Changes between Version 1 and Version 2 of OldPresentations2018S1

17 Sep 2018, 09:36:54 (5 years ago)
Ralph Hofferbert



  • OldPresentations2018S1

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     1||'''Date''' ||'''Speaker    ''' ||'''Topic''' ||
     2|| '''02.02.2018[[BR]](10hrs, HdA)''' || '''Joachim Wolf [[BR]](KIT-ETP)''' || '''KATRIN - the "Karlsruhe Tritium Neutrino Experiment"'''[[BR]][[BR]]Apart from photons, neutrinos  are the most abundant particles in the universe. Therefore even the small neutrino mass has an impact on the evolution of the visible universe. And also in particle physics the neutrino mass is an important parameter. The observation of neutrino oscillations confirmed for the very first time that neutrinos have a mass. But, those experiments only allow to measure the difference of squared mass values of the different neutrino generations, i.e. absolute mass values cannot be deduced. A model independent method to determine the neutrino mass is the precise measurement of the beta spectrum of a radioactive decay.[[BR]][[BR]]Goal of the KATRIN experiment, which is currently commissioned at the  "Karlsruher Institut für Technologie" (KIT), is the determination of the neutrino mass, more specifically, the effective mass of electron anti-neutrinos in the decay of molecular tritium gas. A finite neutrino mass would lead to a tiny change in the form of the beta spectrum at its kinematic endpoint of 18,6 keV, which has to be measured with high precision. Since only about 2 x 10^-13^  of all beta electrons possess an energy in the last eV below this endpoint, the source requires a high intensity. With a sensitivity of m,,n,, = 0.2 eV/c^2^, KATRIN will improve all previous limits of tritium measurements by a factor of 10.[[BR]][[BR]]The complete setup of the KATRIN experiment has a total length of 70 m and can be divided into two main areas: In the source and transport range the tritium decay is happening (~10^11^  Bq), the electrons are guided to the spectrometer range using super conducting magnets and the remaining tritium gas is pumped with such a high efficiency that only a fraction of less than 10^-14^  of the original amount of gas reaches the spectrometer. Finally, in this spectrometer and detector area the energy of the electrons is measured with highest precision. This happens in the main spectrometer with 10m of diameter and 23m of length, comprising an ultra-high vacuum of 10^-11^  mbar in a volume of 1240 m^3^. For the energy measurement the so-called MAC-E  filter technique is applied using an electrostatic high-pass filter, which only allows electrons above a certain voltage threshold to reach the detector, and finally getting counted.  The talk explains the measurement of the neutrino mass and the KATRIN experiment and discusses the technological and physical challenges.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     3|| 09.02.2018[[BR]](10hrs, HdA) || || ||
     4|| '''16.02.2018[[BR]](10hrs, HdA)''' || '''Robert Harris (ZAH-LSW)''' || '''Astrophotonics'''[[BR]][[BR]]The field of Astrophotonics bridges the gap between the small mass-produced devices manufactured for the telecommunications industry and large one-off astronomical instruments. [[BR]][[BR]]In this talk Robert Harris will summarise the developments in the field, the technologies that made this possible and some of the successes. He will examine where these technologies could be of use and some of the future devices which could be manufactured.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     5|| '''23.02.2018[[BR]](10hrs, HdA)''' || '''Ernest A. Michael (RAIG, University of Chile)''' || '''Fiber-based Heterodyne Infrared Interferometer: Towards a small  proof-of-principle Prototype at 1.55 µm '''[[BR]] [[BR]]Ernest Michael presents the concept for a comparatively inexpensive near-infrared  heterodyne interferometer based on commercial 1.55µm fiber components.  First lab results were obtained for the telescope to single-mode fiber  coupling control, LO phase-stabilization between both telescopes, and  the heterodyne correlation receiver system. He also discusses the  applicability of this concept for long-baseline, high telescope number  systems and mid-infrared wavelengths.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     6|| '''02.03.2018[[BR]](10hrs, HdA)''' || '''Gabriele Rodeghiero''' || '''Preliminary Design of the MICADO Calibration Assembly'''[[BR]][[BR]]This presentation will survey the preliminary design of the MICADO Calibration Assembly (MCA). MICADO is targeted to be one of the first light  instruments of the Extremely Large Telescope (ELT) and it will embrace  imaging, spectroscopic and astrometric capabilities including their  calibration. The astrometric requirements are particularly ambitious  aiming for 50 µas differential precision within a single epoch. After a  complete overview of the MCA subsystems, their functionalities, design  and status, particular emphasis will be placed on the ongoing efforts (both prototype testing and simulation) on the astrometric calibration  of the optical distortions of the instrument and the telescope.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     7|| '''09.03.2018[[BR]](11hrs, MPIA Hoersaal)''' || '''Joerg Wagner (ISD, University of Stuttgart)''' || '''J.G.F. Bohnenberger: [[BR]]Astronomer, Geodesist and Inventor of the Gyroscope'''[[BR]][[BR]]Johann Gottlieb Friedrich Bohnenberger (1765-1831) was a professor of physics, mathematics, and astronomy at the University of Tuebingen, the scientific head surveying officer of the early Kingdom of Wuerttemberg, and an important German astronomer of the 19th century. He made both major contributions to introducing modern geodesy in Germany and invented various physical instruments. The "Machine of Bohnenberger" is considered the first gyro with cardanic suspension and forms the precursor of Foucault’s Gyroscope of 1852. This presentation discusses this apparatus as well as the life and the scientific work of J.G.F. Bohnenberger.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     8|| '''16.03.2018[[BR]](11hrs, MPIA Hoersaal)''' || '''Klaus Meisenheimer''' || '''MATISSE — its Way to "First Light" and Beyond [[BR]]'''[[BR]]MATISSE is the next MIR instrument for ESO's VLT Interferometer. Seven European institutes are cooperating in this project since 2011. After the integration of the Dutch "cold optics" in the cryostats at MPIA and the delivery to OCA Nice end of 2014, MATISSE made a rather laborious rise to its Preliminary Acceptance Europe (PAE) in September 2017. After the arrival on Paranal end of October the integration and commissioning went smoothly and culminated in the coherent 4-telescope-observation of Sirius on February 19th. [[BR]][[BR]]Klaus  Meisenheimer will explain functionality and major advantages of MATISSE and he will recapitulate the developements up to "First Light". An outlook will highlight the fascinating scientific possibilities for MPIA and its partners from 2019 on. [[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     9|| '''23.03.2018'''[[BR]]'''(10hrs, HdA)''' || '''Peter Bizenberger''' || '''The ELT METIS Imager'''[[BR]][[BR]]MPIA is involved in the METIS project for the ELT. Two main work  packages are under responsibility of our institute, the adaptive optics control and the imager. In this presentation, Peter Bizenberger introduces the imager: the functionality, the role within METIS, but also how we design, built  and test this part of the instrument. [[BR]][[BR]]Beside presenting the instrumental side, i.e. designing an instrument for the ELT, he will also highlight how this task is achieved within a European  consortium. Here also the managerial side is addressed.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     10|| 30.03.2018 || -- || Good Friday ||
     11|| 06.04.2018 || -- || Easter break ||
     12|| '''13.04.2018[[BR]](11hrs, MPIA Hoersaal)''' || '''José Crespo[[BR]](MPIK, Heidelberg)'''[[BR]] || '''How to make, trap and observe microscopic star plasmas in the laboratory, and use them as clocks'''[[BR]]       [[BR]]       Some of us will certainly remember José Crespo's enthusiasm for the technical sophistications employed in fundamental  research, which we experienced when he gave us a noteworthy lab tour during the visit of our technical departments to  MPIK last October. We have invited him to the AstroTechTalk in order to tie in with this experience.[[BR]]       [[BR]]       __His topic:__[[BR]]       Electron beam ion traps make it possible to create and trap   stationary plasmas of microscopic size capable of achieving in the lab the most extreme temperature conditions prevalent in atomic matter in the universe. The composition and the   production of defined types of radiation (the "excitation    conditions") can be controlled very precisely. This way very  precise experimental data are obtained that drive the theory. MPIK Heidelberg has developed the worldwide largest collection of such apparatus. Using a variety of spectrometers the characteristics of astrophysical plasmas can be studied in detail.[[BR]]       [[BR]]       Furthermore, highly charged ions have been proposed as pulse generators for the next generation of optical atomic clocks. MPIK is collaborating with the Physikalisch-Technische Bundesanstalt to create such clocks, which will perform time measurements with a precision of more than 19 decimal points.[[BR]][[BR]]       __Background:__[[BR]]       Some stars contain plasmas with temperatures of several    hundred million degrees. At its core, our Sun has a temperature of 15.7 million degrees, and its corona is     about 2 million degrees hot. In supernova explosions, X-ray binary systems and active galactic nuclei that surround black holes even higher temperatures occur. In this kind of environment atoms are very highly ionized and posses just a few bound electrons. The signals emitted by these ions range  from X-rays to the visible spectral region and are essential for astrophysical diagnostics.[[BR]][[BR]]       Concerning the atomic clocks with their targeted precision,   they will be used to address the fundamental question whether the constants of nature are stable.[[BR]]       [[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     13|| '''20.04.2018 [[span(style=color: #FF0000, (10:30Uhr, Seminarroom) )]]''' || '''Peter Bizenberger''' || '''Slide-Show:[[BR]]Life at LBT - how it actually is [[BR]] '''[[BR]]A few impressions about the work and the daily routine at the LBT. How to get there, what you can do and what you are supposed to do, how it looks there and all around. Many pictures, but no instruments and no astronomy, only the day-to-day survival. [[BR]]Presented basically for those, who haven't made the experience yet, and to describe how a business trip to LBT typically looks like. And certainly for those, who know it and enjoyed it already. [[BR]] [[BR]]Lots of photos - no text[[BR]] [[BR]]Language: German ||
     14|| 27.04.2018 || || ||
     15|| 04.05.2018 || || ||
     16|| 11.05.2018 || -- || Bridge day after Ascension Day ||
     17|| 18.05.2018 || || ||
     18|| 25.05.2018 || -- || Pentecost holidays ||
     19|| 01.06.2018 || -- || Pentecost holidays ||
     20|| '''08.06.2018 [[BR]](11hrs, MPIA Hoersaal)''' || '''Jacopo Farinato (INAF-Padova)''' || '''SHARK-NIR, the coronographic camera for the LBT, [[BR]]is currently under construction'''[[BR]][[BR]]SHARK-NIR is a second generation instrument for the LBT, consisting essentially of a coronagraphic camera which can provide direct imaging, coronagraphic imaging, low resolution spectroscopy and dual band imaging in Y, J and H bands over a FoV of 18"x18". The main science driver for the instrument is planet finding and characterization. Since the very good sensitivity of the LBT AO system allows to use very faint stars for the WFS, other science cases are possible as well. This includes the study of the morphological properties of jets and disks around stars or the characterization of AGN and of the brightest quasars in our galaxy.[[BR]][[BR]]The instrument consortium is composed of INAF, MPIA and Steward Observatory. SHARK-NIR has been approved for construction in July 2017, and a status update of the instrument, which is now entering the AIV phase, will be given.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     21|| '''06.07.2018 [[BR]](11hrs, MPIA Hoersaal)''' || '''Julio Rodríguez (IAA)''' || '''From Granada to Mars and the Stars'''[[BR]][[BR]]Join us in this exciting trip!  The speaker will take this opportunitiy to explain the technical participation of the IAA (Instituto de Astrofísica de Andalucía) in the space missions !ExoMars-TGO and PLATO.  In particular, he will highlight the design aspects of the instrument NOMAD, onboard !ExoMars-TGO, and MEU (Main Electronics Units of PLATO).  MEU and SINBAD (onboard software for NOMAD) are both under his responsability as project manager.[[BR]][[BR]]Presentation: English[[BR]]Slides: English[[BR]]Questions: English ||