EOVSA Data products: Difference between revisions

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Welcome to the EOVSA data products documentation. EOVSA observes the full disk of the Sun at all times when the Sun is >10 degrees above the local horizon, which is season dependent and ranges from 7-12 hours duration centered on 20 UT. During January, coverage will be 16-24 UT daily, 7 days/week. EOVSA will provide microwave spectra and imaging at up to 451 frequencies between 1 and 18 GHz. We deliver the radio interferometry data in level 0-2.  
EOVSA observes the full disk of the Sun at all times when the Sun is >10 degrees above the local horizon (season dependent and ranges from 7-12 hours duration centered on 20 UT). EOVSA records data at 451 science frequency channels each second, in four polarization products, as well as additional total flux measurements from each individual antenna. Raw data in the visibility domain are processed through a pipeline processing system to produce images and spectrograms in the time- and frequency-dependent image plane (the block diagram in Figure 1 shows the data flow in the pipeline).  
[[File:pipeline_flowchart.jpg|center|600px]]
[[File:pipeline_flowchart.jpg|center|600px|EOVSA pipeline block diagram/flow chart ]]


=Data Definition=
We deliver the radio interferometry data on the following three levels:
==Level 0 - Raw visibility data from the instrument==


==Level 1 - Calibrated visibility data==
Level 1 data have all of the required content to produce Level 2 data products
===[http://www.ovsa.njit.edu/fits/UDBms_slfcaled# CASA 1-min averaged ms]===
===CASA Event ms===


==Level 2 - Images and spectrogram data in standard FITS format ==
=Level 0 - Raw visibility data from the instrument=
===[http://www.ovsa.njit.edu/fits/synoptic# All-day TP spectrum]===
 
Daily total power full-Sun-integrated spectrogram calibrated in solar flux units are provided at 451 frequencies and 1 s time resolution.
As outlined in Figure 1, EOVSA creates raw data products in the left-hand column (labeled Level 0). This includes observations of cosmic sources for phase calibration, and gain and pointing observations required for total power calibration.
 
==Raw "Interim" Database (IDB) visibility data==
Full-resolution raw "Interim" Database (IDB) visibility data. They are stored in Miriad format, and hence may not be that useful for most people. Be patient after clicking the link--this is a very long list of directories, one for each available date. These data can be retrieved from the following page:
 
http://www.ovsa.njit.edu/fits/IDB/
 
==Raw 1-min-averaged visibility data==
This is the same as for the IDB data, except with 1-minute time integration applied. This is typically not useful for flares, but is perfectly fine for imaging active regions and full Sun. These data can be retrieved from the following page:
 
http://www.ovsa.njit.edu/fits/UDB/
 
=Level 0.5 - Calibrated visibility data=
After applying calibration and other preliminary processing to the raw (level 0) data, we create the CASA ms’s in the second column in Figure 1 (labeled "level 0.5"). These visibility data are in the Fourier domain of the true images in the plane of the sky and are not immediately ready for spectral imaging analysis yet. However, they have all of the required content to produce images and spectrogram data in standard FITS format (level 1.0).  We provide a set of standard ms’s for each day (red boxes in Figure 1), for use by researchers who know how to deal with visibility data.
 
==Calibrated full-resolution visibility data for flare events==
Calibrated and self-calibrated visibility data for flare events (purple boxes in Figure 1) will typically be available within 7 days after they are taken. They will be released at our flare list site soon: https://ovsa.njit.edu/flarelist
 
==Self-calibrated 1-min-averaged visibility data==
EOVSA 1-min averaged visibility data in CASA ms format can be retrieved from the following page:
 
http://www.ovsa.njit.edu/fits/UDBms_slfcaled
 
=Level 1.0 - Images and spectrogram data in standard FITS format =
 
Most users, however, will prefer to work with spectrogram (frequency-time) and image data, which are also outputs of the pipeline system shown in Figure 1 (orange boxes). Spectrograms are provided as standard FITS tables containing the frequency list, list of times, and data in both total power (TP) and a sum of amplitudes over intermediate-length baselines (cross power or XP). Likewise, image data products are in FITS format with standard keywords and are converted into the Helioprojective Cartesian coordinate system compatible with the World Coordinate System (WCS) convention, along with correct registration for the spatial, spectral, and temporal coordinates. Both the spectrogram and image data products are calibrated properly and have physical radio intensity units (sfu for spectrograms and brightness temperature for radio images).
 
We provide the following data products:
* Synoptic products:
** All-day total-power spectrograms:
** All-day cross-power spectrograms:
** All-day synoptic images:
* Event-based products:
** Flare spectrograms: These are full time and frequency resolution spectrograms produced from the median of calibrated cross-power visibilities in FITS format, cropped to cover the flare duration. Pre-flare background is also subtracted. Compared to total-power spectrograms, these spectrograms have the advantage of revealing details of the flare evolution by "filtering out" the large-scale, continuous background from the visibilities (as they are poorly correlated by baselines with intermediate lengths). Note that for flares that have a large source size, the flux shown by the cross-power spectrograms can be lower than its true flux (as a fraction of the flux will be "resolved out"). In this case, one might compare the spectrograms with our total-power spectrogram products.
** Pipeline-produced spectral images: We also have a semi-automated flare imaging pipeline to produce calibrated (and self-calibrated) images at 12-s cadence in up to 10 frequency bands. They are saved in standard FITS format and have been registered into Helioprojective coordinates. They can be read by SSWIDL or astropy/sunpy. These data have already been calibrated to physical units and are usually good to be compared with context data. But please be cautious when using them for quantitative spectral analysis.
 
'''List of Level 1 data products currently provided'''
{| class="wikitable"
|-
! scope="col"| Category
! scope="col"| Data Product
! scope="col"| Naming Convention
! scope="col"| Download Link
|-
! rowspan="2" | Synoptic Spectrograms
| All-day TP Spectrograms
| EOVSA_TPall_yyyymmdd.fts
!rowspan="9" | https://ovsa.njit.edu/browser
|-
| All-day XP Spectrograms
| EOVSA_XPall_yyyymmdd.fts
|-
! rowspan="7" | Synoptic Images
|-
| Synoptic 1.4 GHz images
| eovsa_yyyymmdd.spw00-01.tb.disk.fits
|-
| Synoptic 3.0 GHz images
| eovsa_yyyymmdd.spw02-05.tb.disk.fits
|-
| Synoptic 4.5 GHz images
| eovsa_yyyymmdd.spw06-10.tb.disk.fits
|-
| Synoptic 6.8 GHz images
| eovsa_yyyymmdd.spw11-20.tb.disk.fits
|-
| Synoptic 10.2 GHz images
| eovsa_yyyymmdd.spw21-30.tb.disk.fits
|-
| Synoptic 13.9 GHz images
| eovsa_yyyymmdd.spw31-43.tb.disk.fits
|-
! rowspan="1" | Flare Spectrograms
| Full-resolution cross-power Spectrogram
| eovsa.spec.flare_id_YYYYMMDDHHMMSS.fits
!rowspan="2" | https://ovsa.njit.edu/flarelist
|-
! rowspan="1" | Flare Spectral Images
| Pipeline-produced spectral images
| eovsa.lev1_mbd_12s.YYYY-MM-DDTHHMMSSZ.image.fits
|-
|}
 
==Getting level 1 data==  
===Synoptic level 1 data===
EOVSA Level 1 synoptic data products can be retrieved with the following steps:
* Go to [http://ovsa.njit.edu/browser/ EOVSA browser] page.
* Browse to the date of interest.
* Click "synoptic fits" button next to the calendar tool.
* Select the data product based on the names listed in the table above.
[[File:eovsa_browser.jpg|800px|center]]
 
===Flare level 1 data===
EOVSA flare list with spectrograms and spectral images can be queried and downloaded at https://ovsa.njit.edu/flarelist.
 
==Reading level 1 data==
===Software===
We have developed a package for EOVSA data processing and analysis:
[https://github.com/suncasa/suncasa SunCASA] A wrapper around [https://casa.nrao.edu/ CASA (the Common Astronomy Software Applications package)] for synthesis imaging and visualizing solar spectral imaging data. CASA is one of the leading software tools for "supporting the data post-processing needs of the next generation of radio astronomical telescopes such as ALMA and VLA", an international effort led by the [https://public.nrao.edu/ National Radio Astronomy Observatory]. The current version of CASA uses Python (2.7) interface. More information about CASA can be found on [https://casa.nrao.edu/ NRAO's CASA website ]. Note, CASA is available ONLY on UNIX-BASED PLATFORMS (and therefore, so is SunCASA). We are developing a new version of SunCASA based on CASA 6 (which offers a modular approach) so that users have the flexibility to build CASA tools and tasks in their Python environment.
 
Please [http://www.ovsa.njit.edu/wiki/index.php/SunCASA_Installation follow this link] for details regarding the installation of SunCASA on your own machine (only available on Unix-bases OS). This will take you to another page.
 
===Flare Spectrograms and Multi-Frequency Images ===
* An example of how to read and plot these FITS data in Python (with Astropy and SunPy) can be accessed at [https://colab.research.google.com/drive/1Y3ONWCxLPYvWda5_LqFNxafJtwZDNJBD?usp=sharing#scrollTo=ueiMoHbdxfo- this Google Colab Jupyter notebook].
* We are working on an example with SSWIDL and will release it soon.
 
===All-day TP spectrum===
Daily total power full-Sun-integrated spectrogram calibrated in solar flux units are provided at 451 frequencies (134 frequencies prior to 2019 Feb 22) and 1 s time resolution.
 
To read a spectrogram file in Python using the suncasa library:
 
<pre style="background-color: #FCEBD9;">
<pre style="background-color: #FCEBD9;">
from suncasa.eovsa import eovsa_dspec as ds
from suncasa.eovsa import eovsa_dspec as ds
## define the dynamic spectrum file.
from astropy.time import Time
tpfits = 'EOVSA_TPall_20191225.fts'
from matplotlib.colors import LogNorm
## display the dynamic spectrum.
## Read EOVSA Dynamic Spectrum FITS file <filename>
ds.dspec(tpfits)
filename = 'EOVSA_TPall_20170713.fts'
s = ds.get_dspec(filename, doplot=True, cmap='gist_heat', norm=LogNorm(vmax=2.1e3, vmin=40))
## To access the data in the spectrogram object, use
spec = s['spectrogram']                    ## (Array of amplitudes in SFU, of size nfreq,ntimes)
fghz = s['spectrum_axis']                  ## (Array of frequencies in GHz, of size nfreq)
tim = Time(s['time_axis'], format='mjd')  ## (Array of UT times in astropy.time object, of size ntimes)
 
</pre>
</pre>
The '''get_dspec''' function is accessible on [https://github.com/suncasa/suncasa-src/blob/master/suncasa/eovsa/eovsa_dspec.py GitHub]. For comprehensive guidance, please refer to suncasa's [https://suncasa-src.readthedocs.io/en/latest/autoapi/suncasa/eovsa/eovsa_dspec/index.html ReadtheDocs page].
[[File:TPSP.jpeg|center|500px]]
[[File:TPSP.jpeg|center|500px]]


===[http://www.ovsa.njit.edu/fits/synoptic# All-day XP spectrum]===
Daily cross power spectrogram (mean flux from baselines with "intermediate" lengths) calibrated in solar flux units are provided at 451 frequencies and 1 s time resolution. XP spectrogram has much better sensitivity to weak bursts.


<source lang="python" line='line'>
The following code will read the spectrogram file in IDL:
from suncasa.eovsa import eovsa_dspec as ds
## define the dynamic spectrum file.
tpfits = 'EOVSA_XPall_20191225.fts'
## display the dynamic spectrum.
ds.dspec(tpfits)
</source>
<source lang="python">
# Pseudo-interactive CASA
taskname('input parameters')
</source>


[[File:XPSP.jpeg|500px| center]]
<pre style="background-color: #FCEBD9;">
function dspec,filename,doplot=doplot
  ; Read EOVSA Dynamic Spectrum FITS file <filename> and return a spectrogram object.
  ; Optionally show an overview plot if doplot switch is set
  ;
  ; Usage:
  ;    s = dspec(<filename>)            ; Returns spectrogram object
  ;    s = dspec(<filename>,/doplot)    ; Plots spectrum and returns spectrogram object
  ;
  ; To access the data in the spectrogram object, use
  ;    spec = s.get(/spectrogram)    (Array of amplitudes in SFU, of size ntimes, nfreq)
  ;    fghz = s.get(/spectrum_axis)  (Array of frequencies in GHz, of size nfreq)
  ;    ut = s.get(/time_axis)        (Array of UT times in anytim format, of size ntimes)
 
  default,doplot,0
  spec = mrdfits(filename,0)
  freq = mrdfits(filename,1)
  time = mrdfits(filename,2)
  fghz = freq.sfreq
  ut = anytim(time)
  s = spectrogram(spec,ut,fghz)
  if doplot then begin
    window,/free,xsiz=1024,ysiz=600
    ; Find min and max of data from 5% to 95% of sorted array (eliminates outliers)
    sarr = sort(spec)
    dlim = minmax(spec[sarr[n_elements(sarr)*0.05:n_elements(sarr)*0.95]])
    ; Set drange with margin factor of 2 on low end and 5 on high end
    s.set,drange=dlim*[0.5,5]
    loadct,3
    s.plot,/log,/xsty,/ysty,ytitle='Frequency [GHz]',charsize=1.5
  endif
return,s
end
</pre>
[[File:IDL_TPSP.png|center|500px]]


===[http://www.ovsa.njit.edu/fits/synoptic# Synoptic 6-band Images]===
===Synoptic 6-band Images===
Full disk images at 6 selected frequency bands centered at 1.4, 3.0, 4.5, 6.8, 10.2, and 13.9 GHz are provided once per day, calibrated in brightness temperature. [[File:synoptic_image.jpg| center |400px]]
Full disk images at 6 selected frequency bands centered at 1.4, 3.0, 4.5, 6.8, 10.2, and 13.9 GHz are provided once per day, calibrated in brightness temperature. [[File:synoptic_image.jpg| center |400px]]


===10-min 6-band Images===
The EOVSA full disk image FITS files are compressed with the RICE algorithm implemented in the FITS file handling module (astropy.io.fits) in Astropy. EOVSA FITS files are very similar to the compressed SDO/AIA FITS files from JSOC. Popular coding languages can easily read compressed images directly.
===Event images===
 
In IDL, you can use read_sdo in the ONTOLOGY package, which should be installed by default in SolarSoftWare (SSW), to read compressed EOVSA FITS files. The following code will read the EOVSA image FITS file in SSWIDL:
 
<pre style="background-color: #FCEBD9;">
read_sdo,'eovsa_20191225.spw11-20.tb.disk.fits',header,data,/UNCOMP_DELETE
index2map,header,data,eomap
plot_map,eomap
</pre>
 
[[File:eovsa_20191225_image_sswidl.jpg| center |250px]]
 
In Python, you can use SunPy map module to read EOVAS FITS files. SunPy is an open solar data analysis environment for Python. The installation instruction can be found at [https://sunpy.org/ SunPy official website].
<pre style="background-color: #FCEBD9;">
import matplotlib.pyplot as plt
from sunpy import map as smap
eofile='eovsa_20191225.spw11-20.tb.disk.fits'
eomap = smap.Map(eofile)
eomap.plot()
plt.show()
</pre>
[[File:eovsa_20191225_image_py.jpg| center |250px]]
 
Although the Sunpy Python package already exists for doing analysis of solar data, it has a significant learning curve and lacks the generality of the Mapping routines written by Dominic Zarro for the IDL-based Solarsoft (SSW). We provided IDL Mapping routines available in Python that may help those IDL users who have been avoiding learning Python. '''The mapping routines work equally well in both Python 2.7 and Python 3'''.
Get the [http://www.ovsa.njit.edu/wiki/index.php/Mapping_Software Mapping routines]
The following code will read the EOVSA image FITS file in python:
<pre style="background-color: #FCEBD9;">
from mapping.plot_map import plot_map
from mapping.fits2map import fits2map
eofile='eovsa_20191225.spw11-20.tb.disk.fits'
eomap, h = fits2map(eofile,header=True)
plot_map(eomap, grid=15, limb=True,cmap='gray')
</pre>
[[File:eovsa_20191225_image_py_ssw-mapping.jpg| center |250px]]

Latest revision as of 20:53, 28 March 2024

EOVSA observes the full disk of the Sun at all times when the Sun is >10 degrees above the local horizon (season dependent and ranges from 7-12 hours duration centered on 20 UT). EOVSA records data at 451 science frequency channels each second, in four polarization products, as well as additional total flux measurements from each individual antenna. Raw data in the visibility domain are processed through a pipeline processing system to produce images and spectrograms in the time- and frequency-dependent image plane (the block diagram in Figure 1 shows the data flow in the pipeline).

EOVSA pipeline block diagram/flow chart

We deliver the radio interferometry data on the following three levels:


Level 0 - Raw visibility data from the instrument

As outlined in Figure 1, EOVSA creates raw data products in the left-hand column (labeled Level 0). This includes observations of cosmic sources for phase calibration, and gain and pointing observations required for total power calibration.

Raw "Interim" Database (IDB) visibility data

Full-resolution raw "Interim" Database (IDB) visibility data. They are stored in Miriad format, and hence may not be that useful for most people. Be patient after clicking the link--this is a very long list of directories, one for each available date. These data can be retrieved from the following page:

http://www.ovsa.njit.edu/fits/IDB/

Raw 1-min-averaged visibility data

This is the same as for the IDB data, except with 1-minute time integration applied. This is typically not useful for flares, but is perfectly fine for imaging active regions and full Sun. These data can be retrieved from the following page:

http://www.ovsa.njit.edu/fits/UDB/

Level 0.5 - Calibrated visibility data

After applying calibration and other preliminary processing to the raw (level 0) data, we create the CASA ms’s in the second column in Figure 1 (labeled "level 0.5"). These visibility data are in the Fourier domain of the true images in the plane of the sky and are not immediately ready for spectral imaging analysis yet. However, they have all of the required content to produce images and spectrogram data in standard FITS format (level 1.0). We provide a set of standard ms’s for each day (red boxes in Figure 1), for use by researchers who know how to deal with visibility data.

Calibrated full-resolution visibility data for flare events

Calibrated and self-calibrated visibility data for flare events (purple boxes in Figure 1) will typically be available within 7 days after they are taken. They will be released at our flare list site soon: https://ovsa.njit.edu/flarelist

Self-calibrated 1-min-averaged visibility data

EOVSA 1-min averaged visibility data in CASA ms format can be retrieved from the following page:

http://www.ovsa.njit.edu/fits/UDBms_slfcaled

Level 1.0 - Images and spectrogram data in standard FITS format

Most users, however, will prefer to work with spectrogram (frequency-time) and image data, which are also outputs of the pipeline system shown in Figure 1 (orange boxes). Spectrograms are provided as standard FITS tables containing the frequency list, list of times, and data in both total power (TP) and a sum of amplitudes over intermediate-length baselines (cross power or XP). Likewise, image data products are in FITS format with standard keywords and are converted into the Helioprojective Cartesian coordinate system compatible with the World Coordinate System (WCS) convention, along with correct registration for the spatial, spectral, and temporal coordinates. Both the spectrogram and image data products are calibrated properly and have physical radio intensity units (sfu for spectrograms and brightness temperature for radio images).

We provide the following data products:

  • Synoptic products:
    • All-day total-power spectrograms:
    • All-day cross-power spectrograms:
    • All-day synoptic images:
  • Event-based products:
    • Flare spectrograms: These are full time and frequency resolution spectrograms produced from the median of calibrated cross-power visibilities in FITS format, cropped to cover the flare duration. Pre-flare background is also subtracted. Compared to total-power spectrograms, these spectrograms have the advantage of revealing details of the flare evolution by "filtering out" the large-scale, continuous background from the visibilities (as they are poorly correlated by baselines with intermediate lengths). Note that for flares that have a large source size, the flux shown by the cross-power spectrograms can be lower than its true flux (as a fraction of the flux will be "resolved out"). In this case, one might compare the spectrograms with our total-power spectrogram products.
    • Pipeline-produced spectral images: We also have a semi-automated flare imaging pipeline to produce calibrated (and self-calibrated) images at 12-s cadence in up to 10 frequency bands. They are saved in standard FITS format and have been registered into Helioprojective coordinates. They can be read by SSWIDL or astropy/sunpy. These data have already been calibrated to physical units and are usually good to be compared with context data. But please be cautious when using them for quantitative spectral analysis.

List of Level 1 data products currently provided

Category Data Product Naming Convention Download Link
Synoptic Spectrograms All-day TP Spectrograms EOVSA_TPall_yyyymmdd.fts https://ovsa.njit.edu/browser
All-day XP Spectrograms EOVSA_XPall_yyyymmdd.fts
Synoptic Images
Synoptic 1.4 GHz images eovsa_yyyymmdd.spw00-01.tb.disk.fits
Synoptic 3.0 GHz images eovsa_yyyymmdd.spw02-05.tb.disk.fits
Synoptic 4.5 GHz images eovsa_yyyymmdd.spw06-10.tb.disk.fits
Synoptic 6.8 GHz images eovsa_yyyymmdd.spw11-20.tb.disk.fits
Synoptic 10.2 GHz images eovsa_yyyymmdd.spw21-30.tb.disk.fits
Synoptic 13.9 GHz images eovsa_yyyymmdd.spw31-43.tb.disk.fits
Flare Spectrograms Full-resolution cross-power Spectrogram eovsa.spec.flare_id_YYYYMMDDHHMMSS.fits https://ovsa.njit.edu/flarelist
Flare Spectral Images Pipeline-produced spectral images eovsa.lev1_mbd_12s.YYYY-MM-DDTHHMMSSZ.image.fits

Getting level 1 data

Synoptic level 1 data

EOVSA Level 1 synoptic data products can be retrieved with the following steps:

  • Go to EOVSA browser page.
  • Browse to the date of interest.
  • Click "synoptic fits" button next to the calendar tool.
  • Select the data product based on the names listed in the table above.
Eovsa browser.jpg

Flare level 1 data

EOVSA flare list with spectrograms and spectral images can be queried and downloaded at https://ovsa.njit.edu/flarelist.

Reading level 1 data

Software

We have developed a package for EOVSA data processing and analysis: SunCASA A wrapper around CASA (the Common Astronomy Software Applications package) for synthesis imaging and visualizing solar spectral imaging data. CASA is one of the leading software tools for "supporting the data post-processing needs of the next generation of radio astronomical telescopes such as ALMA and VLA", an international effort led by the National Radio Astronomy Observatory. The current version of CASA uses Python (2.7) interface. More information about CASA can be found on NRAO's CASA website . Note, CASA is available ONLY on UNIX-BASED PLATFORMS (and therefore, so is SunCASA). We are developing a new version of SunCASA based on CASA 6 (which offers a modular approach) so that users have the flexibility to build CASA tools and tasks in their Python environment.

Please follow this link for details regarding the installation of SunCASA on your own machine (only available on Unix-bases OS). This will take you to another page.

Flare Spectrograms and Multi-Frequency Images

  • An example of how to read and plot these FITS data in Python (with Astropy and SunPy) can be accessed at this Google Colab Jupyter notebook.
  • We are working on an example with SSWIDL and will release it soon.

All-day TP spectrum

Daily total power full-Sun-integrated spectrogram calibrated in solar flux units are provided at 451 frequencies (134 frequencies prior to 2019 Feb 22) and 1 s time resolution.

To read a spectrogram file in Python using the suncasa library:

from suncasa.eovsa import eovsa_dspec as ds
from astropy.time import Time
from matplotlib.colors import LogNorm
## Read EOVSA Dynamic Spectrum FITS file <filename>
filename = 'EOVSA_TPall_20170713.fts'
s = ds.get_dspec(filename, doplot=True, cmap='gist_heat', norm=LogNorm(vmax=2.1e3, vmin=40))
## To access the data in the spectrogram object, use
spec = s['spectrogram']                    ## (Array of amplitudes in SFU, of size nfreq,ntimes)
fghz = s['spectrum_axis']                  ## (Array of frequencies in GHz, of size nfreq)
tim = Time(s['time_axis'], format='mjd')   ## (Array of UT times in astropy.time object, of size ntimes)

The get_dspec function is accessible on GitHub. For comprehensive guidance, please refer to suncasa's ReadtheDocs page.

TPSP.jpeg


The following code will read the spectrogram file in IDL:

function dspec,filename,doplot=doplot
  ; Read EOVSA Dynamic Spectrum FITS file <filename> and return a spectrogram object.
  ; Optionally show an overview plot if doplot switch is set
  ; 
  ; Usage:
  ;    s = dspec(<filename>)            ; Returns spectrogram object
  ;    s = dspec(<filename>,/doplot)    ; Plots spectrum and returns spectrogram object
  ;
  ; To access the data in the spectrogram object, use
  ;    spec = s.get(/spectrogram)    (Array of amplitudes in SFU, of size ntimes, nfreq)
  ;    fghz = s.get(/spectrum_axis)  (Array of frequencies in GHz, of size nfreq)
  ;    ut = s.get(/time_axis)        (Array of UT times in anytim format, of size ntimes)
  
  default,doplot,0
  spec = mrdfits(filename,0)
  freq = mrdfits(filename,1)
  time = mrdfits(filename,2)
  fghz = freq.sfreq
  ut = anytim(time)
  s = spectrogram(spec,ut,fghz)
  if doplot then begin
    window,/free,xsiz=1024,ysiz=600
    ; Find min and max of data from 5% to 95% of sorted array (eliminates outliers)
    sarr = sort(spec)
    dlim = minmax(spec[sarr[n_elements(sarr)*0.05:n_elements(sarr)*0.95]])
    ; Set drange with margin factor of 2 on low end and 5 on high end
    s.set,drange=dlim*[0.5,5]
    loadct,3
    s.plot,/log,/xsty,/ysty,ytitle='Frequency [GHz]',charsize=1.5
  endif
return,s
end
IDL TPSP.png

Synoptic 6-band Images

Full disk images at 6 selected frequency bands centered at 1.4, 3.0, 4.5, 6.8, 10.2, and 13.9 GHz are provided once per day, calibrated in brightness temperature.

Synoptic image.jpg

The EOVSA full disk image FITS files are compressed with the RICE algorithm implemented in the FITS file handling module (astropy.io.fits) in Astropy. EOVSA FITS files are very similar to the compressed SDO/AIA FITS files from JSOC. Popular coding languages can easily read compressed images directly.

In IDL, you can use read_sdo in the ONTOLOGY package, which should be installed by default in SolarSoftWare (SSW), to read compressed EOVSA FITS files. The following code will read the EOVSA image FITS file in SSWIDL:

read_sdo,'eovsa_20191225.spw11-20.tb.disk.fits',header,data,/UNCOMP_DELETE
index2map,header,data,eomap
plot_map,eomap
Eovsa 20191225 image sswidl.jpg

In Python, you can use SunPy map module to read EOVAS FITS files. SunPy is an open solar data analysis environment for Python. The installation instruction can be found at SunPy official website.

import matplotlib.pyplot as plt
from sunpy import map as smap
eofile='eovsa_20191225.spw11-20.tb.disk.fits'
eomap = smap.Map(eofile)
eomap.plot()
plt.show()
Eovsa 20191225 image py.jpg

Although the Sunpy Python package already exists for doing analysis of solar data, it has a significant learning curve and lacks the generality of the Mapping routines written by Dominic Zarro for the IDL-based Solarsoft (SSW). We provided IDL Mapping routines available in Python that may help those IDL users who have been avoiding learning Python. The mapping routines work equally well in both Python 2.7 and Python 3. Get the Mapping routines The following code will read the EOVSA image FITS file in python:

from mapping.plot_map import plot_map
from mapping.fits2map import fits2map
eofile='eovsa_20191225.spw11-20.tb.disk.fits'
eomap, h = fits2map(eofile,header=True)
plot_map(eomap, grid=15, limb=True,cmap='gray')
Eovsa 20191225 image py ssw-mapping.jpg