Ground-based and Airborne Instrumentation for Astronomy IV, 2012
ABSTRACT We present the preliminary design of the WEAVE next generation spectroscopy facility for... more ABSTRACT We present the preliminary design of the WEAVE next generation spectroscopy facility for the William Herschel Telescope (WHT), principally targeting optical ground-based follow up of upcoming ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2 degree prime focus field of view at the WHT, with a buffered pick and place positioner system hosting 1000 multi-object (MOS) fibres or up to 30 integral field units for each observation. The fibres are fed to a single spectrograph, with a pair of 8k(spectral) x 6k (spatial) pixel cameras, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R similar to 5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R similar to 20000.
Ground-based and Airborne Instrumentation for Astronomy III, 2010
Summary: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integr... more Summary: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph currently in manufacturing, assembly and integration phase. MUSE has a field of 1x1 arcmin sampled at 0.2x0.2 arcsec and is assisted by the VLT ground ...
Reflectivity of Mo/Si multilayer systems for EUVL. [Proceedings of SPIE 3676, 844 (1999)]. Eric L... more Reflectivity of Mo/Si multilayer systems for EUVL. [Proceedings of SPIE 3676, 844 (1999)]. Eric Louis, Andrey E. Yakshin, Peter C. Goerts, Salim Abdali, Edward LG Maas, R. Stuik, Fred Bijkerk, Detlef Schmitz, Frank Scholze, Gerhard Ulm, Markus Haidl. Abstract. ...
Portable diagnostics for EUV light sources. [Proceedings of SPIE 4146, 121 (2000)]. R. Stuik, Ral... more Portable diagnostics for EUV light sources. [Proceedings of SPIE 4146, 121 (2000)]. R. Stuik, Raluca C. Constantinescu, Petra Hegeman, Jeroen Jonkers, HF Fledderus, Vadim Banine, Fred Bijkerk. Abstract. The EUV light source ...
Optical System Alignment, Tolerancing, and Verification IV, 2010
ASSIST, The Adaptive Secondary Setup and Instrument STimulator, is being developed to provide a t... more ASSIST, The Adaptive Secondary Setup and Instrument STimulator, is being developed to provide a testing facility for the ESO Adaptive Optics Facility (AOF). It will allow the off-telescope testing of three elements of the VLT AOF; the Deformable Secondary Mirror (DSM) and the AO systems for MUSE and HAWK-I (GALACSI and GRAAL). The core of ASSIST consists of a 2-mirror setup (AM1-AM2) allowing the on-axis test of the DSM in interferometric mode. However, during the initial stages of ASSIST integration, DSM would not be present. This makes the task of aligning AM1-AM2 to within an accuracy of 0.05mm/1 arcmin rather challenging. A novel technique known as Shack-Hartmann method has been developed and tested in the lab for this purpose. A Shack Hartmann wavefront sensor will be used to measure the mis-alignment between AM1-AM2 by recording the coma and astigmatism in the presence of large spherical aberration introduced because of tilt/decenter of AM2 with respect to AM1. Thereafter, 20 optical components including lenses, flat mirrors and beam-splitter cubes divided into five sub-assemblies should be aligned to AM1-AM2- DSM axis which ultimately passes through the mechanical axis of large AMOS rotator.
ABSTRACT METIS, the Mid-infrared E-ELT Imager and Spectrometer is foreseen to be the third instru... more ABSTRACT METIS, the Mid-infrared E-ELT Imager and Spectrometer is foreseen to be the third instrument on the European Extremely Large Telescope (E-ELT) and the only instrument to provide high sensitivity mid-IR imaging and spectroscopy to the E-ELT. In order to reach the maximum resolution and sensitivity, an adaptive optics system is required. Since the operational wavelength of METIS is the longest of all E-ELT instruments and the field is relatively small, the complexity of the AO system is significantly reduced, both in required speed as well as order of the AO system. Adaptive Optics has been demonstrated to deliver consistently high performance for the current generation of 6-10 meter class telescopes at mid-infrared wavelengths, and similar performance is expected for METIS on the E-ELT. But in order to provide a reliable system on the E-ELT, several effects which have a minor impact on 6-8 meter class telescopes will need to be investigated for their impact on METIS AO. These effects include refractivity, atmospheric composition variations, but also the operation in a complex operational environment given by both METIS as well as the E-ELT. In this paper we describe the scientific requirements on the METIS AO system, the specific issues related to Adaptive Optics in the mid-IR and expected performance of the METIS AO system on the E-ELT.
Proceedings of SPIE - The International Society for Optical Engineering
MASCARA, the Multi-site All-Sky CAmeRA, will consist of several fully-automated stations distribu... more MASCARA, the Multi-site All-Sky CAmeRA, will consist of several fully-automated stations distributed across the globe. Its goal is to find exoplanets transiting the brightest stars, in the mV = 4 to 8 magnitude range, currently probed neither by space- nor by ground-based surveys. The nearby transiting planet systems that MASCARA is expected to discover will be key targets for future detailed planet atmosphere observations. The target population for MASCARA consists mostly of hot Jupiters. The main requirement set on MASCARA to detect these planets around stars down to magnitude 8 is to reach a minimum Signal-to-Noise Ratio of 100 within one hour of observation. Each MASCARA station consists of five low-noise off-the-shelf full-frame CCD cameras, fitted with standard Canon 24 mm , f/1.4 lenses, monitoring the near-entire sky down to magnitude 8 at that location. Measurements have demonstrated that the required Signal-to-Noise Ratio of 100, can be achieved in less than thirty minutes...
Proceedings of SPIE - The International Society for Optical Engineering
MASCARA, the Multi-site All-Sky CAmeRA, consists of several fully-automated stations distributed ... more MASCARA, the Multi-site All-Sky CAmeRA, consists of several fully-automated stations distributed across the globe. Its goal is to find exoplanets transiting the brightest stars, in the V = 4 to 8 magnitude range, currently probed neither by space- nor by ground-based surveys. The nearby transiting planet systems that MASCARA is expected to discover will be key targets for future detailed planet atmosphere observations. Each station contains five wide-angle cameras monitoring the near-entire sky at each location. Once fully deployed, MASCARA will provide a nearly continuous coverage of the dark sky, down to magnitude 8, at sub-minute cadence. Effectively taking an image of the full sky every 6.4 seconds, MASCARA will produce approximately 500 GB of raw data per night, per station. This data needs to be processed in order to produce calibrated light curves, for up to ~40,000 stars down to magnitude 8 and with a signal-to-noise-ratio of better than 100. The aim of the data reduction pi...
Proceedings of SPIE - The International Society for Optical Engineering
In telescopes with a Deformable Secondary Mirror, the testing and calibration of both the DSM its... more In telescopes with a Deformable Secondary Mirror, the testing and calibration of both the DSM itself as well as the instruments using this DSM are expensive and time consuming processes. Especially in telescopes without an intermediate focus before the DSM, a number of calibrations can only be performed on a real star during night time. A full suite of Adaptive Optics systems and AO-assisted instruments is currently under development for the VLT, also know as the VLT Adaptive Telescope. ASSIST was developed to assist in the integration and testing of three elements of the VLT Adaptive Telescope Facility; the DSM; the MUSE AO system 'GALACSI' and the HAWK-I AO system 'GRAAL.' The core of ASSIST is a support infrastructure to integrate the DSM in a compact and stable test setup. A Nasmyth rotator simulator will be provided for attaching the two AO systems, while ASSIST will be fed by a star simulator and turbulence generator for realistic performance measurements of bo...
ABSTRACT The ESO Very Large Telescope Adaptive Optics Facility (VLT-AOF) will transform the VLT U... more ABSTRACT The ESO Very Large Telescope Adaptive Optics Facility (VLT-AOF) will transform the VLT Unit Telescope 4 to an Adaptive Telescope. In absence of an intermediate focus before the Adaptive Secondary in this Ritchey-Chrétien type telescope and in order to reduce the testing and calibration of the system on-sky, ASSIST, The Adaptive Secondary Setup and Instrument STimulator, was developed. It provides an off-sky testing facility for the ESO AOF and will provide a full testing environment for three elements of the VLT Adaptive Optics Facility: the Deformable Secondary Mirror (DSM) and the AO modules for MUSE and HAWK-I (GALACSI and GRAAL). ASSIST was delivered to ESO Garching, where it was assembled and tested. Currently ASSIST is being integrated with the Deformable Secondary Mirror, the first step in the full system testing of the two AO systems for the VLT AOF on ASSIST. This paper briefly reviews the design and properties of ASSIST and reports on the first results of ASSIST in stand-alone mode.
Ground-based and Airborne Instrumentation for Astronomy IV, 2012
ABSTRACT We present the preliminary design of the WEAVE next generation spectroscopy facility for... more ABSTRACT We present the preliminary design of the WEAVE next generation spectroscopy facility for the William Herschel Telescope (WHT), principally targeting optical ground-based follow up of upcoming ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2 degree prime focus field of view at the WHT, with a buffered pick and place positioner system hosting 1000 multi-object (MOS) fibres or up to 30 integral field units for each observation. The fibres are fed to a single spectrograph, with a pair of 8k(spectral) x 6k (spatial) pixel cameras, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R similar to 5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R similar to 20000.
Ground-based and Airborne Instrumentation for Astronomy III, 2010
Summary: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integr... more Summary: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph currently in manufacturing, assembly and integration phase. MUSE has a field of 1x1 arcmin sampled at 0.2x0.2 arcsec and is assisted by the VLT ground ...
Reflectivity of Mo/Si multilayer systems for EUVL. [Proceedings of SPIE 3676, 844 (1999)]. Eric L... more Reflectivity of Mo/Si multilayer systems for EUVL. [Proceedings of SPIE 3676, 844 (1999)]. Eric Louis, Andrey E. Yakshin, Peter C. Goerts, Salim Abdali, Edward LG Maas, R. Stuik, Fred Bijkerk, Detlef Schmitz, Frank Scholze, Gerhard Ulm, Markus Haidl. Abstract. ...
Portable diagnostics for EUV light sources. [Proceedings of SPIE 4146, 121 (2000)]. R. Stuik, Ral... more Portable diagnostics for EUV light sources. [Proceedings of SPIE 4146, 121 (2000)]. R. Stuik, Raluca C. Constantinescu, Petra Hegeman, Jeroen Jonkers, HF Fledderus, Vadim Banine, Fred Bijkerk. Abstract. The EUV light source ...
Optical System Alignment, Tolerancing, and Verification IV, 2010
ASSIST, The Adaptive Secondary Setup and Instrument STimulator, is being developed to provide a t... more ASSIST, The Adaptive Secondary Setup and Instrument STimulator, is being developed to provide a testing facility for the ESO Adaptive Optics Facility (AOF). It will allow the off-telescope testing of three elements of the VLT AOF; the Deformable Secondary Mirror (DSM) and the AO systems for MUSE and HAWK-I (GALACSI and GRAAL). The core of ASSIST consists of a 2-mirror setup (AM1-AM2) allowing the on-axis test of the DSM in interferometric mode. However, during the initial stages of ASSIST integration, DSM would not be present. This makes the task of aligning AM1-AM2 to within an accuracy of 0.05mm/1 arcmin rather challenging. A novel technique known as Shack-Hartmann method has been developed and tested in the lab for this purpose. A Shack Hartmann wavefront sensor will be used to measure the mis-alignment between AM1-AM2 by recording the coma and astigmatism in the presence of large spherical aberration introduced because of tilt/decenter of AM2 with respect to AM1. Thereafter, 20 optical components including lenses, flat mirrors and beam-splitter cubes divided into five sub-assemblies should be aligned to AM1-AM2- DSM axis which ultimately passes through the mechanical axis of large AMOS rotator.
ABSTRACT METIS, the Mid-infrared E-ELT Imager and Spectrometer is foreseen to be the third instru... more ABSTRACT METIS, the Mid-infrared E-ELT Imager and Spectrometer is foreseen to be the third instrument on the European Extremely Large Telescope (E-ELT) and the only instrument to provide high sensitivity mid-IR imaging and spectroscopy to the E-ELT. In order to reach the maximum resolution and sensitivity, an adaptive optics system is required. Since the operational wavelength of METIS is the longest of all E-ELT instruments and the field is relatively small, the complexity of the AO system is significantly reduced, both in required speed as well as order of the AO system. Adaptive Optics has been demonstrated to deliver consistently high performance for the current generation of 6-10 meter class telescopes at mid-infrared wavelengths, and similar performance is expected for METIS on the E-ELT. But in order to provide a reliable system on the E-ELT, several effects which have a minor impact on 6-8 meter class telescopes will need to be investigated for their impact on METIS AO. These effects include refractivity, atmospheric composition variations, but also the operation in a complex operational environment given by both METIS as well as the E-ELT. In this paper we describe the scientific requirements on the METIS AO system, the specific issues related to Adaptive Optics in the mid-IR and expected performance of the METIS AO system on the E-ELT.
Proceedings of SPIE - The International Society for Optical Engineering
MASCARA, the Multi-site All-Sky CAmeRA, will consist of several fully-automated stations distribu... more MASCARA, the Multi-site All-Sky CAmeRA, will consist of several fully-automated stations distributed across the globe. Its goal is to find exoplanets transiting the brightest stars, in the mV = 4 to 8 magnitude range, currently probed neither by space- nor by ground-based surveys. The nearby transiting planet systems that MASCARA is expected to discover will be key targets for future detailed planet atmosphere observations. The target population for MASCARA consists mostly of hot Jupiters. The main requirement set on MASCARA to detect these planets around stars down to magnitude 8 is to reach a minimum Signal-to-Noise Ratio of 100 within one hour of observation. Each MASCARA station consists of five low-noise off-the-shelf full-frame CCD cameras, fitted with standard Canon 24 mm , f/1.4 lenses, monitoring the near-entire sky down to magnitude 8 at that location. Measurements have demonstrated that the required Signal-to-Noise Ratio of 100, can be achieved in less than thirty minutes...
Proceedings of SPIE - The International Society for Optical Engineering
MASCARA, the Multi-site All-Sky CAmeRA, consists of several fully-automated stations distributed ... more MASCARA, the Multi-site All-Sky CAmeRA, consists of several fully-automated stations distributed across the globe. Its goal is to find exoplanets transiting the brightest stars, in the V = 4 to 8 magnitude range, currently probed neither by space- nor by ground-based surveys. The nearby transiting planet systems that MASCARA is expected to discover will be key targets for future detailed planet atmosphere observations. Each station contains five wide-angle cameras monitoring the near-entire sky at each location. Once fully deployed, MASCARA will provide a nearly continuous coverage of the dark sky, down to magnitude 8, at sub-minute cadence. Effectively taking an image of the full sky every 6.4 seconds, MASCARA will produce approximately 500 GB of raw data per night, per station. This data needs to be processed in order to produce calibrated light curves, for up to ~40,000 stars down to magnitude 8 and with a signal-to-noise-ratio of better than 100. The aim of the data reduction pi...
Proceedings of SPIE - The International Society for Optical Engineering
In telescopes with a Deformable Secondary Mirror, the testing and calibration of both the DSM its... more In telescopes with a Deformable Secondary Mirror, the testing and calibration of both the DSM itself as well as the instruments using this DSM are expensive and time consuming processes. Especially in telescopes without an intermediate focus before the DSM, a number of calibrations can only be performed on a real star during night time. A full suite of Adaptive Optics systems and AO-assisted instruments is currently under development for the VLT, also know as the VLT Adaptive Telescope. ASSIST was developed to assist in the integration and testing of three elements of the VLT Adaptive Telescope Facility; the DSM; the MUSE AO system 'GALACSI' and the HAWK-I AO system 'GRAAL.' The core of ASSIST is a support infrastructure to integrate the DSM in a compact and stable test setup. A Nasmyth rotator simulator will be provided for attaching the two AO systems, while ASSIST will be fed by a star simulator and turbulence generator for realistic performance measurements of bo...
ABSTRACT The ESO Very Large Telescope Adaptive Optics Facility (VLT-AOF) will transform the VLT U... more ABSTRACT The ESO Very Large Telescope Adaptive Optics Facility (VLT-AOF) will transform the VLT Unit Telescope 4 to an Adaptive Telescope. In absence of an intermediate focus before the Adaptive Secondary in this Ritchey-Chrétien type telescope and in order to reduce the testing and calibration of the system on-sky, ASSIST, The Adaptive Secondary Setup and Instrument STimulator, was developed. It provides an off-sky testing facility for the ESO AOF and will provide a full testing environment for three elements of the VLT Adaptive Optics Facility: the Deformable Secondary Mirror (DSM) and the AO modules for MUSE and HAWK-I (GALACSI and GRAAL). ASSIST was delivered to ESO Garching, where it was assembled and tested. Currently ASSIST is being integrated with the Deformable Secondary Mirror, the first step in the full system testing of the two AO systems for the VLT AOF on ASSIST. This paper briefly reviews the design and properties of ASSIST and reports on the first results of ASSIST in stand-alone mode.
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Papers by Remko Stuik