NOTES: 8th Sec in Ant 16 out completely- will need to flag 7th & 8th galaxy scans FULL in Ant 16 Ant 21 looks fine even though there's a warning about it in the log C1POSSM_27b_RR.tiff: Definite slope from ~4.43 to 4.38 Jy, but that's only a ~1.6% effect, so not really a problem Good rotation (channels ~59-145) and there's at least 1 continuum source in the FOV, but not very close to the galaxy. LITTLE THINGS AIPS Reduction of Haro36, C1 (AN) config.: VLA Obs. of 24mar08 ===================================================================== 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 28jul09-29jul09 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 C1 configuration (AN) From observing log (available online as an html file at http://www.lowell.edu/users/dah/littleteam/haro36/vla/obs/logs_AH927_AN.html): Observing: 24Mar08 04:03:59-10:02:10 (23Mar08 21:03:59 - 24Mar08 03:02:10 local time) * Wind/API rms phase/clouds: 24Mar 04:03:20 NE at 2.5 m/s 3.0 API Sky clear. 24Mar 04:59:46 N at 0.7 m/s 0.8 API Sky clear. 24Mar 06:59:57 NW at 1.5 m/s 1.2 API Sky clear. 24Mar 08:59:09 SE at 0.2 m/s 1.4 API Sky clear. * ant. 7, 15, 25, 26, 27 (recently updated baseline parameters) * ant. 2, 4 (do not have good baseline positions because recently moved) * EVLA antennas: 1, 4, 11, 13, 14, 16, 17, 18, 19, 21, 23, 24, 25, 26 (14 antennas) * ant. 5 LOST (EVLA: EVLA testing) (whole time) * ant. 6 LOST (SERVO: Antenna is stuck at its azimuth limit.) (whole time) * ant. 4 LOST (SERVO: ACU Circuit Breaker & AZ motor #1 fault. Antenna is stowed & e-stopped.) (whole time) * ant. 21 Unknown effect (FRONT END: IF A fringe amplitudes are about 50% of normal at L band.) (whole time) ^1. FILLM executed on 28jul09 ^a. Request archive data: requested AH927_AN_1 and saved temporarily as /Users/herrmann/Desktop/AH927_C_AN_1 ^b. FILLM -> Haro36-C1.CH 0.1, Haro36-C1.LINE.1 (1 & 2) default FILLM datain '/Users/herrmann/Desktop/AH927_C_AN_ nfiles 0 $ don't skip any files band 'L' qual 1 $ restricts FILLM to the galaxy+calibrators of interest (qual 1 only here) vlaobs 'AH927' timerang 0 0 $ No other scans before or after Haro36 outna 'Haro36-C1 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_C_AN_1 tortue> FILLM1: tortue> FILLM1: *** ATTENTION - default: loading subarray 1 *** tortue> FILLM1: tortue> FILLM1: tape file # 1, start date/time = 20080324/04:04:00 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 24 antennas. tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Program = AH927 ; Tape revision number = 33. tortue> FILLM1: Create Haro36-C1 .CH 0 . 1 (UV) on disk 1 cno 1 tortue> FILLM1: Ref. date = 20080324 A-C = 1.417999 B-D = 1.417999 GHz tortue> FILLM1: Create Haro36-C1 .LINE . 1 (UV) on disk 1 cno 2 tortue> FILLM1: Ref. date = 20080324 A-C = 1.417999 B-D = 1.417999 GHz tortue> FILLM1: FLMFQ: FQ entry tolerance = 1.608D+02 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 04:03:55.0 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 24 antennas. tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Ref. date = 20080324 A-C = 1.417999 B-D = 1.417999 GHz tortue> FILLM1: Appending new data to: Haro36-C1 .CH 0 . 1 disk 1 tortue> FILLM1: Ref. date = 20080324 A-C = 1.417999 B-D = 1.417999 GHz tortue> FILLM1: Appending new data to: Haro36-C1 .LINE . 1 disk 1 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 04:04:05.0 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 04:08:55.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 04:15:05.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 04:20:05.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 04:45:55.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 04:50:45.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 05:16:35.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 05:21:35.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 05:47:25.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 05:52:25.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 06:15:35.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 06:20:35.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 06:43:35.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 06:48:35.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 07:11:35.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 07:16:35.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 07:42:25.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 07:47:25.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 08:13:15.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 08:18:15.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 08:44:15.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 08:49:25.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 09:15:25.0 tortue> FILLM1: Found HARO36 : 1 1.562 MHz at IAT 0/ 09:20:25.0 tortue> FILLM1: Found 1400+621 : 1 1.562 MHz at IAT 0/ 09:46:35.0 tortue> FILLM1: Found 1331+305 : 1 1.562 MHz at IAT 0/ 09:56:55.0 tortue> FILLM1: Read 538096 visibilities from 1 files tortue> FILLM1: Appears to have ended successfully ^2. TASAV -> LINSAV.1 executed on 28jul09 ***We TASAV right away, because VLANT changes the AN table. Did I mention we're paranoid? default TASAV outna 'Haro36C1BgTb 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 28jul09 ***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 (34) unless otherwise specified. ^4. LISTR/SCAN --> Haro36-C1.listr ***We do this before VLANT because we need to know FREQIDs for VLANT default LISTR optype 'SCAN' docrt -1 outpr '/Users/herrmann/Desktop/Haro36-C1.listr getn 34 $ *.LINCOP --> *.listr tortue LISTR(31DEC08) 4 28-JUL-2009 14:26:23 Page 1 File = Haro36-C1 .LINCOP. 1 Vol = 1 Userid = 4 Freq = 1.417999480 GHz Ncor = 2 No. vis = 538096 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0001 A 1 0/04:07:35 - 0/04:13:55 1 1 9632 2 1400+621 : 0001 C 1 0/04:15:05 - 0/04:19:15 1 9633 16547 3 HARO36 : 0001 1 0/04:20:05 - 0/04:45:05 1 16548 57924 4 1400+621 : 0001 C 1 0/04:45:55 - 0/04:49:55 1 57925 64755 5 HARO36 : 0001 1 0/04:50:45 - 0/05:15:45 1 64756 105603 6 1400+621 : 0001 C 1 0/05:16:35 - 0/05:20:45 1 105604 112756 7 HARO36 : 0001 1 0/05:21:35 - 0/05:46:35 1 112757 153936 8 1400+621 : 0001 C 1 0/05:47:25 - 0/05:51:35 1 153937 160805 9 HARO36 : 0001 1 0/05:52:25 - 0/06:14:35 1 160806 197431 10 1400+621 : 0001 C 1 0/06:15:35 - 0/06:19:35 1 197432 204331 11 HARO36 : 0001 1 0/06:20:35 - 0/06:42:35 1 204332 240763 12 1400+621 : 0001 C 1 0/06:43:35 - 0/06:47:35 1 240764 247663 13 HARO36 : 0001 1 0/06:48:35 - 0/07:10:35 1 247664 284210 14 1400+621 : 0001 C 1 0/07:11:35 - 0/07:15:35 1 284211 291110 15 HARO36 : 0001 1 0/07:16:35 - 0/07:41:35 1 291111 332510 16 1400+621 : 0001 C 1 0/07:42:25 - 0/07:46:35 1 332511 338850 17 HARO36 : 0001 1 0/07:47:25 - 0/08:12:25 1 338851 378590 18 1400+621 : 0001 C 1 0/08:13:15 - 0/08:17:25 1 378591 385743 19 HARO36 : 0001 1 0/08:18:15 - 0/08:43:15 1 385744 426889 20 1400+621 : 0001 C 1 0/08:44:15 - 0/08:48:25 1 426890 433674 21 HARO36 : 0001 1 0/08:49:25 - 0/09:14:25 1 433675 475327 22 1400+621 : 0001 C 1 0/09:15:25 - 0/09:19:25 1 475328 482104 23 HARO36 : 0001 1 0/09:20:25 - 0/09:45:35 1 482105 523503 24 1400+621 : 0001 C 1 0/09:46:35 - 0/09:50:35 1 523504 530380 25 1331+305 : 0001 A 1 0/09:56:55 - 0/10:02:05 1 530381 538096 tortue LISTR(31DEC08) 4 28-JUL-2009 14:26:23 Page 2 File = Haro36-C1 .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 17348 2 1400+621 : 0001 C 14:00:28.6526 62:10:38.526 0.000 0.000 0.000 0.000 82400 3 HARO36 : 0001 12:46:56.4000 51:36:47.000 0.000 0.000 0.000 0.000 438348 ID Source Freq(GHz) Velocity(Km/s) Rest freq (GHz) 1 All Sources 1.4180 0.0000 0.0000 Frequency Table summary FQID IF# Freq(GHz) BW(kHz) Ch.Sep(kHz) Sideband 1 1 1.41799948 1312.2560 6.1035 1 Primary: 6:30, 5:20-> 11:50 Secondary: 4:20, 4:10, 4:20, 4:20, 4:10, 4:10, 4:10, 4:20, 4:20, 4:20, 4:10, 4:10 -> 51:00 Galaxy: 25:10, 25:10, 25:10, 22:20, 22:10, 22:10, 25:10, 25:10, 25:10, 25:10, 25:20 -> 268:10 total However, subtract 10s out of 2 scans-> so 4.464 hrs here = 267:50 mins ^5. VLANT -> AN/1, CL/2 executed on 28jul09 ***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 34 $ *.LINCOP tortue> VLANT1: WARNING: 1 ANTENNAS MAY STILL GET MORE CORRECTION tortue> VLANT1: Copied CL file from vol/cno/vers 1 34 1 to 1 34 2 tortue> VLANT1: CL version input 1 output 2 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(16) = 'W6 ' tortue> VLANT1: VLANT XCOR(16) = 0.0013 tortue> VLANT1: VLANT YCOR(16) = 0.0008 tortue> VLANT1: VLANT ZCOR(16) = 0.0002 tortue> VLANT1: Appears to have ended successfully %%% Probably the warning is about antenna 2, 4, 5, 6, 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 34 $ *.LINCOP getona 34 $ *.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 34 $ *.LINCOP Location Of VLA Antennas N18 ( 7) N16 (13)* N14 (27) N12 (18)* N8 ( 9) N6 (26)* N4 (12) N2 (25)* N1 (15) (22) W2 E2 (21)* *(19) W4 ( ) *(16) W6 E6 (28) ( ) E8 (10) *( 1) W10 E10 (11)* *(24) W12 E12 (20) *(17) W14 E14 ( 3) ( 8) W16 E16 (14)* ( ) E18 (23)* VLA:_OUT ( 2) VLA:_OUT ( 4) VLA:_OUT ( 5) VLA:_OUT ( 6) 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: 22 $ W2 ^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= 3C147 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 CnB) 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 C1950 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: 1400+621 1400+621 J2000 C 14h00m28.6526s 62d10'38.526" 1358+624 B1950 C 13h58m58.3600s 62d25'06.700" ----------------------------------------------------- BAND A B C D FLUX(Jy) UVMIN(kL) UVMAX(kL) ===================================================== 20cm L P P P P 4.40 6cm C P P P P 1.72 3.7cm X S P P P 1.08 400 2cm U X S S S 0.67 400 1.3cm K X X S S 0.48 400 0.7cm Q X X W W 0.28 400 ===> secondary cal --- No UVMax restriction %%% Don't need to worry about restrictions because D array max is 4.9 kL ^7b. SETJY -> SU/1 executed on 28jul09 ***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 34 $ *.LINCOP ; --> / 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 =14.7381 (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 34 $ *.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 34 $ *.LINCOP ; ^7c. CALRD executed on 28jul09 ***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)=807 $ Pick a baseline -- here, baseline 8-7 (large and both are VLA) docrt 132 getn 34 $ *.LINCOP --> calib: 10s (both) source: 10s ^9. UVFLG -> FG/1 executed on 28jul09 ***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 28jul09 ***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 2, 4, 5, 6, 29 out completely (as in PRTAN) %%% 8th Sec in Ant 16 out completely- will need to flag 7th & 8th galaxy scans FULL in Ant 16 %%% EVLA-EVLA baselines flagged properly %%% RR: 0.253 - 6.255 (Pretty good, except first few timelines abnormally bright) %%% LL: 0.294 - 6.867 (Same as above) Trimmed first 7 timelines from 1st Pri-> 2.708 & 3.029 Trimmed straggly timelines from Secs: 1st, 4th, 8th, 9th, 10th, 11th, 12th Trimmed 4 straggly timelines from 2nd Pri Final: RR: (0.253 - 2.708), LL: (0.294 - 3.029) ^AMP DIFF to check for variable gains %%% RR: 0.00 - 92.65 (Pretty clean- a few bright spots in Pris) %%% LL: 0.0 - 129.4 (same as above, but spots brighter) Clipping interactively separately to 75 -> now 74.76 & 77.67 Final: RR: (0.00 - 74.76), LL: (0.00 - 77.67) ^PHS DIFF to check for variable atmosphere/gains %%% RR: 0.00 - 11.76 (Looks okay- all nastiness in 1st Pri in Ant 3) %%% LL: 0.00 - 8.668 (same as above) Final: RR: (0.00 - 11.76), LL: (0.00 - 8.668) %%% Saved as Figures/C1TVFLG_10_(AMP/AMPDIFF/PHSDIFF)_(RR/LL).tiff using Grab ^ 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 %%% Total of 128 flagging commands (b/c of interactive clipping) ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). ^10b. TABED FG/1 executed on 28jul09 ***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 34 $ *.LINCOP --> LINCOP FG/1 ^10c. (EXTRA) WIPER on Calibrators in LINCOP executed on 28jul09 (Just to see if there are any hot pixels) default WIPER $ sources '1331+305','' $ Primary $ sources '1400+621','' $ 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 34 $ *.LINCOP %%% no hot columns, and no hot spots- max is ~4.4 Jy (C1WIPER_10c.tiff) ^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 on 28jul09 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 22 $ 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 34 $ *.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 22 $ 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 34 $ *.LINCOP --> BP/1 x11b2. BPASS FREQID 2 -> BP/2 not necessary ***Same as 11C1, 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 22 $ 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 34 $ *.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 34 $ *.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 34 $ *.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 34 $ *.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 34 $ *.LINCOP getona 34 $ *.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 34 $ *.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 34 $ *.LINCOP tvinit dotv -1; go %%% PL 1-12 for LINCOP are POSSM results, 9 per page There are two plots for each antenna (RR & LL) for the before & after primary calibrator 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 34 $ *.LINCOP outfile '/Users/herrmann/Desktop/C1POSSMplots11c1.ps invers 0 for i = 1 to 12; plver = i; go; wait lwpla; end ^11c2. Apply BP table to 2ndary calibrator & plot individual baselines default POSSM source='1400+621','' $ 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 34 $ *.LINCOP tvinit %%% Everything looks normal (looked at one whole time) ^11c3. Apply BP table to 2ndary calibrator & vector average all data default POSSM source='1400+621','' $ 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 34 $ *.LINCOP 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 24.5 mJy for all channels 1(RR): phase is generally -105 +/- 5 degrees, but a bit higher at beginning 1(LL): Relatively flat around 14.5 mJy for all channels 1(LL): phase is generally 124 +/- 6 degrees dotv -1; go tget lwpla for i = 13 to 14; plver = i; go; wait lwpla; end %%% (Added to C1POSSMplots11c1.ps) ^12. AVSPC -> NEWCH0.1 (2,3) executed on 28jul09 ***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 34 $ *.LINCOP 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 (35) 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 34 $ *.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 34 $ *.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 35 $ *.NEWCH0 outprint '/Users/herrmann/Desktop/Haro36-C1_12d.listr tortue LISTR(31DEC08) 4 28-JUL-2009 15:32:04 Page 1 File = Haro36-C1 .NEWCH0. 1 Vol = 1 Userid = 4 Freq = 1.417999480 GHz Ncor = 2 No. vis = 538096 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0001 A 1 0/04:07:35 - 0/04:13:55 1 1 9632 2 1400+621 : 0001 C 1 0/04:15:05 - 0/04:19:15 1 9633 16547 3 HARO36 : 0001 1 0/04:20:05 - 0/04:45:05 1 16548 57924 4 1400+621 : 0001 C 1 0/04:45:55 - 0/04:49:55 1 57925 64755 5 HARO36 : 0001 1 0/04:50:45 - 0/05:15:45 1 64756 105603 6 1400+621 : 0001 C 1 0/05:16:35 - 0/05:20:45 1 105604 112756 7 HARO36 : 0001 1 0/05:21:35 - 0/05:46:35 1 112757 153936 8 1400+621 : 0001 C 1 0/05:47:25 - 0/05:51:35 1 153937 160805 9 HARO36 : 0001 1 0/05:52:25 - 0/06:14:35 1 160806 197431 10 1400+621 : 0001 C 1 0/06:15:35 - 0/06:19:35 1 197432 204331 11 HARO36 : 0001 1 0/06:20:35 - 0/06:42:35 1 204332 240763 12 1400+621 : 0001 C 1 0/06:43:35 - 0/06:47:35 1 240764 247663 13 HARO36 : 0001 1 0/06:48:35 - 0/07:10:35 1 247664 284210 14 1400+621 : 0001 C 1 0/07:11:35 - 0/07:15:35 1 284211 291110 15 HARO36 : 0001 1 0/07:16:35 - 0/07:41:35 1 291111 332510 16 1400+621 : 0001 C 1 0/07:42:25 - 0/07:46:35 1 332511 338850 17 HARO36 : 0001 1 0/07:47:25 - 0/08:12:25 1 338851 378590 18 1400+621 : 0001 C 1 0/08:13:15 - 0/08:17:25 1 378591 385743 19 HARO36 : 0001 1 0/08:18:15 - 0/08:43:15 1 385744 426889 20 1400+621 : 0001 C 1 0/08:44:15 - 0/08:48:25 1 426890 433674 21 HARO36 : 0001 1 0/08:49:25 - 0/09:14:25 1 433675 475327 22 1400+621 : 0001 C 1 0/09:15:25 - 0/09:19:25 1 475328 482104 23 HARO36 : 0001 1 0/09:20:25 - 0/09:45:35 1 482105 523503 24 1400+621 : 0001 C 1 0/09:46:35 - 0/09:50:35 1 523504 530380 25 1331+305 : 0001 A 1 0/09:56:55 - 0/10:02:05 1 530381 538096 tortue LISTR(31DEC08) 4 28-JUL-2009 15:32:04 Page 2 File = Haro36-C1 .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 14.738 0.000 0.000 0.000 17348 2 1400+621 : 0001 C 14:00:28.6526 62:10:38.526 0.000 0.000 0.000 0.000 82400 3 HARO36 : 0001 12:46:56.4000 51:36:47.000 0.000 0.000 0.000 0.000 438348 ID Source Freq(GHz) Velocity(Km/s) Rest freq (GHz) 1 1331+305 1.4180 -138.1365 0.0000 2 1400+621 1.4180 0.0000 0.0000 3 HARO36 1.4180 0.0000 0.0000 Frequency Table summary FQID IF# Freq(GHz) BW(kHz) Ch.Sep(kHz) Sideband 1 1 1.41799948 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 34 $ *.LINCOP getona 35 $ *.NEWCH0.1 --> 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 34 $ *.LINCOP getona 35 $ *.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 34 $ *.LINCOP getona 35 $ *.NEWCH0.3 --> NEWCH0.3, FG/1 ^14. CALIB -> NEWCH0.1(,2,3) SN/1 executed on 28jul09 (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 22 $ 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 35 $ *.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 3.123E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 3.069E+00 tortue> CALIB1: Found 96 good solutions tortue> CALIB1: Average closure rms = 0.0009 +- 0.0002 tortue> CALIB1: No data were found > 99.0 rms from solution %%% 24 antennas, before & after pri's-> 24 * 2(RR&LL) * 2(bef&aft) - 0(RR&LL)*0 missing = 96 $ This time there is no second primary default CALIB get2n 210 $ 3C147_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 22 $ 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 35 $ *.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 1400+621: no restrictions, no solar interference, so uvra= 0.0,0 default CALIB calsour '1400+621','' $ 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 22 $ 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 35 $ *.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 1.488E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 1.462E+00 tortue> CALIB1: Found 574 good solutions tortue> CALIB1: Average closure rms = 0.0092 +- 0.0005 tortue> CALIB1: No data were found > 99.0 rms from solution %%% 24 antennas, 1 Sec missing-> 24 * 2(RR&LL) * 12(# of Secs) - 2 missing() = 574 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 35 $ *.NEWCH0.2 getona 35 $ *.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 35 $ *.NEWCH0.3 getona 35 $ *.NEWCH0.1 --> NEWCH0.1, SN/3 ^15b. GETJY SN/1-3, SU/1 executed on 28jul09 ***Find flux density of secondary calibrator, and set SN table amplitude gains to reflect a common flux density scale. default GETJY sources '1400+621','' $ Secondary (phase) calibrators) calsour '1331+305','' $ Primary (flux) calibrators '0542+498','0137+331', freqid -1 snver 0 $ Use all SN tables getn 35 $ *.NEWCH0.1 tortue> GETJY1: Task GETJY (release of 31DEC08) begins tortue> GETJY1: Source:Qual CALCODE IF Flux (Jy) tortue> GETJY1: 1400+621 : 1 C 1 4.40081 +/- 0.01498 %%% (Very close to expected 4.40 Jy.) 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 22 $ Change this to your refant getn 35 $ *.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 35 $ *.NEWCH0.1 getona 35 $ *.NEWCH0.2 getona 35 $ *.NEWCH0.3 ^16. SN table checks ^16a. SNPLT last SN table executed on 28jul09 ^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 35 $ *.NEWCH0.1 tvinit ===> 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, then second primary In general, few jumps (1-28) (besides the jump from primary to secondary which is ok) EXCEPT: 8th Sec in Ant 16 missing (as expected from TVFLG) (Note: Ref antenna 22 red triangles at values of 0 because everything relative to it.) %%% Grabbed each frame: C1SNPLT_16a1_PHS(a-c).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 35 $ *.NEWCH0.1 ===> 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) EXCEPT: 8th Sec in Ant 16 missing (as expected from TVFLG) A bit of a jump in 2nd Sec in 14RR %%% Grabbed each frame: C1SNPLT_16a2_AMP(a-c).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 28jul09 default LISTR optype 'gain'; inext 'sn'; inver 1; freqid -1 antennas -2,4,5,6,29,0; $ 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/Haro36-C1_16b.listr getn 35 $ *.NEWCH0.1 --> 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 28-JUL-2009 16:03:58 Page 1 File = Haro36-C1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.417999480 GHz Ncor= 2 No. vis= 538096 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 = 1.417999480 GHz Time Source -1- -3- -7- -8- -9--10-*11*-12--13-!14!-15--16-*17**18*-19--20--21--22--23-*24*-25-*26*-27--28- max % diff 1.6 0.6 0.8 0.7 0.7 0.6 5.1 0.6 0.7 11. 0.5 4.3 9.4 7.8 4.2 0.7 3.8 0.3 4.7 5.5 4.9 6.8 0.6 0.6 Day # 0 04:11:25 1331+305 215 255 311 285 236 308 262 272 353 367 303 362 289 423 341 293 375 265 357 314 448 331 247 291 04:17:15 1400+621 215 258 315 287 238 310 261 275 354 369 305 360 284 427 339 294 370 266 353 312 448 336 248 296 04:47:55 1400+621 213 258 313 288 239 310 259 278 355 408 305 357 294 436 338 294 359 267 378 313 473 345 247 296 05:18:40 1400+621 213 259 313 287 238 309 259 278 351 366 306 357 292 445 338 294 352 266 375 313 456 342 248 293 05:49:35 1400+621 213 257 315 289 240 312 258 278 352 365 305 353 289 444 333 293 355 266 373 310 452 343 249 295 06:17:35 1400+621 209 258 316 286 237 310 257 275 354 364 303 338 258 417 339 293 356 267 347 289 439 328 250 294 06:45:35 1400+621 211 257 314 289 240 310 258 276 354 362 304 335 254 419 336 293 359 266 346 304 455 326 250 294 07:13:35 1400+621 209 256 317 288 239 310 256 277 351 360 306 353 291 421 335 292 356 266 345 299 443 343 250 294 07:44:35 1400+621 211 256 314 288 238 309 246 278 352 363 304 261 393 325 291 354 266 349 302 436 319 249 296 08:15:25 1400+621 212 257 315 287 238 310 265 277 352 361 305 349 282 431 350 294 353 267 369 304 447 358 247 296 08:46:25 1400+621 214 257 314 289 238 310 265 275 352 360 303 351 280 427 345 293 355 266 366 307 454 353 248 294 09:17:30 1400+621 215 258 313 288 238 309 264 277 354 360 304 348 289 429 346 291 352 266 366 309 454 358 248 294 09:48:40 1400+621 214 259 314 289 238 311 263 276 351 358 304 351 290 425 347 294 355 266 367 309 452 356 247 294 09:59:55 1331+305 212 254 311 285 236 307 265 273 352 355 302 351 293 437 348 289 352 263 365 307 452 339 245 291 tortue LISTR(31DEC08) 4 28-JUL-2009 16:03:58 Page 2 File = Haro36-C1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.417999480 GHz Ncor= 2 No. vis= 538096 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 = 1.417999480 GHz Time Source -1- -3- -7- -8- -9--10--11--12--13--14--15--16-*17*-18--19--20--21--22--23--24--25--26--27--28- max % diff 0.7 1.1 0.6 0.7 1.2 0.5 1.4 0.7 0.5 1.1 0.6 3.9 6.7 2.2 2.2 1.0 1.7 0.4 2.1 2.9 1.7 2.4 0.7 0.8 Day # 0 04:11:25 1331+305 257 301 308 240 212 291 328 252 323 357 261 389 258 399 347 299 376 247 360 367 389 315 243 283 04:17:15 1400+621 264 302 310 240 212 292 329 252 328 350 261 386 254 399 348 300 374 247 359 364 392 316 243 285 04:47:55 1400+621 262 301 309 240 213 291 326 253 327 356 262 384 262 397 360 300 375 247 356 362 388 315 242 284 05:18:40 1400+621 262 303 307 241 213 290 325 253 328 356 262 385 261 406 359 298 371 247 354 362 395 313 243 285 05:49:35 1400+621 263 299 308 241 215 292 325 253 326 353 261 381 258 405 357 296 371 247 353 359 396 314 244 285 06:17:35 1400+621 261 300 308 239 211 291 325 251 329 353 259 368 240 396 362 299 374 247 352 355 389 314 243 283 06:45:35 1400+621 263 299 307 242 214 290 324 251 328 350 260 364 236 398 359 299 375 247 351 361 387 310 244 284 07:13:35 1400+621 262 297 309 240 213 290 322 251 326 352 261 368 242 401 355 297 370 246 350 355 393 313 245 285 07:44:35 1400+621 263 297 308 241 211 291 323 253 327 353 260 239 390 357 297 368 245 352 355 396 312 243 286 08:15:25 1400+621 264 299 308 240 212 290 322 250 326 352 260 363 238 396 356 300 368 245 350 374 397 323 244 285 08:46:25 1400+621 263 299 308 241 212 289 324 250 329 350 260 364 236 390 351 301 367 245 348 369 398 317 244 282 09:17:30 1400+621 264 300 308 241 213 289 323 252 329 352 260 361 239 394 353 299 364 245 346 373 397 320 244 285 09:48:40 1400+621 262 301 308 241 211 292 324 251 327 350 259 364 241 393 353 301 367 245 349 374 394 319 244 282 09:59:55 1331+305 260 298 307 240 212 291 324 251 324 350 261 363 239 396 353 298 367 244 348 372 387 316 243 285 tortue LISTR(31DEC08) 4 28-JUL-2009 16:03:58 Page 3 File = Haro36-C1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.417999480 GHz Ncor= 2 No. vis= 538096 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 = 1.417999480 GHz Time Source -1- -3- -7- -8- -9--10--11--12--13--14--15--16--17--18--19--20--21--22--23--24--25--26--27--28- max diff 5 4 3 4 2 2 4 2 2 8 2 2 4 3 3 4 4 0 6 4 6 3 2 2 Day # 0 04:11:25 1331+305-105 16 176 109-147 27-137 157 138 174 161-136 164-121 -66 65-112 0 127 46 168 -38-102 31 04:17:15 1400+621-105 10 176 109-150 27-139 156 138 175 160-136 162-119 -66 62-115 0 125 46 167 -39-103 30 04:47:55 1400+621-103 7 175 105-151 25-140 155 139 171 159-136 158-117 -65 63-113 0 128 49 164 -41-104 29 05:18:40 1400+621-105 6 176 104-152 25-142 155 138 168 158-136 157-118 -66 65-115 0 127 50 163 -42-102 29 05:49:35 1400+621-104 7 178 105-151 26-144 156 139 166 160-135 159-117 -64 65-116 0 125 52 167 -42-102 31 06:17:35 1400+621-104 7 177 105-151 27-147 156 137 170 162-137 159-119 -63 66-119 0 124 50 166 -45-103 31 06:45:35 1400+621-105 8 175 105-151 27-150 155 135 175 161-138 158-121 -64 65-121 0 121 52 160 -46-104 31 07:13:35 1400+621-105 9 172 106-152 27-151 155 134 169 161-139 158-121 -64 64-121 0 120 54 163 -46-106 31 07:44:35 1400+621-106 13 173 102-153 27-152 153 135 174 161 154-123 -65 66-124 0 122 50 157 -48-105 33 08:15:25 1400+621-109 9 172 103-151 25-156 151 134 176 161-144 155-123 -65 62-125 0 116 50 159 -50-105 32 08:46:25 1400+621-114 9 172 101-150 25-157 152 132-176 161-146 153-126 -68 63-129 0 116 47 156 -52-106 32 09:17:30 1400+621-112 8 172 102-151 25-158 153 131-177 161-146 150-127 -68 62-130 0 115 47 156 -54-106 32 09:48:40 1400+621-112 7 172 102-151 25-157 152 132 176 160-145 149-126 -69 62-130 0 115 46 157 -54-106 32 09:59:55 1331+305-108 8 172 107-148 26-161 155 132-173 162-146 150-123 -64 66-130 0 113 52 156 -54-105 32 tortue LISTR(31DEC08) 4 28-JUL-2009 16:03:58 Page 4 File = Haro36-C1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.417999480 GHz Ncor= 2 No. vis= 538096 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 = 1.417999480 GHz Time Source -1- -3- -7- -8- -9--10--11--12--13--14--15--16--17--18--19--20--21--22--23--24--25--26--27--28- max diff 7 5 4 6 3 3 4 3 3 7 3 4 5 5 5 7 6 0 6 6 4 4 5 2 Day # 0 04:11:25 1331+305-108-129 -64 5 171 59 123 175 104-118 69 72 109 87 -96 20 37 0 -89-112 112 174 83-177 04:17:15 1400+621-108-135 -63 6 171 59 121 175 106-117 69 74 108 90 -96 19 35 0 -89-111 113 174 83-178 04:47:55 1400+621-102-138 -60 6 174 60 124 176 109-118 71 78 106 95 -91 24 41 0 -84-105 116 176 85-176 05:18:40 1400+621-102-137 -58 7 174 61 124 176 111-118 73 80 107 96 -90 30 41 0 -82-101 118 177 90-174 05:49:35 1400+621-101-137 -56 7 175 62 122 176 111-121 74 81 109 97 -88 31 40 0 -84-100 119 176 90-173 06:17:35 1400+621-102-137 -58 5 174 61 118 173 109-118 77 77 107 95 -88 31 36 0 -86-101 116 173 88-174 06:45:35 1400+621-103-136 -60 4 172 61 115 171 106-112 77 76 106 93 -89 31 35 0 -89-100 113 172 87-175 07:13:35 1400+621-103-136 -64 3 170 60 113 169 104-119 76 74 104 91 -91 28 32 0 -92-100 112 170 83-176 07:44:35 1400+621-106-133 -65 -3 168 58 110 166 103-116 75 99 89 -93 29 29 0 -91-104 110 167 82-174 08:15:25 1400+621-110-138 -68 -3 166 55 106 164 102-115 75 67 97 87 -94 22 26 0 -97-106 107 164 79-176 08:46:25 1400+621-117-141 -69 -7 164 54 104 164 99-108 73 64 94 83 -98 19 21 0 -98-109 103 160 78-178 09:17:30 1400+621-114-142 -70 -6 165 54 104 166 99-108 73 65 92 83 -97 18 21 0 -99-109 104 159 77-177 09:48:40 1400+621-113-144 -69 -6 164 55 105 166 99-114 73 66 92 84 -98 18 22 0 -98-109 104 159 77-177 09:59:55 1331+305-109-142 -68 0 167 56 101 169 100-103 75 65 92 88 -92 21 23 0 -99-103 104 161 79-176 %%% Max Phase dips/jumps: All bounces <= 8 degrees, so leave as is %%% Amp changes: One 11.4% difference, then everything else <=9.4% differences-> no problems! %%% Only flagging needed for the missing Sec (8th) in Ant 16 (7th & 8th galaxy in 16 FULL) ^17. UVFLG -> NEWCH0.1 FG/1 executed on 28jul09 ***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 7th & 8th galaxy scans in: FULL: Ant 16 default UVFLG timer 0 07 16 30 0 07 41 40 $ the source scan between the offending ph.cal scans (7th galaxy) antenna 16, 0 $ the antennas which "jumped" stokes 'FULL' outfgver 1 opcode 'FLAG' reason 'missing sec' $ normally 'phase jump' getn 35 $ *.NEWCH0.1 timer 0 07 47 20 0 08 12 30 $ 8th galaxy --> NEWCH0.1 FG/1 ^18. CLCAL NEWCH0 --> CL/3 executed on 28jul09 ***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 22 $ Change this to your refant getn 35 $ *.NEWCH0.1 $ do this for all NEWCH0 with primary (flux) $ calibrator data ^18b. CLCAL for the phase calibrator and galaxy -> CL/3 default CLCAL sour= '1400+621','Haro36','' $ Secondary (phase) calibrator + galaxy calsour= '1400+621','' $ 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 22 $ 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 35 $ *.NEWCH0.1 $ 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 28jul09 ***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/C1ANBPL_19a.txt getn 35 $ *.NEWCH0.1 $ Must do this separately for every NEWCH0 file tvinit %%% Grabbed each frame: C1ANBPL_19(a-c).tiff (MIDDLE times!) Some high & low weights: ~06:20 in 1RR, 7RR, 9RR, 11RR, 13RR, 14RR, 16RR, 17RR, 18RR, 19RR, 23RR, 24RR, 25RR, 26RR 0 06 20 30 0 06 22 00; RR; 1,7,9,11,13,14,16,17,18,19,23,24,25,26 ~05:50 in 8RL, 13RL, 17RL, 21RL, 25RL 0 05 52 20 0 05 52 30; FULL; ALL antennas (either bad or nothing there) ~07:50 in 8RL, 13RL, 17RL, 19RL, 21RL, 25RL 0 07 47 20 0 07 47 30; FULL; ALL antennas (either bad or nothing there) ^19b. UVFLG to eliminate very high weights executed on 28jul09 ***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 35 $ *.NEWCH0 timer 0 05 52 20 0 05 52 30 antennas 0 stokes '' outfgver 1 opcode 'FLAG' reason 'BAD WEIGHT' timer 0 07 47 20 0 07 47 30; go timer 0 06 20 30 0 06 22 00 antennas 1,7,9,11,13,14,16,17,18,19,23,24,25,26,0 stokes 'RR' tget ANBPL; outprint '/Users/herrmann/Desktop/C1ANBPL_19a1.txt Looks good now! default prtmsg docrt -1 outprint '/Users/herrmann/Desktop/AIPSMSGSRV_C1_Steps1_19.log prtmsg clrmsg ^20. TVFLG FG/1 executed on 28jul09 ^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 35 $ *.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 ^ Check AMPLITUDE, AMP DIFF, PHS DIFF. Be wary of known source structure and uv-range limits!! %%% AMP RR: (3.69 - 15.81) Looks good AMP LL: (3.78 - 15.72) Looks good AMP DIFF RR: (0.0 - 759.5) Looks good AMP DIFF LL: (0.0 - 683.0) Looks good PHS DIFF RR: (0.0 - 12.45) Good enough PHS DIFF LL: (0.0 - 8.407) Good enough ***Note: occasionally, flagging using UVFLG can be more straightforward (e.g., deleting an antenna). %%% 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 35 $ *.NEWCH0.1 getona 35 $ *.NEWCH0.2 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 35 $ *.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 35 $ *.NEWCH0.2 getona 35 $ *.NEWCH0.3 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 35 $ *.NEWCH0.3 ^21. Calibration/flagging checks: calibrators ^21a. UVPLT executed on 28jul09 ***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 35 $ *.NEWCH0.1 $ do this for each NEWCH0 file bparm 0 $ amp. vs. uv-distance dotv -1; go -> PL version 1 same as grabbed C1UVPLT_21a_AMP.tiff -> Looks good! Primary generally ~14.7 +/- 0.7 Jy; supposed to be 15.0 Jy; nice & flat (except some wiggles) Secondary generally ~4.4 +/- 0.4 Jy; supposed to be 4.40 Jy; nicely clean Constant the whole way-> as expected because no limits on UVmax bparm 0, 2 $ phase vs. uv-distance dotv -1; go -> PL version 2 same as grabbed C1UVPLT_21a_PHS.tiff %%% Nicely clean! Mostly 0 +/- 5, with all scatter within -10 to 14 (most of the "nasty" stuff in 1st Pri, probably Ant 3) ^21b. IMAGR executed on 28jul09 [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 '1400+621','' $ calibrator to image docalib 1; gainuse 3 $ apply latest calibration flagver 1 $ apply latest flags -- set this to the $ highest-numbered FG table outname 'Haro36C1sec $ 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 35 $ *.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, but the secondary is slightly elongated, and has a faint source @ 1 o'clock tortue> IMAGR1: Loading field 1 from -6.67E-03 to 4.40E+00 interp by 2 tortue> IMAGR1: Field 1 final Clean flux 4.382 Jy (Pretty close to expected 4.40 Jy from GETJY & 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 has a fairly circular inside with some extra stuff outside Grabbed C1UVPLT_uv_coverage.tiff (same as PL version 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 04 20 00 0 07 10 40 $ 1st - 6th galaxy scans $ timer 0 06 48 30 0 09 45 40 $ 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 35 $ *.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: AMPLITUDE RR: (0.2 - 776.0) Pretty clean- some gaps at beginning of 5th scan -> trimmed AMPLITUDE LL: (0.4 - 678.0) Pretty clean Flagging 0 straggly timelines AMPL DIFF RR: (0.0 - 519.1) Looks pretty good AMPL DIFF LL: (0.0 - 508.5) Looks pretty good PHAS DIFF RR: (0.0 - 180.0) Pretty random PHAS DIFF LL: (0.0 - 179.9) Pretty random %%% 1 flagging command made. 6th - 11th galaxy scans: AMPLITUDE RR: (0.3 - 790.8) Pretty clean AMPLITUDE LL: (0.000 - 4.889) 1 hot pixel Flagging LL: 12-23, 07:21:06 -> now 0.3-594.9 Flagging 2 straggly timelines (9 & 11) AMPL DIFF RR: (0.0 - 514.8) Looks pretty good AMPL DIFF LL: (0.0 - 376.8) Looks pretty good PHAS DIFF RR: (0.0 - 179.9) Pretty random PHAS DIFF LL: (0.0 - 179.9) Pretty random %%% 3 flagging commands made. 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 35 $ *.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 28jul09 ***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 'Haro36','' 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 35 $ *.NEWCH0.1 $ whichever file holds the galaxy bparm 0 $ amp. vs. uv-distance Some structure; amplitude a bit higher at low kL Some banding in RR but not in LL dotv -1; go -> PL version 4 same as grabbed C1UVPLT_23a_AMP.tiff ^23b. IMAGR executed on 28jul09 *** Note: If uvwtfn is set to 'NA' it will override any value given to robust. default IMAGR sources 'Haro36','' $ the galaxy docalib 1; gainuse 3 $ apply latest calibration flagver 1 $ apply latest flags -- set this to the $ highest-numbered FG table outname 'Haro36C1_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 35 $ *.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. %%% Fuzzy structure at center plus perhaps 9 extended point sources around it- in ~4 groups ^24. TASAV -> CH0SAV.1,2,3 executed on 28jul09 default TASAV getn 35 $ *.NEWCH0 $ loop over NEWCH0 files (= FREQIDs) outna 'Haro36C1MdTb 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 28jul09 ***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 35 $ *.NEWCH0.1 $ if single FREQID $ getn 35 $ *.NEWCH0.3 $ if multiple FREQIDs: set this to file you flagged $ on most recently (usually the file with the $ galaxy in it) getona 34 $ *.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 35 $ *.NEWCH0 $ if multiple FREQIDs: all should have same merged SN $ table so you can use whichever NEWCH0 file you want getona 34 $ *.LINCOP --> LINCOP SN/1 ^26. CLCAL LINCOP SN/1 --> CL/3 executed on 28jul09 ***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 22 $ Change this to your refant getn 34 $ *.LINCOP ^26b. CLCAL for the phase calibrator and galaxy -> CL/3 default CLCAL sour= '1400+621','Haro36','' $ Secondary (phase) calibrator + galaxy calsour= '1400+621','' $ 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 22 $ 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 34 $ *.LINCOP ^27. Calibration/flagging checks: calibrators ^27a. WIPER executed on 28jul09 ###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 34 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed as C1WIPER_27a_AMP.tiff-> looks pretty clean! Primary: ~15.0 +/- 4.0 Jy (15.0 Jy in catalog) (a little larger scatter, though) Secondary: ~4.5 +/- 3.5 Jy (4.40 Jy in catalog) (but some scatter...) No solar interference evident bparm(2) 2 $ phase vs. uv-distance %%% Pretty good! (C1WIPER_27a_PHS.tiff) Primary: 0 +/- 15 Secondary: 0 +/- 50 with some scatter to +/-180, but not much ^27b. POSSM executed on 28jul09 ***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='1400+621','' $ 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 34 $ *.LINCOP tvinit %%% Grabbed C1POSSM_27b_RR.tiff & C1POSSM_27b_LL.tiff 1(RR): PROBLEM! Slopes from ~4.43 to 4.38 Jy (only a ~1.6% effect, so not really a problem) 1(RR): phase is pretty much 0 +/- 0.3 degree 1(LL): Fairly flat, ~4.40 +/- 0.02 Jy 1(LL): phase is pretty much 0 +/- 0.2 degree, but slight slope down ^27c. IMAGR not necessary [if desired -- this is not really necessary] executed on 29jul09 *** Note: If uvwtfn is set to 'NA' it will override any value given to robust. default IMAGR source='1400+621','' $ 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 'Haro36C1Sec2 $ 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 34 $ *.LINCOP Started 11:48:40 and finished 11:55:26 ***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 41 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: No real differences (as expected) default tvmovie; ltype 6; getn 41; tvinit; tvmovie Looks pretty constant, fairly clean, and pretty much alone. ^28. Calibration/flagging checks: sources ^28a.1 WIPER executed on 29jul09 ###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 'Haro36','' 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 34 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed C1WIPER_28a.tiff: Max is ~75 Jy with everything else < 10 Jy, so one column to clean. uvrange 10 12; stokes 'RR'-> column in 10.0 10.5 & only in RR (between 10.2 & 10.3) timer 0 04 20 00 0 07 10 40 -> somewhere in 1st 6 galaxy scans timer 0 04 20 00 0 05 46 40 -> not in 1st 3 timer 0 05 52 20 0 06 14 40 -> not in 4th timer 0 06 20 30 0 06 42 40 -> not in 5th timer 0 06 48 30 0 07 10 40 -> in 6th tget TVFLG; getn 34; stokes 'RR'; flagver 2; outfgver 2; timer 0 06 48 30 0 07 10 40; uvrange 10.0 10.5 Flagging RR, All channels: 3-17, 06:50:36 tget WIPER; stokes ''; uvrange 0 0; timer 0 0 Now max is 9.4 Jy, so should be good. (C1WIPER_28a1.tiff) All the banding is basically in RR, though. (C1WIPER_28a1_LL.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= 9.4 Jy (No clipping needed) ###This is the value that you will be using in CLIP when combining your data!!! ^28x. POSSM [Eliminated from the recipe] executed on 29jul09 anyways ***Check vector average of all data for the galaxy. You should see your HI line! default POSSM source='Haro36','' $ 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 34 $ *.LINCOP tvinit %%% Results: OBVIOUSLY there! 1 RR: phs: 0 +/- 150 on ends, except for ~80-140 where it's 0 +/- 10 amp: < 5 mJy on ends but beautiful peak at ~25 mJy C1POSSM_28_RR.tiff 1 LL: phs: 0 +/- 150 on ends, except for ~80-140 where it's 0 +/- 10 amp: < 5 mJy on ends but beautiful peak at ~25 mJy C1POSSM_28_LL.tiff ^28b. IMAGR executed on 29jul09 default IMAGR sources 'Haro36', '' 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 'Haro36C1gal $ 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 34 $ *.LINCOP Started 12:26:30, and done by 12:53:54 ***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 43 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: The bright galaxy blob moved a bit. default tvmovie; ltype 6; getn 43; tvinit; tvmovie Good rotation (channels ~59-145) and there's at least 1 continuum source in the FOV, but not very close to the galaxy. ?28c. Noise Estimations: calculated on 29jul09 ##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: 1.5 mJy x expected rms = K/SQRT[N(N-1)(N_IF*T_int*Delta_nu_M)] in mJy ^ expected rms = 1.5 mJy (here) where: K = 8.0 (for L band) N = # of Antennas (24 here) N_IF = 2 (for 2 polarizations) T_int = total on-source integration time in HOURS (4.464 hrs here = 267:50 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 = 1.6 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 = 1 94; trc = 512 126 default IMSTAT getn 43 $ Haro36C1gal movie blc 1 94 10 $ 10th channel, bottom left corner of box containing primary sources in the image trc 512 126 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: 1.6 mJy ^29. TASAV -> EndTaB.LINSAV.1 executed on 29jul09 default TASAV outna 'Haro36C1EdTb outcla 'linsav' outdi 2 $ Ideally set this to a different disk from indisk, $ in case of disk crashes getn 34 $ *.LINCOP ^30. FITTP executed on 29jul09 dataout '/Users/herrmann/Desktop/C1-BeginTasav.FITS create: ^Haro36_C1_UV_CALIB_NEWCH0.FITS $ one per FREQID ^Haro36_C1_UV_CALIB_LINCOP.FITS ^Haro36_C1-BeginTasav.FITS ^Haro36_C1-MidTasav.FITS $ one per FREQID ^Haro36_C1-EndTasav.FITS ^Add the end date to the start of this file! ^PRTMSG & CLRMSG ^31. Send to DEIDRE 29jul09 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. Haro36 C1 (AN) calibration Hi Deidre, The Haro36 C1 array (AN) data is ready to be ftped, so I've started ftping it all to the NRAO system. (Yesterday I finished ftping all the data I calibrated earlier this summer.) 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: 8th Sec in Ant 16 out completely- will need to flag 7th & 8th galaxy scans FULL in Ant 16 Ant 21 looks fine even though there's a warning about it in the log C1POSSM_27b_RR.tiff: Definite slope from ~4.43 to 4.38 Jy, but that's only a ~1.6% effect, so not really a problem Good rotation (channels ~59-145) and there's at least 1 continuum source in the FOV, but not very close to the galaxy. Total Time on Source = 267:50 min (4.464 hrs) (Two 10s scans were lost due to flagging straggly time scans.) The expected rms is 1.5 mJy and the measured rms is 1.6 mJy, so 1.5 [1.6]. The measured value is a bit higher than the expected value, which is not surprising since 13 out of 24 antennas were EVLA. (Antennas 2, 4 [Ant problem], 5 [EVLA testing], 6 [Ant problem], and 29 were lost. Again, there were no explanations in the log for antennas 2 and 29 being lost, but I still don't think Ant 29 has even been used.) N = 24 antennas, Tint = 4.464 hrs, delta_nu_M = 6.1035156e-3 MHz, N_IF = 2, K = 8.0 (for L band) The uv data files that I am ftping to the NRAO site are: Haro36_C1_UV_CALIB_NEWCH0.FITS Haro36_C1_UV_CALIB_LINCOP.FITS Haro36_C1-BeginTasav.FITS Haro36_C1-MidTasav.FITS Haro36_C1-EndTasav.FITS In addition, I have created a figuresC1 subdirectory (in the calib directory) as usual and already uploaded all the .tiff and .ps files mentioned in the data reduction log. I also put the data reduction log and 2 log files from the AIPS_MSGSRV window in the notes directory. Lastly, the observation log should already be in the obs directory as an html file, so I didn't add anything to the obs directory. I think that's it! There are 4 more data sets for Haro36 that I'll work on around my 2nd referee report stuff. Kim =)