| Both sides previous revisionPrevious revisionNext revision | Previous revision |
| technical:description [2026/03/05 14:34] – [(10) Spectrograph slit at F2] etienne | technical:description [2026/03/17 15:57] (current) – etienne |
|---|
| \\ | \\ |
| <html><font color="#ff0000" size="2.5"> Page in construction ; Last Update January 2026 </font></html> | <html><font color="#ff0000" size="2.5"> Page in construction ; Last Update March 2026 </font></html> |
| |
| |
| Overall, the working characteristics of THEMIS are the following: | Overall, the working characteristics of THEMIS are the following: |
| * Observational electromagnetic spectrum range: 400-1100 nm | * Observational electromagnetic spectrum range: 400-1100 nm |
| * Imaging field-of-view : ~2’x2’; square shaped | * Imaging field-of-view : ~2’x2’ square shaped without polarisation analysis; ~1’x1’ with polarisation |
| * Overall focal ratio : f/62 | * Overall focal ratio : f/62 |
| * Effective aperture: 92 cm | * Effective aperture: 92 cm |
| <newcolumn *40%*> | <newcolumn *40%*> |
| |
| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:themis_optpath_functionaldiagram2.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:themis_optpath_functionaldiagram2.jpg" style="width:90%; height: auto;"></a></html> | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:themis_optpath_functionaldiagram.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:themis_optpath_functionaldiagram.jpg" style="width:90%; height: auto;"></a></html> |
| |
| </columns> | </columns> |
| ==== (2) Full-Sun guider ==== | ==== (2) Full-Sun guider ==== |
| |
| A full-sun guider has been setup on the telescope outer ring of the heat protection, near the 1m entrance plate. It uses a 45/500 mm objective, an Herschel prism, a neutral filter, a broadband (10 nm) green continuum 540nm photosphere filter (Baader Planetarium GmbH), and a ZWO ASI 178 mono (2000x3000 pixel²) CMOS camera. The full-sun guider image is always available in the control room of THEMIS. The full-Sun guider images are not meant for pure scientific analysis. Please note that given the location of the entrance pupil and depending on the telescope/dome relative positions, this guider may be momentarily obscured by the dome edge(for less than 30 seconds in any circumstance). <html><font color="#ff9900"> Camera settings can be changed by the user in the control room. Acquisition is left to the needs and appreciation of the user. </font></html>\\ | A full-sun guider has been setup on the telescope outer ring of the heat protection, near the 1m entrance plate. It uses a 45/500 mm objective, an Herschel prism, a neutral filter, a broadband (10 nm) green continuum 540nm photosphere filter (Baader Planetarium GmbH), and a ZWO ASI 178 mono (2000x3000 pixel²) CMOS camera. The full-sun guider image is always available in the control room of THEMIS. The full-Sun guider images are not meant for pure scientific analysis. Please note that given the location of the entrance pupil and depending on the telescope/dome relative positions, this guider may be momentarily obscured by the dome edge (for less than 30 seconds in any circumstance). <html><font color="#ff9900"> Camera settings can be changed by the user in the control room. Acquisition is left to the needs and appreciation of the user. </font></html>\\ |
| |
| <html><font color="#0000ff"> The image from this camera is an available data product </font></html> [[observation:data#Full-sun guider images| (cf. THEMIS data products)]]. | <html><font color="#0000ff"> The image from this camera is an available data product </font></html> [[observation:data#Full-sun guider images| (cf. THEMIS data products)]]. |
| |
| Simplified cartoon of the light-path within THEMIS identifying the main instrumental blocks. The spectrograph is not represented. \\ | Simplified cartoon of the light-path within THEMIS identifying the main instrumental blocks. The spectrograph is not represented. \\ |
| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:themis.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:themis.png" style="width:80%; height: auto;"></a></html> \\ | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:themis.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:themis.png" style="width:80%; height: auto;"></a></html> \\ |
| |
| \\ | \\ |
| |
| Animation of THEMIS and systems and old optical path, before the installation of the adaptive optics. \\ | Animation of THEMIS and systems and old optical path, before the installation of the adaptive optics. \\ |
| <html><video onloadedmetadata="this.muted = true" style="width:80%; height: auto;" controls autoplay loop><source src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:building_and_telescope.mp4" type="video/mp4"></video></html> \\ | <html><video onloadedmetadata="this.muted = true" style="width:80%; height: auto;" controls autoplay loop><source src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:building_and_telescope.mp4" type="video/mp4"></video></html> \\ |
| |
| </columns> | </columns> |
| |
| |
| ==== (3) First optical focus instrumentation, F1 ==== | ==== (3) First optical focus (F1) : light polarization analysis instrumentation ==== |
| |
| The original //raison d'être// of THEMIS was to be a polarisation free telescope thanks to polarimetric analysis being performed immediately at the first optical focus, while adaptive optics (AO) is standardly located at F1 in professional telescopes. Maintaining its excellent polarimetric sensitivity has been one of the main challenge of developing the THEMIS AO. | The original fundamental //raison d'être// and strength of THEMIS is to be a polarisation-calibration-free telescope thanks to the polarimetric analysis being performed immediately at the first optical focus (F1). This contrasts with imagery-driven telescope for which adaptive optics (AO) is usually located at F1. |
| | |
| | Maintaining THEMIS excellent polarimetric sensitivity has been one of the main challenge of the upgrade of THEMIS and the development of [[technical:tao |THEMIS adpative optics (TAO)]]. The original optical design of THEMIS was composed of a double beam, each of them carrying the opposite polarisation state and having its own optical path. This design was not compatible with the existence of an AO in which the wavefront correction requires an unique light beam. The inclusion of TAO has thus required the complete redisign of THEMIS optical path as well as polarisation analysis instrumentation. |
| | |
| | As of today, a Full-Stokes analyzer (An4) is located at F1, producing superposed dual-beam polarimetry with beam exchange. The analyser is composed of double Savart plates. The first Savart plates generate the dual beam, each of them carrying opposite polarisation state, e.g. I±S, with S the Stokes polarization parameter. The second Savart plates then superimpose both beams, each of them in a polarisation state that is orthogonal to each other. Both beams then do behave as one, differing only by their linear polarization state. |
| | |
| | Thanks to THEMIS “polarization friendly” new optical path (geometry of the elevation axis, field rotator, coatings), polarizer output can travel through the telescope and reach the spectrograph cameras “minimally perturbed”. Latter, just ahead of each of the spectral cameras, a Wollaston prism splitter separates the superimposed beam into complementary Stokes components to form the spectral focal plane. |
| | |
| Polarimetric analyser : <html><font color="#ff0000" size="1.5"> Information to be added</font></html> | <html><font color="#ff0000"> As of today, THEMIS remains a strongly polarization-calibration-free telescope, ideal for excellent spectropolarimetric measurements.</font></html>. Further information, such as THEMIS Mueller matrix can be consulted on the dedicated page about [[technical:polarisation | THEMIS polarimetric analysis scheme.]] |
| |
| |
| |
| Cartoon of THEMIS light-path with the different systems and optical focuses, omitting the spectrograph. \\ | Cartoon of THEMIS light-path with the different systems and optical focuses, omitting the spectrograph. \\ |
| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=:results:gallery:schema:opticalpath_themis_withoutspectrograph.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:opticalpath_themis_withoutspectrograph.png" style="width:80%; height: auto;"></a></html> \\ | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=:science:gallery:schema:opticalpath_themis_withoutspectrograph.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:opticalpath_themis_withoutspectrograph.png" style="width:80%; height: auto;"></a></html> \\ |
| |
| |
| |
| |
| ==== (6) Field scanning (OBJ2) ==== | ==== (6) Fine field-of-view scanning mirror (OBJ2) ==== |
| |
| The OBJ2 movable mirror allow a fine scanning of the field of view one the Sun. This allows to move the field of view on the target without the need to move the telescope (the latter being much less precise). This scanning mirror enables displacement with increment as small as 0.01" arcsec. This would however be smaller than the seeing limits even with adaptive optics working. Typical observations uses scanning steps of the range 0.1" to a few arcseconds. | The OBJ2 movable mirror allow a fine scanning of the field-of-view (fov) on the Sun. This allows to displace the fov on the target without the need to move the telescope (the latter being much less precise). This scanning mirror enables displacement with increment as small as 0.01" arcsec. This would however be smaller than the seeing limits even with adaptive optics working. Typical observations uses scanning steps of the range 0.1" to a few arcseconds. |
| |
| <html><font color="#ff9900"> Users not performing sit-and-stare observations shall define the scanning properties for their observations. </font></html> | <html><font color="#ff9900"> Users not performing sit-and-stare observations shall define the scanning properties for their observations. </font></html> |
| <newcolumn *40%*> | <newcolumn *40%*> |
| Cartoon of the beam splitting options. | Cartoon of the beam splitting options. |
| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:beamsplitteroptions.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:schema:beamsplitteroptions.jpg" style="width:90%; height: auto;"></a></html> \\ | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:beamsplitteroptions.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:schema:beamsplitteroptions.jpg" style="width:90%; height: auto;"></a></html> \\ |
| </columns> | </columns> |
| <columns 100% 60%> | <columns 100% 60%> |
| ==== (8-9) Broadband Imaging (BBI) filter & camera ==== | ==== (8-9) Broadband Imaging (BBI) filter & camera ==== |
| |
| If illuminated, the BBI camera offers a broadband high-resolution image with a square field-of-view of about ~55"x55". A broadband red filter, with a ~3nm passband centred around 656 nm is placed upstream of the camera. THEMIS BBI camera thus currently provides images or the red visible continuum. | If illuminated, the BBI camera offers a broadband high-resolution image with a square field-of-view of about ~55"x55". A broadband red filter, with a ~3nm passband centred around 630 nm is placed upstream of the camera. THEMIS BBI camera thus currently provides images or the red visible continuum. |
| |
| THEMIS BBI camera is currently a 2000 x 2000 pixels Andor Zyla camera. This camera relies on the scientific CMOS technology (active-pixel sensor). This offers a high quality image of a subset of the THEMIS field-of-view with a very fast read-out, enabling the capture of a burst of images capture (up to 40 images/second) that are ideal for post image reconstruction. <html><font color="#ff9900"> Camera acquisition settings can be changed by the user in the THEMIS control room. Acquisition is left to the needs and appreciation of the user. </font></html>\\ | THEMIS BBI camera is currently a 2000 x 2000 pixels Andor Zyla camera. This camera relies on the scientific CMOS technology (active-pixel sensor). This offers a high quality image of a subset of the THEMIS field-of-view with a very fast read-out, enabling the capture of a burst of images capture (up to 40 images/second) that are ideal for post image reconstruction. <html><font color="#ff9900"> Camera acquisition settings can be changed by the user in the THEMIS control room. Acquisition is left to the needs and appreciation of the user. </font></html>\\ |
| <columns 100% 60%> | <columns 100% 60%> |
| |
| ==== (10) Spectrograph slit at F2 ==== | ==== (10) Instrument selector ==== |
| | |
| | A translation stage that enables to (dis-)engage a mirror that direct the light beam either toward the MTR2 long slit spectrograph of toward the IBIS 2.0 spectro-imager |
| | |
| | |
| | ==== (11) Spectrograph slit at F2 ==== |
| |
| The second optical focus F2 hosts the entrance slit of the spectrograph. <html><font color="#ff9900"> THEMIS currently offers 2 slit configurations. </font></html> | The second optical focus F2 hosts the entrance slit of the spectrograph. <html><font color="#ff9900"> THEMIS currently offers 2 slit configurations. </font></html> |
| When polarimetric observations are performed, because of the latter need of a dual beam polarimetric output, the field of view must be reduced to 2'x 1' (along the slit length). <html><font color="#ff9900"> The orientation of the slit relatively to the field of view can be modified. Typical solar observation permits to put the slit align with the solar north or parallel to the solar equator. </font></html> | When polarimetric observations are performed, because of the latter need of a dual beam polarimetric output, the field of view must be reduced to 2'x 1' (along the slit length). <html><font color="#ff9900"> The orientation of the slit relatively to the field of view can be modified. Typical solar observation permits to put the slit align with the solar north or parallel to the solar equator. </font></html> |
| | |
| ==== (11-12) Slit-jaw filter & camera === | ==== (12-13) Slit-jaw filter & camera === |
| |
| If the slit-jaw slit configuration has been chosen at F2, the light not entering the spectrograph is captured by the slit-jaw camera. Slit-jaw images offers the context images of the spectrograph slit and allows a precise knowledge of the localisation of the slit. | If the slit-jaw slit configuration has been chosen at F2, the light not entering the spectrograph is captured by the slit-jaw camera. Slit-jaw images offers the context images of the spectrograph slit and allows a precise knowledge of the localisation of the slit. |
| |
| As almost all the remaining 15 watts of radiative power are then directed toward the camera, filters shall be place upstream of the camera to reduce the light flux. Presently a green continuum filter at XXX nm, with a 10 nm passband is used. | As almost all the remaining 15 watts of radiative power are then directed toward the camera, filters shall be place upstream of the camera to reduce the light flux. Presently a green continuum filter at 540 nm, with a 10 nm passband is used. |
| |
| The slit-jaw camera is currently a ZWO ASI 178MM camera capturing the F2 field-of-view on a 3000x2000 pixels array. It's a CMOS camera. Without polarimetry, the field of view is 2'x2', while it is reduced to 2'x1' when polarimetric analysis are carried. | The slit-jaw camera is currently a ZWO ASI 178MM camera capturing the F2 field-of-view on a 3000x2000 pixels array. It's a CMOS camera. Without polarimetry, the field of view is 2'x2', while it is reduced to 2'x1' when polarimetric analysis are carried. |
| <columns 100% 60%> | <columns 100% 60%> |
| |
| ==== (13) MTR2 spectrograph ==== | ==== (14) MTR2 spectrograph ==== |
| |
| The THEMIS spectrograph is an essential block of the THEMIS instrumentation that enable the formation of the solar spectrum and its detailed analysis. | The THEMIS spectrograph is an essential block of the THEMIS instrumentation that enable the formation of the solar spectrum and its detailed analysis. |
| [[technical:mtr2| More complete information shall be obtain on the MTR2 description webpage.]] In particular, user can check the list of [[technical:mtr2:maskplates | existing masks]] (the physical wavelengths selector within the spectrograph) to have an idea of possible line observation combination. | [[technical:mtr2| More complete information shall be obtain on the MTR2 description webpage.]] In particular, user can check the list of [[technical:mtr2:maskplates | existing masks]] (the physical wavelengths selector within the spectrograph) to have an idea of possible line observation combination. |
| |
| ==== (14) Spectral cameras ==== | ==== (15) MTR2 spectral cameras ==== |
| |
| At the exit of the spectrograph, several cameras are placed so that to record spectral images (lambda,y) simultaneously in different wavebands. The spectrographic images have a typical spectral range of 6-7 Å (0.6-0.7 nm) depending of the wavelength. The spatial direction has an extend of 1' when performing polarised observations, 2' otherwise. When performing polarimetric observations, two spectrographs are fitted on the camera field-of-view, each including the opposite polarimetric state (e.g. I+V and I-V Stokes). | At the exit of the spectrograph, several cameras are placed so that to record spectral images (lambda,y) simultaneously in different wavebands. The spectrographic images have a typical spectral range of 6-7 Å (0.6-0.7 nm) depending of the wavelength. The spatial direction has an extend of 1' when performing polarised observations, 2' otherwise. When performing polarimetric observations, two spectrographs are fitted on the camera field-of-view, each including the opposite polarimetric state (e.g. I+V and I-V Stokes). |
| |
| |
| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=:results:gallery:schema:spectro_synoptic.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=:results:gallery:schema:spectro_synoptic.png" style="width:90%; height: auto;"></a></html> \\ | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=:science:gallery:schema:spectro_synoptic.png"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=:science:gallery:schema:spectro_synoptic.png" style="width:90%; height: auto;"></a></html> \\ |
| Cartoon of optical path and systems of the THEMIS MTR2 spectrograph. \\ | Cartoon of optical path and systems of the THEMIS MTR2 spectrograph. \\ |
| |
| </columns> | </columns> |
| |
| | ==== (16-17) IBIS 2.0 spectro-imager (in construction) ==== |
| | |
| | [[https://www.ibis20.inaf.it/| Interferometric BIdimensional Spectrometer - IBIS 2.0]] spectro-imager. |
| |
