9 research outputs found
SPHERE ZIMPOL: overview and performance simulation
International audienc
Project overview of OPTIMOS-EVE: The fibre-fed multi-object spectrograph for the E-ELT
OPTIMOS-EVE (OPTical Infrared Multi Object Spectrograph - Extreme Visual Explorer) is the fibre fed multi object spectrograph proposed for the European Extremely Large Telescope (E-ELT), planned to be operational in 2018 at Cerro Armazones (Chile). It is designed to provide a spectral resolution of 6000, 18000 or 30000, at wavelengths from 370 nm to 1.7 μm, combined with a high multiplex (>200) and a large spectral coverage. Additionally medium and large IFUs are available. The system consists of three main modules: a fibre positioning system, fibres and a spectrograph. The recently finished OPTIMOS-EVE Phase-A study, carried out within the framework of the ESO E-ELT instrumentation studies, has been performed by an international consortium consisting of institutes from France, Netherlands, United Kingdom and Italy. All three main science themes of the E-ELT are covered by this instrument: Planets and Stars; Stars and Galaxies; Galaxies and Cosmology. This paper gives an overview of the OPTIMOS-EVE project, describing the science cases, top level requirements, the overall technical concept and the project management approach. It includes a description of the consortium, highlights of the science drivers and resulting science requirements, an overview of the instrument design and telescope interfaces, the operational concept, expected performance, work breakdown and management structure for the construction of the instrument, cost and schedule. © 2010 Copyright SPIE - The International Society for Optical Engineering
Project overview of OPTIMOS-EVE: the fibre-fed multi-object spectrograph for the E-ELT
OPTIMOS-EVE (OPTical Infrared Multi Object Spectrograph - Extreme Visual Explorer) is the fibre fed multi object spectrograph proposed for the European Extremely Large Telescope (E-ELT), planned to be operational in 2018 at Cerro Armazones (Chile). It is designed to provide a spectral resolution of 6000, 18000 or 30000, at wavelengths from 370 nm to 1.7 ÎĽm, combined with a high multiplex (>200) and a large spectral coverage. Additionally medium and large IFUs are available. The system consists of three main modules: a fibre positioning system, fibres and a spectrograph. The recently finished OPTIMOS-EVE Phase-A study, carried out within the framework of the ESO E-ELT instrumentation studies, has been performed by an international consortium consisting of institutes from France, Netherlands, United Kingdom and Italy. All three main science themes of the E-ELT are covered by this instrument: Planets and Stars; Stars and Galaxies; Galaxies and Cosmology. This paper gives an overview of the OPTIMOS-EVE project, describing the science cases, top level requirements, the overall technical concept and the project management approach. It includes a description of the consortium, highlights of the science drivers and resulting science requirements, an overview of the instrument design and telescope interfaces, the operational concept, expected performance, work breakdown and management structure for the construction of the instrument, cost and schedule
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RefPlanets: Search for reflected light from extra-solar planets with SPHERE/ZIMPOL
RefPlanets is a guaranteed time observation (GTO) programme that uses the
Zurich IMaging POLarimeter (ZIMPOL) of SPHERE/VLT for a blind search for
exoplanets in wavelengths from 600-900 nm. The goals of this study are the
characterization of the unprecedented high polarimetic contrast and
polarimetric precision capabilities of ZIMPOL for bright targets, the search
for polarized reflected light around some of the closest bright stars to the
Sun and potentially the direct detection of an evolved cold exoplanet for the
first time. For our observations of Alpha Cen A and B, Sirius A, Altair, Eps
Eri and Tau Ceti we used the polarimetric differential imaging (PDI) mode of
ZIMPOL which removes the speckle noise down to the photon noise limit for
angular separations >0.6". We describe some of the instrumental effects that
dominate the noise for smaller separations and explain how to remove these
additional noise effects in post-processing. We then combine PDI with angular
differential imaging (ADI) as a final layer of post-processing to further
improve the contrast limits of our data at these separations. For good
observing conditions we achieve polarimetric contrast limits of 15.0-16.3 mag
at the effective inner working angle of about 0.13", 16.3-18.3 mag at 0.5" and
18.8-20.4 mag at 1.5". The contrast limits closer in (<0.6") depend
significantly on the observing conditions, while in the photon noise dominated
regime (>0.6"), the limits mainly depend on the brightness of the star and the
total integration time. We compare our results with contrast limits from other
surveys and review the exoplanet detection limits obtained with different
detection methods. For all our targets we achieve unprecedented contrast
limits. Despite the high polarimetric contrasts we are not able to find any
additional companions or extended polarized light sources in the data that has
been taken so far