Project Support

Project Support

The ARGOS projects will equip the LBT, the Large Binocular Telescope, with an up to date laser guide star and wavefront sensing facility. ARGOS will utilize multiple pulsed lasers to generate artificial guide stars. A total of six laser guide stars will be used to correct the ground layer turbulence above each of the LBT mirrors. The primary goal of the facility is to correct the atmospheric turbulence induced distortions, thus enhancing the imaging and spectroscopic capabilities for LUCI over a wide field of view
The electronic group is responsible for the system elektronics.

ARGOS

The ARGOS projects will equip the LBT, the Large Binocular Telescope, with an up to date laser guide star and wavefront sensing facility. ARGOS will utilize multiple pulsed lasers to generate artificial guide stars. A total of six laser guide stars will be used to correct the ground layer turbulence above each of the LBT mirrors. The primary goal of the facility is to correct the atmospheric turbulence induced distortions, thus enhancing the imaging and spectroscopic capabilities for LUCI over a wide field of view


The electronic group is responsible for the system elektronics.

Our electronics group is responsible for planning, developing, manufacturing and testing of the onboard-electronic, which deals with controlling and processing the data from the 7 CCD cameras, and the thermal control of the cameras and the mirror modules.

eROSITA

Our electronics group is responsible for planning, developing, manufacturing and testing of the onboard-electronic, which deals with controlling and processing the data from the 7 CCD cameras, and the thermal control of the cameras and the mirror modules.

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GRAVITY is the second-generation VLTI instrument for precision narrow-angle astrometry and interferometric imaging. It will bring the most advanced vision to the VLT: with its fiber-fed integrated optics, wavefront sensors, fringe tracker, beam stabilization, and a novel metrology concept, GRAVITY will push the sensitivity and accuracy far beyond what is offered today. 
In this project the electronics group is responsible for the control system of the beam positioning as well as the temperature stabilization, the reading electronics for cameras and detectors, the electrical supply and communication between devices and processors.

GRAVITY

GRAVITY is the second-generation VLTI instrument for precision narrow-angle astrometry and interferometric imaging. It will bring the most advanced vision to the VLT: with its fiber-fed integrated optics, wavefront sensors, fringe tracker, beam stabilization, and a novel metrology concept, GRAVITY will push the sensitivity and accuracy far beyond what is offered today.

In this project the electronics group is responsible for the control system of the beam positioning as well as the temperature stabilization, the reading electronics for cameras and detectors, the electrical supply and communication between devices and processors.

GROND is an imaging instrument to investigate Gamma-ray Burst Afterglows and other transients simultaneously in seven filter bands. Several dichroic beamsplitters feed light into three NIR channels and four visual channels, each equipped with its own detector. GROND is mounted at the MPI/ESO 2.2m telescope on La Silla (Chile), and is operational since 2007.
The electronics group developed and manufactured the complete control electronics for all components and process controlled temperature stabilisation and the monitoring electronics for probable disturbances.

GROND

GROND is an imaging instrument to investigate Gamma-ray Burst Afterglows and other transients simultaneously in seven filter bands. Several dichroic beamsplitters feed light into three NIR channels and four visual channels, each equipped with its own detector. GROND is mounted at the MPI/ESO 2.2m telescope on La Silla (Chile), and is operational since 2007.

The electronics group developed and manufactured the complete control electronics for all components and process controlled temperature stabilisation and the monitoring electronics for probable disturbances.

LUCI is built by a German consortium led by the Landessternwarte in Heidelberg. MPE contributes the multi-object spectrograph unit  that handles the slit masks for LUCI1 and LUCI2. The unit was developed, integrated, and testet at MPE. In addition, MPE was involved in the fabrication of the LBT hardpoints. The hardpoints are extremely stiff variable length actuators, six of which are used to control the position in space of each of the LBT primaries.
The electronics group developed the control and monitoring electronics.

LUCI

LUCI is built by a German consortium led by the Landessternwarte in Heidelberg. MPE contributes the multi-object spectrograph unit  that handles the slit masks for LUCI1 and LUCI2. The unit was developed, integrated, and testet at MPE. In addition, MPE was involved in the fabrication of the LBT hardpoints. The hardpoints are extremely stiff variable length actuators, six of which are used to control the position in space of each of the LBT primaries.

The electronics group developed the control and monitoring electronics.

OPTIMA is a high-speed photoncounter which is used to measure (Gamma-ray) interesting objects, especially pulsars with high time resolution (10-6 s.) and high sensitivity.Meanwhile it is used to observe also other rapid variable objects (e.g. Cataclysmic Variables or Gamma Ray Burst afterglows) from observatories world wide.  OPTIMA is mobile and can be used at a variety of telescopes.
The electronics group is responsible fort he processing oft he counter signals and the recording electronics. As FEE (front-end electronics) charge sensitive amplifiers (A 250) were used.

OPTIMA

OPTIMA is a high-speed photoncounter which is used to measure (Gamma-ray) interesting objects, especially pulsars with high time resolution (10-6 s.) and high sensitivity.Meanwhile it is used to observe also other rapid variable objects (e.g. Cataclysmic Variables or Gamma Ray Burst afterglows) from observatories world wide.  OPTIMA is mobile and can be used at a variety of telescopes.

The electronics group is responsible fort he processing oft he counter signals and the recording electronics. As FEE (front-end electronics) charge sensitive amplifiers (A 250) were used.

Plasmakristallexperiment 4 (PK-4)




last change 2014-09-23 by J. Zanker-Smith

 
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