vs04v Results
Submitted checklist.txt and checklist.tex is also available		   [Summary | AIPS | Difmap ]
Analyst: Philip Edwards
Date Prepared: 12-10-2005
 

Summary
 
Observation code : vs04v    AIPS Version : 31dec02   
Date of Observation : 2001/159    Difmap Version : 2.3c 
Source Name : J0303-62    vsop_difmap used : Yes 
Calibration Source(s) : J0450-81, J0635-75         
Ground telescopes : HH, HO, MP  Model Fitted to data : Yes 
Tracking Station(s) : UZ    Image made : No 
Correlator : Penticton         

 
Abstract
Extraction from GOT w422e. Hobart data dodgy, and Penticton report fringes to HALCA with HH only in second tracking pass (RZ) so extract 3 hours including first tracking pass (UZ) urvey obs. Space fringes found. Two component modelfit provides acceptable fit, though doesn't reproduce structure seen on long HALCA baselines all that well.
Model
Flux (Jy)
Radius (mas)
Theta (deg)
Major (mas)
Axial ratio
Phi (deg)
TB (10^12 K)
1.19887 0.0209007 -50.6833 0.385518 1.00000 -128.972 0.3936
0.329561 0.666302 79.7671 0.488269 1.00000 -161.756 0.0675
(*) Quoted Brightness temperatures assume Gaussian components and are in the local (z=0) frame.


AIPS Data Reduction Notes
 
Task
Adverbs
CL
in
SN
in
CL
out
SN
out
Comments
FITLD
 
 
 
 
 two files read in from disk 
INDXR
 
 
1 
 
  
PRTAN
 
 
 
 
  
LISTR
 
 
 
 
  
DTSUM
 
 
 
 
  
UVPLT
 
 
 
 
  
ANTAB
 
 
 
 
 Nominal Tsys for HALCA and MP, logged values for HH, HO 
APCAL
 
 
 
1 
  
CLCAL refant=3
1 
1 
2 
 
  
FRING solint=5
 
3 
 
 
 (sn2 made with solint=3) 
CLCAL
2 
3 
3 
 
  
SPLIT
 
 
 
 
  
FITTP
 
 
 
 
  

AIPS Input Files
Comments
- None -

AIPS Output Files
PRTAN.LIS
LISTR.LIS
DTSUM_0.LIS		 POSSM_AP_1.PS
VPLOT_AP_1.PS
SN_CALIB_SNR_1.PS		 SN_CALIB_DEL_1.PS
SN_CALIB_RAT_1.PS


Difmap Data Reduction Notes
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? No
Comments on Difmap processing
Hobart data is no good (possibly crossed pols), leaving Mopra, Hart and HALCA. AS the source is a long way south, the ground baselines provide very little (u,v) plane coverage. There's evidence of structure on the HALCA baselines, but finding a model that provides a good fit is difficult. The two circular gaussian fit may be acceptable. It would seem a third component may be necessary to provide a better fit on the long HALCA baselines. The effect on the core size and flux density may not be large though.

Modelfit
Ampl, Phase vs (u,v) Distance
PS (28 kb)
JPEG (39 kb)
 Ampl, Phase vs Time
PS (147 kb)
JPEG 1, 2		 (u,v) Coverage
PS (15 kb)
JPEG (27 kb)
Closure Phase vs Time
PS (121 kb)
JPEG 1		 Image with model components
PS (33 kb)
JPEG (38 kb)

More details on the Images and Modelfits are found in this page.

Model
Flux (Jy)
Radius (mas)
Theta (deg)
Major (mas)
Axial ratio
Phi (deg)
TB (10^12 K)
1.19887 0.0209007 -50.6833 0.385518 1.00000 -128.972 0.3936
0.329561 0.666302 79.7671 0.488269 1.00000 -161.756 0.0675
(*) Quoted Brightness temperatures assume Gaussian components and are in the local (z=0) frame.


Last updated on Wed Oct 12 08:14:56 UTC 2005
by db_results.pl version 0.3.