Difference between revisions of "Sunspot Band6 Feathering for CASA 5.1"
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Revision as of 00:37, 5 February 2018
This portion of the Sunspot Band6 CASA Guide for CASA 5.1 covers the combine process between the synthesized solar image and the full-sun image obtained with TP array. It begins where the calibration of the visibility data and single-dish data, image synthesis, and creating of the full-sun map are completed. If you do not complete them, at first,
1) Download the file of the un-calibrated data package ‘Sunspot_Band6_UncalibratedData.tgz’, do the calibration of the data, and create the images from the interferometric data and single-dish data, along with the ‘Sunspot_Band6_*_for_CASA_5.1’ tutorials.
2) Download the file of the calibrated data package ‘Sunspot_Band6_CalibratedData.tgz’, and synthesize the image from interferometric data along the ‘Sunspot_Band6_Imaging_for_CASA_5.1’ tutorial.
In case 1), we assume that you are working on the working directory ‘Sunspot_Band6_UncalibratedData’. On the other hand, when you started the tutorial from the calibrated package (case 2), we assume that the working directory is ‘Sunspot_Band6_CalibratedData.’
From next, we will show all commands for combining the images.
Obtaining the RA/Dec coordinate of the sun center at the reference time
Before starting the combination process on CASA, we need to know the RA/Dec coordinate of the sun center at the reference time that is used for the image synthesis, because the observing time of the TP-array is not the same as the reference time exactly. The Sun was moving on the RA/Dec coordinate frame during the gap between the times. To combine the synthesized image with the full-sun image obtained from the TP array, we need to shift the coordinate of the full-sun image based on the coordinate of the sun center at the reference time. Hence, we obtain the solar coordinate from the JPL’s HORIZONS system.
The reference time in this tutorial is 19:49:00UT, December 18 2015. At the time, the RA/Dec coordinate of the sun center estimated by JPL’s HORIZONS system is RA: 266.01898 degree, Dec: -23.38648 degrees.
Preparation for Feathering task: The Single-Dish data
We start the process on CASA by defining some names of the data.
# In Casa int_base = 'AR12470_B6AllSpw_I' # basename of the synthesized image sd_img_base = 'uid___A002_Xae00c5_X2e6b.PM03.StkI.Spw3' # basename of the full-sun map out_base = 'AR12470_B6AllSpe_I_Feather' # basename of the final products
</figure> <figure id="sdspot">
</figure> We shift the coordinate of the full-sun map created from the single-dish data, based on the RA/Dec coordinate obtained in the previous section, as follows.
# In Casa sun_ra = str(266.01898 * pi/180.) sun_dec = str(-23.38648 * pi/180.) imhead(imagename = sd_img_base+'.rescl', mode = 'put', hdkey = 'crval1', hdvalue = sun_ra) imhead(imagename = sd_img_base+'.rescl', mode = 'put', hdkey = 'crval2', hdvalue = sun_dec)
The unit of the full-sun map is Kelvin. On the other hand, the unit of the synthesized image is Jy/beam. So, the conversion of the unit has to be done. In the tutorial, we convert the unit of the full-sun image to Jy/beam, using the following commands.
# In Casa crval4S= imhead(sd_img_base+'.rescl', mode='get',hdkey='crval4') freqSD = crval4S.values() sbema = imhead(sd_img_base+'.rescl', mode='get',hdkey='beammajor') sbemi = imhead(sd_img_base+'.rescl', mode='get',hdkey='beamminor') sbmajor = sbema.values() sbminor = sbemi.values() convKJb = str(13.6 * (300./(freqSD/1.e9))**2. * (1./sbmajor)*(1./sbminor)) immath(imagename=sd_img_base+'.rescl', expr='IM0/'+convKJb, outfile=sd_img_base+'.jyb.im') imhead(imagename = sd_img_base+'.jyb.im', mode = 'put', hdkey = 'crval3', hdvalue = ['I']) imhead(imagename = sd_img_base+'.jyb.im', mode = 'put', hdkey = 'bunit', hdvalue = 'Jy/beam')
The result of the process is shown in <xr id="fullsun" />. A look of the image is not changed, but you can find the changing of the values and unit from the <xr id="fullsun" /> in ‘Sunspot_Band6_SingleDish_for_CASA_4.7’ tutorial.
Then we do the re-gridding and trimming to fit the map area to that of the synthesized image. The area of the trimming is set to the same as the CLEAN box, in the tutorial.
# In Casa #re-griding of SD data imregrid(imagename=sd_img_base+'.jyb.im', template=int_base+'.image', axes=[0, 1], output=sd_img_base+'.jyb.regrid') # Trimming to exclude noisy edge regions in the TP image imsubimage(imagename=sd_img_base+'.jyb.regrid', outfile=sd_img_base+'.jyb.regrid.subim', box='555,565,1505,1490')
As the final process of the preparation of the single-dish data, we multiply the trimmed image by the primary beam response, as follows.
# In Casa imsubimage(imagename=int_base+'.flux',outfile=int_base+'.flux.subim',box='555,565,1505,1490') immath(imagename=[sd_img_base+'.jyb.regrid.subim',int_base+'.flux.subim'], expr='IM0*IM1', outfile=sd_img_base+'.jyb.regrid.subim.depb')
Preparation for Feathering task: The Synthesized image
</figure> To fit the map area to that of the trimmed single-dish image, we do the trimming for the synthesized image.
# In Casa imsubimage(imagename=int_base+'.image', outfile=int_base+'.image.subim', box='555,565,1505,1490')
Combining, primary beam correction, and creating of the FITS file.
The combining of the maps can be done using ‘feathering’ task, as the same as the non-solar data.
CAUTION: In this tutorial and the packages of the solar SV data released on 2017/01/18, we use the default parameters of the task, as shown above. As a result, the averaged brightness temperature of the combined image is always larger a few % than the temperature brightness at the same position in the single-dish map, although the values have to be the same basically. It means that you need to tune the “sdfactor" parameter of the task for obtaining consistent images, before using combined images for your science. The detail of the parameter is described in Section 5.6 of “CASA User Reference & Cookbook Release 4.7.0”.
After the feathering process, we do the primary beam correction, as follows.
# In Casa impbcor(imagename=out_base+'.image', pbimage=int_base+'.flux.subim', outfile=out_base+'.pbcor', mode='divide')
To convert the unit from Jy/beam to Kelvin, we use the following commands. <figure id="final">
# In Casa crval4I= imhead(int_base+'.image', mode='get',hdkey='crval4') freq = crval4I.values() fbema = imhead(out_base+'.image', mode='get',hdkey='beammajor') fbemi = imhead(out_base+'.image', mode='get',hdkey='beamminor') fbmajor = fbema.values() fbminor = fbemi.values() convKJb2 = str(13.6 * (300./(freq/1.e9))**2. * (1./fbmajor)*(1./fbminor)) immath(imagename=out_base+'.pbcor',expr='IM0*'+convKJb2, outfile= out_base+'_K.pbcor') imhead(imagename = out_base+'_K.pbcor', mode = 'put', hdkey = 'bunit', hdvalue = 'K')
Finally, we create the FITS file of the combined and primary corrected map.
# In Casa exportfits(imagename=out_base+'_K.pbcor', fitsimage=out_base+'_K.fits')
The result of the combining is shown in <xr id="final" /> .