PRIMA instrument sees first light
September 24, 2008--The Phase Referenced Imaging and Microarcsecond Astrometry (PRIMA) instrument of the ESO Very Large Telescope Interferometer (VLTI) has seen "first light" at its new home atop Cerro Paranal in Chile.
September 24, 2008--The Phase Referenced Imaging and Microarcsecond Astrometry (PRIMA) instrument of the ESO Very Large Telescope Interferometer (VLTI) has seen "first light" at its new home atop Cerro Paranal in Chile. When fully operational, PRIMA will boost the capabilities of the VLTI to see sources much fainter than any previous interferometers. PRIMA will be used for the detection of exoplanets.
"PRIMA is specifically designed to see if one star 'wobbles' to and fro because it is has unseen planetary companions," says instrument scientist Gerard van Belle. "This allows us to not only detect exoplanets, but to measure their mass." PRIMA's expected astrometric precision of about 10-5 arcsec is unmatched by any other existing astronomical facility, whether on the ground or in orbit. In addition to taking astrometric measurements, PRIMA will be key to the imaging of faint sources with the VLTI using the Mid-Infrared Interferometer (MIDI) and the Astronomical Multiple Beam Recombiner (AMBER).
Using interferometry, PRIMA can pick out details as sharply as a single telescope with a diameter equivalent to the largest distance between the telescopes. For the VLTI, the distance between the two telescope elements is about 200 m.
The PRIMA instrument is unique among the VLTI instruments in that it is effectively two interferometers in one. PRIMA will take data from two sources on the sky simultaneously: the brighter source can be used for tracking, allowing the interferometer to "stare" at the fainter source for longer than is now possible with conventional interferometers. Although there have been earlier pathfinder experiments to test this technique, PRIMA represents the first facility-class instrument of its kind that is open to all astronomers.
PRIMA parts arrived at the summit at Paranal at the end of July and were integrated and tested during the following month. On September 2, 2008, as a first milestone, starlight from two VLTI 1.8 m auxiliary telescopes was fed into the PRIMA system and interference fringes detected on PRIMA's Fringe Sensor Unit. Three days later the system was routinely using active tracking on the fringes, compensating for atmospheric turbulence.
First light (or, in the case of interferometric instruments, first fringes) actually occurred ahead of the ambitious schedule set out by lead engineer Francoise Delplancke. "There were many activities that all had to be successful simultaneously for this to happen, but the assembly, integration, and verification went smoothly--I was pleased by how easy and reliable the fringe tracking was, for our first try," he said.
All PRIMA subsystems have been installed successfully for use with two auxiliary telescopes and will now be submitted to intensive commissioning tests before being offered to the community of users for routine observations.