[daip] BL247E1 and BL247E2 data

[Li Jingjing]

Dear Sir/Madam,

I have a question about the calibration of the BL247E1 and BL247E2 data. In the key files, the source name is IC443M.  But in the data files, the source name was changed to IC443M' and ‘IC443M’, respectively.  I can not use these source names in the AIPS. You know if you use 
>source ‘IC443M’
AIPS can not find this source.

Can you tell me if I can change the name of source in the AIPS and how to do, or other method to solve this problem?

Looking forward to your reply.

Jingjing Li 

> On Oct 6, 2017, at 04:29, analysts at nrao.edu wrote:
> 
> 
> Dear PI,
> 
> We have correlated and examined the data for project BL247E1 which observed on 23 Sep. 2017.
> The contact person for this project was Data Analysts. 
> 
> Preliminary notes and information:
> 
> SC: Did not observe; internet down due to hurricanes.
> 
> 
> **Dual RDBE special note:**  
> If your project used 8 DDC channels, or 4 IFs, please report any problems seen in 
> your data to the scientific helpdesk at https://help.nrao.edu.  
> 
> 1. All observers should visit http://www.vlba.nrao.edu/astro/messages/ 
>   for important messages. 
> 
> 2. For possible problems and additional information which may have
>   affected this observation, please consult the VLBA System Monitoring 
>   page located at the Internet URL:
>   http://www.vlba.nrao.edu/astro/VOBS/astronomy/vlba_sysmon.html
>   Select (click on) the link for the 2017 VLBA System Monitoring Calendar.
>   Then select (click on) the monitoring project code(s) 'DQ***'
>   that observed during the concurrent week for this
>   observation.  This will display the selected monitoring project directory
>   where a report summary named monitor.txt can be viewed or retrieved.
>   This directory also contains useful plots under reference antenna
>   subdirectories.
> 
> 3. Access to the file server is provided to view and retrieve text and PostScript files,
>   This can be reached through the VLBA homepage at http://www.vlba.nrao.edu/astro/VOBS/astronomy/
> 
> 4. Disk weights versus time plots have been generated for the entire time range
>   of your experiment. These are a measure of disk record/playback quality,
>   representing the fraction of valid data samples. Data with weights below
>   70-75% should be flagged. However, you may want to be more cautious
>   when dealing with non-VLBA stations.  The easiest way to estimate
>   the best weight threshold is by looking at the disk weights vs. time
>   plots generated here.  You can find the weights plots at
>   http://www.vlba.nrao.edu/astro/VOBS/astronomy/sep17/bl247e1/jobs/sniffer
>   /*wts.ps.  
>   See http://www.vlba.nrao.edu/astro/VOBS/astronomy/doc/readme-sniffer.txt
>   for instructions on how to interpret this
>   plot.
> 
> 5. Delay, rate, phase, and amplitude plots were made for the observation.
> 
> 6. Autocorrelation bandpass plots were generated for all antennas for scans
>   on all sources.
> 
> 7. Cross-correlation bandpass plots were generated for all baselines to LA
>   for scans on all sources.
> 
> 8. Gzipped PostScript plots of Tsys and other monitor data for each available
>   VLBA antenna can be found at:
>   http://www.vlba.nrao.edu/astro/VOBS/astronomy/sep17/bl247e1.
> 
> 9. The jobs associated with the correlation of BL247E1 can be found at:
>   http://www.vlba.nrao.edu/astro/VOBS/astronomy/sep17/bl247e1/jobs.
>   These files provided the correlator with all ancillary data
>   needed for VLBI, including:  correlation parameters and telescopes
>   correlated in the final production.
> 
> 
>   Automated Calibration Transfer for VLBA Correlator Output
>   ---------------------------------------------------------
> The first phase of automated calibration transfer for data from
> the VLBA correlator has been completed, and was used
> for your observation.  This transfer of calibration information includes
> data from the 10 VLBA antennas, as well as selected information from the VLA, GB
> and Effelsberg, which currently provide VLBA-style
> monitor data.  Significant changes to AIPS have been required to
> introduce calibration transfer, so users must have the patched
> version of 15OCT98 AIPS, or any later version, beginning with 15APR99.
> It is highly recommended that users download the 31DEC10 version
> of AIPS to take advantage of new tools and current updates.
> Help files for a number of AIPS tasks have been updated to
> reflect the new calibration procedures.  There also is a new
> version of the VLBI chapter of the AIPS cookbook, available
> from http://www.cv.nrao.edu/aips/aipsdoc.html, that includes
> more details on how to cope with the calibration transfer process.
> 
> The calibration-transfer process relieves observers of the
> burden of creating and inputting calibration files for VLBA
> antennas.  Instead, this information is now provided as tables
> attached to the FITS data sets output by the VLBA correlator.
> The ancillary data include antenna gain (GC table), system
> temperature (TY table), pulse calibration (PC table), flags (FG
> table), and weather (WX table).  The wise observer will not
> modify these original tables; processing errors might then force
> the data to be reloaded using FITLD.  See the description of
> MERGECAL in Section 9.2.1.7 of the new cookbook chapter for more
> detail.  Of course, skeptical users can simply delete the appropriate
> tables created by FITLD and generate their tables in the old manner.
> 
> At present, ancillary data from most external telescopes must still
> be loaded in the old manner, and observations of strong sources
> may be needed for manual pulse calibration at those telescopes.
> Up-to-date instructions on coping with observations including
> external telescopes can be found at
> http://www.vlba.nrao.edu/astro/obscor/cal-transfer/.
> 
> Please send comments on calibration transfer to amiodusz at nrao.edu, 
> and send bug reports to daip at nrao.edu, with a copy to amiodusz at nrao.edu.
> 
> 
>   End of Letter