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--- proj:european_solar_telescope_design_study_est_ds [2011/11/22 17:51] – bgelly
+++ proj:european_solar_telescope_design_study_est_ds [2014/11/19 18:10] (current) – bgelly
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+** The European Solar Telescope (EST)**
+  * The [[http://www.iac.es/proyecto/EST/|European Solar Telescope]] homepage
+  * The [[http://www.astro-east.org/|]] European Association for Solar Telescopes homepage
+----
+\\
+** Design study**
+\\
+[[this>lib/exe/fetch.php?cache=&media=proj:est:est_general.png|{{:proj:est:est_general.png?120 }}]]
+\\ \\
+  * French solar community involvement in EST [[this>_wdata/ThDoc/EST-EAST/Est.html|here]] (including Themis team)
+  * EST/DS Phase III (final) [[this>_wdata/ThDoc/EST-EAST/EST/PhaseIII_Report_422.pdf| report]]
+  * End of Phase III [[this>_wdata/ThDoc/EST-EAST/EST/EoPIII%20Freibug%20/index.htm|meeting slides]] (Freiburg, May 2011)
+\\
+----
+** EST performances requirements **
+| 4.2.1 |Field of view | 2´x2’ (goal 3´x3’).  3’x3’ Mosaic mode with optimal resolution in 1’x1’ patches NOT CONSIDERED FOR OPTICAL DESIGN (implies moving the telescope FoV) |
+| 4.2.2 |Total throughput| >10% (30% telescope; 30% instruments)|
+| 4.2.3 |Wavelength coverage | 390nm to 2.3μm (goal 350 nm to 2.3μm) with AO correction (Coudé focus) 315 nm to 20 μm without AO (Nasmyth focus)|
+| 4.2.4 |Light distribution| Configurable with different fractions of light going to different instrument channels|
+| 4.2.5 |Photon flux | > 2.106 photon/(pixel·s) instrument detector plane|
+| 4.2.6 |Polarimetric sensitivity | 3.10-5 in S/I, S any stokes parameter|
+| 4.2.7 |Polarimetric accuracy | Accuracy to know crosstalk between Stokes parameters|
+| 4.2.8 |Scattered light at 500nm |< 10 % at 1” distance from the scattered light source on the science focal plane, \\ < 1% at 5” distance \\ Coronal observations, flux from the observed line >1 ADU before the background saturates detector |
+|4.2.9 |Sky coverage | Ecliptic above 10º on the horizon (goal full sky)|
+|4.2.10 |Observable radius away from the Sun| 200” from the solar limb \\>5 º (goal >2º) away from the Sun avoiding solar illumination |
+|4.2.11 |Image stability| 0.004”/10s (goal 0.003”/10s) with closed loop AO. \\ 0.05arcsec/10s without closed loop AO |
+|4.2.12 |Image scanning step | Time<0.1s |
+|4.2.13 |Image scanning repeatability| 0.002´´ Spectrographs 1” (TBC) mosaic mode for BB and NB imagers |
+|4.2.14 |mage scanning stability | 0.01” over 1 hour |
+|4.2.15 |Absolute pointing accuracy | <3” |
+|4.2.16 |Open loop tracking accuracy | <1” /10minutes |
+|4.2.17 |Image quality with closed loop MCAO | SR500nm=0.3 (TBC) for 1´FoV and SR500nm=0.4 (TBC) for 30”FoV for r0>20cm. \\ SR500nm=0.15 (TBC) for Ø1´FoV and SR500nm=0.25 (TBC) for Ø30”FoV for r0>10cm |
+|4.2.18 |Closed loop MCAO for near-limb observations |AO low order mode for observations near the limb, using Hα images. Performances TBD|
+|4.2.19 |Image quality without closed loop AO | Image quality degradation <10% seeing conditions for good seeing conditions (r0 =20cm at 500 nm) |
+|4.2.20 |Data flow | Data flux 200GB/sec Data volume 275PB/year |
+|4.2.21 |Maximum time between image acquisitions in mosaic mode | 2s for contiguous subfields \\ 6s for non contiguous subfields |
+//(Table from L. Cavaller (IAC & GranTeCan) & the EST project)//