| VS04b Results
Submitted checklist.txt and checklist.tex is also available |
[Summary | AIPS | Difmap ] |
| Observation code | : | VS04b | AIPS Version | : | 15OCT98 (15APR99) |
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| Date of Observation | : | 1998/191 | Difmap Version | : | 2.3c | |||
| Source Name | : | J0334-40 | vsop_difmap used | : | Yes | |||
| Calibration Source(s) | : | |||||||
| Ground telescopes | : | HartRAO, Mop, Usuda64 | Model Fitted to data | : | Yes | |||
| Tracking Station(s) | : | UZ,RZ | Image made | : | Yes | |||
| Correlator | : | Penticton |
| Abstract
No fringes were found to Mop telescope. This resulted in a 2 GRTs experiment. Fringes were detected on Halca during the entire RZ pass (4~hrs). The ground Usuda64 was on source for only ~1hr. Seems Usuda64 had problem during the observations since the correlated flux densities on the baselines to Usuad64 had an unreasonable decrease with time when compared to another ground telescope HartRAO. The image was made to this limited dataset with the phase self-calibration only. A point source model was fit the calibrated data. |
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| FITLD | douvcomp=1;dotable=1 |
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load the uv FITS data with 15APR99 version AIPS to overcome the timestamp problem when the first FITS file ran cross the 24-hour boundary. Later data reduction was kept with 15OCT98 version. |
| MSORT | sort='TB' |
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sort the data to 'TB' order |
| INDXR | cparm(3)=1 |
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index uv data with 1 min CL entry interval |
| TACOP |
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protect original CL1 | |
| ANTAB |
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determine the Tsys and gain curve (see ANTAB.TXT file). Tsys=95K for Halca. | |
| APCAL | opcode=' ' |
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generate an amplitude calibration solution table |
| CLCAL | opcode='CALI' interpol=' ' refant=1 |
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apply amplitude calibration solution |
| FRING | docalib=1 flagv=-1;solint=4;refant=1 aparm=2,0,0,0,0,1,2,0 dparm=1,0,0,0,1,0 antwt=1,1,30,1 |
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FFT fringe searching (after several trial runs) |
| CLCAL | opcode='CALP';interpol='AMBG';smotype='VLBI' refant=1 |
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apply FFT solutions |
| FRING | docalib=1 flagv=-1;solint=4;refant=1 aparm=2,0,0,0,0,1,3,0 dparm=1,0 antwt=1,1,30,1 |
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(FFT+LS) fringe fitting |
| CLCAL | opcode='CALP';interpol='AMBG';smotype='VLBI' refant=1 |
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apply full fringe fitting solutions |
| TACOP |
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save calibration table CL7 | |
| CLCOR | antenna=0;opcode='GAIN';clcorprm=0.91,0 |
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Penticton gain correction |
| TASAV |
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copy all extension tables to a dummy file | |
| SPLIT | docalib=1;douvcomp=1;aparm=2,0,0,1,0 |
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make calibrated single-source data files: J0334-40.SPLIT |
| FITTP |
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export each single-source file in FITS format to disk file for further imaging analysis |
AIPS Input Files
| INDXR.TXT ANTAB.TXT |
Comments - None - |
AIPS Output Files
| Phase selfcal applied? | Yes |
| Global amplitude selfcal (gscal) applied? | No |
| Amplitude selfcal on non-global timescales used? | No |
| Modelfit made and saved? | Yes |
| Image Made and saved? | Yes |
| Comments on Difmap processing
average data over 30 sec (uvaver 30,true) raise the weight of HALCA (selfant VSOP_SC,false,100) keep non-closing data during phase self-cal (selfflag false,3,4) clean and phase self-cal with uniform weighting (uvw 2,-1 ... etc) switch to natural weighting to clean more flux (uvw 0,-1 ... etc) (*NO* amplitude self-cal with eventually only 3 antennas available) switch back to obtain a uniform weighting clean image: peak=0.296 Jy/beam, RMS=9.3 mJy/beam; beam=0.438 mas x 0.249 mas @ 15.8 deg Both point source and circular gaussian models were tried to fit the calibrated data. Finally, a point source model was accepted. |
| Image | ||||
| Ampl, Phase vs (u,v) Distance PS (59 kb) GIF (8 kb) |
Ampl, Phase vs Time PS (341 kb) GIF 1, 2 |
(u,v) Coverage PS (31 kb) GIF (5 kb) | Closure Phase vs Time PS (156 kb) GIF 1 |
Clean Image PS (30 kb) GIF (100 kb) |
| Modelfit | ||||
| Ampl, Phase vs (u,v) Distance PS (59 kb) GIF (8 kb) |
Ampl, Phase vs Time PS (340 kb) GIF 1, 2 |
(u,v) Coverage PS (31 kb) GIF (5 kb) | Closure Phase vs Time PS (156 kb) GIF 1 |
Image with model components PS (30 kb) GIF (6 kb) |
More details on the Images and Modelfits are found in this page.
