Measuring the throughput in spectrographs
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1 Measuring the throughput in spectrographs By Gerardo Avila & Carlos Guirao CAOS ( 1 St. Niklausen - ASpekt 2017
2 CAOS group Gerardo Avila Vadim Burwitz Carlos Guirao Jesús Rodriguez 2 St. Niklausen - ASpekt 2017
3 Purposes of our presentation The spectrograph throughput is one of the most important features for astronomy observations. However its measurement is difficult and usually is calculated by extrapolation of individual component efficiencies. We propose a simple method of measuring the overall efficiency at single wavelength by using a laser based device. We demonstrate it on a fiber linked Echelle spectrograph. 3
4 Efficiency of an optical system The optical efficiency of an optical system is defined as the rate of optical energy through the system, divided by the energy coming directly from the source: h= E i E o 100% 4
5 Basic Echelle design Full parabola as collimator Output fibre end 9º CCD Tele-objective X-disperser Échelle 5
6 Echelle spectrograph efficiency The efficiency includes: Fibre link: telescope-fibre coupling, fibre transmission and fibre-collimator coupling Collimator Echelle Cross-disperser (Prism or Grating) Camera CCD 6
7 Fibre link efficiency (1) Pinhole seeing ratio Pinhole lens/fibre misalignment F/# matching and misalignment Polishing quality Fresnel, input and output lenses Lenses misalignment errors and aberrations Internal fibre transmission Focal ratio degradation (FRD) 7
8 Pinhole - seeing ratio 8
9 Fibre link efficiency (2) Typical values Pinhole seeing (when seeing = ø fibre) 50% Polishing quality 95% Fresnel, input and output lenses 92% Lenses misalignment errors 98% Internal fibre transmission (length) 96% Focal ratio degradation (FRD) 60-95% Total (not including seeing) 49-78% 9
10 r ot a imll o C t maeb upt O u scit p Oer bi F er utrepa epocsel T e CAOS Telescope fibre coupling - FRD er utrepa maebt upni 10
11 Telescope fibre input coupling Telescope Image Telescope pupil Fibre F F' Star Telescope pupil Star Fibre 11
12 Fibre coupling With 1x grin-lens With 2x grin-lenses 12
13 Fibre output collimator coupling F/3 f 5mm F/20 13
14 Collimator mirror reflectivity Edmund-Optics coatings for mirrors: 14
15 Echelle grating efficiency CAOS The maximum efficiency of echelles is maintained near the Littrow condition (when angle of incidence equals angle of diffraction) Within each order, the efficiency will be maximum at the middle of the order. Typically reaching 50 to 75%. It drops to about one-half these values at the crossover points (free spectral range) Out of Littrow configuration, the echelle reflectivity reduces rapidly (shadowing effect) 15
16 Echelle orders efficiency Peak efficiency (100%) Green laser 532nm (94%) Correction coefficient:
17 Relative efficiecny CAOS Shadowing effect BN 100 Shadowing in Echelles Grating angle
18 Échelle out of Littrow CAOS The grating angle should be as small as possible in order to approach the Littrow configuration where the efficiency is the maximum. In our FLECHAS design, we found that 9 was the best compromise between the size of the camera objective and the optical table. Full parabola as collimator 9º Output fibre end CCD Tele-Objective X-disperser Échelle 18
19 FLECHAS Spectrograph Parabola f 444 mm, ø 75 mm, Edmund Optics Collimator beam F/18 Pupil 25 mm Échelle 79 li/mm 63º , Thorlabs X-disperser Prism N-F2 60º 60x60x60mm Objective f 200 F/2.8, Canon CCD Atik µm (24 35) 19
20 Fibre link Fibre ø 50 µm and 10 m long, Polymicro FIP Fibre Injection F# F/3 Fibre Output F# F/3 Output lens Doublet f = 5 mm, ø 3 mm, Linos Collimator F# F/18.5 Beam projection at the collimator (pupil) ø 24 mm Fibre image at the collimator (slit equivalent) ø 308 µm 20
21 Optical efficiency according to manufacturer Parabolic Mirror 95 % Échelle 55 % Echelle vignetting 95 % Prism 92 % Canon objective 90 % Fibre efficiency 49%-78 % Spectrograph only 41% Spectrograph + Fibre 20%-32% 21 St. Niklausen Aspekt 2017
22 Internal transmission (%) CAOS Fibre efficiency Fibre transmission (internal) in 20 m. FLECHAS uses the FBP type 20 m FBP FVP Wavelength (nm) 22
23 Transmission (%) CAOS Parabolic mirror reflectivity Lab measurements 100 Reflectivity Enhanced Aluminium Wavelength (nm) 23
24 Transmission (%) CAOS X-disperser. Transmission grating efficiency Lab measurements X-disperser Newport Wavelength (nm) 24
25 Transmission (%) X-disperser. Prism efficiency Lab measurements CAOS 100 Prism N-F x60x60mm Wavelength (nm) 25
26 Measuring prism efficiency 26
27 Transmission (%) Camera efficiency Lab measurements CAOS Canon 200mm F/2.8 EF Wavelength (nm) 27
28 Measurement of the reference flux (100%) 0.5 mm pinhole Iris F/3 Laser 3 X objective 16 X objective Integrating sphere I / V transducer Photo diode 28
29 Measurement of the flux through fibre Laser 0.5 mm pinhole Iris F/3 Fibre 3 X objective 16 X objective Iris F/3 Integrating sphere I / V transducer 29 Photo diode
30 Integration sphere 30
31 Measurements CAOS 31 St. Niklausen Aspekt 2017
32 Measurements Injection in fibre F/3 Laser wavelength 532 nm Peak correction coefficient h= E i E o 100 (%) Fibre efficiency 82.4% Spectrograph only 39.7% 42.2% (*) Spectrograph + fibre 32.7% 34.8% (*) (*) After applying peak correction coefficient 32
33 Conclusions CAOS The efficiency of an instrument is a feature as important as any other (resolution, wavelength range, etc..) Most critical component: the fibre. A bad FDR could cause you loosing 30% of the light (imagine you need a telescope 30% bigger!). Efficiency measurements can be easily performed with lasers (blue, green and red). 33
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