Changes between Version 1 and Version 2 of OldPresentations2016S2

21 Dec 2016, 09:23:49 (7 years ago)
Ralph Hofferbert



  • OldPresentations2016S2

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     1||'''Date''' ||'''Speaker    ''' ||'''Topic''' ||
     2|| '''16.09.2016''' || '''Michael Biermann (ARI)''' || '''GAIA as seen by a First Look Scientist[[BR]]'''[[BR]]As  a daily routine, the Gaia First Look Scientists evaluate the quality of  the scientific data and check the status of the Gaia instruments. In  this talk a few examples out of the pool of findings by the Gaia First  Look Scientists  will be presented and discussed. This should -on the  one hand side- highlight the capability of this highly accurate  astrometry mission, but -on the other hand side- also demonstrate the  problems of the related data analysis work. [[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English][[BR]]Questions: German, English ||
     3|| '''23.09.2016''' || '''Anna Boehle (UCLA)''' || '''Upgrade of the detector in the integral field spectrograph OSIRIS[[BR]]'''[[BR]]OSIRIS  is a near-infrared  (1 - 2.5 microns) integral field spectrograph (IFS)  on the Keck I  10-meter telescope in Hawaii.  This adaptive-optics-fed  instrument uses  an array of small lenses to sample a rectangular  section of the focal  plane, producing up to 3,000 spectra  simultaneously with a spectral  resolution of ~3,800 and  diffraction-limited spatial resolution.  The  unique capabilities of  this IFS have allowed it to contribute to a  variety of science programs  since its commissioning in 2005, such as  characterizing the  atmospheres of extrasolar planets and tracing the  motions of gas and  stars at the centers of the Milky Way and other  galaxies.[[BR]][[BR]]In  January 2016, the detector in OSIRIS was upgraded from the original  Rockwell Hawaii-2 to a Teledyne Hawaii-2RG with lower read noise, lower  dark current, and higher quantum efficiency.  In  addition to the  upgraded detector, the detector head was also mounted  on a linear  stage, allowing the position of the detector to be  accurately adjusted  along the optical path when the instrument is at  cryogenic temperatures  (~80 K).  This linear stage greatly reduced the  number of cool downs  required to put the detector image plane at the  spectrograph camera  focus and adjust any residual tip/tilt of the  detector image plane.  [[BR]][[BR]]In  this talk, Anna Boehle will give a brief overview of  integral field  spectroscopy and its advantages and challenges and also  present the  details and the results of the upgrade of the OSIRIS detector.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     4|| '''30.09.2016''' || '''Martin Kuerster''' || '''A special planet on our cosmic doorstep:  Proxima Centauri b'''[[BR]][[BR]]The  recent discovery of a potentially Earth-like planet around our nearest  stellar neighbour Proxima Centauri has made a splash. In this talk  Martin Kürster will tell us how this discovery was made, why it is  special, and how the study of this planet is supposed to continue.[[BR]][[BR]]The  talk will be widely understandable as the speaker would like to reach  all interested colleagues at the institute. After all, each of us  contribute our share to making these amazing scientific results  possible.[[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English][[BR]]Questions: German, English ||
     5|| '''07.10.2016''' || '''Silvia Scheithauer''' || '''CIAO - Wavefront sensors for GRAVITY[[BR]]'''[[BR]]GRAVITY   is a near-infrared instrument for the Very Large Telescope    Interferometer (VLTI) at the ESO Paranal observatory in Chile. GRAVITY   combines the light of all four 8,2m telescopes to mimic a virtual 130m  telescope. The thereby possible, drastically increased sensitivity and  resolution, however, can only be reached, if the image blur due to  atmospheric turbulence above every single telescope is corrected by the  real-time deformable mirrors of an adaptive optics system.  Hence,  GRAVITY has to provide not only the „Beam Combiner Instrument“ (BCI) in  the VLTI-lab, but also four infrared wavefront sensors to analyze the  atmospheric turbulence. These wavefront sensors are located in the four   Coudé-rooms of the telescopes, therefore called „Coudé Infrared   Adaptive Optics“ (CIAO). [[BR]][[BR]]The CIAO wavefront sensors were built  under the responsibility of MPIA in close cooperation with ESO and the  MPE-led GRAVITY consortium. While the BCI has been installed already in  October 2015 on Paranal, the assembly of the four CIAO systems lasted  from February to September 2016. Currently, the scientific commissioning  of the complete GRAVITY instrument is ongoing.[[BR]][[BR]]One important  scientific goal is the observation of objects in the direct vicinity of  the black hole in the center of our Milky Way. In addition, GRAVITY will  allow to study young stellar objects and shaped-up stars with an  unprecedented sensitivity. In spring 2017, when the galactic center is  again observable from Paranal, observations of the star „S2“ will start.  The close fly-by of this star relative to the black hole will allow to  test Einstein's general theory of relativity with an extreme accuracy.  [[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English][[BR]]Questions: German, English ||
     6|| '''14.10.2016''' || '''Claudia Reinlein (Fraunhofer IOF, Jena)''' || '''Active and Adaptive Optics at the Fraunhofer IOF'''[[BR]][[BR]]Active  and Adaptive Optics is more and more used in ground-based telescopes  and also in discussion for space telescopes. For both types of systems  there are completely different technological requirements. While space  telescopes mainly aim for active optics, ground-based systems apply both  active and adaptive optics.[[BR]][[BR]]This talk describes the  technological features and the state of the art of "deformable mirrors /  AO systems". And here the focus will be set onto research and  development projects of the Fraunhofer IOF (Jena).[[BR]][[BR]]In the  framework of an ESA project, a test breadboard is developed, in order to  demonstrate the capability to compensate for static aberrations in  using active mirrors in space telescopes. In the future, telescopes with  a diameter of 4-16m will be used for the search for extraterrestrial  life. In this context, IOF develops and investigates an active mirror  with "set-and-forget" characteristics to compensate for aberrations  conditional of manufacture and assembly. [[BR]][[BR]]For the European  Extremely Large Telescope  (E-ELT) a technology development for extreme  AO (X-AO)  is conducted. In this context, the talk will inform about a  technological pre-investigation (design) of a deformable mirror with  11000 actuators.  [[BR]][[BR]]For laser communication between a  ground-station and a geostationary satellite, the pre-compensation of  aberrations is a technique to increase the signal intensity at the  receiver and to attenuate disturbing speckles. The talk will also  present the real-time AO of the Fraunhofer IOF and its compensatory  efficiency as a function of the correction angle.[[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English][[BR]]Questions: German, English ||
     7|| '''21.10.2016 '''[[BR]]'''[[span(style=color: #FF0000, HdA-Auditorium!!)]]''' || '''Eike Guenther + Michael Pluto (TLS, Tautenburg)''' || '''Instrumentation projects of the [[BR]]Thüringer Landessternwarte''' '''Tautenburg '''[[BR]][[BR]]The  Thüringer Landessternwarte (TLS) operates a 2m Alfred-Jensch telescope  and a LOFAR radio telescope in Tautenburg and is involved in a number of  instrumentation projects for various telescopes. In this talk the  instrumentation of the telescopes in Tautenburg and other projects are  reviewed. [[BR]][[BR]]Although the Alfred-Jensch telescope was built more  than 50 years ago, it is continuously upgraded with new instrumentation.  Currently in use are a high-resolution Echelle spectrograph, which is  used for exoplanet-research, and a low-resolution faint-object  spectrograph. Additionally, there is also a CCD camera in the  prime-focus, which is used for imaging. Building on the experience with  these instruments the TLS also participated in a number of international  instrumentation projects. The first one was GROND, a multi-channel  camera for the ESO/MPG 2.2m telescope at La Silla. Others were the  HERMES spectrograph for the Mercator telescope in La Palma and the two  calibration units for CARMENES. Still ongoing is the upgrade of CRIRES  to CRIRES+, which is a high-resolution NIR spectrograph for the VLT.  Being studied is GTI, a multi-channel camera that is specifically  designed for the follow-up observations of exoplanet candidates of TESS  and PLATO. [[BR]][[BR]]The TLS also hosts a LOFAR station. LOFAR is the  Low-Frequency Array, an instrument for performing radio astronomy in the  wavelength range from 1.2 to about 10 m. It is being built by ASTRON,  the Netherlands Institute for Radio Astronomy and its international  partners, and operated by ASTRON's radio observatory of the Netherlands  Organisation for Scientific Research. About 40 stations are located in  the Netherlands, additional ones are in Great Britain, France, Sweden,  and Germany.[[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English Part1] [ Part2][[BR]]Questions: German, English ||
     8|| '''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]][ Slides: English][[BR]]Questions: German, English ||
     9|| '''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]][ Slides: English Part1] [ Part2][[BR]]Questions: German, English ||
     10|| '''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|| '''18.11.2016[[BR]][[span(style=color: #FF0000, HdA-Auditorium!!)]]''' || '''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]][ Slides: German][[BR]]Questions: German, English ||
     12|| '''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]][ Slides: English][[BR]]Questions: German, English ||
     13|| 02.12.2016 || || ||
     14|| '''09.12.2016[[BR]][[span(style=color: #FF0000, HdA-Auditorium!!)]]''' || '''Thomas Henning''' || '''Astronomy in Heidelberg - [[BR]]From the Koenigstuhl into the World'''[[BR]][[BR]]In  this talk, Thomas Henning will give his personal view of the  development of instruments at MPIA using specific examples. Some  important discoveries in the field of planet formation and exoplanets,  which were achieved with these instruments, will be highlighted in the  talk. [[BR]][[BR]]Presentation: German                  [[BR]][ Slides: German][[BR]]Questions: German, English ||
     15|| 16.12.2016 || || ||
     16|| 23.12.2016 || -- || Christmas break ||