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Astronomy Technology Program Overview

Astronomy Technology Overview TMT 2nd Genera9on instruments

NRC Herzberg

David Loop September 2015

Astronomy Technology Program Overview 2

Program Scope

The NRC Herzberg Astronomy Technology Program (ATP) is •  a science driven effort •  that develops and delivers innova9ve technology,

instrumenta9on, and observatory facili9es •  in support of the NRC parliamentary mandate to

operate and administer astronomical observatories on behalf of the Government of Canada


Stakeholders

•  Canadian astronomy community, represented by CASCA and ACURA

•  Interna9onal observatories that Canada is partnered with, CFHT, Gemini, ALMA, TMT, SKA, VLA

•  Canadian academic & industry technology researchers, with support from NSERC and CFI

•  Government of Canada


Long Range Plan (LRP) ATP priori9es are closely aligned with the Canadian Long Range Plan for Astronomy (LRP)

LRP2000 called for a ‘world observatories’vision, with major focus on Canadian par9cipa9on in ALMA, JWST, TMT, and SKA

LRP2010 reinforced this vision


High Level Outcomes

•  Increased Canadian astronomy & astrophysics science research poten9al

•  Advanced technology innova9on transfer to Canadian industry

•  Increased capacity of highly qualified people in Canada


Business Model

Aligned separately with each interna9onal observatory agreement •  A range of in-‐kind and fee-‐for-‐service labour

delivery •  A range of observatory and community supported

material capital cost funding •  Mul9ple phase, 5 to 10 year collabora9ve

developments, with interna9onal peer reviews


Program Resources

Cri9cal mass of human, infrastructure, and financial resources •  2 sites -‐ Victoria and Pen9cton, with well

established special purpose laboratories •  A new TMT-‐scale Integra9on & Test lab under

construc9on in Victoria •  60 staff -‐ engineers, scien9sts, technicians, and

support staff – matrix organiza9on


NRC Herzberg Key Strengths

Key strengths, •  Multidisciplinary technical and science expertise •  Co-located with strong science researchers •  Efficient matrix structure •  Systems engineering, project management •  Continuity, institutional ‘memory’ •  Collaboration expertise, international reputation •  Strong university and industry engagement

International Peer Review Committee (2009) comments, ‘HIA ranks among the best in the world in astronomy technology

and development for existing and future telescopes’


R&D CompeJJve Ranking

Majority of projects awarded a^er interna9onal compe99on, •  ALMA Band 3 -‐ originally to be done by NRAO, but we

demonstrated that we have the exper9se •  Gemini GPI -‐ LLNL led group competed with U Arizona

led group •  TMT NFIRAOS facility AO system -‐ competed with

Caltech •  TMT WFOS Instrument -‐ competed with Caltech,

Rochester Ins9tute of Technology •  Gemini GLAO -‐ competed with U Arizona & U Durham


World Class R&D ATP has made many world class contribu9ons,

•  ALMA Band 3 receivers -‐ approaching the theore9cal limits of receiver noise performance

•  Wavefront sensors – ATP delivered the 1st on-‐instrument wavefront sensor for CFHT MOS/SIS in 1992 -‐ most major ground and space telescopes have now adopted this approach

•  Integrated Modeling – ATP developed integrated modeling tools that are comparable to the space mission tools developed by JPL -‐ our integrated modeling is being used for TMT, GPI, NFIRAOS

•  Workhorse instruments – ATP has contributed to many workhorse instruments at CFHT, JCMT, Gemini, ALMA

•  AO systems -‐ Gemini ALTAIR system was 9ghtly integrated with the observatory -‐ proved that ‘push-‐budon’ AO opera9on possible


Canada France Hawaii Telescope (CFHT)

•  ATP contributions –  HRCam High Resolution Camera first camera with fast tip-tilt correction –  MOS/SIS multi-object spectrograph and imaging spectrograph –  PUEO adaptive optics system with

curvature wavefront sensor –  MEGAPRIME wide field corrector and

focus stage –  IMAKA GLAO, and SITELLE

instrument studies –  SPIRou NIR cryomechanics –  Next generation ngCFHT/MSE


Gemini Observatories North & South

•  ATP contribu9ons –  OCS Observatory Control System –  GMOS Mul9 Object Spectrographs –  ALTAIR NGS/LGS adap9ve op9cs –  GLAO studies –  Flamingos-‐2 OIWFS On-‐Instrument

Wavefront Sensor –  GPI Gemini Planet Imager –  GRACES fiber link to CFHT ESPADons

hires op9cal spectrograph –  GHOST hires op9cal spectrograph –  MOVIES spectrograph study


Gemini Planet Imager (GPI) • Project management (LLNL) • Systems engineering (HIA) • AO system (LLNL, HIA) • Calibration Unit (JPL) • Coronograph (AMNH) • Science IFS (UCLA, U. Montreal) • Top Level Computer (HIA) • Opto-Mechanical Structure (HIA)


Atacama Large Millimeter Array (ALMA) 66 movable 12 meter antennas ~2012, Atacama, Chile US, Europe, Japan, Chile, Taiwan, Canada 33 GHz to 1 THz in 10 bands

•  ATRG-‐V par9cipa9on –  Band3 cryogenic receivers –  Band1 cryogenic components


Extended Very Large Array (EVLA)

27 movable 25 meter antennas Socorro, New Mexico ~2005, NRAO 1 to 50 GHz

•  HIA par9cipa9on –  WIDAR Correlator,

> 4 million channels, frequency resolu9on < 1 Hz


James Webb Space Telescope (JWST)

6.5 meter infrared telescope ~2018, L2 orbit NASA, ESA, CSA 0.6 to 27 µm wavelengths NIRCam, NIRSpec, MIRI, TFI science instruments

•  ATP par9cipa9on –  John Hutchings, CSA Project Scien9st –  FGS detector, op9cs, mechanics consul9ng, with U de Montreal


Thirty Meter Telescope (TMT)

30 meter op9cal/IR telescope ~2023, Mauna Kea site U Cal, Caltech, Canada, Japan, China, India •  ATP par9cipa9on

–  VLOT precursor design –  System Engineering –  Instrumenta9on

Management –  Telescope & Enclosure –  WFOS, IRMOS, IRIS OIWFS,

and PFI instrument studies –  NFIRAOS Mul9 Conjugate

AO system


Square Kilometer Array (SKA) SKA1-‐Mid 133 dish antennas SKA1-‐Low 130,000 elements UK, Netherlands, Italy, Sweden, Australia, South Africa, India, China, Canada 70 MHz to 20 GHz

•  ATP contribu9ons –  Science Steering Commidee –  Engineering Working Group –  SKA-‐Mid Correlator/Beamformer –  Composite reflector antennas –  Phased array feeds & digital beam forming –  Cryogenic Low Noise Amplifiers –  Single Pixel feed digi9zers


Industry Partnerships ATP has developed Canadian industry partnerships to share our

exper9se, license intellectual property, and engage in collabora9ve research & development.

•  Dynamic Structures Ltd (AMEC, now Empire) -‐ ongoing rela9onship on telescope & enclosure structures

•  TMT NFIRAOS design to spec contracts – INO, ABB, Comdev, Quantum Technologies

•  Nanowave Technologies -‐ produc9on contracts for Band3 and MeerKat cryogenic LNAs and mixer assemblies

•  Daniels Electronics -‐ produc9on contracts for Band3 materials, QA, cartridge body assembly

•  MacDonald Detwiler– SKA correlator project management •  SED Systems – SKA composites manufacturing studies


University Partnerships ATP has developed partnerships with many Canadian universi9es to

collaborate on research & development and provide support. •  ACURA -‐ collabora9ve effort on TMT •  U Toronto -‐ Arc9c site tes9ng, Gemini F2T2 tunable etalon filters,

CFHT IMAKA GLAO study, IRIS instrument •  U Bri9sh Columbia -‐ TMT NFIRAOS, LGS sodium layer, Arc9c site

tes9ng, CFHT IMAKA GLAO study •  U Montreal -‐ GPI instrument, JWST FGS, infrared WFS, SPIRou

instrument •  U Victoria -‐ AO test bench, Raven on-‐sky MOAO demonstrator,

planar antennas, segmented mirror control •  U Laval – SITELLE study, SPIRou instrument, Pyramid WFS •  U Manitoba – low voltage MEMS deformable mirrors •  Dalhousie – cryogenic bolometer tes9ng


InternaJonal CollaboraJons ATP is well respected in the interna9onal astronomy community for its

ability to collaborate on projects. •  ALMA Band3 -‐ NRAO, U Virginia, RAL, ASIAA •  ALMA Band1 -‐ Chile, ASIAA/NTU Taiwan •  TMT IRIS – UCLA, Caltech, NAOJ, U Toronto •  TMT IRMOS – U Florida •  Gemini GPI -‐ LLNL, UCLA, UCSC, JPL, U Montreal, AMNH, UC Berkley •  Gemini GMOS -‐ U Durham, UK ATC •  Gemini GLAO -‐ U Durham, U Arizona •  Gemini GHOST – AAO, ANU •  Gemini MOVIES – U Montreal, Ohio State •  CFHT MegaPrime -‐ CEA-‐DAPNIA, Obs Paris, IAP, CNRS-‐INSU, Sagem •  CFHT SPIRou – Toulouse, U Montreal, Laval, Grenoble, Geneva, OHP •  Raven – U Victoria, Subaru, NAOJ


TMT InstrumentaJon Interests NRC Herzberg is keenly interested in aligning its TMT instrumenta9on interests with the Canadian science community.

ATP has capability and has done preliminary work. •  High resolu9on op9cal spectrograph – recent work on GRACES and GHOST instruments > HROS

•  High resolu9on NIR spectrograph – recent work on SPIRou > NIRES

•  Mul9ple Object AO – recent work on RAVEN and con9nuing technology research > IRMOS

•  Exoplanets – recent work on GPI and con9nuing research on new exoplanet techniques > PFI


Two HROS concepts were compe99vely studied as part of the TMT instrument feasibility study phase in 2005 -‐ 2006. One concept (“MTHR”) originated from the UC Santa Cruz (PI: S. Vogt) – a classical Echelle solu9on , and the other concept (“CU-‐HROS”) was proposed by a University of Colorado team (PI: C. Froning) – a design leveraging image slicing and wavelength division.

HROS Top-Level Requirements


HROS “MTHR” Concept (UCSC)

  “classic” echelle design using a 1m x 3.5m gra9ng mosaic   Very large instrument -‐ total size

10m x 11m x 4m   proven technology – a challenge

to implement at this scale.


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CU-‐HROS Concept Concept uses high performance dichroics and image slicing to divide and conquer... Technology yet to be proven!


HROS 2.0 (John Pazder-NRC)

Technology progress in the last decade seen progress in image slicing, dichroic, VPH grating, and detector capabilities and performance. These technologies are being applied to the NRC-H Gemini GHOST spectrograph to build a super efficient bench spectrograph. These technologies are going to be applied to HROS.


Infra-Red Multi-Object Spectograph (IRMOS)

Wide Field Multi-Object AO + Multi-IFU combines diffraction-limited resolution of TMT with a multiplex advantage that would make IRMOS a workhorse TMT instrument Great scientific potential •  Observe large samples of the first

objects to light up the universe •  Detailed studies of galaxies from the

peak era of star formation •  Metallicities and dynamics of star

clusters


Envisioning a MOAO instrument: IRMOS for TMT

5 arcmin field of regard ~100% sky coverage

Up to 50% Strehl ratio in H-band

8 LGS WFS

~20x 2” IFUs ~20 Deformable Mirrors

~20 Spectrographs ~20 2K NIR Arrays

TMT IRMOS Feasability Study; Eikenberry, Andersen et al. 2006


Canada can build upon MOAO experience gained in last decade

Demonstrated Open Loop Control on-sky using VOLT (Andersen et al.2008) Built CFI-funded Raven – 1st MOAO instrument on 8m class telescope (UVic, NRC, Subaru, 2014-2015)

Lardiere, Andersen, Bradley and the Raven team

Raven Pick-‐off Arms

No AO

GLAO

MOAO

Tradi9onal AO

3 arcminute field


Technologies for MOAO/IRMOS Low voltage MEMS deformable mirrors under development with U Manitoba – bump bonded CMOS drive electronics concept under consideration

Avalanche photodiode (APD) NIR detectors under development by Selex Infrared in collaboration with ESO & UH

•  Small format WFS detectors working in-house

•  2k large format detectors under development for ESA

Pyramid WFSs prototyped on Mont-Megantic with INO & U Laval

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Challenges of MOAO/IRMOS IRMOS is an expensive instrument, even if just the cost of NIR arrays is considered

MOAO is still new and relatively unproven

•  Raven and Canary (ESO MOAO demonstrator) both work, but not as well as closed-loop AO systems

•  The risk of meeting expected performance is still big and it is difficult to retire

•  Calibration is critical for achieving the best system performance

Providing calibration for both the spectrographs and MOAO systems will require clever solutions

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Discussion

Thank-‐you

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