Changes between Version 243 and Version 244 of AstroTechTalk

Timestamp:

22 Nov 2016, 11:31:07 (7 years ago)

Author:

Ralph Hofferbert

Comment:

--

AstroTechTalk

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 || '''28.10.2016''' || '''Santiago Barboza''' || '''The MICADO derotator and its test stand at           MPIA'''[[BR]]      [[BR]]The Multi-AO Imaging Camera for       Deep Observations (MICADO), a first light instrument for the 39m       European       Extremely Large Telescope (E-ELT), is being designed and optimized       to work with       the Multi-Conjugate Adaptive Optics (MCAO) module MAORY using       laser guide stars.       The MICADO-MAORY configuration will provide diffraction limited       imaging over a large       53arcsec field of view. [[BR]]     [[BR]]     The current concept of the       MICADO instrument consists of a structural cryostat (2.1m       diameter and 2m       height) with the wavefront sensor (WFS) on top (cryostat + WFS ≈       4.000kg). The cryostat is mounted via its central flange directly to a large 2.5m-diameter image derotator. The whole       assembly is       suspended above the E-ELT Nasmyth platform by a hexapod-type       support structure,       which is located underneath the MAORY bench.[[BR]]     [[BR]]     MPIA is responsible for the       design and development of the MICADO derotator, a key mechanism       that must precisely       rotate the cryostat assembly around its optical axis with a       differential       angular positioning accuracy lower than 10 arcsec, in order to       compensate       the field rotation due to the alt-azimuth mount of the E-ELT. This       device       consists of a high precision bearing, gear wheels, motors, encoders       and very stiff mechanical       interfaces. The MICADO derotator is being developed using a       custom-made high-precision       four-point contact ball bearing. [[BR]]     [[BR]]     With the intention of probing       the current concept of the derotator in an early phase of the       project, a       prototype has been built using a standard 1.2m-diameter bearing. The test campaign is about to start       during the next       days and we will figure out if the proposed concept is able to       reach the challenging       angular positioning accuracy and other key performance figures required by the MICADO instrument.[[BR]][[BR]]Presentation: English[[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-10-28_MICADODerot.pdf Slides: English][[BR]]Questions: German, English ||
 || '''04.11.2016 '''[[BR]]'''[[span(style=color: #FF0000, HdA-Auditorium!!)]]''' || '''Stefan Hippler''' || '''Adaptive optics for VLT and E-ELT'''[[BR]][[BR]]This talk summarizes in a very general approach the principles of adaptive optics (AO) and its value in the astronomical application. In part one, Stefan Hippler will specifically and phenomenologically describe how images are formed up during an observation through optical turbulence.  A brief historical summary highlighting the achieved experimental milestones will conclude this introduction. [[BR]][[BR]]In part two of the talk, the AO systems of the famous ESO observatories on Paranal (VLT) and Armazones (E-ELT) will be brought into focus. With NACO and CIAO, two examples of already running instruments will be described in detail. This also allows a foresight to the currently designed advanced systems for ESO's new flagship mission in the mid twenty-twenties.  [[BR]][[BR]]Presentation: German                  [[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-11-04_AOOverview_Part1.pdf Slides: English Part1] [https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-11-04_AOOverview_Part2.pdf Part2][[BR]]Questions: German, English ||
-|| '''11.11.2016 ''' || '''Vianak Naranjo''' || '''Characterization of Infrared Detectors - What is that?''' [[BR]][[BR]]Infrared instrumentation at MPIA is one of the major technical activities in house. It brings together the work of very different engineering areas, but for this talk the focus will be on the infrared detector and its characterization. What is this all about and why is it so important? An infrared detector cannot operate alone: as a complex unit of an infrared system the detector serves as a connection between the readout electronics and the software. The characterization process is the way of understanding how the detector works and how it behaves, and it is the key to guarantee the best performance of an instrument during operation. [[BR]][[BR]]If you have ever wondered what do the people working with infrared detectors do, please join us and find out! Everybody is welcome! [[BR]][[BR]]Presentation: German [[BR]]Slides: English [[BR]] Questions: German, English ||
+|| '''11.11.2016 ''' || '''Vianak Naranjo''' || '''Characterization of Infrared Detectors - What is that?''' [[BR]][[BR]]Infrared instrumentation at MPIA is one of the major technical activities in house. It brings together the work of very different engineering areas, but for this talk the focus will be on the infrared detector and its characterization. What is this all about and why is it so important? An infrared detector cannot operate alone: as a complex unit of an infrared system the detector serves as a connection between the readout electronics and the software. The characterization process is the way of understanding how the detector works and how it behaves, and it is the key to guarantee the best performance of an instrument during operation. [[BR]][[BR]]If you have ever wondered what do the people working with infrared detectors do, please join us and find out! Everybody is welcome! [[BR]][[BR]]Presentation: German [[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-11-11_IRDetectors.pdf Slides: English] [[BR]] Questions: German, English ||
 || '''18.11.2016''' || '''Sascha Douffet''' || '''Safety officers - Main actors and their tasks'''[[BR]][[BR]]The last  talk about occupational safety gave an overview, covering history,  structure, regulatory framework and tasks. Since the topic is very  complex, important questions are still to be answered about the main  actors and their tasks. [[BR]][[BR]]The following topics will be discussed  in the second part: Who are the main actors? What means "responsibility"  with respect to occupational safety? What are the main tasks? What may  happen, if responsibilities are not assumed and tasks are not fulfilled? [[BR]][[BR]]Every  employee should know, which functions and activities are implemented at  MPIA. Not only every colleague should know who is responsible for  occupational safety, also the responsible persons should know about  their tasks, such that those become a practical reality in the  day-to-day work. And hence, the risk for accidents is automatically  reduced. [[BR]][[BR]]Presentation: German                  [[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-11-18_Safety2.pdf Slides: German][[BR]]Questions: German, English ||
 || '''25.11.2016''' || '''Michael Boehm (ISYS, Stuttgart)''' || '''OVMS-plus: Disturbance compensation at the LBT'''[[BR]][[BR]]Interferometry at modern large ground-based telescopes often utilizes an array of telescopes. However, this is only possible if the length of the light path is equal for all telescopes, i.e. the optical path difference (OPD) has to be zero. Because the optical elements of the telescopes tend to vibrate due to wind excitation, for example, the OPD is usually oscillating with peak-to-peak amplitudes of several µm and frequencies up to 60Hz. Without proper active compensation, this would render most measurement attempts in the near-infrared (NIR), rather useless, since . Thus, large telescopes such as the Large Binocular Telescope (LBT) are equipped with a dedicated OPD and vibration monitoring system (OVMS) to be able to measure these disturbances and compensate for them in a fast feed-forward manner.[[BR]][[BR]]At the beginning of the talk Michael Boehm will briefly revisit the OVMS at the LBT and describe how the accelerometer readings can be used for disturbance compensation. The second part of the talk will present the new enhanced and centralized software architecture, called OVMS-plus, and illustrate several challenges faced during the implementation phase. [[BR]][[BR]]Finally, measurement results from LBTI proving the effectiveness of the approach and the ability to compensate for a large fraction of the telescope induced vibrations will be presented.[[BR]][[BR]]Presentation: German[[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-11-25_OVMSplus.pdf Slides: English][[BR]]Questions: German, English ||