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

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

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

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

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

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

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

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

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

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

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 GRS1915+105) 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