Testing Date - 2003.12.15 Tester - S.T. Myers (AOC) Platform - Linux (sandrock) P4 2.00 GHz 512MB Last Revised - 2003.12.19 Note: bugs are denoted by lines with prefix: >>>BUG: and queries are denoted by lines with prefix: >>>QUERY: while comments are prefixed by: >>>COMMENT: Some enhancement requests are given after >>>REQUEST: Notes added later for clarification are indicated by >>>NOTE: ------------------------------------------------------------------------------- GOAL: carry out testing of IRAM data =============================================================================== Date - 2003.12.18 Version - stable (1.9 build 275) Directory - /home/sandrock/smyers/Testing/2003-12-15/ Data - /home/sola/dss/alma.tsting.data.tmp/l02d/fits/* =============================================================================== 1. [2003.12.18] Load data using almatifiller function, script /home/sandrock/smyers/Testing/2003-12-15/loaddata.g There were 4 days of data: --------------------------------------------------------------- 23-jan-2002-l02d-*.fits (01-11) Crashed on file /home/sola/dss/alma.tsting.data.tmp/l02d/fits/23-jan-2002-l02d-04.fits (others ok) 26-jan-2002-l02d-*.fits (01-10) Crashed on file /home/sola/dss/alma.tsting.data.tmp/l02d/fits/26-jan-2002-l02d-01.fits /home/sola/dss/alma.tsting.data.tmp/l02d/fits/26-jan-2002-l02d-07.fits (probably others bad also) 29-jan-2002-l02d-*.fits (01-20) Crashed on file /home/sola/dss/alma.tsting.data.tmp/l02d/fits/29-jan-2002-l02d-03.fits (probably others bad also) 30-mar-2002-l02d-*.fits (01-14) Crashed on files /home/sola/dss/alma.tsting.data.tmp/l02d/fits/30-mar-2002-l02d-12.fits /home/sola/dss/alma.tsting.data.tmp/l02d/fits/30-mar-2002-l02d-13.fits (others ok) =============================================================================== Date - 2003.12.19 Version - stable (1.9 build 275) Directory - /home/sandrock/smyers/Testing/2003-12-15/ Data - /home/sandrock2/smyers/Testing/Data/L02D/* =============================================================================== 2. [2003.12.19] Data 26-jan-2002 (Day 2) Get clean copy of data from Leonardo Testi Load data using almatifiller function, script /home/sandrock/smyers/Testing/2003-12-15/loaddata.g 23-jan-2002-l02d-*.fits reported to be bad. Skip this day. Start with 2nd day (26-jan-2002) --------------------------------------------------------------- 26-jan-2002-l02d-*.fits (01-10) MeasurementSet Name: /home/sandrock/smyers/Testing/2003-12-15/26-jan-2002-l02d.ms MS Version 2 Observer: Project: L02D Observation: IRAM_PDB Data records: 35040 Total integration time = 101960 seconds Observed from 27-Jan-2002/05:45:47 to 28-Jan-2002/10:05:07 ObservationID = 1 ArrayID = 1 Date Timerange Scan Field DataDescIds 27-Jan-2002/05:45:47.0 - 05:45:47.0 2604 3C273 [1,..., 32] 05:46:47.0 - 05:46:47.0 2605 3C273 [1,..., 32] 05:47:47.0 - 05:47:47.0 2606 3C273 [1,..., 32] 05:48:47.0 - 05:48:47.0 2607 3C273 [1,..., 32] 05:49:47.0 - 05:49:47.0 2608 3C273 [1,..., 32] 05:50:47.0 - 05:50:47.0 2609 3C273 [1,..., 32] 05:51:47.0 - 05:51:47.0 2610 3C273 [1,..., 32] 05:52:47.0 - 05:52:47.0 2611 3C273 [1,..., 32] 05:53:47.0 - 05:53:47.0 2612 3C273 [1,..., 32] 05:54:47.0 - 05:54:47.0 2613 3C273 [1,..., 32] 06:04:36.5 - 06:04:36.5 2616 MWC349 [1,..., 32] 06:05:21.5 - 06:05:21.5 2617 MWC349 [1,..., 32] 06:06:06.5 - 06:06:06.5 2618 MWC349 [1,..., 32] 06:06:51.5 - 06:06:51.5 2619 MWC349 [1,..., 32] 06:07:36.5 - 06:07:36.5 2620 MWC349 [1,..., 32] 28-Jan-2002/07:26:37.0 - 07:26:37.0 2645 3C273 [1,..., 32] 07:27:37.0 - 07:27:37.0 2646 3C273 [1,..., 32] 07:28:37.0 - 07:28:37.0 2647 3C273 [1,..., 32] 07:29:37.0 - 07:29:37.0 2648 3C273 [1,..., 32] 07:30:37.0 - 07:30:37.0 2649 3C273 [1,..., 32] 07:31:37.0 - 07:31:37.0 2650 3C273 [1,..., 32] 07:32:37.0 - 07:32:37.0 2651 3C273 [1,..., 32] 07:33:37.0 - 07:33:37.0 2652 3C273 [1,..., 32] 07:34:37.0 - 07:34:37.0 2653 3C273 [1,..., 32] 07:35:37.0 - 07:35:37.0 2654 3C273 [1,..., 32] 07:47:11.5 - 07:47:11.5 2658 MWC349 [1,..., 32] 07:47:56.5 - 07:47:56.5 2659 MWC349 [1,..., 32] 07:48:41.5 - 07:48:41.5 2660 MWC349 [1,..., 20] 07:49:26.5 - 07:49:26.5 2661 MWC349 [1,..., 32] 07:50:11.5 - 07:50:11.5 2662 MWC349 [1,..., 32] 08:16:22.5 - 08:16:22.5 2672 2013+370 [1,..., 32] 08:17:07.5 - 08:17:07.5 2673 2013+370 [1,..., 32] 08:17:52.5 - 08:17:52.5 2674 2013+370 [1,..., 32] 08:21:35.0 - 08:21:35.0 2679 20126+4104 [1,..., 32] 08:22:35.0 - 08:22:35.0 2680 20126+4104 [1,..., 32] 08:23:35.0 - 08:23:35.0 2681 20126+4104 [1,..., 32] 08:24:35.0 - 08:24:35.0 2682 20126+4104 [1,..., 32] 08:25:35.0 - 08:25:35.0 2683 20126+4104 [1,..., 32] 08:26:35.0 - 08:26:35.0 2684 20126+4104 [1,..., 32] 08:27:35.0 - 08:27:35.0 2685 20126+4104 [1,..., 32] 08:28:35.0 - 08:28:35.0 2686 20126+4104 [1,..., 32] 08:29:35.0 - 08:29:35.0 2687 20126+4104 [1,..., 32] 08:30:35.0 - 08:30:35.0 2688 20126+4104 [1,..., 32] 08:31:35.0 - 08:31:35.0 2689 20126+4104 [1,..., 32] 08:32:35.0 - 08:32:35.0 2690 20126+4104 [1,..., 32] 08:33:35.0 - 08:33:35.0 2691 20126+4104 [1,..., 32] 08:34:35.0 - 08:34:35.0 2692 20126+4104 [1,..., 32] 08:35:35.0 - 08:35:35.0 2693 20126+4104 [1,..., 32] 08:36:35.0 - 08:36:35.0 2694 20126+4104 [1,..., 32] 08:37:35.0 - 08:37:35.0 2695 20126+4104 [1,..., 32] 08:38:35.0 - 08:38:35.0 2696 20126+4104 [1,..., 32] 08:39:35.0 - 08:39:35.0 2697 20126+4104 [1,..., 32] 08:40:35.0 - 08:40:35.0 2698 20126+4104 [1,..., 32] 08:43:15.5 - 08:43:15.5 2703 2013+370 [1,..., 32] 08:44:00.5 - 08:44:00.5 2704 2013+370 [1,..., 32] 08:44:45.5 - 08:44:45.5 2705 2013+370 [1,..., 32] 08:48:19.0 - 08:48:19.0 2710 20126+4104 [1,..., 32] 08:49:19.0 - 08:49:19.0 2711 20126+4104 [1,..., 32] 08:50:19.0 - 08:50:19.0 2712 20126+4104 [1,..., 32] 08:51:19.0 - 08:51:19.0 2713 20126+4104 [1,..., 32] 08:52:19.0 - 08:52:19.0 2714 20126+4104 [1,..., 32] 08:53:19.0 - 08:53:19.0 2715 20126+4104 [1,..., 32] 08:54:19.0 - 08:54:19.0 2716 20126+4104 [1,..., 32] 08:55:19.0 - 08:55:19.0 2717 20126+4104 [1,..., 32] 08:56:19.0 - 08:56:19.0 2718 20126+4104 [1,..., 32] 08:57:19.0 - 08:57:19.0 2719 20126+4104 [1,..., 32] 08:58:19.0 - 08:58:19.0 2720 20126+4104 [1,..., 32] 08:59:19.0 - 08:59:19.0 2721 20126+4104 [1,..., 32] 09:00:19.0 - 09:00:19.0 2722 20126+4104 [1,..., 32] 09:01:19.0 - 09:01:19.0 2723 20126+4104 [1,..., 32] 09:02:19.0 - 09:02:19.0 2724 20126+4104 [1,..., 32] 09:03:19.0 - 09:03:19.0 2725 20126+4104 [1,..., 32] 09:04:19.0 - 09:04:19.0 2726 20126+4104 [1,..., 32] 09:05:19.0 - 09:05:19.0 2727 20126+4104 [1,..., 32] 09:06:19.0 - 09:06:19.0 2728 20126+4104 [1,..., 32] 09:07:19.0 - 09:07:19.0 2729 20126+4104 [1,..., 32] 09:10:02.5 - 09:10:02.5 2734 2013+370 [1,..., 32] 09:10:47.5 - 09:10:47.5 2735 2013+370 [1,..., 32] 09:11:32.5 - 09:11:32.5 2736 2013+370 [1,..., 20] 09:19:09.5 - 09:19:09.5 2742 2013+370 [1,..., 32] 09:19:54.5 - 09:19:54.5 2743 2013+370 [1,..., 32] 09:20:39.5 - 09:20:39.5 2744 2013+370 [1,..., 32] 09:28:35.0 - 09:28:35.0 2749 20126+4104 [1,..., 32] 09:29:35.0 - 09:29:35.0 2750 20126+4104 [1,..., 32] 09:30:35.0 - 09:30:35.0 2751 20126+4104 [1,..., 32] 09:31:35.0 - 09:31:35.0 2752 20126+4104 [1,..., 32] 09:32:35.0 - 09:32:35.0 2753 20126+4104 [1,..., 32] 09:33:35.0 - 09:33:35.0 2754 20126+4104 [1,..., 32] 09:34:35.0 - 09:34:35.0 2755 20126+4104 [1,..., 32] 09:35:35.0 - 09:35:35.0 2756 20126+4104 [1,..., 32] 09:36:35.0 - 09:36:35.0 2757 20126+4104 [1,..., 32] 09:37:35.0 - 09:37:35.0 2758 20126+4104 [1,..., 32] 09:38:35.0 - 09:38:35.0 2759 20126+4104 [1,..., 32] 09:39:35.0 - 09:39:35.0 2760 20126+4104 [1,..., 32] 09:40:35.0 - 09:40:35.0 2761 20126+4104 [1,..., 32] 09:41:35.0 - 09:41:35.0 2762 20126+4104 [1,..., 20] 09:42:35.0 - 09:42:35.0 2763 20126+4104 [1,..., 32] 09:43:35.0 - 09:43:35.0 2764 20126+4104 [1,..., 32] 09:44:35.0 - 09:44:35.0 2765 20126+4104 [1,..., 32] 09:45:35.0 - 09:45:35.0 2766 20126+4104 [1,..., 32] 09:46:35.0 - 09:46:35.0 2767 20126+4104 [1,..., 32] 09:47:35.0 - 09:47:35.0 2768 20126+4104 [1,..., 32] 09:50:18.5 - 09:50:18.5 2773 2013+370 [1,..., 32] 09:51:03.5 - 09:51:03.5 2774 2013+370 [1,..., 32] 09:51:48.5 - 09:51:48.5 2775 2013+370 [1,..., 32] 10:00:07.0 - 10:00:07.0 2780 20126+4104 [1,..., 32] 10:01:07.0 - 10:01:07.0 2781 20126+4104 [1,..., 32] 10:02:07.0 - 10:02:07.0 2782 20126+4104 [1,..., 32] 10:03:07.0 - 10:03:07.0 2783 20126+4104 [1,..., 32] 10:04:07.0 - 10:04:07.0 2784 20126+4104 [1,..., 32] 10:05:07.0 - 10:05:07.0 2785 20126+4104 [1,..., 20] Fields: 4 ID Name Right Ascension Declination Epoch 1 3C273 12:29:06.70 +02.03.08.60 J2000 2 MWC349 20:32:45.54 +40.39.36.64 J2000 3 2013+370 20:15:28.73 +37.10.59.51 J2000 4 20126+4104 20:14:26.04 +41.13.32.52 J2000 Data descriptions: 32 (32 spectral windows and 1 polarization setups) ID Ref.Freq #Chans Resolution TotalBW Correlations 1 93620.8MHz 1 38000 kHz 38000 kHz XX 2 96409 MHz 1 -38000 kHz 38000 kHz XX 3 93620.8MHz 512 78.125 kHz 40000 kHz XX 4 96409 MHz 512 -78.125kHz 40000 kHz XX 5 93478.8MHz 1 152000 kHz 152000 kHz XX 6 96551 MHz 1 -152000kHz 152000 kHz XX 7 93479.4MHz 128 1250 kHz 160000 kHz XX 8 96550.4MHz 128 -1250 kHz 160000 kHz XX 9 93280.8MHz 1 38000 kHz 38000 kHz XX 10 96749 MHz 1 -38000 kHz 38000 kHz XX 11 93280.9MHz 512 78.125 kHz 40000 kHz XX 12 96749 MHz 512 -78.125kHz 40000 kHz XX 13 93673.8MHz 1 304000 kHz 304000 kHz XX 14 96356 MHz 1 -304000kHz 304000 kHz XX 15 93675 MHz 128 2500 kHz 320000 kHz XX 16 96354.8MHz 128 -2500 kHz 320000 kHz XX 17 93338.8MHz 1 152000 kHz 152000 kHz XX 18 96691 MHz 1 -152000kHz 152000 kHz XX 19 93339.4MHz 128 1250 kHz 160000 kHz XX 20 96690.4MHz 128 -1250 kHz 160000 kHz XX 21 238082 MHz 1 38000 kHz 38000 kHz XX 22 241017 MHz 1 -38000 kHz 38000 kHz XX 23 238082 MHz 512 78.125 kHz 40000 kHz XX 24 241017 MHz 512 -78.125kHz 40000 kHz XX 25 238215 MHz 1 304000 kHz 304000 kHz XX 26 240884 MHz 1 -304000kHz 304000 kHz XX 27 238216 MHz 128 2500 kHz 320000 kHz XX 28 240883 MHz 128 -2500 kHz 320000 kHz XX 29 237955 MHz 1 304000 kHz 304000 kHz XX 30 241144 MHz 1 -304000kHz 304000 kHz XX 31 237956 MHz 128 2500 kHz 320000 kHz XX 32 241143 MHz 128 -2500 kHz 320000 kHz XX Feeds: 5: printing first row only Antenna Spectral Window # Receptors Polarizations 1 -1 1 [ X] Antennas: 5: ID Name Station Diam. Long. Lat. 1 1 107 15.0 m -110.56.57.6 +19.54.31.4 2 2 129 15.0 m -155.58.24.6 +42.46.20.8 3 3 304 15.0 m -046.25.36.7 -34.55.04.3 4 4 212 15.0 m -088.54.01.5 -01.06.57.5 5 5 323 15.0 m +070.02.40.6 -19.04.06.1 Tables: MAIN 35040 rows ANTENNA 5 rows DATA_DESCRIPTION 32 rows DOPPLER FEED 5 rows FIELD 4 rows FLAG_CMD FREQ_OFFSET HISTORY OBSERVATION 1 row POINTING POLARIZATION 1 row PROCESSOR SOURCE 4 rows SPECTRAL_WINDOW 32 rows STATE SYSCAL WEATHER --------------------------------------------------------------- 3. [2003.12.22] Continue reduction, start with Day 2 = 26-jan-2002 - include 'iramcalibrater.g'; T - shadow(msname="26-jan-2002-l02d.ms", trial=F, minsep=15.0); T - ical:=iramcalibrater(msname="26-jan-2002-l02d.ms", initcal=T); - ical.phcor(trial=F); Found spwid for band 3mm is [1 2 5 6 9 10 13 14 17 18] Found spwid for band 3mm is [3 4 7 8 11 12 15 16 19 20] Found spwid for band 1mm is [21 22 25 26 29 30 15 16 19 20] Found spwid for band 1mm is [23 24 27 28 31 32 15 16 19 20] : index (= 47) out of range, array length = 45 File: iramcalutil.g, Line 691 Stack: .(), iramcalibrater.g line 200 .() We will hope this is benign. Output: ----Beginning method: phcor successful readonly open of default-locked table 26-jan-2002-l02d.ms/SOURCE: 14 columns, 4 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/FIELD: 9 columns, 4 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/SPECTRAL_WINDOW: 14 columns, 32 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/ANTENNA: 8 columns, 5 rows successful read/write open of default-locked table 26-jan-2002-l02d.ms: 29 columns, 35040 rows Uncorr Flag for ant1 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant2 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant3 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant4 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant5 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant1 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant2 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant3 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant4 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant5 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant1 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant2 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant3 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant4 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant5 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant1 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant2 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant3 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant4 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant5 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant1 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant2 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant3 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant4 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant5 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant1 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant2 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant3 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant4 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant5 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant1 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant2 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant3 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant4 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant5 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant1 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant2 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant3 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant4 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant5 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant1 scan 2614 to 2616 Uncorr Flag for ant2 scan 2614 to 2616 Uncorr Flag for ant3 scan 2614 to 2616 Uncorr Flag for ant4 scan 2614 to 2616 Uncorr Flag for ant5 scan 2614 to 2616 Uncorr Flag for ant1 scan 2645 to 2647 Uncorr Flag for ant3 scan 2645 to 2647 Uncorr Flag for ant1 scan 2647 to 2649 2646 to 2648 Uncorr Flag for ant3 scan 2647 to 2649 2646 to 2648 Uncorr Flag for ant5 scan 2646 to 2648 Uncorr Flag for ant1 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant3 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant5 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant1 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant3 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant5 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant1 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant3 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant4 scan 2649 to 2651 Uncorr Flag for ant5 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant1 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant3 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant4 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant5 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant1 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant3 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant4 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant5 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant1 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant3 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant4 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant5 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant1 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant3 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant4 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant5 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant1 scan 2655 to 2657 Uncorr Flag for ant3 scan 2655 to 2657 Uncorr Flag for ant4 scan 2655 to 2657 Uncorr Flag for ant5 scan 2655 to 2657 Uncorr Flag for ant1 scan 2702 to 2704 Uncorr Flag for ant2 scan 2702 to 2704 Uncorr Flag for ant3 scan 2702 to 2704 Uncorr Flag for ant4 scan 2702 to 2704 Uncorr Flag for ant5 scan 2702 to 2704 Uncorr Flag for ant1 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant2 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant3 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant4 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant5 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant1 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant2 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant3 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant4 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant5 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant1 scan 2706 to 2708 Uncorr Flag for ant2 scan 2706 to 2708 Uncorr Flag for ant3 scan 2706 to 2708 Uncorr Flag for ant4 scan 2706 to 2708 Uncorr Flag for ant5 scan 2706 to 2708 Uncorr Flag for ant1 scan 2741 to 2743 Uncorr Flag for ant2 scan 2741 to 2743 Uncorr Flag for ant3 scan 2741 to 2743 Uncorr Flag for ant4 scan 2741 to 2743 Uncorr Flag for ant5 scan 2741 to 2743 Uncorr Flag for ant1 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant2 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant3 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant4 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant5 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant1 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant2 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant3 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant4 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant5 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant1 scan 2745 to 2747 Uncorr Flag for ant2 scan 2745 to 2747 Uncorr Flag for ant3 scan 2745 to 2747 Uncorr Flag for ant4 scan 2745 to 2747 Uncorr Flag for ant5 scan 2745 to 2747 Uncorr Flag for ant1 scan 2773 to 2775 Uncorr Flag for ant2 scan 2773 to 2775 Uncorr Flag for ant3 scan 2773 to 2775 Uncorr Flag for ant5 scan 2773 to 2775 Uncorr Flag for ant1 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant2 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant3 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant5 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant1 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant2 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant3 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant5 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant1 scan 2776 to 2778 Uncorr Flag for ant2 scan 2776 to 2778 Uncorr Flag for ant3 scan 2776 to 2778 Uncorr Flag for ant5 scan 2776 to 2778 successful readonly open of default-locked table 26-jan-2002-l02d.ms/SPECTRAL_WINDOW: 14 columns, 32 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/SOURCE: 14 columns, 4 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/FIELD: 9 columns, 4 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/SPECTRAL_WINDOW: 14 columns, 32 rows successful readonly open of default-locked table 26-jan-2002-l02d.ms/ANTENNA: 8 columns, 5 rows successful read/write open of default-locked table 26-jan-2002-l02d.ms: 29 columns, 35040 rows Uncorr Flag for ant1 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant2 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant3 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant4 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant5 scan 2606 to 2608 2605 to 2607 Uncorr Flag for ant1 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant2 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant3 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant4 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant5 scan 2607 to 2609 2606 to 2608 Uncorr Flag for ant1 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant2 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant3 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant4 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant5 scan 2608 to 2610 2607 to 2609 Uncorr Flag for ant1 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant2 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant3 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant4 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant5 scan 2609 to 2611 2608 to 2610 Uncorr Flag for ant1 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant2 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant3 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant4 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant5 scan 2610 to 2612 2609 to 2611 Uncorr Flag for ant1 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant2 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant3 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant4 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant5 scan 2611 to 2613 2610 to 2612 Uncorr Flag for ant1 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant2 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant3 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant4 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant5 scan 2612 to 2614 2611 to 2613 Uncorr Flag for ant1 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant2 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant3 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant4 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant5 scan 2613 to 2615 2612 to 2614 Uncorr Flag for ant1 scan 2614 to 2616 Uncorr Flag for ant2 scan 2614 to 2616 Uncorr Flag for ant3 scan 2614 to 2616 Uncorr Flag for ant4 scan 2614 to 2616 Uncorr Flag for ant5 scan 2614 to 2616 Uncorr Flag for ant1 scan 2644 to 2646 Uncorr Flag for ant3 scan 2644 to 2646 Uncorr Flag for ant5 scan 2644 to 2646 Uncorr Flag for ant1 scan 2646 to 2648 2645 to 2647 Uncorr Flag for ant3 scan 2646 to 2648 2645 to 2647 Uncorr Flag for ant5 scan 2646 to 2648 2645 to 2647 Uncorr Flag for ant1 scan 2647 to 2649 2646 to 2648 Uncorr Flag for ant3 scan 2647 to 2649 2646 to 2648 Uncorr Flag for ant5 scan 2647 to 2649 2646 to 2648 Uncorr Flag for ant1 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant3 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant4 scan 2647 to 2649 Uncorr Flag for ant5 scan 2648 to 2650 2647 to 2649 Uncorr Flag for ant1 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant3 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant4 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant5 scan 2649 to 2651 2648 to 2650 Uncorr Flag for ant1 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant3 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant4 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant5 scan 2650 to 2652 2649 to 2651 Uncorr Flag for ant1 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant3 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant4 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant5 scan 2651 to 2653 2650 to 2652 Uncorr Flag for ant1 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant3 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant4 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant5 scan 2652 to 2654 2651 to 2653 Uncorr Flag for ant1 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant3 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant4 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant5 scan 2653 to 2655 2652 to 2654 Uncorr Flag for ant1 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant3 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant4 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant5 scan 2654 to 2656 2653 to 2655 Uncorr Flag for ant1 scan 2655 to 2657 Uncorr Flag for ant3 scan 2655 to 2657 Uncorr Flag for ant4 scan 2655 to 2657 Uncorr Flag for ant5 scan 2655 to 2657 Uncorr Flag for ant1 scan 2702 to 2704 Uncorr Flag for ant2 scan 2702 to 2704 Uncorr Flag for ant3 scan 2702 to 2704 Uncorr Flag for ant4 scan 2702 to 2704 Uncorr Flag for ant5 scan 2702 to 2704 Uncorr Flag for ant1 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant2 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant3 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant4 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant5 scan 2704 to 2706 2703 to 2705 Uncorr Flag for ant1 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant2 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant3 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant4 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant5 scan 2705 to 2707 2704 to 2706 Uncorr Flag for ant1 scan 2706 to 2708 Uncorr Flag for ant2 scan 2706 to 2708 Uncorr Flag for ant3 scan 2706 to 2708 Uncorr Flag for ant4 scan 2706 to 2708 Uncorr Flag for ant5 scan 2706 to 2708 Uncorr Flag for ant1 scan 2741 to 2743 Uncorr Flag for ant2 scan 2741 to 2743 Uncorr Flag for ant3 scan 2741 to 2743 Uncorr Flag for ant4 scan 2741 to 2743 Uncorr Flag for ant5 scan 2741 to 2743 Uncorr Flag for ant1 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant2 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant3 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant4 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant5 scan 2743 to 2745 2742 to 2744 Uncorr Flag for ant1 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant2 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant3 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant4 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant5 scan 2744 to 2746 2743 to 2745 Uncorr Flag for ant1 scan 2745 to 2747 2772 to 2774 Uncorr Flag for ant2 scan 2745 to 2747 2772 to 2774 Uncorr Flag for ant3 scan 2745 to 2747 2772 to 2774 Uncorr Flag for ant4 scan 2745 to 2747 Uncorr Flag for ant5 scan 2745 to 2747 2772 to 2774 Uncorr Flag for ant1 scan 2774 to 2776 2773 to 2775 Uncorr Flag for ant2 scan 2774 to 2776 2773 to 2775 Uncorr Flag for ant3 scan 2774 to 2776 2773 to 2775 Uncorr Flag for ant5 scan 2774 to 2776 2773 to 2775 Uncorr Flag for ant1 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant2 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant3 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant5 scan 2775 to 2777 2774 to 2776 Uncorr Flag for ant1 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant2 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant3 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant5 scan 2776 to 2778 2774 to 2776 Uncorr Flag for ant1 scan 2776 to 2778 Uncorr Flag for ant2 scan 2776 to 2778 Uncorr Flag for ant3 scan 2776 to 2778 Uncorr Flag for ant5 scan 2776 to 2778 successful readonly open of default-locked table 26-jan-2002-l02d.ms/SPECTRAL_WINDOW: 14 columns, 32 rows -----Finished method: phcor >>>COMMENT: phcor did not seem to fail as it said it might in the Cookbook. Also, I would put the phcor description in the filling section and not the calibration section. At this point make backup of ms in case we need to return to this point: cp -r 26-jan-2002-l02d.ms 26-jan-2002-l02d.b1 =============================================================================== Date - 2004.1.6 Version - stable (1.9 build 275) Directory - /home/sandrock/smyers/Testing/2003-12-15/ Data - /home/sola/dss/alma.tsting.data.tmp/l02d/fits/* =============================================================================== 4. [2004.1.6] Figure out what the spectral windows contain: >>>COMMENT: THIS APPEARS TO BE DSB DATA Data descriptions: 32 (32 spectral windows and 1 polarization setups) 3mm Data: ID Ref.Freq #Chans Resolution TotalBW Correlations 1 93620.8MHz 1 38000 kHz 38000 kHz XX 2 96409 MHz 1 -38000 kHz 38000 kHz XX 3 93620.8MHz 512 78.125 kHz 40000 kHz XX 4 96409 MHz 512 -78.125kHz 40000 kHz XX 5 93478.8MHz 1 152000 kHz 152000 kHz XX 6 96551 MHz 1 -152000kHz 152000 kHz XX 7 93479.4MHz 128 1250 kHz 160000 kHz XX 8 96550.4MHz 128 -1250 kHz 160000 kHz XX 9 93280.8MHz 1 38000 kHz 38000 kHz XX 10 96749 MHz 1 -38000 kHz 38000 kHz XX 11 93280.9MHz 512 78.125 kHz 40000 kHz XX 12 96749 MHz 512 -78.125kHz 40000 kHz XX 13 93673.8MHz 1 304000 kHz 304000 kHz XX 14 96356 MHz 1 -304000kHz 304000 kHz XX 15 93675 MHz 128 2500 kHz 320000 kHz XX 16 96354.8MHz 128 -2500 kHz 320000 kHz XX 17 93338.8MHz 1 152000 kHz 152000 kHz XX 18 96691 MHz 1 -152000kHz 152000 kHz XX 19 93339.4MHz 128 1250 kHz 160000 kHz XX 20 96690.4MHz 128 -1250 kHz 160000 kHz XX 1mm Data: ID Ref.Freq #Chans Resolution TotalBW Correlations 21 238082 MHz 1 38000 kHz 38000 kHz XX 22 241017 MHz 1 -38000 kHz 38000 kHz XX 23 238082 MHz 512 78.125 kHz 40000 kHz XX 24 241017 MHz 512 -78.125kHz 40000 kHz XX 25 238215 MHz 1 304000 kHz 304000 kHz XX 26 240884 MHz 1 -304000kHz 304000 kHz XX 27 238216 MHz 128 2500 kHz 320000 kHz XX 28 240883 MHz 128 -2500 kHz 320000 kHz XX 29 237955 MHz 1 304000 kHz 304000 kHz XX 30 241144 MHz 1 -304000kHz 304000 kHz XX 31 237956 MHz 128 2500 kHz 320000 kHz XX 32 241143 MHz 128 -2500 kHz 320000 kHz XX Looks like these are overlapping but somewhat distinct windows, so we will need to reduce them all. Note that the continuum (1 channel) windows are just sums over the line channels. Look at the data: - include 'viewer.g' - dv.gui() There are two scans on 3C273 and MWC349 on 27-Jan a day before the bulk of the data. The first scan on 3C273 is clearly bad, I see no reason to keep the MWC349 scan either given that these scans are repeated on the second day. It is useful to put the Channels on the y-axis which puts time on the animation axis. The viewer is not described in the cookbook, so I will skip this for now. DO WE WANT TO ADVOCATE THE VIEWER FOR MS EDITING? Use msplot to look at data as in cookbook: - plot := msplot(msfile='26-jan-2002-l02d.ms', edit=T); >>>COMMENT: our field ids are: Fields: 4 ID Name Right Ascension Declination Epoch 1 3C273 12:29:06.70 +02.03.08.60 J2000 2 MWC349 20:32:45.54 +40.39.36.64 J2000 3 2013+370 20:15:28.73 +37.10.59.51 J2000 4 20126+4104 20:14:26.04 +41.13.32.52 J2000 You can see the bad scan on 3C273 on 27-Jan and the orphaned MWC349 scan that day also. Plot up amp vs. channel for the various windows: For the 128-channel data, the gibbs channels 1,64,65,128 are generally bad. Looking at amplitudes SPW = 7,8,19,20,27,28,31,32 obviously bad=1,128 SPW = 15,16 obviously bad=1,64,65,128 To be conservative, should flag 1,64,65,128 on all these windows. For the 512-channel data, the lowest channels were noisy, particularly the first channel or two. Look at the calibrater data amp vs. time. Generally pretty good, particularly on 3C273 and MWC349 which were only single scans. 2013+370 has problems with AN1 in scans at 0842 and 0920, about 30% lower. I'm not sure how the gain calibration will handle this, probably poorly. 5. [2004.1.6] Flag data. Delete times 1-15 (27-Jan-2002/05:45:47.0 to 06:07:36.5) - include 'flagger.g' - fg:=flagger('26-jan-2002-l02d.ms'); - fg.settimerange(starttime='27-Jan-2002/05:00:00.0', endtime='27-Jan-2002/07:00:00.0'); - fg.state(); Measurement Set : "26-jan-2002-l02d.ms" Timerange: starttime: "27-Jan-2002/05:00:00.0" endtime: "27-Jan-2002/07:00:00.0" Times: times: [] delta: "10s" Antennas : [] Baselines : [] Feeds : [] UV-Range : [] Array IDs : [] Field IDs : [] Spectral window IDs : [] Channels : [] Polarizations : [] Flagmode : 'flagged ' Last query : '' - fg.flag(trial=T); Flagging would flag 4800 rows - fg.flag(); Flagging 4800 rows : tf[, , ] invalid array addressing File: flagger.g, Line 213 Stack: .(), flagger.g line 162 .() Did this work???? Check back in the viewer I guess... (NO THIS DID NOT FLAG THE DATA) Try this instead - fg.timerange("27-Jan-2002/05:00:00.0", "27-Jan-2002/07:00:00.0",trial=T); Flagging would occur for 27-Jan-2002/05:00:00.0 to 27-Jan-2002/07:00:00.0 Flagging would flag 4800 rows - fg.timerange("27-Jan-2002/05:00:00.0", "27-Jan-2002/07:00:00.0"); Flagging 27-Jan-2002/05:00:00.0 to 27-Jan-2002/07:00:00.0 Flagging 4800 rows : tf[, , ] invalid array addressing File: flagger.g, Line 213 Stack: .(), flagger.g line 162 .(), flagger.g line 597 .(), flagger.g line 646 .() Crap! Try specifying spectral windows or something? - fg.timerange("27-Jan-2002/05:00:00.0", "27-Jan-2002/07:00:00.0", trial=F); T OK, this worked. Maybe have to go through windows of the same shape. First the 1-channel windows: - fg.setids(spectralwindowid=[1,2,5,6,9,10,13,14,17,18,21,22,25,26,29,30]); - fg.settimerange(starttime='27-Jan-2002/05:00:00.0', endtime='27-Jan-2002/07:00:00.0'); - fg.flag() Flagging 2400 rows Now the 128-channel windows: - fg.setids(spectralwindowid=[7,8,15,16,19,20,27,28,31,32]); - fg.flag() Flagging 1500 rows Now the 512-channel windows: - fg.setids(spectralwindowid=[3,4,11,12,23,24]); - fg.flag() Flagging 900 rows This worked. THERE SHOULD BE A NOTE TO THIS EFFECT IN THE COOKBOOK AND IN THE FLAGGER URM DOCS. >>>BUG: submitted as defect AOCso04707 Now flag the bad channels. - fg.reset() - fg.setids(spectralwindowid=[7,8,15,16,19,20,27,28,31,32]); - fg.setchan(chan=[1,64,65,128]); : different-length operands in expression (4 vs. 32): (chan > private.nchan) File: flagger.g, Line 365 Stack: any(), flagger.g line 365 .() What the heck??? - fg.state() Looks like the channels got set. Try flagging. - fg.flag(trial=T) Flagging would flag 10940 rows - fg.flag() Flagging 10940 rows Checked in msplot, seems to have flagged these correctly. >>>BUG: submitted as AOCso04708 Now the 512-ch windows first 2 chan. - fg.setids(spectralwindowid=[3,4,11,12,23,24]); - fg.setchan(chan=[1,2]); : different-length operands in expression (2 vs. 32): (chan > private.nchan) File: flagger.g, Line 365 Stack: any(), flagger.g line 365 .() - fg.state() - fg.flag() Flagging 6580 rows For now, leave ANT 1 in there. - fg.done(); >>>COMMENT: these uses of flagger are not detailed in the Cookbook, though they would seem to be common ones. >>>COMMENT: Kumar points out that autoflag is to be preferred and the Cookbook should be updated to show this. 6. [2004.1.6] Flux Scale From the file: /home/sola/dss/alma.tsting.data.tmp/l02d/l02d.note Calibrators =========== 96.5 GHz 241.1 GHz Fluxes (Jy): read computed read computed 3C273 10.87 10.87 F 6.00 6.00 F MWC349 1.01 M 0.95 1.75 M 1.75 F 2013+370 2.79 2.79 1.80 1.80 Set 3mm flux scale: - imset:=imager(filename='26-jan-2002-l02d.ms'); - imset.setjy(fieldid=1,spwid=1,fluxdensity=[10.87,0,0,0]); 3C273 spwid= 1 [I=10.87, Q=0, U=0, V=0] Jy, (user-specified) - imset.setjy(fieldid=3,spwid=1,fluxdensity=[2.79,0,0,0]); 2013+370 spwid= 1 [I=2.79, Q=0, U=0, V=0] Jy, (user-specified) Will have to do this for all 3mm windows. Best to loop: - for(spw in 1:20){ imset.setjy(fieldid=1,spwid=spw,fluxdensity=[10.87,0,0,0]); } - for(spw in 1:20){ imset.setjy(fieldid=3,spwid=spw,fluxdensity=[2.79,0,0,0]); } For all 1mm windows: - for(spw in 21:32){ imset.setjy(fieldid=1,spwid=spw,fluxdensity=[6.00,0,0,0]); } - for(spw in 21:32){ imset.setjy(fieldid=2,spwid=spw,fluxdensity=[1.75,0,0,0]); } - for(spw in 21:32){ imset.setjy(fieldid=3,spwid=spw,fluxdensity=[1.80,0,0,0]); } 6. [2004.1.7] 3mm Bandpass Calibration - cal:=calibrater(filename='26-jan-2002-l02d.ms'); Initial phase solutions for bpass calibrator (3C273) First the 128-chan windows [7,8,15,16,19,20] Leave out first and last 2 unflagged channels First the LSB [7,15,19] - cal.setdata(mode='channel',start=4, step=1, nchan=122, msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [7,15,19]'); >>>COMMENT: when setting for multiple spectral windows get error "Illegal step pixel = 1" which can be ignored. - cal.setsolvegainspline(table='26-jan-2002-l02d.3mmLSB.gcal0', mode='PHAS', preavg=0, # there isnt enough data for long avg splinetime=10000, # spline fit timescale (~3hrs), refant=2, # refant = 2, npointaver=10, # minimize phase wrap pblms phasewrap=260, append=F); # create new table - cal.solve(); Solving for G Slot= 1, field= 3C273 , spw= 7, nchan= 122 Slot= 2, field= 3C273 , spw= 15, nchan= 122 Slot= 3, field= 3C273 , spw= 19, nchan= 122 This produces files 26-jan-2002-l02d.ms.phase.log which contains *****PHASE summary******** Antenna based spline coefficients 1 [1.06204, 1.2447, 0.955554, 0.92996, 0, 0, 0, 0] 2 [0, 0, 0, 0, 0, 0, 0, 0] 3 [0.240531, 1.33002, 0.0651159, 0.559212, 0, 0, 0, 0] 4 [0.26282, -0.146545, 0.899324, 0.115507, 0, 0, 0, 0] 5 [0.288446, 3.48838, -0.227843, 1.25581, 0, 0, 0, 0] RMS Fit per baseline Antenna1 Antenna2 rmsfit 1 2 0.233101 1 3 0.099103 1 4 0.0782534 1 5 0.176591 2 3 0.312699 2 4 0.173017 2 5 0.411312 3 4 0.15762 3 5 0.128214 4 5 0.243542 and 26-jan-2002-l02d.ms.PHAS.ps These are pretty poor fits, mostly because the phases are not that bad and a linear fit would probably be as good. Good enough for this... Move these files - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.3mmLSB.gcal0.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.3mmLSB.gcal0.phase.log') Now the USB [8,16,20] - cal.reset(); - cal.setdata(mode='channel',start=4, step=1, nchan=122, msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [8,16,20]'); - cal.setsolvegainspline(table='26-jan-2002-l02d.3mmUSB.gcal0', mode='PHAS', preavg=0, # no preavg too short, splinetime=10000, # spline fit timescale (~3hrs), refant=2, # refant = 2, npointaver=10, # minimize phase wrap pblms phasewrap=260, append=F); # create new table - cal.solve(); Solving for G Slot= 1, field= 3C273 , spw= 8, nchan= 122 Slot= 2, field= 3C273 , spw= 16, nchan= 122 Slot= 3, field= 3C273 , spw= 20, nchan= 122 *****PHASE summary******** Antenna based spline coefficients 1 [1.06167, 1.25432, 0.965104, 0.925376, 0, 0, 0, 0] 2 [0, 0, 0, 0, 0, 0, 0, 0] 3 [0.220869, 1.35189, 0.0393676, 0.544402, 0, 0, 0, 0] 4 [0.256165, -0.154363, 0.909989, 0.107491, 0, 0, 0, 0] 5 [0.253357, 3.58891, -0.281848, 1.27535, 0, 0, 0, 0] RMS Fit per baseline Antenna1 Antenna2 rmsfit 1 2 0.242161 1 3 0.101163 1 4 0.0826642 1 5 0.180519 2 3 0.322332 2 4 0.179763 2 5 0.428326 3 4 0.161675 3 5 0.133327 4 5 0.252527 Similar to LSB... - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.3mmUSB.gcal0.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.3mmUSB.gcal0.phase.log') Now do bandpass solutions, first apply the USB phase table to preserve the LSB-USB offsets (per Kumar's instructions). - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [7,15,19]'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mmUSB.gcal0'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mm.bpoly', degamp=12, degphase=24, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); Solving for B Freq. group 3mm-LSB, spw= 7, nchan= 128 Freq. group 3mm-LSB, spw= 15, nchan= 128 Freq. group 3mm-LSB, spw= 19, nchan= 128 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmLSB.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmLSB.BP_amp.ps') These look pretty good. Though there are some amp offsets on some of the baselines due presumably to some non closing offsets? Now USB - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [8,16,20]'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mmUSB.gcal0'); Now append solution. Also use more amp deg (per Kumar) - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mm.bpoly', degamp=18, degphase=24, visnorm=F, bpnorm=F, refant=2, append=T); - cal.solve(); Solving for B Freq. group 3mm-USB, spw= 8, nchan= 128 Freq. group 3mm-USB, spw= 16, nchan= 128 Freq. group 3mm-USB, spw= 20, nchan= 128 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmUSB.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmUSB.BP_amp.ps') Looks pretty good. 7. [2004.1.7] 3mm Gain Calibration Phase calibrate the 3mm LSB & USB 128-ch data for the calibrators. Start with bandpass solution from 3C273, and resolve for all gains. - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setsolvegainspline(table='26-jan-2002-l02d.3mm.gcal', mode='PHAS', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260, append=F); - cal.solve(); Solving for G Slot= 1, field= 3C273 , spw= 7, nchan= 122 Slot= 2, field= 3C273 , spw= 8, nchan= 122 Slot= 3, field= 3C273 , spw= 15, nchan= 122 Slot= 4, field= 3C273 , spw= 16, nchan= 122 Slot= 5, field= 3C273 , spw= 19, nchan= 122 Slot= 6, field= 3C273 , spw= 20, nchan= 122 Slot= 7, field= MWC349 , spw= 7, nchan= 122 Slot= 8, field= MWC349 , spw= 8, nchan= 122 Slot= 9, field= MWC349 , spw= 15, nchan= 122 Slot= 10, field= MWC349 , spw= 16, nchan= 122 Slot= 11, field= MWC349 , spw= 19, nchan= 122 Slot= 12, field= MWC349 , spw= 20, nchan= 122 Slot= 13, field= 2013+370, spw= 7, nchan= 122 Slot= 14, field= 2013+370, spw= 8, nchan= 122 Slot= 15, field= 2013+370, spw= 15, nchan= 122 Slot= 16, field= 2013+370, spw= 16, nchan= 122 Slot= 17, field= 2013+370, spw= 19, nchan= 122 Slot= 18, field= 2013+370, spw= 20, nchan= 122 *****PHASE summary******** Antenna based spline coefficients 1 [0.931881, 3.39967, 1.46488, 1.54389, 0, 0, 0, 0] 2 [0, 0, 0, 0, 0, 0, 0, 0] 3 [0.520098, 1.26136, 1.30599, 1.00818, 0, 0, 0, 0] 4 [0.281919, -0.0497709, 1.40454, -0.0149999, 0, 0, 0, 0] 5 [1.1032, 3.54344, 1.37676, 2.15775, 0, 0, 0, 0] RMS Fit per baseline Antenna1 Antenna2 rmsfit 1 2 0.306304 1 3 0.174665 1 4 0.289856 1 5 0.351422 2 3 0.31314 2 4 0.250128 2 5 0.537221 3 4 0.246707 3 5 0.321986 4 5 0.537356 >>>COMMENT: got a bunch of "warnings" to the glish window saying: F-CHEB, abs(xcap).gt.1 These are fortran errors from the Chebyshev solution (these are from the IRAM code and appear in GILDAS also!) because there are channels outside the solution window. Will go away with this weeks new bpoly check-in (sez George). - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.3mm.gcal.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.3mm.gcal.phase.log') Fits look good. Now the amplitude calibration of 3mm 128-ch data. Start from bandpass and the phase solution above. Note that these will be merged with the previous phase solution in the table. - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvegainspline(table='26-jan-2002-l02d.3mm.gcal', mode='AMP', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260); WARN: Calibration table 26-jan-2002-l02d.3mm.gcal exists, and append=F. Therefore, this table will be updated. I think this is what is desired. - cal.solve(); Solving for G Slot= 1, field= 3C273 , spw= 7, nchan= 122 Slot= 2, field= 3C273 , spw= 8, nchan= 122 Slot= 3, field= 3C273 , spw= 15, nchan= 122 Slot= 4, field= 3C273 , spw= 16, nchan= 122 Slot= 5, field= 3C273 , spw= 19, nchan= 122 Slot= 6, field= 3C273 , spw= 20, nchan= 122 Slot= 7, field= MWC349 , spw= 7, nchan= 122 Slot= 8, field= MWC349 , spw= 8, nchan= 122 Slot= 9, field= MWC349 , spw= 15, nchan= 122 Slot= 10, field= MWC349 , spw= 16, nchan= 122 Slot= 11, field= MWC349 , spw= 19, nchan= 122 Slot= 12, field= MWC349 , spw= 20, nchan= 122 Slot= 13, field= 2013+370, spw= 7, nchan= 122 Slot= 14, field= 2013+370, spw= 8, nchan= 122 Slot= 15, field= 2013+370, spw= 15, nchan= 122 Slot= 16, field= 2013+370, spw= 16, nchan= 122 Slot= 17, field= 2013+370, spw= 19, nchan= 122 Slot= 18, field= 2013+370, spw= 20, nchan= 122 *****AMPLITUDE summary******** Antenna based spline coefficients 1 [-0.00893732, 0.106765, -0.0261889, 0.0153782, 0, 0, 0, 0] 2 [0.0124416, 0.312743, 0.0379053, 0.114385, 0, 0, 0, 0] 3 [0.00153935, 0.163342, -0.0922112, 0.0284693, 0, 0, 0, 0] 4 [-0.00245631, 0.0215154, 0.0384309, 0.0491021, 0, 0, 0, 0] 5 [-0.00115826, 0.320181, 0.110177, 0.149947, 0, 0, 0, 0] RMS Fit per baseline Antenna1 Antenna2 rmsfit 1 2 0.0535202 1 3 0.0385685 1 4 0.0363035 1 5 0.0719057 2 3 0.071173 2 4 0.0544085 2 5 0.111402 3 4 0.0506796 3 5 0.0612005 4 5 0.0900398 Again, the "F-CHEB, abs(xcap).gt.1" stuff. - shell('mv 26-jan-2002-l02d.ms.AMP.ps 26-jan-2002-l02d.3mm.gcal.amp.ps') - shell('mv 26-jan-2002-l02d.ms.amp.log 26-jan-2002-l02d.3mm.gcal.amp.log') Looks reasonable. Now, we had left the flux of MWC349 undetermined. Scale it from the others. - cal.fluxscale(tablein='26-jan-2002-l02d.3mm.gcal', tableout='26-jan-2002-l02d.3mm.fcal', reference="3C273 2013+370", transfer='MWC349'); error, numeric and non-numeric types mixed error, non-compatible types for assignment : invalid number of indexes for: [[1:1,,1,1,1] 0 [1:1,,1,1,2] 0 [1:1,,1,1,3] 0 ... ] File: tableserver.g, Line 799 Stack: .(), calibrater.g line 651 .() Flux density for MWC349 (spw=1) is: nan +/- nan Jy This does the same thing if you try a single source - its because fluxscale cannot handle polynomials! >>>BUG: submitted as AOCso04709 >>>NOTE: Im not sure that there is a way to make fluxscale work with polys unless there is a poly per field somehow. Go ahead and make a T solution as in the cookbook and other scripts: - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolve(type='T', # Solve for any residual phase table='26-jan-2002-l02d.3mm.tcal', # errors with a timescale of t=300, # 5 min. refant=2); # Use ant 2 as reference. - cal.solve(); Found 48 good T Jones solutions. 0 solution intervals failed. 18 solution intervals had insufficient data. Should I worry about those solutions? I probably wont apply this table anyway. Again, the "F-CHEB, abs(xcap).gt.1" stuff. Try the fluxscale again - cal.fluxscale(tablein='26-jan-2002-l02d.3mm.tcal', tableout='26-jan-2002-l02d.3mm.fcal', reference="3C273 2013+370", transfer='MWC349'); It seems to solve for all spwids even though not all are in the table. Setting the flux density scale using reference calibrators Flux density for MWC349 (spw=1) is: nan +/- nan Jy Flux density for MWC349 (spw=2) is: nan +/- nan Jy Flux density for MWC349 (spw=3) is: nan +/- nan Jy Flux density for MWC349 (spw=4) is: nan +/- nan Jy Flux density for MWC349 (spw=5) is: nan +/- nan Jy Flux density for MWC349 (spw=6) is: nan +/- nan Jy Flux density for MWC349 (spw=7) is: 1.004 +/- 0.002 Jy Flux density for MWC349 (spw=8) is: 1.039 +/- 0.006 Jy Flux density for MWC349 (spw=9) is: nan +/- nan Jy Flux density for MWC349 (spw=10) is: nan +/- nan Jy Flux density for MWC349 (spw=11) is: nan +/- nan Jy Flux density for MWC349 (spw=12) is: nan +/- nan Jy Flux density for MWC349 (spw=13) is: nan +/- nan Jy Flux density for MWC349 (spw=14) is: nan +/- nan Jy Flux density for MWC349 (spw=15) is: 1.015 +/- 0.006 Jy Flux density for MWC349 (spw=16) is: 1.047 +/- 0.007 Jy Flux density for MWC349 (spw=17) is: nan +/- nan Jy Flux density for MWC349 (spw=18) is: nan +/- nan Jy Flux density for MWC349 (spw=19) is: 0.992 +/- 0.004 Jy Flux density for MWC349 (spw=20) is: 1.050 +/- 0.004 Jy Flux density for MWC349 (spw=21) is: nan +/- nan Jy Flux density for MWC349 (spw=22) is: nan +/- nan Jy Flux density for MWC349 (spw=23) is: nan +/- nan Jy Flux density for MWC349 (spw=24) is: nan +/- nan Jy Flux density for MWC349 (spw=25) is: nan +/- nan Jy Flux density for MWC349 (spw=26) is: nan +/- nan Jy Flux density for MWC349 (spw=27) is: nan +/- nan Jy Flux density for MWC349 (spw=28) is: nan +/- nan Jy Flux density for MWC349 (spw=29) is: nan +/- nan Jy Flux density for MWC349 (spw=30) is: nan +/- nan Jy Flux density for MWC349 (spw=31) is: nan +/- nan Jy Flux density for MWC349 (spw=32) is: nan +/- nan Jy >>>BUG: should be able to ignore or choose spwids, submitted as AOCso04710 This matches with the IRAM log Calibrators =========== 96.5 GHz Fluxes (Jy): read computed MWC349 1.01 M 0.95 close enough! Can look at these: - cal.plotcal(tablename='26-jan-2002-l02d.3mm.tcal',plottype='PHASE'); - cal.plotcal(tablename='26-jan-2002-l02d.3mm.tcal',plottype='AMP'); - cal.plotcal(tablename='26-jan-2002-l02d.3mm.fcal',plottype='AMP'); Ironically, the default 1 Jy is probably close enough also so you cant see a difference and dont really need to fluxscale! >>>COMMENT: I went about this the wrong way, I should have done the amplitude gspline after doing the scaling thing. We could have (and probably should have) used the value 1.01 or 0.95 from the unclear docs we were given, but I wanted to exercise fluxscale. Here is the correct procedure: - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setsolvegainspline(table='26-jan-2002-l02d.3mm.gcal', mode='PHAS', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.3mm.gcal.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.3mm.gcal.phase.log') - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolve(type='T', # Solve for residual gain table='26-jan-2002-l02d.3mm.tcal', # errors with a timescale of phaseonly=F, t=300, # 5 min. refant=2); # Use ant 2 as reference. - cal.solve(); Found 48 good T Jones solutions. 0 solution intervals failed. 18 solution intervals had insufficient data. - cal.fluxscale(tablein='26-jan-2002-l02d.3mm.tcal', tableout='26-jan-2002-l02d.3mm.fcal', reference="3C273 2013+370", transfer='MWC349'); ... Flux density for MWC349 (spw=7) is: 1.046 +/- 0.006 Jy Flux density for MWC349 (spw=8) is: 1.082 +/- 0.007 Jy ... Flux density for MWC349 (spw=15) is: 1.057 +/- 0.008 Jy Flux density for MWC349 (spw=16) is: 1.091 +/- 0.009 Jy ... Flux density for MWC349 (spw=19) is: 1.034 +/- 0.006 Jy Flux density for MWC349 (spw=20) is: 1.093 +/- 0.004 Jy ... Looks like the value 1.06 is the average. - for(spw in 1:20){ imset.setjy(fieldid=2,spwid=spw,fluxdensity=[1.06,0,0,0]); } - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [7,8,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvegainspline(table='26-jan-2002-l02d.3mm.gcal', mode='AMP', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.AMP.ps 26-jan-2002-l02d.3mm.gcal.amp.ps') - shell('mv 26-jan-2002-l02d.ms.amp.log 26-jan-2002-l02d.3mm.gcal.amp.log') Looks good. Now apply these solutions to all the 128ch and 512ch data: - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [3,4,7,8,11,12,15,16,19,20]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.correct(); 8. [2004.1.7] 1mm Bandpass and Gain Calibration 1mm Data: ID Ref.Freq #Chans Resolution TotalBW Correlations 21 238082 MHz 1 38000 kHz 38000 kHz XX 22 241017 MHz 1 -38000 kHz 38000 kHz XX 23 238082 MHz 512 78.125 kHz 40000 kHz XX 24 241017 MHz 512 -78.125kHz 40000 kHz XX 25 238215 MHz 1 304000 kHz 304000 kHz XX 26 240884 MHz 1 -304000kHz 304000 kHz XX 27 238216 MHz 128 2500 kHz 320000 kHz XX 28 240883 MHz 128 -2500 kHz 320000 kHz XX 29 237955 MHz 1 304000 kHz 304000 kHz XX 30 241144 MHz 1 -304000kHz 304000 kHz XX 31 237956 MHz 128 2500 kHz 320000 kHz XX 32 241143 MHz 128 -2500 kHz 320000 kHz XX Initial phase solutions for bpass calibrator (3C273) Use the 128-chan windows [27,28,31,32] Leave out first and last 2 unflagged channels First the LSB [27,31] - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [27,31]'); - cal.setsolvegainspline(table='26-jan-2002-l02d.1mmLSB.gcal0', mode='PHAS', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.1mmLSB.gcal0.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.1mmLSB.gcal0.phase.log') Pretty crappy. Now the USB channels [28,32] - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [28,32]'); - cal.setsolvegainspline(table='26-jan-2002-l02d.1mmUSB.gcal0', mode='PHAS', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.1mmUSB.gcal0.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.1mmUSB.gcal0.phase.log') The actual bandpass calibration for 1mm LSB, using USB phases to preserve offset so it will be removed after application of bpass. - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [27,31]'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mmUSB.gcal0'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.1mm.bpoly', degamp=6, degphase=12, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); Solving for B Freq. group 1mm-LSB, spw= 27, nchan= 128 Freq. group 1mm-LSB, spw= 31, nchan= 128 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.1mmLSB.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.1mmLSB.BP_amp.ps') Now for 1mm USB, appending to table - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [28,32]'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mmUSB.gcal0'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.1mm.bpoly', degamp=6, degphase=12, visnorm=F, bpnorm=F, refant=2, append=T); - cal.solve(); Solving for B Freq. group 1mm-USB, spw= 28, nchan= 128 Freq. group 1mm-USB, spw= 32, nchan= 128 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.1mmUSB.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.1mmUSB.BP_amp.ps') We now derive the phase solution at 1mm. - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [27,28,31,32]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mm.bpoly'); We will use a curve transfer of 3mm solution to 1mm to reduce phase wrapping, though I havent tried a raw transfer or no transfer at all. This will be an incremental solution with cumulative output table, as usual. - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvegainspline(table='26-jan-2002-l02d.1mm.gcal', mode='PHAS', preavg=0, splinetime=10000, refant=2, npointaver=10, phasewrap=260, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.PHAS.ps 26-jan-2002-l02d.1mm.gcal.phase.ps') - shell('mv 26-jan-2002-l02d.ms.phase.log 26-jan-2002-l02d.1mm.gcal.phase.log') We had set all the fluxes for the 1mm windows, so we can go ahead and solve for amplitudes: - cal.reset(); - cal.setdata(mode='channel', start=4, step=1, nchan=122, msselect='FIELD_ID IN [1,2,3] && SPECTRAL_WINDOW_ID IN [27,28,31,32]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.setsolvegainspline(table='26-jan-2002-l02d.1mm.gcal', mode='AMP', preavg=0.0, splinetime=10000, refant=2, npointaver=10, phasewrap=260); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.AMP.ps 26-jan-2002-l02d.1mm.gcal.amp.ps') - shell('mv 26-jan-2002-l02d.ms.amp.log 26-jan-2002-l02d.1mm.gcal.amp.log') These look reasonable. Go ahead and apply - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [23,24,27,28,31,32]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.correct(); 9. [2004.1.8] Bandpasses for the 512ch data? In the cookbook, a 1st order bpoly is done on the 512ch data. It is not clear whether this is useful or not, but we can try: - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID IN [3,11]'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mm512.bpoly', degamp=1, degphase=1, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); Solving for B Freq. group 3mm-LSB, spw= 3, nchan= 512 Freq. group 3mm-LSB, spw= 11, nchan= 512 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmLSB512.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmLSB512.BP_amp.ps') Note that the two windows are about 350MHz apart and there are significant offsets in amp and phase between them (this is what the poly is fitting). Looks like there may be enough signal to do the windows individually. - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==3'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); Note that I am assuming it will allow incremental bpolys. - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mmLSBa.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); Lets try third order - cal.solve(); Solving for B Freq. group 3mm-LSB, spw= 3, nchan= 512 - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmLSBa.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmLSBa.BP_amp.ps') Looks reasonable, 3rd order might have been a bit much on the phase though. Do the other windows - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==11'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mmLSBb.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmLSBb.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmLSBb.BP_amp.ps') - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==4'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mmUSBa.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmUSBa.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmUSBa.BP_amp.ps') - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==12'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.3mmUSBb.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.3mmUSBb.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.3mmUSBb.BP_amp.ps') This last one has some noticeable phase structure in the bandpass. Now (re)correct the data - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [3]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mmLSBa.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.correct(); - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [11]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mmLSBb.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.correct(); - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [4]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mmUSBa.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.correct(); - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [12]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.3mmUSBb.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.3mm.gcal'); - cal.correct(); OK, now repeat for the 1mm 512ch windows - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==23'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.1mmLSBa.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.1mmLSBa.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.1mmLSBa.BP_amp.ps') - cal.reset(); - cal.setdata(msselect='FIELD_ID==1 && SPECTRAL_WINDOW_ID==24'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mm.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.setsolvebandpoly(table='26-jan-2002-l02d.1mmUSBa.bpoly', degamp=3, degphase=3, visnorm=F, bpnorm=F, refant=2, append=F); - cal.solve(); - shell('mv 26-jan-2002-l02d.ms.RF_PHASE.ps 26-jan-2002-l02d.1mmUSBa.BP_phase.ps') - shell('mv 26-jan-2002-l02d.ms.RF_AMP.ps 26-jan-2002-l02d.1mmUSBa.BP_amp.ps') These are much noisier than 3mm but still the low order should be fine. And apply - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [23]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mmLSBa.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.correct(); - cal.reset(); - cal.setdata(msselect='FIELD_ID IN [1,2,3,4] && SPECTRAL_WINDOW_ID IN [24]'); - cal.setapply(type='BPOLY', table='26-jan-2002-l02d.1mmUSBa.bpoly'); - cal.setapply(type='GSPLINE', table='26-jan-2002-l02d.1mm.gcal'); - cal.correct(); Finally done with calibration - cal.done(); - imset.done(); 10. [2004.1.9] Split out the data - myms:=ms('26-jan-2002-l02d.ms', readonly=F); Now average the 122 middle channels of the 128ch 3mm continuum spw to 1 channel - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmCONT.ms', fieldids=[4], spwids=[7,8,15,16,19,20], nchan=[1], start=[4], step=[122], whichcol='CORRECTED_DATA'); The 3mm line data - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmLSB128a.ms', fieldids=[4], spwids=[7], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmLSB128b.ms', fieldids=[4], spwids=[15], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmLSB128c.ms', fieldids=[4], spwids=[19], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmUSB128a.ms', fieldids=[4], spwids=[8], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmUSB128b.ms', fieldids=[4], spwids=[16], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmUSB128c.ms', fieldids=[4], spwids=[20], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmLSB512a.ms', fieldids=[4], spwids=[3], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmLSB512b.ms', fieldids=[4], spwids=[11], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmUSB512a.ms', fieldids=[4], spwids=[4], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.3mmUSB512b.ms', fieldids=[4], spwids=[12], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); Now the 1mm continuum - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmCONT.ms', fieldids=[4], spwids=[27,28,31,32], nchan=[1], start=[4], step=[122], whichcol='CORRECTED_DATA'); And the 1mm line data - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmLSB128a.ms', fieldids=[4], spwids=[27], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmLSB128b.ms', fieldids=[4], spwids=[31], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmUSB128a.ms', fieldids=[4], spwids=[28], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmUSB128b.ms', fieldids=[4], spwids=[32], nchan=[128], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmLSB512a.ms', fieldids=[4], spwids=[23], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.split(outputms='20126+4104.26-jan-2002-l02d.1mmUSB512a.ms', fieldids=[4], spwids=[24], nchan=[512], start=[1], step=[1], whichcol='CORRECTED_DATA'); - myms.done(); 11. [2004.1.9] Image the data Look at the 3mm continuum - imgr:=imager(filename='20126+4104.26-jan-2002-l02d.3mmCONT.ms'); - imgr.setdata(mode='channel', nchan=1, start=1, step=1, spwid=1, fieldid=1); - imgr.advise(takeadvice=F,amplitudeloss=0.05,fieldofview='55arcsec') Maximum uv distance = 100620 wavelengths Recommended cell size < 1.02497 arcsec Recommended number of pixels = 64 Dispersion in uv, w distance = 61353.8, 16630.4 wavelengths Best fitting plane is w = 0.406704 * u + -0.150854 * v Dispersion in fitted w = 4491.66 wavelengths Wide field cleaning is not necessary Note the FWHM of the 15m IRAM antennas should be 75'/f(GHz), or 47" at 96GHz and 19" at 240GHz. Lets oversample by 4x - imgr.setimage(nx=256, ny=256, # Set image plane parameters cellx='0.25arcsec', celly='0.25arcsec', stokes='I', # Image total intensity mode='mfs', # Doesnt matter here nchan=1, start=1, # step=1, spwid=1, fieldid=1); - imgr.weight(type='briggs', # Set up Robust weighting rmode='norm', robust=0.5); Make a dirty image and psf - imgr.makeimage(type='psf',image='20126+4104.3mmCONT.psf'); - imgr.fitpsf(psf='20126+4104.3mmCONT.psf'); Beam fit: 2.27651 by 1.26026 (arcsec) at pa 76.0539 (deg) - imgr.makeimage(type='corrected',image='20126+4104.3mmCONT.dirty'); Put up a viewer window - include 'viewer.g' - dv.gui() Load up the dirty image and psf and blink. Looks like a point source! Clean it - imgr.clean(algorithm='clark', # Image & deconvolve with 100 iterations niter=100, # using the Clark CLEAN algorithm. gain=0.1, model='20126+4104.3mmCONT.model', image='20126+4104.3mmCONT.clean', residual='20126+4104.3mmCONT.resid', mask='', # Inner quarter (no mask set) interactive=F); There is a 15 mJy source, but the clean picked up sidelobes so this should be windowed. The easiest is to use interactive - imgr.clean(algorithm='clark', # Image & deconvolve with 100 iterations niter=100, # using the Clark CLEAN algorithm. gain=0.1, model='20126+4104.3mmCONT.model', image='20126+4104.3mmCONT.clean', residual='20126+4104.3mmCONT.resid', mask='', interactive=T,npercycle=50); Caught exception: valid Table operation: SetupNewTable 20126+4104.3mmCONT.resid is already opened (is in the table cache) Even though I deleted the prev .resid etc. from disk? Kumar suggested runnning setimage again to clear? YES this worked. The interactive clean did enough on 50 iterations, but there were lots of sidelobes still around, so I probably did a poor calibration job, or there may be real extended structure there. Should probably do some selfcal, but I wont bother right now. It would have been nice if clean reported the total cleaned flux also! Can automate the box cleaning: - im:=image('20126+4104.3mmCONT.dirty'); - im.statistics(statsout=statrec); - im.done(); - maxblc:= [statrec.maxpos[1]-10, statrec.maxpos[2]-10, 1, 1]; - maxtrc:= [statrec.maxpos[1]+10, statrec.maxpos[2]+10, 1, 1]; - imgr.boxmask(mask='maxbox', blc=maxblc, trc=maxtrc); Setting 'maxbox' blc=[119, 118, 1, 1] trc=[139, 138, 1, 1] to 1 - imgr.clean(algorithm='clark', # use the Clark CLEAN algorithm niter=50, # 50 iterations gain=0.1, model='20126+4104.3mmCONT.model', image='20126+4104.3mmCONT.clean', residual='20126+4104.3mmCONT.resid', mask='maxbox', # Use our box interactive=F); Max of restored image is 19 mJy. Now restart from this model and clean the inner quarter: - shell('cp -r 20126+4104.3mmCONT.model 20126+4104.3mmCONT.model2') - imgr.clean(algorithm='clark', niter=50, # 50 more iterations gain=0.1, model='20126+4104.3mmCONT.model2', image='20126+4104.3mmCONT.clean2', residual='20126+4104.3mmCONT.resid2', mask='', # Inner quarter (no mask set) interactive=F); OK, enough of this. - imgr.done(); Make a 1mm continuum image. - imgr:=imager(filename='20126+4104.26-jan-2002-l02d.1mmCONT.ms'); - imgr.setdata(mode='channel', nchan=1, start=1, step=1, spwid=1, fieldid=1); Scale by factor 2.5 for frequency from 3mm parameters - imgr.setimage(nx=256, ny=256, # Set image plane parameters cellx='0.1arcsec', celly='0.1arcsec', stokes='I', # Image total intensity mode='mfs', # Doesnt matter here nchan=1, start=1, # step=1, spwid=1, fieldid=1); - imgr.weight(type='briggs', # Set up Robust weighting rmode='norm', robust=0.5); Make a dirty image and psf - imgr.makeimage(type='psf',image='20126+4104.1mmCONT.psf'); - imgr.fitpsf(psf='20126+4104.1mmCONT.psf'); Beam fit: 0.788734 by 0.50205 (arcsec) at pa 77.0888 (deg) - imgr.makeimage(type='corrected',image='20126+4104.1mmCONT.dirty'); - im:=image('20126+4104.1mmCONT.dirty'); - im.statistics(statsout=statrec); - im.done(); Note max is 139mJy at 1mm, rising spectrum! 10x that at 3mm???? - maxblc:= [statrec.maxpos[1]-10, statrec.maxpos[2]-10, 1, 1]; - maxtrc:= [statrec.maxpos[1]+10, statrec.maxpos[2]+10, 1, 1]; - imgr.boxmask(mask='maxbox', blc=maxblc, trc=maxtrc); - imgr.clean(algorithm='clark', # use the Clark CLEAN algorithm niter=50, # 50 iterations gain=0.1, model='20126+4104.1mmCONT.model', image='20126+4104.1mmCONT.clean', residual='20126+4104.1mmCONT.resid', mask='maxbox', # Use our box interactive=F); - shell('cp -r 20126+4104.1mmCONT.model 20126+4104.1mmCONT.model2') - imgr.clean(algorithm='clark', niter=50, # 50 more iterations gain=0.1, model='20126+4104.1mmCONT.model2', image='20126+4104.1mmCONT.clean2', residual='20126+4104.1mmCONT.resid2', mask='', # Inner quarter (no mask set) interactive=F); This image is strongly point-source dominated. - imgr.done(); Now the 1mm cubes. First 512ch LSB: - imgr:=imager(filename='20126+4104.26-jan-2002-l02d.1mmLSB512a.ms'); - imgr.setdata(mode='channel', nchan=512, start=1, step=1, spwid=1, fieldid=1); Now a 256x256x512 cube of 4-byte reals will fill 134MB. Lets fudge a bit and make a 128x128x256 image (16MB) at 0.15" resolution - imgr.setimage(nx=128, ny=128, # Set image plane parameters cellx='0.15arcsec', celly='0.15arcsec', stokes='I', # Image total intensity mode='channel', # Cube nchan=256, # Average together 2 chans start=1, step=2, spwid=1, fieldid=1); - imgr.weight(type='briggs', # Set up Robust weighting rmode='norm', robust=0.5); - imgr.makeimage(type='corrected',image='20126+4104.1mmLSB512a.dirty'); Don't see anything, even the continuum, though I guess the rms is 370mJy per 150kHz combined channel. - imgr.done(); Try the USB... - imgr:=imager(filename='20126+4104.26-jan-2002-l02d.1mmUSB512a.ms'); - imgr.setdata(mode='channel', nchan=512, start=1, step=1, spwid=1, fieldid=1); - imgr.setimage(nx=128, ny=128, # Set image plane parameters cellx='0.15arcsec', celly='0.15arcsec', stokes='I', # Image total intensity mode='channel', # Cube nchan=256, # Average together 2 chans start=1, step=2, spwid=1, fieldid=1); - imgr.weight(type='briggs', # Set up Robust weighting rmode='norm', robust=0.5); - imgr.makeimage(type='corrected',image='20126+4104.1mmUSB512a.dirty'); Nothing obvious here either. Try 3mm 128ch cubes. - imgr:=imager(filename='20126+4104.26-jan-2002-l02d.3mmUSB128a.ms'); - imgr.setdata(mode='channel', nchan=128, start=1, step=1, spwid=1, fieldid=1); - imgr.setimage(nx=256, ny=256, # Set image plane parameters cellx='0.25arcsec', celly='0.25arcsec', stokes='I', # Image total intensity mode='channel', # Cube nchan=128, # each channel start=1, step=1, spwid=1, fieldid=1); - imgr.weight(type='briggs', # Set up Robust weighting rmode='norm', robust=0.5); - imgr.makeimage(type='corrected',image='20126+4104.3mmUSB128a.dirty'); Note, could probably image with 0.4arcsec cells x 128 images x 256 chan for the 512ch cubes. Nothing. Probably need to add in the other 2 good days of data to have a hope. Script for this session available as: /home/sandrock/smyers/Testing/2003-12-15/script.l02d.26jan02.g NOTE: This script is not exactly what was done here, it has been refined slightly.