Tohban EOVSA Imaging Tutorial A-Z V2 - Revision history

Schhabra: Blanked the page

2022-07-07T23:16:19Z

Blanked the page

Schhabra at 08:41, 7 July 2022

2022-07-07T08:41:18Z

← Older revision		Revision as of 08:41, 7 July 2022
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	Page Last Updated: 07/06/2022		Page Last Updated: 07/07/2022

Schhabra at 08:38, 7 July 2022

2022-07-07T08:38:13Z

← Older revision		Revision as of 08:38, 7 July 2022
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	==== How to connect to pipeline ====		==== How to connect to pipeline ====
	'''Windows:''' On a windows machine Mobaxterm can be used to connect to Pipeline. ~~For details, see .~~..		'''Windows:''' On a windows machine Mobaxterm can be used to connect to Pipeline. The process to add rsa keys to access gues@ovsa is slightly complicated. Please contact Dale for the set up.

	'''Linux/Unix:''' On a linux/Mac, the guest account will be used for people to log in as Tohban. Rather than using a password, access will be tied to specific computers that you use. One needs to generate a public + private ssh key pair using ssh-keygen or equivalent program that will result in a public key (plain text) file called id_rsa.pub, created in your ~/.ssh folder, the contents of which can be emailed to Dale or Owen to be added under "authorized keys". The ssh commands can then be used directly through the terminal:		'''Linux/Unix:''' On a linux/Mac, the guest account will be used for people to log in as Tohban. Rather than using a password, access will be tied to specific computers that you use. One needs to generate a public + private ssh key pair using ssh-keygen or equivalent program that will result in a public key (plain text) file called id_rsa.pub, created in your ~/.ssh folder, the contents of which can be emailed to Dale or Owen to be added under "authorized keys". The ssh commands can then be used directly through the terminal:

Schhabra at 08:36, 7 July 2022

2022-07-07T08:36:58Z

← Older revision		Revision as of 08:36, 7 July 2022
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	'''Windows:''' On a windows machine Mobaxterm can be used to connect to Pipeline. For details, see ...		'''Windows:''' On a windows machine Mobaxterm can be used to connect to Pipeline. For details, see ...

	'''Linux/Unix:''' On a linux/Mac the ssh commands can be used directly through the terminal:		'''Linux/Unix:''' On a linux/Mac, the guest account will be used for people to log in as Tohban. Rather than using a password, access will be tied to specific computers that you use. One needs to generate a public + private ssh key pair using ssh-keygen or equivalent program that will result in a public key (plain text) file called id_rsa.pub, created in your ~/.ssh folder, the contents of which can be emailed to Dale or Owen to be added under "authorized keys". The ssh commands can then be used directly through the terminal:

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">

	ssh -L 5902:helios.solar.pvt:20000 guest@ovsa.njit.edu ### ~~when prompted, enter~~ password ~~to guest@ovsa~~ ###		ssh -L 5902:helios.solar.pvt:20000 guest@ovsa.njit.edu ### will not ask for a password for your computer's authorized key ###
	ssh -XY your_username@pipeline ### add your username and enter password to your pipeline account, when prompted ###		ssh -XY your_username@pipeline ### add your username and enter password to your pipeline account, when prompted ###
	</pre>		</pre>
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	# ============ Prior definitions for spectral windows, antennas, pixel numbers =========		# ============ Prior definitions for spectral windows, antennas, pixel numbers =========
	spws=[str(s+1) for s in range(30)] # spws=[str(s+1) for s in range(49)] # For post-2020 data		spws=[str(s+1) for s in range(30)] ###spws=[str(s+1) for s in range(49)] # For post-2020 data
	antennas='0~12&0~12'		antennas='0~12&0~12'
	npix=512		npix=512
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	hf.imreg(vis=slfcalms,imagefile=im_init+'.image.pbcor',fitsfile=im_init+'.fits',		hf.imreg(vis=slfcalms,imagefile=im_init+'.image.pbcor',fitsfile=im_init+'.fits',
	timerange=trange,usephacenter=False,verbose=True)		timerange=trange,usephacenter=False,verbose=True)
	clnjunks = ['.flux', '.mask', '.model', '.psf', '.residual','.sumwt','.pb','.image'] #Do not run the next 4 lines if needed to view and assess the subset of clean process images		clnjunks = ['.flux', '.mask', '.model', '.psf', '.residual','.sumwt','.pb','.image'] ###Do not run the next 4 lines if needed to view and assess the subset of clean process images
	for clnjunk in clnjunks:		for clnjunk in clnjunks:
	if os.path.exists(im_init + clnjunk):		if os.path.exists(im_init + clnjunk):
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	for n in range(nround):		for n in range(nround):
	slfcal_tb_g= calprefix+'.G'+str(n)		slfcal_tb_g= calprefix+'.G'+str(n)
	fig = plt.figure(figsize=(8.4,7.)) # fig = plt.figure(figsize=(14, 7)) # For post-2020 data (50 spws)		fig = plt.figure(figsize=(8.4,7.)) # fig = plt.figure(figsize=(14, 7)) # For post-2020 data (50 spws)
	gs = gridspec.GridSpec(5, 6) # gs = gridspec.GridSpec(5, 10) # For post-2020 data (50 spws)		gs = gridspec.GridSpec(5, 6) # gs = gridspec.GridSpec(5, 10) # For post-2020 data (50 spws)
	for s,sp in enumerate(spws):		for s,sp in enumerate(spws):
	print 'processing spw: '+sp		print 'processing spw: '+sp
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	# only the first round uses nearby spws for getting initial model		# only the first round uses nearby spws for getting initial model
	if n == 0:		if n == 0:
	spbg=max(int(sp)-2,1) # spbg=max(int(sp)-2,0) # For post-2020 data (50 spws)		spbg=max(int(sp)-2,1) # spbg=max(int(sp)-2,0) # For post-2020 data (50 spws)
	sped=min(int(sp)+2,30) # sped=min(int(sp)+2,49) # For post-2020 data (50 spws)		sped=min(int(sp)+2,30) # sped=min(int(sp)+2,49) # For post-2020 data (50 spws)
	spwran=str(spbg)+'~'+str(sped)		spwran=str(spbg)+'~'+str(sped)
	print('using spw {0:s} as model'.format(spwran))		print('using spw {0:s} as model'.format(spwran))
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	ax.set_xlim(xran)		ax.set_xlim(xran)
	ax.set_ylim(yran)		ax.set_ylim(yran)
	plt.pause(0.5) # Allows viewing of each image as it is plotted.		plt.pause(0.5) # Allows viewing of each image as it is plotted.
	os.system('rm -f '+ fitsfile)		os.system('rm -f '+ fitsfile)

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	sp_e=int(sp)+2		sp_e=int(sp)+2
	sp_i=int(sp)-2		sp_i=int(sp)-2
	if sp_i < 1: # if sp < 0: # For post-2020 data (50 spws)		if sp_i < 1: # if sp < 0: # For post-2020 data (50 spws)
	sp_i = 1 # sp_i = 0 # For post-2020 data (50 spws)		sp_i = 1 # sp_i = 0 # For post-2020 data (50 spws)
	if sp_e > 30: # if sp_e > 49: # For post-2020 data (50 spws)		if sp_e > 30: # if sp_e > 49: # For post-2020 data (50 spws)
	sp_e = 30 # sp_e = 49 # For post-2020 data (50 spws)		sp_e = 30 # sp_e = 49 # For post-2020 data (50 spws)
	sp_=str(sp_i)+'~'+str(sp_e)		sp_=str(sp_i)+'~'+str(sp_e)
	try:		try:
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	subplot=431,plotrange=[-1,-1,0,2.],iteration='antenna',figfile=slfcal_tb_g+'.png',showgui=False)		subplot=431,plotrange=[-1,-1,0,2.],iteration='antenna',figfile=slfcal_tb_g+'.png',showgui=False)
	os.chdir(workdir)		os.chdir(workdir)
	plt.pause(0.5) # Allows viewing of the plot		plt.pause(0.5) # Allows viewing of the plot


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	fitsfiles.append(fitsfile)		fitsfiles.append(fitsfile)

	fig = plt.figure(figsize=(8.4,7.)) # fig = plt.figure(figsize=(14, 7)) # For post-2020 data (50 spws)		fig = plt.figure(figsize=(8.4,7.)) # fig = plt.figure(figsize=(14, 7)) # For post-2020 data (50 spws)
	gs = gridspec.GridSpec(5, 6) # gs = gridspec.GridSpec(5, 10) # For post-2020 data (50 spws)		gs = gridspec.GridSpec(5, 6) # gs = gridspec.GridSpec(5, 10) # For post-2020 data (50 spws)
	for s,sp in enumerate(spws):		for s,sp in enumerate(spws):
	cfreq=cfreqs[int(sp)]		cfreq=cfreqs[int(sp)]

Schhabra at 08:22, 7 July 2022

2022-07-07T08:22:34Z

← Older revision		Revision as of 08:22, 7 July 2022
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	</pre>		</pre>

	[[file:Figure1_imagingtutorial.png\|thumb\|right\|~~250px~~\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]		[[file:Figure1_imagingtutorial.png\|thumb\|right\|300px\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]

	==== Step 3: Calibration ====		==== Step 3: Calibration ====
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	[[file:Figure2_imagingtutorial.png\|thumb\|right\|~~250px~~\|Figure 3: Full-Sun image after initial clean to find the flare location.]]		[[file:Figure2_imagingtutorial.png\|thumb\|right\|300px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]
	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 1, doing a full-Sun image to find out phasecenter and appropriate field of view =========		# =========== Step 1, doing a full-Sun image to find out phasecenter and appropriate field of view =========
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	</pre>		</pre>

	[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|~~250px~~\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]		[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|300px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]
	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 2 (optional), generate masks =========		# =========== Step 2 (optional), generate masks =========
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	</pre>		</pre>

	[[file:Slf.G0.png\|thumb\|right\|~~250px~~\|Figure 5: Phase before self-calibration]]		[[file:Slf.G0.png\|thumb\|right\|300px\|Figure 5: Phase before self-calibration]]
	[[file:Slf.G1.png\|thumb\|right\|~~250px~~\|Figure 6: Phase after self-calibration]]		[[file:Slf.G1.png\|thumb\|right\|300px\|Figure 6: Phase after self-calibration]]
	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 3, main step of selfcalibration =========		# =========== Step 3, main step of selfcalibration =========
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	</pre>		</pre>

	[[file:Slf_t0_n0.png\|thumb\|right\|~~250px~~\|Figure 7: Multi-frequency images before self-calibration]]		[[file:Slf_t0_n0.png\|thumb\|right\|300px\|Figure 7: Multi-frequency images before self-calibration]]
	[[file:Slf_t0_n1.png\|thumb\|right\|~~250px~~\|Figure 8: Multi-frequency images after self-calibration]]		[[file:Slf_t0_n1.png\|thumb\|right\|300px\|Figure 8: Multi-frequency images after self-calibration]]

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">

Schhabra at 11:47, 6 July 2022

2022-07-06T11:47:22Z

← Older revision		Revision as of 11:47, 6 July 2022
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	===Advanced Calibration and Imaging===		===Advanced Calibration and Imaging===
	====Step 4: Self-calibration====		====Step 4: Self-calibration====
	[[file:Figure3_imagingtutorial.png\|thumb\|~~right~~\|~~250px~~\|Figure 2: Cotton-Schwab clean major and minor cycles. [Source: http://www.aoc.nrao.edu/~rurvashi/ImagingAlgorithmsInCasa/node2.html].]]		[[file:Figure3_imagingtutorial.png\|thumb\|center\|400px\|Figure 2: Cotton-Schwab clean major and minor cycles. [Source: http://www.aoc.nrao.edu/~rurvashi/ImagingAlgorithmsInCasa/node2.html].]]
	Follow the steps below to run the self-calibration of the imaging data and produce the calibrated images in .fits format. https://github.com/binchensun/casa-eovsa/blob/master/slfcal_example.py		Follow the steps below to run the self-calibration of the imaging data and produce the calibrated images in .fits format. https://github.com/binchensun/casa-eovsa/blob/master/slfcal_example.py

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	npix=512		npix=512
	nround=3 #number of slfcal cycles		nround=3 #number of slfcal cycles
			</pre>


			[[file:Figure2_imagingtutorial.png\|thumb\|right\|250px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]
			<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 1, doing a full-Sun image to find out phasecenter and appropriate field of view =========		# =========== Step 1, doing a full-Sun image to find out phasecenter and appropriate field of view =========
	if dofullsun:		if dofullsun:
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	plt.show()		plt.show()
	viewer(im_init+'.image.pbcor')		viewer(im_init+'.image.pbcor')
	~~</pre>~~
	~~[[file:Figure2_imagingtutorial.png\|thumb\|right\|250px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]~~
	[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|250px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]
	~~<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">~~
	# parameters specific to the event (found from step 1)		# parameters specific to the event (found from step 1)
	phasecenter='J2000 10h02m59 11d58m07' ###Change accordingly###		phasecenter='J2000 10h02m59 11d58m07' ###Change accordingly###
	xran=[280,480] ###Change accordingly###		xran=[280,480] ###Change accordingly###
	yran=[-50,150] ###Change accordingly###		yran=[-50,150] ###Change accordingly###
			</pre>

			[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|250px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]
			<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 2 (optional), generate masks =========		# =========== Step 2 (optional), generate masks =========
			# The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window. The instructions for doing this can be found by hovering over those icons. See Figure 4.
	# if skipped, will not use any masks		# if skipped, will not use any masks
	if domasks:		if domasks:
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	</pre>		</pre>

			[[file:Slf.G0.png\|thumb\|right\|250px\|Figure 5: Phase before self-calibration]]
	~~The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window~~. ~~The instructions for doing this can be found by hovering over those icons~~. ~~See~~ Figure 4.		[[file:Slf.G1.png\|thumb\|right\|250px\|Figure 6: Phase after self-calibration]]

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# =========== Step 3, main step of selfcalibration =========		# =========== Step 3, main step of selfcalibration =========
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	split(ms_in, ms_slfcaled,datacolumn='corrected')		split(ms_in, ms_slfcaled,datacolumn='corrected')
	</pre>		</pre>
	[[file:~~Slf.G0~~.png\|thumb\|right\|250px\|Figure 1: ~~Phase~~ before self-calibration]]
	[[file:~~Slf.G1~~.png\|thumb\|right\|250px\|Figure 2: ~~Phase~~ after self-calibration]]		[[file:Slf_t0_n0.png\|thumb\|right\|250px\|Figure 7: Multi-frequency images before self-calibration]]
			[[file:Slf_t0_n1.png\|thumb\|right\|250px\|Figure 8: Multi-frequency images after self-calibration]]

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
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	The .fits files of the self calibrated images at each frequency for the given time are saved at /slfcal/images_slfcaled in your working directory.		The .fits files of the self calibrated images at each frequency for the given time are saved at /slfcal/images_slfcaled in your working directory.

	~~[[file:Slf_t0_n0.png\|thumb\|right\|250px\|Figure 3: Multi-frequency images before self-calibration]]~~
	~~[[file:Slf_t0_n1.png\|thumb\|right\|250px\|Figure 4: Multi-frequency images after self-calibration]]~~

	====Step 5: Quick-look imaging ==== <!-- ====Step 6: Making the full set of images==== -->		====Step 5: Quick-look imaging ==== <!-- ====Step 6: Making the full set of images==== -->

Schhabra at 11:36, 6 July 2022

2022-07-06T11:36:33Z

← Older revision		Revision as of 11:36, 6 July 2022
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	</pre>		</pre>
	[[file:Figure2_imagingtutorial.png\|thumb\|right\|250px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]		[[file:Figure2_imagingtutorial.png\|thumb\|right\|250px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]
			[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|250px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]
	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
	# parameters specific to the event (found from step 1)		# parameters specific to the event (found from step 1)
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	pickle.dump(masks,open(slfcaldir+'masks.p','wb'))		pickle.dump(masks,open(slfcaldir+'masks.p','wb'))
	</pre>		</pre>
	[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|250px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]

	The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window. The instructions for doing this can be found by hovering over those icons.
			The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window. The instructions for doing this can be found by hovering over those icons. See Figure 4.

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">

Schhabra at 11:34, 6 July 2022

2022-07-06T11:34:13Z

← Older revision		Revision as of 11:34, 6 July 2022
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	vis = calibeovsa.calibeovsa(msfiles, doconcat=True, concatvis=concatvis, caltype=['refpha','phacal'], doimage=True)		vis = calibeovsa.calibeovsa(msfiles, doconcat=True, concatvis=concatvis, caltype=['refpha','phacal'], doimage=True)
	### If doimage=True, a quicklook image will be produced (by integrating over the entire time) as shown ~~below~~ ###		### If doimage=True, a quicklook image will be produced (by integrating over the entire time) as shown in Figure 1 ###

	vis_str = str(' '.join(vis))		vis_str = str(' '.join(vis))
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	</pre>		</pre>

	[[file:Figure1_imagingtutorial.png\|thumb\|right\|~~350px~~\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]		[[file:Figure1_imagingtutorial.png\|thumb\|right\|250px\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]

	==== Step 3: Calibration ====		==== Step 3: Calibration ====
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	vis_str = str(' '.join(vis))		vis_str = str(' '.join(vis))
	caled_vis=vis_str.replace('.ms','_cal.ms') ### Append '_cal' to the ms filename ###		caled_vis=vis_str.replace('.ms','_cal.ms') ### Append '_cal' to the ms filename ###

	split(vis=' '.join(vis),outputvis=caled_vis,datacolumn='corrected',timerange='',correlation='XX') ### Split the corrected column to the new 'caled' ms ###		split(vis=' '.join(vis),outputvis=caled_vis,datacolumn='corrected',timerange='',correlation='XX') ### Split the corrected column to the new 'caled' ms ###
	</pre>		</pre>
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	===Advanced Calibration and Imaging===		===Advanced Calibration and Imaging===
	====Step 4: Self-calibration====		====Step 4: Self-calibration====
	[[file:Figure3_imagingtutorial.png\|thumb\|~~center~~\|~~500px~~\|Figure 2: Cotton-Schwab clean major and minor cycles. [Source: http://www.aoc.nrao.edu/~rurvashi/ImagingAlgorithmsInCasa/node2.html].]]		[[file:Figure3_imagingtutorial.png\|thumb\|right\|250px\|Figure 2: Cotton-Schwab clean major and minor cycles. [Source: http://www.aoc.nrao.edu/~rurvashi/ImagingAlgorithmsInCasa/node2.html].]]
	Follow the below ~~given steps~~ to run the self-calibration of the imaging data and produce the calibrated images in .fits format. https://github.com/binchensun/casa-eovsa/blob/master/slfcal_example.py		Follow the steps below to run the self-calibration of the imaging data and produce the calibrated images in .fits format. https://github.com/binchensun/casa-eovsa/blob/master/slfcal_example.py

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
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	viewer(im_init+'.image.pbcor')		viewer(im_init+'.image.pbcor')
	</pre>		</pre>
	[[file:Figure2_imagingtutorial.png\|thumb\|~~center~~\|~~500px~~\|Figure 3: Full-Sun image after initial clean to find the flare location.]]		[[file:Figure2_imagingtutorial.png\|thumb\|right\|250px\|Figure 3: Full-Sun image after initial clean to find the flare location.]]

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
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	pickle.dump(masks,open(slfcaldir+'masks.p','wb'))		pickle.dump(masks,open(slfcaldir+'masks.p','wb'))
	</pre>		</pre>
	[[file:Figure4_imagingtutorial.PNG\|thumb\|~~center~~\|~~800px~~\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]		[[file:Figure4_imagingtutorial.PNG\|thumb\|right\|250px\|Figure 4: Interactive clean window to create masks over the source. The white outline surrounding the source is the mask selected by the polygon drawing option.]]

	The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window. The instructions for doing this can be found by hovering over those icons.		The outlines drawn for masks can be created by any of the icons with the letter 'R' in the Viewer window. The instructions for doing this can be found by hovering over those icons.
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	split(ms_in, ms_slfcaled,datacolumn='corrected')		split(ms_in, ms_slfcaled,datacolumn='corrected')
	</pre>		</pre>
	[[file:Slf.G0.png\|thumb\|~~center~~\|~~500px~~\|Figure 1: Phase before self-calibration]]		[[file:Slf.G0.png\|thumb\|right\|250px\|Figure 1: Phase before self-calibration]]
	[[file:Slf.G1.png\|thumb\|~~center~~\|~~500px~~\|Figure 2: Phase after self-calibration]]		[[file:Slf.G1.png\|thumb\|right\|250px\|Figure 2: Phase after self-calibration]]

	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
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	The .fits files of the self calibrated images at each frequency for the given time are saved at /slfcal/images_slfcaled in your working directory.		The .fits files of the self calibrated images at each frequency for the given time are saved at /slfcal/images_slfcaled in your working directory.

	[[file:Slf_t0_n0.png\|thumb\|~~center~~\|~~500px~~\|Figure 3: Multi-frequency images before self-calibration]]		[[file:Slf_t0_n0.png\|thumb\|right\|250px\|Figure 3: Multi-frequency images before self-calibration]]
	[[file:Slf_t0_n1.png\|thumb\|~~center~~\|~~500px~~\|Figure 4: Multi-frequency images after self-calibration]]		[[file:Slf_t0_n1.png\|thumb\|right\|250px\|Figure 4: Multi-frequency images after self-calibration]]

	====Step 5: Quick-look imaging ==== <!-- ====Step 6: Making the full set of images==== -->		====Step 5: Quick-look imaging ==== <!-- ====Step 6: Making the full set of images==== -->

Schhabra at 11:27, 6 July 2022

2022-07-06T11:27:29Z

← Older revision		Revision as of 11:27, 6 July 2022
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	</pre>		</pre>

	[[file:Figure1_imagingtutorial.png\|~~frame~~\|~~center~~\|~~800px~~\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]		[[file:Figure1_imagingtutorial.png\|thumb\|right\|350px\|'''Figure 1:''' Quick-look full-Sun image after the initial calibration.]]

	==== Step 3: Calibration ====		==== Step 3: Calibration ====

Schhabra at 11:24, 6 July 2022

2022-07-06T11:24:21Z

← Older revision		Revision as of 11:24, 6 July 2022
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	<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">		<pre style="background-color: #FCEBD9;overflow: auto;width: auto;">
			bash
			loadcasa5
			suncasa


	from suncasa.utils import helioimage2fits as hf		from suncasa.utils import helioimage2fits as hf
	import os		import os