LRP2020 Nov2019townhall Int

LRP2020_Nov2019TownHall_Intro_HAA 2 Kavelaars_DRI 8 vanderMarel_protoplanetary_disks 19 Marois_ExoplanetImg 39 Cote_Gemini-LRP2020 73 McConnachie_WideFieldAstro_LRP2020 89 Ellison_HAA_LRP_discuss 130 LRP2020 town hall introduction

Pauline Barmby & Bryan Gaensler LRP Co-Chairs

Email: [email protected] WWW: casca.ca/lrp2020 Twitter: @LRP2020 Slack: bit.ly/LRP_Slack

LRP2020_Nov2019TownHall_Intro_HAA 2 Why are we here?

Discuss key decisions for the community!

For a given topic: › relevant white papers & their scope? › key recommendations from the community? › relevant timelines, facilities and resources? › key questions, challenges & concerns?

LRP2020_Nov2019TownHall_Intro_HAA 3 Why are we not here?

› summarizing individual white papers (can’t cover every topic) › arguing that a specific project is The Most Important Thing › complaining about (lack of) funding

LRP2020_Nov2019TownHall_Intro_HAA 4 Schedule HAA See http://bit.ly/lrp_th

0915-0930 Digital infrastructure JJ Kavelaars 0930-0945 Protoplanets and disks Nienke van der Marel 0945-1000 Exoplanet imaging Christian Marois 1000-1030 Discussion Bryan Gaensler (moderator) 1030-1100 Coffee break 1100-1115 Gemini Stéphanie Côté 1115-1130 Wide-field OIR surveys Alan McConnachie 1130-1200 Discussion Pauline Barmby (moderator) 1200-1230 Facilitated discussion Sara Ellison 1230-1245 General discussion and wrap-up Sara Ellison (moderator)

LRP2020_Nov2019TownHall_Intro_HAA 5 Logistics

› Meeting is being Zoomed for remote participation, recorded for LRP panel use › Speakers: please repeat questions/comments so they’re recorded › Slides will be made public unless requested › Backchannels: - LRP2020 Slack #town-halls channel - Twitter #LRP2020

LRP2020_Nov2019TownHall_Intro_HAA 6 Afterwards › Future town halls: Edmonton Nov 29

› Continue the discussion! - LRP2020 Slack #town-halls channel - Twitter #LRP2020

LRP2020_Nov2019TownHall_Intro_HAA 7 DIGITAL INFRASTRUCTURE AND MACHINE LEARNING LRP-2020 Victoria Townhall.

Kavelaars_DRI 18 Digital Research Infrastructure

Transitioning 'up to’ $375M

Kavelaars_DRI 9 NATIONAL RESEARCH COUNCIL CANADA 2 Digital Research Infrastructure

'EngageDRI’ was the sole submission to the call for proposal to form a new organization to operate Canada’s DRI.

From ISED: The submission proposed to build a seamless ecosystem that is researcher-focused, accountable, agile, strategic, sustainable and rooted in a shared vision that enables researchers to access the digital research services they need.

ISED also released an additional $50M in funding to the 5-Advanced Research Computing (ARC) centres – U-Vic, SFU, U-W, UofT, and McGill.

Kavelaars_DRI 10 NATIONAL RESEARCH COUNCIL CANADA 3 CC Resources (pre $50M)

Center Storage CPU Cores GPU Beluga 8.9 PB 34880 688 Graham 12 PB 33376 320 Niagara 2 PB 60000 0 Cedar 10 PB 58416 584 Arbutus* 5.7 PB 9048 4* 38.4 195720 1596

Kavelaars_DRI 11 NATIONAL RESEARCH COUNCIL CANADA 4 CADC Resources

Currently in the midst of hardware refresh • 4.5 PB of storage • 500 CPU Core

• Database, Web-Service, Development • 40 Gbit WAN and LAN Approx. $7M Investment from NRC over 3 years with 5 year life time: $0.01/GB/month (AWS – $0.02/GB/month + Compute)

Kavelaars_DRI 12 NATIONAL RESEARCH COUNCIL CANADA 5 CADC Resources

Real Advantage – People 23 members of the CADC: • 9 Developers • 7 Data Specialists / Research Astronomers + (1) • 4 Operations + (1) • 1 Project Manager

Kavelaars_DRI 13 NATIONAL RESEARCH COUNCIL CANADA 6 Community Needs

Looking just at storage needs. Major data projects in astronomy SKA alone requires more capacity (for an Canadian SRC) than the entirety of Canadian DRI capacity by Facility Storage factor of 5. Most of that capacity is SKA and occurs in 2025 and SKA 237 PB beyond. LSST would be equal in capacity to current Canadian DRI. LSST 30 PB CHIME storage is project based and just a guess.

CHIME 10 PB

Kavelaars_DRI 14 NATIONAL RESEARCH COUNCIL CANADA 7 Digital Research Infrastructure

How to take advantage? 'up to’ $375M

Kavelaars_DRI 15 NATIONAL RESEARCH COUNCIL CANADA 8 Machine Learning

Papers with “Machine Learning” in content Application of new statistical modelling approaches

6000 CNN type techniques rely on large training datasets and repeated training 5000 Specialty knowledge is in the design / layout of the network 4000

Need some3000 approach to train students in these methods

Training is2000 GPU intensive and Data

–1000Application is data intensive

0 2011 2012 2013 2014 2015 2016 2017 2018 2019

Kavelaars_DRI 16 NATIONAL RESEARCH COUNCIL CANADA 9 Canada is ahead in deploying Service layers built up via multiple projects • CIRADA • ALMA – Development Study • CANARIE Funding (hopeful) • NRC Support

Kavelaars_DRI 17 NATIONAL RESEARCH COUNCIL CANADA 10 THANK YOU First name Last name • Position • [email protected]

Kavelaars_DRI 18 Protoplanets and disks

LRP2020 Townhall Nienke van der Marel NRC Herzberg/University of Victoria November 27th 2019 vanderMarel_protoplanetary_disks 19 BACKGROUND

ExoplanetsExoplanets 4133 planets!

Large diversity exoplanets, very vanderMarel_protoplanetary_disksdiﬀerent from Solar System http://exoplanet.eu, 2019-11-2620 BACKGROUND Planet formation

gas (current) grains pebbles rocks planetesimals/ migration scattering cores giant exoplanets

1μm 1mm 1m 1km 1 Mm 1 Gm planet-planet/ planet-disk exoplanet overcome pebble accretion/ planetesimal core accretion interaction demographics growth barriers streaming interaction (hydrodynamics) instability (dynamics)

vanderMarel_protoplanetary_disks 21 BACKGROUND Planet formation

gas (current) grains pebbles rocks planetesimals/ migration scattering cores giant exoplanets

Multi-wavelength Requires knowledge of: spatially resolved Disk mass - Exoplanet detections observations of gas Disk evolution - + bias analysis: and dust distributions Disk accretion - true demographics (infrared-cm) - Disk lifetime - Disk composition vanderMarel_protoplanetary_disks 22 BACKGROUND Planet formation

gas (current) grains pebbles rocks planetesimals/ migration scattering cores giant exoplanets

• When do planets form?

• 1μm 1mm 1m How1km do1 Mm planets1 Gm form? overcome • pebble accretion/Where do planets form?planet-disk planet-planet fragmentation/ streaming core accretion interaction interaction drift barriers instability (hydrodynamics) (dynamics) • In which conditions do planets form? Observable Theoretical Observable

Debris disk Protoplanetary disk with planetary system

vanderMarel_protoplanetary_disks 24 BACKGROUND Circumstellar disks

Protoplanetary disk Debris disk

• Gas-rich • Gas-poor • 1-10 Myr old • few Myr - few Gyr old • Dust mass 0.5-100 ME • Dust mass 0.001-0.1 ME • Dynamics dominated by gas • Dynamics dominated by dust collisions • Generally found in clusters at (second-generation components) ~100-200 pc • Generally scattered out, detectable out • Recent/on-going gas giant to <50-100 pc formation • Terrestrial planet formation (no core accretion when gas is gone)

vanderMarel_protoplanetary_disks 25 WHEN DO PLANETS FORM Large surveys: disk mass

Typical protoplanetary disks do not have sufﬁcient solid material to form rocky cores for giant planet formation at few Myr Giant planets may already form in embedded stage!

PPDs Protostars Embedded disks

Small terrestrial planets can still form in debris disk Manara et al. 2018 vanderMarel_protoplanetary_disks 26 Tychoniec et al. 2018 HOW DO PLANETS FORM Tracing grain sizes

Protoplanetary disk: IRS 48 VLT 18 micron Debris disk: Formalhaut HST Herschel ALMA

Protoplanetary disk: J1604-2130 ALMA ALMA-CO NIR (Subaru)

Van der Marel et al. 2013, 2015 Matthews et al. 2019 Multi-wavelengthvanderMarel_protoplanetary_disks observations show grain size distribution Dong et al. 201727 WHERE DO PLANETS FORM Planet signatures in PPDs ALMA: gaps and rings Direct imaging: planet!

ALMA: warps Scattered light (GPI): Hydro simulations: gaps, shadows, spirals spiral arms!

Van der Marel et al. 2019 Dong et al. 2015 Casassus et al. 2015 vanderMarel_protoplanetary_disks Disk structures predict giant planets at tens of AU 28 Muller et al. 2018 WHERE DO PLANETS FORM Planet signatures in debris disks

vanderMarel_protoplanetary_disks Hughes et al. 201829 WHERE DO PLANETS FORM

Highest ALMA ALMA disks and exoplanet resolution Typical ALMA gap radii demographics have opposite biases! optically thick

Exoplanets: Structures in ALMA disks: bias towards closest-in bias towards large scales vanderMarel_protoplanetary_disks 30 IN WHICH CONDITIONS DO PLANETS FORM

Classical accretion disk: turbulent

Viscous spreading to conserve Planet formation at snowlines in disks? accretion angular momentum

Measurements of low turbulence challenge classic disk model: disk wind?

Chemical complexity and snowlines in disks affect planet composition Ionised disk wind/jet Flaherty et al. 2016 Cowan et al. 2015 vanderMarel_protoplanetary_disks 31 Ali-Dib 2017 NEXT STEPS Key questions

• Does planet formation already start in the embedded phase? WHEN? • Are we underestimating disk dust mass (optical depth)? • Where are the centimetre-sized grains? HOW? • Can we detect the protoplanets predicted by disk structures directly? • How do we match the exoplanet demographics with protoplanet WHERE? locations? • Can we ﬁnd planet signatures in the inner part of the disks? • How do planets migrate through the disk after formation? WHICH • Can we ﬁnd disk winds (through ionized emission) and revise our disk CONDITIONS? accretion model? • What is the chemical composition of disks and how does it compare with exoplanet atmosphere compositions?

vanderMarel_protoplanetary_disks 32 NEXT STEPS Canadian expertise McM UBC UT

McGill UofR UVic NRC Planet formation Dynamics McM NRC theory UWO BU Star Exoplanets formation UT UdM (galactic) UofC Disks mm/cm Big data, instrument archiving, technology processing

NIR Interferometry technology expertise

vanderMarel_protoplanetary_disks 33 NEXT STEPS Planet formation: LRP 2020

Science •W005: Signposts of planet formation in protoplanetary disks (van der Marel) •W066: Debris disks (Matthews) •W063: The formation of stars (di Francesco) •W059: Exoplanet imaging (Marois) •W065: Exoplanet instrumentation (Benneke) •W056: Molecular astrophysics and astrochemistry (Cami)

Facilities •W019: Development plans for ALMA (Wilson) •W032: The ngVLA (di Francesco) •W046: The SKA (Spekkens) •W048: Submillimeter single dish (Chapman) •W022: Gemini (Cote) W057: JWST (Doyon) •W035: Mid- through Far Infrared astronomy (Johnstone) •W062: Digital infrastructure (Kavelaars)

vanderMarel_protoplanetary_disks 34 NEXT STEPS Facilities (radio) PPDs: ALMA, ngVLA and/or SKA High resolution mm/cm-observations:

• Measure disk dust masses • Locate centimeter grains • Trace inner regions disks • Detect disk winds • Complex organic molecules in disks

vanderMarel_protoplanetary_disksDDs: ATLAST, OST, SPICA 35 NEXT STEPS Facilities (OIR) Gemini

Optical/NIR observations:

• Detect protoplanets in disks • Trace inner disk chemistry • Exoplanet atmosphere JWST composition • Measure distribution small grains

vanderMarel_protoplanetary_disks 36 NEXT STEPS Recommendations

Gemini • Further investment in observational planet formation research • Better coordination between related research ﬁelds (e.g. star formation, exoplanets, dynamics, theory, astrochemistry, etc.) • Investing and partnership in (future) facilities for centimeter observations including ALMA, ngVLA, SKA, ATLAST and OST. • Continued upgrades of Gemini/GPI for direct imaging capabilities • Further support for computational facilities (e.g.CANFAR, CADC) • Training in use of interferometric facilities, in particular for graduate students

vanderMarel_protoplanetary_disks 37 vanderMarel_protoplanetary_disks 38 Exoplanet Imaging Christian Marois NRC, Herzberg Astronomy & Astrophysics & collaborators

Marois_ExoplanetImg 39 Exoplanet Imaging Christian Marois NRC, Herzberg Astronomy & Astrophysics & collaborators

Marois_ExoplanetImg 40 Why imaging?

• Galactic astronomy: Stellar astrophysics (physical parameters, composition, age, • Where do we come from? activity, binary, space motion), star formation regions, young clusters/moving groups, brown dwarfs, disks. • Solar system astronomy: planets, comets, asteroids, dynamics.

• Exoplanets: Multi-planet systems, orbital dynamics, formation process, physical • Are we alone? parameters, chemistry, clouds, time variability, continents, moons.

• Life: Earth science, exobiology. Finding biomarker signatures on other worlds.

4,093 (Nov 7, 2019) known exoplanets New era of comparative exoplanetology Marois_ExoplanetImg 41 Complementary to other techniques

Advantages

• No transit/alignment required • Fast discovery (min/hours) • Planet photons, phot/spec • Orbit • Dynamical mass (with RV)

Limitations

• Resolving/contrast • Young self-luminous planets (for now) • > 5 AU gas giants (for now) • Model-dependent mass (no RV) • “Extreme” instruments for Earth-size in HZ

Marois_ExoplanetImg 42 3. HOWFS RTC

deformable 1. AO Real Time How? mirror (DM) Controller (RTC)

dichroic

Science camera/ low order WFS (LOWFS)/ high coronagraph order WFS (HOWFS) AO Wave- Front 2. LOWFS RTC Sensor (WFS) ADI SDI

LOCI

Marois_ExoplanetImg 43 3. HOWFS RTC

deformable 1. AO Real Time How? mirror (DM) Controller (RTC)

dichroic

Science camera/ low order WFS (LOWFS)/ high coronagraph order WFS (HOWFS) AO Wave- Front 2. LOWFS RTC Sensor (WFS) ADI SDI

LOCI

Marois_ExoplanetImg 44 A Strong Canadian Legacy

• ADI, SDI and LOCI Marois et al. 2008, 2010 Lafrenière et al. 2008/2009 • AO/RTC: ALTAIR, GPI, NFIRAOS

• Cameras: MONICA, KIR & TRIDENT

• IFS: GPI • Hires spectrographs: SPIROU & NIRPS

Naud et al. 2014 Macintosh et al. 2015

Marois_ExoplanetImg 45 What we need

Better coronagraph, better low order mode corrections, ADI & SDI/HDC

Better coronagraph, wavefront control, ADI & SDI/HDC

(this NASA ﬁgure is missing a population of ice/giants around other stars) Marois_ExoplanetImg 46 Imaging challenges

B. Gerard

A sea of “speckles”

AO limitations, coronagraph leaks, none-common path aberrations, temporal stability, chromaticity, polarization.

Flat ﬁeld & optical distortions Marois_ExoplanetImg 47 Imaging challenges

B. Gerard

A sea of “speckles”

AO limitations, coronagraph leaks, none-common path aberrations, temporal stability, chromaticity, polarization.

Flat ﬁeld & optical distortions Marois_ExoplanetImg 48 “Linearizing” the problem using extreme SDI - High-Dispersion Coronagraphy -

Requires broadband high-contrast images to acquire many lines. A level of SDI that has never been tested to that contrast level. 2 x 2 != 4 in high-contrast imaging. Marois_ExoplanetImg Still photon noise limited and model-dependent. 49 “Linearizing” the problem using kHz focal plane WFS - Freezing speckles with FAST - Measuring phase/amplitude aberrations at kHz speed

Gerard et al. 2018

(a) Abs{FT{}} (fringes) (c)

Modulation Transfer Function

(b) (d)

Needs a few photons to see fringes Monochromatic Small BP EFC Photon noise limited Imager Marois_ExoplanetImg Calibration/stability HCIT JPL 50 “Linearizing” the problem using kHz focal plane WFS - Freezing speckles with FAST - Measuring phase/amplitude aberrations at kHz speed

Gerard et al. 2018

(a) Abs{FT{}} (fringes) (c)

Modulation Transfer Function

(e)(b) (d)

Needs a few photons to see fringes Monochromatic Small BP EFC Photon noise limited Imager Marois_ExoplanetImg Calibration/stability HCIT JPL 51 Combining techniques to maximize contrast

Dark hole to allow low and hires spectroscopy. Minimize req. on SDI/HDC contrast gains. Faster detections with less photon noise.

Marois_ExoplanetImg Broad range of science cases, from gas giants to rocky planets. 52 A Canadian R&D Perspective

NRC NEW EARTH, AO, DM, RTC, SAPHIRA, Coronagraphy, IFS/spec NRC Photonics Coronagraphy

UdeM IFS, spectrograph

ULaval UVic Optics, AO, IFS, HiCIBaS AO, RTC, Coronagraphy

Dalhousie AO, DM U of Alberta Coronagraphy U of Manitoba DM UT Honeywell, BMV, NUVU, and ABB Marois_ExoplanetImg AO, SAPHIRA, microsat + international partners53 NRC AO Lab

AO lab HeNOS: Herzberg NFIRAOS Optical Simulator Advanced WFS bench • A flexible test platform with the ability to emulate various • In-house development, testing and types of observing conditions. characterization of a wide variety of devices. • Multiple sources and WFSs to isolate and combine • Create custom optical test setups for each unique correction signals from different spatial and temporal device: domains. • Reconstructor can be changed or modified to test various • DMs algorithms. Next up is LTAO, MCAO. • Pyramids • Calibration of NCPA using focal plane sharpening and phase • OAPs diversity. • Motion Stages • High Resolution WFS

Marois_ExoplanetImg From Kate Jackson 54 Real Time Computers From Jennifer Dunn

Real-Time Controllers (RTC) at HAA

• Developing the Herzberg Extensible Adaptive optics Real-time NFIRAOS Toolkit (HEART) • a software framework and collection of utility tools for construction of an AO Real-Time Controller (RTC) • Starting build of the RTC for Narrow Field Infrared Adaptive Optics System (NFIRAOS), the first-light AO system for the Thirty Meter Telescope (TMT) • Conceptual design of RTC for Multi-conjugate Adaptive Optics RelaY (MAORY) for the ELT in progress MAORY

LGS mode in RED HEART NFIRAOS RTC NGS mode in BLUE

Marois_ExoplanetImg1 55 New DM technology Why MEMS and ASICs?

• Offer a compact low-power solution at a reduced price. • Application: • Essential components for MOAO systems • Significantly reduce cost + complexity of highly multiplexed system

Xinetics Inc. for Mt. Palomar “Palm 3000” AO System Proposed system architecture Packaged AISC

Marois_ExoplanetImg 56 From Scott Chapman Technology development: MEMS DM and ASIC Driver Packages

• MEMS Lorentz Deformable Mirror

• ASIC • Low-voltage • Low-power

Marois_ExoplanetImg 57 From Scott Chapman Zero noise cameras

Infrared Wavefront Sensor (IRWFS) Camera • Camera uses Leonardo’s SAPHIRA Mark 13 array • SAPHIRA array cooled to 85 K using SunPower’s CryoTel MT cryocooler • Custom controller used to program and readout the array using 16 channels (2 kHz frame rate using 80 x 80 region of interest) • Nominal read noise of 50 !" RMS. Sub-electron read noise achieved using reverse-bias voltages beyond 12V (APD gain ≥ 50).

New detector system under development based on a 512x512 pixel array with 64 channels, capable of full frame readout at 2 kHz

EMCCDs at NUVU FromMarois_ExoplanetImg Suresh Sivanandam, Andre Anthony & Tim Hardy 58 NEW EARTH Lab New technologies for high-contrast imaging

FAST focal plane mask (KAUST) TG focal plane mask Reﬂecting Lyot mask • Testing new coronagraph masks • Validating new focal plane WFS techniques • IFS design for high-contrast imaging • Visible/NIR systems • GPI 2.0/3.0, PSI, HiCIBaS, etc • With ESO, NRC unique toward facility-class systems BMV Univ. of Alberta Lyot image

Marois_ExoplanetImgpupil pinhole 59 Orbiting LASER beacons Christian Marois When stars are just not bright enough… William Thompson Kate Jackson Vis/NIR spec. of rocky planets around M dwarfs to Sun-like stars with ground-based telescopes

NEW HOPE LASER beacon constellation 2 km diameter ground “spot"

Thompson et al. 2019 100,000,000 photons ~10,000 photons RMS Background limited regime (800nm) Stellar I-mag Non AO AO not sky limited (mag/“^2) mag/(lambda/D)^2 10 photons < 1photon for Earth 2.0 ~3 photons RMS < 1 photon RMS ~3x gain ~10,000x gain 8m 20 28 < 3

30m 20 34 < 9 Atmospheric speckle Atmospheric speckle In-band LASER speckle ms integration after ms integration ms integration A 30m can resolve the HZ around Sun-like stars up to 15-20pc DM correction while NOT being background noise limited Marois_ExoplanetImg “Assuming perfect correlation" 60 Toward Earth 2.0

WFIRST

JWST NIR imaging

LUVOIR HabEx

Marois_ExoplanetImg 61 Toward Earth 2.0

WFIRST

JWST NIR imaging

GPI 3.0 VIS/NIR

LUVOIR HabEx

Marois_ExoplanetImg 62 Toward Earth 2.0

WFIRST

JWST NIR imaging NIR low/mid/high RES 30-m

10 microns 30-m

GPI 3.0 low resolution VIS/NIR

LUVOIR HabEx

Marois_ExoplanetImg 63 Toward Earth 2.0

Orbiting LASER 30-m NIR/VIS WFIRST JWST NIR imaging NIR low/mid/high RES 30-m

10 microns 30-m

GPI 3.0 low resolution VIS/NIR

LUVOIR HabEx

Marois_ExoplanetImg 64 2020-2030 Pathﬁnders

Gemini Planet Imager High-Contrast Imager Balloon Telescope

Toward GPI 2.0 and beyond Space technologies and TRL Validating new technologies for ELTs. Toward HabEx and LUVOIR contributions.

Also other opportunities with international collaborators (Subaru, Keck, ESO)

Marois_ExoplanetImg 65 HiCIBaS: High Contrast Imaging Balloon System

FromMarois_ExoplanetImg Simon Thibault 66 2020-2030 2020 2021 2022 2023 2024 2025 2026 2027 2028 2029

NIR R&D, BB fpwfs, SAPHIRA NIR ELTs optimization NEW EARTH Lab Vis ExAO R&D, broadband fpwfs, HDC, NUVU: >10E8 contrast

GPI upgrades Design Construction @GN @ GN phase 2 Design Construction phase 3?

PSI-Red Preliminary Study Design Construction @TMT

TMT PSI-Blue Preliminary Study Design Construction MICHI Preliminary Study Design Construction

HiCIBaS Flight #2 Flight #3 Flight #4

Other E-ELT 1st light GMT 1st light TMT 1st light observatories JWST Launch WFIRST Launch

Reflected-light NIR Science Earth-size M dwarfs highlights NIR Reflected-light Thermal of RV gas giants Reflected light Vis/NIR gas giants Saturn-mass NIR wide separation NIR Saturn-mass >5 AU L/M-band hot Super-Earth gas giants >10 AU >10 AU Forming planets Forming planets Forming planets (GPI/SPHERE/SCExAO) Thermal Earth-like Alpha Cent A & B Thermal Earth-like around (JWST) 10 Sun-like stars. (GPI/SPHERE/SCExAO, ELTs)

Marois_ExoplanetImg (WFIRST, ELTs) 67 TBD E-ELT HIRES, small sat missions, or possible Subaru/SCExAO/Keck collaboration as well. A strong support for frontier R&D to enable Breakthrough Science in the 2020s and beyond Alpha Cent A & B

Vis/NIR

exo-Venus A Exo-Earth exo-Jupiter exo-Earth

exo-Mars Alpha Centauri B Alpha Centauri Marois_ExoplanetImg8m @ 10 microns 30m @ 10 microns68 100h 8m 25h TMT (Chile) Canada has the skill & experience to play a major role in the search for exolife

NRC NEW EARTH, AO, DM, RTC, SAPHIRA, Coronagraphy, IFS/spec NRC Photonics Coronagraphy

UdeM IFS/spec

ULaval UVic Optics, AO, IFS, HiCIBaS AO, RTC, Coronagraphy

Dalhousie AO, DM U of Alberta Coronagraphy U of Manitoba DM UT Honeywell, BMV, NUVU, and ABB NSERCMarois_ExoplanetImg TEPS and NTCO CREATE AO, SAPHIRA, microsat + international partners69 Recommendations

1.Support the development of high-contrast technologies, at NRC at the NEW EARTH laboratory, in Universities and in the industry. This is mandatory for new instruments to reach the sensitivity to search for life signatures on other planets.

2.Stress the importance to hire Canadian high-contrast expertise at NRC and in universities. These will ensure that we have a strong diversiﬁed workforce that can lead to major Canadian deliverables to future large-scale instruments/observatories for both ground and space.

3.Retain Gemini/GPI access, as this is the main ground-based facility where Canadian can deploy new technologies for ground-based telescopes.

4.Subaru/SCExAO partnership is worth exploring for both its science potential and instrument program.

5.The Canadian funding system is inadequate to prepare for projects on the scale of ELT instruments. The current funding stream is mainly through CFI or observatories. For example, the main expertise in high-contrast imaging is located at NRC where CFI funding can’t be transferred to support instruments for Canadian observatories, limiting the scope of observatory-independent funding to develop visitor-class pathﬁnders/upgrades.

Marois_ExoplanetImg 70 Recommendations

6.Stress the importance of seed funding for instrument proposal preparation to large funding agency, such as CFI. With instruments becoming larger, more complex and more expensive for ELTs, the lack of funding to properly design and cost instruments is a real concerned, potentially generating issues once money is awarded and actual in-depth work in design and costing is performed.

7.Early access to an ELT is crucial. It is important to further stress the importance of a GMT/E- ELT/TMT partnership to share telescope time and get access to both hemispheres. For example, Alpha Centauri A and B, along with Proxima Centauri, important targets in high- contrast imaging given their proximity, are only visible from the southern hemisphere with no equivalent in the northern hemisphere.

8.CSA stratospheric balloon ﬂights and its FAST program are crucial to test space technologies and increase their technology readiness level (TRL). A new funding scheme is necessary to enable long-term support for strategic initiatives such as HiCIBaS.

9.Discussions are needed as soon as possible to develop contributions (at the JWST level) and a funding plan for future participation in B$ ﬂagship space missions such as HABEX and LUVOIR.

Marois_ExoplanetImg 71 We want CANADA to play a leading role in the search for life outside our solar system

R&D investments are needed to achieve this goal!

Christian Marois (NRC), Benjamin Gerard (UVic), William Thompson (UVic), Ruobing Dong (UVic), Stanimir Metchev (UWO), Nienke van der Marel (UVic), Suresh Sivanandam (U. Toronto), Simon Thibault (U. Laval), Étienne Artigau (UdeM), Frédérique Baron (UdeM), Jason Row (Bishop), Scott Chapman (NRC/ Dalhousie), Frédéric Grandmont (ABB), Eve Lee (McGill), Bruce Macintosh (Stanford), Scott Roberts (NRC), Björn Benneke (UdeM), Célia Blain (Gemini), Aaron Boley (UBC), Colin Bradley (UVic), Greg Burley (NRC), Adam Butko (UoT), Neil Cook (UdeM), Nicolas Cowan (McGill), René Doyon (UdeM), Colin Goldblatt Marois_ExoplanetImg(UVic), Tim Hardy (NRC), Olivier Lardière (NRC), Brenda Matthews (NRC), Max Millar-Blanchar (Caltech), Jean-Pierre Véran (NRC) 72 Gemini in the Coming Decade LRP Townhall Victoria

Stéphanie Côté, Head of CGO Tim Davidge, Joel Roediger, Eric Steinbring, Laura Ferrarese (NRC), John Blakeslee (Gemini), Sarah Gallagher (Western U)., Craig Heinke (U of Alberta), Laura Parker (McMaster), Suresh Sivanandam (Dunlap Institute, U of Toronto), Kim Venn (U of Victoria)

27 November 2019 - Victoria

Cote_Gemini-LRP2020 73 Q1: What are the relevant White Papers? Main White Paper: W022: Gemini in the Coming Decade (Côté et al) Other White Papers: • W03 Young Nearby Associations (Gagné) Characterization of low mass members of nearby associations • W05 Planet Formation in Protoplanetary disks (van der Marel) High contrast imaging to detect disks and internal structures within disks, GPI2.0 • W06 Canadian Partnership with Subaru (Balogh) Complementarity of Gemini (high angular resolution) and Subaru science • W08 Canadian Astronomy on Maunakea (Neilson) Telescope time for Native Hawaiians • W015 Canadian Participation in the LSST (Fraser) Key roles of GN and GS for transient follow-ups . • W020 The Euclid Mission (Percival) GIRMOS follow-ups of Euclid sources • W024 Star Clusters Near and Far (Hénault-Brunet) Chemo-dynamical evolution of Globular Clusters with GIRMOS • W025 The next decade of optical wide-field astronomy in Canada (McConnachie) Gemini follow-ups of wide-field imaging surveys • W026 Probing Diverse Phenomena through Data-Intensive Astronomy (Rahman) Gemini for national Legacy-type observing programs

Cote_Gemini-LRP2020 74 Q1: What are the relevant White Papers?

• W041 The cosmic origin and evolution of the elements (Fernandez et al) GHOST to find metal-poor stars; LIGO follow-ups, SN remnants • W042 Multi-Messenger Astrophysics in the next decade (Ruan) ToO photometric and spectroscopic monitoring • W051 Science with the LSST (Hlozek) LSST follow-ups with SCORPIO; efficient scheduling • W056 Molecular Astrophysics & Astrochemistry (Cami) Characterization of molecular spectral signatures • W059 Exoplanet imaging (Marois) GPI2.0. Keeping Gemini/GPI2.0 access for the next decade • W060 Characterizing Galaxies in the Early Universe (Man) GIRMOS for distant galaxy studies • W065 Exoplanet Instrumentation (Benneke) GPI upgrades

Roughly a quarter of all WPs describe future projects on Gemini. This shows Gemini’s workhorse nature to deliver on a broad range of science goals

Cote_Gemini-LRP2020 75 Highlights:

• Canadian Papers: The overall science Impact of Canadian Gemini Papers (based on citations) is at 2.4, higher than Gemini average (1.7), and in fact higher than any other 8-m class telescope worldwide such as Keck, Subaru, VLT!

Average Impact 2013-2017

Canadian Papers 2.4 1st author Cnd P 1.6 Gemini (All) 1.7

Keck 2.0 VLT 1.6 Subaru 1.4

• Press Releases: Canadian astronomers are leaders or collaborators on almost half (46%) of all science press releases released by Gemini between 2009 to 2017 4

Cote_Gemini-LRP2020 76 Highlights:

• Student Theses: There are now over 71 Canadian MSc and PhDs theses based on Gemini data, more than from any telescopes to which Canadians have access • Student Internships: During the period 2009-2017 Canadian undergraduates in co-op programs have filled 33 internships at Gemini. They worked as Science interns but also operation interns or Science software testers.

• Student Visits: Viraja Khatu (PhD student at UWO) in a NSERC CREATE internship 2019 wrote a From 2009 to 2017, 31 Canadian students GNIRS Python reduction pipeline visited the Telescopes (through the Maunakea Graduate School, Or Bring One, Get one!)

Cote_Gemini-LRP2020 77 In the Coming Decade:

Over the coming 5 years Gemini will enjoy an instrumental renaissance, with the commissioning of a revitalized instrumentation suite.

Thanks to a $26M Award from US NSF: • New Multi-Conjugate Adaptive Optics at Gemini-North (GNAO) [synergy with JWST] • Operations software and data pipeline developments for rapid follow-up Time Domain Astronomy (TDA) [synergy with LSST] Thanks to $CAN15M from CFI + Provincial & University partners grants: • GIRMOS – Multi-IFUs with AO IR spectrograph

Cote_Gemini-LRP2020 78 In the Coming Decade:

• GHOST : Gemini High resolution Optical SpecTrograph Two-object+sky over whole 0.37 to 1µm at R=50K to 75K [Exoplanets, Metal-poor stars, Globular Clusters, Galactic structure, GAIA follow-ups, Dwarf Galaxies, GRBs ]

• SCORPIO : Wide-band medium-resolution spectrograph and imager 8-channel imager & spectrograph in optical & IR 0.4 to 2.35 µm at R=4K [LSST follow-ups, solar system bodies, neutron stars, Xray binaries, . Supernovae, AGNs, and GRBs, fast changing phenomena ]

• IGRINS2 : Echelle near-IR spectrograph R~45K resolution over entire H&K windows in a single exposure Developed by Korea as part of their initial contribution to joining the Gemini partnership . [ISM, star formation, early evolution of stars & planetary systems ]

• GPI2.0: Upgraded GPI for G-North with higher contrast imaging [Exoplanets, Brown dwarfs, Debris disks]

Cote_Gemini-LRP2020 79 In the Coming Decade:

Gemini-North AO + GNAOI : • Canada has had strong interest in GN having such a capability for many years • MCAO system with 2-arcmin field of view: • 30% Strehl correction in K at median seeing - GNAO should at least match the performance of GeMS, and take full advantage of Maunakea. Goal is 50% Strehl. • PSF astrometry better than 1 mas across field (single detector) • Better sky coverage than users have seen on GeMs (now also upgraded NGS2) • Operable by standard Gemini night crew, without the need for an additional laser operator, so will be available every suitable night.

Cote_Gemini-LRP2020 80 In the Coming Decade:

• GIRMOS : Gemini InfraRed Multi-Object Spectrograph High angular resolution, multi-integral-field spectrograph and imager, employing an Multi-Object Adaptive Optics (MOAO) system behind Gemini MCAO Developed in Canada with CFI $ by a team led by Suresh Sivanandam (U of Toronto, Dunlap) https://arxiv.org/abs/1807.03797 Four IFU arms : deployable over full 120” diameter field of view Spatial Sampling : 25×25 mas, 50×50 mas, 100×100 mas. IFU field of view : 1.0 × 1.0, 2.0 × 2.0, or 4.0 × 4.0 arcsec 8.0 × 8.0 arcsec (all IFUs combined) Spectral Coverage : 1.0–2.4 m Spectral Resolution: R = 2500 to 6000 Pathfinder for TIRMOS on TMT Science: Galaxy mass assembly and evolution, galaxy clusters, first galaxies and reionization, AGNs, star formation; stellar populations; near field cosmology, protoplanetary disks.

Cote_Gemini-LRP2020 81 Software Development for Operations and Scheduling:

Enhancing Rapid Response & Dynamic Scheduling for rapid follow-up of transients identified in current and future Time Domain surveys such as LSST .

Solar system moving sources (hazardous objects or interstellar voyagers); Type 1a supernovae for cosmological studies; core- collapse supernovae of all varieties for studying the diversity of stellar evolution; distant AGNs for understanding the process of SMBHs growths in galaxies; hypernovae for constraining the rate of neutron star mergers; exotic sources that may represent new classes of phenomena Software to select, schedule, execute and process observations of . the most compelling transient targets Evolution of the Gemini Observatory Control System (with easier Phase1/Phase2)

• BOTH Gemini-North and Gemini- South benefit from optimally scheduled and efficiently executed observations and the development of automated data reduction pipelines. STATIC SKY USERS TOO! Scheduling: pre-defined filtering of transients via event broker and optimized scheduling via a Target Observation Manager

Cote_Gemini-LRP2020 82 Gemini in the mid-20s

GEMINI NORTH GEMINI SOUTH The premier facility for AO Science The premier facility for rapid response

° GMOS optical multi-object, longslit and IFU ° GMOS optical multi-object, longslit and IFU spectrograph and imager spectrograph and imager ° NIRI 1-5 µm imager ° FLAMINGOS2 1-2.4 µm spectrograph ° GNIRS 1-5 µm longslit and cross-dispersed and imager spectrograph with new IFU ° GSAOI 0.9-2.4 µm high-resolution imager ° GEMS Multi-conjugate AO system

° GPI 2.0 (2024) ° GHOST (2020) ° GNAO + ° SCORPIO (2022) ° GNAOI (2024) ° IGRINS2 (2023) ° GIRMOS (2024)

Cote_Gemini-LRP2020 83 Q2: Timeline:

GHOSTGHOST

Cote_Gemini-LRP2020 84 Q2: Timeline:

Gemini International Agreement:

The current Gemini International Agreement is scheduled to expire in December 2021. The November 2018 Board meeting was an official « Gemini Assessment Point »: Partners had to declare their interest in renewing the Agreement past 2021 to NSF.

An extensive Review process in Canada in the summer/fall of 2018 (review from appointed panel, including community survey and Townhall discussion, report sent to open review through casca- list), demonstrated that interest in Gemini remains strong.

Following approval from NRC President, Canada committed in November 2018 to NSF to its continued involvement in the Gemini partnership past 2021 and at the same 18.15% level

The new Gemini International Agreement will run from January 2022 to December 2027 .

Canada will need to decide (around 2024) if it will renew its Agreement past 2027 and at what level.

Cote_Gemini-LRP2020 85 Q3: Challenges or concerns ?

• Renewal of the Maunakea Master Lease Agreement , to allow observatories to continue beyond 2033 , is a concern. - The Master Lease for the Maunakea Science Reserve is granted by the State of Hawaii to UH and expires in 2033. Gemini, like the other non-UH telescopes, holds a sublease from UH in exchange of 10% observing time. - UH wants a new lease for the entire 11,288-acre Maunakea Science Reserve plus the . Halepohaku mid-level facilities, the 525-acre astronomy precinct and support facilities. - Gov. David Ige’s 10-point plan for Maunakea (2015): return 10,000 acres outside the astronomy precinct to the state Department of Land and Natural Resources. - The UH Board of Regents voted this month to recommend the closure of 5 telescopes on MK.

• So far Gemini-North staff (as well as other current observatories) have been allowed to move through the blockade including bringing large instruments up and down (eg: ‘Alopeke). 14

Cote_Gemini-LRP2020 86 Beyond 2027:

° GNAO and GIRMOS commissioning in 2024 . These are new capabilities with much interest in the Canadian community. Unwise to diminish our share of Gemini time (or pull out) when so much . exciting science in the making

° Gemini-South will offer the only access to the south for the Canadian community (=maximizing science impact of ALMA and SKA)

° Canadian time on the TMT will be modest , after NSF entry at <15\% Gemini will still be needed to accommodate our community needs. Gemini can continue to enable a large number of students theses. As for the JWST, its nominal lifetime is 5.5 years up to 10 years max (to be decommissioned by around 2030).

° The transient science enabled by the LSST will still be in its infancy in 2027 . TMT might be able to follow-up on fainter triggers, Gemini time will still be needed to follow-up and characterize brighter triggers (critical for interpreting fainter objects).

Cote_Gemini-LRP2020 87 Beyond 2027:

° The first generation of TMT instruments will in no way cover the wide range of capabilities offered on Gemini . High-resolution spectroscopy at spectral resolution > 8000 in the optical medium resolution in the near- ir>4000 will not be available on the TMT until its 2nd generation of instruments nor on the JWST. There is a strong appetite in Canada for high-resolution spectroscopy.

° Advantage to Canadians to test instrument prototypes for TMT instruments and other technological concepts Enormous amount of resources are needed for developing a TMT-sized instrument . (in the range of 40 to 50M\$ each). Like the TMT, the Gemini telescopes were designed for high angular resolution imaging, . . and can become the best testbeds for TMT instrument development

Canadian access to Gemini will remain crucial even in the TMT era. We therefore urge the LRP panel to recommend that Canada renew its participation . in the Gemini partnership past the coming Agreement ending around 2027. .

Cote_Gemini-LRP2020 88 McConnachie_WideFieldAstro_LRP2020 89 The next decade of optical wide ﬁeld astronomy in Canada Alan McConnachie Michael Balogh (WFAC, Subaru WP) Jo Bovy (Wide Field Spectroscopy) Ray Carlberg (Euclid) Pat Cote (CASTOR WP) Wes Fraser (LSST Data Center WP)

McConnachie_WideFieldAstro_LRP2020 90 Directly relevant facility white papers…

• W001 Hutchings: Space Astronomy • W006 Balogh: Subaru • W013 Boley: Small Moderate Telescopes • W015 Fraser: LSST Participation • W018 Cote: CASTOR • W022: S. Cote: Gemini • W051 Hlozek: LSST Science • W020 Percival: Euclid • W030 Hall: MSE • W039: Andersen: TMT Instrumentation • W062: Kavelaars: Digital Infrastructure

McConnachie_WideFieldAstro_LRP2020 91 McConnachie_WideFieldAstro_LRP2020 92 Nature Astronomy, January 2019

McConnachie_WideFieldAstro_LRP2020 93 The past year alone…

McConnachie_WideFieldAstro_LRP2020 94 The past year alone…

McConnachie_WideFieldAstro_LRP2020 95 The past year alone…

McConnachie_WideFieldAstro_LRP2020 96 The past year alone…

McConnachie_WideFieldAstro_LRP2020 97 The past year alone…

McConnachie_WideFieldAstro_LRP2020 98 Where we are now….

McConnachie_WideFieldAstro_LRP2020 99 Where we are now….

• The Canada-France-Hawaii Telescope: a backbone of the community for the last 40 years

McConnachie_WideFieldAstro_LRP2020 100 Where we are now….

• The Canada-France-Hawaii Telescope: a backbone of the community for the last 40 years • The CADC: the main reason that Canada is still a sought after collaborator (at a national level) in wide ﬁeld OIR astronomy

McConnachie_WideFieldAstro_LRP2020 101 Where we are now….

• CFHT has had tremendous impact over the years, ﬁrst as the best optical telescope in the world, then as best-in-class • Impact of CFHT undoubtedly increased due to CADC decision to provide easily accessible data archive for MegaCam • Arrival of Subaru/HSC required MegaCam to concentrate on its niches: u band, narrow-band ﬁlters • 2017+: CFIS; Vestige (MegaCam), CFHT IR parallax (WIRCAM), SLS (Spirou); SIGNALS (Sitelle) • Also a couple of “effectively Large Programs”: Pristine, CLAUDS

McConnachie_WideFieldAstro_LRP2020 102 Where we are now….

• The Canada-France-Hawaii Telescope: a backbone of the community for the last 40 years • 10000 sq.deg deep u survey, 5000 sq.deg deep r survey • 135 collaborators, mostly in Canada, France and Hawaii (39 Canadians at 15 institutes) • Broad range of stand-alone science (focused on Galactic archaeology and weak lensing) • Grew out of “Luau” LP, and used to “buy in” Canada to Euclid Euclid

CFIS PanSTARRS TBD McConnachie_WideFieldAstro_LRP2020u, r i, z g 103 Where we are now….

• The Canada-France-Hawaii Telescope: a backbone of the community for the last 40 years • 10000 sq.deg deep u survey, 5000 sq.deg deep r survey • 135 collaborators, mostly in Canada, France and Hawaii (39 Canadians at 15 institutes) • New collaborations with UH (PanSTARRS) for i(z), time- exchange with Subaru for g (Hudson, Chambers), and new collaboration with Japan for z • The LSST of the north for the static sky CFIS u, r UNIONS PanSTARRS Subaru

McConnachie_WideFieldAstro_LRP2020i, (shallow) z g, (deep) z 104 Where we might be in 10 years… (Strategic Canadian leadership of key capabilities)

McConnachie_WideFieldAstro_LRP2020 105 Where we might be in 10 years… (Strategic Canadian leadership of key capabilities)

• The Cosmological Advanced Survey Telescope for Optical and UV Research (CASTOR) • Canadian-led UV wide field space telescope with a 1m aperture. • Closely matches the image quality of HST in this wavelength range, but with a discovery efficiency that exceeds HST by a factor of 100. T • Unique imaging, grism and low-resolution spectroscopic capabilities. • Natural complement to the NIR-optimized wide field space telescopes, Euclid and WFIRST • The Maunakea Spectroscopic Explorer: wide field MOS for the 2020s 2030s • Refurbishment of the 3.6m CFHT to an 11.25m wide field MOS survey facility • ~4200 objects per 1.5 sq.deg FoV, including ~3000 objects at R~3000, and ~1000 objects at R~40000 • 10 million fiber hours per year of 10m-class spectroscopy • An SDSS-Legacy-worth of data every 7 weeks • Canadian are founding members of the concept, the science McConnachie_WideFieldAstro_LRP2020 case, and the facility design 106 Getting from here to there…

McConnachie_WideFieldAstro_LRP2020 107 Getting from here to there…

McConnachie_WideFieldAstro_LRP2020 108 Getting from here to there…

• Critical fact 1: At a national level, Canada has absolutely no leadership in any of the major wide ﬁeld OIR initiatives of the 2020s

McConnachie_WideFieldAstro_LRP2020 109 Getting from here to there…

McConnachie_WideFieldAstro_LRP2020 110 Getting from here to there…

• Critical fact 1: At a national level, Canada has absolutely no leadership in any of the major wide ﬁeld OIR initiatives of the 2020s • Critical fact 2: At a national level, Canada is not participating in any of the major ground based wide ﬁeld OIR initiatives of the 2020s • You are not going to get to there from here if this continues. And people not here will have no desire to come here, and people already here will not have a reason to stay McConnachie_WideFieldAstro_LRP2020 111 Trying not to get lost along the way…

McConnachie_WideFieldAstro_LRP2020 112 Trying not to get lost along the way…

• Leadership versus participation: • A balanced portfolio of projects should include projects that allow participation of a broad community to facilitate the development of the community and the training of HQP, and to leverage capabilities for future capabilities. • It should also include projects that demonstrate Canadian leadership in the ﬁeld and which set the stage for future projects with Canadian leadership. • Without the former, it is impossible to develop the latter; without the latter, there is little to differentiate Canada from the herd, and no reason that the best talent will seek to work or stay in Canada. • Building infrastructure versus doing science: • Most wide-ﬁeld astronomy is now driven by long-term, large-team, international projects. • Impactful participation in such projects is enabled by stable funding opportunities that can cover both salary for postdoctoral researchers and survey buy-in costs not covered by in-kind contributions.

McConnachie_WideFieldAstro_LRP2020 113 Trying not to get lost along the way…

McConnachie_WideFieldAstro_LRP2020• We envision a future where Gaia, CFHT (UNIONS), SDSS, PanSTARRS, Euclid, LSST, SKA 114 and other data sets can be (virtually) stored and analysed together. Finding the right path…

• Maintaining CFHT in its present form should not be considered beyond the mid 2020s • In 2024, CFHT will be 45 years old; MegaCam will be 21 years old. Already, competition includes DECam, Subaru/HSC and soon LSST • It is nearing the end of its internationally-competitive life in terms of large scale wide ﬁeld astronomy intiatives • But right now it forms a critical node for UNIONS (including Euclid access), and is the starting point for MSE • It is unclear what the near-term plan for CFHT is: it is currently trying juggle a signiﬁcant fraction of PI time, and doing a large number of Large Programs, including the largest its ever done, and its recently added 2 instruments while decommissioning none. And its going to convert to a 11m-telescope.

McConnachie_WideFieldAstro_LRP2020 115 Finding the right path…

• Canadian leadership in the development of large aperture MOS should continue with the intent of securing a leadership role in the first on-sky dedicated large-aperture MOS facility: • Canada has had a central role in pushing MSE forward, and there is intense international interest in the facility and the capability • MSE can provide a leadership role for Canada in 2030s wide field astronomy • Canada should ensure it has a founding stake in the first on-sky realization of this capability, McConnachie_WideFieldAstro_LRP2020and all effort should be made to ensure MSE is advanced and constructed in a timely manner116 Finding the right path…

• Canada must get access to at least one front-line ground-based wide ﬁeld facility for the 2020s. Three non-mutually exclusive possible actions: • 1. Join one of the next-gen MOS options • Generally expensive (PFS and SDSSV likely only practical options; PFS costs around USD5M for a group of 10 astronomers). • 2. Join Subaru • Simultaneously gives us access to forefront imaging (HSC) and forefront spectroscopy (PFS, from about 2021-22) • ~USD2M for Board membership and ~24 nights. Requires diversifying our portfolio of observatories (not a good idea to abandon CFHT or Gemini, but seems reasonable to examine modifying investments in each) • 3. Join LSST • Not in competition with joining Subaru because • the facilities are fundamentally different (an observatory versus a pre-deﬁned survey, essentially a supplier of data-products) • the pathways are fundamentally different (attempting to repurpose/supplement observatory operations budgets versus providing a data center/archive via CADC)

McConnachie_WideFieldAstro_LRP2020 117 Finding the right path…

• CADC/CANFAR should be supported in its continued drive to become a major data hub and science portal for the wide ﬁeld astronomy datasets of the 2020s • Hosting the LSST data, or some sub-set of the data, is a natural continuation of CADC’s mission and expertise • Thanks to changes in the LSST participation model, such a contribution would likely allow Canada to join LSST • Given the data that is already hosted by CADC, and their involvement in various future initiatives (e.g., UNIONS, Euclid, CIRADA, ARCADES), CADC could become the major (international) science portal for astronomy for the 2020s and 2030s. This can only beneﬁt all of Canada’s astronomers.

McConnachie_WideFieldAstro_LRP2020 118 Finding the right path…

• CASTOR is a unique facility and can provide Canada with a strategic scientific capability and a flagship mission for the CSA • Everything about CASTOR is excellent - the science, the strategy, and the ambition • As stated in the last LRP, Canada is at the stage where it could lead a major space mission, and CASTOR has the scientific and technical grounding to be a flagship mission for the CSA and Canadian astronomy • Decisive action is required by the CSA/Government in the next year or so to ensure Canada can help realize this facility on-sky, especially with international interest, most notably from India • The LRP should ensure that its voice is heard in a timely manner to help advance CASTOR given the critical timing over the next year or so • Basically, find out what needs to be said to who and when, and say it, even if it means making public statements before final publication

McConnachie_WideFieldAstro_LRP2020 119 The wide ﬁeld OIR sky of the future

McConnachie_WideFieldAstro_LRP2020 120 A path from here to there…?

McConnachie_WideFieldAstro_LRP2020 121 A path from here to there…?

CFHT completes UNIONS and transitions to MSE CFI funding + existing CFHT funding + in-kind + ??

McConnachie_WideFieldAstro_LRP2020 122 A path from here to there…?

CFHT completes UNIONS and transitions to MSE CFI funding + existing CFHT funding + in-kind + ?? CADC/CANFAR provides a data centre for LSST New digital infrastructure, CFI?, other?

McConnachie_WideFieldAstro_LRP2020 123 A path from here to there…?

CFHT completes UNIONS and transitions to MSE CFI funding + existing CFHT funding + in-kind + ?? CADC/CANFAR provides a data centre for LSST New digital infrastructure, CFI?, other? Canada rebalances/augments funding for CFHT/Gemini to include Subaru, for initial period of 5 years

McConnachie_WideFieldAstro_LRP2020 124 A path from here to there…?

McConnachie_WideFieldAstro_LRP2020 125 A path from here to there…?

Canada enjoys and trains itself with PFS, and plans MSE surveys using UNIONS, HSC, LSST and Euclid

McConnachie_WideFieldAstro_LRP2020 126 A path from here to there…?

Canada enjoys and trains itself with PFS, and plans MSE surveys using UNIONS, HSC, LSST and Euclid Canada prepares for Euclid using UNIONS and LSST via CADC science portal

McConnachie_WideFieldAstro_LRP2020 127 A path from here to there…?

Canada enjoys and trains itself with PFS, and plans MSE surveys using UNIONS, HSC, LSST and Euclid Canada prepares for Euclid using UNIONS and LSST via CADC science portal

McConnachie_WideFieldAstro_LRP2020 128 A path from here to there…?

Canada enjoys and trains itself with PFS, and plans MSE surveys using UNIONS, HSC, LSST and Euclid Canada prepares for Euclid using UNIONS and LSST via CADC science portal

Canadians enjoy wide ﬁeld NIR data from Euclid, while working with India to build CASTOR

McConnachie_WideFieldAstro_LRP2020 129 1) Topic for discussion: what non-science elements should be prioritized for discussion in the LRP?

• Funding • Training • Equity, diversity and inclusion (EDI) • Outreach • Environmental/sustainability in research • Data management • ……

Ellison_HAA_LRP_discuss 130 2) Topic for discussion: Structuring recommendations: to rank or not to rank?

Ranking pros and cons: + Clear message of priority + Emphasizes we have thought hard and made difficult decisions + Easier to convey/sell priorities to funding agencies/government

- Reduces flexibility/ability to be nimble and respond to changes in funding/landscape/new opportunities - Hard to compare across wavelength/science fields/projects at differing levels of maturity - Priorities/preferences can depend on non-science factors (e.g. geography, seniority). - Not everyone gets a mention

Ellison_HAA_LRP_discuss 131 2) Topic for discussion: Structuring recommendations: to rank or not to rank?

Ranking within funding bracket/ground, space pros and cons:

+ Recognizes different funding mechanisms + Similar format to (previous) US decadal survey + More things get mentioned

- More lists to process – loss of clarity - Perception of trying to ‘do everything’ - More things get mentioned

Ellison_HAA_LRP_discuss 132 3) Topic for discussion: the future of Canadian astronomy on Maunakea, and TMT in the LRP.

Beyond scientific recommendations for facilities, how should the LRP tackle the future of astronomy on Maunakea?

• Timescale for decisions? • Implications for existing (e.g. CFHT, Gemini) and future (e.g. MSE) facilities? • Future approaches to site selection/partnership/management?

Ellison_HAA_LRP_discuss 133