CASA Guides:VLBA Basic Phase-referencing Calibration and Imaging
This CASA Guide is for Version 6.4.0 of CASA. If you are using a later version of CASA and this is the most recent available guide, then you should be able to use most, if not all, of this tutorial.
Overview
This CASA Guide describes the procedure for calibrating a phase-referenced VLBA observation of the radio galaxy J1203+6031 (IVS 1200+608, ICRF3 J120303.5+603119). The data were taken specifically for this tutorial. The observation made use of the DDC observing personality, using dual polarization with 4 spectral windows per polarization. Each spectral window is has a bandwidth of 64 MHz, and is divided into 128 spectral channels.
This tutorial will focus on calibrating the data and creating continuum (Stokes I) images.
How to Use This CASA Guide
There are a number of possible ways to run CASA, described in more detail in Getting Started in CASA. In brief, there are at least three different ways to use CASA:
- Interactively examining task inputs. In this mode, one types taskname to load the task, inp to examine the inputs, and go once those inputs have been set to your satisfaction. Allowed inputs are shown in blue and bad inputs are colored red. The input parameters themselves are changed one by one, e.g., selectdata=True. Screenshots of the inputs to various tasks used in the data reduction below are provided, to illustrate which parameters need to be set. More detailed help can be obtained on any task by typing help taskname. Once a task is run, the set of inputs are stored and can be retrieved via tget taskname; subsequent runs will overwrite the previous tget file.
- Pseudo-interactively via task function calls. In this case, all of the desired inputs to a task are provided at once on the CASA command line. This tutorial is made up of such calls, which were developed by looking at the inputs for each task and deciding what needed to be changed from default values. For task function calls, only parameters that you want to be different from their defaults need to be set.
- Non-interactively via a script. A series of task function calls can be combined together into a script, and run from within CASA via execfile('scriptname.py'). This and other CASA Tutorial Guides have been designed to be extracted into a script via the script extractor by using the method described at the Extracting_scripts_from_these_tutorials page. Should you use the script generated by the script extractor for this CASA Guide, be aware that it will require some small amount of interaction related to the plotting, occasionally suggesting that you close the graphics window and hitting return in the terminal to proceed. It is in fact unnecessary to close the graphics windows (it is suggested that you do so purely to keep your desktop uncluttered).
If you are a relative novice or just new to CASA, it is strongly recommended to work through this tutorial by cutting and pasting the task function calls provided below after you have read all the associated explanations. Work at your own pace, look at the inputs to the tasks to see what other options exist, and read the help files. Later, when you are more comfortable, you might try to extract the script, modify it for your purposes, and begin to reduce other data.
Obtaining the Data
This Guide is intended to cover the entire process one would follow for calibrating their own VLBA observation. Therefore, we will start with a FITS-IDI file rather than a Measurement Set. The FITS-IDI file for this Guide is: PROVIDE LINK TO IDIFITS FILE HERE (file size 3.8 GB).
If users prefer, they may download the data from the NRAO Archive. In the archive search inputs, enter the project code "TL016" and look for the file VLBA_TL016B_tl016b_BIN0_SRC0_1_220307T210851.idifits. Once you have downloaded the FITS-IDI file, it may be useful to change the filename to "TL016B.idifits".
The Observation
Before diving into the calibration, it is always a good idea to look over the observing log to make check for notes from the operators that can inform us about potential issues with the data (missing stations, bad weather, etc.). These logs are always emailed to the PI's of an observation, but you can also access them later from the NRAO's vlbiobs fileserver. To locate an observing log, first find the directory for observing month and the last two digits of the year (for the observation used in this Guide, that directory is feb22 for February 2022). Once inside the proper month+year directory, look for the project code (in this case, tl016b). Look for a file named <project code>log.vbla (tl016blog.vlba).
The observing log for this particular observation looked like this:
VERY LONG BASELINE ARRAY OBSERVING LOG
--------------------------------------
Project: TL016B
Observer: Linford, J.
Project type: VLBA
Obs filename: t;016b.vex
Date/Day: 2022FEB21/052
Ants Scheduled: SC HN NL FD LA PT KP OV BR MK
=UT-Time===Comment===============================================MF#===%AD==AMD=
Operator is Betty Ragan
0559 Begin
0559 %SC raining
0559 %KP windy
1327 End.
Downtime Summary:
Total downtime : 0 min
Percentage downtime of observing: 0.0%
Average downtime per hour : 0.0 min
Total scheduled observing time (# Antennas): 4480 min (10)
Notes:
* = Entries where data was affected.
% = Entries where data may have been affected.
& = Entries where the site tech was called out.
WEA = Weather entries.
MF# = Maintenance form or major downtime category associated with a problem.
%AD = The percentage of an antenna affected by a problem.
AMD = Total antenna-minutes downtime for a problem.
Tsys = System Temperature (TP/SP x Tcal/2)
ACU = Antenna Control Unit
FRM = Focus/Rotation Mount
RFI = Radio Frequency Interference
VME = Site control computer
CB = Circuit Breaker
vclock = Program that compares site clock time to a standard.
There are no major issues reported by the operators for this observation and all ten antennas participated for the entire time (no downtime). However, there was rain at Saint Croix (SC) and it was windy at Kitt Peak (KP). We'll need to keep that in mind as we proceed with the calibration. We should pay special attention to SC and KP as we inspect the data and the calibration solutions we generate.
NOTE: This is an exceptionally good observing log! Most observations will have at least a small amount of downtime for various reasons.
Creating the Measurement Set
Before beginning our data reduction, we must start CASA. If you have not used CASA before, some helpful tips are available on the Getting Started in CASA page. Remember to start CASA in the directory containing the data.
Once you have CASA up and running, it is time to get the data into a format that CASA can use. Unlike VLA data, a VLBA observation is only available as a FITS-IDI file and cannot be downloaded as a CASA Measurement Set. So, the first step in calibrating a VLBA observation with CASA is to create a Measurement Set from the FITS-IDI file. To do this, we will use the task importfitsidi:
# In CASA
importfitsidi(fitsidifil='TL016B.idifits', vis='tl016b.ms', constobsid=True, scanreindexgap_s=15)
The scanreindexgap_s parameter is used to reconstruct scan boundaries in those cases where sources do not change between scans. In general, it is good to set scanreindexgap_s to some non-zero number to help CASA properly organize the scan list. The recommended value is 15, but shorter values may work as well (although you probably don't want to go much shorter than about 5 seconds). If you find that the resulting MS contains too few scans, run importfitsidi again with scanreindexgap_s set to a smaller number. If your MS has too many scans, especially multiple scans on the same source when you think it should just be one scan, run importfitsidi again with scanreindexgap_s set to a larger number.
Inspecting the Data
Now that we have a Measurement Set, it is time to look over the data, identify a good reference antenna, and find a good time range to use for calibrating the single band delay.
The Observation Summary
It will be useful later to have the basic information about the observation. The task listobs will return a list of all the scans, the sources observed, which stations were used, and the frequency setup. It is possible to run listobs in two ways: printing information in the CASA logger, or saving the information to a file.
To simply display the information in the CASA logger:
#In CASA
listobs(vis='tl016b.ms')
You should see the listobs output in the CASA logger window:
================================================================================
MeasurementSet Name: tl016b.ms MS Version 2
================================================================================
Observer: PLUTO Project: TL016B
Observation: VLBA
Data records: 1992052 Total elapsed time = 26010 seconds
Observed from 21-Feb-2022/06:13:39.0 to 21-Feb-2022/13:27:09.0 (UTC)
ObservationID = 0 ArrayID = 0
Date Timerange (UTC) Scan FldId FieldName nRows SpwIds Average Interval(s) ScanIntent
21-Feb-2022/06:13:39.0 - 06:17:09.0 1 0 4C39.25 23100 [0,1,2,3] [2, 2, 2, 2]
06:18:34.0 - 06:19:34.0 2 1 J1154+6022 6200 [0,1,2,3] [2, 2, 2, 2]
06:19:44.0 - 06:21:44.0 3 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:21:55.0 - 06:22:35.0 4 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:22:45.0 - 06:24:45.0 5 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:24:55.0 - 06:25:35.0 6 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:25:46.0 - 06:27:46.0 7 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:27:56.0 - 06:28:36.0 8 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:28:47.0 - 06:30:47.0 9 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:30:57.0 - 06:31:37.0 10 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:31:47.0 - 06:33:47.0 11 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:33:58.0 - 06:34:38.0 12 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:34:48.0 - 06:36:48.0 13 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:36:59.0 - 06:37:39.0 14 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
06:37:49.0 - 06:39:49.0 15 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:40:00.0 - 06:40:40.0 16 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
06:40:50.0 - 06:42:50.0 17 2 J1203+6031 13160 [0,1,2,3] [2, 2, 2, 2]
06:43:01.0 - 06:43:41.0 18 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
06:43:51.0 - 06:45:51.0 19 2 J1203+6031 13160 [0,1,2,3] [2, 2, 2, 2]
06:46:02.0 - 06:46:42.0 20 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
06:46:53.0 - 06:48:53.0 21 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
06:49:03.0 - 06:49:43.0 22 1 J1154+6022 4356 [0,1,2,3] [2, 2, 2, 2]
06:57:02.0 - 06:57:58.0 23 1 J1154+6022 5004 [0,1,2,3] [2, 2, 2, 2]
06:58:08.0 - 07:00:08.0 24 2 J1203+6031 13160 [0,1,2,3] [2, 2, 2, 2]
07:00:19.0 - 07:00:59.0 25 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:01:10.0 - 07:03:10.0 26 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:03:20.0 - 07:04:00.0 27 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
07:04:11.0 - 07:06:11.0 28 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:06:21.0 - 07:07:01.0 29 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
07:07:12.0 - 07:09:12.0 30 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:09:22.0 - 07:10:02.0 31 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:10:13.0 - 07:12:13.0 32 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:12:23.0 - 07:13:03.0 33 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:13:14.0 - 07:15:14.0 34 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:15:24.0 - 07:16:04.0 35 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:16:14.0 - 07:18:14.0 36 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:18:25.0 - 07:19:05.0 37 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:19:15.0 - 07:21:15.0 38 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:21:26.0 - 07:22:06.0 39 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:22:16.0 - 07:24:16.0 40 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:24:26.0 - 07:25:06.0 41 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:25:16.0 - 07:27:16.0 42 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:27:26.0 - 07:28:06.0 43 1 J1154+6022 4188 [0,1,2,3] [2, 2, 2, 2]
07:40:49.0 - 07:44:19.0 44 0 4C39.25 23100 [0,1,2,3] [2, 2, 2, 2]
07:46:03.0 - 07:47:03.0 45 1 J1154+6022 6200 [0,1,2,3] [2, 2, 2, 2]
07:47:12.0 - 07:49:12.0 46 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
07:49:22.0 - 07:50:02.0 47 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
07:50:12.0 - 07:52:12.0 48 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
07:52:22.0 - 07:53:04.0 49 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
07:53:13.0 - 07:55:13.0 50 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
07:55:23.0 - 07:56:03.0 51 1 J1154+6022 4220 [0,1,2,3] [2, 2, 2, 2]
07:56:13.0 - 07:58:15.0 52 2 J1203+6031 13240 [0,1,2,3] [2, 2, 2, 2]
07:58:24.0 - 07:59:04.0 53 1 J1154+6022 4240 [0,1,2,3] [2, 2, 2, 2]
07:59:14.0 - 08:01:14.0 54 2 J1203+6031 13040 [0,1,2,3] [2, 2, 2, 2]
08:01:24.0 - 08:02:06.0 55 1 J1154+6022 4620 [0,1,2,3] [2, 2, 2, 2]
08:02:15.0 - 08:04:15.0 56 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:04:25.0 - 08:05:07.0 57 1 J1154+6022 4620 [0,1,2,3] [2, 2, 2, 2]
08:05:16.0 - 08:07:16.0 58 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:07:26.0 - 08:08:06.0 59 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
08:08:16.0 - 08:10:18.0 60 2 J1203+6031 12060 [0,1,2,3] [2, 2, 2, 2]
08:10:27.0 - 08:11:07.0 61 1 J1154+6022 4240 [0,1,2,3] [2, 2, 2, 2]
08:11:17.0 - 08:13:17.0 62 2 J1203+6031 13064 [0,1,2,3] [2, 2, 2, 2]
08:13:27.0 - 08:14:09.0 63 1 J1154+6022 4484 [0,1,2,3] [2, 2, 2, 2]
08:14:18.0 - 08:16:18.0 64 2 J1203+6031 13064 [0,1,2,3] [2, 2, 2, 2]
08:16:28.0 - 08:17:10.0 65 1 J1154+6022 4484 [0,1,2,3] [2, 2, 2, 2]
08:24:47.0 - 08:25:47.0 66 1 J1154+6022 6096 [0,1,2,3] [2, 2, 2, 2]
08:25:56.0 - 08:27:56.0 67 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
08:28:06.0 - 08:28:48.0 68 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
08:28:57.0 - 08:30:57.0 69 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
08:31:07.0 - 08:31:47.0 70 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
08:31:57.0 - 08:33:57.0 71 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:34:07.0 - 08:34:49.0 72 1 J1154+6022 4620 [0,1,2,3] [2, 2, 2, 2]
08:34:58.0 - 08:36:58.0 73 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:37:08.0 - 08:37:48.0 74 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
08:37:58.0 - 08:39:58.0 75 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:40:08.0 - 08:40:50.0 76 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
08:40:59.0 - 08:42:59.0 77 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
08:43:09.0 - 08:43:49.0 78 1 J1154+6022 4220 [0,1,2,3] [2, 2, 2, 2]
08:43:59.0 - 08:45:59.0 79 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
08:46:09.0 - 08:46:49.0 80 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
08:46:59.0 - 08:48:59.0 81 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:49:09.0 - 08:49:51.0 82 1 J1154+6022 4424 [0,1,2,3] [2, 2, 2, 2]
08:50:00.0 - 08:52:00.0 83 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
08:52:10.0 - 08:52:50.0 84 1 J1154+6022 4204 [0,1,2,3] [2, 2, 2, 2]
08:53:00.0 - 08:55:00.0 85 2 J1203+6031 13004 [0,1,2,3] [2, 2, 2, 2]
08:55:10.0 - 08:55:50.0 86 1 J1154+6022 4204 [0,1,2,3] [2, 2, 2, 2]
08:56:00.0 - 08:58:00.0 87 2 J1203+6031 13004 [0,1,2,3] [2, 2, 2, 2]
08:58:10.0 - 08:58:50.0 88 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
08:59:00.0 - 09:01:02.0 89 2 J1203+6031 13420 [0,1,2,3] [2, 2, 2, 2]
09:01:11.0 - 09:01:51.0 90 1 J1154+6022 4396 [0,1,2,3] [2, 2, 2, 2]
09:16:23.0 - 09:19:53.0 91 0 4C39.25 23100 [0,1,2,3] [2, 2, 2, 2]
09:21:06.0 - 09:22:06.0 92 1 J1154+6022 6200 [0,1,2,3] [2, 2, 2, 2]
09:22:16.0 - 09:24:16.0 93 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
09:24:27.0 - 09:25:07.0 94 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
09:25:18.0 - 09:27:18.0 95 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
09:27:29.0 - 09:28:09.0 96 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
09:28:19.0 - 09:30:21.0 97 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
09:30:30.0 - 09:31:12.0 98 1 J1154+6022 4580 [0,1,2,3] [2, 2, 2, 2]
09:31:21.0 - 09:33:23.0 99 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
09:33:33.0 - 09:34:15.0 100 1 J1154+6022 4412 [0,1,2,3] [2, 2, 2, 2]
09:34:24.0 - 09:36:26.0 101 2 J1203+6031 13212 [0,1,2,3] [2, 2, 2, 2]
09:36:35.0 - 09:37:17.0 102 1 J1154+6022 4412 [0,1,2,3] [2, 2, 2, 2]
09:37:26.0 - 09:39:28.0 103 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
09:39:38.0 - 09:40:20.0 104 1 J1154+6022 4580 [0,1,2,3] [2, 2, 2, 2]
09:40:29.0 - 09:42:31.0 105 2 J1203+6031 13212 [0,1,2,3] [2, 2, 2, 2]
09:42:42.0 - 09:43:22.0 106 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
09:43:33.0 - 09:45:35.0 107 2 J1203+6031 13420 [0,1,2,3] [2, 2, 2, 2]
09:45:45.0 - 09:46:25.0 108 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
09:46:36.0 - 09:48:38.0 109 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
09:48:48.0 - 09:49:28.0 110 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
09:49:39.0 - 09:51:41.0 111 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
09:51:51.0 - 09:52:31.0 112 1 J1154+6022 4360 [0,1,2,3] [2, 2, 2, 2]
09:59:53.0 - 10:00:51.0 113 1 J1154+6022 5288 [0,1,2,3] [2, 2, 2, 2]
10:01:00.0 - 10:03:02.0 114 2 J1203+6031 13212 [0,1,2,3] [2, 2, 2, 2]
10:03:11.0 - 10:03:53.0 115 1 J1154+6022 4412 [0,1,2,3] [2, 2, 2, 2]
10:04:03.0 - 10:06:05.0 116 2 J1203+6031 13340 [0,1,2,3] [2, 2, 2, 2]
10:06:15.0 - 10:06:57.0 117 1 J1154+6022 4540 [0,1,2,3] [2, 2, 2, 2]
10:07:06.0 - 10:09:08.0 118 2 J1203+6031 13240 [0,1,2,3] [2, 2, 2, 2]
10:09:18.0 - 10:10:00.0 119 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
10:10:09.0 - 10:12:11.0 120 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
10:12:21.0 - 10:13:03.0 121 1 J1154+6022 4540 [0,1,2,3] [2, 2, 2, 2]
10:13:12.0 - 10:15:14.0 122 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
10:15:24.0 - 10:16:06.0 123 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
10:16:15.0 - 10:18:17.0 124 2 J1203+6031 13240 [0,1,2,3] [2, 2, 2, 2]
10:18:27.0 - 10:19:09.0 125 1 J1154+6022 4580 [0,1,2,3] [2, 2, 2, 2]
10:19:18.0 - 10:21:20.0 126 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
10:21:30.0 - 10:22:12.0 127 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
10:22:21.0 - 10:24:23.0 128 2 J1203+6031 13240 [0,1,2,3] [2, 2, 2, 2]
10:24:32.0 - 10:25:14.0 129 1 J1154+6022 4440 [0,1,2,3] [2, 2, 2, 2]
10:25:24.0 - 10:27:26.0 130 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
10:27:35.0 - 10:28:17.0 131 1 J1154+6022 4580 [0,1,2,3] [2, 2, 2, 2]
10:28:26.0 - 10:30:28.0 132 2 J1203+6031 13380 [0,1,2,3] [2, 2, 2, 2]
10:30:37.0 - 10:31:19.0 133 1 J1154+6022 4580 [0,1,2,3] [2, 2, 2, 2]
10:42:23.0 - 10:45:53.0 134 0 4C39.25 18900 [0,1,2,3] [2, 2, 2, 2]
10:46:48.0 - 10:47:48.0 135 1 J1154+6022 6056 [0,1,2,3] [2, 2, 2, 2]
10:47:57.0 - 10:49:57.0 136 2 J1203+6031 13040 [0,1,2,3] [2, 2, 2, 2]
10:50:07.0 - 10:50:49.0 137 1 J1154+6022 4460 [0,1,2,3] [2, 2, 2, 2]
10:50:58.0 - 10:52:58.0 138 2 J1203+6031 13040 [0,1,2,3] [2, 2, 2, 2]
10:53:08.0 - 10:53:50.0 139 1 J1154+6022 4460 [0,1,2,3] [2, 2, 2, 2]
10:53:59.0 - 10:55:59.0 140 2 J1203+6031 13040 [0,1,2,3] [2, 2, 2, 2]
10:56:09.0 - 10:56:49.0 141 1 J1154+6022 4240 [0,1,2,3] [2, 2, 2, 2]
10:56:59.0 - 10:59:01.0 142 2 J1203+6031 13260 [0,1,2,3] [2, 2, 2, 2]
10:59:10.0 - 10:59:50.0 143 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:00:00.0 - 11:02:00.0 144 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:02:10.0 - 11:02:50.0 145 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:03:00.0 - 11:05:02.0 146 2 J1203+6031 13420 [0,1,2,3] [2, 2, 2, 2]
11:05:11.0 - 11:05:51.0 147 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:06:01.0 - 11:08:01.0 148 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:08:11.0 - 11:08:53.0 149 1 J1154+6022 4424 [0,1,2,3] [2, 2, 2, 2]
11:09:02.0 - 11:11:02.0 150 2 J1203+6031 13020 [0,1,2,3] [2, 2, 2, 2]
11:11:12.0 - 11:11:52.0 151 1 J1154+6022 4204 [0,1,2,3] [2, 2, 2, 2]
11:12:02.0 - 11:14:04.0 152 2 J1203+6031 13224 [0,1,2,3] [2, 2, 2, 2]
11:14:13.0 - 11:14:53.0 153 1 J1154+6022 4204 [0,1,2,3] [2, 2, 2, 2]
11:15:03.0 - 11:17:03.0 154 2 J1203+6031 13004 [0,1,2,3] [2, 2, 2, 2]
11:17:13.0 - 11:17:53.0 155 1 J1154+6022 4396 [0,1,2,3] [2, 2, 2, 2]
11:25:18.0 - 11:26:08.0 156 1 J1154+6022 4888 [0,1,2,3] [2, 2, 2, 2]
11:26:17.0 - 11:28:17.0 157 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:28:27.0 - 11:29:09.0 158 1 J1154+6022 4412 [0,1,2,3] [2, 2, 2, 2]
11:29:18.0 - 11:31:18.0 159 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:31:28.0 - 11:32:08.0 160 1 J1154+6022 4192 [0,1,2,3] [2, 2, 2, 2]
11:32:18.0 - 11:34:18.0 161 2 J1203+6031 12992 [0,1,2,3] [2, 2, 2, 2]
11:34:28.0 - 11:35:10.0 162 1 J1154+6022 4412 [0,1,2,3] [2, 2, 2, 2]
11:35:19.0 - 11:37:19.0 163 2 J1203+6031 12992 [0,1,2,3] [2, 2, 2, 2]
11:37:29.0 - 11:38:09.0 164 1 J1154+6022 4192 [0,1,2,3] [2, 2, 2, 2]
11:38:19.0 - 11:40:21.0 165 2 J1203+6031 13420 [0,1,2,3] [2, 2, 2, 2]
11:40:31.0 - 11:41:11.0 166 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:41:20.0 - 11:43:20.0 167 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:43:31.0 - 11:44:11.0 168 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:44:21.0 - 11:46:21.0 169 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:46:32.0 - 11:47:12.0 170 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:47:22.0 - 11:49:22.0 171 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:49:32.0 - 11:50:12.0 172 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:50:23.0 - 11:52:23.0 173 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:52:33.0 - 11:53:13.0 174 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:53:23.0 - 11:55:23.0 175 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:55:33.0 - 11:56:13.0 176 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:56:24.0 - 11:58:24.0 177 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
11:58:34.0 - 11:59:14.0 178 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
11:59:24.0 - 12:01:24.0 179 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:01:34.0 - 12:02:14.0 180 1 J1154+6022 4396 [0,1,2,3] [2, 2, 2, 2]
12:13:23.0 - 12:16:53.0 181 0 4C39.25 18900 [0,1,2,3] [2, 2, 2, 2]
12:17:50.0 - 12:18:50.0 182 1 J1154+6022 5752 [0,1,2,3] [2, 2, 2, 2]
12:19:00.0 - 12:21:00.0 183 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:21:10.0 - 12:21:50.0 184 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:22:00.0 - 12:24:00.0 185 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:24:11.0 - 12:24:51.0 186 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:25:01.0 - 12:27:01.0 187 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:27:11.0 - 12:27:51.0 188 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:28:01.0 - 12:30:01.0 189 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:30:12.0 - 12:30:52.0 190 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:31:02.0 - 12:33:02.0 191 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:33:12.0 - 12:33:52.0 192 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:34:02.0 - 12:36:02.0 193 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:36:13.0 - 12:36:53.0 194 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:37:03.0 - 12:39:03.0 195 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:39:13.0 - 12:39:53.0 196 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:40:03.0 - 12:42:03.0 197 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:42:14.0 - 12:42:54.0 198 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:43:04.0 - 12:45:04.0 199 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:45:14.0 - 12:45:54.0 200 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:46:04.0 - 12:48:04.0 201 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:48:15.0 - 12:48:55.0 202 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
12:56:06.0 - 12:57:04.0 203 1 J1154+6022 4536 [0,1,2,3] [2, 2, 2, 2]
12:57:14.0 - 12:59:14.0 204 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
12:59:24.0 - 13:00:04.0 205 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:00:15.0 - 13:02:15.0 206 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:02:25.0 - 13:03:05.0 207 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:03:15.0 - 13:05:15.0 208 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:05:25.0 - 13:06:05.0 209 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:06:16.0 - 13:08:16.0 210 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:08:26.0 - 13:09:06.0 211 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:09:16.0 - 13:11:16.0 212 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:11:26.0 - 13:12:06.0 213 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:12:17.0 - 13:14:17.0 214 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:14:27.0 - 13:15:07.0 215 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:15:17.0 - 13:17:17.0 216 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:17:27.0 - 13:18:07.0 217 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:18:17.0 - 13:20:17.0 218 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:20:28.0 - 13:21:08.0 219 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:21:18.0 - 13:23:18.0 220 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:23:28.0 - 13:24:08.0 221 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
13:24:18.0 - 13:26:18.0 222 2 J1203+6031 13200 [0,1,2,3] [2, 2, 2, 2]
13:26:29.0 - 13:27:09.0 223 1 J1154+6022 4400 [0,1,2,3] [2, 2, 2, 2]
(nRows = Total number of rows per scan)
Fields: 3
ID Code Name RA Decl Epoch nRows
0 4C39.25 09:27:03.013941 +39.02.20.85181 J2000 107100
1 J1154+6022 11:54:04.535308 +60.22.20.81576 J2000 513668
2 J1203+6031 12:03:03.507154 +60.31.19.16302 J2000 1371284
Spectral Windows: (4 unique spectral windows and 1 unique polarization setups)
SpwID Name #Chans Frame Ch0(MHz) ChanWid(kHz) TotBW(kHz) CtrFreq(MHz) Corrs
0 none 128 GEO 5004.000 500.000 64000.0 5035.7500 RR LL
1 none 128 GEO 5068.000 500.000 64000.0 5099.7500 RR LL
2 none 128 GEO 5132.000 500.000 64000.0 5163.7500 RR LL
3 none 128 GEO 5196.000 500.000 64000.0 5227.7500 RR LL
The SOURCE table is absent: see the FIELD table
Antennas: 10:
ID Name Station Diam. Long. Lat. Offset from array center (m) ITRF Geocentric coordinates (m)
East North Elevation x y z
0 BR BR 25.0 m -119.40.59.8 +47.56.23.6 -0.0000 0.0000 6366573.1493 -2112065.339753 -3705356.513964 4726813.595927
1 FD FD 25.0 m -103.56.41.4 +30.27.59.8 -0.0000 0.0000 6374225.1270 -1324009.438905 -5332181.956657 3231962.338382
2 HN HN 25.0 m -071.59.11.7 +42.44.30.3 -0.0000 0.0000 6368555.4418 1446374.723555 -4447939.698170 4322306.215011
3 KP KP 25.0 m -111.36.44.7 +31.47.01.6 -0.0000 0.0000 6374084.6442 -1995678.959790 -5037317.696765 3357327.949827
4 LA LA 25.0 m -106.14.44.2 +35.35.34.2 -0.0000 0.0000 6372831.2478 -1449752.711882 -4975298.576836 3709123.785811
5 MK MK 25.0 m -155.27.19.9 +19.40.44.8 -0.0000 0.0000 6379464.0809 -5464075.303632 -2495247.548640 2148297.629883
6 NL NL 25.0 m -091.34.26.9 +41.34.49.1 -0.0000 0.0000 6368913.6306 -130872.637324 -4762317.087915 4226850.972202
7 OV OV 25.0 m -118.16.37.4 +37.02.47.3 -0.0000 0.0000 6371546.5839 -2409150.566965 -4478573.065876 3838617.291460
8 PT PT 25.0 m -108.07.09.1 +34.07.19.7 -0.0000 0.0000 6373749.2143 -1640954.066439 -5014816.028293 3575411.724719
9 SC SC 25.0 m -064.35.01.1 +17.38.42.4 -0.0000 0.0000 6376148.1024 2607848.714994 -5488069.460221 1932739.843634
NOTE: You can also assign the listobs output to a python dictionary (e.g., "obs_dict") by typing "obs_dict = listobs(vis='tl016b.ms')".
It is usually useful to have a copy of the listobs output in a file that you can refer to later. To save the listobs output to a file named "tl016b_listobs.txt':
#In CASA
listobs(vis='tl016b.ms', listfile='tl016b_listobs.txt')
A few things that are useful to note from the listobs output:
- While the antenna number, field number, and spw number all start at 0, the scan number starts at 1.
- The fringe finder is 4C39.25, with 5 scans of about 3.5 minutes each.
- The phase reference calibrator is J1154+6022. Each phase reference scan is about 1 minute long.
Identifying a Good Reference Antenna
VLBA calibration makes use a reference antenna: one antenna that all other antennas can be referenced to when generating solutions. Usually, you will want to use one of the more central stations: FD, KP, LA, or PT.
To determine which is the best to use as the reference antenna, use plotms to plot phase vs frequency for a single scan on a bright source (usually the fringe finder or bandpass calibrator). For this observation, use the third scan on 4C39.25, which is scan 91 from the listobs output. Inspect each of the 4 central antennas and use the one which has the most well-behaved phases.
NOTE: For our observation, we know that it was windy at KP so we probably do not want to use that one as the reference antenna.
#In CASA
plotms(vis='tl016b.ms', xaxis='frequency', yaxis='phase', field='4C39.25', scan='91', correlation='ll', antenna='FD,LA,PT', iteraxis='baseline', coloraxis='spw')
Use the GUI to step though the baselines look at each antenna and look at both right- and left-hand polarization (correlation='rr' and correlation='ll' ). Our observation does not include the cross-hand polarizations (lr and rl), and you usually won't worry about inspecting them anyway since they will usually be too low to see anything useful.
You should also use the GUI to change the yaxis to amplitude to inspect the shapes of the bandpasses and look for RFI. If antenna has strong RFI, you should not use it as the reference antenna.
For this observation, we will use Fort Davis (FD) as the reference antenna. Its phases are fairly smooth, it is free of RFI, and the bandpasses look pretty clean (especially compared to PT in spw 2 and 3).
Identifying a Good Time Range for the Insrumental Delay Calibration
Next, we will look for a good time interval (about 1 minute long) for the instrumental delay calibration. This will be done using the fringe finder (4C39.25), so we should inspect each scan on it: 1, 44, 91, 134, and 181. We will want to plot amplitude vs time for each of these scans. To save time, we will just plot the baselines to the reference antenna, FD.
#In CASA
plotms(vis='tl016b.ms', xaxis='frequency', yaxis='amp', field='4C39.25', antenna='FD', scan='1', correlation='rr,ll', iteraxis='baseline', coloraxis='corr')
Use the GUI to step through each baseline for the scan. Then, look at the next scan in the list. Look for outliers in the amplitude data. We want to use a time range with no RFI and with all antennas on source.
Notice that Saint Croix (SC) did not observe during scans 134 and 181, so we do not want to use either of those.
Scan 91 is close to the middle of the observation, and looks mostly clean. Use the plotms GUI to set scan='91' and yaxis='time' and step through the baselines again. Notice that some baselines have some higher amplitude points early on in this scan. We will want to avoid these early times. The time range 09:17:00 to 09:18:00 looks nice for each baseline to the reference antenna, so we will use that for our instrumental delay calibration later.
Flagging Data
Quack
VLBA observations often include a little bit of bad data at the beginnings of the scans, and sometimes at the ends of scans. An easy way to deal with this is to "quack" the data. Quacking is a completely optional step, and you should only do it if you see evidence for bad data at the beginnings or ends of scan.
In CASA, you can quack your data using the flagdata task and setting mode='quack'. The amount of data to be flagged is controlled by the quackinterval parameter, which sets the time interval in seconds.
To flag the first 4 seconds of each scan:
#In CASA
flagdata(vis='tl016b.ms', mode='quack', quackinterval=4.0, quackmode='beg', quackincrement=True)
To flag the last 4 seconds of each scan:
#In CASA
flagdata(vis='tl016b.ms', mode='quack', quackinterval=4.0, quackmode='endb', quackincrement=True)
For those who are interested: There is some uncertainty about the origins of the term "quack". However, discussions with people who were working at NRAO in the late 1970s indicates it has nothing to do with waterfowl. Instead, "quack" refers to an unscrupulous/incompetent physician who treats the symptoms of a disease without treating the disease itself. The original QUACK routine was written for the VLA DEC-10 computers and flagged the beginnings of scans because they often contained bad data, but nobody could figure out what was causing the bad data.
Automated Flagging
The the flagdata task includes a useful automated flagging mode known as "TFCrop".
To begin, you just want to get a feel for what TFCrop will do to the data, which means you should set action='calculate' .
#In CASA
flagdata(vis='tl016b.ms', mode='tfcrop', datacolumn='data', timecutoff=4.0, freqcutoff=3.0, action='calculate', display='both')
This will open a new window with a GUI. The top row of the GUI will display the data as it currently is. The bottom row shows what the data will look like after the flags are applied (blue regions are flagged). Step through the antennas by clicking "Next Baseline". Step through the spectral windows by clicking "Next SPW". Step through at least a few scans by clicking "Next Scan".
Using the default cut-off values of timecutoff=4.0, freqcutoff=3.0, and flagdimension='freqtime' appears to make the flagger focus on mostly on the edge channels. We do not necessarily want to get rid of those just yet. To exit the GUI, click "Quit". We will change the way TFCrop looks for bad data by setting flagdimension='time' , which will only look for outliers along the time axis. This should be fine, since we did not see any strong evidence for persistant RFI in the frequency dimension. Take a look at how the automatic flagging will approach things now:
#In CASA
flagdata(vis='tl016b.ms', mode='tfcrop', datacolumn='data', timecutoff=4.0, flagdimension='time', action='calculate', display='both')
Step through the baselines, spectral windows, and scans again. Note that the program now leaves the edge channels alone, but it still occasionally finds some outliers in along the time axis. With timecutoff=4.0, it should really only flag those data points that are 4-times the standard deviation in the time dimension. This should be sufficient to remove the worst of the time-dependent RFI in our observation.
To generate the flags, we will need to run flagdata again with action='apply' .
#In CASA
flagdata(vis='tl016b.ms', mode='tfcrop', datacolumn='data', timecutoff=4.0, flagdimension='time', action='apply', display='both')
You should double check that the automatic flagging will behave as you expect. Once you are satisfied that the flagging will do what you want, click "Stop Display". The program will then look through the entire observation and apply the flags.
NOTE: You can always exit the TFCrop mode without applying any flags by clicking "Quit", even when you set action='apply' .
Flagging "By Hand"
As telescope arrays become larger and more complex, automated flagging will become the primary means of excluding bad data (just look at what ALMA does). However, the current VLBA is still small enough that inspecting and flagging data oneself is not too painful.
You can look for obvious bad data using plotms. Be aware that while you can flag data in plotms, a major drawback to using plotms to flag data is that it makes undoing flags very difficult. The preferred method of flagging by hand is to identify the bad data with plotms, and then generate the flags with flagdata. It is recommended to be somewhat careful with flagging early on in the calibration process and only flag those data points that are obviously bad.
To start with, let's plot the bandpasses for each baseline to FD for all 5 scans on 4C39.25.
#In CASA
plotms(vis='tl016b.ms', xaxis='frequency', yaxis='amp', field='4C39.25', antenna='FD', scan='', correlation='rr,ll', iteraxis='baseline', coloraxis='scan')
Using the GUI to step through the baselines, we can immediately see there is a problem with the FD-HN baseline for one scan. In the "Axes" tab of the GUI, switch the "X Axis" to "Time". Now we can see that the final scan on 4C39.25 at HN was much lower than the other scans. It's likely that the source was at very low elevation, so we should not trust those data. To make sure the problem was at HN, check that all baselines to HN have similar behavior; in the "Data" tab of the GUI, change "antenna" to "HN" and click "Plot". We can see that the final scan on 4C39.25 was low on all HN baselines. Flag that scan using flagdata.
#In CASA
flagdata(vis='tl016b.ms', mode='manual', field='4C39.25', antenna='HN', scan='181')
If you kept your plotms window open, you can verify that the flagging has worked by checking the "Reload" box in the GUI and clicking "Plot" to re-plot the data. You should now see that the final scan on 4C39.25 is missing on all baselines to HN.
Next, let's take a look at the phase reference calibrator. To make sure 4C39.25 is the only source that got low at later times, we will start by plotting amplitude vs. time. We will use antenna='*&*' to plot only the cross-correlations.
#In CASA
plotms(vis='tl016b.ms', xaxis='time', yaxis='amp', field='J1154+6022', antenna='*&*', scan='', correlation='rr,ll', iteraxis='baseline', coloraxis='scan')
Note: You can plot just the autocorrelations by setting antenna='*&&&' , which can be a good way to look for RFI at a single station.
As you step through the baselines, you can see that J1154+6022 is fairly well-behaved. However, there are a few things that stand out. For example, there is a very hot time on the BR-PT baseline. Using the "Mark Regions" and "Locate" tools in the plotms, we can see that the problem is in scan 10. Using the GUI, we can take a closer look at scan 10; set antenna='BR&PT' , scan='10' , and spw='0' , then look at the other 3 spectral windows. There is obviously some bad data at the end of scan 10 in each spectra window. In fact, compating scan 10 to other nearby scans (scan='6~14' ), it looks like all of scan 10 might be questionable. So, we will flag scan 10 on the BR-PT baseline using flagdata.
#In CASA
flagdata(vis='tl016b.ms', mode='manual', field='J1154+6022', antenna='BR&PT', scan='10')
Continuing to inspect the baselines, we can spot other problems.
#In CASA
flagdata(vis='tl016b.ms', mode='manual', field='J1154+6022', antenna='KP&LA', scan='221')
flagdata(vis='tl016b.ms', mode='manual', field='J1154+6022', antenna='LA&PT', scan='207')
flagdata(vis='tl016b.ms', mode='manual', field='J1154+6022', antenna='NL&PT', scan='213')
Calibrating the Data
Amplitude Corrections from Autocorrelations
Determine the amplitude corrections from the autocorrelations with accor.
#In CASA
accor(vis='tl016b.ms', caltable='tl016b.accor', solint='30s')
NOTE: This step is not required for EVN data, because the EVN correlator performs it during correlation.
Inspect the tl016b.accor solution table with plotms.
#In CASA
plotms(vis='tl016b.accor', xaxis='time', yaxis='amp', iteraxis='antenna', coloraxis='spw')
Ideally, all of the solutions should be very close to 1.0. Stepping through the antennas, it is clear that pretty much every station has significant outliers.
The AIPS VLBA utility script VLBACCOR smooths the autocorrelation corrections by default (with a smoothing time of 30 minutes). It is possible to do this smoothing in CASA 6.3 and later using the smoothcal task. Based on what we saw in our plotting, these data would likely benefit from some smoothing.
#In CASA
smoothcal(vis='tl016b.ms', tablein='tl016b.accor', caltable='tl016b_smooth.accor', smoothtype='median', smoothtime=1800.0)
Remember to check the smoothed solutions with plotms to make sure it was an improvement.
#In CASA
plotms(vis='tl016b_smooth.accor', xaxis='time', yaxis='amp', iteraxis='antenna', coloraxis='spw')
Things look better, but there are still some areas we will need to keep an eye on. Brewster (BR), Los Alamos (LA), and Saint Croix (SC) all have significant structure at later times, especially at the higher frequencies (spw's 2 and 3). Surprisingly, Kitt Peak (KP) very nice, even though we know there was rain at that station for at least a portion of the observation.
A Priori Calibration
Unlike the VLA, the VLBA cannot rely on bootstrapping absolute flux density calibration from a well-modeled calibrator. Instead, the VLBA relies on a combination of the system temperature and the known gain curve of the antennas (how the gain of the antenna changes with elevation). Both the system temperatures and gain curves are included in the FITS-IDI file. To get this information into a form that CASA can use for calibration, we use the gencal task to generate calibration tables.
System temperature:
gencal(vis='tl016b.ms', caltable='tl016b.tsys', caltype='tsys', uniform=False)
You will see several messages appear informing you that the Tsys values for many times were negative and will be flagged. Notice that the antenna associated with these bad Tsys values is "antenna id=0", which is Brewster (BR). Also, all of the bad Tsys values are in spw 2 and 3. From our plotting of the accor values, we knew that BR likely had issues in the upper spw's 2 and 3.
Check the system temperature table with plotms.
#In CASA
plotms(vis='tl016b.tsys', xaxis='time', yaxis='tsys', iteraxis='antenna', coloraxis='spw')
Make sure to also plot the solutions with xaxis='freq' .
You should see that the remaining Tsys values for BR in spw 2 and 3 are pretty terrible. Also, KP spw 3, LA spw 2, NL spw 3, and SC spw 3 are a bit gross. Our chosen reference antenna, FD, looks pretty good except for one spike.
You may flag the minor outliers in plotms, if you wish. While it is generally a bad idea to flag data in plotms, that mainly applies to data in the measurement set. The Tsys table can easily be regenerated by running gencal again if we discover we made a mistake in our flagging. However, note that many of the "outlier" points are scans on the fringe finder 4C39.25. In most cases, the 4C39.25 outlier points are the last scan on the source (scan 181), which could mean the source was simply at a very low elevation at most stations. We will need to be careful as we continue with the calibration to not use that last scan on 4C39.25 because it could introduce errors into our calibration. To be safe, we will flag that scan.
#In CASA
flagdata(vis='tl016b.ms', mode='manual', field='4C39.25', scan='181')
At this point, it is good to remind ourselves of the radio astronomer's credo: "Bad data is worse than no data." With that in mind, we will flag the data in the measurement set correspnding to the really bad Tsys values using flagdata.
#In CASA
flagdata(vis='tl016b.ms', mode='manual', antenna='BR', spw='2,3')
flagdata(vis='tl016b.ms', mode='manual', antenna='KP', spw='3')
flagdata(vis='tl016b.ms', mode='manual', antenna='LA', spw='2')
flagdata(vis='tl016b.ms', mode='manual', antenna='NL', spw='3')
flagdata(vis='tl016b.ms', mode='manual', antenna='SC', spw='3', scan='135~223')
Gain curve:
#In CASA
gencal(vis='tl016b.ms', caltable='tl016b.gcal', caltype='gc')
For this observation at 5 GHz, the gain curve is not very interesting, so we will not bother looking at the solutions now (although you can if you really want to). If your observation is at 12 GHz or higher, you will probably want to inspect the gain curve table with plotms.
Instrumental Delay Calibration
Solve for the instrumental delays by using fringefit on a bright source (the "fringe finder"). In our case, the fringe finder is 4C39.25. Set the timerange to the time span you identified while inspecting the data earlier.
#In CASA
fringefit(vis='tl016b.ms', caltable='tl016b.sbd', field='4C39.25', timerange='!!TIME RANGE!!', solint='inf', zerorates=True, refant='REFANT', minsnr=10, gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys'], interp=['nearest', 'nearest', 'nearest,nearest'], parang=True)
Ideally, the SNR for each station should be very high (>10). Watch the logger for any reports of low SNR and failures to converge on a solution.
Apply the instrumental delay corrections using applycal.
#In CASA
applycal(vis='tl016b.ms', gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd>'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest'], parang=True)
NOTE: In applycal, the order in which you specify the list for gaintable sets the order for both interp and spwmap. If you change the order of gaintable, be sure to also change the order of interp and spwmap! Also, if you smoothed any of the solutions, be sure to use the appropriate filename for the smoothed table.
Check that applying the solutions resulted in improvements:
#In CASA
plotms(vis='tl016b.ms', field='4C39.25', xaxis='frequency', yaxis='phase', ydatacolumn='corrected', timerange='!!SAME AS SBD STEP!!', correlation='rr,ll', antenna='*&*', iteraxis='antenna' coloraxis='antenna2')
Global Fringe Fitting
Now, we will solve for the time and frequency-dependent effects in phase using fringefit, also known as "global fringe fitting" (or sometimes "multi-band delay", if you combine all of the bands). We will need to pick a solution interval that is appropriate for our data. It should be at least 10 seconds, and no longer than the scan length on the phase reference calibrator. For this observation, we will use XX seconds.
For refant, enter a list of antennas to try as the reference antenna. The preferred refant should be listed first, followed by the second choice, then third choice, and so on. It is not recommended to include Mauna Kea (MK) or Saint Croix (SC) in the list, unless the phase reference calibrator is very bright on the longest baselines. Set field to the fringe finder and phase reference calibrator.
#In CASA
fringefit(vis='tl016b.ms', caltable='tl016b.mbd', field='4C39.25, J1154+6022', solint='!!SOLINT!!', minsnr=5, zerorates=False, refant='FD,PT,LA,KP,OV,NL,BR,HN !!CHECK REFANT LIST!!', gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest'], parang=True)
This step may take quite a while, so this is a good opportunity to go get a tasty beverage.
When the fringefit task is done, check the logger for the solution statistics ("expected/attempted/succeeded"). You want all three numbers to be the same, or at least very similar. Also, look for instances when the SNR was beloew your threshold (minsnr) and times when it took many iterations to get a good fit. You may need to try longer solution intervals to get the global fringe fit to work optimally.
After fringefit has successfully completed and you are satisfied that the number of solutions is appropriate, take a look at the solutions with plotms.
#In CASA
plotms(vis='tl016b.mbd', xaxis='time', yaxis='phase', iteraxis='antenna')
Use the GUI to switch the yaxis between 'delay', 'phase', and 'delayrate'. The delay and phase solutions should both vary smoothly with time. If they do not, you may need to smooth the table before applying it. The rates should be centered on zero with some scatter.
When you are confident that the global/multi-band solutions are good, apply them with applycal.
#In CASA
applycal(vis='tl016b.ms', gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd', 'tl016b.mbd'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest', 'linear'], parang=True)
It will probably take a while (about 5 minutes or longer) for applycal to run this time.
Take a look at the calibrated data with plotms to make sure the corrections are improving the phases.
#In CASA
plotms(vis='tl016b.ms', SOMETHING, SOMETHING ELSE, SOMETHING EVEN MORE)
Bandpass Calibration
Now we will correct for the shape of the bandpass using the bandpass task. This step requires a very bright source (perferably >1 Jy on all baselines), so we will use our fringe finder 4C39.25. However, unlike when we solved for the instrumental delay (above), we will use all of the scans on the source.
#In CASA
bandpass(vis='tl016b.ms', caltable='tl016b.bpass', field='4C39.25', solint='inf', refant='!!REFANT!!', solnorm=True, bandtype='B', gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd', 'tl016b.mbd'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest', 'linear'], parang=True)
Inspect the solutions with plotms.
#In CASA
plotms(vis='tl016b.bpass', xaxis='frequency', yaxis='amp', iteraxis='antenna')
While looking over the solutions, also make sure to check the phases (uses the GUI to set yaxis='phase').
Apply the solutions with applycal.
#In CASA
applycal(vis='tl016b.ms', gaintable=['tl016b_smooth.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd', 'tl016b.mbd', 'tl016b.bpass'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest', 'linear', 'linear,linear'], parang=True)
It will probably take a while for applycal to run again, since you are also applying the solutions from the global fringe fitting.
After aplpying the bandpass solutions, take a look at the calibrated data with plotms.
#In CASA
plotms(vis='tl016b.ms', xaxis='frequency', yaxis='amp', ydatacolumn='corrected', field='4C39.25', antenna='*&*', correlation='rr,ll', iteraxis='antenna', coloraxis='spw')
The bandpass calibration often does not perfectly calibrate the channels at the beginning and end of each spectral window. It is often a good idea to get rid of the edge channels that are not well-calibrated. If you notice that the edges of the spectral windows look at bit nasty (much higher than the rest of the band), feel free to flag those channels. This flagging can be done in plotms, but it is often easier (and more reliable) to do it in with flagdata.
For our data, we will flag the first and last 3 channels of each spw.
#In CASA
flagdata(vis='tl016b.ms', spw='0~2;125~127')
Many experienced VLBA observers will not have any second thoughts about cutting out 8 or 12 channels on each side of the spw for continuum observations. If you start with flagging 3 channels on each side and think the amplitude vs frequency plots still look pretty gross, feel free to flag some more.
Final Amplitude Scaling and Flux Calibration
Any VLBA observation with wide bandwidths (>256 MHz), which is any observation done a bit rate of 2 Gbps or more, will require one extra calibration step at this point. The flux density scale for wideband VLBA observations can be off by up to 30% (although it usually only off by a few percent) if the calibration does not correctly account for the wide bandpasses. To do this, you need to run accor again after the bandpass calibration has been applied. The AIPS task that was developed to address this issue is called ACSCL. For more details on this topic, and how it was handled in AIPS, see VLBA Scientific Memo #37.
Prior to running accor this time, it is strongly recommended that users inspect the calibrated data and determine whether any channels will need to be excluded from imaging or other post-processing. Edge channels may need to be excluded if the bandpass calibration did not properly correct the band at the edges. From VLBA Scientific Memo #37, the standard recommendation is to use the inner ~75% of channels for PFB observations and the inner ~89% of channels for DDC observations. Any channels that are suspected to contain RFI should also be excluded. The actual channels used will depend on the individual observation and science goals.
Final re-scaling of the auto-correlation amplitudes with accor. NOTE: DO NOT APPLY THE SYSTEM TEMPERATURE OR GAIN CURVE TABLES WHEN DERIVING THESE SOLUTIONS.
#In CASA
accor(vis='tl016b.ms', spw='*:7~121', caltable='tl016b.acscl', solint='2min', gaintable=['tl016b.accor', 'tl016b.sbd', 'tl016b.mbd', 'tl016b.bpass'], interp=['nearest', 'nearest', 'linear', 'linear,linear'])
NOTE: Use all the channels that will be used for imaging or other post-processing.
The AIPS VLBA utility script VLBAAMP smooths the autcorrelation corrections by default in exactly the same way as VLBACCOR. We will replicate the AIPS method by using the \texttt{smoothcal} task to smooth our .acscl table.
#In CASA
smoothcal(vis='tl016b.ms, tablein='tl016b.acscl', caltable='tl016b_smooth.acscl', smoothtype='median', smoothtime=1800.0)
Apply the final amplitude solutions with applycal. You should apply the system temperature and gain curve tables in this step.
#In CASA
applycal(vis='<your filename>.ms',
field='',
gaintable=['tl016b.accor', 'tl016b.gcal', 'tl016b.tsys', 'tl016b.sbd', 'tl016b.mbd', 'tl016b.bpass', 'tl016b_smooth.acscl'], interp=['nearest', 'nearest', 'nearest,nearest', 'nearest', 'linear', 'linear,linear', 'nearest'], parang=True)
Congratulations! The data should be mostly calibrated at this point. At the very least, you should be able to make images of the calibrators.
Split Out Calibrated Data
It is generally recommended to split the measurement set after the initial calibration is complete. If you have multiple science targets, you should create a new MS for each science target + phase reference calibrator pair by setting the field paremeter to the appropriate values. Even if your observation only involved a single target, it is a good idea to split the MS once the initial calibration is complete. This will preserve the initially-calibrated data in case you make a mistake in any of the next steps and need to start over. Think of it as a "save point" in a video game (do you really want to have to go back to the beginning of the game when you could just start from the beginning of the current level?).
Split the calibrated MS using split.
#In CASA
split(vis='tl016b.ms', outputvis='tl016b_cal1.ms', field='J1154+6022,J1203+6031', spw='*:7~121', antenna='*&*', datacolumn='corrected')
You can name the new MS whatever you want, but using a naming scheme that keeps track of where it was in the calibration process will make your life easier if you make mistakes down the line. For this tutorial, we will use "tl016b_cal1.ms" to indicate it is where we ended up after the first calibration steps. Setting antenna='*&*' will leave the autocorrelations out of our new MS (we don't need them anymore). We should not need 4C39.25 for any of the next steps, so we will not bother to keep that source in our new MS. Also, note that we have selected only the spectral channels that we used during the final amplitude scaling step.
Self-Calibration of Phase Reference Calibrator
Despite our best efforts with the initial calibration, VLBA osbervations will almost always require additional steps to improve the calibration. We will start by generating a model of the phase reference calibrator, and use that model to refine the calibration. This is known as "self-calibration".
Tracking Improvement
Imaging the Calibrator
#In CASA
tclean(vis='tl016b_cal1.ms', field='J1154+6022', imagename='J1154_sc1', imsize=[640], cell=['0.0003arcsec'], stokes='I', deconvolver='clark', weighting='natural', niter=1000, interactive=True, savemodel='modelcolumn')
Phase Self-Calibration
First, we will refine the delays.
#In CASA
gaincal(vis='tl016b_cal1.ms', field='J1154+6022', caltable='tl016b_cal1.dcal', solint='inf', refant='PT', minblperant=3, gaintype='K', calmode='p', parang=False)
Next, we will refine the phases.
#In CASA
gaincal(vis='tl016b_cal1.ms', field='J1154+6022', caltable='tl016b_cal1.pcal', solint='20s', refant='PT', minblperant=3, gaintype='G', calmode='p', gaintable=['tl016b_cal1.dcal'], interp=['linear'], parang=False)
Apply the phase self-calibration soultions to the phase reference calibrator.
#In CASA
applycal(vis='tl016b_cal1.ms', field='J1154+6022', gaintable=['tl016b_cal1.dcal',tl016b_cal1.pcal'], interp=['linear','linear'], parang=False)
Make a new image after the improved phase calibration.
#In CASA
tclean(vis='tl016b_cal1.ms', field='J1154+6022', imagename='J1154_sc2', imsize=[640], cell=['0.0003arcsec'], stokes='I', deconvolver='clark', weighting='natural', niter=1000, interactive=True, savemodel='modelcolumn')
Amplitude Self-Calibration
#In CASA
gaincal(vis='tl016b_cal1.ms', field='J1154+6022', caltable='tl016b_cal1.apcal', solint='inf', refant='PT', minblperant=4, gaintype='G', calmode='ap', solnorm=True, gaintable=['tl016b_cal1.dcal','tl016b_cal1.pcal'], interp=['linear','linear'], parang=False)
Apply the amplitude solutions to the phase reference calibrator.
#In CASA
applycal(vis='tl016b_cal1.ms', field='J1154+6022', gaintable=['tl016b_cal1.dcal',tl016b_cal1.pcal','tl016b_cal1.apcal'], interp=['linear','linear','linear'], parang=False)
Apply Calibration to Science Target
#In CASA
applycal(vis='tl016ac_cal1.ms', field='J1203+6031', gaintable=['tl016ac_cal1.dcal',tl016ac_cal1.pcal','tl016ac_cal1.apcal'], interp=['linear','linear','linear'], applymode='calonly', parang=False)
Split Out Science Target
#In CASA
split(vis='tl016b_cal1.ms', outputvis='tl016b_cal2.ms', field='J1203+6031', datacolumn='corrected')
Image the Science Target
#In CASA
tclean(vis='tl016b_cal2.ms', field='J1203+6031', imagename='J1203_im1', imsize=[640], cell=['0.0003arcsec'], stokes='I', deconvolver='clark', weighting='natural', niter=1000, interactive=True, savemodel='modelcolumn')
