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- W1674650147 abstract "We present as an example of the polarimetric differential imaging technique our VLT/NACO study of the circumstellar disk around TW Hya, and report on the progress of ongoing instrumentation projects, in particular the CONICA Polarimetric Differential Imager (PDI) upgrade for the VLT, and “CHEOPS”, a VLT 2nd generation high-order adaptive optics system combined with an IR integral field spectrograph and a ZIMPOL-type high precision polarimeter (see contribution by Schmid et al.). 1. Limitations of Partially Compensated Adaptive Optics Observations Studies of stellar environments require high contrast and high angular resolution. The latter is now routinely achieved with ground based telescopes equipped with adaptive optics. Residual wavefront errors, however, in general prevent high contrast ratios. One way to reduce the residuals is the method of dual(or differential-) imaging. Here, two images (either in two orthogonal polarization states see Kuhn et al. 2001 or in two neighbouring wavelength regions see Racine et al. 1999) have to be obtained simultaneously. By taking the difference of these two images, the photons from the bright star (which does not exhibit a high degree of polarization or strong wavelength-dependent spectral features) effectively cancel out, while the much fainter signal from, e.g., a circumstellar disk (seen in scattered, i.e., polarized light) or a substellar companion (with strong molecular absorption bands) clearly stands out (Figure 1). Figure 1. Examples of speckle noise and the gain in noise suppression by using dual imaging with a Wollaston (lab experiment using the VLT AO system NAOS & CONICA (Brandner & Potter 2001). 75" @default.
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- W1674650147 date "2005-12-01" @default.
- W1674650147 modified "2023-10-15" @default.
- W1674650147 title "Polarimetric Differential Imaging Studies of Stellar Environments: Disks and Planets" @default.
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