B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS ESO VLT SECOND GENERATION INSTRUMENTATION Optical designs ESO VLT SECOND GENERATION INSTRUMENTATION Optical designs ANGRA DOS REIS - BRAZIL November 2003 B.Delabre (ESO)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS This presentation will show possible optical designs for ESO second generation VLT instrumentation. All instruments are still in Phase A studies

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS List of VLT second generation instruments: HAWK-I (IR imager) HAWK-I (IR imager) KMOS (multi-objects Integral field spectrograph) KMOS (multi-objects Integral field spectrograph) MUSE (visible integral field spectrograph) MUSE (visible integral field spectrograph) X-SHOOTER (Medium resolution echelle spectrograph from nm) X-SHOOTER (Medium resolution echelle spectrograph from nm) Planet finder (not included in the presentation) Planet finder (not included in the presentation)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS HAWK-I HAWK-I Large field Infrared Imager Large field Infrared Imager Build by : ESO PI : Alan Moorwood (ESO)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Characteristics Field of view 8.0 x 8.0 arc min or 8.5 x 8.5 arc min Field of view 8.0 x 8.0 arc min or 8.5 x 8.5 arc min depending of the selected concept depending of the selected concept Wavelength range 800 – 2500 nm Wavelength range 800 – 2500 nm Scale or arc sec/pixel Scale or arc sec/pixel F/N F/3.8 or F/3.6 F/N F/3.8 or F/3.6 Detector 4k x 4k (18µm pixel) Detector 4k x 4k (18µm pixel) No spectroscopy available ( by design) No spectroscopy available ( by design)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I 3 designs are considered : - Compact dioptric design with small filters - Compact dioptric design with small filters - Larger dioptric design with large filters - Larger dioptric design with large filters - All reflective design with large filters - All reflective design with large filters

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I DESIGN 1 DESIGN 1 Compact dioptric solution Compact dioptric solution 8.5 x 8.5 arc min field 8.5 x 8.5 arc min field

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I 1 m

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I accessible pupil accessible pupil possibility to use standard 2 inches filters possibility to use standard 2 inches filters image quality comparable to pixel size for the entire field image quality comparable to pixel size for the entire field distortion free distortion free no ghost images no ghost images no very high incidence angles on the lenses to avoid extreme sensitivity to element tilts and decentrings, no very high incidence angles on the lenses to avoid extreme sensitivity to element tilts and decentrings, even at the cost of an extra element. even at the cost of an extra element. all spherical surfaces. all spherical surfaces. comfortable back focal distance comfortable back focal distance The thickness and material of the filter must be constant High incidence angles on the filters do not permit an effective use of Narrow band filters

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Pupil aberrations The cold stop is attached to the filter

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Spot diagrams Polychromatic nm Box = 1 pixel

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Spot diagrams 850 – 1000nm Box = 1 pixel

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I DESIGN 2 DESIGN 2 Large dioptric design Large dioptric design 8.5 x 8.5 arc min field

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I This design has the following advantages with respect to the compact design : - Less optical elements (only 5 lenses) - Less optical elements (only 5 lenses) - No restriction on filter material and thickness, two filter - No restriction on filter material and thickness, two filter wheels are accommodated in front of the detector wheels are accommodated in front of the detector - Cold stop outside the objective - Cold stop outside the objective - Relaxed tolerances on lens centerings - Relaxed tolerances on lens centerings - Narrow band filters can be used - Narrow band filters can be used

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I 1.2 m 1.2 m

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Spot diagrams Polychromatic nm Box = 1 pixel

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Pupil for J band Pupil for H band Pupil for K band The cold stop is adjusted for K band, vignetting will occur for J and H

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I DESIGN 3 DESIGN 3 All reflective design All reflective design 8.0 x 8.0 arc min field

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Advantages of this design : - Efficiency (93% without filter) - Efficiency (93% without filter) - Relaxed centering tolerances - Relaxed centering tolerances - Achromatic - Achromatic - Problem of refractive indices at cryogenic temperature does not exist - Problem of refractive indices at cryogenic temperature does not exist Drawbacks of this design : - Large size - Large size - Slightly reduced field of view - Slightly reduced field of view - Distortion is not fully corrected (around %) - Distortion is not fully corrected (around %)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I 2.3 m

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I Axis arc min Axis arc min 4 arc min 25 μm arc min 25 μm arc min arc min arc min arc min arc min arc min Axis Axis arc min arc min arc min arc min arc min arc min arc min arc min Image quality 80% geometrical energy (diameter)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I The 3 concepts are represented at the same scale

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE MUSE MUSE Visible integral field spectrograph Visible integral field spectrograph Built by external consortiums : Lyon- Cambridge – Durham – Leiden – Oxford – Postdam - Zurich PI : Roland Bacon (Lyon)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Integral field spectrograph Spectral range : 465 – 930 nm Field of view : 1.0 x 1.0 arc min (low resolution mode) 7.5 x 7.5 arc sec (high resolution mode) 7.5 x 7.5 arc sec (high resolution mode) Spatial sampling: 0.2 arc sec (low resolution mode) arc sec (high resolution mode) arc sec (high resolution mode) Spectral sampling : 0.1 (LR) or (HR) arc sec/pixel Spectrographs : 24 single mode spectrographs equipped with 4K x 4K CCD equipped with 4K x 4K CCD Resolving power : R=3000 at 700 nm for 2 pixels resolving element Possibility to operate with adaptive optics

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Opticalbench 2 x 4 spectrographs spectrographs AO module 2 x 4 2 x 4spectrographs 1000 mm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 2 x 4 spectrographs AOmodule Optical bench Calibration Adaptor flange 1000 mm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Spectrographcryostat Image slicers cryostat cryostat cryostat Spectrograph Spectrograph Spectrograph 2100 mm 400 mm Spectrograph Spectrograph Spectrograph Spectrograph Spectrograph Spectrograph Spectrograph Spectrograph 1000 mm SPECTROGRAPH RACKS ( 2 X 4 SPECTROGRAPHS) ( 2 X 4 SPECTROGRAPHS)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The fore optics The fore optics

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The fore optics consists of : - An optical relay to produce an image of the telescope focus on a field splitter (this optic has 2 magnifications) - An optical relay to produce an image of the telescope focus on a field splitter (this optic has 2 magnifications) - An optical derotator - An optical derotator - A field splitter which cut the field of view in 24 sub-fields - A field splitter which cut the field of view in 24 sub-fields - 24 transfer optics to send the light to the spectrographs - 24 transfer optics to send the light to the spectrographs

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Adaptorflange NasmythFocus Derotator F/25 focus Field splitter Large field (1.0 x 1.0 arc min) 1035 mm 600 mm Optical relay

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Circle = 0.1 arc sec Large field Spot diagrams mm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Small field (7.5 X 7.5 arc sec) F/200 Field splitter Derotator Nasmyth focus AdaptorFlange Exchangeablelenses Optical relay

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Circle = 0.05 arc sec mm Small field Spot diagrams

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 203 mm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Adaptorflange NasmythFocus Derotator F/25 focus Field splitter Large field 1035 mm 600 mm Adaptiveoptics Optical bench Calibration Calibration unit unit

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Field slicer and transfer optics (developed at CRAL by B.Lanz) The 1 x 1 arc min field of view is cut in 24 fields of 20 x 7.5 arc sec A transfer optic is used to send individually each field to an image slicer This optic produces also an anamorphic magnification : F/25 to F/104 (spatial) F/25 to F/104 (spatial) F/25 to F/208 (spectral) F/25 to F/208 (spectral)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The Image slicers developed at CRAL by B.Lanz and F.Henault

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The Spectrographs

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE A classical design will be too expensive A classical design will be too expensive No glasses like CaF2 or FK54…. can be afforded. Only glasses with a price similar (max x2.5) to BK7 should be used if possible. No glasses like CaF2 or FK54…. can be afforded. Only glasses with a price similar (max x2.5) to BK7 should be used if possible. The spectrographs should be small to reduce cost, volume and weight The spectrographs should be small to reduce cost, volume and weight No mechanical functions are permitted (no refocusing and no exchange of dispersive elements) No mechanical functions are permitted (no refocusing and no exchange of dispersive elements) Design guidelines :

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Detector 4K x 4K with 15 microns pixels Detector 4K x 4K with 15 microns pixels Entrance F/N F/4.5 (slit direction) Entrance F/N F/4.5 (slit direction) F/9.0 (dispersion) F/9.0 (dispersion) Output F/N F/2.0 (slit direction) Output F/N F/2.0 (slit direction) F/4.0 (dispersion) F/4.0 (dispersion) Flat entrance slit Flat entrance slit Entrance pupil 3 m after the slit Entrance pupil 3 m after the slit Dispersive element : VPH 700 mm-1 Dispersive element : VPH 700 mm-1 Pupil size 45 x 90 mm Pupil size 45 x 90 mm Wavelength range 465 – 930 nm Wavelength range 465 – 930 nm Estimated transmission around 0.85 without VPH Estimated transmission around 0.85 without VPH Characteristics :

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE No expensive glasses is equivalent to poor chromatic correction No expensive glasses is equivalent to poor chromatic correction Chromatism is compensated by a tilt of the field lens and the detector Chromatism is compensated by a tilt of the field lens and the detector The VPH is not operating in a perfect parallel beam. It has some contributions to the correction of image quality The VPH is not operating in a perfect parallel beam. It has some contributions to the correction of image quality No refocusing required for correction of temperature variation (the variation of focus position is 4 µm/°C for the current design) No refocusing required for correction of temperature variation (the variation of focus position is 4 µm/°C for the current design) Exchanges of dispersive elements or spectral ranges are not possible Exchanges of dispersive elements or spectral ranges are not possible

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 920 mm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 465 nm 540 nm Boxes are 2 x 2 pixels

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 620 nm 698 nm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 775 nm 852 nm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 930 nm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE WavSlit mm axis Rms spot diameters

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The collimator is made of 4 lenses in 3 groups The collimator is made of 4 lenses in 3 groups The materials are BK7 (3 lenses) and PBH1 (1 lens) The materials are BK7 (3 lenses) and PBH1 (1 lens) The field curvature is not corrected (the correction is done by a cylindrical surface on back side of the cryostat window. The field curvature is not corrected (the correction is done by a cylindrical surface on back side of the cryostat window. Collimator

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS -MUSE The camera includes 5 lenses made of BK7-NaLF7-BK7 PbH1-PbH1. The field lens is not included in the camera The Camera

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The field lens will also act as cryostat window. A cylindrical surface on its back side will correct the field curvature of the slit and collimator. The lens is perpendicular to the CCD The full cryostat is decentered and tilted with respect to the camera axis The field lens

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE MUSE ADAPTIVE OPTICS MUSE ADAPTIVE OPTICS

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE MUSE IS COMPATIBLE WITH 3 OPERATION MODES: MUSE IS COMPATIBLE WITH 3 OPERATION MODES: - WITHOUT ADAPTIVE OPTIC - WITHOUT ADAPTIVE OPTIC - TELESCOPE ADAPTIVE SECONDARY - TELESCOPE ADAPTIVE SECONDARY - MULTI-CONJUGATE ADAPTIVE OPTICS - MULTI-CONJUGATE ADAPTIVE OPTICS No major modification of MUSE are requested to change from one operation mode to another.

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE TELESCOPE ADAPTIVE SECONDARY TELESCOPE ADAPTIVE SECONDARY (ONE DEFORMABLE MIRROR) (ONE DEFORMABLE MIRROR)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE LGSs attached to telescope center piece rotate like telescope pupil at Nasmyth LGSs attached to telescope center piece rotate like telescope pupil at Nasmyth 1’ Scientific FOV rotates like Nasmyth field rotation 1’ Scientific FOV rotates like Nasmyth field rotation Differential rotation between LGSs and scientific FOV Differential rotation between LGSs and scientific FOV LGS focus varies from km LGS focus varies from km LGS Nasmyth varies from: mm LGS Nasmyth varies from: mm At Nasmyth focal plane LGS footprint varies from: 12-5mm At Nasmyth focal plane LGS footprint varies from: 12-5mm Nasmyth pixel scale is 582µm/” Nasmyth pixel scale is 582µm/” => LGS at 1’x√2/2+ half LGS foot-print ~70” off-axis => LGS at 1’x√2/2+ half LGS foot-print ~70” off-axis FOV for LGS-WFS is >4” (spot elongation+3σ seeing) FOV for LGS-WFS is >4” (spot elongation+3σ seeing)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Laser& NGS light passes through Plate 1 Laser& NGS light passes through Plate 1 Plate 2 reflects only the LGS light toward Plate 1 Plate 2 reflects only the LGS light toward Plate 1 Plate 2 translates along optical axis to compensate for LGS focus Plate 2 translates along optical axis to compensate for LGS focus Plate 1 has 4 small mirrors, located in the central obstruction of each laser beam to reflect the LGS light toward the WFS Plate 1 has 4 small mirrors, located in the central obstruction of each laser beam to reflect the LGS light toward the WFS Plate 1 rotates to compensate for LGS rotation and SH pupil rotation Plate 1 rotates to compensate for LGS rotation and SH pupil rotation WFSs and Plate 1 rotate together WFSs and Plate 1 rotate together Plate 2 has a notch filter in the center ~1.5’ field to block the scattered laser light and transmit the scientific field Plate 2 has a notch filter in the center ~1.5’ field to block the scattered laser light and transmit the scientific field Plate 2 has a dichroic slit in the reflective area to transmit the NGS toward MUSE Plate 2 has a dichroic slit in the reflective area to transmit the NGS toward MUSE Plate 2 rotates for the acquisition and tracking of the NGS in the slit Plate 2 rotates for the acquisition and tracking of the NGS in the slit NGS field rotation is compensated with the 3’ derotator NGS field rotation is compensated with the 3’ derotator

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 80 km Laser focal plane LGS derotator table LGS focus tracking Mirror/dichroic Scientific field LGS reflected light NGS light LGS Pupil image LGS collimator NASMYTH FOCAL PLANE Plate 1 Plate 2

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 180 km Laser focal plane LGS focus tracking Mirror/dichroic Scientific field LGS reflected light NGS light LGS derotator table LGS Pupil image LGS collimator Plate 1 Plate 2

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE LGS mirror Notch filter NGS acq. slit Functions: LGS mirror (at 70” off-axis) LGS focus correction Field stop for laser light (1.5’-3’) LGS dichroic/notch filter (0-1.5’) NGS selector & transmitter Plate 2

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Natural guide Star area LGSbeam Scientificfield LGS at 160 km Plate 1 Natural guide Star area LGSbeam Scientificfield Plate 1 LGS at 80 km

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE FoV 140” Fast Read-Out CCD Pupil Re- imaging Lens XY Table Lenslet Array

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE MULTI CONJUGATES ADAPTIVE OPTICS MULTI CONJUGATES ADAPTIVE OPTICS (2 DEFORMABLE MIRRORS + TIP-TILT MIRROR) (2 DEFORMABLE MIRRORS + TIP-TILT MIRROR)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE OPTICAL COMPONENTS OPTICAL COMPONENTS Ground layer deformable mirror : 180 mm 8.5 km layer deformable mirror : 150 mm Tip-tilt mirror : 180 mm 3 lenses objective 1 total reflection prism 1 pupil relay lens 2 folding mirrors

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE The full system is located between the adaptor flange and the Nasmyth focus (250 mm only are available) The image produced is identical and at the same location than the original Nasmyth image in order to operate MUSE with or without Adaptive Optics with no modification of the instrument.

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Characteristics Characteristics 4 laser guide stars at 70 arc sec off axis 3 arc min field of view for natural guide star Wavelength range nm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 16:15:16 Scale: Oct-03 XZ MM Tip-tilt Mirror 8.5 km layer Ground layer Nasmyth Focus Pupil relay Lens Objective (gamma=1) Folding Mirror MUSE Multi conjugate AO (front view)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE 16:23:07 13-Oct MM MUSE Multi conjugate AO (side view) Adaptor flange 8.5 km layer Objective Focus (F/15)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE Optical bench Natural Guide star FocusCompensationplate WSdetector WSdetector Derotator PupilReimaginglens Pupil Reimaging prism Large field objective rotates like the field rotates like the pupil

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Multi-object integral field spectrograph Multi-object integral field spectrograph for near IR ( nm)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Another way of building multi-object integral field spectrographs The selection of objects is a very critical problem in IR multi-object spectroscopy because it requires a lot of cryogenic functions. Based on the concept of a KMOS study done for ESO, we have developed the baseline of a new solution which could strongly improve the reliability of the instrument at the cost of a small increase of background (2 warm mirrors).

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOS Main features of the new concept : - Object selection done at ambient temperature (only 2 warm reflections) - Object selection done at ambient temperature (only 2 warm reflections) - Small optical derotator inside or outside the cryostat - Small optical derotator inside or outside the cryostat - The instrument doesn’t need to rotate - The instrument doesn’t need to rotate - The entrance window is small - The entrance window is small - Only two cryogenic functions (derotator and grating exchange mechanism) - Only two cryogenic functions (derotator and grating exchange mechanism)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOS THE OBJECT ACQUISITION THE OBJECT ACQUISITION SYSTEM SYSTEM

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Field mirrors (1 x 1 arc min) (36 mirrors ) Pupil mirrors (steering mirrors) Telescope focal plane TELESCOPE TO DEROTATOR Each field mirror images a Pupil on its own steering mirror

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS STEERING MIRRORS TELESCOPE FOCAL PLANE OPTICAL DEROTATOR OBJECT SELECTION WARM PART COLD PART Pseudo pupil to image slicers Field mask

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Main advantages of this concept : Main advantages of this concept : - Steering mirrors are accessible - Field slicer can be exchanged to have flexibility for object selection - Small entrance window for the cryostat - The instrument does not rotate, requirement on flexure are much easier to fulfill. to fulfill. - The spectrograph operates horizontal. Most of the lens mounting problems disappear. - High reliability (only two cryogenic functions) - Possibility to include a warm viewing system for object acquisition.

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS THE IMAGE SLICERS This devices have been developed at the LAM in Marseille (France) A presentation by Eric Prieto will be (or has been) given during this workshop All reflective slicers could also be used.

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Object selection deviceImageslicers Spectrograph

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS THE SPECTROGRAPH THE SPECTROGRAPH

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS The following table summarizes the characteristics of the instrument: Entrance F/N F/17 (spatial) F/34 (spectral) Output F/N F/3.1 (spatial) F/6.2 (spectral) Entrance field of view 2 slits of 400 mm separated by 200 mm Detector 4K x 4K (18 µm pixel) Pupil size (on the grating) 100 x 50 mm 100 x 50 mm Magnification Scale (spatial) arc sec / pixel Scale (spectral) arc sec / pixel Entrance pupil position infinity Slit curvature flat

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Focal length: 1700 mm Pupil diameter: 100 mm Wavelength range: 1000 – 2500 nm Field of view: 200 x 400 mm The Collimator

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Caf2Baf2 IRG3 Silica

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS J Band: 400 mm- 1 R=4070 (2 pixels) between 1060 and 1345 nm H Band: 300 mm- 1 R=4660 (2 pixels) between 1430 and 1800 nm K Band: 225 mm- 1 R=4340 (2 pixels) between 2000 and 2440 nm List of gratings

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Focal length: 310 mm Pupil diameter: 100 mm Wavelength range: 1000 – 2500 nm Field of view: 74 x 74 mm The Camera

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Caf2 Caf2 Irg3Silica SilicaZnSe Aspheric

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS Image quality : Image quality has been computed with a full circular pupil of Image quality has been computed with a full circular pupil of 100 x 100 mm. In fact the spectrograph has a nominal pupil 100 x 100 mm. In fact the spectrograph has a nominal pupil of 100 x 50 mm. of 100 x 50 mm. The full pupil of 100 x 100 mm allows to collect the light which The full pupil of 100 x 100 mm allows to collect the light which is diffracted by the slicers. is diffracted by the slicers.

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS J Band Wavelength 1060 nm 1130 nm 1200 nm 1275 nm 1345 nm Positions mm mm mm -9.0 mm -0.2 mm Axis mm mm % geometrical energy diameter

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS H Band Wavelength 1430 nm 1500 nm 1600 nm 1700 nm 1800 nm Positions -35.9mm mm mm -9.9 mm -0.5 mm Axis mm mm % geometrical energy diameter

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS K Band Wavelength 2000 nm 2100 nm 2200 nm 2320 nm 2440 nm Positions mm mm mm -8.9 mm -0.4 mm Axis mm mm % geometrical energy diameter

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS X - Shooter Built by : Astron – Copenhagen Obs. – ESO - INAF - Obs Paris-Meudon PI’s : D. D’Odorico – F. Hammer - L. Kaper - R.Pallavicini – P.K. Rasmussen P.K. Rasmussen Medium resolution Echelle spectrograph

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER Characteristics : Instrument located at Cassegrain Focus Fore optics : light split in 3 channels by dichroic plates 3 optical relays F/13.6 to F/7.5 3 optical relays F/13.6 to F/7.5 2 of these relays include an ADC 2 of these relays include an ADC Spectrographs : 3 “UVES” type spectrographs – Echelle format Blue 300 – 550 nm Blue 300 – 550 nm Red 500 – 1000 nm Red 500 – 1000 nm IR 1000 – 1800 nm (or 2500 ?) IR 1000 – 1800 nm (or 2500 ?)

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER 14:26:05 ESO 07-Nov MM 14:29:26 Red channel 500 – 1000 nm Blue channel 300 – 550 nm TelescopeFocus ADC ADC Red mirror 2nd dichroic 1 St dichroic 14:59:26 IR Channel nm

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER b PRESLIT OPTICS – SPOT DIAGRAMS IR Channel nm Red channel 500 – 1000 nm Blue channel 300 – 550 nm AXIS 5 ARCSEC 10 ARCSEC Circle = 0.5 arcsec

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER Entrance F/N F/7.5 Output F/N F/2.7 Entrance field of view 11 arc sec (3.2 mm) Detector 2K x 4K (15 µm pixel) Pupil size 100 mm 100 mm Collimator focal length 750 mm Camera focal length 270 mm Scale (spatial) 0.14 arc sec/pixel Resolving power 4500 (for 1 arc sec slit) Order separation between 110 and 200 pixels BLUE Spectrograph

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER 16:06:40 Position: 7 05-Nov MM Parabolicmirror F/2.7 Camera 60 deg silica prisms 180 mm-1 grating Blazed at 42 deg Slit 2K x 4K CCD X-Shooter Blue spectrograph Folding mirror

B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTER orders orders nm nm X=-18.8 y= nm nm X=-9.4 y= nm nm X=-0.2 y= nm 522.2nm X=7.7 y= nm nm X=15.2 y= nm nm X=-16.3 y= nm nm X=-8.2 y= nm nm X=-0.1 y= nm nm X=6.7 y= nm nm X=13.4 y= nm X=-13.5 y= nm X=-13.5 y= nm X=-6.8 y= nm X=-6.8 y= nm X=-0.1 y= nm X=-0.1 y= nm X=5.7 y= nm X=5.7 y= nm X=11.4 y= nm X=11.4 y= nm nm X=-11.4 y= nm nm X=-5.8 y= nm nm X=-0.0 y= nm nm X=4.9 y= nm nm X=9.8 y= nm nm X=-10.3 y= nm nm X=-5.2 y= nm nm X=-0.1 y= nm nm X=4.4 y= nm nm X=9.1 y= % geometrical energy (diameter)