Changes between Version 1 and Version 2 of OldPresentations2017S2

8 Jan 2018, 09:36:11 (6 years ago)
Ralph Hofferbert



  • OldPresentations2017S2

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     1||'''Date''' ||'''Speaker    ''' ||'''Topic''' ||
     2|| 22.09.2017[[BR]](10hrs, HdA) || || First talk after the summer break ||
     3|| '''29.09.2017[[BR]](10hrs, HdA)''' || '''Theodoros Anagnos     (ZAH, LSW)''' || '''Simulation and Optimization of an Astrophotonic Reformatter [[BR]] '''[[BR]]Image  slicing is a powerful technique in astronomy. It allows the  instrument  designer to reduce the angular slit width of the  spectrograph,  increasing spectral resolving power, whilst retaining  throughput.  Conventionally this is done using bulk optics, such as  mirrors and  prisms, however more recently astro-photonic components known  as  photonic lanterns and photonic reformatters have also been used. [[BR]] [[BR]]These  devices reformat the multimode input light from a telescope into   single mode outputs, which can then be re-arranged to suit the   spectrograph. The photonic dicer is one such device, an integrated   photonic reformatter (image slicer) designed to reduce the dependence of   spectrograph size on telescope aperture and eliminate "modal noise". [[BR]] [[BR]]In  this talk Theodoros Anagnos will describe his work simulating the  photonic dicer by using both an adaptive optics simulator and a beam  propagation software. He will show the combined results and compare them  to on-sky data. Furthermore, he will show optimisations to the design  of the device, improving  throughput and making it more compact.  Finally, the  significance of these findings in terms of future designs  of devices will be discussed,  including their influence on adaptive  optics instruments.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     4|| '''06.10.2017[[BR]](10hrs, HdA)''' || '''Julien Milli (ESO)''' || '''Current performance and future prospects [[BR]]of the extreme-AO instrument SPHERE [[BR]]after 3 years of operations on Paranal'''[[BR]][[BR]]SPHERE  is the high-contrast exoplanet imager at the VLT. After more than  2  years of regular operations, we will review the performance of the   infrared channel. A specific emphasis will be put on the dependence of   the performance of the  AO system with the atmospheric conditions  encountered at the Paranal  observatory, as measured by the suite of  dedicated instruments which are part of  the astronomical site monitor  and as seen by the SPHERE real-time  calculator. We will detail how this  information can be  used to plan the observations, and to guide the  astronomer when  processing his/her data. [[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     5|| 13.10.2017 || -- || No talk (MPIA Science Day) ||
     6|| 20.10.2017 (10hrs, HdA) || || ||
     7|| '''27.10.2017[[BR]](10:30hrs, HdA)''' || '''Nicolas Baroan (NIT)''' || '''Novel Scientific high dynamic range SWIR camera: technology, capabilities and application in astronomy'''[[BR]][[BR]]High Dynamic Range is being widely adopted in different markets, like automotive, Industrial machine vision, defense…[[BR]][[BR]]Scientific  cameras, usually driven by low light performances and extended  Wavelength spectral response, is now considered also as a potential  “consumer” of these emerging extended dynamic range devices.[[BR]][[BR]]Developed  with its patented High Dynamic Range Pixel structure and with the LPA  expertise in optronics ( i.e. : Laboratoire Pierre Aigrain – Ecole  Nationale Supérieure ), NIT and LPA will present the first scientific  Short Wave Infrared High dynamic Range camera.[[BR]][[BR]]The deep cooled  camera performances and features will be illustrated through an  interesting astronomy application case made at the “Pic du Midy”  Observatory at the top of the French Pyrenees.[[BR]][[BR]]A comparison with a state of the art cooled !InGaAs camera, in similar conditions, will briefly be described.[[BR]][[BR]]Presentation: English[[BR]]Slides: English[[BR]]Questions: English ||
     8|| 03.11.2017[[BR]](10hrs, HdA) || || ||
     9|| '''10.11.2017[[BR]](11hrs, MPIA lecture hall)''' || '''Wolfgang Gaessler''' || '''4MOST - An Update'''[[BR]][[BR]]The  4MOST project upgrades the 4m VISTA  telescope on Paranal to a  spectroscopic facility. Two low resolution  spectrographs (R ~ 5000) and  one high resolution spectrograph (R ~  20000) are fed with light from  2400 fibers. [[BR]][[BR]]In the first 10  years of operation, 4MOST will  serve 11 surveys of the responsible  consortium. In addition, whole  community surveys are planned to observe  nearly everything on sky  (except for exoplanets): individual stars in  the Milky Way galaxy and  in the Magellanic Clouds, AGN, supernovae and  their hosts, quasars,  LRGs, ELGs, and galaxy clusters. [[BR]][[BR]]Wolfgang Gaessler will give a project update and will explain interesting technical features in more detail.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     10|| '''17.11.2017[[BR]](10hrs, HdA)''' || '''Hans J. Kaercher  (MT Mechatronics GmbH)''' || '''Thinking in Forces [[BR]](as a Tool for designing Telescope Structures)'''[[BR]][[BR]]What  is a force? One can start reflecting about it and philosophers have  written whole books about this question. Ludwig Buechner, a   „middle-class materialist“ of the 19th century wrote in his book „Kraft  und Stoff“: „Kraft kann nichts weiter sein als eine  Eigenschaft der  Materie“, or „Kräfte lassen sich nicht mitteilen,  sondern nur wecken“,  and in this sense he is obviously with Isaac Newton, who is the  originator of "thinking in forces" following his famous observation of  the falling apple. Much later this led to the special engineering branch  "structural mechanics", which was originally applied to bridge and  building construction, lateron even in the more sophisticated branch of  aerospace engineering.[[BR]][[BR]]„Thinking in forces“ in the form of  "graphical structural analysis" became a branch of engineering in the  middle of the 19th century. This enables to think in both the "physical  space" and the "force space", i.e. besides a design drawing also a force  diagram is required. This is similar to projective geometry, where also  dual spaces exist. Hans Kaercher will explain this approach in three  examples:[[BR]]1) designing reflectors for radio telescopes;[[BR]]2) designing primary mirror supports for large optical telescopes;[[BR]]3) designing tracking mounts for large optical elements.[[BR]]These  examples will be discussed in the framework of design contributions to  different telescope projects, like e.g. the radio telescope LMT/GTM, the  IR telescope SOFIA and the optical telescope ELT.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     11|| 24.11.2017[[BR]](10hrs, HdA) || || ||
     12|| '''01.12.2017[[BR]](10hrs, HdA)''' || '''Thomas Henning''' || '''Perspectives in Astronomy'''[[BR]][[BR]]The  talk will discuss the new and currently investigated U.S. initiatives  for large space missions. In this context a special focus will be set  onto the characterization of extrasolar planets. [[BR]][[BR]]Presentation: German[[BR]][ Slides: German][[BR]]Questions: German, English ||
     13|| '''08.12.2017[[BR]](10hrs, HdA)''' || '''Philipp Hottinger (ZAH, LSW)''' || '''3D-printed         microlens-array as tip-tilt sensor[[BR]]'''[[BR]]In          this talk Philipp Hottinger introduces the possibility to use a  microlens-array         (MLA)         as tip-tilt sensor device with  integrated single mode fiber         coupling.         A first prototype  has been presented by Dietrich & Harris et         al.          (2017) and is directly printed onto a multi-core fiber          consisting of         7 single mode cores. [[BR]][[BR]]Philipp Hottinger  will present his ongoing work on further         development         of  this device. This includes characterization, modeling and         on-sky          requirements for upcoming testing at the iLocater spectrograph          at         the LBT.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     14|| '''15.12.2017[[BR]](10hrs, HdA)''' || '''Olivier Absil (Université de Liège)''' || '''Five years of harvest with the vortex coronagraph[[BR]]'''[[BR]]While  the concept of vortex coronagraphy dates back to 2005, the first  science-grade Annular Groove Phase Masks (AGPM), working in the thermal  infrared regime, have been installed at the VLT only in 2012. They are  now also equipping the Keck telescope and the Large Binocular Telescope,  and will soon be at the core of more ground-based high-contrast imaging  instruments. [[BR]][[BR]]In this talk, Olivier Absil will shortly review  the technology development undertaken over the last 10 years, and  describe the on-sky operations and performance of the vortex  coronagraph. He will then present the main scientific results obtained  since 2012, and explain how his team has recently adapted deep learning  techniques to the problem of post-processing in high-contrast imaging.  He will finally discuss the perspectives with new instruments, including  the Breakthrough Watch project.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English Part1] [ Part2][[BR]]Questions: German, English ||
     15|| 22.12.2017[[BR]](10hrs, HdA) || || Last talk before the Christmas break ||