Changes between Version 1 and Version 2 of OldPresentations2017S1

26 Jul 2017, 09:32:54 (6 years ago)
Ralph Hofferbert



  • OldPresentations2017S1

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     1||'''Date''' ||'''Speaker''' ||'''Topic''' ||
     2|| 06.01.2017 || -- || Christmas break ||
     3|| '''13.01.2017''' || '''Philipp Dietrich (KIT)''' || '''Printed Micro-Optics and More[[BR]][[BR]]'''3D-micro-printing  based on two-photon-absorption allows to manufacture  free-form-structures of an arbitrary shape. The particular of this  method is the creation of the desired structure at the very location of  its later application. A subsequent positioning is not required, i.e. a  perfect alignment is possible. [[BR]][[BR]]Only in this way, 200nm silicon  waveguides can be linked via 3d-printed free-form-waveguides  („photonic-wirebonds“), which solves fundamental problems of integrated  optics. Other options result from the capability to print  free-form-lenses onto facets of optical components -like optical  fibers-, whereby light is coupled much more efficiently into such  fibers. But applications are not restricted to optics alone: Even the  needle of a scanning-force-microscope is printable, such that each probe  gets its optimal scanning head. [[BR]][[BR]]Philipp Dietrich's talk will focus on optical devices, but will also highlight possible applications for astronomy.[[BR]][[BR]]Presentation: German                  [[BR]][ Slides: English][[BR]]Questions: German, English ||
     4|| 20.01.2017 || || ||
     5|| '''27.01.2017''' || '''Mathias Voss''' || '''Presentation of Construction Projects at MPIA [[BR]](All-Institute-Meeting)[[BR]][[BR]]'''Invitation and abstract will be distributed by the speaker himself. ||
     6|| '''03.02.2017''' || '''Domenico Bonaccini Calia   (ESO)''' || '''Laser Guide           Star Systems: [[BR]]ESO LGS Facilities and Technology R&D[[BR]]'''[[BR]]In  this           talk Domenico Bonaccini Calia will review the current  LGS facilities on UT4 and present the resuts of the commissioning at the  VLT of the Four Laser Guide Star Facility, which is           part of  the new Adaptive Optics Facility on the UT4 telescope of the VLT at  Cerro Paranal. [[BR]][[BR]]The main experimental results will be presented  and compared with the requirements. In addition, a report on the  activities in the area of the LGS systems R&D will be given. These  are being done in collaboration with the AO community in the ESO member            states, where currently two of in total four tasks have been  completed.[[BR]][[BR]]Domenico Bonaccini Calia will           also report on  the systematic measurement of the LGS return fluxes and on the LGS-AO  loop results obtained with largely elongated LGS, similar to those  foreseen for the EELT configuration. An outlook on the future, approved  R&D will also be given.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     7|| '''10.02.2017''' || '''Dr. Felipe Guzmán (DLR)''' || '''Laser measurement science in gravitational physics'''[[BR]][[BR]]Coherent  light enables length measurements of exquisite sensitivity that lie at  the core of fascinating observations in fundamental and quantum physics,  astrophysics, geodesy and measurement science.[[BR]][[BR]]In particular,  observations from the Laser Interferometer Gravitational-Wave  Observatory (LIGO) over the past year not only confirmed crucial  gravitational physics effects, but have now also officially launched the  era of Gravitational Wave Astronomy and Multi-Messenger observations.  Similar laser-interferometric measurements have been demonstrated and  are now flying on LISA Pathfinder, exceeding expectations and paving the  way for a spaceborne Gravitational Wave Observatory that will allow us  to survey the gravitational universe otherwise inaccessible to us from  ground.[[BR]][[BR]]Moreover, GRACE follow-on will continue to provide  valuable information about fluctuations of the Earth’s gravitational  field to the geophysical and climatology science community starting  early 2018, whose observations will be greatly enhanced by  interspacecraft laser gradiometric measurements.[[BR]][[BR]]In the area of  cavity optomechanics and novel compact and integrated photonics, the  combination of low-loss devices and optomechanically coupled coherent  light fields enables us to reach unprecedented measurement accuracies  near the quantum sensing limit, which are of relevance in applications  such as Atom Interferometers, Gravimeters, and particularly broadband  inertial sensing.[[BR]][[BR]]I will discuss the advances and implementation  aspects of spaceborne laser measurements for gravitational physics and  novel optomechanical inertial sensing technologies that have been the  focus of my research over the last few years.[[BR]][[BR]]Presentation: English [[BR]] [ Slides: English][[BR]]Questions: German, English ||
     8|| 17.02.2017 || || ||
     9|| 24.02.2017 || || ||
     10|| 03.03.2017 || || ||
     11|| '''10.03.2017 (from 11hrs on, Lab 034)''' || '''Martin Kuerster''' || '''Demo of the New 100-Star Model[[BR]]'''[[BR]]Our  model of the stars in the solar neighborhood, first shown at the last  open house day, is now shining in a new light.  In the meantime it has  been reconditioned, improved, and complemented.[[BR]][[BR]]Among its new  features is a control electronics system that makes it possible to  address selected stars or groups of stars thereby providing new  possibilities for the illustration of astronomical contexts.  Integrated  coordinate planes help with the orientation.[[BR]][[BR]]Our model allows  observers to study fundamental astronomical questions:  Which is the  most abundant type of stars?  Why can we not find most of the stars that  we know from the night sky among the over 100 nearest stars in our  neighborhood?  Why are there no giant stars among them, but their  descendants, the white dwarfs?[[BR]][[BR]]Logistics:[[BR]][[BR]]For the demo of  the model we will meet at its location in Lab 034 (basement).  We need  to form groups of 20 people for this each of which will get together for  20 minutes:[[BR]][[BR]]Group 1: 11.00 - 11.20 a.m. - Language: German[[BR]]Group 2: 11.25 - 11.45 a.m. - Language: English[[BR]]Group 3: 11.50 - 12.10 a.m. - Language: German[[BR]]Group 4: 12.15 - 12.35 a.m. - Language: Englisch[[BR]][[BR]]Choose a time, but be warned that we may have to ask you to[[BR]]wait when we have already reached a group size of 20 people.[[BR]][[BR]]Talk: German, English alternating[[BR]]Slides: n/a[[BR]]Questions: German, English ||
     12|| '''17.03.2017 (11hrs, MPIA)''' || '''Wilma Trick''' || '''The Secret Life of the Galaxies'''[[BR]][[BR]]During  dark nights the Milky Way is observable as a wide band of stars and  dust in the sky. The Milky Way is our home galaxy hosting also our solar  system, but is only one of one hundred billion galaxies in the whole  universe. There are spiral galaxies, huge elliptic galaxies, cloud-like  dwarf galaxies, and galaxies dancing around each other before they  finally merge into one. [[BR]][[BR]]Where do all these galaxies come from?[[BR]]And why do they look as they look?[[BR]][[BR]]In  the past decades astro physicists have act as space detectives and have  collected evidence for a better understanding of galaxy formation and  evolution. One of the prime witnesses: The motion of stars. This led for  instance to the discovery of super massive black holes and the  mysterious dark matter of which we actually know only very little, apart  from its omnipresent existence and its necessity for the formation of  galaxies. [[BR]][[BR]]Presentation: German[[BR]][ Slides: German][[BR]]Questions: German, English ||
     13|| '''24.03.2017[[BR]](11hrs, MPIA)''' || '''Robert Harris (ZAH, LSW)''' || '''Photonic Reformatting'''[[BR]][[BR]]As  astronomical telescopes grow in size the instruments  behind them also  grow. As the individual components become bigger, they  become more  difficult to manufacture, increasing the cost and making  them more  fragile (meaning unless you’ve got a particularly careful PhD  student  the cost of having spares also goes up). This has lead to many   instruments using techniques such as image slicing to reduce the size of   individual components and make the point spread function from the   telescope manageable. [[BR]][[BR]]Astrophotonics  is a field that aims to  combat the problems of size, cost and  complexity. The idea is to take  devices and technologies developed for the  field of photonics and make  use of them in astronomy. In this talk Robert Harris will  describe his  past, current and future work in a subfield of  astrophotonics, photonic  reformatting. This is akin to image slicing,  but occurs within the  fibre, meaning the devices are fully integrated. He  will discuss both  theoretical and practical aspects of his work and draw  conclusions as  to where he feels the field will go next.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     14|| '''31.03.2017 (11hrs, MPIA)''' || '''Damien Gratadour  (Observatoire de Paris)''' || '''Green Flash : Energy efficient real-time computing for ELTs'''[[BR]][[BR]]Controlling          sophisticated AO systems on the future ELTs is a challenge  which         is         yet to be resolved. As the ELTs are adaptive  telescopes, this is         critical to all ELT instrumentation. Green  Flash is an         international         EU funded joint industrial and  academic project intended to         study and         exploit future  and emerging computing technologies for ELT scale         AO          real-time control. This includes the hard real-time data          pipeline,         the soft real-time supervisor module as well as a  real-time         capable         ELT-scale simulation to test and  verify proposed solutions. [[BR]][[BR]]To         date,         we have  initiated in-depth studies on GPUs, MICs and FPGAs.         Moreover,          beyond computing capabilities, it is critical for these future          AO RTC         to address the data flow challenges both in terms of  the large         rate         of streaming data from sensors and in  terms of heterogeneous         data         streams in the system. A  strong emphasis is thus made in the         project         around  interconnect strategies using dedicated hardware,         middleware          and software. With this R&D program we aim at feeding the          E-ELT         AO systems preliminary design studies, led by the  selected         first-light instruments consortia, with technological          validations         supporting the designs of their RTC modules. [[BR]][[BR]]The  culmination of         the         project will be an on-sky  demonstration of a chosen solution.         However, all proposed  solutions will include a detailed study of         capabilities and  scalability. Here we review the project goals         and         the  results from the studies at the mid-point of this three year          endeavor and we describe the downselection process that will          lead to         the design of a full featured prototype to be eventually          implemented         in the lab and tested with the real-time  simulator.[[BR]][[BR]]Presentation: English[[BR]][ Slides: English][[BR]]Questions: German, English ||
     15|| 07.04.2017 || || ||
     16|| 14.04.2017 || -- || Good Friday ||
     17|| 21.04.2017 || -- || Easter Break ||
     18|| '''28.04.2017 (10hrs, HdA)''' || '''Thomas Bertram''' || '''A bit closer to the stars: [[BR]]LINC-NIRVANA on the way to "first light" [[BR]] '''[[BR]]Eleven  months after the arrival on Mt. Graham, LINC-NIRVANA finally found his  designated position on the LBT. In a total of nine trips and 630 person  days the instrument has been re-assembled, internally aligned and in  September 2016 finally installed at the telescope.   In subsequent  trips, LN and LBT have been aligned with respect to each other and a set  of "on sky" tests were successfully passed. Highlight of the last weeks  was the first "closed loop" with one of the two groundlayer wavefront  sensor using a total of five guide stars. [[BR]] [[BR]]This presentation  gives an overview of the activities in the past 18 months, talks about  the challenges, the team had to cope with, the conditions at LBT and  about the achieved results. [[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     19|| '''05.05.2017[[BR]](10hrs, HdA)''' || '''Carolin Liefke''' || '''Remote Observing with HdA/MPIa's 50cm Telescope[[BR]]'''[[BR]]Since  October 2009, the western dome of the Elsaesser lab hosts a modern  semi-professional 50cm telescope. Although equipped with high-level  instrumentation, it is currently used very rarely. This should change  with the opportunity to operate it completely remote via the internet. [[BR]][[BR]]This  presentation shows the general requirements and operating principles of  a remote telescope, demonstrates the current status of the  modifications to the 50cm telescope and its dome, and gives an overview  of future opportunities to use it.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     20|| '''12.05.2017[[BR]](10hrs, HdA)''' || '''Thomas Mueller''' || '''Visualization in Astronomy[[BR]]'''[[BR]]The  aim of scientific visualization in general and visualization       in  astronomy in particular is to graphically illustrate scientific data to        enable scientists to better understand and explore their data in  detail, as well as       to help presenting their work to the general  public. [[BR]][[BR]]       Astronomical data coming from observations and  numerical       simulations cover a large range of different data types,  dimensionality, and       complexity, and thus pose new challenges to  visualization techniques and algorithms, in       particular if the  visualization is to be nearly interactive.[[BR]][[BR]]       After a brief  introduction to different kinds of data sets and how       they can be  visualized, Thomas Mueller will present several visualization projects  with       scientists from MPIA.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     21|| '''19.05.2017[[BR]](10hrs, HdA)''' || '''Tobias Bretschi (AIRBUS APWORKS GmbH)''' || '''Metal 3D Printing[[BR]][[BR]]'''In the upcoming !AstroTechTalk, the central topic will be ''additive manufacturing of metal materials''  (metal 3D  printing). AIRBUS APWORKS, a 100% subsidiary of Airbus  Defence &  Space from Munich will present their competencies in this  field of  manufacturing and will explain the advantages and  disadvantages  of the SLM process (Selective Laser Melting) with the  help of numerous  parts - mainly from Aerospace projects. Additionally,  typical metal  materials for 3D printing will be presented, including  the high strength  aluminum alloy Scalmalloy®, which was specifically   developed for additive manufacturing and which shows excellent   properties for Aerospace applications (high yield strength, low CTE, …).[[BR]][[BR]]Information about the presenter:[[BR]]* Born in Heidelberg[[BR]] * Aerospace Engineering Studies at the University of Stuttgart and at Virginia Tech, USA[[BR]] * Dissertation at Airbus Group Innovations, the research centre of Airbus (supervised by TU Darmstadt)[[BR]] * Focal Point for all Aerospace customers at AIRBUS APWORKS[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     22|| 26.05.2017 || -- || Bridging day after Ascension Day ||
     23|| '''02.06.2017 (10hrs, HdA)''' || '''Justus Zorn (MPIK)''' || '''CHEC-M - A Camera Prototype for the small-size Telescopes of the Cherenkov-Telesope-Array (CTA)[[BR]][[BR]]'''The  Gamma-ray Cherenkov Telescope (GCT) is proposed for the Small-Sized   Telescope component of the Cherenkov Telescope Array (CTA). GCT’s   dual-mirror Schwarzschild-Couder (SC) optical system allows the use of a   compact camera with small form-factor photosensors. [[BR]][[BR]]The GCT  camera is ∼  0.4 m in diameter and has 2048 pixels; each pixel has a ∼  0.2 degree angular  size, resulting in a wide field-of-view. The design  of the GCT camera is  high performance at low cost, with the camera  housing 32 front-end  electronics modules providing full waveform  information for all of the  camera’s 2048 pixels. The first GCT camera  prototype, CHEC-M, was  commissioned during 2015, culminating in the  first Cherenkov images  recorded by a SC telescope and the first light  of a CTA prototype. [[BR]][[BR]]In this talk, Justus Zorn will present  results from CHEC-M from both lab measurements and  on-telescope  operations. Furthermore, he will discuss first results from  CHEC-S, the  second GCT-prototype based on a silicon photomultiplier.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||
     24|| 09.06.2017 || -- || Pentecost holidays ||
     25|| 16.06.2017 || -- || Pentecost holidays ||
     26|| '''23.06.2017 [[BR]](10hrs, HdA)''' || '''Luis Hoffman (Nerf, Imec)''' || '''Silicon multi electrode-optrode arrays (MEOA) for optogenetics[[BR]][[BR]]'''Optogenetics  allows precise spatiotemporal control of neurons using light which has  opened new possibilities in the study of neuronal circuits in the brain.  A successful application of optogenetics requires devices that deliver  light into the brain. These devices should be lightweight, small and  free of complicated tethers. Additionally, such devices should  incorporate many light outputs and recording electrodes with a very high  resolution to allow for the manipulation of individual neurons and  increase the degrees of freedom for neuroscientific experimental design.[[BR]][[BR]]This  work presents a collection of novel electrode-optrode arrays for in  vitro and in vivo optogenetic applications. These devices integrate  silicon nitride waveguide technology with titanium nitride electrodes to  channel light into the optrode array site and record the electrical  response of the neurons. The light from external sources (laser diodes  or optical fibers) is coupled into these waveguides and subsequently  out-coupled orthogonally at the array site by means of optical grating  couplers. The in vivo optical neural probe (optoprobe) incorporates 12  miniaturized optical outputs (optrodes) for light of 450 nm and 590 nm  with an effective size of 6 × 10 µm^2^. They are interlaced along 24 recording electrodes of 10 × 10 µm^2^  on a 100 µm wide and 30 µm thick shank. The in vitro MEOA consists of  an array of 8 by 8 optrodes – identical to the in vivo device –  interlaced with an array of 8 by 8 electrodes of 60 µm diameter. Both  have a pitch of 100 µm. The systems were capable of local artifact-free  excitation and recording of channelrhodopsin 2 transduced neurons.[[BR]][[BR]]Presentation: English[[BR]]Slides: English[[BR]]Questions: English ||
     27|| 30.06.2017 || || ||
     28|| 07.07.2017 || -- || No room available ||
     29|| 14.07.2017 || -- || MPIA summer festival ||
     30|| '''21.07.2017 [[BR]](10hrs, HdA)''' || '''Roman Follert (TLS Tautenburg)''' || '''Resurrection of the beast - Impressions of the CRIRES^+^       MAIT phase and a project update'''[[BR]][[BR]]High-resolution  infrared (IR) spectroscopy plays an important       role in  astrophysics from the search for exoplanets to cosmology.       The  majority of existing IR spectrographs were and are limited by        their small simultaneous wavelength coverage. The adaptive optics        (AO) assisted CRIRES instrument, previously installed at the Very        Large Telescope (VLT), was an IR (0.92 - 5.2 μm) high-resolution        spectrograph which was in operation since 2006. CRIRES was a        unique instrument, accessing a parameter space (wavelength range        and spectral resolution), which up to now was largely uncharted,        as described in Käufl et al. (2004). However, the setup was        limited to a narrow, single-shot, spectral range of about 1/70 of        the central wavelength, resulting in low observing efficiency for        many modern scientific programmes requiring a broad spectral        coverage. [[BR]][[BR]]By introducing crossdispersing elements and larger  detectors, the simultaneous wavelength range       can be increased by a  factor of ten with respect to the old       configuration, while the  total operational wavelength range can be       preserved: CRIRES^+^  has passed its Final Design Review in April       2016. Since then,  installation of the instrument has come a long way. Roman Follert will  present the most recent status of the instrument, give       an overview  of the design and how it has been realized by now. He       will also  summarize the test results (mostly subsystem) obtained       so far.  Last but not least, an update on the project schedule will be given.[[BR]][[BR]]Presentation: German[[BR]][ Slides: English][[BR]]Questions: German, English ||