| 28 | | || '''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]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2017S2/2017-09-29_PhotonicDicer.pdf Slides: English][[BR]]Questions: German, English || |
| 29 | | || 06.10.2017[[BR]](10hrs, HdA) || Julien Milli (ESO) || Current performance and future prospects of the extreme-AO instrument SPHERE after 3 years of operations on Paranal || |
| | 28 | || '''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]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2017S2/2017-09-29_PhotonicDicer.pdf Slides: English][[BR]]Questions: German, English || |
| | 29 | || '''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]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2017S2/2017-10-06_SPHEREupdate.pdf Slides: English][[BR]]Questions: German, English || |
