TRACE Analysis Guide
Transition Region and Coronal Explorer
Editor: R.D. Bentley
This Copy Produced: Jan 27, 2001
Version 0.99, 5-Dec-1998
Version 1.09, 24-Feb-1999
Version 1.20, 1-Jul-1999
Version 1.23 - Date Below
This Copy Produced: Jan 27, 2001
Mullard Space Science Laboratory
University College London
A Useful TRACE Software
B TRACE Instrument Items
B.1 Amount of Instrument Data per day
B.2 Missing and Lost Data
B.3 Searching for TRACE Data
B.4 The Eclipse Season
C Installing SolarSoft
D ANA and the ANA Browser
E Web and Others Versions of the TAG
This is the TRACE Analysis Guide (TAG). The Guide is in two main parts, the TRACE Users Guide (Section 2) and the TRACE Instrument Guide (Section 3). The User Guide describes how to analyse TRACE data and the Instrument Guide discusses aspect of the TRACE instrument. Additional information is provided in the Appendices.
TRACE is a NASA Small Explorer (SMEX) mission designed to investigate the connections between fine-scale magnetic fields and the associated plasma structures on the Sun. The instrument collects images of solar plasmas from 104 to 107 K, with one arc second resolution and excellent temporal resolution and continuity.
The TRACE spacecraft was launched on April 2, 1998 (UT) into a Sun-synchronous (98°) orbit of 600×650 km. The baseline mission duration was 1 year. Its orbit allowed continuous observations of the Sun to be made for 7 months before entering an eclipse season of 3 months. Each subsequent year of operation will have a 9 month (mid February to mid November) non-eclipse season. TRACE is operated in coordination with SoHO from an Experimental Operational Facility (EOF) at GSFC, close to the SoHO EOF.
The 30 cm aperture TRACE telescope uses four normal-incidence (NI) coatings in quadrants on its primary and secondary mirrors. Observations are made at several UV and EUV wavelengths, selected using a sector wheel and two filter wheels. A Lumogen-coated 1024×1024 CCD collects images over a 8.5×8.5 arcminute field of view. The images are coaligned and internally stabilized against spacecraft jitter. See the Instrument Guide (Section 3) for more information about the instrument.
The TRACE instrument produces a lot of data - it has been averaging just over 3 GBytes per week. The TRACE instrument data are blocked into hour-long FITS files which have names of the form `` triyyyymmdd.hh00'', where ``tri'' is the prefix for the reformatted files, and ``yyyymmdd.hh'' is the start time of the file. The files contain in-line JPEG compressed images, as downlinked from the spacecraft. They need to be decompressed before the data can be used - this is done automatically by the analysis routine read_trace using the shared object binary trace_decode_idl.so.
The data files are normally stored under directories that hold a weeks worth of files and have names that correspond to the date of the starting day of the week, i.e. ``weekyyyymmdd'' where ``yyyymmdd'' is the week start date. The directories are addressed in the analysis software through the environment variable $TRACE_I1_DIR.
If data are requested from the TRACE DATA CENTER, the Multiple eXtension FITS (.mxf) files that are returned cover a specific time interval, and contain images that are already decompressed. The name of this file has the form `` trbyyymmmdd_hhmm.mxf'', where ``trb'' is the prefix of the file, and ``yyyymmdd_hhmm'' is its start date and time. As with the hourly tri files, the .mxf files can be read using read_trace.
Detailed TRACE analysis need certain ancillary data files, including the dark current files (tdc files). What observations have been made by TRACE can be determined from the catalog files (tcl, tcs and tce). The location of the spacecraft, etc. can be found from the ephemeris files (fdss_*). These files are all held under directories addressed through the environment variable $tdb and are normally distributed within the SolarSoft database tree ($SSWDB or /sdb) - see Appendix C for more information.
The TRACE DATA CENTER allows the user to request data based on entries in the TRACE Data Catalog. There are other ways of searching for particular TRACE data - these are detailed in Appendix B.3, and include:
TRACE Investigation and Technical Plan (Phase III & IV), August 1994, LMSC P017270P-1.
``The Transition Region and Coronal Explorer (TRACE)'', 1994, Tarbell et al., Estes Park proceedings.
``The Transition Region and Coronal Explorer'', 1999, Handy et al., Sol. Phys., 187, 229.
``Data Analysis with the SolarSoft System'', 1998, Freeland and Handy, Sol. Phys., 182, 497.
Alan Title (LMSAL) firstname.lastname@example.org Jake Wolfson (LMSAL) email@example.com Ted Tarbell (LMSAL) firstname.lastname@example.org Karel Schrijver (LMSAL) email@example.com Dick Shine (LMSAL) firstname.lastname@example.org Sam Freeland (LMSAL) email@example.com Rich Nightingale (LMSAL) firstname.lastname@example.org Leon Golub (SAO) email@example.com Ed DeLuca (SAO) firstname.lastname@example.org Brian Handy (MSU) email@example.com Charles Kankelborg (MSU) firstname.lastname@example.org
This chapter describes the software used to analyze TRACE data. Except for section 2.9, all the descriptions relate to IDL software.
All TRACE software is distributed as part of the SolarSoft (SSW) software tree which is mastered at NASA-GSFC. To analyse TRACE data, the gen/, trace/ and packages/binaries/ branches of the tree need to be installed; to use the ANA Browser, the packages/ana/ branch must also be installed. To use the TRACE catalog, and to apply some of the corrections in trace_prep, the TRACE branch of the SolarSoft DataBase (SSWDB) must also be installed. More details about installing SolarSoft are given in Appendix C.
Within SolarSoft, at the Unix shell level configure your software
environment for TRACE, or TRACE and other instruments by entering:
> setssw trace
> setssw trace sxt mdi
IDL is then started with the command
The User's Guide gives an outline of how to use the software to analyse TRACE data. For help on how to get additional information on the TRACE software, see Section 2.10. One-line description of useful routines are given in Appendix A.
The TRACE catalogs hold details of the times, wavelengths, pointing, etc. of all observations made by the TRACE instrument. Since the TRACE instrument data files are large and it is therefore difficult for many sites to hold a large number of them on-line, the catalog makes an excellent entry point into the TRACE data. There are several catalogs, all are held under $tdb: tcl files form the normal catalog; the tcs files are a short-form of the catalog; and tce are an engineering log. The catalog may be read and listed using the routines trace_cat and trace_list_index, thus:
IDL> trace_cat, start_time, end_time, catalog [,/short]
IDL> more, trace_list_index(catalog)
The catalog structure can be used to read in the index and data arrays (see the examples in Section 2.2.2) and plot lightcurves of the average intensity (see Section 2.3.4).
There is an archive of full-disk images taken by TRACE which is formed from mosaics of many spacecraft pointings (available if $tdb is installed). This can also provide an insight into what TRACE was observing. The image for a selected date (or the nearest image to that date) may be viewed with view_trace_mosaic:
The names of any reformatted TRACE files that are on-line at the installation you are using (between a start and end time) may be determined with the function trace_files:
IDL> more, trace_files(start_time, end_time)
Information relating the TRACE ephemeris can be read with rd_fdss, and listed using pr_fdss. The fdss files used by these routines are held under $tdb:
IDL> fdss_struct = rd_fdss(start_time, end_time, type)
IDL> pr_fdss, fdss_tsruct
IDL> pr_fdss, start_time, end_time, type
where the text string type can have the values: `durevt' (day, radiation belts (SAA and HLZ's), etc.), `grndtrk' (spacecraft ground track), `orbevt' (orbit nodes), `viewpd' (station-pass view of the spacecraft), and 'station' (station-pass id).
During each orbit, passages through the radiation belts produce EUV images with a large number of spikes in the data due to energetic particles. Also, each year TRACE is in its eclipse season for a few weeks around the winter solstice between November and February. The status of the spacecraft in relation to these items can be confirmed using the routine pr_fdss:
IDL> pr_fdss, start_time, end_time, 'durevt'
Any TRACE file (including .mxf files) may be read with the routine read_trace. If the file contains JPEG compressed data, the packages/binaries/ branch must be included in your SolarSoft installation (this contains the shared object binary trace_decode_idl.so).
Calling read_trace with only one output parameter will just do a fast read of the headers and map them into an IDL structure vector with the same TAGs/field names. The equivalence of the ``FITS FIELDS'' and IDL structure tags permits vectorized searching on instrument parameters without any string parsing normally associated with FITS files. The same logic applies to SXT, EIT, MDI, etc. when accessed via SolarSoft.
The following commands read the index records (and optionally the data) in the specified files - the ss parameter specifies which images are required; -1 means all images. Again, the trace_list_index can be used to list the index structure:
IDL> more, trace_list_index(index)
The routine trace_prep can also read images with a similar calling sequence.
If you have already extracted a catalog structure using trace_cat, this may be used to read in the index and data arrays using trace_cat2data with the following calls.
IDL> trace_cat2data,catalog,index [,data]
The TRACE images are large and there are a lot of them, so it is better to select a subset before attempting to read them in. The function trace_sswhere provides a filter to do this, allowing the user to select images through a widget interface. Thus:
IDL> read_trace,files,-1,index ; get all the index structures
IDL> ss = trace_sswhere(index) ; select wavalength, etc. of choice
IDL> read_trace,files,ss,index,data ; read in the desired data
For a given index or catalogue structure, the function trace_sswhere allows the following to be selected by the user:
trace_sswhere can be used to select a subset of images from a catalog structure before the data is read in:
IDL> trace_cat, start_time, end_time, catalog
IDL> ss = trace_sswhere(catalog)
It may also be desirable to only read part of the the image since individual images can be quite large, and an array can take a lot of memory. The routine read_trace_fov allows the user to select a sub-frame within the first selected image before reading the data:
IDL> trace_cat, start_time, end_time, catalog
IDL> ss = trace_sswhere(catalog)
read_trace_fov can also be called with just the files and ss arrays:
Filtering can also be done at the IDL command level. For example, this three line segment reads NN file headers (subset of -1 implies all images), applies a filter for full resolution 171 Å images and then reads that data cube.
IDL> read_trace,files,-1,index ; read all HEADERS->structs
IDL> ss=where(index.wave_len eq '171' and index.naxis1 eq 1024) ;some FILTER
IDL> read_trace,files,ss,index,data ; read subset DATA (3D)
The routine struct_where is a more generalized filter that works on
index or catalog structures. The selection is made according to filters
supplied in a configuration file or string array. This method is
particularly useful when the same set of filters are always employed to
process data, e.g. when making a movie.
IDL> ss = struct_where(index, count, conf_file=conf_file)
IDL> ss = struct_where(index, count, test_array=test_array)
Where the contents of conf_file or test_array are of the form:
<TAG> <OPERARTOR> <VALUE>For example, a configuration file might contain:
; you can include free-form comments using ';' delimiter NAXIS1 = 512,1024 ; Lists (comma delimited) IMG_MIN > 1. ; Single value (boolean) WAVE_LEN = 171,195,284 ; XCEN=600.~800. ; Range (tilde separated) IMG_AVG > 100 && IMG_MAX < 4096 ; Compound BooleanOr, the following test_array filter would select all TRACE images in 171 Å of 1024×1024 pixels:
IDL> filter = ['wave_len = 171','naxis1 = 1024'] IDL> ss = struct_where(index,count,test_array=filter)
If you need to select a series of images at a pre-defined cadence from an
index or catalog structure, then use grid_data. To select images at
a particular time, use tim2dset. For example:
IDL> ss = grid_data(index, min=5)
IDL> trace_cat,'31-may-98 12:00','31-may-98 14:00',cat
IDL> ss = tim2dset(cat,'31-may-98 13:08')
If you have a list of favourite images generated by the ANA Browser (section 2.9), this can be read into IDL using read_analist. The index and data arrays can then be read with read_trace.
The routine trace2x will also read a list produced by the ANA Browser (section 2.9) and return a scaled (windowed) array - see the file header for more information.
Image files created by ANA can be read into IDL using anafrd:
IDL> img = anafrd(ana_image_filename,head)
For qualitative work, there are a number of routines to try. Here we assume that the index and data arrays have already been read in, e.g. using read_trace. Since the TRACE index structure contains the SolarSoft standards for time and pointing references, you can use a lot of standard software including utplot, the mapping software, etc..
For single (2D) images, try the following:
IDL> sdata=trace_scale(index,data,/despike,/byte) ; "standard" scaling
IDL> wdef,im=sdata ; make a window the right size
IDL> trace_colors,index ; Load standard wave color table
Here the function trace_scale is used to scale the TRACE image to the desired range, and trace_colors loads the standard TRACE color table. If the image is large, it may also be viewed with slide_image (the optional keyword inputs change the image display size):
IDL> slide_image,sdata [,xvis=400,yvis=400]
When whole (1024×1024 pixel) TRACE images are viewed, the effects of vignetting are evident - the cause of this is decribed in Section 3.2.3.
TRACE image cubes may be viewed with the generic viewer xstepper. This needs a data array, and optionally an information array. The generic IDL (structure to text array) translator get_infox is one way of producing the required info array. Sample calls may thus be:
IDL> xstepper, sdata, info
IDL> xstepper, sdata, get_infox(index,'naxis1,wave_len,',/fmt_tim)
The xstepper procedure can also be used to blink between two images. Just load the image pair when starting xstepper and adjust the frame rate as desired.
TRACE movies can also be made by other routines, including trace_uniq_movies and image2movie. To see examples of the Web of movies created with the software mentioned here, look at < http://vestige.lmsal.com/TRACE/last_movies/ > .
Lightcurves of a selected area of an image cube may be made using lcur_image:
IDL> lcur_image,index,data [,lcur]
To mark an arc on an image (e.g. to pick out a loop) and plot the intensity along the strip use plot_arc. The lightcurve of the arc may optionally be returned:
IDL> plot_arc, index, image, width [, xlcur=xlcur, lcur=lcur]
Time series of parameters may be plotted with utplot.
IDL> utplot,index,index.XXX ; time series of some SSW parameter
IDL> outplot,index,index.YYY ; overplot
IDL> evt_grid,index,ticklen=.1 ; overlay 'events' on existing utplot
The normalized lightcurve of the average counts in an image may be plotted using plot_trace:
In this example, the average counts of the 1600 Å band from TRACE index (or catalog) structure is plotted (selecting the 256×256 pixel images). Counts in the .img_avg tag are used because the .img_max values are affected by particle-induced spikes in the data. The countrates are normalized for exposure time, after the CCD readout pedestal (section 3.2.2) has been subtracted. Note: The times listed in the index (and catalog) structures are the time the shutter closes (section 3.2.5). The times plotted by plot_trace are the mean time, i.e. the end time minus half the exposure time. By default, bad data is filtered from the plot.
The routine trace_prep is intended to guide the processing of TRACE data from raw to level 0 according to the order and algorithms defined by the TRACE PI Team. For those familiar with SolarSoft, it is similar in philosophy and interface to sxt_prep and eit_prep. A number of TRACE database files need to be installed under $tdb to run trace_prep - these include the dark current frame files (tdc) - see Appendix C for more information.
The trace_prep routine will work with both 2D and 3D data arrays. Assuming that the index and data records have already been read in, the call to trace_prep is:
Examine the procedure header for the current status of trace_prep, or e-mail Richard Nightingale at Lockheed (email@example.com). As of November 1999, trace_prep performs the following steps:
Optionally, the following corrections are applied if the appropriate keywords are used:
In the future, it is hoped that trace_prep will also:
The TRACE images are large and numerous and it may be necessary to work with only part of each image. Since some of the corrections are best performed on complete TRACE images, the extraction should be done after the corrections have been applied. There are four keyword parameters within trace_prep that allow the user to extract part of an image after it has been processed. These are: sllex and slley (which specify the coordinates of the subimage lower left corner), and subimgx and subimgy (which specify the number of pixels in the x and y axes). If the data are extracted in this way, the pointing and image tags in the index record are updated; the use of the /new_avg keyword is also recommended. An example of a call including these paramaters, and the keywords to correct the images would be:
IDL> trace_prep,index,data,outindex,outdata, $
The trace_prep routine can also be used to read directly from the raw FITS file and write calibrated data to a new file. Examine the procedure header for more information. Such files can be read in using read_trace.
Below are examples of calls for routines that are used in correcting and calibrating TRACE data. Most can be called as options in trace_prep and as such do not need to be called separately. Note: the advantage of calling the routines within trace_prep is that history records are included in the index structure to flag that the correction has been applied - this reduces the chance of applying the same correction more than once.
Spikes caused by high energy particles in the images (see 3.2.2 and 3.2.7) can be removed by tracedespike or trace_unspike. The routines trace_unspike and trace_destreak (together with trace_cleanjpg) can be used to remove spikes and streaks, and repair some of the damage caused when the spikes are compressed by the JPEG algorithm. If you have a series of images, the routine trace_unspike_time will removing spike-like features that only occur in one frame.
The herring-bone patterning on the CCD pedestal (see 3.2.2) can be removed with trace_knoise.
IDL> imout = tracedespike(tracedespike(image)) ;twice for faint fields
IDL> imout = tracedespike(image,statistics=6) ;correct > 6sigma outliers
IDL> imout = tracedespike(image,minimum=100,ri=3) ;low-quartile correrctions
IDL> imout = trace_unspike(image, /cleanjpg [, sens=sens])
IDL> imout = trace_destreak(image [, sens=sens, thresh=thresh])
IDL> clean_data = trace_unspike_time(index,data [,threshold=threshold])
IDL> imout = trace_knoise(image)
The routine trace_wave2point is used to correct the index structure for differences in the alignment of the TRACE images in different channels (see 3.2.3).
IDL> newindex = trace_wave2point(index [,/noapply] [,version=xx] )
Processed TRACE data may be stored in files in a number of formats. Remember that the data will no longer be compressed and the files will be much bigger than the raw files if all the frames are included. Use write_trace to write such files. The default is a FITS file, but GIF, TIFF and JPEG are also possible:
TRACE is often rastered about the disk to generate a mosaic image of all or part of the sun: full-disk mosaics are a standard synoptic campaign when EIT is not running, and TRACE began making Lyman Alpha observations of the solar limb in collaboration with UVCS in early 1999. An alternative to using the mosaic database is to generate the mosaics by hand with trace_build_mosaic. It is not necessary to have all the images from the mosaic on hand to generate a partial solar mosaic.
IDL> file = trace_files('05:00:00 16-JUN-1999', '05:30:00 16-JUN-1999')
IDL> read_trace, file, -1, i, /nodata
IDL> subs = where(i.obs_prog eq 'STD.smallmosaic', count)
IDL> read_trace, file, subs, i, d
IDL> for j=0, count-1 do begin & d[*,*,j]=trace_unspike(d[*,*,j],/cleanjpg)
IDL> trace_prep, i, d, iout, dout
IDL> trace_build_mosaic, iout, dout, mosaic
It is possible to overlay TRACE images with images from other sources using IDL Map Objects (<http://orpheus.nascom.nasa.gov/ ~ zarro/idl/maps.html>) - this is a family of routines that was developed by Dominic Zarro (SAC/NASA-GSFC; firstname.lastname@example.org). From the index and data arrays the routines create Map Objects which can be spatially scaled, differentially rotated, overlayed, plotted with the limb or a latitude and longitude grid. Note the sequence read_trace > index2map > plot_map used in the example below to create and plot map objects - a similar sequence can be used for many other instruments supported by SolarSoft. For the best source of information on what options are currently available, see the header of the routine plot_map.
Assuming that the index and data arrays have been read in, a Map Object of TRACE data may be created and plotted using index2map and plot_map:
IDL> index2map, index, data, tracemap ; make a map from scaled data
IDL> plot_map, tracemap, fov=10, grid=5 ; plot it, centered in 10 arcmin
; FOV , overlay 5" solar grid
Note that image center defined in the index (or catalog) structure represents the center of the TRACE White Light channel - this is the same in the FITS file header. Since the centers of EUV and UV channels are offset with respect to the white light image (see the Instrument Guide, Section 3.2.6), a correction must be applied before the images can be co-aligned. The correction can be made using trace_wave2point - this can be optionally applied when using trace_prep.
A useful routine to use with Map Objects is ssw_track_fov. This extracts a sub-field from the SSW-compliant (2D) image data given the time and image coordinates from a reference Map Object; alternatively, a desired reference time and set of heliocentric coordinates can be supplied as keywords. The interactive selection of coordinates is also possible:
IDL> ssw_track_fov, index, data, outindex, outdata, ref_map=ref_map
IDL> ssw_track_fov, index, data, outindex, outdata, helio=[LAT, LON], $
IDL> ssw_track_fov, index, data, outindex, outdata, /interactive
The co-alignment of images from various sources can be improved by using
cross-correlation. There are a number of routine in the SSW tree to do
this, but one way is shown below using align_cube_correl:
IDL> mreadfits, files, index, data [, outsize=xxx] ; xxx= 256 or 512
IDL> [normalize data cube if possible - might try 'normalize_cube']
IDL> align_cube_correl, data, outdata [,reference=NN] ; CC alignment
Routines that use the TRACE data to determine plasma diagnostics are detailed below. See the Instrument Guide (Section 3.4) for more information on the techniques involved and the limitations of the data.
When TRACE is in or near its eclipse season, care should be taken when using data for diagnostic purposes because of the effects of atmospheric absorption - see Appendix B.4.
The response of the TRACE EUV channels with respect to temperature is given by trace_t_resp. To plot the response of a channel against temperature use:
IDL> temp=1.0e5+1.0e4*findgen(200) ; generate temperature vector
IDL> response=trace_t_resp('171ao',temp) ; calculate and plot response
The routine trace_dem characterizes the differential emission measure (DEM) along the line of sight by fitting a 3-parameter model. It uses linear techniques to solve what is normally considered an ill-posed inversion problem. The keyword paramater ``basis'' contains the name of the function that will supply the basic elements necssary of constructing the DEM curves - the default is trace_sbasis (see trace_dem_setup); trace_tbasis is another routine that can be used. The call for trace_dem is given below:
IDL> trace_dem, index, data, emc, Tavg [,basis=basis]
The routine trace_tmap produces maps of temperature and emission measure, given two or more TRACE EUV channels as input - it uses chi-squared minimization. The routine is computationally intensive and takes a lot of memory. Like trace_tmap, the routine trace_isothermal uses chi-squared minimization, but is less memory intensive. Neither method is particularly fast - trace_isothermal is extremely slow and its use is only recommended for small fields-of-view.
IDL> trace_tmap, index, data, tmap=tmap, em=em
IDL> trace_isothermal, index, data, tmap=tmap, em=em
The results of trace_tmap and trace_isothermal can be displayed using trace_disp_tem. This produces maps that visualize temperature and emission measure simultaneously by means of hue angle and lightness. The maps look best when viewed on a 24-bit display, although the output may also be written to the PostScript device. When using an 8-bit display, the /quantize keyword is required.
IDL> trace_disp_tem, tmap, em [,/legend] [,/quantize]
It is also possible to calculate the temperature and emission measure maps from a pair of of TRACE EUV images using the routine trace_teem. This is a filter-ratio method that is based on the assumption that a structure seen in the two wavelengths is i) isothermal, and ii) of a temperature that lies between the peak temperatures of the response functions of the two wavelength filters, T1 < T < T2; suitable pairs are 171 and 195 Å, and 195 and 284 Å. The trace_teem is faster than trace_isothermal because of its vectorization and because it only requires two wavelength images.
where index1 and data1 relate to the lower wavelength image, and index2
and data2 relate to the higher wavelength image. All data should be
prepared using trace_prep.
The routine civ_subtract can be used to generate a clean C IV image, given an input set of TRACE UV images at 1550 Å, 1600 Å and 1700 Å. Any pair of these channels will produce a result, but the quality is degraded if only two channels are used. The call for civ_subtract is:
IDL> civ_subtract, index, data, iout, dout
It is possible to browse TRACE data using ANA. The ANA utility was developed during the SMM era by Dick Shine and others. The Browser was written to assist the analysis of data from the SOUP instrument on Spacelab 2. A detailed description of the ANA Browser is given in the write-up by Dick Shine (email@example.com; Appendix D), but a few pointers are given here. At most stages, help can be obtained by hitting the ``Help'' button in a particular Browser window.
The ANA Browser is started at the Unix shell level by entering:
When writing a 3-D array, three separate arrays may be written to disk. The three files have default extensions of ``.cube'', ``.times'', and ``.notes'' - the filename is supplied by the user (the default is ``movie''). Timing information available from the TRACE hourly files (i.e. the time of each exposure) can be saved in the ``.times'' array; the ``.notes'' array is for optional extra comments. 3-D arrays may be written as either FITS or FZ files.
Arrays of 2-D images may be written in the same formats as single images. The filenames are created from a numbered list based on the file name template (using the ``#'' character) and range. For example, ``movie####.file'' with a range of 1-10 will write ten images with file names ``movie0001.file'' through ``movie0010.file''.
Note: There is a WYSIWYG file write option, but this works only for users running from Silicon Graphics machines.
An image cube created by ANA can be imported into IDL using the routines open_anacube, window_anacube, and close_anacube. After opening the cube with open_anacube, the desired sub-window of a reference image can be read using window_anacube; frames can be selected using an ss vector. Some selection before reading is recommended since the cubes are often quite large. More recently written cubes may have ``.times'' and ``.notes'' files associated with the ``.cube'' file - these contain timing and other information.
IDL> cube = window_anacube(ref_no,/read [,ss=ss])
Within IDL, the routines doc_library, doc_library2, xdoc, sswloc and chkarg can provide imformation on the software - sswloc also works at the Unix shell level. Thanks to Dominic Zarro, there is now a searchable WWW front end to routines in the the SolarSoft tree through a Hypertext version of the xdoc routine (<http://orpheus.nascom.nasa.gov/ ~ zarro/xdoc/>) - try searching on read_trace to check this out.
Within the ANA Browser, at most stages help can be obtained by hitting the ``Help'' button.
Appendix C gives information on installing SolarSoft.
The Instrument Guide is intended to give the user an outline of the TRACE instrument and spacecaft, and to convey some of the salient points relating to the instrument that may be of assistance when analysing the data. It is by no means the only source of this information. The TRACE instrument (Section 3.1) is described in considerably more detail in Handy et al. (1999). Aspects of the instrument properties and calibration (Sections 3.2 and 3.3) are described in a number of calibration notes (see the list in Section 3.5). The C IV diagnostic capabilites of TRACE (Section 3.4) are described in Handy et al. (1998).
The TRACE instrument consists of a 30 cm diameter Cassegrain telescope and a filter system feeding a CCD detector (see Figure 3.1). Each quadrant of the primary mirror is coated for sensitivity to a different wavelength range. Since the four coatings share a common substrate, images in all ranges are co-aligned well. The corresponding quadrants of the secondary mirror are coated in a similar manner. All four mirror quadrants have multilayer coatings, which serve to define the passbands at each wavelength. Entrance filters exclude all visible Light and most of the energy in the UV - this help reduces scattered light and the heat load inside the instrument. A pair of filter wheels contains filters to select particular UV spectral regions. The 1024×1024 pixel CCD camera was developed for the SoHO/MDI program. An image stabilization system drives an active secondary mirror to compensate for spacecraft pointing jitter to a level of 0.1¢¢. A data handling computer performs basic image manipulation and compression in order to reduce telemetry requirements.
Light entering the instrument passes first through the entrance filter assembly which transmits only far and extreme UV. Visible and near UV radiation (and hence most of the solar energy) are reflected back into space. Radiation transmitted through the entrance filters passes to a quadrant selector wheel that blocks three quadrants of the aperture so that only one quadrant of the telescope is illuminated at a time. Photons passing the wheel's open quadrant proceed to the primary mirror, encountering a multilayer coating for a narrow-band EUV quadrant or a broad-band coating for the UV quadrant.
The reflected beam from the primary mirror proceeds to the secondary mirror which reflects it towards the focal plane. The secondary mirror is active to correct for pointing jitter and has coatings matching those on the four quadrants of the primary mirror - it is also stepped to adjusted the focus of the different TRACE channels. The converging beam from the secondary mirror passes through the central hole in the primary mirror where it encounters two filter wheels in series.
Each four-position wheel has three filters and one open position (see Tables 3.1 and 3.2). The two wheels contain thin film aluminum filters for use with the EUV channels, and four UV filters. A thin aluminum (EUV) filter is located in each wheel for use in series if pinholes in both of them become a problem. This has not been necessary and the baseline/front filter has always been used thus far. The Lyman-a filter (1216 Å) is deposited on a magnesium fluoride substrate and the remaining UV filters are on quartz substrates. A narrow band UV filter for the C IV lines at 1548 and 1550 Å is deposited on crystalline quartz (as is a narrow band filter peaking at 1570 Å). The filter for the continuum at 1600 Å is made with the same deposition coating on a fused quartz substrate. This substrate sharply attenuates the C IV lines and makes it possible to subtract the longwave transmission of the 1550 Å narrow band filter. Normally one filter wheel is set at open; the other selects the spectral region. To observe in the 5000 Å band, one filter wheel is open and fused-silica is selected on the other.
Radiation passing the filter wheel assembly next encounters the focal plane shutter. The shutter mechanism consists of a disk mounted directly on the shaft of a brushless DC motor. Two apertures are provided in the disk, wide for exposures longer than 20 msec and narrow for exposures that are multiples of 1.6 ms. The final element in the optical train is the Lumogen-coated CCD camera. Its 21 micron pixels each subtend 0.5×0.5¢¢ at the focus of the telescope. Ray traces of the optical system show that optical aberrations are smaller than one pixel throughout the field of view, even with maximum secondary mirror tilt.
|Mirror Quadrant||FW 1 (FWD)||FW 2 (AFT)|
|A: 171 Å (EUV)||1: Open||1: Open|
|B: UV and WL||2: 1600 Å||2: 1216 Å|
|C: 195 Å (EUV)||3: Aluminum||3: Aluminum|
|D: 284 Å (EUV)||4: 1550 Å||4: Fused Silica|
|#||Quadrant||FW 1||FW 2||Name||Comments|
|0||A (171)||1 (open)||1 (open)||171oo|
|1||A (171)||1 (open)||3 (Al)||171oa|
|2||A (171)||3 (Al)||1 (open)||171ao||* Baseline|
|3||A (171)||3 (Al)||3 (Al)||171aa|
|4||C (195)||1 (open)||1 (open)||195oo|
|5||C (195)||1 (open)||3 (Al)||195oa|
|6||C (195)||3 (Al)||1 (open)||195ao||* Baseline|
|7||C (195)||3 (Al)||3 (Al)||195aa|
|8||D (284)||1 (open)||1 (open)||284oo|
|9||D (284)||1 (open)||3 (Al)||284oa|
|10||D (284)||3 (Al)||1 (open)||284ao||* Baseline|
|11||D (284)||3 (Al)||3 (Al)||284aa|
|12||B (UV)||1 (open)||1 (open)||UVoo||alternate white light|
|13||B (UV)||1 (open)||2 (1216)||1216||* Lyman alpha|
|14||B (UV)||1 (open)||3 (Al)||UVoa||pinholes|
|15||B (UV)||1 (open)||4 (FS)||WL||* White Light (FS = fused silica)|
|16||B (UV)||2 (1600)||1 (open)||1600||* Continuum + C IV + other lines|
|17||B (UV)||2 (1600)||2 (1216)||1216L||L for long wavelength leakage|
|18||B (UV)||2 (1600)||4 (FS)||1700||* Continuum + weak lines|
|19||B (UV)||3 (Al)||1 (open)||UVao||pinholes|
|20||B (UV)||3 (Al)||3 (Al)||UVaa||pinholes|
|21||B (UV)||4 (1550)||1 (open)||1550||* C IV + other lines + continuum|
|22||B (UV)||4 (1550)||4 (FS)||1550L||L for long wavelength leakage|
TRACE is a 3-axis stabilized, Sun-pointing spacecraft. It is in a Sun-sychnronous (98°) orbit of 600×650 km.
The TRACE attitude control system (ACS) includes three reaction wheels, three electromagnetic torquers, a 3-axis magnetometer, a gyro system, coarse sun sensors, and a fine sun sensor. High sensitivity pitch and yaw error signals are provided to the ACS by the TRACE Guide Telescope. The ACS uses these signals to limit pointing jitter to < 20¢¢; the Image Stabilization System (ISS) removes residual jitter using higher frequency signals from the guide telescope.
Within the guide telescope, a pair of independently rotatable wedge prisms mounted between the entrance filter and the objective lens allows the optic axis of the telescope to be deflected in any direction within a cone of 1 degree half-angle centered about the optic axis of the main telescope. The spacecraft is maneuvered by offsetting the optical axis of the guide telescope such that the main telescope points to the desired portion of the solar disk.
The ISS drives the active secondary mirror to compensate for spacecraft pointing jitter to a level of 0.1¢¢. It is an open-loop control system in the sense that the error signal is derived from the guide telescope rather than from motion of the image in the main telescope.
TRACE does not use a star tracker. The roll axis is defined using Earth's magnetic field; the gyro system provides error signals for roll stabilization. Steady slow drifts in roll ( ~ 0.7 degree/hr) can be accepted without degrading the science.
TRACE uses a flight spare CCD from the SoHO MDI instrument - it was designed by Loral for MDI. It is a 1024×1024, 3-phase, Multi-Phase Pinned (MPP), 21 micron pixel design which incorporates dual serial registers for redundancy; is front-illuminated, and is not thinned. The pixels each subtend 0.5×0.5¢¢ at the focus of the telescope.
The CCD is phosphor-coated to give it UV sensitivity. The material used was Lumogen, made by B&K, and deposited by Lorel. The sensitivity of the Lumogen-coated CCD is about 0.08 at the EUV wavelengths, 0.09 at 1216 Å, 0.15 at 1600Å, and ~ 0.40 in the visible. The system gain of the camera is ~ 12 electrons/Data Number (DN) when using the A amplifier (which is normally the case); the B amplifier system gain is ~ 45 electrons/DN. The response of the camera is very linear with exposure; weak pixels are also linear.
The 12-bit ADC tops-out at 4096 counts - count levels in excess of this return this value. This represents only 20% of the full-well capacity of a pixel, so unless the countrate is extremely high there is little spreading from (ADC) saturated pixels.
The CCD is designed to operate at temperatures below -55 °C. It is cooled by an aft-facing passive radiator system located at the rear of the spacecraft. The detector runs cold to reduce dark current, and mitigate radiation damage effects.
The peak data rate of TRACE is theoretically limited by the time taken to read the CCD, and practically limited by signal level considerations. The amount of time required to obtain a 1024×1024 image is determined by the CCD read rate of 500 Kpixels/s to be 2.2 seconds. N×N subarrays can be read out faster by a factor of almost 1024/N; there is usually some fixed ``overhead''. On-chip summing and/or binning of pixels in the image processor can be used to invoke compromises of spatial resolution, FOV, signal level and peak image rate. The 12-bit pixels are compressed in cells using a JPEG algorithm.
Flat field correction maps have been derived but show little departure from unity - for white light typical excursions across the field show ~ 1.5% peak-to-peak. To date, the flat field correction are not applied.
Calibration images of the CCD dark-current are taken roughly every two weeks. The dark current is essentially zero ( ~ 0.1 DN/sec), has changed little during the mission, and varies slightly with temperature. The routine trace_prep presently uses a fixed dark current for all exposures, but will soon use a temperature dependant value.
There is a readout pedestal on the CCD of almost 87 DN (in non-summing mode). This varies for different summing modes and when different parts of the CCD are readout (e.g. the middle 256×256), but is not dependent on exposure time. It increases in magnitude and becomes less uniform over the CCD with progressively higher summation modes (2×2, 4×4, 8×8). The pedestal decreases slightly as the temperature increases. The routine trace_prep presently removes a fixed pedestal but will soon use a temperature dependant value.
The CCD readout noise is typically less than 2-3 DN/sec. This is probably electronic in origin and includes a herring-bone pattern on the image. The pattern is modulated by vertical stripes that may be caused by the CCD maufacturing process. CCD readout noise is discussed further in the section on image quality.
The TRACE CCD experiences a lot of problems with orbital background (i.e. SAA and HLZ's). The effect is greater than was anticipated before launch for HLZ's and data are no longer taken in the (longer exposure) EUV channels when TRACE is in the radiation belts. The problem takes the form of spikes or tracks left in the CCD image. The effects of orbital background are discussed further in the section on image quality (see Section 3.2.7). The approximate timing of passages through the belts can be determined from the fdss files (see Section 2.1.2).
The pointing coordinates included in the TRACE index records are for the White-light channel. The EUV channels, and the UV Lyman-a (1216 Å) channel, are offset slightly from the white light and other UV channels - a set of measured offsets is given in Table 3.3. For alignment with data from other instruments, the index record needs to be adjusted - this is done by the routine trace_wave2point.
|(arcsec; WE)||(arcsec; NS)|
Because of slight differences in the optics, it is necessary to change the focus between exposures for the different TRACE channels - an adjustment of ±5 mm in the position of the secondary mirror is provided for this purpose. The focus of each channel has been determined since launch by imaging solar features with fine structure at several focus adjustment positions and determining the best focus by examining the sharpness of each image - e.g. solar prominences were used for the 1216 Å channel. Note, a new set of inter-channel offsets has been derived for the new set of focus positions adopted on September 24, 1998 - these are given in Table 3.3. The new focus adjustment positions brings the 1216 Å channel closer to the positions used for the other channels than was the case prior to then.
The pointing accuracy of TRACE is probably good to 5-10¢¢ - this may improve when a better wedge calibration is available. The pointing stability within a stream of images is very good - better than a few tenths of a pixel. Movements of the quad-shutter causes a ~ 4¢¢ disturbance that takes a few seconds to damp down, and can leave a residual change of 0.5¢¢ or less.
There is a small pointing wobble over the course of an orbit, of the order ±1¢¢. This correlates well with temperature and may be caused by a slight flexing between the guide telescope and the main TRACE telescope; it will be removed by the analysis software once it has been characterized. In movies, an apparent pointing drift can occur if the roll of the spaceraft is not properly aligned to Solar north-south - a 1° error in the roll axis would represent 17¢¢ at the limb. Since TRACE does not have a star tracker, data from the SOHO/MDI instrument are needed for an absolute roll calibration.
Although TRACE collects images over a 8.5×8.5 arcminutes field-of-view (FOV), the images are vignetted by the telescope optics. The vignetting is caused by the filter-wheel, is not symmetric about the center of the FOV, and is different for each channel because each uses a different mirror quadrant. For the UV passbands, since the same mirror quadrant and filter wheel position are used, the vignetting should be the same for all channels, although the different focus position for the 1216 Å channel has some effect.
TRACE often uses a simple Automatic Exposure Control (AEC) algorithm, very similar to its predecessor on Yohkoh/SXT. The algorithm adjusts the exposure index based on a 128-bin histogram of the previous CCD image, which is taken after the removal of bad pixels and the CCD readout pedestal. For most applications, the AEC is programmed to maximize dynamic range while avoiding saturation of the CCD. Simply stated, the approach is to choose the greatest exposure time that will not saturate pixels in the highest percentile of intensity. AEC behavior is controlled by several adjustable parameters which are stored in the AEC table - this contains entries for each wavelength and target class that define thresholds and amounts by which the exposure should be adjusted in case of over- or under-exposure.
Details of the TRACE Automatic Exposure Control algorithm, including a description of the parameters used to control it, can be found on the TRACE Web pages at MSU.
The image time downlinked in telemetry is the time that the shutter closes. The start of the exposure can be determined by subtracting the exposure time. There is an uncertainly of ~ 0.1 secs in the timing.
The plate-scale of the white-light TRACE images have been determined by J.-P. Wuelser to be:
The plate scale is thought to be effectively the same for all channels, if they are in focus. The resolution of TRACE is therefore very close to its planned 1¢¢.
TRACE uses a modified 12-bit JPEG algorithm for data compression. The algorithm has a nearly lossless mode that preserves 12-bit data with a maximum error of 1 count and a wide range of lossy options which are tailored to different image characteristics. The image is compressed in cells of 8×8 pixels - these can clearly be seen if a decompressed TRACE image is closely examined.
In itself, JPEG compression affects an image in a manner that is well understood, but for TRACE there are some additional effects described below:
The characteristics of the TRACE channels are given in Table 3.4, where the sensitivity is defined as:
Mirror Reflectivity × Filter Transmission × CCD Quantum Efficency
The wavelength response of the TRACE optical and UV channels is shown in Figure 3.2, and of the EUV channels in Figure 3.3. The temperature response of the TRACE EUV quadrants are shown in Figure 3.4.
|5000||Continuum||broad||.00010||3.6 - 3.8|
|1700||Continium||200.0||.00006||3.6 - 4.0|
|1600||C I, Fe II + cont.||275.0||????||3.6 - 4.0|
|1550||C IV + cont.||20.0||.00068||4.8 - 5.4|
|1216||H Lya||84.0||.00055||4.0 - 4.5|
|171||Fe IX||6.4||0.017||5.2 - 6.3|
|195||Fe XII||6.5||0.011||5.7 - 6.3|
|284||Fe XV||10.7||0.0035||6.1 - 6.6|
Details of the manufacture of the TRACE mirrors and filters, and the sensitivity of the TRACE channels, and the calibration of the instrument are given on the TRACE Web pages at SAO and Lockheed-Martin.
On-orbit flat fields of the TRACE CCD and optics in WL and 1700 Å wavelengths have been generated using the the Kuhn-Lin flat-field algorithm. This algorithm uses a number of images at slightly shifted locations on the CCD, with the images out of focus to reduce contrast.
The WL flat field is quite flat and of good quality (in the sense that it corrects WL images to high accuracy). The flatness and quality has changed very little since launch, with a difference image of two flat fields taken 7 months apart showing ±1.0% peak-to-peak variations, the same range as the flat fields themselves.
Several features are evident in the WL flat field of Figure 3.5a. There are many small dark spots of ~ 1-3 pixels across with intensities of 20-80% of the normalized field. These were present on the CCD prior to launch and correct well in the WL images. Because the spots interact poorly with the JPEG data compression algorithm, most of them are treated on-board as bad pixels and are replaced by a good nearest neighbour.
Larger spots ( ~ 50-60 pixel diameter with an intensity of ~ 96-98%) are also evident on the WL flat field. These are most likely shadows of dust particles on the fused silica filter in the aft filter wheel. They disappeared when a WL flat field was generated from images that did not use the fused silica filter. In these flat fields, another set of larger ( ~ 80 pixels), less well focused, and lower contrast ( ~ 97-99% intensity) spots became apparent as a regular array on the CCD. This array was seen at several wavelengths during CCD testing prior to launch and is believed to be a CCD fabrication artifact. All of these features correct well in the WL images.
A pair of bad partial rows (CCD columns actually) are visible in the WL flat field. In addition, vertical and horizontal dark lines are seen every 24 pixels at very low contrast. These are a CCD fabrication artifact.
The flat field at 1700 Å (Figure 3.5b) shows some degradation in the relative response across the field of the CCD in the center. Although 30 images were utilized in the analysis of the flat field, most of the CCD structure is not resolved at this wavelength due to higher contrast, lower count rates, and changing structure in the original images when compared to those in WL. Despite defocusing, the 1700 Å images in quiet sun have network features three times brighter than average intensity. However, the pair of bad partial pixel rows observed in the WL flat field is also present in the 1700 Å flat field.
The 1700 Å flat field for 7 January 1999 demonstrates a degradation of about 5-8% in the center region of the CCD with a small portion degrading up to ~ 10%. A 1700 Å flat field from 9 October 1998 displayed about a 2-5% relative degradation in the same region. This relative degradation in response across the field is probably occurring in the Lumogen coating on the front of the CCD. A similar loss has been noted near the CCD center in EUV images of loops on the limb when compared to images with the limb moved to regions near the outer, non-degraded portions of the CCD area. The decrease in Lumogen sensitivity near the center of the CCD is probably a result of damage by the accumulated EUV dosage. However, the degree of degredation is less than was anticipated.
Efforts are ongoing to generate satisfactory flat-field images for the other lines. The EUV wavelengths are particularly resistant to this method, as they are of extremely high contrast with much of the image at a very low count rate. Flat field data taken in the 171 and 195 Å channels in May 1999 suggests that the degredation in sensitivity in the EUV is similar to that at 1700 Å.
For the most recent information on flat field measurements, see the TRACE Web pages at Lockheed-Martin.
TRACE can provide information on the morphology of the magnetic field directly from its images and can also provide a number of other diagnostics.
When TRACE is in or near its eclipse season, care should be taken when using data for diagnostic purposes because of the effects of atmospheric absorption - see Appendix B.4.
The three EUV channels overlap in temperature coverage and can be used to investigate the temperature of the coronal plasma. As all the EUV wavelength bands are dominated by different ionization stages of iron, ratios do not depend on a knowledge of iron abundance. The band ratios are extremely sensitive to temperature changes, varying by factors of up to 40 over typical coronal temperature ranges. This compares favorably with broad-band temperature diagnostics (e.g., factors of 2-4 for Yohkoh/SXT temperature ratios).
Figure 3.6 shows the relative contributions of the three EUV bands. Ratios of the bands are multivalued and are ambiguous for certain temperatures. Obtaining images in all three EUV channels can help to resolve the ambiguity if the plasma is nearly isothermal. In practice, this is only likely to work if careful background subtraction is done. Without background subtraction, temperature ratios yield inconsistent or nonsensical results in nearly all cases.
It is surprisingly easy to derive differential emission measure distributions from TRACE data, primarily because there are few channels and so an inversion by linear techniques is well-behaved. There are, however, several pitfalls:
TRACE uses a set of three filters to observe and correct the C IV images (Handy et al, 1998). The filters characteristics are:
Reduction of a set of three observations uses simple matrix methods. Let P(i) represent the image made with the ith filter. Let I(j) represent the intensities of the C IV lines (j=1), the chromospheric contribution (j=2) and the long wavelength continuum (j=3), respectively. Then the matrix representation of the set of images is:
[P] = [A][I]
where [P] and [I] are column vectors and [A] is the matrix A(i,j) representing the transmission of the i th filter to the j th wavelength. The formal solution is:
[I] = [a][P]
where [a] is the inverse of [A]. The transmissions A(i,j) is measured during instrument calibration; the matrix solution is expected to be well behaved because of the nature of the problem. (Note that A(3,1) and A(3,2) are both zero and that A(l,j) and A(2,j) are linearly independent because of the way the filters are designed).
The reduced observations provide images of the chromosphere (from the C I and Fe II lines) as well the transition zone. The long wavelength continuum image is probably formed somewhere between the high photosphere and the temperature minimum, based on the work of Foing (1986). Finally, images taken through the UV entrance filter only are dominated by wavelengths near 2500 Å, which arises in the photosphere. These images are used extensively for co-alignment with SoHO and other observations.
See Aiken et al., 19?? for more information on this type of science.
TRACE Investigation and Technical Plan (Phase III & IV), August 1994, LMSC P017270P-1
``The Transition Region and Coronal Explorer'', 1999, Handy et al., Sol. Phys., in press.
``UV Observations with TRACE'', 1998, Handy et al., Sol. Phys., 183, 29
``Thermospheric Molecular Oxygen??'', 19??, Aiken et al., ???.
|TRACE Calatog and Ephemeris|
|trace_cat||read TRACE catalog (via setup/call to 'read_genxcat')|
|view_trace_mosaic||View TRACE mosaic for date closest to selected date|
|rd_fdss||To read the FDSS files and put the data into structures|
|pr_fdss||Print an FDSS files for the selected time interval|
|read_trace||Read TRACE data image files, headers or headers & data|
|trace_cat2data||use catalog entries to get the data (or filelist/dset)|
|read_analist||Reads a list of files and frame indices created by the ANA Browser|
|write_trace||write trace index/data to specified type of FITS or WWW file|
|trace_sswhere||Select subset of TRACE images with widget interface|
|struct_where||filter a structure array; return SubScripts which satisfy|
|grid_data||return gridded subset of input ( fixed cadence if no gaps)|
|tim2dset||Given a structure (roadmap or index), find the dataset with the time closest to an input time.|
|read_trace_fov||Reads selected sub-image, etc.|
|trace2x||Ingests the ANA Browser's Fav Img file and reads each image and writes out as gif files or creates an IDL array.|
|open_anacube||Opens ANA data cube for reading with WINDOW_ANACUBE|
|window_anacube||Read ANA image cube opened with OPEN_ANACUBE; windowed region selectable by cursors.|
|close_anacube||Close ANA data cube opened with OPEN_ANACUBE|
|Plotting TRACE Data|
|slide_image||Create a scrolling graphics window for examining large images.|
|utplot||Plot X vs Y with Universal time labels on bottom X axis.|
|lcur_image||To display a normalized light curve plot for image data.|
|plot_arc||To allow a user to mark an arc on an image and the intensity along that arc will be plotted|
|index2map||Make an image map from index/data pair|
|plot_map||Plot an image map|
|ssw_track_fov||Extract a sub-field from the SSW-compliant (2D) image data based on the reference time and reference coordinates.|
|xstepper||Widget interface/ X-Windows data cube reviewer|
|trace_special_movie||TRACE movies - > WWW|
|image2movie||convert an image file sequence (3d, gif, jpeg) to mpeg or gif animation URL Reference: http://www.|
|trace_prep||Process TRACE image(s).|
|tr_dark_sub||Subtract a previously averaged, 1 second exposed dark current image, which includes an ADC offset, from a TRACE image after selecting and reading in the closest dark fits file for the first image.|
|tracedespike||despike an image using a median filter (default) that eliminates spikes exceeding `threshold' percent (detault = 15%), or using a statistical correction that corrects pixels diviating by more than|
|trace_knoise||Remove readout noise from TRACE images by identifying and zeroing spikes in the FFT.|
|trace_unspike_time||temporal despiking of TRACE images using neighbor images|
|trace_wave2point||apply wavelength dependent adjustments to trace pointing tags|
|Diagnostics and Modelling|
|civ_subtract||Given an arbitrary set of UV images from TRACE out of the 1550, 1600 and 1700 Images, generate a "Clean" C IV image, per Handy et al.|
|trace_t_resp||Returns TRACE EUV response to a solar plasma at temperature T.|
|trace_dem||Calculate differential emission measure and EM weighted average temperature for a set of TRACE images in all three EUV wavelengths (171, 195, 284).|
|trace_dem_setup||Calculate and invert the temperature response matrix for a 3-component model of the differential emission measure.|
|trace_tbasis||Implement three DEM basis functions, indexed 0, 1, 2, for use with TRACE_DEM and TRACE_DEM_SETUP.|
|trace_tmap||Compute temperature and emission measure maps based on an isothermal model.|
|trace_isothermal||Create temperature and emission measure maps from TRACE EUV images, assuming an isothermal plasma along the line of sight for each pixel.|
|trace_t2em||Given an array of possible temperatures and one, two, or three pixel values in DN for any of the TRACE EUV passbands, calculate the corresponding|
|trace_disp_tem||Create a map of temperature and emission measure.|
|trace_teem||calculates temperature and emission measure from a wavelength pair of 2 TRACE images (e.|
|trace_files||return trace reformatted file names between t0 and t1|
|trace_list_index||produces listing of TRACE index structure|
|trace_colors||return TRACE wave dependent RGB; optionally loadit|
|trace_scale||scale TRACE images (SSW wrapper for Karel Schryver routines)|
|tr_ext_subimg||To extract a sub image out of a TRACE image with no change of the image resolution|
|trace_data_filter||return subscripts of 'good' or 'bad' trace data|
|tr_get_disp||Given a datacube of images, measure the rigid displacement between each image and the first in the cube and optionally shift each image to coalign the entire cube.|
|align_cube_correl||align a data cube via cross correlation; update coordinates|
|normalize_cube||empirically normalize cube of data from relative signal levels|
|grid_data||return gridded subset of input ( fixed cadence if no gaps)|
|trace_uniq_movies||identify uniq movies from input structures (index or catalog)|
|gt_tagval||return value stored in specified tag - (nested N-deep struct OK)|
|gtt_orbit||To read the FDSS files and output an array of answers corresponding to the array of input times based on code|
|gtt_info||To extract information from the TRACE index information.|
|gtt_ccd_cen||To compute solar coordinates of the CCD center for a trace image index|
|gtt_mnem||TRACE routine to extract mnemonic information from data|
|gtt_shutter_exp||Compute and return shutter exposure time from index of an image.|
|gtt_wave_tru||Compute and return wave length name from index of an image.|
On average, TRACE has generated just over 3 GBytes of data per week - by the end of the first year of operation it had produced just over 161 Gbytes of data. A detailed breakdown of the data generated each day by TRACE can be found on a page in the Web version of this document.
TRACE data may be lost for a number of reasons: data overflow in the on-board memory, missed downlink, etc. Often, the data is just missing as the result of a bad or missed transmission from the ground-station. Where possible, the TRACE team attempt to recover this data by retransmission and reformatting, and update the TRACE data archive when this is done.
The first major data gap was at the start of the first eclipse season when TRACE was shutdown from 17:00 on 7 November 1998 to 12:00 on 11 November 1998. Each year there is a gap of several days when TRACE was switched off as a precaution during the Leonid meteor shower (16-19 November 1998; 17-19 November 1999).
A list showing the status of missing TRACE data files can be found on a Web page at Lockheed-Martin (<http://vestige.lmsal.com/TRACE/Data/Missing/>).
There are several ways of searching for particular TRACE data.
The TRACE DATA CENTER uses a Search Engine based on the TRACE Data CATALOG. The user select parameters in a web-based form and submits the request; an IDL task linked to the page generates quicklook images and allows the selection to be refined before creating a FITS file of the selected modes. See URL:
Alternatively, you can use a Search Engine based on the TRACE Observing PLANS provided by the TRACE EOF. The user enters search parameters (e.g Objective/Science, Date, JOP or Campaign No., FOV center, etc.) and is presented with a list of the planned observations that match the parameters. See URL:
There is also a TRACE Event List - sorted by event type that has been assembled by team at the TRACE EOF. The user selects a type of event and a time interval and is presented with a list of the dates that such events were observed. See URL:
<http://chippewa.nascom.nasa.gov/ ~ despres/data_archive/datarch1.html>
The TRACE spacecraft is in a Sun-synchronous orbit. Every year, for about 6 weeks either side of the Winter Solstice, TRACE is eclipsed for part of its orbit. The timing of the eclipse may be determined from the ephemeris files (see Section 2.1.2). The first eclipse season started on 7 November 1998 and ended on 5 February 1999; the second covered a similar interval (7 November 1999 to 5 February 2000).
While TRACE is in its eclipse season, and for several weeks either side, care should be taken when using TRACE data. In each orbit, for several minutes either side of the eclipse, the signal is still attenuated by the Earth's atmosphere and the response of the EUV lines is compromised. The attenuation on successive images changes rapidly and the effect is very difficult to predict. While the images are still fine for morphological studies, they should only be used for diagnostic purposes with extreme caution.
The effects of atmospheric absorption are present for several weeks either side of the interval when TRACE is fully eclipsed and extends from mid-October to the beginning of March. The durations of the eclipse and absorption for each orbit are shown during the first eclipse season in figure B.7 - the eclipse duration is the dashed curve in the centre. The routine trace_prep warns users if the data they have selected were taken during these times.
SolarSoft is described on Web pages hosted at Lockheed-Martin in Palo Alto, California - see the URL <http://www.lmsal.com/solarsoft/>. Pages referenced from this home page describe the Installation and Upgrading of the SolarSoft tree - the steps necessary to configure your system are also described. Another page describes some of the concepts of SolarSoft.
It is not necessary to install the whole of SolarSoft to analyse TRACE data. For TRACE, when requesting an installation through the SSW Installation Form, you should request TRACE under Others..., and request binaries and ANA under Packages... Once you have made your SolarSoft installation, it is recomended that you update it regularly.
In order to use some of the TRACE software, e.g. trace_prep, you need some of the ancillary TRACE files and therefore need to install $tdb branch of the SolarSoft DataBase (SSWDB) tree. This is a separate tree to SolarSoft and will require a separate mirror package - see the web page at Lockheed-Martin describing SolarSoft DataBase (SSWDB) Installation if you wish to install the database branch. Note: Take care when requesting the mosaics/ sub-branch, it is quite large.
A description of ANA1, together with an on-line manual and instructions on how to install it, can be found on one of the Lockheed-Martin Web sites on URL <http://ana.lmsal.com/>. The latest version merges two strands of ANA that had evolved (developed by Dick Shine and Louis Strous), and is backwardly compatible with both earlier versions (with some minor exceptions).
If you need more information about ANA, or have any questions, contact Zoe Frank (firstname.lastname@example.org), Louis Strous (email@example.com), or Dick Shine (firstname.lastname@example.org).
The TRACE Analysis Guide (TAG) may be viewed as a Web document on the URL's:
The TAG is available as a PostScript document; it is in two formats: for A4 paper, and for US Letter paper. Choose the one appropriate for your printer - it is designed to be printed double-sided. If you want a printed copy of the TAG, the PostScript version is recommended since the screen representation of special characters in the Hypertext version does not produce good printed output.
The TAG was prepared at the YDAC (located at the Mullard Space Science Laboratory, University College London) by Bob Bentley. The Hypertext version was translated from LaTeX using TtH, and further formatted using IDL.
In the Web version of the TAG, the changes between versions are listed.
This version of the TAG was prepared on: Jan 27, 2001
Calibrating TRACE data, 2-4
Eclipse season, B-4
Help on software, 2-10
JPEG compression, 3-2
Making Mosaics, 2-6
Particle background, 2-4, 3-2
Searching for Data, 1-3, B-3
Useful software, A-0
1 ANA - A Non Acronym