HIRES System summary Roma 15 Giugno 2015 Outline

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HIRES: System summary Roma – 15 Giugno 2015

HIRES: System summary Roma – 15 Giugno 2015

Outline • • • Modular configuration Instrument Description System Architecture Cost estimation Conclusions 2

Outline • • • Modular configuration Instrument Description System Architecture Cost estimation Conclusions 2 Roma – 15 Giugno 2015

Top level requirement Requirement Spectral Res Multiplexing HR Single Obj. Mode >= 150’ 000

Top level requirement Requirement Spectral Res Multiplexing HR Single Obj. Mode >= 150’ 000 1 HR Single Obj. Mode >= 100’ 000 1 MR Multiplexed Mode 10’ 000 -20’ 000 1 -10 (few arcmin Fo. V) 0. 37 -2. 5 Spectral coverage (mm) Min Blue 370 nm wavel Allowed wavel No substantial gaps Wavelength Espresso template for the VIS TBD for IR calibration Stability 10 cm/s for VIS (goal 2 cm/2), TBD for IR throughput Espresso template for the VIS (12%), ECHO template for IR (8 mag s/n 10’ 000 per res element in 100 min or better) HR AO-assisted IFU >= 100’ 000 IFU Polarimetry mode n. a. 4 0. 39 -2. 4 390 nm No substantial n. a. 10 cm/s Espresso template for the VISible, TBD for IR n. a. Espresso template 80% for the VIS(12%), (BVRIYJH) ECHO template for ECHO template IR (8 mag s/n for IR (8 mag s/n 20% 10’ 000 per res (K) element in 100 min element in or better) 100 min or better) Roma – 15 Giugno 2015

E-ELT I/F EELT Interfaces for Scientific Instruments E-TRE-ESO-586 -0252 3. 0 29/07/10 Optical Linear

E-ELT I/F EELT Interfaces for Scientific Instruments E-TRE-ESO-586 -0252 3. 0 29/07/10 Optical Linear FOV Ø 1957. 7 mm Focal length 673878 mm Focal ratio F/17. 48 Plate scale 0, 3 Asec/mm Stability 0. 3 arcsec rms With GLAO 10 -50 mas rms Roma – 15 Giugno 2015

Fiber Efficiency Roma – 15 Giugno 2015

Fiber Efficiency Roma – 15 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Configurations Fiber MOS and IFU only in YJH Roma – 15 Giugno 2015

Configurations Fiber MOS and IFU only in YJH Roma – 15 Giugno 2015

Configurations UB + VRI +K MOS and IFU Preserved YJH Roma – 15 Giugno

Configurations UB + VRI +K MOS and IFU Preserved YJH Roma – 15 Giugno 2015

Configurations Roma – 15 Giugno 2015

Configurations Roma – 15 Giugno 2015

Roma – 15 Giugno 2015

Roma – 15 Giugno 2015

HIRES Instrument Product Tree HIRES Instrument Spectrograph Modulae common elements B Spectrograph VRI Spectrograph

HIRES Instrument Product Tree HIRES Instrument Spectrograph Modulae common elements B Spectrograph VRI Spectrograph Front end Fiber optics YJH Spectrograph K Spectrograph Calibration Software Polarimetric pickoff Exposure Meters Roma – 15 11 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Slit illumination Roma – 15 Giugno 2015

Slit illumination Roma – 15 Giugno 2015

Front end Roma – 15 Giugno 2015

Front end Roma – 15 Giugno 2015

Slicing Roma – 15 Giugno 2015

Slicing Roma – 15 Giugno 2015

Scrambling Roma – 15 Giugno 2015

Scrambling Roma – 15 Giugno 2015

Spectrographs Roma – 15 Giugno 2015

Spectrographs Roma – 15 Giugno 2015

preslit Roma – 15 Giugno 2015

preslit Roma – 15 Giugno 2015

Mosaic Gratings Roma – 15 Giugno 2015

Mosaic Gratings Roma – 15 Giugno 2015

Detectors e 2 v 9 k X 9 k used in ESPRESSO HAWAII 4

Detectors e 2 v 9 k X 9 k used in ESPRESSO HAWAII 4 RG Roma – 15 Giugno 2015

Main Parameters Parameter Input slit length Beam aperture at slit Main collimator Collimated beam

Main Parameters Parameter Input slit length Beam aperture at slit Main collimator Collimated beam on main disperser Main disperser Dichroics and field lenses/mirrors Transfer collimator Collimated beam after transfer collimator Collimated beam after cross-disperser Beam on detector Detector ESPRESSO-VLT 10 mm HIRES 31 mm F/10 x F/15 Parabola f=3 m double pass 300 mm x 200 mm R 4 echelle, 1. 2 m x 0. 2 m Close to the intermediate focus Sphere f=1. 5 m Parabola f=2. 25 m 150 mm x 100 mm 225 mm x 150 mm 120 mm x 205 mm F/2. 6 x F/2. 6 9 k 2 9 cm x 9 cm F/1. 7 x F/1. 0 (IR) F/2. 2 x F/1. 3 (VIS) 4 k 2 6 cm x 6 cm (IR) 9 k 2 9 cm x 9 cm (VIS) Roma – 15 Giugno 2015

Polarimetric arm Roma – 15 Giugno 2015

Polarimetric arm Roma – 15 Giugno 2015

MOS Roma – 15 Giugno 2015

MOS Roma – 15 Giugno 2015

System Team • It is integral part of the HIRES Project Office • It

System Team • It is integral part of the HIRES Project Office • It is lead by the HIRES System Engineer and SW System Engineer • It is composed by – Architects (depending on project phase) • Optical, Mechanical, Electrical, Thermal, Software – AIV manager – SW team – Sub-System Engineers Roma – 15 24 Giugno 2015

Product Breakdown Structure Polarimetric pickoff #: B, VRI, YJH, K SS Project Management Optical

Product Breakdown Structure Polarimetric pickoff #: B, VRI, YJH, K SS Project Management Optical Architecture Mechanical Architecture PA/QA Electronical Architecture AIV Software Architecture Thermal Architecture Front End # Spectr SS Project Management SSystem Engineering PA/QA AIV Science Support SSystem Engineering PA/QA AIV Slit Subsystem Optical Components Optical Bench Echelle Dewar and Detectors Dichroics ADC SSystem Engineering OPS Optical Components Optical Bench Fiber Link SS Project Management Calibration SS Project Management AIV SSystem Engineering Fibers PA/QA Scrambler Science Support Optical Bench Thermal sys. Calib Lamp Thermal sub-sys. SSystem Engineering PA/QA TCCD MOS? DAS Fibers Optical Components Toggling Mechanicsm DRS Deployment mech Optical Bench Vacuum Vessel SS Project Management SW System Engineering AIV Optical Components Software Shutter Exposure Meters SS Project Management SSystem Engineering PA/QA AIV Laser Comb Optical Components Fabry Perot TCCD Fibers Roma –Optical Bench 15 25 Giugno 2015

Hardware cost estimation Unit FE B VRI YJH K Calibration unit SW (ICS+DRS) Adds

Hardware cost estimation Unit FE B VRI YJH K Calibration unit SW (ICS+DRS) Adds on Cost Reduced (2 mod) k€ 3. 710, 00 k€ 4. 712, 50 k€ 7. 992, 50 k€ 9. 422, 50 k€ 5. 587, 50 k€ 2. 620, 00 k€ 100, 00 k€ 3. 100, 00 Total Contingency (20%) Gran total k€ 2. 710, 00 k€ 7. 992, 50 k€ 9. 422, 50 k€ 1. 320, 00 k€ 100, 00 k€ 37. 245, 00 k€ 21. 545, 00 k€ 7. 449, 00 k€ 4. 309, 00 k€ 44. 694, 00 k€ 25. 854, 00 Full Optical Coudè will require 7 -8 M€ in addition Roma – 15 Giugno 2015

Technical Readiness Level Requirement Spectral Resolution Compliance C TRL 9 Heritage Harps, Espresso, XShooter,

Technical Readiness Level Requirement Spectral Resolution Compliance C TRL 9 Heritage Harps, Espresso, XShooter, Crires, Giano Wavelength range C Spatial Resolution Entrance Aperture C C 7 (there a lot of examples of reduced wavelength the modular concept preserves the high level of TRL) 7 9 for the 2 point sources Wavelength precision and Accuracy C 7 for the 10 sources 7 for the Visible K-mos Espresso Stability Sky subtraction Polarimetry Other C C 6 for the Infrared 9 9 6 6 Carmenes Crires, Carmenes Harps Pepsi Harps Espresso ? ? Harps, Espresso Roma – 15 Giugno 2015

Conclusion I: feasibility • An Instrument able to provide High resolution spectroscopy (100000) in

Conclusion I: feasibility • An Instrument able to provide High resolution spectroscopy (100000) in a wide wavelength range (0. 37 to 2. 5 um) IS FEASIBLE with the current available technology. • It is anyway possible to foreseen dedicated R&D to maximize performances and or reduce the cost. – – – – Larger Detector (mainly IR side) Larger Pixel size Curved Detector Grating Ruling processes Laser Frequency Comb Stabilized Fabry-Perot Fibers throughput Roma – 15 Giugno 2015

Conclusion II: time adaptability • Hires modularity will guarantee TO FULLFILL ALL THE TLR

Conclusion II: time adaptability • Hires modularity will guarantee TO FULLFILL ALL THE TLR REQUIREMENT in the best way. On the other hand will also allow different timeline for the different spectrographs and add-on pending on the available money. It is possible to consider an early delivery of one or two arms, with a lighter front end; the other arms and full capabilities (polarimetric, MR and HR 2 modes) can be added later. Roma – 15 Giugno 2015

Conclusion III: layout adaptability • Hires modularity will also allow DIFFERENT CONFIGURATIONS on the

Conclusion III: layout adaptability • Hires modularity will also allow DIFFERENT CONFIGURATIONS on the telescope, namely different location of the modules on the platform (Nasmith and Coudè) within the boundary defined by the fibers throughput. This means for example that the location of the different modules may also adapt with the development of the telescope. • The telescope I/F are evolving, so it is necessary to be involved in the discussion at least as auditor. Roma – 15 Giugno 2015

Conclusion IV: telescope pupil • Beeing Hires a fiber fed instrument its main performances

Conclusion IV: telescope pupil • Beeing Hires a fiber fed instrument its main performances will NOT BE INFLUENCED by reduced telescope M 1 without inner rings (except for the observation depth). Roma – 15 Giugno 2015

Conclusion V: AO dependance • In addition for the science cases that needs Single

Conclusion V: AO dependance • In addition for the science cases that needs Single targets where there are no background sources that could contaminate the observation, at short wavelength observations , observations of extended sources, the AO will not increase significantly the performances. This means that Hires is able to provide the required performances even without it. Roma – 15 Giugno 2015

Conclusion VI: Mass issue • Critical point can be found in the Overall Mass

Conclusion VI: Mass issue • Critical point can be found in the Overall Mass of the Instrument which could be between 30 and 40 Ton. Despite of that the modularity of the System will help allowing a distribution of the masses that can be optimized to minimize the impact on the platforms. Roma – 15 Giugno 2015

Conclusion • All this conclusions drive to the main good results that Hires can

Conclusion • All this conclusions drive to the main good results that Hires can be modulated to provide reasonable fraction of the required science with almost ANY early 1 st light of ANY ELT. Roma – 15 Giugno 2015

Grazie! Roma – 15 Giugno 2015

Grazie! Roma – 15 Giugno 2015

Ub echellogram Roma – 15 Giugno 2015

Ub echellogram Roma – 15 Giugno 2015

VRI echellogram Roma – 15 Giugno 2015

VRI echellogram Roma – 15 Giugno 2015

YJH echellogram Roma – 15 Giugno 2015

YJH echellogram Roma – 15 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Instrument Layout Roma – 15 Giugno 2015

Roma – 15 Giugno 2015

Roma – 15 Giugno 2015