The NOVA-OIR group is hosted by ASTRON in Dwingeloo and is specialised in the development of infrared opto-mechanical cryogenic systems.

The NOVA Optical Infrared Astronomical Instrumentation Group develops systems and subsystems for the most advanced optical and infrared telescopes in the world and in space. This includes all development stages: from generation of novel ideas and technologies, to the use of the latest standards in design and manufacturing, and ensuring top quality by rigorous integration and testing.

NOVA is a major supplier of scientific instruments for the European Southern Observatory (ESO) Very Large Telescope (VTL), with instruments like: MATISSE, SPHERE, X-shooter, VISIR, SINFONI, MIDI. Instruments for the Isaac Newton Group (ING) at La Palma include: Wyffos, WEAVE and HARPS3. Telescope developments include: Meerlicht and the BlackGEM telescope array at ESO La Silla. We also develop space instrumentation, of which the most notably is the Mid InfraRed Instrument MIRI for the James Webb Space Telescope (NASA ESA JWST).

Our focus for the coming period is to develop instruments for the Extremely Large Telescope (ESO ELT). This includes the thermal infrared instrument METIS, a global collaboration where NOVA is the Primary Investigator institute. Other developments are: MICADO, MOSAIC and EPICS. With these instruments at the ELT, NOVA tries to solve the riddles of the universe: investigate the formation of stars and galaxies, determine properties of dark matter and dark energy, and characterize atmospheres of exoplanets.

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Daily image of the week

On June 13-17, the LOFAR Family Meeting took place in Cologne. After two years LOFAR researchers could finally meet in person again. The meeting brings together LOFAR users and researchers to share new scientific results.

Our renewed ‘Melkwegpad’ (Milky Way Path) is finished! The new signs have texts in Dutch on the one side and in English on the other side. The signs concerning planets have a small, 3D printed model of that planet in their centre.
#Melkwegpad @RTVDrenthe

Daily image of the week

The background drawing shows how the subband correlator calculates the array correlation matrix. In the upper left the 4 UniBoard2s we used. The two ACM plots in the picture show that the phase differences of the visibilities vary from 0 to 360 degrees.

Daily image of the week: Testing with the Dwingeloo Test Station (DTS)
One of the key specifications of LOFAR2.0 is measuring using the low- and the highband antenna at the same time. For this measurement we used 9 lowband antenna and 3 HBA tiles.