e-VLBI

What is e-VLBI?

e-VLBI, or electronic Very Long Baseline Interferometry, uses fibre optic networks to connect radio telescopes to a central data processor, which correlates the data from the telescopes in real-time. The astronomers can inspect their results almost immediately. In classic VLBI the data are recorded on disks and shipped to the correlator for processing, which can take weeks.

e-VLBI is the obvious choice for studying transient events such as supernova explosions and gamma-ray bursts; follow-on observations can be triggered in time, also in other spectral regions. But e-VLBI is not only quicker, it is also easier to organize once the procedures are clear. So, it might become the standard way of doing VLBI.

For more information about e-VLBI, or to try a virtual interferometer for yourself, see our Introduction to e-VLBI.

 

JIVE and e-VLBI

Through the EXPReS project (2006-2009), the EVN correlator at JIVE was upgraded for e-VLBI operations, up to 16 telescopes at a time, 1 Gb/s from each telescope; the same capacity as for classic VLBI. As a result of these upgrades, the EVN now offers regularly scheduled e-VLBI sessions, as well as opportunities for target-of-opportunity observations.

The NEXPRes project (2010-2013), of which JIVE is the coordinator, is addressing the current bottlenecks of e-VLBI which prevent it from being used for all EVN observations. Among other activities, NEXPReS will develop high-speed recording/transmitting capabilities which will allow for data re-correlation and remove the distinction between disk-based and electronic VLBI.

For more information about JIVE's contributions to the development of e-VLBI, watch JIVE: Forging a Path to the Future of Radio Astronomy (15 minutes, 387 MB mp4, best viewed with VLC). 

 

e-VLBI Progress

The following links provide some information about the current e-VLBI capabilities and status.

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