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--- observation:2026campaign [2025/12/11 19:36] – etienne
+++ observation:2026campaign [2025/12/11 19:57] (current) – [Available instrumentation for 2026] etienne
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 [[technical:tao|TAO]] is available and tested over sunspots and granulation with good results over significantly long periods of time (seeing dependent).
     * A slowed-down (100Hz) version of the same system can be used to stabilize Mercury.
-    * While it is not possible to use TAO over the solar limb (or for neighboring prominences), in 2026 tests have been carried to observe prominences with the AO was focused on granulation in an offset disc region of THEMIS FOV. EVen though the TAO isoplanatic region is located far from the targeted prominence, TAO nonetheless provided significant improvements as shown in the [[science:imofmonth#August 2025|August THEMIS image of the month]].
+    * While it is not possible to use TAO over the solar limb (or for neighboring prominences), during the 2025 campaign, tests have been carried to observe prominences while TAO was focused on granulation in an offset disc region of THEMIS FOV. Even though the TAO isoplanatic region is located far from the targeted prominence, TAO nonetheless provided significant improvements, as shown in the [[science:imofmonth#August 2025|August THEMIS image of the month]].
 === MTR2 in spectroscopy mode ===
 In this mode, up to 4 (old) EMCCD Andor iXon camera (512x512) and up to 2 (new) Andor Zyla (2kx2k) cameras are available. Both 6 cameras can be setup and used at the same time (with their respective specs),  in accordance with the SP2 output physical limitations.
 [[technical:mtr2 | More information about the MTR2 spectrograph.]]
-      * Reconstructed maps quick-look softwares are available for on site analysis.
 === MTR2 in spectropolarimetry mode: ===
-THEMIS polarimetric analysis scheme is based on a full-Stokes analyzer located at the F1 prime focus. For any solar polarization state to measure, the output of the analyzer is made of dual superimposed complementary linear polarizations. Thanks to THEMIS "polarization friendly" new optical scheme, this output travels through the telescope and arrives unperturbed on the spectrograph cameras [[technical:mtr2 |(cf. information about MTR2 spectrograph)]]. Just in front of the camera, a Wollaston splitter separates the beam into complementary Stokes components to form the spectral focal plane. THEMIS own three Wollaston, hence 3 cameras/3 wavebands at most can be simultaneously observed with polarimetric signal, among the 6 spectral cameras that THEMIS propose. It is however possible to combine polarimetric and non-polarimetric cameras.
+THEMIS polarimetric analysis scheme is based on a full-Stokes analyzer located at the F1 prime focus. For any solar polarization state to measure, the output of the analyzer is made of dual superimposed complementary linear polarizations. Thanks to THEMIS "polarization friendly" new optical scheme, this output travels through the telescope and arrives unperturbed on the spectrograph cameras [[technical:mtr2 |(cf. information about MTR2 spectrograph)]]. Just in front of the camera, a Wollaston splitter separates the beam into complementary Stokes components to form the spectral focal plane. THEMIS own three Wollaston, hence 3 cameras/3 wavebands at most can be simultaneously observed with polarimetric signal, among the 6 spectral cameras that THEMIS proposes. It is however possible to combine polarimetric and non-polarimetric cameras.
 Regarding the available analysis software:
-      * A Stokes map quick-look is available.
-      * Thanks to V. Bommier, a basic magnetic field inversion software package (running locally in IDL) is available.
 === Broadband imaging context camera: ===
 THEMIS BBI fast camera (40 frames/s) is running concurrently with the spectrograph. Current setup is for 656 nm (red), but can be changed optionally to G-band or other.
+=== Available analysis softwares ===
+   * Knox Thompson image reconstruction for BBI
+   * Reconstructed spectral map quick-looks for on site analysis, to be adapted to specific wavelength.
+   * Stokes map quick-looks
+   * Thanks to V. Bommier, a basic magnetic field inversion software package (running locally in IDL) is also available.
 /* == 2024 known problems (and solutions) ==