LOFAR will enter its first operational phase starting from the middle of 2012, following a period of commissioning in 2010 and 2011. Most of the remaining stations are planned to be completed by the end of 2012.

Software and instrumental development and commissioning are coordinated to provide a first set of observing and data analysis functionality available to the telescope users.

This is collectively called "LOFAR Version 1.0". 

LOFAR Version 1.0 

LOFAR "Version 1.0" will provide a stable, robust system that enables:

1) the specification, planning, managing, and automatic execution of imaging observations using the Standard Imaging Pipeline in the post-processing cluster up to and including  producing the first images. There will not be a self-calibration loop.

2) the specification, planning, managing, and automatic execution of beam formed observations up to and including processing on the BG/P.

Starting the ‘known pulsar’ pipeline will be provided as an Expert Mode, and will involve significant interaction with the Science Support Group.

Four tied array modes will be supported: Coherent Stokes, Incoherent Stokes, Complex Voltages and Fly's Eye mode.

3) an initial Long Term Archive that supports:

a) ingesting imaging data products (visibilities and images) and Beam Formed data products (complex voltages, coherent and incoherent stokes, fly's eye mode).

b) A search and retrieve function for LTA data products.

Observing will be in the LBA and in the HBA frequency ranges. 

Automatic observation and processing, using the 160 MHz clock will not yet be supported in LOFAR v1.0, meaning that routine observing between 190 MHz and 210 MHz will not be supported.

In Imaging mode observing with up to 8 independent beams will be supported.

In Beam Formed mode observing with up to 127 pencil beams will be supported.