NOTES: 2nd Pri doesn't seem to be there at all... But there's a lot of 1st Pri (basically 2 sections) 10: Had to flag large amount of 1st Pri (1st section) in Ants 12 & 27 b/c it was very faint 14: CALIB failed on 4 solutions (must be Ant 12 & 27 FULL) (but BPASS of Ants 12 & 27 look fine) 16, 19, 20: No 1st Pri shown for Ants 12 & 27 Tried 12 & 13 (new NEWCH0) and then CALIB again with refant 12 then 6-> same results Didn't want to lose ALL of Ant 12 & 27 data... (Why do both look calibrated properly then?) Go back to start- new LINCOP & NEWCH0 but flag all the first section of the first Pri (Megan's suggestion)-> now CALIB works! The galaxy is barely there, and it is rotating (channels ~80-130). There appears to be only 1 continuum source. LITTLE THINGS AIPS Reduction of Haro29, B2 (X) config.: VLA Obs. of 30jan08 ===================================================================== calibration recipe v. 2.0: mrupen 10oct08 calibration recipe v. 2.1: mrupen 13oct08 calibration recipe v. 2.1.update: Dana Ficut Vicas 29Oct08 (new adverbs in Aips) calibration recipe v. 2.2: Dana Ficut Vicas 11Dec08(tiny bits) calibration recipe v. 2.3: Dana Ficut Vicas 11 Feb 09(UVCOP ambiguities) calibration recipe v. 2.4: Dana Ficut Vicas 3 Mar 09(team raised issues) Latest update: 3rd March 2009 (Actually, this is a tiny bit different- all parameters are ordered as in AIPS) Data reduced by Kim Herrmann, Lowell 26jun09-30jun09 Suggestion: STARTING with D ARRAY and then working through C array and B array is recommended. D array data will allow you to have a look at the whole field (the strong continuum sources that might give problems will be obvious here), is more stable and will give you the best feel for the data. The recipe lists the B-array reduction, but obviously the same steps apply to all configurations. ^0. Basic stuff B2 configuration (X) From observing log (available online at http://www.lowell.edu/users/dah/littleteam/haro29/vla/obs/logs_AH927_X.html): Observing: 30Jan08 08:06:19-14:04:19 (30Jan08 01:06:19-07:04:19 local time) * Wind/API rms phase/clouds: 30Jan 08:04:51 SW at 3.3 m/s N/A API Sky clear. Gusty winds. 30Jan 08:59:34 SW at 7.4 m/s N/A API Sky clear. Gusty winds. 30Jan 10:59:43 W at 5.8 m/s N/A API Sky clear. 30Jan 12:59:48 W at 6.9 m/s N/A API Sky clear. * ant. 1 (does not have a good baseline position because recently moved) * EVLA antennas: 1, 11, 13, 14, 16, 17, 18, 19, 21, 23, 24, 25, 26 (13 antennas) * ant. 4 LOST (EVLA: Antenna is undergoing EVLA testing.) (whole time) * ant. 14 LOST (EVLA: L-301 module will not lock. Attempted re-booting MIB but it will not respond.) (whole time) ^1. FILLM executed on 26jun09 ^a. Request archive data: requested AH927_X_1 and saved temporarily as /Users/herrmann/Desktop/AH927_B_X_1 ^b. FILLM -> Haro29-B2.CH 0.1, Haro29-B2.LINE.1 (1 & 2) default FILLM datain '/Users/herrmann/Desktop/AH927_B_X_ nfiles 0 $ normally don't skip any files band 'L' qual 1 $ restricts FILLM to the galaxy+calibrators of interest vlaobs 'AH927' timerang 0 0 $ No other scans before Haro29 so no need for different qual # outna 'Haro29-B2 outseq 0; outdisk 1 douvcomp=-1 $ allow channel/IF-dependent weights doconcat=-1 $ Change this to DOCONCAT=1 to add data to an existing file ncount 1 $ read one file doweight 10 $ use memo 108 weights (i.e., put weights in 1/Jy^2) cparm 0 cparm(4)=25.1 $ one needs to explicitly flag shadowed antennas $ since the ModComps were retired on 27 June 2007 $ this requires FILLM in 31DEC08 after 18Nov08 MNJ cparm(7)= 0 $ assigns new FREQID if frequency changes by more than $ the max. Doppler shift between sources 180 degrees $ apart. Setting this to -1 forces all data to have same FREQID. bparm= -1,-1 $ avoid opacity & gain corrections doall -1 $ DOESN'T SEEM TO BE THERE ***N.B. FILLM's channel 0 will ONLY be used for initial flagging. We're quite paranoid here. tortue> FILLM1: ****************************************************** tortue> FILLM1: ** Times written by FILLM are now centered in ** tortue> FILLM1: ** the integration, before they were at the end ** tortue> FILLM1: ****************************************************** tortue> FILLM1: Shadow flag limit = 2.510E+01 meters. tortue> FILLM1: No opacity correction in CL table. tortue> FILLM1: No gain curve correction in CL table. tortue> FILLM1: Opening /Users/herrmann/Desktop/AH927_B_X_1 tortue> FILLM1: tortue> FILLM1: *** ATTENTION - default: loading subarray 1 *** tortue> FILLM1: tortue> FILLM1: tape file # 1, start date/time = 20080130/08:06:20 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 26 antenn tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Program = AH927 ; Tape revision number = 32. tortue> FILLM1: Create Haro29-B2 .CH 0 . 1 (UV) on disk 1 cno tortue> FILLM1: Ref. date = 20080130 A-C = 1.419128 B-D = 1.419128 GHz tortue> FILLM1: Create Haro29-B2 .LINE . 1 (UV) on disk 1 cno tortue> FILLM1: Ref. date = 20080130 A-C = 1.419128 B-D = 1.419128 GHz tortue> FILLM1: FLMFQ: FQ entry tolerance = 1.609D+02 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 08:0 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 26 antenn tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Ref. date = 20080130 A-C = 1.419128 B-D = 1.419128 GHz tortue> FILLM1: Appending new data to: Haro29-B2 .CH 0 . 1 disk 1 tortue> FILLM1: Ref. date = 20080130 A-C = 1.419128 B-D = 1.419128 GHz tortue> FILLM1: Appending new data to: Haro29-B2 .LINE . 1 disk 1 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 08:0 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 08:1 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 08:2 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 08:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 08:5 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 08:5 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 09:2 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 09:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 09:5 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 09:5 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 10:1 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 10:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 10:4 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 10:5 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 11:1 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 11:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 11:5 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 11:5 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 12:2 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 12:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 12:5 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 12:5 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 13:2 tortue> FILLM1: Found HARO29 : 1 1.562 MHz at IAT 0/ 13:2 tortue> FILLM1: Found 1313+549 : 1 1.562 MHz at IAT 0/ 13:5 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 14:0 tortue> FILLM1: Read 647907 visibilities from 1 files tortue> FILLM1: Appears to have ended successfully ^2. TASAV -> LINSAV.1 executed on 26jun09 ***We TASAV right away, because VLANT changes the AN table. Did I mention we're paranoid? default TASAV outna 'Haro29B2BgTb outcla 'LINSAV' outdi 2 $ Ideally set this to a different disk from indisk, $ in case of disk crashes getn 2 $ *.LINE ^3. UVCOP -> LINCOP.1 executed on 26jun09 (twice) ***Discard the first and last channels: 1st and last 10 channels if 127 channels total 1st and last 20 channels if 255 channels total ***We discard these Evil Channels because (1) they're pretty much useless; (2) they seem to confuse BPASS (which takes the solution from channel N as the initial guess for channel N+1); (3) their noise characteristics are quite different from the rest of the channels, which can be confusing e.g. in clipping and imaging. default UVCOP outcla 'LINCOP' bchan 21; echan 235 $ Use bchan 21; echan 235 for 255 channels $ Use bchan 11; echan 117 for 127 channels uvcopprm 0 uvcopprm(4) 1 $ report progress getn 2 $ *.LINE ***From now on we operate on LINCOP data (64, then 66) unless otherwise specified. ^4. LISTR/SCAN --> Haro29-B2.listr ***We do this before VLANT because we need to know FREQIDs for VLANT default LISTR optype 'SCAN' docrt -1 outpr '/Users/herrmann/Desktop/Haro29-B2.listr getn 64 $ *.LINCOP --> *.listr tortue LISTR(31DEC08) 4 26-JUN-2009 13:58:08 Page 1 File = Haro29-B2 .LINCOP. 1 Vol = 1 Userid = 4 Freq = 1.419127750 GHz Ncor = 2 No. vis = 647907 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0001 A 1 0/08:06:35 - 0/08:20:25 1 1 26828 2 1313+549 : 0001 C 1 0/08:21:35 - 0/08:25:35 1 26829 34928 3 HARO29 : 0001 1 0/08:26:15 - 0/08:51:15 1 34929 83303 4 1313+549 : 0001 C 1 0/08:51:55 - 0/08:56:05 1 83304 91703 5 HARO29 : 0001 1 0/08:56:45 - 0/09:21:45 1 91704 140589 6 1313+549 : 0001 C 1 0/09:22:25 - 0/09:26:35 1 140590 148750 7 HARO29 : 0001 1 0/09:27:15 - 0/09:52:15 1 148751 196735 8 1313+549 : 0001 C 1 0/09:52:55 - 0/09:57:05 1 196736 204870 9 HARO29 : 0001 1 0/09:57:45 - 0/10:17:55 1 204871 243123 10 1313+549 : 0001 C 1 0/10:18:35 - 0/10:22:45 1 243124 251263 11 HARO29 : 0001 1 0/10:23:25 - 0/10:48:25 1 251264 300023 12 1313+549 : 0001 C 1 0/10:49:05 - 0/10:53:15 1 300024 308473 13 HARO29 : 0001 1 0/10:53:55 - 0/11:18:55 1 308474 357325 14 1313+549 : 0001 C 1 0/11:19:45 - 0/11:23:45 1 357326 365425 15 HARO29 : 0001 1 0/11:24:35 - 0/11:49:35 1 365426 414321 16 1313+549 : 0001 C 1 0/11:50:35 - 0/11:54:45 1 414322 422771 17 HARO29 : 0001 1 0/11:55:45 - 0/12:20:35 1 422772 471521 18 1313+549 : 0001 C 1 0/12:21:25 - 0/12:25:35 1 471522 479652 19 HARO29 : 0001 1 0/12:26:25 - 0/12:51:35 1 479653 525578 20 1313+549 : 0001 C 1 0/12:52:25 - 0/12:56:25 1 525579 533678 21 HARO29 : 0001 1 0/12:57:15 - 0/13:22:15 1 533679 582578 22 1313+549 : 0001 C 1 0/13:22:55 - 0/13:27:05 1 582579 590706 23 HARO29 : 0001 1 0/13:27:45 - 0/13:52:55 1 590707 639759 24 1313+549 : 0001 C 1 0/13:53:35 - 0/13:57:35 1 639760 647884 25 1331+305 : 0001 A 1 0/14:00:35 - 0/14:04:15 1 647885 647907 tortue LISTR(31DEC08) 4 26-JUN-2009 13:58:08 Page 2 File = Haro29-B2 .LINCOP. 1 Vol = 1 Userid = 4 Source summary Velocity type = ' ' Definition = ' ' ID Source Qual Calcode RA(2000.0) Dec(2000.0) IFlux QFlux UFlux VFlux No. vis 1 1331+305 : 0001 A 13:31:08.2879 30:30:32.958 0.000 0.000 0.000 0.000 26851 2 1313+549 : 0001 C 13:13:37.8529 54:58:23.894 0.000 0.000 0.000 0.000 98420 3 HARO29 : 0001 12:26:16.0000 48:29:37.000 0.000 0.000 0.000 0.000 522636 ID Source Freq(GHz) Velocity(Km/s) Rest freq (GHz) 1 All Sources 1.4191 0.0000 0.0000 Frequency Table summary FQID IF# Freq(GHz) BW(kHz) Ch.Sep(kHz) Sideband 1 1 1.41912775 1312.2560 6.1035 1 Primary: 14:00, 3:50-> 17:50 Secondary: 4:10, 4:20, 4:20, 4:20, 4:20, 4:20, 4:10, 4:20, 4:20, 4:10, 4:20, 4:10 -> 51:20 Galaxy: 25:10, 25:10, 25:10, 20:20, 25:10, 25:10, 25:10, 25:00, 25:20, 25:10, 25:20 -> 272:10 total However, subtract 10s out of 2 scans-> so 271:50 total (4.531 hrs = 04:31:50) ^5. VLANT -> AN/1, CL/2 executed on 26jun09 (twice) ***Note that VLANT can be run only for data observed from 1992 onwards. Data earlier than 1991 produce the following error message: VLANT1: Task VLANT (release of 31DEC07) begins VLANT1: ANT DATA UNAVAILABLE FOR YEAR 1991 DATA START WITH 1992 VLANT1: Purports to die of UNNATURAL causes For earlier data we skip baseline corrections entirely, and hope for the best. If there are clear and systematic phase gradients with time, consult the baseline corrections at http://www.vla.nrao.edu/astro/archive/baselines/ and apply corrections via CLCOR (which is basically what VLANT does). ***Note that if you get an error like the following: /tmp/baselines.vlais09 copied from the VLA web site, ZABORS: signal 11 received, ABORT! you can probably solve this by going to http://www.vla.nrao.edu/astro/archive/baselines/ and copying the list of baseline corrections from the current year (say, 2009) into aips/TEXT/STARS/VLA.ant.2009 (Make sure there are no empty lines at the start of the file) ***10oct08: Currently VLANT works on only one FREQID at a time. We therefore have to run VLANT multiple times for data with multiple FREQIDs. Unfortunately VLANT (1) produces a new CL table every time, and (2) updates the AN table positions every time as well. : CL tables: I'd like to maintain the convention that CL/1 is the original CL table and CL/2 has all the corrections that should have been applied on-line but weren't -- mainly, antenna position corrections. For multiple FREQIDs therefore this recipe calls for deleting the intermediate CL tables created by VLANT, using the rather clumsy mechanism of TASAVing to a temporary file, deleting the original CL tables, and copying the latest one back from the TASAV'd data set. Blah. : AN table: For now, this recipe resets to the original AN table just before running VLANT the last time. This means that only one run of VLANT updates the AN entries, leading to a correct AN table as needed for (e.g.) UVFIX. I've e-mailed DAIP to see about fixing all this, by allowing FREQID= -1 to mean "calculate corrections for all FREQIDs" (currently FREQID= -1 is reset to FREQID= 1). We'll see what Eric says. #####VLANT no longer has freqid as a parameter. ^5a. default VLANT getn 64 $ *.LINCOP (then 66) tortue> VLANT1: WARNING: 2 ANTENNAS MAY STILL GET MORE CORRECTION tortue> VLANT1: Copied CL file from vol/cno/vers 1 64 1 to 1 64 2 tortue> VLANT1: CL version input 1 output 2 tortue> VLANT1: VLANT STNID( 1) = 'W10' tortue> VLANT1: VLANT XCOR( 1) = -0.0047 tortue> VLANT1: VLANT YCOR( 1) = -0.0092 tortue> VLANT1: VLANT ZCOR( 1) = -0.0092 tortue> VLANT1: VLANT STNID(10) = 'E8 ' tortue> VLANT1: VLANT XCOR(10) = 0.0013 tortue> VLANT1: VLANT YCOR(10) = 0.0000 tortue> VLANT1: VLANT ZCOR(10) = 0.0004 tortue> VLANT1: VLANT STNID(13) = 'N16' tortue> VLANT1: VLANT XCOR(13) = 0.0042 tortue> VLANT1: VLANT YCOR(13) = -0.0005 tortue> VLANT1: VLANT ZCOR(13) = 0.0020 tortue> VLANT1: Appears to have ended successfully %%% Probably the warning is about antenna 4, 5, or 29 which aren't being used (from step 6 PRTAN) x5b. If VLANT does not create a new CL table (no antennas moved), or the data were taken before 1992: default TACOP getn 64 $ *.LINCOP getona 64 $ *.LINCOP inext 'CL' ; inver 1 ; ncount 1 ; outver 2 ***The goal here is to keep the recipe uniform for all data. ^6. PRTAN AN/1 default PRTAN docrt 132 getn 64 $ *.LINCOP (then 66) Location Of VLA Antennas N36 ( 7) N32 (26)* N28 (27) N24 (25)* N20 ( 2) N16 (13)* N12 (18)* N8 ( 9) N4 (12) *(19) W4 E4 (15) ( 6) W8 E8 (10) *( 1) W10 ( ) *(24) W12 E12 (20) ( 8) W16 E16 (14)* ( ) E20 (21)* *(16) W24 E24 (28) *(17) W28 E28 ( 3) ( ) E32 (11)* (22) W36 E36 (23)* VLA:_OUT ( 4) VLA:_OUT ( 5) VPT:_OUT (29) * => EVLA ANTENNA ***To choose the reference antenna the following algorithm should be followed: 1. should be present throughout the run 2. should be on an "inner" pad, but NOT N1/E1/W1 (to avoid shadowing) 3. NOT on the master pad (since those are always weird) 4. NOT an EVLA antenna (since those are often weird) 5. try to avoid the north arm in the smaller configurations (to avoid shadowing) 6. NOT listed in any interesting way in the log file (to avoid problems with the reference antenna) 7. preferably consistent with other recent runs 8. should be a fairly stable antenna (can't tell until TVFLG/CALIB of course...) ===> Refant: 15 $ E4 ^7. Calibrators ***Check out the calibrators in the on-line calibrator manual: http://www.vla.nrao.edu/astro/calib/manual/index.shtml ***Max baseline at 21 cm in B array is 54.3 klambda C array is 16.2 klambda D array is 4.9 klambda primary (flux/bandpass) calibrators: 0137+331= 3C48 0542+498= 3B247 1331+305= 3C286 $ This one once @ beginning & at end ***You can ignore the uv-ranges for these, since there are now models for the most important ones. %%%HOWEVER, in UVPLT the amplitude for 0542+498 will drop off (as in B2) because UVmax is 50 kL %%%Same for 0137+331, because UVmax is 40 kL 1331+305 J2000 A 13h31m08.287984s 30d30'32.958850" Aug01 3C286 1328+307 B2950 A 13h28m49.657700s 30d45'58.640000" ----------------------------------------------------- BAND A B C D FLUX(Jy) UVMIN(kL) UVMAX(kL) ===================================================== 90cm P S S S S 26.00 visplot 20cm L S S P P 15.00 visplot 6cm C S S S P 7.47 3.7cm X S P P P 5.23 400 visplot 2cm U S S S S 3.40 visplot 1.3cm K X S S P 2.59 visplot 0.7cm Q X S P P 1.45 300 visplot secondary (gain) calibrator: 1313+549 1313+549 J2000 C 13h13m37.852959s 54d58'23.894700" Aug01 CJ2 1311+552 B2950 C 13h11m33.920700s 55d14'15.872000" ----------------------------------------------------- BAND A B C D FLUX(Jy) UVMIN(kL) UVMAX(kL) ===================================================== 20cm L P P S X 1.31 6 visplot 6cm C S S S S 0.53 visplot 3.7cm X S S S S 0.30 0.7cm Q X X X X 0.0 ===> secondary cal --- No UVMax restriction %%% Don't need to worry about restrictions because B array max is 54.3 kL ^7b. SETJY -> SU/1 executed on 26jun09 (twice) ***Set aparm(2) to correspond to date of observation. If date <1990 aparm(2)=3 If 19921998 aparm(2)=0 ***We need to enter a flux density for each primary (flux) calibrator. If we have only one FREQID, this is easy: default SETJY sources '1331+305','' $ primary (flux) calibrator(s) '0542+498','0137+331', optype 'CALC' freqid = 1 $ First FREQID aparm 0,0 $ data taken after 1998 (2008) getn 64 $ *.LINCOP (then 66) --> / Flux calculated using known spectrum tortue> SETJY1: / Flux calculated using known spectrum tortue> SETJY1: BIF = 1 EIF = 1 /Range of IFs tortue> SETJY1: '1331+305 ' IF = 1 FLUX =14.7325 (Jy calcd) tortue> SETJY1: / Using (1999.2) VLA or Reynolds (1934-638) coefficients ***If we have more than one FREQID, we assume that the frequency offsets used are small, so that the flux densities of the flux calibrators are nearly the same for each FREQID. Typical frequency offsets are of order the bandwidth, +/-3 MHz; at 1420 MHz, for a worst-case spectral index of -1, this leads to an error of 2*3 MHz/1420 MHz= 0.4% -- not worth worrying about. So, we use any FREQID which covers all primary flux calibrators. If flux calibrator A is observed only with FREQID 1, while flux calibrator B is observed only with FREQID 2, we have to run SETJY twice: default SETJY sources '0137+331','' $ primary (flux) calibrator A optype 'CALC'; freqid=1 $ FREQID for A aparm 0,0 $ data taken after 1998 getn 64 $ *.LINCOP ; default SETJY sources '0542+498','' $ primary (flux) calibrator B optype 'CALC'; freqid=2 $ FREQID for B aparm 0,0 $ data taken after 1998 getn 64 $ *.LINCOP ; ^7c. CALRD executed on 26jun09 (twice) ***Read in models of flux density calibrators: $ default CALRD $ object '3c48'; band 'L';$ 0137+331 $ default CALRD $ $ object '3c147'; band 'L';$ 0542+498 default CALRD $ 4 object '3c286'; band 'L';$ 1331+305 ***Note: These models are in J2000 coordinates. If your data are in C1950, change the model images to C1950 with EPOSWTCH. We will later use UVFIX to fix the uv-data. %%% Data is in J2000 coordinates, so no EPOSWTCH needed ^8. PRTUV (used to find integration times on calibrators & sources) default PRTUV cparm 0; cparm(9)=307 $ Pick a baseline -- here, baseline 3-7 (large and both are VLA) docrt 132 getn 64 $ *.LINCOP --> calib: 10s (both) source: 10s ^9. UVFLG -> FG/1 executed on 26jun09 ***We toss the EVLA-EVLA baselines, to avoid dealing with aliasing. There should still be plenty of VLA-EVLA baselines to allow antenna-based solutions for the EVLA... but keep an eye out for oddities (e.g., in BPASS)! default EVLA $ In case doinvers was set to 1 (true) getn 1 $ *.CH0 print EVLA %%% EVLA list is accurate default UVFLG getn 1 $ *.CH0 $ Note that we use FILLM's CH0 for initial flags -- we'll TACOP later. antenna=EVLA; baseline=EVLA; outfgver 1; opcode 'flag'; reason 'EVLA' ***NOTE!!! do NOT run UVFLG if EVLA=0 (try PRINT EVLA to check) -- otherwise you'll delete ALL of your data. ^10. TVFLG -> FG/1 executed on 26jun09 ***Again, we *only* use the original CH 0 from FILLM for initial flagging. Here we flag calibrators only, to remove any gross, obvious problems. ^ Check the first scan carefully -- often the system isn't "organized" on this first scan x On-line flagging isn't as reliable as in the old days, so there are plenty of hot pixels and hiccups. x We are NOT quacking, because (1) FILLM's NX table isn't correct; (2) QUACK flags data from the beginning-of-scan, whereas we want to flag data from antennas-on-source. default TVFLG docat -1 $ avoid saving temporary files dohist -1 $ avoid creation of history entries calcode '*' $ calibrators only freqid 1 $ must step through all FREQIDs! docalib -1 flagver 1; outfgver 1 $ keep all flags in FG/1 dparm 0 dparm(3) 1 $ show baselines twice, to treat all antennas identically -- $ this displays baseline 27-1 as well as 1-27 dparm(6)=10 $ time resolution: should be set to the calibrators' integration $ time, in seconds getn 1 $ *.CH0 $ note this is the ONLY time we use FILLM's Channel 0! ***Within TVFLG: ^ Set useful defaults: ^SMOOTH=1 to avoid averaging date before displays ^SCAN= 20 to use a long time for median filters (AMP/PH DIFF) xFLAG ALL CHANNELS ^FLAG STOKES FULL (usually -- sometimes you'll want NORR or NOLL) ***If individual Stokes need to be flagged, make sure you set the STOKES FLAG to correspond to the polarization that is displayed on the TV ^SWITCH SOURCE FLAG to ONE-SOURCE to avoid inadvertantly flagging galaxy (though sometimes you'll want to of course) ^ Be sure to inspect BOTH polarizations! ***We suggest the following steps: ^ Set the above defaults x Flag first integration in every scan (manual QUACK) -- this should be the first integration AFTER most antennas are on-source, which is why we can't use the usual QUACK. %%% In Amp: flagging straggler times (timeline), but not *every* single scan... ^ Inspect the following: ^AMPLITUDE to check for missing records or antennas %%% Ant 4, 5, 29 out completely (as in PRTAN, but 5 & 29 not mentioned in log) %%% Ant 14 looks pretty bad (L-301 module will not lock)- Flag it all via UVFLG %%% 2nd Pri doesn't seem to be there at all... %%% EVLA-EVLA baselines flagged properly %%% RR: 0.001 - 3.124, LL: 0.000 - 3.304 Trimmed 1 straggly timeline from 2nd, 3rd, 4th, & 5th Secs Trimmed 0 straggly timelines from Pri Flagged very faint areas in 1st Pri in Ants 12 & 27 (08:06:36-08:15:06)-> 0.060-3.124 & 0.041-3.304 Final: RR: (0.060 - 3.124), LL: (0.066 - 3.304) ^AMP DIFF to check for variable gains %%% RR: 0.0 - 309.0 (Pretty clean) %%% LL: 0.0 - 571.5 (some hot pixels) Flagging LL: 15-21, 12:25:16; Ant 25, 08:15:26-> 0.0-126.0 Flagging RR: Ant 1, 08:06:36; 08:19:16 1-2 & 1-3; 1-2, 08:16:06, & 2-24, 08:08:06-> 0.0-146.9 Flagging LL: 13:26:56-27:06-> 0.0-126.0 Final: RR: (0.0 - 144.6), LL: (0.0 - 126.0) ^PHS DIFF to check for variable atmosphere/gains %%% RR: 0.00 - 65.85 (all high values in 1st Pri around the split between the two observations) %%% LL: 0.00 - 63.07 (same as above) Flagging FULL: 08:14:46-08:16:16, Ant 24 08:06:36-08:16 Clipping interactively separately to 20 degrees-> 20.30 & 19.96 Final: RR: (0.00 - 20.30), LL: (0.00 - 19.96) %%% Saved as Figures/B2TVFLG_10_(AMP/AMPDIFF/PHSDIFF)_(RR/LL).tiff using Grab x If your data set is in D array (if your source is southern then also check for this problem in the C array) then keep an open eye for solar interference. In TVFLG, choose SORT BY BASELINE. If the short baselines are brighter than the long baselines, then you probably have solar interference. If solar interference is affecting your data, then in CALIB you should use a UVRANGE. %%% No signs of solar interference %%% 161 Flagging commands applied (mainly from interacting clipping) ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). ^10b. TABED FG/1 executed on 26jun09 (twice) ***Here we TABED the CH 0 flags to LINCOP (with FREQID= -1). After this we're done with FILLM's channel 0. default TABED inext 'fg' inver 1; outver 1; bcount 1; ecount 0; $ until recently there was a parameter called ncount which is no longer there opty 'repl' aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 1 $ *.CH0 getona 64 $ *.LINCOP (then 66) (extra UVFLG on 66: timer 0 08 06 30 0 08 16 20) --> LINCOP FG/1 ^10c. (EXTRA) WIPER on Calibrators in LINCOP executed on 26jun09 (Just to see if there are any hot pixels) default WIPER $ sources '1331+305','' $ Primary $ sources '1313+549','' $ Secondary calcode '*' $ just the calibrators flagver 1 $ only FG table so far smooth 7, 215 $ boxcar average over all channels -- use $ smooth 7, 215 if you started with 255 channels & 7, 107 if you started with 127 channels bparm 0 $ amp. vs. uv-distance imsize 512, 512 getn 64 $ *.LINCOP %%% No hot columns or hot dots- max is ~5.0 (B2WIPER_10c.tiff)-> Looks good ^11. BPASS ***This is a first-order BPASS leading to a new Channel 0. The goal is to avoid closure errors in Channel 0 calibration due to huge delays (phase slopes) on VLA-EVLA baselines. We divide each visibility by the vector average of the inner 3/4 of the band (i.e., an on-the-fly channel 0). Thus we remove source structure (tho' getting the weights wrong) and take care of the amplitude scale. ***There is a split here between the easy case (one FREQID for all sources) and the Galactic HI case (multiple FREQIDs, usually different for the bandpass calibrator and the galaxy (and phase calibrator)). Check LISTR/SCAN to see which you're doing. ^11a. BPASS: one FREQID for all sources -> BP/1 executed several times on 26jun09 default BPASS calsour '1331+305','' $ Select bandpass calibrators '0542+498','0137+331', qual -1 freqid 1 $ here we have only one FREQID docal 1; gainuse 2 $ apply VLANT changes. Probably irrelevant. flagver 1 $ apply initial flags solint 0; soltype '' $ one solution per scan refant 15 $ Change this to your refant smooth 0 $ no smoothing weightit 0 $ L1, L1R, etc. seem _less_ stable -- weird minamper 7; minphser 7 $ report closures > 7%/7d bpassprm 0 bpassprm(2) 1 $ some closure info is printed bpassprm(5) 0 $ derive "channel 0" on a record-by-record basis -- $ more biased than averaging first, but avoids $ some subtle pitfalls (see EXPLAIN file) bpassprm(6) 2 $ print avg. closure errors > 2% bpassprm(7) 2 $ print avg. closure errors > 2d ichansel 0 $ derive channel 0 from inner 3/4 of the band getn 64 $ *.LINCOP --> BP/1 x11b. BPASS: Multiple FREQIDs -> BP/1,2,3 not necessary ***The overall plan here is as follows (assuming FREQIDs 1 and 2 refer to the offset [bandpass calibrator] frequencies, and FREQID 3 refers to that of the galaxy & phase calibrator): (1) run BPASS once for FREQID=1 (-> BP/1) and once for FREQID=2 (-> BP/2). (2) check both BP tables with POSSM. They should look virtually identical. (3) If they do appear virtually identical, we concatenate them: (a) write out both tables [TBOUT], (b) concatenate the two [vi/emacs], (c) read them back in [TBIN] as BP/3, (4) If they do NOT appear identical, there is Something Wrong. The case we've come across involves the use of a front-end filter combined with the use of unexpected LOs (see Adrienne's note), so that one FREQID was observed through the edge of the filter. The resulting bandpasses show a strong slope in the amplitude gains for most VLA antennas. So far we've seen this only for central frequencies around 1423 MHz. In this case, simply copy the "good" BP table to BP/3 using TACOP. (5) modify BP/3 to refer to FREQID=3 [TABED]. ***It is a VERY good idea to use POSSM carefully throughout to be sure you're doing what you think you're doing. x11b1. BPASS FREQID 1 -> BP/1 not necessary default BPASS calsour '0137+331','0542+498','' $ Select bandpass calibrators docal 1 ; gainuse 2 $ apply VLANT changes. Probably irrelevant. flagver 1 $ apply initial flags refant 15 $ Change this to your refant Qual -1 solint 0 $ one solution per scan minamper 7 ; minphser 7 $ report closures > 7%/7d smooth 0 $ no smoothing soltype '' ; weightit 0 $ L1, L1R, etc. seem _less_ stable -- weird bpassprm 0 bpassprm(5) 0 $ derive "channel 0" on a record-by-record basis -- $ more biased than averaging first, but avoids $ some subtle pitfalls (see EXPLAIN file) bpassprm(2) 1 $ some closure info is printed bpassprm(6) 2 $ print avg. closure errors > 2% bpassprm(7) 2 $ print avg. closure errors > 2d ichansel 0 $ derive channel 0 from inner 3/4 of the band freqid 1 $ 1st offset FREQID getn 64 $ *.LINCOP --> BP/1 x11b2. BPASS FREQID 2 -> BP/2 not necessary ***Same as 11B2, now on FREQID 2 default BPASS calsour '0137+331','0542+498','' $ Select bandpass calibrators docal 1 ; gainuse 2 $ apply VLANT changes. Probably irrelevant. flagver 1 $ apply initial flags refant 15 $ Change this to your refant Qual -1 solint 0 $ one solution per scan minamper 7 ; minphser 7 $ report closures > 7%/7d smooth 0 $ no smoothing soltype '' ; weightit 0 $ L1, L1R, etc. seem _less_ stable -- weird bpassprm 0 bpassprm(5) 0 $ derive "channel 0" on a record-by-record basis -- $ more biased than averaging first, but avoids $ some subtle pitfalls (see EXPLAIN file) bpassprm(2) 1 $ some closure info is printed bpassprm(6) 2 $ print avg. closure errors > 2% bpassprm(7) 2 $ print avg. closure errors > 2d ichansel 0 $ derive channel 0 from inner 3/4 of the band freqid 2 $ 2nd offset FREQID getn 64 $ *.LINCOP --> BP/2 x11b3. POSSM to compare BP/1 and BP/2 default POSSM $ to check BPASS results flagver 1 aparm 0, 1, 0.7, 1.3, -180, 180, 0, 2, 0, 0 $ Plot BP, with amp/ph ranges source '0137+331','0542+498','1331+305','' $ POSSM doesn't work with $ source '' for some reason! solint -1 $ Separate plots for each scan nplots 9 $ 9 plots per page bparm 0 dotv 1 freqid 1; bpver 1 ; grch 1 freqid 2; bpver 2 ; grch 2 getn 64 $ *.LINCOP tvinit If worried: try POSSM on secondary calibrator, applying this BPASS (if BPASS stable, secondary should look flat) x11b4. *If* BP/1 and BP/2 appear virtually identical, concantenate them to form BP/3: x11b4a. Write the two tables to disk: default TBOUT docrt 500 getn 64 $ *.LINCOP inext 'bp' ; inver 1 outfile 'LT1:bp1.out inext 'bp' ; inver 2 outfile 'LT1:bp2.out x11b4b. Outside AIPS: concatenate the two tables cd $LT1 cat bp1.out bp2.out > bp3.out emacs bp3.out - change NAXIS2 to be equal to the *sum* of NAXIS2 in the two tables - delete from first ***END*PASS*** through ***BEGIN*PASS***, inclusive x11b4c. Read the new concatenated table in as BP/3: default TBIN infile 'LT1:bp3.out getona 64 $ *.LINCOP --> reads in BP/3 x11b5. *If* BP/1 and BP/2 are NOT virtually identical, pick the one that best matches the behavior of the phase calibrator (possibly by doing a quickie BPASS on the phase calibrator and comparing the results), and copy that BP table to BP/3: default TACOP inext 'bp' inver 2 $ Set this to the "good" BP table getn 64 $ *.LINCOP getona 64 $ *.LINCOP --> BP/3 ***You should IGNORE the "bad" FREQID for all subsequent processing. x11b6. TABED BP/3 to set FREQID=-1 (so we can use the same BP table for everyone) --> BP/4 default TABED opty 'repl' inext 'bp' inver 3 ; outver 4 aparm 0 aparm(1) 8 $ Changing column 8 = FREQID keyval= -1,0 $ ...which we change to FREQID= -1 getn 64 $ *.LINCOP --> BP/4 ^11c. POSSM to check BP table ^11c1. Plot BP table itself default POSSM $ to check BPASS results source '0137+331','0542+498','1331+305','' $ POSSM doesn't work with $ source '' for some reason! freqid 1; bpver 1 $ freqid 3; bpver 4 $ for multiple-FREQID data sets flagver 1 aparm 0, 1, 0.7, 1.3, -180, 180, 0, 2, 0, 0 $ Plot BP, with amp/ph ranges solint -1 $ Separate plots for each scan nplots 9 $ 9 plots per page bparm 0 dotv 1 getn 64 $ *.LINCOP (then 66) tvinit dotv -1; go %%% PL 1-6 for LINCOP are POSSM results, 9 per page There are two plots for each antenna (RR & LL) only for the before primary calibrator (no after here) In general, the VLA antennas have very flat bandpasses around 1.0 with near 0 phase default lwpla $ to print the plots to a ps file getn 64 $ *.LINCOP (then 66) (c2) outfile '/Users/herrmann/Desktop/B2POSSMplots11c1.ps invers 0 for i = 1 to 6; plver = i; go; wait lwpla; end (BPs are a little noisier second time- understandably) ^11c2. Apply BP table to 2ndary calibrator & plot individual baselines default POSSM source='1313+549','' $ Secondary (phase) calibrator freqid 1; bpver 1 $ for single-FREQID data sets $ freqid 3; bpver 4 $ for multiple-FREQID data sets docal 1; gainuse 2; flagver 1; doband 1 $ average all BP entries aparm 0 $ Plot data aparm(1) 1 $ vector average solint -1 $ Separate plots for each scan nplots 9 $ 9 plots per page dotv 1 getn 64 $ *.LINCOP (then 66) tvinit %%% Everything looks normal (looked at one whole time) ^11c3. Apply BP table to 2ndary calibrator & vector average all data default POSSM source='1313+549','' $ Secondary (phase) calibrator freqid 1; bpver 1 $ for single-FREQID data sets $ freqid 3; bpver 4 $ for multiple-FREQID data sets docal 1; gainuse 2; flagver 1; doband 1 $ average all BP entries aparm 0 $ Plot data aparm(1) 1 $ vector average solint 0 $ average all time nplots 0 $ average all baselines dotv 1 getn 64 $ *.LINCOP (then 66) tvinit ***This plot should be flat in both amp. and phase as a function of frequency, with no slope.. If some channels are off, note which ones those are and keep an eye out for interference or other bad data. If there are large errors consider running BPASS on the secondary calibrator and using that to correct the galaxy. Note that this will be somewhat painful since AIPS does not allow incremental BP tables -- unlike SN or CL tables. Sigh. 1(RR): Quite flat around 5.0 mJy for all channels 1(RR): phase is generally 192 +/- 12 degrees 1(LL): Rather flat around 8.5 mJy for all channels 1(LL): phase is generally -80 +/- 10 degrees %%% (Possibly identical the 2nd time through) dotv -1; go tget lwpla for i = 7 to 8; plver = i; go; wait lwpla; end %%% (Added to B2POSSMplots11c1.ps then ...c2.ps) ^12. AVSPC -> NEWCH0.1 (2,3) executed on 26jun09 (twice) ***AVSPC must be run once for each FREQID (unfortunately FREQID=-1 purports to work, but creates an empty data set). This entails some nasty bookkeeping for data sets with multiple FREQIDs. Here I assume we have one or three FREQIDs. If BPASS checks above show that one FREQID is useless, you should ignore that one entirely in this and all subsequent processing. ***We will use these NEWCH0 files for (1) further flagging, and (2) time-dependent gain calibration. ^12a. FREQID=1 --> NEWCH0.1 default AVSPC getn 64 $ *.LINCOP (then 66) freqid 1; bpver 1 $ for single-FREQID data sets $ freqid 1; bpver 4 $ for multiple-FREQID data sets docalib -1; gainuse 0; flagver -1 $ do NOT apply flags doband 1 outname inna ; outcl 'NEWCH0' --> NEWCH0.1 (65) (then 67) x12b. FREQID=2 (if multiple-FREQID data set) --> NEWCH0.2 ***Skip FREQID=2 if the corresponding BP table looked irrelevant (see 11b5) default AVSPC docalib -1;gainuse 0; flagver -1 $ do NOT apply flags doband 1 freqid 2; bpver 4 $ for multiple-FREQID data sets getn 64 $ *.LINCOP outname inna ; outcl 'NEWCH0' ; outse= freqid --> NEWCH0.2 x12c. FREQID=3 (if multiple-FREQID data set) --> NEWCH0.3 ***Skip FREQID=3 if the corresponding BP table looked irrelevant (see 11b5) default AVSPC docalib -1;gainuse 0; flagver -1 $ do NOT apply flags doband 1 freqid 3; bpver 4 $ for multiple-FREQID data sets getn 64 $ *.LINCOP outname inna ; outcl 'NEWCH0' ; outse= freqid --> NEWCH0.3 ^12d. LISTR/SCAN ***It is a VERY good idea to run LISTR/SCAN on each of the NEWCH0 data sets at this point, to be sure each has the data you expect. tget LISTR getn 65 $ *.NEWCH0 outprint '/Users/herrmann/Desktop/Haro29-B2_12d.listr tortue LISTR(31DEC08) 4 26-JUN-2009 15:12:53 Page 1 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 Freq = 1.419127750 GHz Ncor = 2 No. vis = 597895 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0001 A 1 0/08:06:35 - 0/08:20:25 1 1 24759 2 1313+549 : 0001 C 1 0/08:21:35 - 0/08:25:35 1 24760 32235 3 HARO29 : 0001 1 0/08:26:15 - 0/08:51:15 1 32236 76935 4 1313+549 : 0001 C 1 0/08:51:55 - 0/08:56:05 1 76936 84687 5 HARO29 : 0001 1 0/08:56:45 - 0/09:21:45 1 84688 129823 6 1313+549 : 0001 C 1 0/09:22:25 - 0/09:26:35 1 129824 137359 7 HARO29 : 0001 1 0/09:27:15 - 0/09:52:15 1 137360 181625 8 1313+549 : 0001 C 1 0/09:52:55 - 0/09:57:05 1 181626 189135 9 HARO29 : 0001 1 0/09:57:45 - 0/10:17:55 1 189136 224406 10 1313+549 : 0001 C 1 0/10:18:35 - 0/10:22:45 1 224407 231921 11 HARO29 : 0001 1 0/10:23:25 - 0/10:48:25 1 231922 276931 12 1313+549 : 0001 C 1 0/10:49:05 - 0/10:53:15 1 276932 284731 13 HARO29 : 0001 1 0/10:53:55 - 0/11:18:55 1 284732 329817 14 1313+549 : 0001 C 1 0/11:19:45 - 0/11:23:45 1 329818 337293 15 HARO29 : 0001 1 0/11:24:35 - 0/11:49:35 1 337294 382422 16 1313+549 : 0001 C 1 0/11:50:35 - 0/11:54:45 1 382423 390222 17 HARO29 : 0001 1 0/11:55:45 - 0/12:20:35 1 390223 435222 18 1313+549 : 0001 C 1 0/12:21:25 - 0/12:25:35 1 435223 442728 19 HARO29 : 0001 1 0/12:26:25 - 0/12:51:35 1 442729 485005 20 1313+549 : 0001 C 1 0/12:52:25 - 0/12:56:25 1 485006 492481 21 HARO29 : 0001 1 0/12:57:15 - 0/13:22:15 1 492482 537613 22 1313+549 : 0001 C 1 0/13:22:55 - 0/13:27:05 1 537614 545116 23 HARO29 : 0001 1 0/13:27:45 - 0/13:52:55 1 545117 590395 24 1313+549 : 0001 C 1 0/13:53:35 - 0/13:57:35 1 590396 597895 tortue LISTR(31DEC08) 4 26-JUN-2009 15:12:53 Page 2 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 Source summary Velocity type = ' ' Definition = ' ' ID Source Qual Calcode RA(2000.0) Dec(2000.0) IFlux QFlux UFlux VFlux No. vis 1 1331+305 : 0001 A 13:31:08.2879 30:30:32.958 14.732 0.000 0.000 0.000 24759 2 1313+549 : 0001 C 13:13:37.8529 54:58:23.894 0.000 0.000 0.000 0.000 90850 3 HARO29 : 0001 12:26:16.0000 48:29:37.000 0.000 0.000 0.000 0.000 482286 ID Source Freq(GHz) Velocity(Km/s) Rest freq (GHz) 1 1331+305 1.4191 -138.0267 0.0000 2 1313+549 1.4191 0.0000 0.0000 3 HARO29 1.4191 0.0000 0.0000 Frequency Table summary FQID IF# Freq(GHz) BW(kHz) Ch.Sep(kHz) Sideband 1 1 1.41912775 4.5705 982.6661 1 ^13. TABED LINCOP FG/1 -> NEWCH0 FG/1 ***We use TABED to set FREQID to -1 (apply to all FREQIDs) in the FG table, since AVSPC will change all FREQIDs to 1 in the NEWCH0 data sets. ^13a. NEWCH0.1 default TABED inext 'fg' inver 1; outver 1 opty 'repl' aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 64 $ *.LINCOP (then 66) getona 65 $ *.NEWCH0.1 (then 67) --> NEWCH0.1, FG/1 x13b. If multiple FREQIDs: NEWCH0.2 default TABED inext 'fg' inver 1 ; outver 1 opty 'repl' aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 64 $ *.LINCOP getona 65 $ *.NEWCH0.2 --> NEWCH0.2, FG/1 x13c. If multiple FREQIDs: NEWCH0.3 default TABED inext 'fg' inver 1 ; outver 1 opty 'repl' aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 64 $ *.LINCOP getona 65 $ *.NEWCH0.3 --> NEWCH0.3, FG/1 ^14. CALIB -> NEWCH0.1(,2,3) SN/1 executed on 26jun09 (twice) (full uvrange) ***If we only have one FREQID, all CALIBs are run on the same NEWCH0.1 . If we have multiple FREQIDs, CALIBs for a given source must be run for all NEWCH0.1,2,3 in which that source appears (probably easiest to check with LISTR/SCAN). ***Note: if 'SN' table must be destroyed: task 'extdest'; inext 'sn'; invers 0 ***If solar interference is affecting your data then in CALIB you should use a UVRANGE. The worst case scenario, baselines up to a distance of 1 kilolambda could be affected, while in the best case scenario baselines are affected only up to 0.5 kilolambda distance. We recommend using: UVRANGE 0.7,0 for D array UVRANGE 0.7,0 for C array After calibration, if UVPLT still shows signs of solar interference, it means that not enough short baselines were discarded; therefore the calibration has to be redone and UVRANGE to be reset. Note that the Sun might rise or set, especially during a long B-array run, in which case you might wish to split the calibration by timerange in a set affected and a set without solar interference. ^14a. Primary (flux density) calibrators --> SN/1 default CALIB get2n 4 $ 3C286_L.MODEL.1 calsour '1331+305','' $ flux density calibrator #1 freqid -1 uvrange 0, 0 $ no signs of solar interference in primary weightit 1 docal 1; gainuse 2; flagver 1 inver 1; ncomp 1e6, 0; nmap 1; cmethod 'DFT' refant 15 $ Change this to your refant solint 0 aparm 4,0,0,0,0,2; $ min 4 antennas; print closures soltype 'L1'; solmode 'A&P' $ true L1 minimization solcon 0 minamper 10; minphser 10 $ complain if >10%/10d off cparm 0,0,10,10,1 $ complain if avg > 10%/10d off snver 1 getn 65 $ *.NEWCH0 $ ***NOTE: must run this for all NEWCH0.1,2,3 in which this calibrator appears! --> SN/1 tortue> CALIB1: RPOL, IF= 1 The average gain over these antennas is 3.168E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 3.103E+00 tortue> CALIB1: Found 46 good solutions tortue> CALIB1: Failed on 4 solutions tortue> CALIB1: Average closure rms = 0.0436 +- 0.0012 tortue> CALIB1: No data were found > 99.0 rms from solution 2nd time through: tortue> CALIB1: RPOL, IF= 1 The average gain over these antennas is 3.108E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 3.042E+00 tortue> CALIB1: Found 50 good solutions tortue> CALIB1: Average closure rms = 0.0011 +- 0.0000 tortue> CALIB1: No data were found > 99.0 rms from solution $ This time there is no second primary default CALIB get2n 210 $ 3B247_L.MODEL.2 calsour '0542+498','' $ no second flux density calibrator freqid -1 uvrange 0, 0 $ no signs of solar interference in primary weightit 1 docal 1; gainuse 2; flagver 1 inver 1; ncomp 1e6, 0; nmap 1; cmethod 'DFT' refant 15 $ Change this to your refant solint 0 aparm 4,0,0,0,0,2; $ min 4 antennas; print closures soltype 'L1'; solmode 'A&P' $ true L1 minimization solcon 0 minamper 10; minphser 10 $ complain if >10%/10d off cparm 0,0,10,10,1 $ complain if avg > 10%/10d off snver 1 getn 65 $ *.NEWCH0 $ ***NOTE: must run this for all NEWCH0.1,2,3 in which this calibrator appears! --> SN/1 ^14b. Secondary (phase) calibrator --> SN/1 ***Check uv restrictions for secondary calibrators carefully. For 1313+549: no restrictions, no solar interference, so uvra= 0.0,0 default CALIB calsour '1313+549','' $ phase calibrator freqid -1 uvrange 0.0, 0 $ Some solar interference wtuv 0.0 $ normally 0.0, but may have to set wtuv 0.01 if solutions are $ crazy and uvrange is not 0,0 weightit 1 docal 1; gainuse 2; flagver 1 refant 15 $ Change this to your refant solint 0 aparm 4,0,0,0,0,2; $ min 4 antennas; print closures soltype 'L1'; solmode 'A&P' $ true L1 minimization solcon 0 minamper 10; minphser 10 $ complain if >10%/10d off cparm 0,0,10,10,1 $ complain if avg > 10%/10d off snver 1 getn 65 $ *.NEWCH0 $ ***NOTE: must run this for all NEWCH0.1,2,3 in which $ this calibrator appears! tortue> CALIB1: RPOL, IF= 1 The average gain over these antennas is 2.697E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 2.640E+00 tortue> CALIB1: Found 600 good solutions tortue> CALIB1: Average closure rms = 0.0072 +- 0.0003 tortue> CALIB1: No data were found > 99.0 rms from solution 2nd time through: tortue> CALIB1: RPOL, IF= 1 The average gain over these antennas is 2.696E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 2.641E+00 tortue> CALIB1: Found 600 good solutions tortue> CALIB1: Average closure rms = 0.0072 +- 0.0003 tortue> CALIB1: No data were found > 99.0 rms from solution x15a. TABED all SN tables to NEWCH0.1 --> SN/2,3 ***This step is only required if we have more than one FREQID (NEWCH0). We copy everything to NEWCH0.1 to match the FREQID=1 case. ***Skip this step if you only have one FREQID! default TABED inext 'sn' inver 1; outver 0 opty 'repl' aparm 0 aparm(1) 6 $ Changing column 3 = FREQID keyval= -1,0 $ ...which we change to FREQID= -1 getn 65 $ *.NEWCH0.2 getona 65 $ *.NEWCH0.1 --> NEWCH0.1, SN/2 default TABED inext 'sn' inver 1 ; outver 0 opty 'repl' aparm 0 aparm(1) 6 $ Changing column 3 = FREQID keyval= -1,0 $ ...which we change to FREQID= -1 getn 65 $ *.NEWCH0.3 getona 65 $ *.NEWCH0.1 --> NEWCH0.1, SN/3 ^15b. GETJY SN/1-3, SU/1 executed on 26jun09 & 29jun09 ***Find flux density of secondary calibrator, and set SN table amplitude gains to reflect a common flux density scale. default GETJY sources '1313+549','' $ Secondary (phase) calibrators) calsour '1331+305','' $ Primary (flux) calibrators '0542+498','0137+331', freqid -1 snver 0 $ Use all SN tables getn 65 $ *.NEWCH0.1 (then 67) tortue> GETJY1: Task GETJY (release of 31DEC08) begins tortue> GETJY1: Source:Qual CALCODE IF Flux (Jy) tortue> GETJY1: 1313+549 : 1 C 1 1.33876 +/- 0.01004 %%% (A bit higher than expected 1.31 Jy.) 2nd time through: tortue> GETJY1: Task GETJY (release of 31DEC08) begins tortue> GETJY1: Source:Qual CALCODE IF Flux (Jy) tortue> GETJY1: 1313+549 : 1 C 1 1.32490 +/- 0.00723 %%% Still a bit higher than expected, but not quite as high as before. x15c. CLCAL/MERG to merge all SN tables -> SN/4 ***This step is only required if we have more than one FREQID (NEWCH0). Skip this step if you only have one FREQID! default CLCAL opcode 'MERG' $ Merge SN tables, for ease of plotting etc. refant 15 $ Change this to your refant getn 65 $ *.NEWCH0.1 --> SN/4 $ creates a merged SN table -- doesn't change CL tables at all. Must now copy this new SN table to all other NEWCH0: default TACOP inext 'SN' getn 65 $ *.NEWCH0.1 getona 65 $ *.NEWCH0.2 getona 65 $ *.NEWCH0.3 ^16. SN table checks ^16a. SNPLT last SN table executed on 26jun09 & 29jun09 ^16a1. SNPLT phase: default SNPLT inext 'sn'; inver 0 pixrange 0; nplots 9; xinc 1 optype 'phas'; opcode 'alsi' do3col 1; symbol 5; factor 2 dotv 1 getn 65 $ *.NEWCH0.1 (then 67) ===> Note any phase jumps (on the phase calibrator) for future flagging. The EVLA antennas, even after applying VLANT, still show quite a bit of phase drift. This is OK so long as a linear interpolation between the phases looks like it will work. %%% Note: displaying first primary, all 12 secondary observations, but no the second primary In general, few jumps (1-28) (besides the jump from primary to secondary which is ok) (Note: Ref antenna 15 red triangles at values of 0 because everything relative to it.) %%% Grabbed each frame: B2SNPLT_16a1_PHS(a-c).tiff (then ...2.tiff) ^16a2. SNPLT amplitude: default SNPLT inext 'sn'; inver 0 pixrange 0; nplots 9; xinc 1 optype 'amp'; opcode 'alsi' do3col 1; symbol 5; factor 2 dotv 1 getn 65 $ *.NEWCH0.1 (then 67) ===> Note whether the amp. is roughly constant for a given antenna/pol'n/IF. %%% In general, some small jumps (1-28) (besides the jump from primary to secondary which is ok) !!! 1st Pri isn't showing for Ant 12 or 27... %%% Grabbed each frame: B2SNPLT_16a2_AMP(a-c).tiff (then ...2.tiff) ***We have seen a couple cases where the first phase cal scan has a significantly different amplitude gain for the EVLA antennas. The reason is not clear but the raw data do show this effect, so CALIB is doing the right thing. This area warrants further tests, to learn whether we should simply flag the EVLA antennas on the first phase calibrator scan. ^16b. LISTR/GAIN print SN table executed on 26jun09 & 29jun09 default LISTR optype 'gain'; inext 'sn'; inver 1; freqid -1 antennas -4,5,14,29,0; $ may have to list missing antennas explicitly, to avoid $ column overrun. To list missing antennas, use the form $ANTENNAS -3,2,0 to have antennas 3 and 2 left out. dparm 5,0; $ Amp & phase factor 0; docrt -1 $ instead of docrt 132 outprint '/Users/herrmann/Desktop/Haro29-B2_16b.listr $ then ...b2.listr getn 65 $ *.NEWCH0.1 (then 67) --> check for phase jumps and other inconsistencies. ***We have seen a couple cases where the first phase cal scan has a significantly different amplitude gain for the EVLA antennas. The reason is not clear but the raw data do show this effect, so CALIB is doing the right thing. This area warrants further tests, to learn whether we should simply flag the EVLA antennas on the first phase calibrator scan. tortue LISTR(31DEC08) 4 26-JUN-2009 15:27:07 Page 1 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419127750 GHz Ncor= 2 No. vis= 597895 Polarization = R Subarray = 0 Listing SN table, version 1 SN table has not been applied to a CL table Gain amplitudes, 1000 = 10.000000 Stokes = R IF = 1 Freq = 1.419127750 GHz Time Source -1- -2- -3- -6- -7- -8- -9--10--11--12--13--15-*16*-17--18--19--20-*21*-22-*23*-24--25-*26*-27--28- max % diff 3.3 1.4 1.0 1.6 1.5 1.2 1.8 2.3 2.7 1.7 3.1 1.9 5.1 3.8 4.1 2.8 1.8 5.0 0.6 5.9 2.0 4.6 5.6 1.0 1.3 Day # 0 08:13:30 1331+305 220 204 258 264 307 285 237 308 276 365 299 382 334 463 355 295 343 264 390 314 468 361 294 08:23:35 1313+549 220 205 263 271 316 288 239 312 270 284 370 306 377 330 462 350 303 343 272 381 309 486 353 251 299 08:54:05 1313+549 218 209 266 273 315 292 242 311 279 282 354 306 378 320 451 345 299 344 270 378 319 499 345 251 299 09:24:35 1313+549 227 205 263 265 316 290 239 312 272 280 372 301 382 329 446 355 301 341 271 377 311 474 349 251 299 09:55:05 1313+549 220 207 265 269 316 288 242 313 276 279 365 311 376 313 448 342 300 339 270 379 308 477 345 253 304 10:20:45 1313+549 218 210 261 270 315 293 246 316 268 284 364 307 368 322 445 343 300 338 269 381 319 476 341 250 297 10:51:10 1313+549 220 210 261 270 315 291 241 322 271 280 360 309 371 307 445 342 307 338 270 378 311 466 338 250 304 11:21:45 1313+549 217 209 262 272 311 295 241 317 271 285 367 308 367 318 464 345 304 338 269 376 314 472 344 251 301 11:52:40 1313+549 220 209 264 268 314 292 242 316 269 283 361 309 353 316 445 344 302 338 271 377 316 476 344 252 301 12:23:35 1313+549 221 208 263 267 318 291 241 313 270 288 368 302 359 322 434 352 299 337 272 375 309 478 341 250 302 12:54:25 1313+549 221 209 263 268 317 292 243 317 272 282 365 308 358 315 437 344 302 339 271 381 312 468 347 253 301 13:25:05 1313+549 219 208 264 270 318 295 242 315 276 284 369 310 362 328 432 343 302 338 271 387 317 480 349 254 302 13:55:35 1313+549 216 207 264 270 319 291 243 312 267 286 369 306 348 310 440 338 301 321 270 355 307 473 324 253 301 tortue LISTR(31DEC08) 4 26-JUN-2009 15:27:07 Page 2 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419127750 GHz Ncor= 2 No. vis= 597895 Polarization = L Subarray = 0 Listing SN table, version 1 SN table has not been applied to a CL table Gain amplitudes, 1000 = 10.000000 Stokes = L IF = 1 Freq = 1.419127750 GHz Time Source -1- -2- -3- -6- -7- -8- -9--10--11--12--13--15--16--17-*18*-19--20--21--22--23--24--25--26--27--28- max % diff 3.1 2.4 1.4 0.9 1.0 1.8 1.5 1.5 3.1 2.0 3.0 1.8 2.8 2.4 5.9 2.0 1.2 1.2 1.0 2.7 3.0 2.8 1.2 1.0 1.0 Day # 0 08:13:30 1331+305 267 216 301 287 304 239 213 290 339 332 245 395 257 437 368 301 370 246 341 390 403 315 281 08:23:35 1313+549 268 217 305 291 311 241 215 293 334 256 339 247 396 254 439 365 308 367 252 343 383 423 320 245 281 08:54:05 1313+549 268 220 309 294 311 242 217 293 347 256 325 250 397 247 430 358 305 365 250 355 383 417 316 246 283 09:24:35 1313+549 275 217 306 290 311 240 215 291 339 254 341 244 391 255 420 368 308 364 252 355 370 410 318 245 283 09:55:05 1313+549 264 219 308 293 313 240 218 296 342 250 331 252 388 245 420 358 307 359 251 355 368 401 316 248 286 10:20:45 1313+549 265 225 304 294 312 239 220 294 333 254 335 249 379 248 417 362 305 362 250 356 382 410 316 245 282 10:51:10 1313+549 268 222 303 292 313 241 215 298 339 255 334 250 383 246 404 359 310 363 248 355 372 405 316 245 286 11:21:45 1313+549 266 218 303 295 309 244 217 294 333 256 337 249 379 248 415 362 310 361 248 351 372 411 314 245 283 11:52:40 1313+549 269 219 302 292 311 242 217 292 334 254 330 249 379 248 417 360 305 365 250 348 377 419 317 248 282 12:23:35 1313+549 268 219 304 290 314 241 215 291 335 259 337 245 383 251 396 368 303 359 250 350 363 414 313 245 284 12:54:25 1313+549 266 220 302 293 312 241 218 294 335 256 338 249 383 246 404 361 308 363 248 354 370 411 317 248 285 13:25:05 1313+549 265 220 305 295 310 246 218 294 340 254 337 250 386 254 411 356 305 365 249 354 379 412 318 249 281 13:55:35 1313+549 260 221 307 293 315 243 216 294 329 256 336 248 388 246 402 354 307 360 247 353 374 407 315 249 283 tortue LISTR(31DEC08) 4 26-JUN-2009 15:27:07 Page 3 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419127750 GHz Ncor= 2 No. vis= 597895 Polarization = R Subarray = 0 Listing SN table, version 1 SN table has not been applied to a CL table Gain phases in degrees Stokes = R IF = 1 Freq = 1.419127750 GHz Time Source -1- -2- -3- -6- -7- *8* -9--10-*11*-12-*13*-15-*16**17**18**19*-20-*21**22**23**24**25**26*-27--28- max diff 9 8 7 4 8 10 3 4 19 3 14 0 11 14 18 11 3 16 12 18 19 11 14 8 5 Day # 0 08:13:30 1331+305 91 -69 -88 -33 160 63-141 110 55 0 0 -88-152 157 -12 -17-174 76 -71 93 -54 3 -29 08:23:35 1313+549 -20 -70 -76 -34 152 61-143 113 -36 131-116 0 162 82 46-124 -14 83 70-162 -1-166-119 64 -21 08:54:05 1313+549 -27 -74 -75 -38 154 56-141 109 -46 130-130 0 151 68 28-133 -16 80 68-169 -8-175-129 65 -20 09:24:35 1313+549 -32 -73 -82 -37 150 56-141 110 -63 129-141 0 145 61 14-137 -13 71 73 173 -12 176-139 63 -25 09:55:05 1313+549 -36 -74 -79 -38 145 60-143 111 -65 130-155 0 141 55 -1-138 -15 64 67 168 -17 165-151 60 -24 10:20:45 1313+549 -41 -71 -77 -37 153 58-142 112 -69 129-158 0 133 50 -9-144 -13 62 74 164 -20 169-148 66 -19 10:51:10 1313+549 -49 -79 -77 -38 152 58-144 111 -75 128-168 0 127 46 -21-153 -16 51 77 162 -23 159-158 60 -21 11:21:45 1313+549 -57 -73 -77 -38 158 57-141 112 -82 130-175 0 120 43 -26-161 -15 47 89 153 -39 156-160 68 -20 11:52:40 1313+549 -64 -76 -83 -37 158 56-141 111-101 131 176 0 115 38 -31-163 -17 31 77 137 -37 146-169 67 -25 12:23:35 1313+549 -67 -73 -86 -35 161 66-141 111-113 131 175 0 118 38 -33-169 -17 28 84 127 -45 143-175 70 -28 12:54:25 1313+549 -76 -77 -89 -35 156 65-141 110-116 131 168 0 111 29 -41-180 -19 17 84 120 -48 133 171 65 -31 13:25:05 1313+549 -84 -78 -89 -36 155 64-141 112-123 131 162 0 102 17 -47 170 -17 11 83 111 -67 124 162 63 -29 13:55:35 1313+549 -92 -78 -86 -37 154 63-141 110-125 128 154 0 96 10 -55 163 -18 8 78 112 -71 120 155 65 -28 tortue LISTR(31DEC08) 4 26-JUN-2009 15:27:07 Page 4 File = Haro29-B2 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419127750 GHz Ncor= 2 No. vis= 597895 Polarization = L Subarray = 0 Listing SN table, version 1 SN table has not been applied to a CL table Gain phases in degrees Stokes = L IF = 1 Freq = 1.419127750 GHz Time Source -1- -2- -3- -6- -7- *8* -9--10-*11*-12-*13*-15-*16**17**18**19*-20-*21**22**23**24**25**26*-27--28- max diff 9 7 8 2 8 10 3 2 18 2 12 0 10 13 16 11 5 16 12 18 19 10 14 7 6 Day # 0 08:13:30 1331+305-173-114 16-120 -25 72 -65 109-128 -161 0-146 70-108 110 -66 67 78 171-147 173 133 91 08:23:35 1313+549 75-115 28-122 -33 71 -66 112 141-155 83 0 105 -55 141 -2 -63 -35 72 80 121 57 11-101 99 08:54:05 1313+549 70-118 30-124 -30 68 -66 110 132-157 71 0 95 -68 126 -10 -61 -37 71 75 114 49 3-100 101 09:24:35 1313+549 65-118 22-122 -34 66 -67 111 115-158 59 0 87 -75 110 -15 -60 -47 74 57 110 41 -8-102 95 09:55:05 1313+549 61-118 25-122 -38 70 -68 112 114-156 47 0 85 -79 97 -15 -60 -52 70 53 106 33 -19-104 97 10:20:45 1313+549 56-114 29-121 -30 70 -67 113 110-156 44 0 77 -84 88 -21 -58 -55 76 49 103 34 -17 -98 102 10:51:10 1313+549 48-121 29-122 -31 69 -69 113 104-156 34 0 72 -86 78 -29 -63 -65 80 47 101 24 -25-102 100 11:21:45 1313+549 40-115 29-122 -25 68 -66 113 97-154 28 0 65 -89 72 -37 -62 -69 92 37 84 22 -28 -95 101 11:52:40 1313+549 34-118 22-121 -25 68 -66 114 79-153 18 0 59 -95 67 -38 -64 -85 80 22 86 12 -37 -95 96 12:23:35 1313+549 31-115 19-119 -23 78 -65 112 67-152 18 0 64 -94 65 -45 -65 -87 88 12 78 9 -43 -93 93 12:54:25 1313+549 22-118 15-119 -28 76 -66 112 63-153 9 0 56-103 57 -56 -67 -99 86 4 75 -1 -57 -97 90 13:25:05 1313+549 14-120 16-120 -30 75 -65 113 57-154 3 0 46-116 50 -66 -65-105 85 -4 56 -10 -67 -99 92 13:55:35 1313+549 5-119 19-121 -31 74 -66 112 54-155 -4 0 41-124 43 -73 -67-107 81 -4 53 -14 -73 -97 93 %%% Max Phase dips/jumps: LOTS of bounces by 10-19 degrees, but looks pretty gradual, so leave as is %%% Amp changes: 5 bounces between 5 and 5.9%, so leave as is %%% No flagging needed. =) %%% Essentially the same 2nd time through. x17. UVFLG -> NEWCH0.1 FG/1 executed on [Not needed!] ***If the SN table shows a phase jump on the phase calibrator, you should flag the data between the two phase cal scans which show the jump (since those cannot be calibrated). ***Note that we flag NEWCH0.1, *regardless* of whether the galaxy appears in this data set. This is because later on (step 20/TVFLG) we flag the NEWCH0 data in order from inseq 1 through inseq freqid_max, copying the FG table from one file to the next. UVFLG itself doesn't care whether the flags you enter actually do anything -- it just adds entries to the FG table, which are then applied (or ignored if irrelevant) by other tasks. ***This step may of course be skipped if there are no obvious phase jumps. Need to flag last 2 galaxy scans in Ant 21 FULL default UVFLG timer 0 10 24 00 0 10 43 30 $ the source scan between the offending ph.cal scans (3rd galaxy) antenna 21, 0 $ the antennas which "jumped" stokes '' outfgver 1 opcode 'FLAG' reason 'some secs shadowed' $ normally 'phase jump' getn 65 $ *.NEWCH0.1 timer 0 10 48 00 0 11 07 30 --> NEWCH0.1 FG/1 ^18. CLCAL NEWCH0 --> CL/3 executed on 26jun09 & 29jun09 ***For multi-FREQID data this becomes rather complicated, since we need a new CL table for every NEWCH0 file, to allow detailed checks and second-order flagging. ***Note that there is no need to work around any phase jumps, since the intervening data are flagged (see step 17 above [UVFLG]). ^18a. CLCAL for the primary calibrators -> CL/3 default CLCAL sour= '1331+305','' $ Primary (flux) calibrators '0542+498','0137+331', calsour= sour interpol 'SELF' dobtween -1 $ Don't interpolate entries for different sources snver 1 $ if single FREQID $ snver 4 $ if multiple FREQIDs gainver 2; gainuse 3 refant 15 $ Change this to your refant getn 65 $ *.NEWCH0.1 (then 67) $ do this for all NEWCH0 with primary (flux) $ calibrator data ^18b. CLCAL for the phase calibrator and galaxy -> CL/3 default CLCAL sour= '1313+549','Haro29','' $ Secondary (phase) calibrator + galaxy calsour= '1313+549','' $ Secondary (phase) calibrator interpol 'SIMP' cutoff 120 $ Don't extrapolate/interpolate beyond 120 minutes dobtween -1 $ Don't interpolate entries for different sources snver 1 $ if single FREQID $ snver 4 $ if multiple FREQIDs gainver 2; gainuse 3 refant 15 $ Change this to your refant ***If your data set used +/- frequency switching for the phase calibrator (our observations did not, but some archival data may), you should use BPARM with SAMPTYPE='BOX' to select a smoothing time which covers both frequency settings. LISTR/SCAN on LINCOP will help you choose this; normally something like 12 minutes should be OK. bparm 12/60 ; samptype='BOX' getn 65 $ *.NEWCH0.1 (then 67) $ do this for all NEWCH0 with secondary (phase) $ calibrator or galaxy data ***At this point we have a new CL table for all NEWCH0 files. ^19a. ANBPL executed on 26jun09 & 29jun09 ***We use ANBPL to check the data weights. Data with very high weights (factor 5-10 or more above normal) should be flagged with UVFLG. ***Note: Red is RR and Blue is LL default ANBPL docalib 1; gainuse 3 flagver 1 do3col 1 $ ...using different colors opcode 'alsi' $ Plot all IFs together bparm 2,17,0 $ Plot antenna-based weight vs. time nplots 9; dotv 1 docrt -1 $ Print as well as plotting weights -- useful for $ finding exact times of bad weights $ Note you can also use outprint to send to a file. outprint '/Users/herrmann/Desktop/B2ANBPL_19a.txt $ then ...a2.txt getn 65 $ *.NEWCH0.1 (then 67) $ Must do this separately for every NEWCH0 file %%% Grabbed each frame: B2ANBPL_19(a-c).tiff (MIDDLE times!) Everything looks good, I guess- no high weights EXCEPT for: a few high weights FULL in Ant 13, 17, 21, 25 ~09:30 (0 09 27 10 0 09 27 20)-> all antennas (either bad or nothing there) ~10:00 (0 09 57 40 0 09 57 50) ~10:25 (0 10 23 20 0 10 23 30) %%% 2nd time through identical, except now the 1st Pri is there for antennas 12 & 27 and there's less Pri in the others ^19b. UVFLG to eliminate very high weights executed on 26jun09 & 29jun09 ***Should UVFLG on NEWCH0.1, even if Evil Weights are seen in NEWCH0.2 or NEWCH0.3 -- we'll be copying FG/1 from NEWCH0.1 to NEWCH0.2 for subsequent second-order flagging. default UVFLG getn 65 $ *.NEWCH0 (then 67) timerang 0 09 27 10 0 09 27 20 antennas 0 $ Can be all antennas in this case because there are either no values or bad values stokes '' outfgver 1 opcode 'FLAG' reason 'HIGH WEIGHT' timer 0 09 57 40 0 09 57 50 timer 0 10 23 20 0 10 23 30 tget ANBPL; outprint 'delete.txt Now everything looks good! default prtmsg docrt -1 outprint '/Users/herrmann/Desktop/AIPSMSGSRV_B2_Steps1_19.log prtmsg clrmsg ^20. TVFLG FG/1 executed on 26jun09 & 29jun09 ^20a. TVFLG on calibrators: NEWCH0.1 The calibrators should now have constant amplitude and zero phase...apart from source structure for the primary (flux) calibrators, and any uvrange for the secondary (phase) calibrators. If we see huge problems on the calibrators we may have to re-run CALIB etc. -- let's hope not!! default TVFLG docat -1 $ avoid saving temporary files dohist -1 $ avoid creation of history entries calcode '*' $ calibrators only docalib 1; gainuse 3 $ apply the new CL table flagver 1; outfgver 1 $ keep all flags in FG/1 dparm 0 dparm(3) 1 $ show baselines twice, to treat all antennas identically -- $ this displays baseline 27-1 as well as 1-27 dparm(6)=10 $ time resolution: should be set to the calibrators' $ integration time, in seconds getn 65 $ *.NEWCH0.1 (then 67) ***Within TVFLG: ^ Set useful defaults: ^SMOOTH=1 to avoid averaging date before displays ^SCAN= 20 to use a long time for median filters (AMP/PH DIFF) xFLAG ALL CHANNELS ^FLAG STOKES FULL (usually -- sometimes you'll want NORR or NOLL) ***If individual Stokes need to be flagged, make sure you set the STOKES FLAG to correspond to the polarization that is displayed on the TV ^SWITCH SOURCE FLAG to ONE-SOURCE to avoid inadvertantly flagging your galaxy (though sometimes you'll want to of course) ^ Be sure to inspect BOTH polarizations! ***We suggest the following steps: ^ Set the above defaults ^ Check AMPLITUDE, AMP DIFF, PHS DIFF. Be wary of known source structure and uv-range limits!! %%% AMP RR: (0.80 - 15.99) Looks good (EXCEPT NO PRI FOR ANTS 12 & 27!!) AMP LL: (0.82 - 15.84) Looks good AMP DIFF RR: (0.000 - 1.201) Looks good (except some nasty spots in Pri of Ant 24) AMP DIFF LL: (0.000 - 1.107) Looks good (except some nasty spots in Pri of Ant 24) PHS DIFF RR: (0.00 - 23.52) Looks good (a bit higher than usual, but this Sec is fainter) PHS DIFF LL: (0.00 - 21.05) Looks good (same as above) ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). %%% No flagging needed. =) 2nd time through: %%% AMP RR: (0.80 - 15.67) Looks good (NOW *WITH* PRI FOR ANTS 12 & 27!) AMP LL: (0.81 - 15.58) Looks good AMP DIFF RR: (0.0 - 960.2) Looks good (except some nasty spots in Pri of Ant 24) AMP DIFF LL: (0.000 - 1.043) Looks good (except some nasty spots in Pri of Ant 24) PHS DIFF RR: (0.00 - 23.58) Looks good (a bit higher than usual, but this Sec is fainter) PHS DIFF LL: (0.00 - 21.04) Looks good (same as above) %%% Still no flagging needed. =) x20b. If we have multiple NEWCH0s (FREQIDs): (1) Copy the FG table: default TABED opty 'repl' inext 'FG' ; inver 1 ; outver 2 bcount 1;ecount 0; aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 65 $ *.NEWCH0.1 getona 65 $ *.NEWCH0.2 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 65 $ *.NEWCH0.2 (2) Assuming there are three FREQIDs, we do this yet again: Copy the FG table: default TABED opty 'repl' inext 'FG' ; inver 2 ;outver 2 bcount 1;ecount 0; aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...to FREQID= -1 getn 65 $ *.NEWCH0.2 getona 65 $ *.NEWCH0.3 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 65 $ *.NEWCH0.3 ^21. Calibration/flagging checks: calibrators ^21a. UVPLT executed on 26jun09 & 29jun09 ***Check the amp & phase vs. uv-distance for all calibrators. Amplitude should match the results of SETJY/GETJY. If there are obvious outliers which are not expected due to source structure, go back and flag those (and possibly re-run CALIB etc.). default UVPLT calcode '*' docal 1; gainuse 3 flagver 1 $ set this to the latest FG version -- may be >1 if $ there are multiple NEWCH0s (FREQIDs). do3col 1 dotv 1 getn 65 $ *.NEWCH0.1 (then 67) $ do this for each NEWCH0 file bparm 0 $ amp. vs. uv-distance dotv -1; go -> PL version 1 same as grabbed B2UVPLT_21a_AMP.tiff -> Looks pretty good Primary generally ~14.7 +/- 0.7 Jy; supposed to be 15.0 Jy; falls off a bit, and some extra scatter Secondary generally ~1.3 +/- 0.5 Jy; supposed to be 1.31 Jy; quite clean Constant the whole way-> as expected because no limits on UVmax EVEN THE SECONDARIES IN ANTS 12 & 27 LOOK BEAUTIFULLY CALIBRATED! (B2UVPLT_21a_AMP_1227.tiff) 2nd tine through: result virtually unchanged: B2UVPLT_21a_AMP2.tiff !!!Stopped HERE to go back... bparm 0, 2 $ phase vs. uv-distance dotv -1; go -> PL version 2 same as grabbed B2UVPLT_21a_PHS.tiff %%% Pretty clean! Looks like Pri is roughly 0 +/- 5 degrees and Secs are 0 +/- 12 degs All scatter within -30 to 25 degrees ^21b. IMAGR executed on 29jun09 [if desired -- this is not really necessary] ***Note: If uvwtfn is set to 'NA' it will override any value given to robust. default IMAGR sources '1313+549','' $ calibrator to image docalib 1; gainuse 3 $ apply latest calibration flagver 1 $ apply latest flags -- set this to the $ highest-numbered FG table outname 'Haro29B2sec cellsize 1 $ for B configuration $ cellsize 3.5 $ for C configuration $ cellsize 10 $ for D configuration imsize 1024 $ for B array $ imsize 512 $ for C and D array uvwtfn 'NA'; robust 0.5 niter 1000 nbox 1; clbox -1,5,512,513 $ calibrator should be in the center (for B) $ nbox 1; clbox -1,5,256,257 $ calibrator should be in the center (for C & D) minpa 121 dotv 1 getn 67 $ *.NEWCH0.xx $ whichever file has the calibrator you're imaging --> shouldn't see obvious calibration errors or striping. CLEANed flux density should roughly match SETJY/GETJY. %%% Looks clean, beautiful point source, and basically alone tortue> IMAGR1: Loading field 1 to TV from -3.794E-03 to 1.322E+00 tortue> IMAGR1: Field 1 final Clean flux 1.280 Jy (A bit low wrt expected 1.32 Jy from GETJY and 1.31 Jy from catalog.) *** Note: If you have extended sources (instead of point sources), probably you just have poor uv-coverage. You can look at your uv-coverage using UVPLT with bparm 6, 7, 0 where good uv-coverage should result in a roughly circular pattern whereas bad uv-coverage may be more like a snowflake with outer gaps. The sources will not be extended when all the data sets are combined. %%% Plot of uv-coverage is nicely circular (excellent uv coverage) Grabbed B2UVPLT_uv_coverage.tiff (same as PL 3) ^22. TVFLG on the galaxy: NEWCH0.xx ***This is our first run of flagging on the galaxy. ^ Check the first scan carefully -- often the system isn't "organized" on this first scan x On-line flagging isn't as reliable as in the old days, so there are plenty of hot pixels and hiccups. x We are NOT quacking, because (1) FILLM's NX table isn't correct; (2) QUACK flags data from the beginning-of-scan, whereas we want to flag data from antennas-on-source. ^22a. If there's only one NEWCH0 (FREQID): default TVFLG docat -1 $ avoid saving temporary files dohist -1 $ avoid creation of history entries calcode '-CAL' $ non-calibrators only $ timer 0 08 26 15 0 11 18 55 $ 1st-6th galaxy scans $ timer 0 10 53 55 0 13 52 55 $ 6th-11th galaxy scans docalib 1; gainuse 3 $ apply the new CL table flagver 1; outfgver 1 $ keep all flags in FG/1 dparm 0 dparm(3) 1 $ show baselines twice, to treat all antennas identically -- $ this displays baseline 27-1 as well as 1-27 dparm(6)=10 $ time resolution: should be set to the sources' $ integration time, in seconds getn 67 $ *.NEWCH0.1 ***Within TVFLG: ^ Set useful defaults: ^SMOOTH=1 to avoid averaging date before displays ^SCAN= 20 to use a long time for median filters (AMP/PH DIFF) xFLAG ALL CHANNELS ^FLAG STOKES FULL (usually -- sometimes you'll want NORR or NOLL) ***If individual Stokes need to be flagged, make sure you set the STOKES FLAG to correspond to the polarization that is displayed on the TV ^SWITCH SOURCE FLAG to ONE-SOURCE to avoid inadvertantly flagging your galaxy (though sometimes you'll want to of course) ^ Be sure to inspect BOTH polarizations! ***We suggest the following steps: ^ Set the above defaults x Flag first integration in every scan (manual QUACK) -- this should be the first integration AFTER most antennas are on-source, which is why we can't use the usual QUACK. ^ Check AMPLITUDE, AMP DIFF, PHS DIFF. Be wary of known source structure and uv-range limits!! ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). 1st-6th galaxy scans: Flagging 1 straggly timeline (2nd scan) AMPLITUDE RR: (0.000 - 1.825) Looks pretty clean, but a hot spot Flagging RR: 3-17, 09:33:16-> now 0.3-687.2 AMPLITUDE LL: (0.00 - 16.84) At least 2 hot pixels Flagging LL: 20-21, 10:10:26 & 6-21, 10:41:06-> now 0.000-2.087 Flagging LL: 8-21, 08:32:56 & 08:50:56-> 0.1-559.2 AMPL DIFF RR: (0.0 - 502.3) Looks pretty good AMPL DIFF LL: (0.0 - 375.6) Same as above PHAS DIFF RR: (0.0 - 180.0) Pretty random PHAS DIFF LL: (0.0 - 180.0) Pretty random 6 flagging commands needed. 6th-11th galaxy scans: Flagging 1 straggly timeline (7th scan) AMPLITUDE RR: (0.2-687.2) Looks pretty clean AMPLITUDE LL: (0.4-549.9) Looks pretty clean AMPL DIFF RR: (0.0 - 502.3) Looks pretty good AMPL DIFF LL: (0.0 - 375.0) Same as above PHAS DIFF RR: (0.0 - 179.9) Pretty random PHAS DIFF LL: (0.0 - 179.9) Pretty random 1 flagging command needed. x22b. If there's more than one NEWCH0 (FREQID): ***I assume here that the galaxy is in NEWCH0.3 . If not, you should first TACOP FG/2 from NEWCH0.3 to the file with the galaxy in it. This will now be FG/3 . default TVFLG calcode '-CAL' $ non-calibrators only docat -1 $ avoid saving temporary files dohist -1 $ avoid creation of history entries docalib 1 ; gainuse 3 $ apply the new CL table flagver 2;outfgver 2 $ or flagver 3 ; outfgver 3 if you had to TACOP $ the FG table from another file dparm 0 dparm(3) 1 $ show baselines twice, to treat all antennas identically -- $ this displays baseline 27-1 as well as 1-27 dparm(6)=10 $ time resolution: should be set to the sources' $ integration time, in seconds getn 65 $ *.NEWCH0.xx $ This should be the file with the galaxy data ***Within TVFLG: - Set useful defaults: SMOOTH=1 to avoid averaging date before displays SCAN= 20 to use a long time for median filters (AMP/PH DIFF) FLAG ALL CHANNELS FLAG STOKES FULL (usually -- sometimes you'll want NORR or NOLL) ***If individual Stokes need to be flagged, make sure you set the STOKES FLAG to correspond to the polarization that is displayed on the TV SWITCH SOURCE FLAG to ONE-SOURCE to avoid inadvertantly flagging your galaxy (though sometimes you'll want to of course) - Be sure to inspect BOTH polarizations! ***We suggest the following steps: - Set the above defaults - Flag first integration in every scan (manual QUACK) -- this should be the first integration AFTER most antennas are on-source, which is why we can't use the usual QUACK. - Check AMPLITUDE (for missing data), AMP DIFF . PHS DIFF may occasionally be useful, but it's likely to be mostly random, unless you have a strong continuum source near your galaxy. ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). ^23. Calibration/flagging checks: sources ^23a. UVPLT executed on 29jun09 ***Check the amp vs. uv-distance for the galaxy. If there are obvious outliers which are not expected due to source structure or RFI (i.e., not mostly on short spacings), go back and flag those. Note any obvious short-spacing horrors, which may be due to solar or terrestrial RFI. default UVPLT source 'Haro29','' docal 1; gainuse 3 flagver 1 $ set this to the latest FG version -- may be >1 if $ there are multiple NEWCH0s (FREQIDs). do3col 1 dotv 1 getn 67 $ *.NEWCH0.1 $ whichever file holds the galaxy bparm 0 $ amp. vs. uv-distance Looks good- a little scatter Some structure; amplitude is higher at low kL dotv -1; go -> PL version 4 same as grabbed B2UVPLT_23a_AMP.tiff ^23b. IMAGR executed on 29jun09 *** Note: If uvwtfn is set to 'NA' it will override any value given to robust. default IMAGR sources 'Haro29','' $ the galaxy docalib 1; gainuse 3 $ apply latest calibration flagver 1 $ apply latest flags -- set this to the $ highest-numbered FG table outname 'Haro29B2_23b cellsize 1 $ for B configuration $ cellsize 3.5 $ for C configuration $ cellsize 10 $ for D configuration imsize 1024 $ for B configuration $ imsize 512 $ for C and D configurations uvwtfn 'NA'; robust 0.5 niter 1000 nbox 0 minpa 121 dotv 1 getn 67 $ *.NEWCH0.xx $ whichever file has the source you're imaging --> shouldn't see obvious calibration errors or striping. Note that this "channel 0" includes HI emission, so you may see some odd effects (e.g., very woofly noise in B configuration) -- don't panic! ### If you find a strong continuum source rippling your map even in a 512x512 imsize D array configuration channel zero image, then refer to Elias and Dana for further steps. %%% VERY faint & fuzzy, extended galaxy smudge plus at least 8 point sources. ^24. TASAV -> CH0SAV.1,2,3 executed on 29jun09 default TASAV getn 67 $ *.NEWCH0 $ loop over NEWCH0 files (= FREQIDs) outna 'Haro29B2MdTb outcla 'ch0sav' outse inseq outdi 2 $ Ideally set this to a different disk from indisk, $ in case of disk crashes ^25. TABED SN, FG tables to LINCOP executed on 29jun09 ***Use TABED to ensure FREQID=-1 for all tables (paranoia is your friend...) ^25a. NEWCH0.xx FG/yy -> LINCOP FG/2 default TABED inext 'fg' inver 1 $ if single FREQID $ inver 3 $ if multiple FREQIDs: set this to max. flag table number outver 2 opty 'repl' aparm 0 aparm(1) 3 $ Changing column 3 = FREQID keyval= -1,0 $ ...which we change to FREQID= -1 getn 67 $ *.NEWCH0.1 $ if single FREQID $ getn 67 $ *.NEWCH0.3 $ if multiple FREQIDs: set this to file you flagged $ on most recently (usually the file with the $ galaxy in it) getona 66 $ *.LINCOP --> LINCOP FG/2 ^25b. NEWCH0.xx SN/yy -> LINCOP SN/1 default TABED inext 'sn' inver 1 $ if single FREQID $ inver 4 $ if multiple FREQIDs outver 0 opty 'repl' aparm 0 aparm(1) 6 $ Changing column 3 = FREQID keyval= -1,0 $ ...which we change to FREQID= -1 getn 67 $ *.NEWCH0 $ if multiple FREQIDs: all should have same merged SN $ table so you can use whichever NEWCH0 file you want getona 66 $ *.LINCOP --> LINCOP SN/1 ^26. CLCAL LINCOP SN/1 --> CL/3 executed on 29jun09 ***We do CLCAL directly on LINCOP rather than copying, to avoid (even more) confusion in the multiple-FREQID case. ***Note that there is no need to work around any phase jumps, since the intervening data are flagged (see step 17 above [UVFLG]). ^26a. CLCAL for the primary calibrators -> CL/3 default CLCAL sour= '1331+305','' $ Primary (flux) calibrators '0542+498','0137+331', calsour= sour freqid= 1 $ You must run CLCAL once for each FREQID with $ the relevant calibators present interpol 'SELF' dobtween -1 $ Don't interpolate entries for different sources snver 1 gainver 2; gainuse 3 refant 15 $ Change this to your refant getn 66 $ *.LINCOP ^26b. CLCAL for the phase calibrator and galaxy -> CL/3 default CLCAL sour= '1313+549','Haro29','' $ Secondary (phase) calibrator + galaxy calsour= '1313+549','' $ Secondary (phase) calibrator freqid= 1 $ You must run CLCAL once for each FREQID with $ the phase calibrator or galaxy present interpol 'SIMP' cutoff 120 $ Don't extrapolate/interpolate beyond 120 minutes dobtween -1 $ Don't interpolate entries for different sources snver 1 gainver 2; gainuse 3 refant 15 $ Change this to your refant ***If your data set used +/- frequency switching for the phase calibrator (our observations did not, but some archival data may), you should use BPARM with SAMPTYPE='BOX' to select a smoothing time which covers both frequency settings. LISTR/SCAN on LINCOP will help you choose this; normally something like 12 minutes should be OK. bparm 12/60 ; samptype='BOX' getn 66 $ *.LINCOP ^27. Calibration/flagging checks: calibrators ^27a. WIPER executed on 29jun09 ###It shows a plot similar to the UVPLT output just quicker. It is also useful for identifying which antennas or baselines have calibration problems. ***Check the amp & phase vs. uv-distance for all calibrators. Amplitude should match the results of SETJY/GETJY, and phase should be zero, apart from known structure (reflected in source model for gain calibrators and uvrange for phase calibrators). If there are obvious, unexpected outliers, go back and flag those (and possibly re-run various tasks...). default WIPER calcode '*' freqid 1 $ set this to match the calibrator docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets smooth 7, 215 $ boxcar average over all channels -- use $ smooth 7, 215 if you started with 255 channels & 7, 107 if you started with 127 channels bparm 0 imsize 512, 512 $ So it doesn't fill the whole screen! getn 66 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed as B2WIPER_27a_AMP.tiff-> looks pretty clean! Primary: ~15.0 +/- 3.0 Jy (15.0 Jy in catalog) (a little larger scatter, though) Secondary: ~2.5 +/- 2.5 Jy (1.31 Jy in catalog) (but some scatter...) No solar interference evident bparm(2) 2 $ phase vs. uv-distance %%% Probably as expected On Pris: B2WIPER_27a_PHS_Pri.tiff: Good- generally 0 +/- 15 with all scatter within -30 to 30 On all 12 Secs: B2WIPER_27a_PHS_Secs.tiff: full range -180 to 180 (because relatively faint) ^27b. POSSM executed on 29jun09 ***Check vector average of all data for each calibrator. Amplitude should match the results of SETJY/GETJY; phase should be flat, and consistent with zero (corresponding to a point source at the origin)...apart from known source structure and possibly HI absorption. default POSSM source='1313+549','' $ Secondary (phase) calibrator freqid 1 $ set this to match the calibrator uvrange= 0.0,0 $ should be set to eliminate known source structure, $ as in CALIB docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets aparm 0 $ Plot data aparm(1) 1 $ vector average solint 0 $ average all time nplots 0 $ average all baselines dotv 1 getn 66 $ *.LINCOP tvinit %%% Grabbed B2POSSM_27b_RR.tiff & B2POSSM_27b_LL.tiff 1(RR): Roughly 1.32 Jy and fairly flat 1(RR): Very flat at 0 +/- 0.4 degrees 1(LL): Roughly 1.32 Jy and fairly flat 1(LL): Fairly flat at 0 +/- 0.5 degrees ^27c. IMAGR not necessary [if desired -- this is not really necessary] executed on 29jun09 *** Note: If uvwtfn is set to 'NA' it will override any value given to robust. default IMAGR source='1313+549','' $ Secondary (phase) calibrator freqid 1 $ set this to match the calibrator docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets outname 'Haro29B2Sec2 cellsize 1 $ for B configuration $ cellsize 3.5 $ for C configuration $ cellsize 10 $ for D configuration imsize 1024 $ for B array $ imsize 512 $ for C and D array uvwtfn 'NA'; robust 0.5 niter 200 $ reasonable for a point source $ nbox 1; clbox -1,5,512,513 $ calibrator should be in the center minpa 121 dotv -1 $ so you can go eat lunch getn 66 $ *.LINCOP Started 15:22:40 and finished by 15:40 ***You shouldn't see obvious calibration errors or striping. CLEANed flux density should roughly match SETJY/GETJY. If you _do_ have Evil Stuff, UVLSF will likely take care of it, so don't get too worked up. default tvlod; getn 73 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: No real differences (as expected) default tvmovie; ltype 6; getn 73; tvinit; tvmovie Looks pretty constant & clean. ^28. Calibration/flagging checks: sources ^28a.1 WIPER executed on 29jun09 ###It shows a plot similar to the UVPLT output just quicker. It is also useful for identifying which antennas or baselines have calibration problems. If you do find things you want to flag, UVFLG is highly recommended. ***Check the amp vs. uv-distance for the galaxy. If there are obvious outliers which are not expected due to source structure or RFI (i.e., not mostly on short spacings), go back and flag those. Note any obvious short-spacing horrors, which may be due to solar or terrestrial RFI. default WIPER sources 'Haro29','' freqid 1 $ set this to match the galaxy docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets smooth 7, 215 $ boxcar average over all channels -- use $ smooth 7, 215 if you started with 255 channels & 7, 107 if you started with 127 channels bparm 0 imsize 512, 512 $ So it doesn't fill the whole screen! getn 66 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed B2WIPER_28a.tiff: maximum is 36 Jy, with one hot column just short of 20 kL. stokes 'LL'-> max is 6.5 Jy stokes 'RR'; uvrange 17.0 20.0-> between 19.5 & 20.0 timer 0 08 26 10 0 11 19 00 $ 1-6-> max is 36 Jy timer 0 08 26 10 0 09 52 20 $ 1-3-> max is 36 Jy timer 0 08 26 10 0 08 51 20 $ 1st-> max is 5.2 Jy timer 0 08 56 40 0 09 21 50 $ 2nd-> max is 5.1 Jy timer 0 09 27 10 0 09 52 20 $ 3rd-> max is 36 Jy timer 0 09 57 40 0 13 53 00 $ 4-11-> max is 6.0 Jy tget TVFLG; getn 66; timer 0 09 27 10 0 09 52 20; stokes 'RR' uvrange 19 20; flagver 2; outfgver 2 Flagging RR, All channels: 10-17, 09:33:16 tget WIPER; timer 0 0; stokes ''; uvrange 0 0 Now maximum is 8.2 Jy, so looks good. (B2WIPER_28a1.tiff) bparm(2) 2 $ phase vs. uv-distance Range: full -180 to 180 in all columns but a few empty ones ^28a.2 Up to which level most of the values (leaving aside the very hot pixels) comfortably fit in? Answer= 8 Jy (Could possibly clip a FEW high values...) ###This is the value that you will be using in CLIP when combining your data!!! ^28x. POSSM [Eliminated from the recipe] executed on 29jun09 anyways ***Check vector average of all data for the galaxy. You should see your HI line! default POSSM source='Haro29','' $ your galaxy freqid 1 $ set this to match the calibrator docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets aparm 0 $ Plot data aparm(1) 1 $ vector average solint 0 $ average all time nplots 0 $ average all baselines dotv 1 getn 66 $ *.LINCOP tvinit %%% Results: Barely there! 1 RR: phs: 180 +/- 180 pretty much everywhere amp: about 3 mJy on ends, but peaks ~9 mJy B2POSSM_28_RR.tiff 1 LL: phs: 0 +/- 150 on ends, except for ~90-110 where it's ~0 +/- 30 amp: about 3 mJy on ends, but peaks ~9 mJy B2POSSM_28_LL.tiff ^28b. IMAGR executed on 29jun09 default IMAGR sources 'Haro29', '' freqid 1 $ set this to match the calibrator docal 1; gainuse 3 flagver 2 $ should be the latest FG table doband 1; bpver 1 $ for single-FREQID data sets $ doband 3; bpver 4 $ for multiple-FREQID data sets outname 'Haro29B2gal cellsize 1 $ for B configuration $ cellsize 3.5 $ for C configuration $ cellsize 10 $ for D configuration imsize 1024 $ for B configuration $ imsize 512 $ for C configuration $ imsize 256 $ for D configuration uvwtfn 'NA'; robust 0.5 niter 1000 $ a light clean, just to see what we've got. niter 0 $ would be ok too, esp. if you IMLIN afterwards nbox 0; clbox 0 minpa 121 dotv -1 $ so you can go eat lunch getn 66 $ *.LINCOP Started 16:13:30, and finished ~17:00 ***You shouldn't see obvious calibration errors or striping. You should however see of order 100 mJy of continuum sources in the field, as well as some indication of your galaxy. The latter may be quite confusing for B configuration, which resolves out most of the structure. Don't fret until you've combined all the array configurations. ***Note: If uvwtfn is set to 'NA' it will override any value given to robust. ###If you find a strong continuum source rippling your map even after trying a 512x512 imsize D array configuration cube than refer to Elias and Dana for further steps. default tvlod; getn 75 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: The faint galaxy blob moved. default tvmovie; ltype 6; getn 75; tvinit; tvmovie The galaxy is barely there, and it is rotating (channels ~80-130). There appears to be only 1 continuum source. ?28c. Noise Estimations: calculated on 29jun09-30jun09 ##The easiest way to calculate the expected sensitivity is to say 7 S(mJy) = ---------------------------- sqrt{ N (N-1) delta_nu t} where 7 is a constant that depends on the system temperature of the receivers(a quite conservative value) N = number of antennas in the array, delta_nu = channel resolution in MHz, and t = integration time in hours. You need to use for N the number of Antennas which have on average been giving good data during the run. The total time should be the actual time spent on source. No need to be super precise, of course. One simply wants to get a ballpark figure which is good to 10-20%. ###Note that for data which are Hanning smoothed (archive data) the channel spacing is equal to the resolution delta_nu. Without Hanning smoothing, the resolution is ~1.4 x delta_nu (note that after offline Hanning smoothing, if you preserve all channels, the resolution becomes 2 x delta_nu; it reverts to a new "double the old delta_nu" if you delete every other channel). ####Finally, if you want to know the noise in a single visibility, use N=2 and t = 1/360, and probably multiply by sqrt{2} because a visibility is a single polarisation as well. The Expected noise level is: 1.4 mJy x expected rms = K/SQRT[N(N-1)(N_IF*T_int*Delta_nu_M)] in mJy ^ expected rms = 1.4 mJy (here) where: K = 8.0 (for L band) N = # of Antennas (25 here) N_IF = 2 (for 2 polarizations) T_int = total on-source integration time in HOURS (4.531 hrs here = 271:50 mins) Delta_nu_M = effective continuum bandwidth or spectral-line channel in MHz (FREQ Coord incr in the header, but that number is in Hz) = 6.1035156e-03 (at least normally- check it) x measured rms: use TVSTAT (or IMSTAT) to measure the noise in a non-signal area ^ measured rms = 1.4 mJy x continuum channels are a good place, or just a clear off-galaxy area x can isolate main galaxy & continuum source area (TVWIN after TVLOD) & then use IMSTAT on outside area ^ TVWIN: blc = 198 617; trc = 212 632 default IMSTAT getn 75 $ Haro29B2gal movie blc 198 617 10 $ 10th channel, bottom left corner of box containing primary sources in the image trc 212 632 10 $ 10th channel, top right corner of box doinvers 1 $ full image except for box defined by blc & trc (afterwards, set doinvers -1) The rms Noise level in a line free channel is: 1.4 mJy ^29. TASAV -> EndTaB.LINSAV.1 executed on 30jun09 default TASAV outna 'Haro29B2EdTb outcla 'linsav' outdi 2 $ Ideally set this to a different disk from indisk, $ in case of disk crashes getn 66 $ *.LINCOP ^30. FITTP executed on 30jun09 dataout '/Users/herrmann/Desktop/B2-BeginTasav.FITS create: ^Haro29_B2_UV_CALIB_NEWCH0.FITS $ one per FREQID ^Haro29_B2_UV_CALIB_LINCOP.FITS ^Haro29_B2-BeginTasav.FITS ^Haro29_B2-MidTasav.FITS $ one per FREQID ^Haro29_B2-EndTasav.FITS ^Add the end date to the start of this file! ^PRTMSG & CLRMSG ^31. Send to DEIDRE 30jun09 See Little THINGS Web site for current instructions. Apart from the FITS data from step 30/FITTP (in calib), the following should be archived (via ftp): * Observing log (in obs) * This data reduction log (in notes) * LISTR/SCAN output (if saved to a file- works well if you just insert it into this log, though) E-mail to Deidre: (See example e-mail below.) * This data reduction log * Any notes about the data set * The names of the .FITS files being ftped * Total time on source (in minutes and also in hours (decimal)) * Expected rms and measured rms 32. Celebrate your victory with an appropriate beverage! ================================================================================ ================================================================================ Ater the data has been checked by an independent member of the team and changes/corrections have been suggested the log should continue here with the steps that have been reiterated and the values used in the reiteration. If you need to recreate tables it is best at this stage to not delete the already existing ones but rather to give the tables higher version numbers. Haro29 B2 (X) calibration Hi Deidre, The Haro29 B2 array (X) data is ready to be ftped, but I'll do the actual ftping once the NRAO system is all set up. Attached is the data reduction log/filled-in-recipe file. Here is the rest of the information that you requested: Several notes about the data: 2nd Pri doesn't seem to be there at all... But there's a lot of 1st Pri (basically 2 sections) 10: Had to flag large amount of 1st Pri (1st section) in Ants 12 & 27 b/c it was very faint 14: CALIB failed on 4 solutions (must be Ant 12 & 27 FULL) (but BPASS of Ants 12 & 27 look fine) 16, 19, 20: No 1st Pri shown for Ants 12 & 27 Tried 12 & 13 (new NEWCH0) and then CALIB again with refant 12 then 6-> same results Didn't want to lose ALL of Ant 12 & 27 data... (Why do both look calibrated properly then?) Go back to start- new LINCOP & NEWCH0 but flag all the first section of the first Pri (Megan's suggestion)-> now CALIB works! The galaxy is barely there, and it is rotating (channels ~80-130). There appears to be only 1 continuum source. The notes above might be a bit cryptic, so let me elaborate a bit. There were 14 minutes of the "before" primary and supposedly 3:50 of the "after" primary, but all the "after" primary was so straggly that there really wasn't anything useful there (and so I had to flag it all). The "before" primary was split into two pieces- with an empty timeline between them. In Ants 12 & 27, the first section of the "before" primary was so faint that it needed to be flagged, leaving the second section of the "before" primary as the only primary to calibrate those two antennas. After only flagging that first section of the "before" primary on those two antennas, all the bandpasses looked fine. However, at step 14, CALIB failed on 4 solutions, which I figured couldn't be good, but I continued along to see the consequences. At steps 16, 19, and finally 20 I noticed that nothing was showing up for the "before" primary in Ants 12 & 27. (Oddly enough, though, the secondaries in Ants 12 & 27 looked beautifully calibrated, even without a primary at all in those two antennas...) I then tracked down the problem to the 4 failed solutions (RR & LL in 12 & 27) from CALIB. I guess AIPS must have flagged the section of primary in Ants 12 & 27 when the solutions failed. At that point, I tried redoing steps 12-14 with different reference antennas (12 & 6) but got the same 4 failed solutions. Megan suggested that I flag the first section of the "before" primary in ALL of the antennas (rather than leaving all the primary in most of the antennas), so I did that by going back to the beginning and creating new LINCOP and NEWCH0 sets. When I got to CALIB, there were no failed solutions! So I continued with those versions and the results through step 21 were almost exactly the same as when AIPS got rid of all of the primaries in Ants 12 & 27, which I find to be rather puzzling! At least I didn't need to lose all of the Ant 12 & 27 data, though, thanks to Megan's suggestion. Total Time on Source = 271:50 mins (4.531 hrs) (Only 2 10s scans were lost due to flagging straggly time scans.) The expected rms is 1.4 (?) mJy and the measured rms is 1.4 mJy, so 1.4 (?) [1.4]. The measured value is basically the same as the expected value, which is perhaps a little odd since 12 out of 25 antennas were EVLA. (Only Antennas 4 [EVLA testing], 5, 14 [L-301 module will not lock], and 29 were lost. Again, there were no explanations in the log for antennas 5 and 29 being lost, but I still don't think Ant 29 has even been used.) N = 25 antennas, Tint = 4.531 hrs, delta_nu_M = 6.1035156e-3 MHz, N_IF = 2, K = 8.0 (for L band) The uv data files that I will eventually ftp to the NRAO site are: Haro29_B2_UV_CALIB_NEWCH0.FITS Haro29_B2_UV_CALIB_LINCOP.FITS Haro29_B2-BeginTasav.FITS Haro29_B2-MidTasav.FITS Haro29_B2-EndTasav.FITS In addition, I will create a figuresB2 subdirectory (in the calib directory) as usual and will upload all the .tiff and .ps files mentioned in the data reduction log. I'll also put the data reduction log and 3 log files from the AIPS_MSGSRV window in the notes directory. Lastly, since the observation log probably is already in the obs directory as an html file, I probably won't need to do anything there. I think that's it! Now Haro29 is calibrated so next I'll start on Haro36. Kim =)