Making quick-look flare spectrograms and images - Revision history

Mwang: /* Step 1: Import the data as CASA measurement set(s) */

2026-02-18T20:42:06Z

Step 1: Import the data as CASA measurement set(s)

← Older revision		Revision as of 20:42, 18 February 2026
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	<pre style="font-family:courier">print(out_ms)		<pre style="font-family:courier">print(out_ms)
	['./IDB20240507162024.ms']</pre>		['./IDB20240507162024.ms']</pre>

			For SoDs, if your existing IDB file has already been processed with 'fs.calIDB' to generate the TP/XP spectra, set udb_corr=False. Please use the code below to generate the CASA measurement set:

			<pre style="font-family:courier">out_ms = importeovsa('IDB20240507162024', udb_corr=False) </pre>

	=== Step 2: Calibrate the CASA measurement set ===		=== Step 2: Calibrate the CASA measurement set ===

CaiusSelhorst: /* Step 3: Produce quicklook image(s) */

2026-01-13T23:39:03Z

Step 3: Produce quicklook image(s)

← Older revision		Revision as of 23:39, 13 January 2026
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	You can also save a .png file of the image:		You can also save a .png file of the image:
	<pre style="font-family:courier">plt.savefig('flare_20240507T162905_8-12GHz.png',dpi=100</pre>		<pre style="font-family:courier">plt.savefig('flare_20240507T162905_8-12GHz.png',dpi=100)</pre>

	One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then confidently record the flare location in your report.		One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then confidently record the flare location in your report.

CaiusSelhorst: /* Step 3: Produce quicklook image(s) */

2026-01-13T23:35:24Z

Step 3: Produce quicklook image(s)

← Older revision		Revision as of 23:35, 13 January 2026
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	[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]

			You can also save a .png file of the image:
			<pre style="font-family:courier">plt.savefig('flare_20240507T162905_8-12GHz.png',dpi=100</pre>

	One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then confidently record the flare location in your report.		One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then confidently record the flare location in your report.

CaiusSelhorst: /* Step 1: Import the data as CASA measurement set(s) */

2026-01-13T22:55:08Z

Step 1: Import the data as CASA measurement set(s)

← Older revision		Revision as of 22:55, 13 January 2026
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	This process would take ~10+ minutes to complete. It would produce a file under the current directory named "IDB20240507162024.ms"		This process would take ~10+ minutes to complete. It would produce a file under the current directory named "IDB20240507162024.ms"

	<pre style="font-family:courier">print(~~outms~~)		<pre style="font-family:courier">print(out_ms)
	['./IDB20240507162024.ms']</pre>		['./IDB20240507162024.ms']</pre>

CaiusSelhorst: /* Step 1: Import the data as CASA measurement set(s) */

2026-01-13T22:33:41Z

Step 1: Import the data as CASA measurement set(s)

← Older revision		Revision as of 22:33, 13 January 2026
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	=== Step 1: Import the data as CASA measurement set(s) ===		=== Step 1: Import the data as CASA measurement set(s) ===
	<pre style="font-family:courier">from suncasa.suncasatasks import importeovsa</pre>		<pre style="font-family:courier">from suncasa.suncasatasks import importeovsa</pre>

			If the last command closes your previous spectrogram figures, you can change the matplotlib backend with the command:

			<pre style="font-family:courier">import matplotlib
			matplotlib.use('qtAgg',force=True) </pre>

	Importeovsa imports one or a list of IDB files into a CASA measurement set. In this case, the flare peak is at 16:29 UT, which is fully covered by the first IDB file "IDB20240507162024". The duration of each IDB file is usually 10 minutes, unless it is at the end of a solar scan. Now we import the IDB file:		Importeovsa imports one or a list of IDB files into a CASA measurement set. In this case, the flare peak is at 16:29 UT, which is fully covered by the first IDB file "IDB20240507162024". The duration of each IDB file is usually 10 minutes, unless it is at the end of a solar scan. Now we import the IDB file:

CaiusSelhorst: /* Step 1: Import the data as CASA measurement set(s) */

2026-01-13T21:58:16Z

Step 1: Import the data as CASA measurement set(s)

← Older revision		Revision as of 21:58, 13 January 2026
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	Importeovsa imports one or a list of IDB files into a CASA measurement set. In this case, the flare peak is at 16:29 UT, which is fully covered by the first IDB file "IDB20240507162024". The duration of each IDB file is usually 10 minutes, unless it is at the end of a solar scan. Now we import the IDB file:		Importeovsa imports one or a list of IDB files into a CASA measurement set. In this case, the flare peak is at 16:29 UT, which is fully covered by the first IDB file "IDB20240507162024". The duration of each IDB file is usually 10 minutes, unless it is at the end of a solar scan. Now we import the IDB file:

	<pre style="font-family:courier">~~outms~~ = importeovsa('IDB20240507162024') </pre>		<pre style="font-family:courier">out_ms = importeovsa('IDB20240507162024') </pre>

	This process would take ~10+ minutes to complete. It would produce a file under the current directory named "IDB20240507162024.ms"		This process would take ~10+ minutes to complete. It would produce a file under the current directory named "IDB20240507162024.ms"

Bchen: /* Step 3: Produce quicklook image(s) */

2026-01-12T23:37:21Z

Step 3: Produce quicklook image(s)

← Older revision		Revision as of 23:37, 12 January 2026
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	[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]

	One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then record the flare location in your report.		One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then confidently record the flare location in your report.
	[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]

Bchen: /* Step 3: Produce quicklook image(s) */

2026-01-12T22:07:04Z

Step 3: Produce quicklook image(s)

← Older revision		Revision as of 22:07, 12 January 2026
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	=== Step 3: Produce quicklook image(s) ===		=== Step 3: Produce quicklook image(s) ===
	Now we will use CASA's tclean to produce an image at the flare peak. More information of how to use the tclean task can be found at [https://casadocs.readthedocs.io/en/stable/api/tt/casatasks.imaging.tclean.html this link]. We need to use the information found from the previous steps to select an appropriate time range, spectral window, and antennas for imaging.		Now we will use CASA's tclean to produce an image at the flare peak. More information of how to use the tclean task can be found at [https://casadocs.readthedocs.io/en/stable/api/tt/casatasks.imaging.tclean.html this link]. We need to use the information found from the previous steps to select an appropriate time range, spectral window, and antennas for imaging.

			First, import tclean
			<pre style="font-family:courier">from casatasks import tclean</pre>

	For the time range, here I choose 10 seconds near the flare peak. Note the syntax is 'start_time~end_time', with time format as yyyy/mm/dd/hh:mm:ss.		For the time range, here I choose 10 seconds near the flare peak. Note the syntax is 'start_time~end_time', with time format as yyyy/mm/dd/hh:mm:ss.

Bchen: /* Step 3: Produce quicklook image(s) */

2026-01-12T19:13:58Z

Step 3: Produce quicklook image(s)

← Older revision		Revision as of 19:13, 12 January 2026
Line 239:		Line 239:
	[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]

	One can then compare with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location. Note that ~~there could be~~ multiple activities across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio ~~source~~ and ~~the~~ EUV ~~source~~. Once confirmed, you can then record the flare location in your report.		One can then compare your radio flare location - see the top right corner of the figure above, which says [725", 437"] with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location at the bottom (marked by the red box). Note that multiple activities may occur across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio and EUV signatures. Once confirmed, you can then record the flare location in your report.
	[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]

Bchen: /* Producing EOVSA quick-look flare images */

2026-01-12T19:02:02Z

Producing EOVSA quick-look flare images

← Older revision		Revision as of 19:02, 12 January 2026
Line 239:		Line 239:
	[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507.jpg\|none\|thumb\|center\|500px\|]]

	One can then compare with, e.g., the [~~Heliophysics Events Knowledgebase entry~~ https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location. Note that there could be multiple activities across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio source and the EUV source. Once confirmed, you can then record the flare location in your report.		One can then compare with, e.g., the [https://www.lmsal.com/hek/her?cmd=view-voevent&ivorn=ivo://helio-informatics.org/FL_SSWLatestEvents_gev_20240507_1621 Heliophysics Events Knowledgebase entry] of this event, or JHelioviewer to confirm the flare location. See below for a JHelioviewer snapshot showing the flare location. Note that there could be multiple activities across the solar disk, and it is important to examine the full disk to confirm the correspondence between the radio source and the EUV source. Once confirmed, you can then record the flare location in your report.
	[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]		[[File:flare_imaging_example_20240507_Jhelioviewer.jpg\|none\|thumb\|center\|500px\|]]