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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. 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  • The Denver Observer May 2016

    The Denver Observer May 2016

    The Denver MAY 2016 OBSERVER A section of a recent Hubble image of the Antennae Galaxies, NGCs 4038 and 4039, reveals intense star formation resulting from the galaxies’ colliding gases. Pink star-forming nebulae and blue (hot), new stars are clearly visible. Image Credit: ESA/Hubble & NASA MAY SKIES by Zachary Singer The Solar System ing 18.6” across from a distance of 0.50 AU. Interestingly, at opposi- Quite frequently in these pages, you’ll see that such-and-so planet tion, Mars will be roughly the same distance from us as Mercury at the is “lost in the solar glare,” and this month, Mercury embraces the spirit transit—so their relative disk sizes, 12 arcseconds vs. 18, quickly give of that phrase with gusto: The planet transits the Sun on the morning you a feel for each planet’s physical size. of May 9th. Already crossing the Sun’s face as it rises just before 6 AM, As May gives way to June, Mars will shrink in the eyepiece, return- the planet will finish its transit around 12:40 PM, as seen from Denver. ing to a 16” disk by early July. Even at the smaller diameter, the planet The planet’s apparent diameter will be 12.1 seconds of arc, making it should present some quite obvious even at moderate power—even small telescopes (with so- of its larger features, Sky Calendar lar filters, naturally) should show it clearly. While the DAS won’t have like ice caps or large 6 New Moon an official presence there, DU will open the Chamberlin Observatory plains like Syrtis Ma- 9 Mercury Transit from 9 AM to 12 noon.