|Instrument||Telescope/Observatory||Resolving power||Wavelengths, nm|
|SEMPOL*/UCLES||Siding Spring(3.9 m)/AAT||70 000||370 – 870|
|MuSiCoS**||TBL(2 m)/Pic-du-Midi||35 000||450 – 660|
|SARG SP||TNG(3.6 m)/Tenerife||46 000 – 164 000||370 – 1020|
|ESPaDONS||CFHT(4 m)/Hawaii||70 000||370 – 1000|
The new generation large telescopes are not yet equipped with high-resolution spectropolarimetric capabilities. The only existing project is PEPSI at the double 8 m LBT (Strassmeier et al., 2004). Low-resolution spectropolarimetry is possible with FORS1 at VLT (Appenzeller et al., 1998). A promising approach to high-precision polarimetry is provided by a ZIMPOL-type spectropolarimeter, which is a transportable system being combined with a spectrograph (Stenflo, 2001).
Magnetic fields in G, K, and M main-sequence stars have been deduced from the broadening of line profiles (e.g., Valenti et al., 1995) or even Zeeman-split spectral lines in M-type dwarf flare stars (Johns-Krull and Valenti, 1996). Using SEMPOL at AAT, Donati et al. (1997) reported detection of Zeeman polarisation in several kinds of active stars, including RS CVn systems, a dwarf flare star of BY Dra type, a FK Com star, and a T Tau star. Several new detections have been made with MuSiCoS (Wade, 2003).
© Max Planck Society and the author(s)