Sunspot Band6 SingleDish for CASA 6.5.4: Difference between revisions
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==Imaging== | ==Imaging== | ||
[[File: | [[File:sunspot_fullsun_spw3_PM03_CASA_6.5.4.png|thumb|right|'''Fig. 1.''' The full-sun image in Band6 observed with PM03, spw 3.]] | ||
Here we image the full sun map of spectral window (spw) 3 obtained with the PM03 antenna using {{tsdimaging_6.5.4}}. | Here we image the full sun map of spectral window (spw) 3 obtained with the PM03 antenna using {{tsdimaging_6.5.4}}. | ||
Revision as of 21:51, 11 April 2024
Last checked on CASA Version 6.5.4
Overview
This guide features CARTA, the “Cube Analysis and Rendering Tool for Astronomy,” which is the new NRAO visualization tool for images and cubes. The CASA viewer (imview) has not been maintained for a few years and will be removed from future versions of CASA. We strongly recommend using CARTA, as it provides a much more efficient, stable, and feature rich user experience. A comparison of the CASA viewer and CARTA, as well as instructions on how to use CARTA at NRAO, is provided in the CARTA section of the CASA docs.
This portion of the Sunspot Band6 guide will cover the calibration and imaging of the data obtained with the Total Power array. We create the map of a full Sun with Band6.
Import the data and split into the files for each antenna
If you completed the calibration of the visibility data following Sunspot_Band6_Calibration_for_CASA_6.5.4, we assume you are working in the directory 'Sunspot_Band6_UncalibratedData'. After starting CASA, we start by defining the directory name of the ASDM and Measurement Set.
#In CASA
sd_asdm = 'uid___A002_Xae00c5_X2e6b' # single dish ASDM file
sd_mso = sd_asdm+'.ms' # measurement set original
sd_msc = sd_asdm+'.ms'+'.split.cal' # measurement set calibrated
ant = 'PM03' # antenna
In this tutorial, we will use the data obtained with the PM03 antenna.
First we will need to convert the data to MS format. This is done with the task importasdm.
#In CASA
importasdm(asdm=sd_asdm, with_pointing_correction=True, verbose=True, vis=sd_mso, overwrite=True)
Then we get some basic information about the data using listobs.
#In CASA
listobs(vis=sd_mso, listfile=sd_asdm+'.listobs.txt')
Observer: lknee Project: uid://A002/X5ca254/X1
Observation: ALMA
Data records: 6336672 Total elapsed time = 578.744 seconds
Observed from 18-Dec-2015/20:11:02.7 to 18-Dec-2015/20:20:41.4 (UTC)
ObservationID = 0 ArrayID = 0
Date Timerange (UTC) Scan FldId FieldName nRows SpwIds Average Interval(s) ScanIntent
18-Dec-2015/20:11:02.7 - 20:11:52.8 1 0 Sun 276480 [0,1,2,3,4,5,6,7] [0.001, 0.001, 0.001, 0.001, 0.001, 0.001, 0.001, 0.001] [CALIBRATE_ATMOSPHERE#AMBIENT,CALIBRATE_ATMOSPHERE#HOT,CALIBRATE_ATMOSPHERE#OFF_SOURCE,CALIBRATE_ATMOSPHERE#REFERENCE]
20:12:14.4 - 20:20:41.4 2 0 Sun 6060192 [0,1,2,3] [0.001, 0.001, 0.001, 0.001] [OBSERVE_TARGET#OFF_SOURCE,OBSERVE_TARGET#ON_SOURCE]
(nRows = Total number of rows per scan)
Fields: 1
ID Code Name RA Decl Epoch SrcId nRows
0 none Sun 17:44:08.590935 -23.23.12.63602 ICRS 0 6336672
Spectral Windows: (8 unique spectral windows and 1 unique polarization setups)
SpwID Name #Chans Frame Ch0(MHz) ChanWid(kHz) TotBW(kHz) CtrFreq(MHz) BBC Num Corrs
0 BB_1#SQLD 1 TOPO 230000.000 2000000.000 2000000.0 230000.0000 1 XX YY
1 BB_2#SQLD 1 TOPO 232000.000 2000000.000 2000000.0 232000.0000 2 XX YY
2 BB_3#SQLD 1 TOPO 246000.000 2000000.000 2000000.0 246000.0000 3 XX YY
3 BB_4#SQLD 1 TOPO 248000.000 2000000.000 2000000.0 248000.0000 4 XX YY
4 BB_1#SQLD 1 TOPO 219559.000 2000000.000 2000000.0 219559.0000 1 XX YY
5 BB_2#SQLD 1 TOPO 219559.000 2000000.000 2000000.0 219559.0000 2 XX YY
6 BB_3#SQLD 1 TOPO 219559.000 2000000.000 2000000.0 219559.0000 3 XX YY
7 BB_4#SQLD 1 TOPO 219559.000 2000000.000 2000000.0 219559.0000 4 XX YY
Sources: 8
ID Name SpwId RestFreq(MHz) SysVel(km/s)
0 Sun 0 - -
0 Sun 1 - -
0 Sun 2 - -
0 Sun 3 - -
0 Sun 4 - -
0 Sun 5 - -
0 Sun 6 - -
0 Sun 7 - -
Antennas: 3:
ID Name Station Diam. Long. Lat. Offset from array center (m) ITRF Geocentric coordinates (m)
East North Elevation x y z
0 PM02 T702 12.0 m -067.45.18.6 -22.53.24.1 -23.6242 -582.3080 22.0682 2225042.276282 -5440125.514185 -2481574.899005
1 PM03 T701 12.0 m -067.45.18.8 -22.53.22.2 -29.1260 -522.7876 22.2057 2225045.996268 -5440149.142221 -2481520.118897
2 PM04 T703 12.0 m -067.45.16.2 -22.53.23.9 42.8802 -575.6911 21.7765 2225104.701297 -5440102.471920 -2481568.689682
Calibration
In the observation, the atmospheric calibration scan (1) was done before the fast-scanning of the Sun (2). We derive calibrations for position switching (ps) and system temperature (Tsys) from the calibration scan, and apply them to the science data using calmode='ps,tsys,apply' in sdcal.
#In CASA
sdcal(infile=sd_mso, calmode='ps,tsys,apply', spw='0,1,2,3')
split(vis=sd_mso, spw='0,1,2,3', outputvis=sd_msc, scan='2', datacolumn='corrected')
Unlike non-solar single-dish observations, the flux calibrator is not observed in solar single-dish observations in Cycle 4. Therefore, we have to calibrate the data using a correction factor which includes various antenna efficiencies of the PM antenna.
Based on the commissioning observations, the average correction factor of the PM antennas with Band6 is 0.862, which enables us to calibrate the observed antenna temperature to the absolute brightness temperature. We will create the calibration table using this value in gencal and apply the table with applycal as follows:
#In CASA
gencal(vis=sd_msc, caltable=sd_asdm+'.cal.eff.tbl', caltype='amp', parameter=[0.862**0.5])
applycal(vis=sd_msc, gaintable=sd_asdm+'.cal.eff.tbl')
Caution: The correction factor in this document is written in White et al. (2017)
Imaging
Here we image the full sun map of spectral window (spw) 3 obtained with the PM03 antenna using tsdimaging.
#In CASA
sd_img = sd_asdm+'.'+ant+'.StkI.Spw3'
tsdimaging(infiles=sd_msc, spw='3', antenna=ant, field='0', nchan=1, cell=['3.0arcsec','3.0arcsec'],
outfile=sd_img, imsize=[800,800], gridfunction='SF', convsupport=6, intent='*ON_SOURCE*', stokes='I')
After this has finished, you should now open the image in CARTA. If using NRAO machines, you can open a new terminal tab, cd to the working directory, then type:
#In bash
carta --no_browser
Copy the output URL into a browser to view your CARTA session. You can see the full-sun image as shown in Figure 1. Select and load:
uid___A002_Xae00c5_X2e6b.PM03.StkI.Spw3
When you carry out the imaging of Band3 data, we recommend the following parameters instead:
#In CASA
tsdimaging(infiles=sd_msc, spw='3', antenna=ant, field='0', nchan=1, cell=['6.0arcsec','6.0arcsec'],
outfile=sd_img, imsize=[400,400], gridfunction='SF', convsupport=6, intent='*ON_SOURCE*', stokes='I')
Calibration (re-scaling) after Imaging
White et al. (2017) recommended that the standard ALMA single-dish image products be scaled to match their best determination of quiet-Sun temperatures at disk center (specifically, 5900 K averaged over an 80″-square region centered on the apparent disk center at Band 6, and 7300 K averaged over a 120″-square region centered on the apparent disk center at Band 3, with uncertainties of about 100 K). For the re-scaling, the following commands are executed.
#In CASA
res = imstat(sd_img+'.image', region='circle[[400pix,400pix],80pix]')
immath(imagename=sd_img+'.image', expr='IM0*'+str(5900./res['mean'][0]), outfile=sd_img+'.rescl')
For Band3:
#In CASA
res = imstat(sd_img+'.image', region='circle[[200pix,200pix],40pix]')
immath(imagename=sd_img+'.image', expr='IM0*'+str(7300./res['mean'][0]), outfile=sd_img+'.rescl')
Note: All full-sun images that are included in the SV data package (ex. Sunspot_Band6_ReferenceImages.tgz) were not applied the re-scaling because the SV data were released before publishing White et al. (2017). When you use the full-sun image of the SV data for your studies, you should be done the re-scaling process. While the archive data obtained in Cycles were applied the re-scaling process.
