27 | 27 | || '''12.09.2014''' || '''Martin Kürster''' || '''The project landscape of the technical departments'''[[BR]][[BR]]Here's another one of those funny names for a new instrument. But actually, [[BR]]what is it about? Do you also sometimes feel like this? Martin Kürster will [[BR]]give us an overview of the instruments we are building at MPIA. From this, [[BR]]we should be able to get the connection between those acronyms and the [[BR]]instruments. But not only that, after several years of heavy overbooking of [[BR]]the technical departments the mid-term future of the project landscape has [[BR]]recently become a bit unclear due to repeated delays of the European [[BR]]Extremely Large Telescope (E-ELT). Martin Kürster will also tell us about [[BR]]possible future initiatives, project acquisitions still under discussion, that will [[BR]]pose new challenges for the technical departments.[[BR]][[BR]]Talk: German [[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/WikiStart/2014-09-12_instrumentation_projects.pdf Slides: English][[BR]]Questions: German, English || |
28 | 28 | || '''19.09.2014''' || '''Ralf-Rainer Rohloff''' || '''Precision metal optics over a large temperature range '''[[BR]] [[BR]]Since long, metal optics are an important part of astronomical instruments. Often [[BR]]diamond turned mirrors of aluminum (Al6061) are used. But it is difficult to polish [[BR]]aluminum. Therefore, the mirror is coated with Nickle Phosphor layer, which can [[BR]]be polished more easily. This is very important at shorter wavelength. But the [[BR]]mirrors deform with temperature changes because of the different coeffient of [[BR]]thermal expansion between aluminum and NiP. [[BR]][[BR]]Ralf-Rainer will tell us about a collaboration between MPIA Heidelberg and IOF [[BR]]Jean, which developed and tested a new material to minimize the temperature [[BR]]related deformation of such mirrors. The material consists of an aluminum [[BR]]silicate, which has a coefficient of thermal expansion close to NiP. Thus, the [[BR]]deformation could be reduced drastically. But now the work just started. Is it [[BR]]possible to built a mirror of this material? Does the material change with time? [[BR]]The best answer would be the study could show that such mirror can be built [[BR]]and are stable over time! [[BR]][[BR]]Talk: German [[BR]]Slides: English [[BR]]Questions: German, English || |
31 | | || 10.10.2014 || '''Casey Deen''' || '''Alignment challenges and strategies for the GRAVITY wavefront sensor cryostat and tower[[BR]]'''[[BR]]Aligning a handful of small mirrors,filters, and lenses with a laser shouldn't be [[BR]]so difficult, right? Surely no more than an afternoon! But after another week [[BR]]spent huddled in a dark laboratory, the light still does not end up in the correct [[BR]]position on the detector! In order to avoid this frustrating situation, an alignment[[BR]]strategy is an important part of building any instrument. Casey Deen presents [[BR]]the alignment concept for the GRAVITY wavefront sensor. This near-infrared [[BR]]sensor works on the Shack-Hartman Principle. Due to their wavelength [[BR]]range, near-infrared sensors have a larger selection of bright guide stars than [[BR]]do optical sensors, as most stars are brightest in the infrared. Optical light is [[BR]]also attenuated more by interstellar dust, making optical sensors impractical [[BR]]in dusty regions like the Galactic Center. The wavefront sensors are located [[BR]]in the Coude rooms of the Unit Telescopes of the Very Large Telescope (VLT). [[BR]]The location and the optical design of the wavefront sensors present several[[BR]]challenges for alignment. Casey and his colleagues present their strategy for [[BR]]alignment of the optics, and are looking forward to hearing opinions, advice [[BR]]and concerns from the assembled experts at MPIA. Expect a lively discussion [[BR]]and insight on what is laboratory work about! [[BR]][[BR]]Vortrag: Englisch [[BR]]Präsentation: Deutsch[[BR]]Fragen: Deutsch, Englisch || |
32 | | || 17.10.2014 || Klaus Meisenheimer ?? || PANIC[[BR]]?? || |
33 | | || 24.10.2014 || || || |
| 31 | || 10.10.2014 || '''Casey Deen''' || '''Alignment challenges and strategies for the GRAVITY wavefront sensor cryostat and tower[[BR]]'''[[BR]]Aligning a handful of small mirrors,filters, and lenses with a laser shouldn't be [[BR]]so difficult, right? Surely no more than an afternoon! But after another week [[BR]]spent huddled in a dark laboratory, the light still does not end up in the correct [[BR]]position on the detector! In order to avoid this frustrating situation, an alignment[[BR]]strategy is an important part of building any instrument. Casey Deen presents [[BR]]the alignment concept for the GRAVITY wavefront sensor. This near-infrared [[BR]]sensor works on the Shack-Hartman Principle. Due to their wavelength [[BR]]range, near-infrared sensors have a larger selection of bright guide stars than [[BR]]do optical sensors, as most stars are brightest in the infrared. Optical light is [[BR]]also attenuated more by interstellar dust, making optical sensors impractical [[BR]]in dusty regions like the Galactic Center. The wavefront sensors are located [[BR]]in the Coude rooms of the Unit Telescopes of the Very Large Telescope (VLT). [[BR]]The location and the optical design of the wavefront sensors present several[[BR]]challenges for alignment. Casey and his colleagues present their strategy for [[BR]]alignment of the optics, and are looking forward to hearing opinions, advice [[BR]]and concerns from the assembled experts at MPIA. Expect a lively discussion [[BR]]and insight on what is laboratory work about! [[BR]][[BR]]Vortrag: Englisch [[BR]]Präsentation: German[[BR]]Fragen: German, Englisch || |
| 32 | || 17.10.2014 || Klaus Meisenheimer || '''PANIC''' || |
| 33 | || 24.10.2014 || Jacopo Farinato || '''SHARK - A optical integral field spectrograph and near-infrared coronagraph for the LBT''' || |