LRP2020 Nov2019 CSA Town

Home , Odin (satellite), Spica

LRP2020_Nov2019_CSA_TownHall_Intro 2 Cowan_CSA_Small_Sats 8 Hlozek_LiteBIRD 29 Hudson_Euclid_LRP 51 Fissel_balloons_lrp2020_csa_townhall_2019oct31 64 Cote_CASTOR_LRP2020_CSA_final 72 Spencer_SPICA_LRP2020_20191031 96 Hoffman_Colibri_CSA_townhall_10-31 112 Gallagher_CASCA_LRPTownhall_final 132 LRP2020 town hall introduction

Pauline Barmby & Bryan Gaensler LRP Co-Chairs

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

LRP2020_Nov2019_CSA_TownHall_Intro 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_Nov2019_CSA_TownHall_Intro 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_Nov2019_CSA_TownHall_Intro 4 Schedule See http://bit.ly/lrp_th 1300-1315 CSA President Sylvain Laporte 1315-1330 Small satellites Nick Cowan 1330-1345 LiteBIRD Renée Hložek 1345-1400 Euclid Mike Hudson 1400-1410 Balloons Laura Fissel 1410-1435 Discussion Pauline Barmby (moderator) 1435-1450 Coffee break 1450-1505 CASTOR Patrick Côté 1505-1520 SPICA Locke Spencer 1520-1535 Colibrì Kelsey Hoffman 1535-1600 Discussion Bryan Gaensler (moderator) 1600-1630 Long-term Planning and Capacity Building S. Gallagher

LRP2020_Nov2019_CSA_TownHall_Intro1630-1645 General discussion and wrap-up S. Gallagher (moderator)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_Nov2019_CSA_TownHall_Intro 6 Afterwards › Future town halls: UdeM tomorrow, Toronto Nov 12, Vancouver Nov 26, Victoria Nov 27, Edmonton Nov 29

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

LRP2020_Nov2019_CSA_TownHall_Intro 7 Canadian Leadership in Small Satellite Astronomy

Nick Cowan (McGill University) w/slides from Taylor Bell, Stan Metchev, Jason Rowe

Cowan_CSA_Small_Sats 8 Why Canadian Small Satellites?

Proven track record Promising new concepts Develop Canadian expertise/leadership CSA can afford them

Cowan_CSA_Small_Sats 9 Track Record of Canadian Small Sats

• Microvariability and Oscillation of Stars (MOST) • 2003-2019 • BRIght Target Explorer (BRITE) Constellation • 2013-present • Near-Earth Object Surveillance Satellite (NEOSSat) • 2013-present

Cowan_CSA_Small_Sats 10 Canada’s space telescope Microvariability & Oscillations of STars Microvariabilité et Oscillations STellaire ✓ Canadian space telescope ✓ 54 kg, 60×60×30 cm ✓ Power: solar panels ✓ peak ~ 38 W ✓ Attitude Control System: ✓ reaction wheels ✓ pointing accuracy ~ 1” ✓ Communication: S-band ✓ frequency ~ 2 GHz ✓ Lifetime: 2003-2019 CONTRACTORS: Dynacon Inc.

Cowan_CSA_Small_SatsU of T Institute for Aerospace Studies 11 MOST science

✓ Sun-like stars ✓ asteroseismology Procyon ✓ surface spots, activity

✓ ancient halo intruders Wolf-Rayet star ✓ magnetic (Ap) stars HD 56925 ✓ massive evolved stars ✓ wind turbulence ✓ pulsations ✓ exoplanet systems

✓ pulsating protostars ✓ red giants … and more! 51 Peg b 51 Peg A Cowan_CSA_Small_Sats 12 BRITE Constellation

Cowan_CSA_Small_Sats 13 Cowan_CSA_Small_Sats 14 NEOSSat

❖ 15-cm optical space telescope

❖ launched February 25, 2013

❖ 800-km polar Sun- synchronous orbit (~100 min period)

❖ CVZ +/- 30 deg DEC

❖ Shared by DRDC and CSA

❖ Canadian AO

❖ Oversubscription of ~4.6

Cowan_CSA_Small_Sats 15 ❖ NEOSSat Photometry of WASP-33 NEOSSat Performance ❖ V~8 mag, mmag photometry with 1-sec exposures

Saturation

Comet 46P

Cowan_CSA_Small_Sats 16 Two Potential Canadian Small Sats • POEP (Photometric Observations of Extrasolar Planets) Science Maturation Study • Jason Rowe (Bishop’s) & Stan Metchev (Western)

• ÉPPÉ (Extrasolar Planet Polarimetry Explorer/ Explorateur polarimétrique des planets extrasolaires) Concept Study • Stan Metchev (Western), Taylor Bell & Nick Cowan (McGill), Christian Marois (NRC)

Cowan_CSA_Small_Sats 17 Primary Goals 1. Measure precision u-band transit depths to detect atmospheric scattering. 2. Detecting HZ rocky planets around low-mass stars.

MISSION OVERVIEW

Launch Date Nov, 2025

Orbit 800 km Sun- Synchronous SMS Completed! Ready for Phase-0 Aperture 15 cm

The baseline mission is a Micro- Filters 300-400 nm (u) satellite with high-efficiency 650-850 nm (i) photometer to obtain dual-band ultra- Integration TImes 1 sec - 5 minutes precision, high duty-cycle measurements of extrasolar planets. Detectors Dual 47-20 Frame- Transfer CCDs Cowan_CSA_Small_Sats 18 Detecting the Atmosphere of an Exoplanet

JAXA

Venus Transiting the Sun

Cowan_CSA_Small_Sats 19 Credit: NAOJ Clouds and Hazes… • Dampen spectral features in transmission and emission What’s the • Determine planetary albedo fuss about • Control climate Aerosols? • Detectability w/ LUVEx • Are hard to study with photometry or spectroscopy • Need Polarimetry!

Cowan_CSA_Small_Sats 20 ÉPPÉ: A CSA funded microsat concept study for exoplanet characterization

Notional Design • D = 30 cm • 흀 = 400–900 nm • Payload: 35x35x85 cm, 81 kg (179 kg wet) • Low-Earth, Sun-synchronous orbit • Differential polarimetry • Unique space-based capability • Pathfinder for biomarker detection on exoplanets Cowan_CSA_Small_Sats Image Credit: CC BY-SA 3.0 Luciano Mendez21 ÉPPÉ Targets

Cowan_CSA_Small_Sats 22 Small Sat Recommendations

• Phase 0 Study for POEP • Science Maturation Study for ÉPPÉ • Continued NEOSSat Operations • Regular, dedicated funding for micro sats

Is there anything small sats can’t do for exoplanets?

Cowan_CSA_Small_Sats 23 Small Sat Recommendations

• Phase 0 Study for POEP • Science Maturation Study for ÉPPÉ • Continued NEOSSat Operations • Regular, dedicated funding for micro sats

Is there anything small sats can’t do for exoplanets? SPECTROSCOPY! (and JWST can’t do 103 planets)

Cowan_CSA_Small_Sats 24 “A space mission consisting of a ∼1 m telescope with an optical–NIR spectrograph could measure molecular absorption for non-terrestrial planets discovered by TESS, as well as eclipses and phase variations for the hottest jovians. Such a mission could observe up to 103 transits per year, thus enabling it to survey a large fraction of the bright (J < 11) hot-Jupiters and warm sub- Neptunes TESS is expected to find.” Cowan, Greene, et al. 2015, PASP

Cowan_CSA_Small_Sats 25 • 1m primary @ L2 • 0.5-7.8 micron simultaneous spectra • Transits, eclipses and phases of 1000 planets • Approved ESA M4, launch in 2028

Cowan_CSA_Small_Sats ARIEL26 Canada has been invited to contribute to these

Cowan_CSA_Small_Sats 27 Small Sat Recommendations

• Phase 0 Study for POEP • Science Maturation Study for ÉPPÉ • Continued NEOSSat Operations • Regular, dedicated funding for micro sats

• Participate in ARIEL !

Cowan_CSA_Small_Sats 28 LiteBIRD

Renée Hlozek for the Canadian LiteBIRD team CSA Town Hall October 31, 2019

Hlozek_LiteBIRD 29 LiteBIRD

Slide: G. Smecher

Hlozek_LiteBIRD 30 LiteBIRD: Summary “Detecting primordial gravitational waves would be one of the most signiﬁcant scientiﬁc discoveries of all time.”

Final report of the task force on cosmic microwave background research “Weiss committee report”, July 11, 2005, arXiv/0604101

LiteBIRD Science impact

•Smoking gun signature for inflation – the physics of the big bang birth of the universe. •Constrain theories of quantum gravity •Host of additional scientific measurements long after nominal mission(reionization history, power spectrum deviation from ɅCDM, galactic magnetic field etc.)

LiteBIRD will see the gravity waves that were produced at the birth of our universe, and answer the most important cosmological question of how the cosmic structures originated.

Hlozek_LiteBIRD 31 July 2019: LiteBIRD was selected as a Japanese LiteBIRD Stretegic Large mission

Hlozek_LiteBIRD 32 GOAL: Map tensor mode spectrum to constraints on inﬂation

Large scale constraints are key: LiteBIRD will improve over Planck by a factor of 20

Hlozek_LiteBIRD 33 Current

B-mode BICEP2+Keck BICEP2+Keck/Planck detections Polarbear SPTpol 0.10 ] 2 K µ [ π /2 BB l

+1)C 0.01 l ( l

r=0.1

0.001 1 10 100 1000 Multipole l LAMBDA - October 2018

Hlozek_LiteBIRD 34 Current B-mode upper bounds

Hlozek_LiteBIRD 35 LiteBIRD make a 3sigma detection of

r = 0.003 ACTPol

Secondary effect SPTPol Inflation (Gravitational lensing)

Full Success s(r) < 1 x 10-3 (for r=0) LiteBIRD 2 ≤ ` ≤ 200

This will distinguish between different inﬂationary scenarios Hlozek_LiteBIRD 36 LiteBIRD will be able to detect the reionization bump at l=4 and the recombindation bump at l=80

Improving constraints on optical depth which is the limiting factor for large scale structure constraints (e.g. massive neutrinos)

Hlozek_LiteBIRD 37 LiteBIRD will make a large scale map of the Galactic polarization, enabling studies of the magnetic ﬁeld of the MW

Canadian facilities like CHIME can leverage this through cross correlation of polarization with rotation measure from CHIME

Hlozek_LiteBIRD 38 Science Space Astronomy Leadership LiteBIRD was highest priority mid-scale mission in Long The majority of the world’s mm-wave telescopes already Range Plan Midterm review in 2016 use Canadian readout electronics on the ground and LiteBIRD will enable Canada to be part of international space stratospheric balloons. Canadian readout is on critical mission that probes fundamental question of our origin by path for LiteBIRD. measuring gravitational waves from inﬂation LiteBIRD would establish leadership in keystone 15 multi-frequency maps generate a host of ancillary science technology for TES detectors on satellite platforms. with LiteBIRD data, Canadian community already leads that LiteBIRD train HQP to continue excellence in developing science software for analysis and diagnostics of space systems.

LiteBIRD and Canada

Commercialization Training and HQP On-board signal processing is a trend expected to LiteBIRD requires radiation-hardness-by-design intensify, for payloads of all types: from communications to methodology. Applications to other missions rely primarily science instruments and Earth Observation on know-how rather than proprietary technology. LiteBIRD LiteBIRD provides an early reduction to practice for new implementations establish this know-how in Canada. on-board DSP techniques that are applicable more Training scientists and engineers as leaders for Canada’s broadly, such as FPGA-based compression. space economy. Technology developed for LiteBIRD transferrable both to Embedding trainees in areas where Canada already has other astronomy facilities (e.g. CHIME) and to ﬁelds world leadership in CMB technology, analysis and theory outside astronomy. for the past 4 decades. Hlozek_LiteBIRD 39 LiteBIRD Technology

DfMux is signature Canadian technology — already used in world- leading ground-based mm-wave telescopes (SPT, POLARBEAR) Flown in EbEx stratospheric balloon, tried and tested technology Baselined for LiteBIRD mission:

Canada has leveraged critical component of LiteBIRD mission contribution to include detector readout design, monitoring software technology and analysis

Hlozek_LiteBIRD 40 LiteBIRD Technology: Canadian critical path

Hlozek_LiteBIRD 41 Science Space Astronomy Leadership LiteBIRD was highest priority mid-scale mission in Long The majority of the world’s mm-wave telescopes already Range Plan Midterm review in 2016 use Canadian readout electronics on the ground and LiteBIRD will enable Canada to be part of international space stratospheric balloons. Canadian readout is on critical mission that probes fundamental question of our origin by path for LiteBIRD. measuring gravitational waves from inﬂation LiteBIRD would establish leadership in keystone 15 multi-frequency maps generate a host of ancillary science technology for TES detectors on satellite platforms. with LiteBIRD data, Canadian community already leads that LiteBIRD train HQP to continue excellence in developing science software for analysis and diagnostics of space systems.

LiteBIRD and Canada

Hlozek_LiteBIRD 43 Science Space Astronomy Leadership LiteBIRD was highest priority mid-scale mission in Long The majority of the world’s mm-wave telescopes already Range Plan Midterm review in 2016 use Canadian readout electronics on the ground and LiteBIRD will enable Canada to be part of international space stratospheric balloons. Canadian readout is on critical mission that probes fundamental question of our origin by path for LiteBIRD. measuring gravitational waves from inﬂation LiteBIRD would establish leadership in keystone 15 multi-frequency maps generate a host of ancillary science technology for TES detectors on satellite platforms. with LiteBIRD data, Canadian community already leads that LiteBIRD train HQP to continue excellence in developing science software for analysis and diagnostics of space systems.

LiteBIRD and Canada

Hlozek_LiteBIRD 45 Science Space Astronomy Leadership LiteBIRD was highest priority mid-scale mission in Long The majority of the world’s mm-wave telescopes already Range Plan Midterm review in 2016 use Canadian readout electronics on the ground and LiteBIRD will enable Canada to be part of international space stratospheric balloons. Canadian readout is on critical mission that probes fundamental question of our origin by path for LiteBIRD. measuring gravitational waves from inﬂation LiteBIRD would establish leadership in keystone 15 multi-frequency maps generate a host of ancillary science technology for TES detectors on satellite platforms. with LiteBIRD data, Canadian community already leads that LiteBIRD train HQP to continue excellence in developing science software for analysis and diagnostics of space systems.

LiteBIRD and Canada

LiteBIRD is the only large scale mission currently approved (by JAXA, under review by NASA)

Hlozek_LiteBIRD 47 LiteBIRD timeline

Hlozek_LiteBIRD 48 LiteBIRD costs

From Hlozek et al. LRP White paper: CMB Science in Canada LiteBIRD is the highest priority mission for fundamental CMB science

Hlozek_LiteBIRD 49 Josh Montgomery installing DfMUX readout at the South Pole Telescope

“Detecting primordial gravitational waves would be one of the most signiﬁcant scientiﬁc discoveries of all time.” As of July 2019, LiteBIRD was selected as a Japanese Stretegic Large mission. LiteBIRD is a key strategic priority for Next step is to prepare the transition CMB science in Canada. to Phase A.

Hlozek_LiteBIRD 50 Euclid

Mike Hudson

on behalf of Canadian Euclid Consortium

Hudson_Euclid_LRP 51 Euclid: a survey machine driven by cosmology

Galaxy clustering Weak lensing BOSS NASA/JPL

Type 1a supernovae Cluster counts CMB cross correlations

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 52 A panchromatic wide-field survey

VIS NISP NISP grism

* NISP simulation does not include cosmic rays

VIS Y J H GRISM Wide 24.5 24 24 24 2x10-16 erg/s/cm2 Deep 26.5 26 26 26 2x10-17 erg/s/cm2

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 53 Euclid reference survey: DR3 secure

Wide 15459 deg2 Deep 40 deg2 10 billion sources

• EDF-N (NEP) 1 billion galaxy shapes • EDF-S (SEP) • EDF-Fornax (CDF-S) 30 million redshifts

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 54 Euclid Legacy

The primary cosmology probes drive the design of the survey, but the resulting data set enables an enormous amount of legacy science, which cannot be done otherwise:

2 Euclid will image 15,000 deg in YJHAB=24, which would take 680 years to complete with VISTA.

2 The deep survey of 40 deg down to YJHAB=26 would take 72 years with VISTA.

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 55 Euclid Legacy

Euclid images of z~1 galaxies will have the same resolution as SDSS images at z~0.05 and will be at least 3 magnitudes deeper … over 15,000 sq degrees!

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 56 SLACS (~2010 - HST): gravitational lensing by galaxies

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 57 SLACS (~2010 - HST): gravitational lensing by galaxies

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 58 The Euclid mission

2008 Proposal 2016 2026 selection

2012 2022 2030 Mission launch End of adoption nominal mission

European Space Agency led mission

• Second medium mission in Cosmic Visions program

• Dark Energy experiment with great auxiliary science opportunities

• 3 years from launch

• 6 year mission

• Incremental public data releases approximately every 2 years

• http://www.euclid-ec.org/

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 59 Euclid Satellite (Structural Thermal Model – STM)

Images: ESA/ADS/ThalesAleniaSpace

CSA 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 60 Euclid & Canada

To date the Euclid Consortium (EC) includes members from 14 European countries with additional contributions from the US and Canada. In total, over 1200 scientists and engineers are registered in the EC, which makes it the largest astronomy consortium to date.

Of which 27 are Canadian faculty: Michael Balogh, Dick Bond, Jo Bovy, Raymond Carlberg, Scott Chapman, Patrick Cote, Nicolas Cowan, Sebastien Fabbro, Laura Ferrarese, Stephen Gwyn, Renee Hlozek, Mike Hudson, John Hutchings, JJ Kavelaars, Dustin Lang, Alan McConnachie, Adam Muzzin, Laura Parker, Will Percival, Chris Pritchet, Marcin Sawicki, David Schade, Douglas Scott, Kendrick Smith, Kristine Spekkens, James Taylor, Chris Willott

Almost all of these “bought” in through Canada-France Imaging Survey data access.

Several Canadians in leadership roles

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 61 Euclid & Canada

2 ways in which Canadians can take advantage of this opportunity

1. Join existing Euclid Science Working Groups (SWGs). Ø Work on Key Projects: participate/lead Key Project papers

2. Use Euclid proprietary data in 1-2 years in advance of public release: Ø “Standard papers”

This is a huge opportunity for Canada.

But need support to take advantage of this opportunity • Postdoctoral funding needed to play important role in SWGs • Funds for travel to team meetings

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 62 References

For more information visit the consortium website at: http://www.euclid-ec.org/

Euclid Definition Study Report, Laureijs et al. 2011, arXiv:1110.3193 (~1500! citations already)

LRP 2019-10-31 M. Hudson, on behalf of the CEC Hudson_Euclid_LRP 63 Opportunities for Canadian near-Space Astronomy with Balloon-borne Platforms

Laura Fissel Queen’s University CSA LRP2020 Townhall October 31st, 2019 See also LRP2020 White Paper E073: “Balloon astrophysics in Canada over the next decade” by Fissel, Doyle, Dobbs, Halpern, Hanna, Marois, Netterfield, and Thibault Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 1 64 Picture: view from the Spider Balloon Telescope Balloon astronomy overview 2 millions cubic metres stratospheric balloon

• Stratospheric helium Boeing 747 balloons can lift science

payloads of up to 2,700 kgs Goodyear blimp up to 46 km above the At launch Earth’s surface. • At present balloons used are zero-pressure Eiffel tower • vent helium if the pressure in Height: 300m the balloon becomes too high NASA/CSBF • limited to short flights (1-2 days), or launch sites where the sun doesn’t set (Antarctic/Arctic summer) • Balloon astronomy allows near-space quality observing conditions at ~1% the cost of an equivalent satellite. Inflating balloon illuminated by sun (Steve Benton, 2012)

Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 2 65 Balloon Astronomy in Canada • Funding and support provided Canadian Space Agency’s (CSA) Flights and Fieldwork for the Advancement of Science and Technology (FAST) program (5 completed calls since 2011, one this year). • Maximum funding cap has ranged over a three year award has ranged from 250,000-500,000 CAD • Strong emphasis on HQP training Timmins balloon facility (CSA) • Canadian stratospheric balloon launch program (STRATOS) • launch site at the Timmins, Ontario airport (1-2 day flights) • launch support provided by CNES (France), through agreement with CSA Canadian payloads can also access other CNES launch sites, such as Kiruna, Sweden and Alice Springs, Australia. • Canadian astronomers are also important contributors to international collaborations (e.g. BLAST, Spider, HELIX), which typically utilize NASA long duration flights from Antarctica (up to 2 months aloft). SuperBIT launch from Timmins Sept th Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 17 2019 (@Superbit18) 3 66 How does investment in balloon astrophysics benefit Canada? • Training of experts for space astrophysics endeavors, the Canadian aerospace industry, and other tech employment fields. • Timescale of a balloon telescope: 3-5 years, well matched to a PhD length • Testing of new technologies in near space conditions to advance their HiCIBaS team prior to a technology readiness level (TRL) for use launch from Timmins (Laval) possible future satellite missions BLASTPol inferred • e.g. terahertz mKIDs detectors with BLAST- magnetic field map TNG, that could be useful for a future of the Vela C star mission like SPICA. forming region • Obtaining amazing science at much lower total cost compared to a space telescope. Fissel et al. 2016

Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 4 67

Figure 1: Intensity and magnetic ﬁeld orientation. Top left: raw map out of TOAST. Top right: linear modelling of the reference region. Bottom left: linear modelling of the reference region. Bottom right: Planck 353 GHz.

2 Priorities and Opportunities for Canadian Balloon Astronomy in the 2020s (1/3) • Continued support for HQP training and through the CSA’s FAST program. • Access to super-pressure and long duration balloon-borne flights Super-pressure balloon • Flight durations: Timmins 1-2 days, Photo: Richard Chirgwin Kiruna 4-6 days • Super-pressure balloons being developed by NASA launch from mid-latitudes for flights of up to 100 days. This would result in a huge increase in science that could be achieved from balloon-borne observatories! NASA SPB Trajectory 2015, 21 day flight from Wanaka NZ Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 5 68 Priorities and Opportunities for Canadian Balloon Astronomy in the 2020s (2/3) • Balloon gondola and flight infrastructure support • currently a large investment required from new PIs in developing balloon-borne experiments besides the telescope: • pointed gondolas • power systems • thermal control • safety analysis • ground station and flight software • we recommend looking into ways to reduce the barrier for new PIs through technology sharing • Similar programs WASP (NASA) arcsecond pointing platform, CNES gondola used by experiments like PILOT and Fireball

Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 6 69 Priorities and Opportunities for Canadian Balloon Astronomy in the 2020s (3/3) • Competitions to fund Canadian led large experiments • Maximum 500,000 CAD CSA-FAST funding can test technology, train HQP, and ensure important Canadian contributions to international balloon astrophysics collaborations, but are not enough to build a competitive balloon telescope with Canadian PIs. • Comparison: NASA-APRA 350,000 CAD to 660,000 per year for up to 5 years (2014-2018) • Suggest a periodic competition for a larger funding envelope for a balloon astronomy: • Should be for 5 years (FAST is 3year) • Possibility to combine funding with CFI Innovation fund • Should include a long-duration balloon flight opportunity • Applicant proposals should demonstrate: • significant training of HQP • support from the mission from the Canadian astronomy community and scientific returns that will benefit Canadian astronomers.

Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 7 70 Final Thought: Looking towards balloon-borne observatories

BLAST-TNG • With improvements in scientific ballooning technology (superpressure balloons), and significant expertise in the Canadian community balloon-borne observatories are possibly something worth considering. • Example: BLAST-TNG sub-mm polarimeter (NASA funded, significant Queen’s involvement) has made 25% of science time available for shared risk proposals. • Community driven balloon-borne observatories could be built for a small fraction of the cost of a satellite (~10 million CAD), but could be an ongoing project that is upgraded with successive flights and could be a pathfinder to future satellite missions. Fissel_balloons_lrp2020_csa_townhall_2019oct3110/31/19 Laura Fissel, CSA LRP2020 Townhall 8 71 The Core of the Virgo Cluster as seen by the Ultraviolet Imaging Telescope (UVIT)

GALEX

Cosmological Advanced Survey Telescope for Optical and uvThe CosmologicalResearch Advanced Survey(CASTOR) Telescope for Optical and uv Research

• Background and Context

• Mission Design and Architecture UVIT

• Science and Surveys

• Schedule and Partnerships

• CASTOR and LRP2020

Patrick Côté (NRC-Herzberg) on behalf of the CASTOR team Canadian Space Agency, St. Hubert, October 31, 2019

Cote_CASTOR_LRP2020_CSA_final https://www.castormission.org 72

GALEX UVIT

Credits: UVIT Team/ISRO/CSA CASTOR Development History The Cosmological Advanced Survey Telescope for Optical and uv Research

• 2010-2011: Long Range Plan for Canadian Astronomy. Highest priority in space astronomy is:

- “...signiﬁcant involvement in the next generation of dark energy missions — ESA‘s Euclid, or the NASA WFIRST mission, or a Canadian-led mission, the Canadian Space Telescope (CST).”

- “...Canadian space astronomy technology has reached the point that we could [now] lead a large space astronomy mission (Canadian Space Telescope).” (CST = CASTOR)

• 2011-2012: CSA study “Canadian Space Telescope mission (CASTOR) Concept Study”.

• 2013-2015: CSA study “Focal Plane Array Technologies for Astronomy”.

• 2015-2016: CSA study “Single Photon Counting Large Format Detectors with Enhanced UV Response for Space Astronomy”.

• 2016: Mid Term Review of the Long Range Plan for Canadian Astronomy:

- “MTR panel strongly recommends that the CSA launch a Phase 0 study, with study results required within 12 months.

• 2016: CSA Canadian Space Exploration Workshop: “Topical Team Final Reports”.

- “…the scientiﬁc potential of the mission is unparalleled.”

• 2016-2017: CSA Study: “Optical Design, Coatings, Filters, Dichroics”.

• 2018-2019: CSA Study: “Science Maturation Study for CASTOR”.

Cote_CASTOR_LRP2020_CSA_final 73 The Core of the Virgo Cluster as seen by the Ultraviolet Imaging Telescope (UVIT)

GALEX

The Cosmological Advanced Survey Telescope for Optical and uv Research

CASTOR Mission Design UVIT and Architecture

Cote_CASTOR_LRP2020_CSA_final 74

GALEX UVIT

Credits: UVIT Team/ISRO/CSA CASTOR Mission Speciﬁcations The Cosmological Advanced Survey Telescope for Optical and uv Research

Mission Design: Signiﬁcantly revised in 2018-2019. - updated science drivers and technical requirements. - schedule, risk and cost. - partnerships opportunities.

Team: Industry 1. Honeywell Aerospace. 2. ABB Inc. 3. Magellan Aerospace.

Government 1. NRC-Herzberg. 2. CSA.

Academia (40 universities and institutes)

International 1. JPL/Caltech/IPAC. 2. Indian Institute of Astrophysics. 3. United Kingdom, STFC.

Cote_CASTOR_LRP2020_CSA_final 75 CASTOR Mission Speciﬁcations The Cosmological Advanced Survey Telescope for Optical and uv Research

UV Spectrometer Photometer

1 Coarse Pointing Gimbal 0.8

0.6 Isolation Mount (as required for specific platform) Telescope 0.4

SystemQE Proximity 0.2 Electronics (pointing OPTRAC controller) (fine pointing control) 0 100# 200# 300# 400# 500# 600#

Cote_CASTOR_LRP2020_CSA_final Wavelength (nm) 76 CASTOR Mission Speciﬁcations The Cosmological Advanced Survey Telescope for Optical and uv Research

Cote_CASTOR_LRP2020_CSA_final 77 The Future of Wide-Field Imaging is in Space The Cosmological Advanced Survey Telescope for Optical and uv Research

UVOIR Region 1. No Atmospheric Turbulence. 2. Access to the Ultraviolet Region. 3. Photometric Calibration and Stability. 4. Low Backgrounds.

Subaru

Hubble

Cote_CASTOR_LRP2020_CSA_final 78 The Core of the Virgo Cluster as seen by the Ultraviolet Imaging Telescope (UVIT)

GALEX

Science and Surveys

The Cosmological Advanced Survey Telescope for Optical and uv Research

Time Domain Cosmology (L. van Waerbeke, UBC) Astrophysics (M. Drout, Toronto) CASTOR

AGNs, Galaxies & Black Holes & Cosmic SF Galactic Nuclei (M. Balogh, Waterloo) (S. Gallagher, Western) UVIT

Near Field Stellar Cosmology Astrophysics (P. Côté, NRC) (K. Venn, Victoria)

Exoplanets Solar System (J. Rowe, Bishop’s) (JJ. Kavelaars, NRC)

Cote_CASTOR_LRP2020_CSA_final 79

GALEX UVIT

Credits: UVIT Team/ISRO/CSA Scientiﬁc Uniqueness The Cosmological Advanced Survey Telescope for Optical and uv Research

Key Capabilities:

State-of-the-art image quality at < 550 nm. FWHM ≈ 5x better than LSST. Continued access to the UV in the post-HST era. Unique access to UV/blue region from space (imaging + spectroscopy). FoV (and discovery efﬁciency) exceeding Hubble by two orders of magnitude. Accurate photometric calibration and stable PSFs possible in space environments. Ultra-deep imaging at UV and blue-optical wavelengths possible due to low backgrounds.

CASTOR vs. Hubble: Comparison of Discovery Efﬁciencies x (Field of View) of x(Field (Total Throughput) Throughput) (Total

Cote_CASTOR_LRP2020_CSA_final 80 The CASTOR Primary Survey The Cosmological Advanced Survey Telescope for Optical and uv Research

Anticipated 5-year mission lifetime, with a possible extension. Key science goals to be addressed through surveys and Guest Observer (GO) programs. Primary survey (1.6 yrs) deﬁned by science working groups.

Cote_CASTOR_LRP2020_CSA_final 81 The Widest, Deepest and Sharpest View of the Universe The Cosmological Advanced Survey Telescope for Optical and uv Research Total Number of Resolution Elements

Decreasing Flux

Cote_CASTOR_LRP2020_CSA_final 82 Science. I. Cosmology and Dark Energy The Cosmological Advanced Survey Telescope for Optical and uv Research

• Stage IV DE experiments (LSST, Euclid, WFIRST) have been designed to combine wide-field, high spatial resolution, broad wavelength coverage, and high cadence to explore the nature of DE. No single experiment satisfies all criteria. • Scientific drivers within the envisioned landscape: 1. Photometric redshifts - short-wavelength data for improved photo-zs - best results for CASTOR + WFIRST + LSST. 2. Object detection and blending - to address the fundamental issues of blending, colour mixing and object detection. 3. Shape measurements - a unique wavelength region to study possible shape - CASTOR Science Report residual systematics as a function of passband. - Graham et al. (2019, submitted).

LSST alone (full depth) add shallow NIR (Euclid) add deep NIR (WFIRST) add UV + deeper u,g (CASTOR)

Cote_CASTOR_LRP2020_CSA_final 83 Science. II. Time Domain Astrophysics The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: sensitivity, scheduling, UV/blue imaging and spectroscopy, ﬁeld of view, angular resolution.

1. CASTOR MMA: ToO Observations for Multi-Messenger Events

• Phase 1: tiling the GW/neutrino localization regions for select MM events. • Phase 2: high-cadence monitoring of identiﬁed UV counterparts and characterization of host environments of known MM events. • multi-band photometry and spectroscopy.

2. CASTOR Cadence: A Wide-Field UV Time Domain Survey

• Monitoring of two 10 deg2 LSST deep drilling ﬁelds. • Daily cadence, with a six month baseline, to a depth of 24.5 mag (S/N=5). • Would probe >5x the volume of any UV survey to date, for 3x as long, with 2x the cadence using a fraction of CASTOR’s time.

Cote_CASTOR_LRP2020_CSA_final 84 Science. III. Galaxies and Cosmic Star Formation The Cosmological Advanced Survey Telescope for Optical and uv Research COSMOS ﬁeld • CASTOR’s niches: UV/blue-optical response, ﬁeld of view, resolution, sensitivity

1. Evolution of the Cosmic Star Formation Rate (SFR)

• deﬁnitive measurement of the cosmic SFR from rest-frame UV ﬂuxes to z=1.5. • UV data combined with OIR data from LSST, Euclid and WFIRST.

2. Ultra-Massive Galaxies (UMGs)

• a survey of UMGs (log M*/M⦿ > 11.5) based on their UVOIR emission. • within the region covered by CASTOR, LSST, Euclid and WFIRST, expect 5600 and 8400 UMGs between 0.1 < z < 0.3 and 0.4 < z < 0.6, respectively.

3. Galaxies at Cosmic Noon

• z=2 galaxies linked to their DM masses through clustering measurements. • high-precision photo-zs at all redshifts will enable the mapping of large scale structure, and hence the environmental dependences of galaxy evolution.

4. Spatially Resolved Star Formation Histories

• mapping of the SFR, dust distribution and stellar populations within galaxies at a resolution previously only achievable by HST, but with small samples. • trace the growth of morphological components (disks, bars, bulges, etc) over cosmic time and across a range of environments.

Cote_CASTOR_LRP2020_CSA_final - courtesy Emily Pass & Michael Balogh85 Science. IV. AGNs and Supermassive Black Holes The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: UV response, ﬁeld of view, scheduling, angular resolution, spectroscopy.

1. AGN Reverberation Mapping Survey

• Reverberation mapping of 12.5 deg2 (>1000 AGNs) for 6 mths.

• Imaging (21 days) and slit-less spectra (130 days) to mUV ~ 24. • Time lags ➜ black hole masses for 10x more AGN than all previous studies, over a wider redshift space.

2. AGN Studies with the CASTOR Primary Survey

• Identiﬁcation of new, faint AGN from UV/blue-optical colours.

- CASTOR Science Report

Cote_CASTOR_LRP2020_CSA_final 86 Science. V. Near Field Cosmology The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: UV/blue response, sensitivity, ﬁeld of view, angular WFIRST only resolution.

1. Tests of Cosmological Models on Sub-Galactic Scales

• Structure and stellar populations of Galactic satellites and stellar streams, including log T(yr) = 6.6, 7, 8, 9, 10 “missing satellites” predicted by ΔCDM models.

• multi-epoch imaging for proper motion measurements and dynamics. WFIRST + CASTOR

2. The CASTOR Nearby Galaxies Survey

• How does the physics of star formation change as a function of density? log T(yr) = 6.6, 7, • A (30 day) UV/u/g survey of 300 galaxies within ~20 Mpc to reconstruct the star 8, 9, 10 formation histories of galaxies in the Local universe. • Resolution ~ 30x that of GALEX. Field of view ~80x that of HST. -

Tractor u-band Simulations (Lang et al. 2016) LSST (10 years) CASTOR (1 hour)

Cote_CASTOR_LRP2020_CSA_final 87 Science. VI. Stellar Astrophysics The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: ﬁeld of view, spatial resolution, UV/blue response, sensitivity, spectroscopy.

1. The Structure and Chemistry of the Galactic Halo

• The three-dimensional metallicity distribution function for the Galactic halo. • Reconstruction of the Galactic star formation history from white dwarfs. • Identiﬁcation of the the chemically pristine halo stars. • Structure and shape of the Milky Way from Blue Horizontal branch stars.

2. The CASTOR Magellanic Clouds Survey Ibata Ibata et al. (2017) • Deep UV/u/g imaging and UV/u spectroscopy for tests of stellar evolutionary models. • Properties of the ISM across both galaxies.

simulated Galactic white dwarfs with the CASTOR primary survey shown.

- courtesyCote_CASTOR_LRP2020_CSA_final Nick Fantin - courtesy Guillaume Thomas 88 Science. VII. Extra-Solar Planets The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: UV/blue response, photometric precision, sensitivity, scheduling, time resolution, angular resolution.

1. Transit Colour Survey • transit-depths to ~10 ppm on 3 hr timescales in all passbands. • targets: 50 bright transiting exoplanets. - Schwieterman et al. (2018, AsBio, 18, 663). • scope: ~100 days over mission lifetime. • atm. opacities ➔ structure, composition, pressure & temperature.

2. Ultra-Precise Phase Curve Survey • g~6 target with a hot-Neptune. 3-hr CDPP to 1 ppm. • UV phase curve measurements over ~80 days (continuous). • scattering properties of atmosphere ➔ particle sizes & compositions.

3. Kepler Eta-Earth Project • fulﬁll Kepler’s primary mission goal: the detection of Earth-sized planets in the habitable zone of Sun-like stars. • ten g~12-14 stars with low-S/B transits. Transit depths 5-200 ppm. • program: 30 days per year over mission lifetime.

4. Exoplanets in Globular Clusters • strategy: photometric monitoring of 1.5 million stars in Omega Cen. • sample: 50x that of Gilliland et al. (2000) and 10x that of Kepler.

• detect: 15% - 65% of transits for planets with 0.6 - 0.8 RJupiter. Cote_CASTOR_LRP2020_CSA_final - Knutson et al. (2007, ApJ, 655, 564).89 Science. VIII. Small Bodies in the Solar System The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR’s niches: spatial resolution, UV/blue response, sensitivity, ﬁeld of view, scheduling.

simulated TNOs detectable by LSST and measurable in the CASTOR primary survey 1. Physical Properties of Excited Trans Neptunian Objects

• simultaneous u/g and red-optical ﬂux measurements for all ‘excited’ TNOs discovered by LSST that fall in the CASTOR primary survey. • 2500 classical Kuiper belt objects, 500 TNOs trapped in resonance with Neptune and > 700 TNOs on orbits that are actively scattering off Neptune. • UVOIR photometry for taxonomy and mineralization; light-curve measurements for shape modeling; binarity for formation and evolution - CASTOR Science Report modelling.

2. High-Resolution Kuiper Belt Binary Characterization Legacy Survey

• Full characterization of orbits for ~600 KB binaries (semi-major axes, eccentricities, inclinations and mass ratios): only possible with space- based observations. • a combination of CASTOR primary survey data and pointed observations of Kuiper Belt binaries discovered by LSST.

3. Solar System Legacy Survey

• deep survey of a ±0.5 deg strip centred on the ecliptic: composition and binarity sample for the low (cold-classical) component of the Kuiper belt.

Cote_CASTOR_LRP2020_CSA_final - Noll et al. (2008, SSBN, 345).90 The Core of the Virgo Cluster as seen by the Ultraviolet Imaging Telescope (UVIT)

GALEX

The Cosmological Advanced Survey Telescope for Optical and uv Research

CASTOR

Schedule and Partnerships UVIT

Cote_CASTOR_LRP2020_CSA_final 91

GALEX UVIT

Credits: UVIT Team/ISRO/CSA Possible Partners and Contributions The Cosmological Advanced Survey Telescope for Optical and uv Research

• Jet Propulsion Laboratory; California Institute of Technology; NASA; USA. - World experts in high-QE UV detectors. WFIRST, Euclid partners. - Proposed Contribution (through NASA Mission of Opportunity): delta-doping and coating, readout electronics, packaging for three assembled focal planes; software for data characterization, processing and calibration.

• Indian Institute of Astrophysics; Indian Space Research Organization; India. - Astrosat heritage. Proposed follow-up mission (INSIST) undergoing 1-yr pre-mission study (Mar. 2018- Mar. 2019). - INSIST-CASTOR meeting in Bangalore: agreement on joint mission, nearly identical to CASTOR. - Capabilities: Launch; DMD spectrograph; bus?; optical components; telescope; dichroics; ﬁlters; ground stations; software; archive.

• UK Space Agency; Science and Technology Facilities Council, UK. - Proposed Contribution: e2v CMOS detectors; opto-mechanics; thermal analysis; simulation software; etc. Euclid.

• Laboratoire d’Astrophysique de Marseille (LAM) and the Centre National d’Études Spatiales (CNES), France. • Grisms and DMD spectrosgraph; GALEX and BATMAN heritage. Euclid.

• Institute of Space and Astronautical Science (ISAS) and Japan Aerospace Exploration Agency (JAXA), Japan. • Chester F. Carlson Center for Imaging Science, Rochester Institute of Technology, USA. • Auckland Space Institute, New Zeland.

Cote_CASTOR_LRP2020_CSA_final 92 Development Schedule The Cosmological Advanced Survey Telescope for Optical and uv Research

• Assuming approval in 2020: • 12-month Phase A 2020 System Requirements. • 12-month Phase B 2021 Requirements → Preliminary Design Review. • 18-month Phase C 2022-3.5 Detailed Design → Critical Design Review. • 24-month Phase D 2024-5 Fabrication, Integration and Testing. • 60-month Phase E 2026 Operations.

2020 2021 2022 2023 2024 2025 2026

Phase A B C C D D E Partner India JPL, UK

LRD LSST Euclid WFIRST CASTOR

Cote_CASTOR_LRP2020_CSA_final 93 CASTOR and LRP2020 The Cosmological Advanced Survey Telescope for Optical and uv Research

• CASTOR is the lone remaining option identiﬁed in LRP2010 as a top priority for space astronomy.

• The concept is scientiﬁcally and technically mature after nearly a decade of study.

• A MIDEX-scale mission, with Canadian leadership possible for an investment comparable to JWST.

• Strong and growing international interest in the project.

• Prospective partners expect a commitment by mid 2020. Leadership is ours to lose.

• Many elements of the mission are well aligned with federal government policies for science and space:

- A compelling and broad science case.

- A new opportunity for Canadian aerospace companies.

- An inspiration to Canadians as a true ﬂagship mission and a symbol of Canada in space.

Cote_CASTOR_LRP2020_CSA_final 94 Cote_CASTOR_LRP2020_CSA_final 95 SPICA SPace Infrared telescope for Cosmology and Astrophysics The next great infrared space observatory An opportunity for Canada

Doug Johnstone and Locke Spencer On behalf of David Naylor and the Canadian SPICA team http://research.uleth.ca/spica

Canada: Abraham (Toronto), Bannister (Queen’s U. Belfast), Baum (Manitoba), Cami (Western), Chapman (Dalhousie), Coude (USRA), Di Francesco (NRC Herzberg), Fissel (Queens), Haggard (McGill), Halpern (UBC), Houde (Western), Hutchings (NRC Herzberg), Johnstone (NRC Herzberg), Joncas (Laval), Matthews (NRC Herzberg), Metchev (Western), O’Dea (Manitoba), Peeters, (Western), Plume (Calgary), Rosolowsky (Alberta), Sadavoy (Queens), Sawicki (St. Mary’s), Scott (UBC), Sivakoff (Alberta), Spencer (Lethbridge), Wilson (McMaster)

Spencer_SPICA_LRP2020_20191031 96 31 October 2019 LRP Town Hall 1 CSA HQ 1 A brief history of SPICA  2007: UL proposal to CSA in response to RFP for Canadian contributions to ESA CV call: tasked with identifying a meaningful role for Canada in the SPICA mission.  2009: funding issues resulted in SPICA lead moving from UK to Netherlands.  SRON had to offload some workpackages. High resolution Fourier transform spectrometer (FTS) package became available. Larger contribution with significantly greater ROI.  Prestigious role well matched to Canadian signature technology and academic strength.  2008 to May 2016 low level SPICA study contracts (UL) to establish a beachhead in SPICA.  SPICA FTS Mechanism Phase 0 (Industrial contract awarded to ABB ended June 2015).  2015 – 2019 STDP 9 (PT17) –Cryogenic Translation Mechanism for Future FIR Missions (ABB).  2016 – 2019 FAST Grant (A07) Cryogenic Fabry-Perot for SAFARI (UL).  SPICA proposal submitted to M5 call 5 October 2016.  SPICA selected as one of three M5 finalists 7 May 2018.  August 2019 STDP SPICATD to raise TRL of cryogenic translation mechanism (ABB).

Spencer_SPICA_LRP2020_20191031 97 31 October 2019 LRP Town Hall 1 CSA HQ 2 Mission Status •Mission well defined oJoint ESA-JAXA mission oSpacecraft elements & responsibilities defined oInstrument complement in final iteration oThree instruments: oSMI - Japan oSAFARI - European/Canadian/US oBBOP – France oESA: SPICA selected as one of three M5 finalists 7 May 2018 •Mission final selection Spring 2021 •Launch 2032(?) •JAXA: SPICA has passed the Mission Definition Review SPICA officially in ‘Pre-project’ phase (~phase A) H3 launch slot tentatively assigned to SPICA Japan will support an ESA SPICA mission at the 300M$ level

Spencer_SPICA_LRP2020_20191031 98 31 October 2019 LRP Town Hall 1 CSA HQ 3 Proposed Canadian contribution: the high resolution spectrometer of SAFARI Canadian CAL SKY ZERO signature mK cooler Focal-Plane Relay technology Beam steering mirror

SW Martin- Puplett VLW

Dichroic Dichroic Flip mirror

LW Grid or MW dichroic

SAFARI block diagram

Spencer_SPICA_LRP2020_20191031 99 31 October 2019 LRP Town Hall 1 CSA HQ 4 Contributions by nation

Approximate relative level of contribution as foreseen by SAFARI consortium partners Spencer_SPICA_LRP2020_20191031 100 31 October 2019 LRP Town Hall 1 CSA HQ 5 SPICA science – Sampler of Topics Unveiling Dusty Matter in the Universe

(Modified slides by Peter Roelfsema See also Johnstone et al. WP035)

10 pc

1 pc

Spencer_SPICA_LRP2020_20191031 101 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 6 The Evolving Universe – Zooming In Gas density

Redshift

Specific star form’n rate

Stellar light

Gas temperature

…SPICA will provide direct measurements of the physical parameters of evolving galaxies, unaffected by extinction

Gas metallicity Illustris-project.org

Spencer_SPICA_LRP2020_20191031 102 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 7 Mapping galaxies - 18-36 µm spectroscopy M81

• Imaging spectroscopy • Full 18-36 µm spectra at R 1300-2300 • Spatial resolution 3.7” at 35 µm • Scanning with wide slit  detailed spectral maps for nearby galaxies

SPICA beam @35 µm

Spencer_SPICA_LRP2020_20191031 103 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 8 Magnetic fields – driver in star formation in ISM filaments? Example: Taurus B211 filaments

Herschel 250 μm and PLANCK magnetic field

2.7 deg ~ 3 pc B-BOP will probe the link between magnetic field, low-density filaments (striations) and dense star-forming filaments characteristic filament width of 0.1 pc observable out to d ~ 350 pc not accessible to ALMA, neither to ground-based SCUBA2-Pol, NIKA2-Pol, neither to SOFIA, nor to balloon-borne Super BLAST-Pol Spencer_SPICA_LRP2020_20191031 104 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 9 HD – probing the mass of planetary disks

• HD 56/112 µm lines in the SAFARI bands Trapman et al 2017 • Direct tracer of gas mass in PPD’s • Opens entirely new domain of disk masses

Spencer_SPICA_LRP2020_20191031 105 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 10 IceIce histories:histories: PristinePristine versusversus diskdisk originorigin

SPICASPICA willwill probeprobe thethe historyhistory ofof waterwater iceice inin hundredshundreds ofof T TauriTauri disksdisks 1.00 crystalline ice (140 K, reference) cooldown (formed in warmwarm environment,environment, transported in disk)disk) 0.95 direct deposit (formed in situsitu inin disk)disk)

]

/ / warmup (formed in cold environment,environment,

m m transported in disk)disk)

/ / 0.90

1 1 0.85

[

n 0.80 includesincludes noisenoise ofof 1010 minmin exposureexposure (R=300)(R=300)

0.75

IcesIces inin emissionemission @ 4040 and/orand/or 6060 mµm 0.70 [TT:[TT: McClureMcClure etet al.al. 2013,2013, 2015;2015; HAeHAe: MalfaitMalfait etet al.al. 1999,1999, MeeusMeeus etet al.al. 2001,2001, MinMin etet al.al. 2016]2016] 40 50 60 70 80 l [micron] Spencer_SPICA_LRP2020_20191031 106 LRPLRP 20202020 CSACSA -- SPICASPICA ScienceScience (from(from P.P. Roelfsema)Roelfsema) 116 Resolution makes the difference – SMI-HRS

Predictions for molecular bands in proto planetary discs as observed SPITZER with Spitzer, JWST and SPICA

JWST

SPICA

Spencer_SPICA_LRP2020_20191031 107 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 12 Mineralogy – e.g. debris discs 69 µm feature for β-Pic (de Vries et al. 2012)

The mineralogy of micron-sized dust particles in discs directly probes the composition of their parent bodies • SPICA provides access to the far-IR resonances of several minerals, allowing a precise determination of their composition and structures • The composition of refractory dust in its exo-comets and make a direct comparison with our Solar System

Spencer_SPICA_LRP2020_20191031 108 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 13 SPICA science – Johnstone et al. WP035 and …

PASA collection: Exploring Astronomical Evolution with SPICA • Roelfsema et al - SPICA—A Large Cryogenic Infrared Space Telescope • Vd Tak et al - Probing the Baryon Cycle of Galaxies with SPICA • Kaneda et al - Unbiased Large Spectroscopic Surveys of Galaxies Selected by SPICA Using Dust Bands • Spinoglio et al - Galaxy Evolution Studies with SPICA: The Power of IR Spectroscopy • Gruppioni et al - Tracing the Evolution of Dust Obscured Star Formation and Accretion Back to the Reionisation Epoch with SPICA • Gonzales-Alfonso et al - Feedback and Feeding in the Context of Galaxy Evolution with SPICA: Direct Characterisation of Molecular Outflows and Inflows • Fernandez-Ontiviros et al - SPICA and the Chemical Evolution of Galaxies: The Rise of Metals and Dust • Egami et.el. - Probing the high-redshift universe with SPICA: Toward the epoch of reionisation and beyond • André et.al.- Probing the cold magnetized Universe with SPICA-POL (B-BOP)

https://www.cambridge.org/core/journals/publications-of-the-astronomical-society-of-australia/collections/exploring-astronomical-evolution-with-spica

Spencer_SPICA_LRP2020_20191031 109 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 14 Summary and conclusions (Naylor WP049) • Between 2008 to 2019, the CSA and UL will have invested over $5M in the SPICA project to establish and preserve a potential role for Canada in the SAFARI instrument. • Canada is positioned to build the mission critical, high resolution spectrometer of the leading infrared observatory of the next decade. • SPICA will be between 2 and 3 orders of magnitude more sensitive than Herschel. This transformational advance will fill the infrared gap between JWST and ALMA. • There is no risk of the science being scooped by another mission. • The ROI to Canadian science will be at least two times that of Herschel, which was one of the highest ROI of any CSA-funded space astronomy mission. • ESA will pick the winner of the three M5 finalists in June 2021. • Programmatically, a letter will be required before this date (i.e. early 2021) from the CSA to ESA effectively stating that if ESA chooses SPICA, Canada is committed to the project. • Securing mission funding requires approval from the Treasury Board of Canada. A strong statement of endorsement for SPICA in the LRP is a necessary prerequisite.

Spencer_SPICA_LRP2020_20191031 110 31 October 2019 LRP Town Hall 1 CSA HQ 15 SPICA science – sampler of topics Unveiling dusty matter in the universe

10 pc

1 pc

Spencer_SPICA_LRP2020_20191031 111 LRP 2020 CSA - SPICA Science (from P. Roelfsema) 16 More Information:

www.colibri-telescope.ca

Taking the pulse of Neutron Stars and Black Holes

Kelsey Hoffman and Daryl Haggard for the Colibrì Team contact: [email protected]

The Colibrì Team: Jeremy Heyl (PI), Ilaria Caiazzo, Kelsey Hoffman, Sarah Gallagher, Daryl Haggard, Piotr Jasiobedzki, Kostis Michelakis, Neil Rowlands, Samar Saﬁ-Harb, Gregory Sivakoff, Luigi Gallo, Ben Guest, Craig Heinke, Demet Kirmizibayrak, Sharon Morsink, Paul Ripoche, Mario Beaudoin, Dwight Caldwell, Andrew Cumming, Andrea Damascelli, Pinder Dosanjh, Josh Folk, Dennis Gregoris, Karl Jessen, Jagannath Kshtriya, Wolfgang Rau, Bob Rutledge, Ingrid Stairs, and Jeff Young

The First Canadian X-ray Telescope Concept Colibrì the Instrument Athena at 100 mCrab Colibrì is a proposed X-ray telescope concept designed to unveil the Colibr`ıSingle mysteries of neutron stars and black holes. With high spectral and time The Colibrì concept is based on multiple aperture non-imaging X-ray collectors similar to Colibr`ıDouble Athena resolution, and high throughput, Colibrì will allow the study of NICER but with cryogenically cooled transition edge detectors for high energy resolution and NICER 1 RXTE ] accretion disks and coronae, including reflection and re-emission of sensitivity. Colibrì aims to achieve an energy resolution finer than 1eV at 2 keV, and count rates 2 XMM radiation by the disk, and observations of isolated and accreting up to 100kHz, in an energy range of 0.5-10 keV. The timing of Colibrì aims to be better than neutron stars. 1!s, matching the innermost orbit period for a 10 solar-mass black hole. The total effective 2 1 Colibrì will take advantage of recent advancements in transition-edge area of Colibrì is to be at least 2000 cm at 6.4 keV. Optics concepts are currently being ective Area [m − ff E sensors (TES) technology to achieve eV-resolution spectroscopy with investigated in order to increase the effective area, for example a single-bounce vs. double- 10 nanoseconds-precision timing. Combining TES-based detectors with bounce collector. A comparison of the effective area anticipated for Colibrì as compared to collector optics, Colibrì will achieve a high throughput and a large other X-ray instruments is shown on the right. effective area. This concept study is being funded by the Canadian Space Agency (under contract number 9F050-170252/004/MTB). The transition-edge sensors (TESs) are to be developed with collaboration with the Stewart 1 10 Blusson Quantum Matter Institute at the University of British Columbia. Energy [keV] Science Questions 1) How do accretion disks transport matter? Test Case: Neutron Star Spectral Lines Black Hole Science 2) How are relativistic jets launched? Recently the Hitomi satellite found evidence for weak and narrow absorption lines The science objectives of Colibrì include the study of from the rotational-powered pulsar PSR J1833-1034 in the supernova remnant accretion disk physics and the effects of strong-field 3) What is the structure of spacetime surrounding black holes? G21.5-0.9 at 4.2345 keV and 9.296 keV. The upper figure shows the line detected with gravity around black holes, as well as probing 1the 4) What are the masses and radii of neutron stars? Hitomi at 4.2345keV from PSR J1833-1034 (blue) compared to simulations for Colibrì spacetime around black holes and putting constraints Mission Parameters for the same observing time with two mirror configurations: single-bounce collector on different theories of gravity. (black) with three times the geometric area of NICER and double-bounce collector • Energy Range: 0.1 - 10 keV (red) with the same geometric area as NICER. The lower figure is the comparison of • Energy Resolution: finer than 1 eV at 2 keV (3 eV at 6 keV) One of the most subtle consequences of GR is the “no- the Hitomi detection of the line at 9.296keV to the same simulations using the two hair” theorem, for which black holes can be fully • High throughput: count rates up to 100 kHz different mirror configurations of Colibrì. Colibrì will allow for the search of narrow characterized by their mass, angular momentum and • Timing resolution: better than 1 !s, matching the innermost spectral lines from a diversity of isolated and accretion powered pulsars, including charge. The only way to test this theorem is to probe orbit period for a 10 solar-mass black hole nursing magnetars and XRBs. the spacetime very close to the hole. Fortunately, the • Total effective area: 2000cm2 at 6.4 keV X-ray emission of accreting black holes carries Black: Colibrì information about the inner region of the accretion Neutron Star Science with single disk, within a few gravitational radii from the hole, bounce collector encoded in the fast variability of its spectrum. In The neutron star science objectives are the study of accreting and particular, the emission from the accretion flow very isolated neutron stars to understand the physics of accretion onto the close to accreting compact objects presents high- surface and measure properties such as mass, radius and atmospheric precision diagnostics of their spacetime, including composition. The high sensitivity and high-timing resolution of Colibrì reverberation mapping and quasi-periodic oscillations. will allow for detection of reverberation lags in neutron star binaries. Furthermore, variability in the X-ray emission from Spectral line observations would measure the atmosphere composition Red: Colibrì with double bounce accreting compact objects also carries information on and the ratio of M/R. Measurement of the width of the spectral line of Blue line: Hitomi detection of line collector the accretion processes themselves. a pulsar with known spin period, as in the case of the 61.9 ms PSR at 4.2345keV of PSR J1833-1034 J1833-1034, could provide extra constraints on the neutron star's radius (See Test Case Box). Reverberation Mapping Blue line: Hitomi detection of line In both neutron stars and black holes, X-ray emission Quasi-Periodic Oscillations at 9.296keV of PSR J1833-1034 Red: Colibrì with CANADA’S FLAGSHIP X-RAY TELESCOPEfrom outside the disk (coming from the neutron star’s Observations of BHBs with RXTE have driven extraordinary progress double bounce surface or from a glowing corona above the black hole) in the study of their variability properties. In many of these systems, collector; note the higher sensitivity can be reflected by the disk into our line of sight. By quasi periodic oscillations (QPOs) were discovered and thought to to hard X-rays. correlating the primary emission with the reflected originate in the inner regions of the accretion disk. The mechanism one we can map the accretion disk: as more distant responsible for QPOs is still debated, but a careful study of their regions of the accretion disk will be illuminated in characteristics can lead to a better understanding of the physics of Black: Colibrì with subsequent times, photons of different energy will black-hole accretion and of general relativistic effects in the strong field single bounce present different time delays. regime. collector The combination of high sensitivity and high timing Observations of the higher-frequency peak of neutron star kHz QPOs resolution of Colibrì will enable the detection of would help to place constraints on the mass-radius relationship of reverberation lags for neutron star binaries. neutron stars.THE COLIBRÌ MISSION

Hoffman_Colibri_CSA_townhall_10-31 112 Colibrì: Take Home Message

High- Time Resolution High-Spectral Resolution High-Throughput

Transition Edge Sensor (TES) Detectors in Space

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 2 113 The Colibrì Team

Jeremy Heyl, UBC Ilaria Caiazzo, UBC Kelsey Hoffman, Bishop’s

Principle Investigator Project Scientist Project Manager

Daryl Haggard, McGill Sarah Gallagher, Western Samar Saﬁ-Harb, Manitoba

Mission Planning Lead Black Holes WG Lead Neutron Star WG Lead

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 3 114 The Colibrì Team

Gregory Sivakoff, Alberta Kostis Michelakis, SBQMI, UBC

Coordinated Observations Lead Detectors

Neil Rowlands, Honeywell Piotr Jasiobedzki, MDA

Payload Satellite

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 4 115 The Colibrì Team

Benson Guest, University of Manitoba

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 5 116 Colibrì Mission Overview

❖ High-time resolution, high-spectral resolution and high throughput

❖ Science questions: 1. Does general relativity apply in the strong gravity regime? Is spacetime around black holes well described by the Kerr metric?

2. Can we better understand the physics of accretion? How do accretion disks lose angular momentum? What is the mechanism behind winds? How are jets launched? 3. How does matter behave in extreme environments in terms of density, gravity and magnetic ﬁelds? What is the physics of ultra-dense matter? What are the masses, radii and atmospheric composition of neutron stars?

❖ Current Status: 18-month concept study (September 2018 - February 2020)

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 6 117 Colibrì Mission Specs

❖ Energy Range: 0.5 - 20 keV ❖ Focal Length: 4.9 m

❖ Energy Resolution: 2 - 5 eV ❖ Number of Arrays: 7

❖ Timing Resolution: 250 ns ❖ Foils per Array: 30

❖ 2 Effective Area: 3000 cm ❖ Coating: Iridium

❖ Count Rate: >100 kHz ❖ Detectors: TES ❖ Orbit: Sun Synchronous, Bolometers 500-800km ❖ Bath Temp: 70 mK

❖ Mission Lifetime: 5 years ❖ Tc = 100 mK ❖ Ground Ops: X-band, CSA Sat-Ops/ NRCan

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 7 118 Colibrì: TES Detectors

❖ Transition Edge Sensors: high ❖ On-board pulse processing - energy resolution and Sample every 5 microseconds sensitivity ❖ Use of Linear ﬁlters (Paul Ripoche, ❖ Canadian TES detector Graduate student at UBC) development to be at Stewart Blusson Quantum Matter Institute at UBC

TES array for X-ray detection from Lee et al. 2015

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 8 119 Colibrì Science Goals

Black Holes Neutron Stars

❖ Reverberation mapping: Test ❖ Lines/Spectroscopy: Isolated GR, measure BH Mass and Accreting

❖ Quasi Periodic Oscillations ❖ Magnetar Spectral Lines ❖ Accretion Disk Winds ❖ Warm/Hot Intergalactic Medium ❖ Quasi Periodic Oscillations

❖ High Velocity Hot Outﬂows ❖ Thermonuclear bursts

❖ See WP 036 for more details, Mass & Radius of Neutron Stars Talk by Ilaria Caiazzo at UBC Town Hall (Nov 26)

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 9 120 Spectral Features: PSR J1833-1034

Key mission specs: High-Spectral Resolution Blue line: Hitomi detection of line at High Throughput 9.296 keV of PSR J1833-1034 High-Time Resolution

Colibrì Double f/10

Colibrì Single f/10

Hitomi Simulations by Benson Guest, PhD Student at U Manitoba

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 10 121 Magnetar Outbursts: SGR 1900+14 1 1 − 6000 Colibrì − XMM-Newton 2000 keV keV 1 1 − −

4000

1000

2000 normalized counts s normalized counts s

0 0 4 2

2 0 model)/error model)/error

− − 0

(data −2 (data −2 5 5 Energy (keV) Energy (keV)

3−May−2019 21:00 Key mission specs: High-Spectral Resolution Simulations by Demet High-Throughput Kirmizibayrak, PhD Student at UBC No pile up issue for bright bursts

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 11 122 SGR 0418+5729 Phase Resolved Spectroscopy

Key mission specs: Simulations by Demet High-Time Resolution Kirmizibayrak, PhD Student at UBC High-Spectral Resolution Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 12 123 Colibrì: Training and Retention

❖ HQP Training:

❖ Student involvement has already been instrumental for the progress of the study

❖ Preparation of the next generation of leaders

❖ HQP Retention:

❖ Science ofﬁce staff positions (R6 of WP: 64)

❖ Continued mission development also supports the Space Sector

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 13 124 Colibrì and the Canadian Landscape

BRITE ? NEOSSat ? JWST XRISM Euclid POEP LiteBIRD CASTOR ÉPPÉ ? ?

Colibrì Pre-Phase A A B C D: MAIT+ SPICA

2020 2025 2030 2035

Main Mission Extended Mission

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 14 125 Colibrì: Next Steps

❖ FAST — Recently submitted, will increase SRL

❖ SMS — Validate Science requirements, increase SRL

❖ Develop secondary science goals

❖ STDP — Increase TRL of Canadian made TES detectors

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 15 126 The Colibrì Mission

❖ Canada’s First Flagship X-ray telescope

❖ Builds on CSA’s investment in Hitomi and XRISM

❖ Study the laws of the Physics of the Extreme

❖ Combination of high-time resolution, high-spectral resolution and high throughput

❖ Development of TES detectors in Canada

❖ Opportunities for HQP training throughout development and mission operations

❖ Job Creation: Through HQP retention via science ofﬁce, grow the detector industry in Canada, support Canadian space sector — Build a robust and experienced workforce in the Space Sciences

❖ In order to continue the development through 2020-2030, build capacity through a space program and support in the LRP report is required

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 16 127 Back up slides

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 17 128 Colibrì Effective Collecting Area

Baseline Mission

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 18 129 Comparison to other X-ray Missions 6 10 ● Colibr`ı 1 ] 2 Colibr`ı 5 RXTE

10 ● 1 XMM EPIC pn Burst − ATHENA ● 10 XMM EPIC pn ● NICER ● ATHENA Blur

Hitomi 4 2 − SXS 10

10 NICER 3

3 Chandra HRC − RXTE XMM Chandra Chandra ACIS E ﬀ ective Area [m

10 ● ● 10 RGS Gratings ● XMM EPIC pn Timing ● ATHENA Maximum Count Rate [Hz] 4 Hitomi SXS − ● 10 2 3 4 1 10 10 10 10 10 102 103 104 105 106 107 108 Spectral Resolution [E/∆E] Time Resolution [ns]

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 19 130 Spectral Features: PSR J1833-1034

Colibrì Single f/10

Colibrì Double f/10

Blue line: Hitomi detection of line at 4.2345keV of PSR J1833-1034 Calculations by Benson Guest, Phd Student at U Manitoba

Hoffman_Colibri_CSA_townhall_10-31 http://www.colibri-telescope.ca 20 131 Planning for the Future

Sarah Gallagher Denis Laurin Mireille Bedirian Jean Dupuis Graeham Ko Yoan St-Onge Isabelle Therrien

Gallagher_CASCA_LRPTownhall_final 132 Canada in Space – Past and Potential Astronomy Missions

SuperBIT 2019 NEOSSAT 2013 HiClBaS BRITE 2015 2013 BIT 2012 ODIN FUSE 2001 SPIDER 1999 2011 Herschel 2009 EBEX 2009 Planck BLAST 2009 2003 CADC AstroSat 1986 2015 MOST 2003

Hitomi SPICA 2016 2032 CASTOR Euclid TBD LiteBird 2022 2027 XRISM JWST 2022 2021 Gallagher_CASCA_LRPTownhall_final 133 2 CSA Spending on Space Astronomy 1999-2019

45 $322M over 20 years 40 JWST

) Other Missions s r

a 30 l l o d JWST

n 25 Co-Investigators and Space Science o

i $183M l

l Enhancement Program i m

( 20 Preparatory Activities t s

o 15 • Space Technology Development

C Program (STDP) 10 • Flights for the Advancement of Science & Technology (FAST) 5 Other Missions • Science Maturation Studies $115M 0 $22M

Gallagher_CASCA_LRPTownhall_final 134 Gallagher 3 CSA Spending on Space Astronomy 1999-2019 excluding JWST

10 Other Missions ) s r

a 8 l

l $7M average Co-Investigators and Space Science o d

Enhancement Program n o i l l

i 6 m ( Preparatory Activities

s Other Missions • Space Technology Development o 4 Program (STDP)

C $115M • Flights for the Advancement of Science & Technology (FAST) 2 • Science Maturation Studies $22M

Gallagher_CASCA_LRPTownhall_final 135 Gallagher 4 City, Province HQP Canadian Astronomy: People Toronto, Ontario 218 Montréal, Québec 200 current faculty, university and industry staff, Outside Canada 164 postdocs, & graduate students Victoria, B.C. 153 Waterloo, Ontario 97 Hamilton, Ontario 92 London, Ontario 61 Edmonton, Alberta 55 Other (Canada) 54 1,400+ Canadian HQP Worldwide Québec, Québec 44 Vancouver, B.C. 42 Halifax, Nova Scotia 39 Kingston, Ontario 37 251 Winnipeg, Manitoba 25 11 3 Calgary, Alberta 25 108 Lethbridge, Alberta 11 28 14 Sherbrooke, Québec 10 513 268 Ottawa, Ontario 9 43 Regina, Saskatchewan 5

Gallagher_CASCA_LRPTownhall_final Outside Canada 55 136 5 Science Roadmaps: Astronomy a new approach

Implementation Plan

1. Develop a template document 2. Tap into the LRP2020 process 3. Iterate with the community 4. Publish and move onto the next science domain

Gallagher_CASCA_LRPTownhall_final 137 Gallagher 6 Who and what is it for? CSA Executive • to communicate with other parts of government and academia − other government departments, ministries, provincial partners − academic leadership • to integrate science & tech investments • to balance science and the mission portfolio CSA Internal • to inform staff − including Policy, Communications Academic Community • to articulate space science landscape − within and between science communities • to connect science & tech development • to communicate with decision-makers − Deans, Vice Presidents Research, granting agencies Gallagher_CASCA_LRPTownhall_final 138 Gallagher 7 What are our goals?

1. Balance in the science mission engagement portfolio in terms of scope and type of activity, scale of mission, and science drivers (between and within communities) 2. Maintenance and development of a robust space science ecosystem 3. Integration of science priorities with technology development 4. Coordinated and proactive interactions with international partners 5. Increased profile of space science activities

Gallagher_CASCA_LRPTownhall_final 139 Gallagher 8 Space Science Vision 2020

Table of Contents

Chapter 1 The Big Questions Chapter 2 Sustaining the Ecosystem Chapter 3 Realizing the Vision: Notional Missions and Technologies

Gallagher_CASCA_LRPTownhall_final 140 Gallagher 9 Chapter 1: The Big Questions

Key science drivers for the community product of Long Range Plan 2020 Are we alone? LRP 2020 How does it all work? Where did it all come from? 2010 2016 2020

Gallagher_CASCA_LRPTownhall_final 141 Gallagher 10 Chapter 2: Sustaining the Ecosystem Guiding Principles

1 Pursue Science-Driven Investments Capacity • Compelling questions to be identified by the science community Development 2 Foster Robust Institutional Networks Science- • CSA as a hub 5 1 Driven • Ties among all partners across the entire ecosystem Transparent Investments 3 Leverage International Partnerships Processes • Initiate connections • Focus on areas of scientific and industrial strength 4 2 4 Implement Transparent Processes Robust • From initial investigations to mission selection International 3 Institutional Partnerships Networks 5 Support Capacity Development • Across all career stages • Infrastructure

Gallagher_CASCA_LRPTownhall_final 142 Gallagher 11 Chapter 3: Realizing the Vision Modes of science mission engagement

Science Data Utilization 01 Analyzing space data to advance science t n Science Working Group Activities e

m Building science cases to determine instrument and operational t s design specifications, to attract partners, and to sell the project

e 02 v n i \ Ground Infrastructure A

S Using ground observatories, ground stations, and data management C 03 centres to support space data acquisition, delivery, and utilization g n i s

a Preparatory Activities e r Developing technology demonstrations on a variety of platforms c 04 n (ground-based, suborbital, and small satellites) I Contribution to International Missions 05 Leveraging partnerships with a focus on Canadian expertise (hardware, software, and science) Canadian-Led Space Missions Gallagher_CASCA_LRPTownhall_final Taking the lead and seeking partnerships 143 06 12 Chapter 3: Mapping Missions to Science Questions

How is the universe JWST expanding? What is the 2021 SPICA nature of dark matter and 2032 dark energy? CASTOR Euclid TBD 2022 When did the first stars turn on? How have galaxies assembled and evolved? What causes cosmic expansion? LiteBird 2027

Gallagher_CASCA_LRPTownhall_final 144 13 Chapter 3: Mapping Missions to Science Questions

What happens under extreme JWST conditions of density and 2021 SPICA CASTOR 2032 temperature? TBD

What can we learn from the E-M signatures of gravitational waves? XRISM 2022 What happens near black holes? LiteBird How are heavy elements created? 2027 Colibrì Athena 2031

Gallagher_CASCA_LRPTownhall_final 145 14 Chapter 3: Mapping Missions to Science Questions

How do planetary systems JWST SPICA form and evolve? 2021 2032

How do stars and their planets form? Microsat Concepts How do planetary system evolve? (POEP, EPPE) Are there habitable Earth-like planets? CASTOR How can we detect signs of life? TBD

Gallagher_CASCA_LRPTownhall_final 146 15 Chapter 3: Mapping Technology Development to Missions

• Optics • Focal plane I

T • FGS • Calibration R S

• NIRISS M • Coatings • CAMS O

• Focal plane T • Fine steering O W • Optics S J • Readout electronics T • Structures I

• Laser A • Optics • AI&T H

• Metrology C • AI&T • Fine guidance • Calibration • Testing • Software • Calibration • Bus • Software • Communication • Etc. • Ground segment • Software • Etc.

Gallagher_CASCA_LRPTownhall_final 147 Gallagher 16 For Discussion • Feedback on plans for − Space Science Vision 2020: suggestions for development and implementation − How can we* strengthen linkages between institutional partners within Canada (government, industry and academia)? − How can we* encourage broader engagement with available resources (preparatory CSA activities including STDP and FAST programs), CFI, other? *CSA + astronomy community

Offline contributions welcome. [email protected]

Gallagher_CASCA_LRPTownhall_final 148 Gallagher @scgQuasar 17