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| call25:2025_user_info [2024/12/19 14:53] – created admin | call25:2025_user_info [2024/12/19 14:54] (current) – [At this moment (Jan 2025) we propose:] bgelly |
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| - **MTR2 in spectroscopy mode** In this mode we propose up to 4 (old) EMCCD Andor iXon camera (512x512) and up to 2 (new) Andor Zyla (2kx2k) cameras. Both 6 cameras can be setup and used at the same time (with their respective specs), in accordance with the SP2 output physical limitations. | - **MTR2 in spectroscopy mode** In this mode we propose up to 4 (old) EMCCD Andor iXon camera (512x512) and up to 2 (new) Andor Zyla (2kx2k) cameras. Both 6 cameras can be setup and used at the same time (with their respective specs), in accordance with the SP2 output physical limitations. |
| - **MTR2 in spectropolarimetry mode**: In this mode, **3 cameras (hence 3 wavelengths) at most** are available, from the above description. It is possible to combine polarimetric and non-polarimetric cameras. Our 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 our "polarization friendly" new optical scheme, this output travels through the telescope and arrives unperturbed on the spectrograph cameras. Just in front of the camera, a Wollaston splitter separates the beam into complementary Stokes components to form the spectral focal plane. Regarding the available analysis software: | - **MTR2 in spectropolarimetry mode**: In this mode, **3 cameras (hence 3 wavelengths) at most** are available, from the above list. It is possible to combine polarimetric and non-polarimetric cameras. Our 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 our "polarization friendly" new optical scheme, this output travels through the telescope and arrives unperturbed on the spectrograph cameras. Just in front of the camera, a Wollaston splitter separates the beam into complementary Stokes components to form the spectral focal plane. Regarding the available analysis software: |
| * A Stokes map quick-look is now available. | * A Stokes map quick-look is now available. |
| * Thanks to V. Bommier, a basic magnetic field inversion software package (running locally in IDL) is available. | * Thanks to V. Bommier, a basic magnetic field inversion software package (running locally in IDL) is available. |
