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This README file contains a description of the sunspot ALMA, EOC,
test data, scripts, and data products. 

Spectral windows include polarized continuum emission. 

The observations were done using configurations C-3 for band 3 on October 13, 2022.

The approximate resolution for band 3 is  ~2.0 x 1.4 arcseconds in band 3.

Additional information can be found in the comments section
included in this README.

The Calibrated Data and Reference Images provided here were produced using CASA version 6.4

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SunPol_Sunspot_Scripts.tar.gz in the "Script" directory contains the calibration and imaging scripts

#Scripts for gain calibration
* X5b57.ms.scriptForCalibration.py
* X66bc.ms.scriptForCalibration.py
* sun_reduction_util.py
#Scripts for polarization calibration
* scriptForPolCalibration.py
#Reference script for sample images (Synthesized images)
* scriptForPolImaging.py
# Scripts for flux calibration of TP data
* scriptForSDCalibration.py
# Scripts for a sample image of TP data
* scriptForSDFullSunImaging.py
# Scripts for sample images (Feathering images)
* scriptForFeathering.py

<.tar.gz in the "Uncalibrated" directory contains the raw data:

Two MS datasets and one ASDM dataset:
# SolPol_Sunspot_X5b57.tar.gz
* SolPol_Sunspot_X5b57.ms (1st EB of the 12m-array observation)
# SolPol_Sunspot_X66bc.tar.gz
* SolPol_Sunspot_X66bc.ms (2nd EB of the 12m-array observation)
# SolPol_Sunspot_TP.tar.gz
* uid___A002_Xff99e1_X666b (The raw data of the TP-array observation) 

*.tar.gz in the "Calibrated" directory contains the calibrated data

Polarization calibrated MS
#SolPol_Sunspot_Calibrated_INT.tar.gz
* SolPol.ms.TDM.cal

Calibrated MS of the TP-array observation
#SolPol_Sunspot_Calibrated_TP.tar.gz
* uid___A002_Xff99e1_X666b.ms.split.cal

To produce this calibrated dataset, synthesized images, and feathering images, 
you will need to execute the calibration and imaging scripts after downloading and 
decompressing the uncalibrated and script files. 
The scripts have to be executed in the following order:

1) execfile('sun_reduction_util.py')
2) execfile('X5b57.ms.scriptForCalibration.py')
3) execfile('X66bc.ms.scriptForCalibration.py')
4) execfile('scriptForPolCalibration.py')
5) execfile('scriptForSDCalibration.py')
6) execfile('scriptForSDFullSunImaging.py')
7) execfile('scriptForFeathering.py')

Note 2) and 3) process takes over a night for each.

*.tar.gz in the "Products" directory contains the fits files

Synthesized full-Stokes images of each Field (without the PB correction)
# SolPol_Sunspot_IntImg.tar.gz
* SynthesizedImages/sunspot_fld??.StkI.fits  
* SynthesizedImages/sunspot_fld??.StkQ.fits  
* SynthesizedImages/sunspot_fld??.StkU.fits  
* SynthesizedImages/sunspot_fld??.StkV.fits  

FullSun map for the Feathring process
# SolPol_Sunspot_FullSun.tar.gz
* FullSun/uid___A002_Xff99e1_X666b.scn06.PM03.spw3.cont.manual.fits

Feathered  Stokes-I and circular polarization-degree map of each Field (with the PB correction)
# SolPol_Sunspot_fthImg.tar.gz
* FeatheringImage/sunspot_fld??.fth.Kpbcor.fits [Stokes-I: Unit 'K']
* FeatheringImage/sunspot_fld??.cpd.fits [Circular polarization degree: Unit '%']

??: Field ID

Caution: Although you can synthesize a MOSAIC map from the dataset, we never guarantee 
the quantities and quality of the MOSAIC map. We recommend using the map of each Field 
for your studies.

Comment1: The polarization observations with the TP-array were not established at the 
observation. Hence, we do not apply the feathering process to the Stokes-V maps, 
and the resolve-out occurs in the maps. As a result, for your studies, 
you should carefully consider the uncertainty of the circular polarization degree maps 
induced by the resolve-out. 

Comment2: The field center of the FIELDID#0 map is shfted from the other maps. 
          The values of the shift are roughly -1.52 arcsec with the RA direction, 
          and -0.45 arcsec with the DEC direction, estimated from the sunspot structures. 

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Publications making use of these data must include the following statement in the acknowledgment:

"This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00011.E. 
ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), 
together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), 
in cooperation with the Republic of Chile. The Joint ALMA Observatory is 
operated by ESO, AUI/NRAO and NAOJ."

In addition, publications from NA authors must include the standard NRAO acknowledgment:

"The National Radio Astronomy Observatory is a facility of the National 
Science Foundation operated under cooperative agreement by Associated 
Universities, Inc."