NOTES: Most of 2nd Pri in Ants 1 & 9 out (weather), also some in Ant 19 out- just flagged 2nd Pri in Ants 1 & 9 completely The galaxy is barely there, and it is rotating (channels ~80-140). There appears to be only 1 continuum source. LITTLE THINGS AIPS Reduction of Haro29, B1 (V) config.: VLA Obs. of 28jan08 ===================================================================== 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 25jun09-26jun09 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 B1 configuration (V) From observing log (available online as a text file at http://www.lowell.edu/users/dah/littleteam/haro29/vla/obs/2008-01-28_0413_AH927.txt, but will also ftp as logs_AH927_V.html): Observing: 28Jan08 10:14:29-16:11:50 (28Jan08 03:14:29-09:11:50 local time) * Wind/API rms phase/clouds: 28Jan 10:04:45 SW at 8.7 m/s 5.3 API Sky cover 70%. Mixed clouds. 28Jan 12:25:00 SW at 9.5 m/s 6.9 API Sky overcast. Mixed clouds. Light rain. 28Jan 15:00:00 NW at 8.0 m/s 12.0 API Sky cover 60%. Mixed clouds. * 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. 1, 9 LOST (WEATHER: Wind gusts are causing the antennas to stow.) (16:06:00-16:12:00) ^1. FILLM executed on 25jun09 ^a. Request archive data: requested AH927_V_1 and saved temporarily as /Users/herrmann/Desktop/AH927_B_V_1 ^b. FILLM -> Haro29-B1.CH 0.1, Haro29-B1.LINE.1 (1 & 2) default FILLM datain '/Users/herrmann/Desktop/AH927_B_V_ nfiles 0 $ normally don't skip any files band 'L' qual 2 $ restricts FILLM to the galaxy+calibrators of interest vlaobs 'AH927' timerang 0 0 $ Other scans before Haro29 but with different qual # outna 'Haro29-B1 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_V_1 tortue> FILLM1: tortue> FILLM1: *** ATTENTION - default: loading subarray 1 *** tortue> FILLM1: tortue> FILLM1: tape file # 1, start date/time = 20080128/04:14:50 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 26 antennas. tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Program = AH927 ; Tape revision number = 32. tortue> FILLM1: Create Haro29-B1 .CH 0 . 1 (UV) on disk 1 cno 1 tortue> FILLM1: Ref. date = 20080128 A-C = 1.419130 B-D = 1.419130 GHz tortue> FILLM1: Create Haro29-B1 .LINE . 1 (UV) on disk 1 cno 2 tortue> FILLM1: Ref. date = 20080128 A-C = 1.419130 B-D = 1.419130 GHz tortue> FILLM1: FLMFQ: FQ entry tolerance = 1.609D+02 tortue> FILLM1: Found 1331+305 : 2 1.562 MHz at IAT 0/ 10:14:55 tortue> FILLM1: MCINI: Processing Correlator Code '2AC ' with 26 antennas. tortue> FILLM1: MCINI - Mode 2AC compatible tortue> FILLM1: Ref. date = 20080128 A-C = 1.419130 B-D = 1.419130 GHz tortue> FILLM1: Appending new data to: Haro29-B1 .CH 0 . 1 disk 1 tortue> FILLM1: Ref. date = 20080128 A-C = 1.419130 B-D = 1.419130 GHz tortue> FILLM1: Appending new data to: Haro29-B1 .LINE . 1 disk 1 tortue> FILLM1: Found 1331+305 : 2 1.562 MHz at IAT 0/ 10:15:05 tortue> FILLM1: Found 1331+305 : 2 1.562 MHz at IAT 0/ 10:15:35 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 10:22:15 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 10:27:05 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 10:52:45 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 10:57:35 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 11:23:25 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 11:28:15 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 11:54:05 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 11:59:15 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 12:25:05 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 12:30:15 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 12:56:05 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 13:00:55 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 13:29:35 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 13:34:25 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 14:00:15 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 14:04:55 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 14:30:35 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 14:35:15 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 15:00:45 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 15:05:25 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 15:31:05 tortue> FILLM1: Found HARO29 : 2 1.562 MHz at IAT 0/ 15:35:45 tortue> FILLM1: Found 1313+549 : 2 1.562 MHz at IAT 0/ 16:01:25 tortue> FILLM1: Found 1331+305 : 2 1.562 MHz at IAT 0/ 16:06:25 tortue> FILLM1: Read 654542 visibilities from 1 files tortue> FILLM1: Appears to have ended successfully ^2. TASAV -> LINSAV.1 executed on 25jun09 ***We TASAV right away, because VLANT changes the AN table. Did I mention we're paranoid? default TASAV outna 'Haro29B1BgTb 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 25jun09 ***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 (54) unless otherwise specified. ^4. LISTR/SCAN --> Haro29-B1.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-B1.listr getn 54 $ *.LINCOP --> *.listr tortue LISTR(31DEC08) 4 25-JUN-2009 12:04:29 Page 1 File = Haro29-B1 .LINCOP. 1 Vol = 1 Userid = 4 Freq = 1.419129970 GHz Ncor = 2 No. vis = 654542 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0002 A 1 0/10:15:05 - 0/10:20:35 1 1 10400 2 1313+549 : 0002 C 1 0/10:22:15 - 0/10:26:25 1 10401 18555 3 HARO29 : 0002 1 0/10:27:05 - 0/10:52:05 1 18556 67320 4 1313+549 : 0002 C 1 0/10:52:45 - 0/10:56:55 1 67321 75770 5 HARO29 : 0002 1 0/10:57:35 - 0/11:22:35 1 75771 124398 6 1313+549 : 0002 C 1 0/11:23:25 - 0/11:27:25 1 124399 132523 7 HARO29 : 0002 1 0/11:28:15 - 0/11:53:15 1 132524 180923 8 1313+549 : 0002 C 1 0/11:54:05 - 0/11:58:15 1 180924 188899 9 HARO29 : 0002 1 0/11:59:15 - 0/12:24:15 1 188900 237874 10 1313+549 : 0002 C 1 0/12:25:05 - 0/12:29:15 1 237875 245930 11 HARO29 : 0002 1 0/12:30:15 - 0/12:55:15 1 245931 295005 12 1313+549 : 0002 C 1 0/12:56:05 - 0/13:00:05 1 295006 303105 13 HARO29 : 0002 1 0/13:00:55 - 0/13:28:55 1 303106 355880 14 1313+549 : 0002 C 1 0/13:29:35 - 0/13:33:45 1 355881 363986 15 HARO29 : 0002 1 0/13:34:25 - 0/13:59:35 1 363987 412039 16 1313+549 : 0002 C 1 0/14:00:15 - 0/14:04:15 1 412040 419964 17 HARO29 : 0002 1 0/14:04:55 - 0/14:29:55 1 419965 467589 18 1313+549 : 0002 C 1 0/14:30:35 - 0/14:34:35 1 467590 475714 19 HARO29 : 0002 1 0/14:35:15 - 0/15:00:05 1 475715 524414 20 1313+549 : 0002 C 1 0/15:00:45 - 0/15:04:45 1 524415 532539 21 HARO29 : 0002 1 0/15:05:25 - 0/15:30:25 1 532540 580789 22 1313+549 : 0002 C 1 0/15:31:05 - 0/15:35:05 1 580790 588914 23 HARO29 : 0002 1 0/15:35:45 - 0/16:00:45 1 588915 637989 24 1313+549 : 0002 C 1 0/16:01:25 - 0/16:05:25 1 637990 646114 25 1331+305 : 0002 A 1 0/16:06:25 - 0/16:11:45 1 646115 654542 tortue LISTR(31DEC08) 4 25-JUN-2009 12:04:29 Page 2 File = Haro29-B1 .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 : 0002 A 13:31:08.2879 30:30:32.958 0.000 0.000 0.000 0.000 18828 2 1313+549 : 0002 C 13:13:37.8529 54:58:23.894 0.000 0.000 0.000 0.000 97393 3 HARO29 : 0002 12:26:16.0000 48:29:37.000 0.000 0.000 0.000 0.000 538321 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 1.41912997 1312.2560 6.1035 1 Primary: 5:40, 5:30-> 11:10 Secondary: 4:20, 4:20, 4:10, 4:20, 4:20, 4:10, 4:20, 4:10, 4:10, 4:10, 4:10, 4:10 -> 50:50 Galaxy: 25:10, 25:10, 25:10, 25:10, 25:10, 28:10, 25:20, 25:10, 25:00, 25:10, 25:10 -> 279:50 total However, subtract 10s out of 0 scans-> so 279:50 total (4.664 hrs = 04:39:50) ^5. VLANT -> AN/1, CL/2 executed on 25jun09 ***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 54 $ *.LINCOP tortue> VLANT1: WARNING: 2 ANTENNAS MAY STILL GET MORE CORRECTION tortue> VLANT1: Copied CL file from vol/cno/vers 1 54 1 to 1 54 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 54 $ *.LINCOP getona 54 $ *.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 54 $ *.LINCOP 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= 3B147 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 B1) 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 B1950 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 B1950 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 25jun09 ***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 54 $ *.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 =14.7325 (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 54 $ *.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 54 $ *.LINCOP ; ^7c. CALRD executed on 25jun09 ***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 54 $ *.LINCOP --> calib: 10s (both) source: 10s ^9. UVFLG -> FG/1 executed on 25jun09 ***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 25jun09 ***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) %%% Large % of 2nd Pri in Ants 1 & 9 out (weather), also some in Ant 19 out %%% EVLA-EVLA baselines flagged properly %%% RR: 0.035 - 3.104, LL: 0.001 - 3.233 2 hot pixels in LL: 3-21, 15:01:06 & 13:31:56 Trimmed 1 straggly timeline from 1st Sec Trimmed 1 straggly timeline from 2nd Pri Flagging 1 existing time in Ant 9 2nd Pri Flagging 4 existing times in Ant 1 2nd Pri Final: RR: (0.035 - 3.066), LL: (0.053 - 3.157) ^AMP DIFF to check for variable gains %%% RR: 0.0 - 138.6 (most nastiness in both Pris in Ant 24) %%% LL: 0.0 - 133.8 (same as above) Final: RR: (0.0 - 138.6), LL: (0.0 - 133.8) ^PHS DIFF to check for variable atmosphere/gains %%% RR: 0.00 - 45.69 (most of highest values in 10th Sec- possibly during light rain?) %%% LL: 0.00 - 57.28 (same as above) Clipping Interactively to 25 degrees in RR then LL-> 25.32 & 26.54 Final: RR: (0.00 - 25.32), LL: (0.00 - 26.54) %%% Saved as Figures/B1TVFLG_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 %%% 166 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 25jun09 ***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 54 $ *.LINCOP --> LINCOP FG/1 ^10c. (EXTRA) WIPER on Calibrators in LINCOP executed on 25jun09 (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 54 $ *.LINCOP %%% No hot columns or hot dots- max is ~4.8 (B1WIPER_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 25jun09 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 54 $ *.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 54 $ *.LINCOP --> BP/1 x11b2. BPASS FREQID 2 -> BP/2 not necessary ***Same as 11B1, 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 54 $ *.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 54 $ *.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 54 $ *.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 54 $ *.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 54 $ *.LINCOP getona 54 $ *.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 54 $ *.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 54 $ *.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 (except for 1 & 9) 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 54 $ *.LINCOP outfile '/Users/herrmann/Desktop/B1POSSMplots11c1.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='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 54 $ *.LINCOP 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 54 $ *.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 5.0 mJy for all channels 1(RR): phase is generally 80 +/- 15 degrees 1(LL): Rather flat around 13.7 mJy for all channels 1(LL): phase is generally -165 +/- 5 degrees dotv -1; go tget lwpla for i = 13 to 14; plver = i; go; wait lwpla; end %%% (Added to B1POSSMplots11c1.ps) ^12. AVSPC -> NEWCH0.1 (2,3) executed on 25jun09 ***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 54 $ *.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 (55) 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 54 $ *.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 54 $ *.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 55 $ *.NEWCH0 outprint '/Users/herrmann/Desktop/Haro29-B1_12d.listr tortue LISTR(31DEC08) 4 25-JUN-2009 16:09:59 Page 1 File = Haro29-B1 .NEWCH0. 1 Vol = 1 Userid = 4 Freq = 1.419129970 GHz Ncor = 2 No. vis = 654542 Scan summary listing Scan Source Qual Calcode Sub Timerange FrqID START VIS END VIS 1 1331+305 : 0002 A 1 0/10:15:05 - 0/10:20:35 1 1 10400 2 1313+549 : 0002 C 1 0/10:22:15 - 0/10:26:25 1 10401 18555 3 HARO29 : 0002 1 0/10:27:05 - 0/10:52:05 1 18556 67320 4 1313+549 : 0002 C 1 0/10:52:45 - 0/10:56:55 1 67321 75770 5 HARO29 : 0002 1 0/10:57:35 - 0/11:22:35 1 75771 124398 6 1313+549 : 0002 C 1 0/11:23:25 - 0/11:27:25 1 124399 132523 7 HARO29 : 0002 1 0/11:28:15 - 0/11:53:15 1 132524 180923 8 1313+549 : 0002 C 1 0/11:54:05 - 0/11:58:15 1 180924 188899 9 HARO29 : 0002 1 0/11:59:15 - 0/12:24:15 1 188900 237874 10 1313+549 : 0002 C 1 0/12:25:05 - 0/12:29:15 1 237875 245930 11 HARO29 : 0002 1 0/12:30:15 - 0/12:55:15 1 245931 295005 12 1313+549 : 0002 C 1 0/12:56:05 - 0/13:00:05 1 295006 303105 13 HARO29 : 0002 1 0/13:00:55 - 0/13:28:55 1 303106 355880 14 1313+549 : 0002 C 1 0/13:29:35 - 0/13:33:45 1 355881 363986 15 HARO29 : 0002 1 0/13:34:25 - 0/13:59:35 1 363987 412039 16 1313+549 : 0002 C 1 0/14:00:15 - 0/14:04:15 1 412040 419964 17 HARO29 : 0002 1 0/14:04:55 - 0/14:29:55 1 419965 467589 18 1313+549 : 0002 C 1 0/14:30:35 - 0/14:34:35 1 467590 475714 19 HARO29 : 0002 1 0/14:35:15 - 0/15:00:05 1 475715 524414 20 1313+549 : 0002 C 1 0/15:00:45 - 0/15:04:45 1 524415 532539 21 HARO29 : 0002 1 0/15:05:25 - 0/15:30:25 1 532540 580789 22 1313+549 : 0002 C 1 0/15:31:05 - 0/15:35:05 1 580790 588914 23 HARO29 : 0002 1 0/15:35:45 - 0/16:00:45 1 588915 637989 24 1313+549 : 0002 C 1 0/16:01:25 - 0/16:05:25 1 637990 646114 25 1331+305 : 0002 A 1 0/16:06:25 - 0/16:11:45 1 646115 654542 tortue LISTR(31DEC08) 4 25-JUN-2009 16:09:59 Page 2 File = Haro29-B1 .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 : 0002 A 13:31:08.2879 30:30:32.958 14.732 0.000 0.000 0.000 18828 2 1313+549 : 0002 C 13:13:37.8529 54:58:23.894 0.000 0.000 0.000 0.000 97393 3 HARO29 : 0002 12:26:16.0000 48:29:37.000 0.000 0.000 0.000 0.000 538321 ID Source Freq(GHz) Velocity(Km/s) Rest freq (GHz) 1 1331+305 1.4191 -138.0264 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 1.41912997 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 54 $ *.LINCOP getona 55 $ *.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 54 $ *.LINCOP getona 55 $ *.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 54 $ *.LINCOP getona 55 $ *.NEWCH0.3 --> NEWCH0.3, FG/1 ^14. CALIB -> NEWCH0.1(,2,3) SN/1 executed on 25jun09 (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 55 $ *.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 3.159E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 3.086E+00 tortue> CALIB1: Found 100 good solutions tortue> CALIB1: Average closure rms = 0.0011 +- 0.0001 tortue> CALIB1: No data were found > 99.0 rms from solution $ This time there is no second primary default CALIB get2n 210 $ 3B147_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 55 $ *.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 55 $ *.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 2.740E+00 tortue> CALIB1: LPOL, IF= 1 The average gain over these antennas is 2.670E+00 tortue> CALIB1: Found 624 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 55 $ *.NEWCH0.2 getona 55 $ *.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 55 $ *.NEWCH0.3 getona 55 $ *.NEWCH0.1 --> NEWCH0.1, SN/3 ^15b. GETJY SN/1-3, SU/1 executed on 25jun09 ***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 55 $ *.NEWCH0.1 tortue> GETJY1: Task GETJY (release of 31DEC08) begins tortue> GETJY1: Source:Qual CALCODE IF Flux (Jy) tortue> GETJY1: 1313+549 : 2 C 1 1.30559 +/- 0.00424 %%% (Basically the same as expected 1.31 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 15 $ Change this to your refant getn 55 $ *.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 55 $ *.NEWCH0.1 getona 55 $ *.NEWCH0.2 getona 55 $ *.NEWCH0.3 ^16. SN table checks ^16a. SNPLT last SN table executed on 25jun09 ^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 55 $ *.NEWCH0.1 ===> 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 normally 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: B1SNPLT_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 55 $ *.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) %%% Grabbed each frame: B1SNPLT_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 25jun09 default LISTR optype 'gain'; inext 'sn'; inver 1; freqid -1 antennas -4,5,29,0; $ 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-B1_16b.listr getn 55 $ *.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 25-JUN-2009 16:24:30 Page 1 File = Haro29-B1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419129970 GHz Ncor= 2 No. vis= 654542 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 = 1.419129970 GHz Time Source -1- -2- -3- -6- -7- -8- -9--10--11--12--13--14--15--16-*17**18*-19--20--21--22-*23*-24--25--26--27--28- max % diff 2.6 2.8 3.5 1.5 2.1 2.5 1.5 1.4 0.9 2.4 2.8 4.0 1.6 1.6 13. 9.0 3.6 1.4 3.7 2.3 14. 2.6 1.4 1.4 3.2 2.5 Day # 0 10:17:50 1331+305 218 206 260 267 316 287 239 311 284 278 363 364 303 358 320 460 352 300 336 260 380 313 473 337 250 295 10:24:25 1313+549 216 208 259 272 320 287 237 316 281 284 365 365 300 350 306 461 348 300 333 263 375 317 467 332 250 297 10:54:50 1313+549 217 206 262 268 317 289 242 314 281 281 365 360 303 357 305 466 350 298 335 262 374 321 464 331 250 298 11:25:25 1313+549 214 209 261 266 314 286 237 310 279 281 359 361 303 358 320 482 350 302 334 264 374 317 467 335 248 298 11:56:15 1313+549 221 212 265 268 316 291 243 315 280 287 368 372 302 358 310 451 366 305 340 266 403 314 475 338 254 302 12:27:15 1313+549 223 214 273 270 324 296 242 318 283 289 371 382 308 355 354 413 362 304 346 271 437 310 477 339 262 308 12:58:05 1313+549 220 205 267 267 323 289 243 313 280 286 369 371 299 352 310 421 353 302 337 266 394 306 472 336 259 302 13:31:45 1313+549 219 208 264 274 321 291 243 313 280 281 363 366 307 353 317 409 354 304 329 265 378 307 476 333 258 301 14:02:15 1313+549 214 210 265 270 319 288 242 311 280 283 361 363 305 348 301 411 353 303 333 266 382 310 465 335 254 303 14:32:35 1313+549 215 206 263 270 321 288 241 317 284 282 353 367 305 350 310 431 359 302 326 265 379 313 471 336 254 301 15:02:45 1313+549 212 205 262 273 319 286 238 311 283 277 371 369 303 354 306 448 352 302 331 265 377 315 474 338 253 299 15:33:05 1313+549 222 209 262 270 320 287 241 313 283 278 360 366 302 352 301 465 348 301 332 264 374 313 469 340 252 298 16:03:25 1313+549 218 207 261 272 312 289 238 314 283 279 355 364 308 357 314 449 345 303 329 263 375 310 468 331 253 300 16:09:10 1331+305 205 261 269 313 287 311 285 278 363 362 302 359 324 454 352 299 334 260 382 314 467 340 251 296 tortue LISTR(31DEC08) 4 25-JUN-2009 16:24:30 Page 2 File = Haro29-B1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419129970 GHz Ncor= 2 No. vis= 654542 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 = 1.419129970 GHz Time Source -1- -2- -3- -6- -7- -8- -9--10--11--12--13--14--15--16-*17**18*-19--20-*21*-22-*23*-24--25--26--27--28- max % diff 3.0 1.4 1.8 1.4 4.1 1.9 1.3 0.7 1.9 1.6 1.8 1.9 0.9 1.8 7.1 5.6 3.3 1.3 7.0 3.3 12. 3.6 1.8 1.5 1.7 2.2 Day # 0 10:17:50 1331+305 262 218 302 290 316 241 216 292 336 254 333 360 247 368 234 408 368 305 361 246 352 383 410 320 242 284 10:24:25 1313+549 258 220 303 294 317 240 214 291 331 256 340 356 245 363 228 416 368 302 364 246 347 382 400 315 242 282 10:54:50 1313+549 266 218 304 289 315 241 216 291 338 251 335 353 246 364 229 411 365 302 362 245 350 391 396 318 242 281 11:25:25 1313+549 258 219 304 290 313 240 214 290 334 255 330 348 248 367 231 423 367 305 358 245 349 381 403 315 243 281 11:56:15 1313+549 269 220 307 291 325 244 218 292 331 254 333 357 245 370 231 395 379 307 375 248 368 381 406 318 245 287 12:27:15 1313+549 271 222 311 293 329 246 216 292 334 253 337 347 249 364 248 394 380 309 388 255 402 380 401 318 245 291 12:58:05 1313+549 265 216 309 287 319 241 216 289 333 255 338 349 246 364 231 398 371 306 366 247 369 370 409 319 248 284 13:31:45 1313+549 266 221 306 291 313 244 218 288 330 252 335 351 249 359 233 390 373 309 361 246 353 376 408 313 246 287 14:02:15 1313+549 261 221 307 291 316 242 216 288 331 255 335 358 249 364 232 390 369 307 359 246 353 372 408 317 244 286 14:32:35 1313+549 260 218 303 287 316 241 216 290 334 254 328 355 248 367 228 401 376 306 357 245 351 379 395 316 244 288 15:02:45 1313+549 257 218 306 290 312 239 213 290 333 251 337 357 247 366 229 413 364 307 351 247 354 375 406 320 242 285 15:33:05 1313+549 260 220 303 287 310 239 216 288 336 249 331 359 246 368 228 429 362 305 355 245 350 372 399 319 242 282 16:03:25 1313+549 265 216 302 289 307 240 216 291 340 253 328 354 249 370 231 414 357 305 356 248 355 371 397 312 244 284 16:09:10 1331+305 218 304 290 309 242 291 339 253 333 354 249 374 233 420 369 304 363 246 357 382 408 318 241 284 tortue LISTR(31DEC08) 4 25-JUN-2009 16:24:30 Page 3 File = Haro29-B1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419129970 GHz Ncor= 2 No. vis= 654542 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 = 1.419129970 GHz Time Source *1* *2* *3* -6- *7* -8- -9--10-*11*-12-*13**14*-15-*16**17**18**19*-20-*21**22**23*-24-*25**26**27**28* max diff 11 14 18 3 24 4 4 5 24 3 16 14 0 14 14 17 18 7 19 13 27 9 14 25 17 13 Day # 0 10:17:50 1331+305 87 -77 -85 -32 146 64-141 112 66 132 22 130 0-118-157 113 -42 -14-172 69 -58 120 -74 21 56 -33 10:24:25 1313+549 83 -75 -88 -33 142 62-142 113 62 130 22 129 0-118-158 112 -44 -14-170 65 -62 122 -73 19 55 -35 10:54:50 1313+549 80 -82 -88 -32 132 62-143 114 50 130 8 123 0-122-168 105 -46 -12-174 58 -77 119 -86 3 47 -32 11:25:25 1313+549 70 -80 -84 -33 136 60-142 114 49 130 -2 115 0-136-179 95 -57 -12 180 52 -79 112 -93 0 50 -29 11:56:15 1313+549 65 -74 -75 -33 135 62-141 114 54 132 0 107 0-143 179 91 -63 -12 175 55 -70 109 -94 -10 51 -24 12:27:15 1313+549 59 -63 -86 -32 144 64-138 114 35 133 -5 93 0-141 172 90 -61 -12 163 62 -97 108-100 -12 58 -33 12:58:05 1313+549 54 -74-101 -33 147 66-137 113 11 134 -21 88 0-145 170 73 -77 -16 149 66-122 101-107 -16 56 -45 13:31:45 1313+549 43 -65 -99 -34 146 68-138 111 4 132 -27 77 0-144 168 62 -95 -13 144 76-124 95-113 -26 57 -41 14:02:15 1313+549 35 -71 -99 -34 149 64-137 111 4 132 -28 71 0-150 159 61 -98 -14 139 67-129 88-118 -29 58 -38 14:32:35 1313+549 27 -73 -86 -35 152 61-139 111 16 131 -34 76 0-160 145 55-106 -11 139 60-114 79-123 -31 63 -30 15:02:45 1313+549 24 -68 -88 -34 166 63-140 110 6 131 -32 71 0-163 144 54-109 -13 135 62-125 78-116 -21 76 -32 15:33:05 1313+549 15 -71-106 -34 145 59-136 110 -11 134 -32 58 0-176 131 53-116 -19 116 49-144 69-130 -46 61 -45 16:03:25 1313+549 14 -57 -97 -31 169 63-136 115 -7 133 -32 57 0-171 132 47-120 -12 117 60-140 71-118 -30 78 -37 16:09:10 1331+305 -53 -96 -32 169 62 114 -2 133 -30 53 0-175 133 48-121 -12 118 60-139 70-114 -24 84 -35 tortue LISTR(31DEC08) 4 25-JUN-2009 16:24:30 Page 4 File = Haro29-B1 .NEWCH0. 1 Vol = 1 Userid = 4 IF = 1 Freq= 1.419129970 GHz Ncor= 2 No. vis= 654542 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 = 1.419129970 GHz Time Source *1* *2* *3* -6- *7* -8- -9--10-*11*-12-*13**14*-15-*16**17**18**19*-20-*21**22**23**24**25**26**27**28* max diff 10 13 18 3 24 5 4 5 24 3 16 14 0 13 16 18 16 7 17 11 26 11 16 26 16 14 Day # 0 10:17:50 1331+305-179-122 21-112 -38 74 -68 113-120-155-143 112 0-178 65-153 77 -60 67 68-180-122 147 148-111 88 10:24:25 1313+549 177-120 19-112 -41 73 -68 114-124-155-141 112 0-177 65-153 75 -59 70 66 177-120 148 148-110 87 10:54:50 1313+549 174-126 19-112 -50 74 -69 116-135-155-155 107 0 179 57-160 73 -56 66 59 163-121 136 131-118 89 11:25:25 1313+549 165-123 24-112 -45 73 -67 118-134-153-164 99 0 166 47-169 65 -55 61 55 162-128 132 130-113 93 11:56:15 1313+549 161-119 31-113 -48 73 -67 116-132-153-163 89 0 159 45-175 57 -57 55 57 170-132 127 118-113 96 12:27:15 1313+549 154-107 21-113 -40 76 -64 116-150-150-168 78 0 162 37-173 60 -58 44 66 145-133 123 117-105 89 12:58:05 1313+549 149-117 5-116 -37 78 -63 115-174-148 176 73 0 157 36 169 44 -63 30 69 119-139 116 112-108 77 13:31:45 1313+549 139-107 8-117 -38 81 -63 115-179-149 170 63 0 159 33 159 28 -61 26 79 118-143 110 105-106 81 14:02:15 1313+549 129-114 6-119 -37 76 -63 111 180-150 169 57 0 152 23 157 22 -63 19 68 112-153 104 100-105 83 14:32:35 1313+549 123-115 19-118 -33 73 -65 113-167-152 164 62 0 142 7 151 14 -60 20 60 127-161 99 98-100 93 15:02:45 1313+549 118-110 17-119 -19 73 -63 111-178-151 165 55 0 137 5 150 11 -63 14 62 114-162 106 107 -87 90 15:33:05 1313+549 111-114 -1-119 -40 70 -59 110 162-149 164 41 0 125 -8 147 4 -68 -3 51 96-173 90 81-103 76 16:03:25 1313+549 109-101 7-116 -16 73 -59 115 168-150 164 40 0 129 -10 141 0 -61 -3 62 100-171 102 97 -88 84 16:09:10 1331+305 -98 9-117 -16 71 114 172-150 166 35 0 125 -7 142 -1 -61 -3 61 100-172 107 103 -82 85 %%% Max Phase dips/jumps: LOTS of bounces by 10-27 degrees, but looks pretty gradual, so leave as is %%% Amp changes: 7 bounces between 5 and 13.5%, so leave as is %%% No flagging needed. =) 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 55 $ *.NEWCH0.1 timer 0 10 48 00 0 11 07 30 --> NEWCH0.1 FG/1 ^18. CLCAL NEWCH0 --> CL/3 executed on 25jun09 ***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 55 $ *.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= '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 55 $ *.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 25jun09 ***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/B1ANBPL_19a.txt getn 55 $ *.NEWCH0.1 $ Must do this separately for every NEWCH0 file %%% Grabbed each frame: B1ANBPL_19(a-c).tiff (MIDDLE times!) Everything looks good, I guess- no high weights, but weird low structure ~11:30-13:00 EXCEPT for: 1 high weight FULL in Ant 13, 17, 21, 25, 26 ~10:25 (0 10 27 00 0 10 27 10) ^19b. UVFLG to eliminate very high weights executed on 25jun09 ***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 55 $ *.NEWCH0 timerang 0 10 27 00 0 10 27 10 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' tget ANBPL; outprint '/Users/herrmann/Desktop/B1ANBPL_19a1.txt Now everything looks good! default prtmsg docrt -1 outprint '/Users/herrmann/Desktop/AIPSMSGSRV_B1_Steps1_19.log prtmsg clrmsg ^20. TVFLG FG/1 executed on 26jun09 ^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 55 $ *.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: (0.66 - 15.56) Looks good AMP LL: (0.77 - 15.58) Looks good AMP DIFF RR: (0.000 - 1.210) Looks good (except some nasty spots in both Pris of Ant 24) AMP DIFF LL: (0.000 - 1.291) Looks good (except some nasty spots in both Pris of Ant 24) PHS DIFF RR: (0.00 - 32.30) Looks good (a bit higher than usual, but this Sec is fainter) PHS DIFF LL: (0.00 - 25.65) Looks good (same as above) ***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 55 $ *.NEWCH0.1 getona 55 $ *.NEWCH0.2 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 55 $ *.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 55 $ *.NEWCH0.2 getona 55 $ *.NEWCH0.3 Re-run TVFLG with same inputs as above, except: flagver 2 ; outfgver 2 getn 55 $ *.NEWCH0.3 ^21. Calibration/flagging checks: calibrators ^21a. UVPLT executed on 26jun09 ***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 55 $ *.NEWCH0.1 $ do this for each NEWCH0 file bparm 0 $ amp. vs. uv-distance dotv -1; go -> PL version 1 same as grabbed B1UVPLT_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 bparm 0, 2 $ phase vs. uv-distance dotv -1; go -> PL version 2 same as grabbed B1UVPLT_21a_PHS.tiff %%% Pretty clean! Looks like Pri is roughly 0 +/- 7 degrees and Secs are 0 +/- 12 degs All scatter within -40 to 30 degrees ^21b. IMAGR executed on 26jun09 [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 'Haro29B1sec 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 55 $ *.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 -7.170E-03 to 1.300E+00 tortue> IMAGR1: Field 1 final Clean flux 1.259 Jy (A bit low wrt expected 1.31 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 not nicely circular (excellent uv coverage) Grabbed B1UVPLT_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 10 27 00 0 13 29 00 $ 1st-6th galaxy scans $ timer 0 13 00 50 0 16 00 50 $ 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 55 $ *.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 0 straggly timelines AMPLITUDE RR: (0.000 - 1.555) Looks pretty clean, but a few hot spots Flagging RR: 1-20, 12:37:26-36 & 12:34:36-> now 0.3-885.5 AMPLITUDE LL: (0.000 - 6.563) At least 1 hot pixel Flagging LL: 12:08:06 21-22-> now 0.2-820.5 AMPL DIFF RR: (0.0 - 635.3) Looks pretty good, but could use some cleaning AMPL DIFF LL: (0.0 - 567.5) Same as above PHAS DIFF RR: (0.0 - 179.9) Pretty random PHAS DIFF LL: (0.0 - 179.9) Pretty random Clipping interactively in AMP separately to 700-> 0.3-698.5 & 0.2-699.4 Now AMPDIFF: 0.0-467.3 & 0.0-469.1 50 flagging commands needed. 6th-11th galaxy scans: Flagging 0 straggly timelines AMPLITUDE RR: (0.3-959.5) Looks pretty clean, but a few hot spots Clipping interactively in AMP separately to 700-> 0.3-693.6 AMPLITUDE LL: (0.2-833.2) Looks pretty clean Clipping interactively in AMP separately to 700-> 0.2-657.7 AMPL DIFF RR: (0.0 - 467.3) Looks pretty good AMPL DIFF LL: (0.0 - 452.4) Same as above PHAS DIFF RR: (0.0 - 179.9) Pretty random PHAS DIFF LL: (0.0 - 180.0) Pretty random 18 flagging commands 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 55 $ *.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 26jun09 ***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 55 $ *.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 B1UVPLT_23a_AMP.tiff ^23b. IMAGR executed on 26jun09 *** 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 'Haro29B1_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 55 $ *.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 26jun09 default TASAV getn 55 $ *.NEWCH0 $ loop over NEWCH0 files (= FREQIDs) outna 'Haro29B1MdTb 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 26jun09 ***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 55 $ *.NEWCH0.1 $ if single FREQID $ getn 55 $ *.NEWCH0.3 $ if multiple FREQIDs: set this to file you flagged $ on most recently (usually the file with the $ galaxy in it) getona 54 $ *.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 55 $ *.NEWCH0 $ if multiple FREQIDs: all should have same merged SN $ table so you can use whichever NEWCH0 file you want getona 54 $ *.LINCOP --> LINCOP SN/1 ^26. CLCAL LINCOP SN/1 --> CL/3 executed on 26jun09 ***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 54 $ *.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 54 $ *.LINCOP ^27. Calibration/flagging checks: calibrators ^27a. WIPER executed on 26jun09 ###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 54 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed as B1WIPER_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: B1WIPER_27a_PHS_Pri.tiff: Good- generally 0 +/- 15 with all scatter within -30 to 35 On all 12 Secs: B1WIPER_27a_PHS_Secs.tiff: full range -180 to 180 (because relatively faint) ^27b. POSSM executed on 26jun09 ***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 54 $ *.LINCOP tvinit %%% Grabbed B1POSSM_27b_RR.tiff & B1POSSM_27b_LL.tiff 1(RR): Roughly 1.30 Jy and fairly flat 1(RR): Fairly flat at 0 +/- 0.4 degrees 1(LL): Roughly 1.30 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 26jun09 *** 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 'Haro29B1Sec2 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 54 $ *.LINCOP Started 10:10:10 and finished 10:23:11 ***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 61 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: No real differences (as expected) default tvmovie; ltype 6; getn 61; tvinit; tvmovie Looks pretty constant & clean. ^28. Calibration/flagging checks: sources ^28a.1 WIPER executed on 26jun09 ###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 54 $ *.LINCOP bparm(2) 1 $ amp. vs. uv-distance Grabbed B1WIPER_28a.tiff: maximum is 9.9 Jy, so pretty clean. 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 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 26jun09 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 54 $ *.LINCOP tvinit %%% Results: Barely there! 1 RR: phs: 0 +/- 150 on ends, except for ~95-115 where it's ~0 +/- 30 amp: about 4 mJy on ends, but peaks ~10 mJy B1POSSM_28_RR.tiff 1 LL: phs: 0 +/- 150 on ends, except for ~90-120 where it's ~0 +/- 30 amp: about 3.5 mJy on ends, but peaks ~9 mJy B1POSSM_28_LL.tiff ^28b. IMAGR executed on 26jun09 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 'Haro29B1gal 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 54 $ *.LINCOP Started 10:34:00, and finished by 11:22:00 ***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 63 tblc 0 0 108; ttrc 0 0 108 $ also tried 88 & 128: The faint galaxy blob moved. default tvmovie; ltype 6; getn 63; tvinit; tvmovie The galaxy is barely there, and it is rotating (channels ~80-140). There appears to be only 1 continuum source. ?28c. Noise Estimations: calculated on 26jun09 ##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: 1.3 mJy x expected rms = K/SQRT[N(N-1)(N_IF*T_int*Delta_nu_M)] in mJy ^ expected rms = 1.3 mJy (here) where: K = 8.0 (for L band) N = # of Antennas (26 here) N_IF = 2 (for 2 polarizations) T_int = total on-source integration time in HOURS (4.664 hrs here = 279:50 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 = 195 612; trc = 216 637 default IMSTAT getn 63 $ Haro29B1gal movie blc 195 612 10 $ 10th channel, bottom left corner of box containing primary sources in the image trc 216 637 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 26jun09 default TASAV outna 'Haro29B1EdTb outcla 'linsav' outdi 2 $ Ideally set this to a different disk from indisk, $ in case of disk crashes getn 54 $ *.LINCOP ^30. FITTP executed on 26jun09 dataout '/Users/herrmann/Desktop/B1-BeginTasav.FITS create: ^Haro29_B1_UV_CALIB_NEWCH0.FITS $ one per FREQID ^Haro29_B1_UV_CALIB_LINCOP.FITS ^Haro29_B1-BeginTasav.FITS ^Haro29_B1-MidTasav.FITS $ one per FREQID ^Haro29_B1-EndTasav.FITS ^Add the end date to the start of this file! ^PRTMSG & CLRMSG ^31. Send to DEIDRE 26jun09 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 B1 (V) calibration Hi Deidre, The Haro29 B1 array (V) 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: Most of 2nd Pri in Ants 1 & 9 out (weather), also some in Ant 19 out- just flagged 2nd Pri in Ants 1 & 9 completely The galaxy is barely there, and it is rotating (channels ~80-140). There appears to be only 1 continuum source. Total Time on Source = 279:50 mins (4.664 hrs) (No 10s scans were lost due to flagging straggly time scans.) The expected rms is 1.3 (?) mJy and the measured rms is 1.6 mJy, so 1.3 (?) [1.6]. The measured value is a bit higher than the expected value, which is expected since 13 out of 26 antennas were EVLA. (Only Antennas 4 [EVLA testing], 5, 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 = 26 antennas, Tint = 4.664 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_B1_UV_CALIB_NEWCH0.FITS Haro29_B1_UV_CALIB_LINCOP.FITS Haro29_B1-BeginTasav.FITS Haro29_B1-MidTasav.FITS Haro29_B1-EndTasav.FITS In addition, I will create a figuresB1 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 2 log files from the AIPS_MSGSRV window in the notes directory. Lastly, since the observation log probably is only in the obs directory as a txt file, I'll probably add it as an html file. I think that's it! One more Haro29 data set to go and then I'll start on Haro36. Kim =)