + | ||
| - | === Fitting a Gaussian to a spatially-averaged spectrum (IDL) === | + | |
| - | + | ||
| - | In this scenario, a spatial region is selected in the raster, perhaps a bright point or a loop, and the spectra are averaged over this region to produce a single, 1D spectrum. Gaussians are then fit to this spectrum. The procedure is as follows: | + | |
| - | + | ||
| - | '' | + | |
| - | IDL> map=spice\_make\_image(file,770.4) ; for Ne VIII 770.4\\ | + | |
| - | IDL> mask=pixel\_mask\_gui(map) ; GUI routine for selecting pixel mask\\ | + | |
| - | IDL> spec=spice\_mask\_spectrum(file,mask) ; create averaged spectrum\\ | + | |
| - | IDL> spec\_gauss\_spice, spec ; GUI routine for fitting Gaussians | + | |
| - | '' | + | |
| - | + | ||
| - | These routines are modified from routines originally written for Hinode/EIS. Further details can be found in [[https://doi.org/10.5281/zenodo.6339584 | + | |
| - | |EIS Software Note 15]]. | + | |
| + | This is used by the [[https://pypi.org/project/pycfit/|PyCFIT]] library, which provides a GUI for fitting the different components. | ||
| === Line window width and spectral tilt === | === Line window width and spectral tilt === | ||
data/data_analysis_manual.1731353283.txt.gz · Last modified: 2024/11/11 20:28 by Peter Young
Page Tools
Except where otherwise noted, content on this wiki is licensed under the following license: CC Attribution-Share Alike 4.0 International
