1. e-VLBI correlator mode: control interfaces
2007 April 17
EXPReS Annual Review: SA1

2. Monitoring tools: Integrating fringe display
2007 April 17
EXPReS Annual Review: SA1

3. Monitoring tools: Data status monitor
2007 April 17
EXPReS Annual Review: SA1

4. Monitoring tools: Data status monitor
2007 April 17
EXPReS Annual Review: SA1

5. Rapid adjustment of correlator params: vex editor
2007 April 17
EXPReS Annual Review: SA1

6. (near) Real-time analysis: streamlining of post processing
2007 April 17
EXPReS Annual Review: SA1

7. Web-based Post-processing
2007 April 17
EXPReS Annual Review: SA1

8. EXPReS Annual Review: SA1
e-VLBI challenges
We are already very good in quick science turnaround: on the fly
data processing/pipelining is possible!
At 512 Mbs and with Effelsberg, Shanghai and other new telescopes,
we will also be very good in sensitivity and resolution (in 2007/2008)
BUT
We are poor with immediate good calibration
The current system is not suitable for real ToOs
We have to be able to produce high dynamic range maps of sources
varying on timescales of hours
We must be able to change schedule on the fly to be able to observe
e.g. new transients with poor coordinates
2007 April 17
EXPReS Annual Review: SA1

9. EXPReS Annual Review: SA1
Algol, 14 December 2006 run:
Simultaneous optical photometry and e-EVN obs.
(5 GHz, 256 Mbps) during secondary minimum
Source flared – total intensity and circular polarization
variations consistent between WSRT and e-EVN data
Flare emission ~2 mas offset from the CP peak
Dedicated observations of such flares
will be challenging even for e-VLBI
Detected proper motion during the
10 hours run –fitted orbital parameters
of the AB close binary (see poster).
Csizmadia et al.
(in prep.)
2007 April 17
EXPReS Annual Review: SA1

10. EXPReS Annual Review: SA1
Westerbork  e-EVN as a unique instrument
Westerbork Synthesis Array data may help in calibration (amplitude, linear
and circular polarization)
May help to confirm detection/non-detection of weak targets
Could be used as a ‘built-in’ alert instrument for the e-EVN
Wb can help improving coordinates of new transients…
…with adaptive scheduling, this could be immediately used for
the VLBI array
Not to mention the additional information on the very large-scale
structure (which we normally waste when we do not reduce Wb data
along with the EVN)
How long will Westerbork be still around ???
2007 April 17
EXPReS Annual Review: SA1

11. EXPReS Annual Review: SA1
The e-EVN as a trigger instrument?
Because we are not good in responding ToOs, but good in providing quick
results, can we turn around the logic?
Initially could monitor known transient sources (e.g. microquasars like
GRS ) in a snapshot mode during the e-VLBI tests, regularly.
In case of a flare, report to the community, providing 0-epoch maps!
(not possible when a ToO VLBI run follows a single dish trigger)
Easily accessible for the whole astronomical community, ready maps from
the EVN archive (all public!)
With more sensitivity and dynamic scheduling, may continue this with
new X-ray transients or gamma bursts
How shall we select these key science targets?
Can we contribute to X-ray and gamma ray missions like GLAST?
Have invested a lot of money in e-VLBI, now let us invest a great deal of observing time!
2007 April 17
EXPReS Annual Review: SA1