| vs02z Results
Submitted checklist.txt and checklist.tex is also available |
[Summary | AIPS | Difmap ] |
| Observation code | : | vs02z | AIPS Version | : | 15APR99 |
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| Date of Observation | : | 1999/265 | Difmap Version | : | 2.3c | |||
| Source Name | : | J0501-0159 | vsop_difmap used | : | No | |||
| Calibration Source(s) | : | 0528+134 | ||||||
| Ground telescopes | : | ATCA, Kashima, Mopra | Model Fitted to data | : | Yes | |||
| Tracking Station(s) | : | RZ (Madrid) | Image made | : | Yes | |||
| Correlator | : | Penticton |
| Abstract
VS02z is a full (~3 hours) GOT experiment (W010f) without extractions. Mopra recorded in a wrong mode, which was partialy corrected for at the correlator. Fringes were found at all times with good SNR. Due to the small number of GRTs and the similarity of Kashima-ATCA and Kashima-Mopra baselines, we cannot make a reliable image of the source. An elliptical gaussian model component fits the data well. |
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| FITLD |
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| MSORT |
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| INDXR | cparm 1 22 1 0 |
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Input: INDXR.TXT |
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| ANTAB |
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Nominal Tsys values and gaincurves were used for all interferometer element. | |
| APCAL |
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| CLCAL | '' |
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| UVFLAG | antennas 4 0 reason 'wrong obsmode' flagver 1 bif 1; eif 1; bchan 1; echan 128; |
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Flag Mopra IF 1 channels 1-128 |
| UVFLAG | antennas 4 0 reason 'wrong obsmode' flagver 1 bif 2; eif 2; bchan 129; echan 256; |
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Flag Mopra IF 2 channels 129-256 |
| FRING | solint 5 flagver 1 aparm 2 0 0 0 0 1 3 0 1 0 search 1 3 4 {it was not needed} dparm 1 2000 100 2 refant 1 {ATCA} |
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"Found 246 good solutions" Note: IFs will be SPLIT-ed separately. |
| CLCAL | refant 1 interpol '2pt' |
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| SPLIT | aparm 2 0.8 0 flagver 1 sources '0528+134' '' sources 'j0501-01' '' |
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SPLIT data for the target and the calibrator. Do not average IFs! |
| UVAVG | xinc 1; yinc 60; zinc 0.8; |
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One minute integration time. |
| FITTP |
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Write spectral and time averaged data to disk. |
AIPS Input Files
| ANTAB.TXT INDXR.TXT |
Comments - None - |
AIPS Output Files
| Phase selfcal applied? | Yes |
| Global amplitude selfcal (gscal) applied? | Yes |
| Amplitude selfcal on non-global timescales used? | No |
| Modelfit made and saved? | Yes |
| Image Made and saved? | Yes |
| Comments on Difmap processing
Expected (sub)mas-scale structure cannot be imaged (see pre-launch and other survey images). ATCA-Mopra relative amplitude calibration is OK. Amplitude correction factor for Kashima can differ significantly from what is given below, depending on imaging strategy. Amplitude correction factors (IF1/IF2): ATCA VSOP_SC Kashima Mopra 0.92/0.93 1.04/1.04 1.20/1.18 0.92/0.88 Source correlated flux density at ~10 Mlambda is much less than in the pre-launch survey. Total flux density decreased according to ATCA data (available till February 1998). |
| Image | ||||
| Ampl, Phase vs (u,v) Distance PS (43 kb) GIF (7 kb) |
Ampl, Phase vs Time PS (143 kb) GIF 1, 2 |
(u,v) Coverage PS (24 kb) GIF (4 kb) | Closure Phase vs Time PS (104 kb) GIF 1 |
Clean Image PS (31 kb) GIF (81 kb) |
| Modelfit | ||||
| Ampl, Phase vs (u,v) Distance PS (43 kb) GIF (7 kb) |
Ampl, Phase vs Time PS (143 kb) GIF 1, 2 |
(u,v) Coverage PS (24 kb) GIF (4 kb) | Closure Phase vs Time PS (104 kb) GIF 1 |
Image with model components PS (35 kb) GIF (7 kb) |
More details on the Images and Modelfits are found in this page.
