DOCSLIB.ORG

LRP2020 Nov2019 CSA Town

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
LRP2020 Nov2019 CSA Town 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
Load more

Recommended publications
  • Where Are the Distant Worlds? Star Maps
    W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star.
    [Show full text]
  • JUICE Red Book
    ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat.
    [Show full text]
  • College of San Mateo Observatory Stellar Spectra Catalog ______
    College of San Mateo Observatory Stellar Spectra Catalog SGS Spectrograph Spectra taken from CSM observatory using SBIG Self Guiding Spectrograph (SGS) ___________________________________________________ A work in progress compiled by faculty, staff, and students. Stellar Spectroscopy Stars are divided into different spectral types, which result from varying atomic-level activity on the star, due to its surface temperature. In spectroscopy, we measure this activity via a spectrograph/CCD combination, attached to a moderately sized telescope. The resultant data are converted to graphical format for further analysis. The main spectral types are characterized by the letters O,B,A,F,G,K, & M. Stars of O type are the hottest, as well as the rarest. Stars of M type are the coolest, and by far, the most abundant. Each spectral type is also divided into ten subtypes, ranging from 0 to 9, further delineating temperature differences. Type Temperature Color O 30,000 - 60,000 K Blue B 10,000 - 30,000 K Blue-white A 7,500 - 10,000 K White F 6,000 - 7,500 K Yellow-white G 5,000 - 6,000 K Yellow K 3,500 - 5,000 K Yellow-orange M >3,500 K Red Class Spectral Lines O -Weak neutral and ionized Helium, weak Hydrogen, a relatively smooth continuum with very few absorption lines B -Weak neutral Helium, stronger Hydrogen, an otherwise relatively smooth continuum A -No Helium, very strong Hydrogen, weak CaII, the continuum is less smooth because of weak ionized metal lines F -Strong Hydrogen, strong CaII, weak NaI, G-band, the continuum is rougher because of many ionized metal lines G -Weaker Hydrogen, strong CaII, stronger NaI, many ionized and neutral metals, G-band is present K -Very weak Hydrogen, strong CaII, strong NaI and many metals G- band is present M -Strong TiO molecular bands, strongest NaI, weak CaII very weak Hydrogen absorption.
    [Show full text]
  • The Odin Orbital Observatory
    A&A 402, L21–L25 (2003) Astronomy DOI: 10.1051/0004-6361:20030334 & c ESO 2003 Astrophysics The Odin orbital observatory H. L. Nordh1,F.vonSch´eele2, U. Frisk2, K. Ahola3,R.S.Booth4,P.J.Encrenaz5, Å. Hjalmarson4, D. Kendall6, E. Kyr¨ol¨a7,S.Kwok8, A. Lecacheux5, G. Leppelmeier7, E. J. Llewellyn9, K. Mattila10,G.M´egie11, D. Murtagh12, M. Rougeron13, and G. Witt14 1 Swedish National Space Board, Box 4006, 171 04 Solna, Sweden Letter to the Editor 2 Swedish Space Corporation, PO Box 4207, 171 04 Solna, Sweden 3 National Technology Agency of Finland (TEKES), Kyllikkiporten 2, PB 69, 00101 Helsinki, Finland 4 Onsala Space Observatory, Chalmers University of Technology, 439 92, Onsala, Sweden 5 Observatoire de Paris, 61 Av. de l’Observatoire, 75014 Paris, France 6 Canadian Space Agency, PO Box 7275, Ottawa, Ontario K1L 8E3, Canada 7 Finnish Meteorological Institute, PO Box 503, 00101 Helsinki, Finland 8 Department of Physics and Astronomy, University of Calgary, Calgary, ABT 2N 1N4, Canada 9 Department of Physics and Engineering Physics, 116 Science Place, University of Saskatchewan, Saskatoon, SK S7N 5E2, Canada 10 Observatory, PO Box 14, University of Helsinki, 00014 Helsinki, Finland 11 Institut Pierre Simon Laplace, CNRS-Universit´e Paris 6, 4 place Jussieu, 75252 Paris Cedex 05, France 12 Global Environmental Measurements Group, Department of Radio and Space Science, Chalmers, 412 96 G¨oteborg, Sweden 13 Centre National d’Etudes´ Spatiales, Centre Spatial de Toulouse, 18 avenue Edouard´ Belin, 31401 Toulouse Cedex 4, France 14 Department of Meteorology, Stockholm University, 106 91 Stockholm, Sweden Received 6 December 2002 / Accepted 17 February 2003 Abstract.
    [Show full text]
  • Virgo the Virgin
    Virgo the Virgin Virgo is one of the constellations of the zodiac, the group tion Virgo itself. There is also the connection here with of 12 constellations that lies on the ecliptic plane defined “The Scales of Justice” and the sign Libra which lies next by the planets orbital orientation around the Sun. Virgo is to Virgo in the Zodiac. The study of astronomy had a one of the original 48 constellations charted by Ptolemy. practical “time keeping” aspect in the cultures of ancient It is the largest constellation of the Zodiac and the sec- history and as the stars of Virgo appeared before sunrise ond - largest constellation after Hydra. Virgo is bordered by late in the northern summer, many cultures linked this the constellations of Bootes, Coma Berenices, Leo, Crater, asterism with crops, harvest and fecundity. Corvus, Hydra, Libra and Serpens Caput. The constella- tion of Virgo is highly populated with galaxies and there Virgo is usually depicted with angel - like wings, with an are several galaxy clusters located within its boundaries, ear of wheat in her left hand, marked by the bright star each of which is home to hundreds or even thousands of Spica, which is Latin for “ear of grain”, and a tall blade of galaxies. The accepted abbreviation when enumerating grass, or a palm frond, in her right hand. Spica will be objects within the constellation is Vir, the genitive form is important for us in navigating Virgo in the modern night Virginis and meteor showers that appear to originate from sky. Spica was most likely the star that helped the Greek Virgo are called Virginids.
    [Show full text]
  • The Observer's Handbook for 1953
    THE OBSERVER’S HANDBOOK FOR 1953 PUBLISHED BY The Royal Astronomical Society of Canada C. A. CHANT, E ditor RUTH J. NORTHCOTT, A s s is t a n t E ditor DAVID DUNLAP OBSERVATORY FORTY-FIFTH YEAR OF PUBLICATION P rice 50 C en ts TORONTO 3 Willcocks Street Printed for the Society By the University of Toronto Press THE ROYAL ASTRONOMICAL SOCIETY OF CANADA The Society was incorporated in 1890 as The Astronomical and Physical Society of Toronto, assuming its present name in 1903. For many years the Toronto organization existed alone, but now the Society is national in extent, having active Centres in Montreal and Quebec, P.Q.; Ottawa, Toronto, Hamilton, London, and Windsor, Ontario; Winnipeg, Man.; Saskatoon, Sask.; Edmonton, Alta.; Vancouver and Victoria, B.C. As well as nearly 1000 members of these Canadian Centres, there are nearly 400 members not attached to any Centre, mostly resident in other nations, while some 200 additional institutions or persons are on the regular mailing list of our publications. The Society publishes a bi-monthly J o u r n a l and a yearly O b serv er's H a n d bo o k . Single copies of the J o u r n a l are 50 cents, and of the H a n d bo o k , 50 cents. Membership is open to anyone interested in astronomy. Annual dues, $3.00; life membership, $40.00. Publications are sent free to all members or may be subscribed for separately. Applications for membership or publications may be made to the National Secretary, 3 Willcocks St., Toronto.
    [Show full text]
  • Messenger-No117.Pdf
    ESO WELCOMES FINLANDINLAND AS ELEVENTH MEMBER STAATE CATHERINE CESARSKY, ESO DIRECTOR GENERAL n early July, Finland joined ESO as Education and Science, and exchanged which started in June 2002, and were con- the eleventh member state, following preliminary information. I was then invit- ducted satisfactorily through 2003, mak- II the completion of the formal acces- ed to Helsinki and, with Massimo ing possible a visit to Garching on 9 sion procedure. Before this event, howev- Tarenghi, we presented ESO and its scien- February 2004 by the Finnish Minister of er, Finland and ESO had been in contact tific and technological programmes and Education and Science, Ms. Tuula for a long time. Under an agreement with had a meeting with Finnish authorities, Haatainen, to sign the membership agree- Sweden, Finnish astronomers had for setting up the process towards formal ment together with myself. quite a while enjoyed access to the SEST membership. In March 2000, an interna- Before that, in early November 2003, at La Silla. Finland had also been a very tional evaluation panel, established by the ESO participated in the Helsinki Space active participant in ESO’s educational Academy of Finland, recommended Exhibition at the Kaapelitehdas Cultural activities since they began in 1993. It Finland to join ESO “anticipating further Centre with approx. 24,000 visitors. became clear, that science and technology, increase in the world-standing of ESO warmly welcomes the new mem- as well as education, were priority areas Astronomy in Finland”. In February 2002, ber country and its scientific community for the Finnish government. we were invited to hold an information that is renowned for its expertise in many Meanwhile, the optical astronomers in seminar on ESO in Helsinki as a prelude frontline areas.
    [Show full text]
  • Long-Term Monitoring of Jupiter's Stratospheric H2O Abundance with the Odin Space Telescope
    EPSC Abstracts Vol. 13, EPSC-DPS2019-484-2, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Long-term monitoring of Jupiter's stratospheric H2O abundance with the Odin Space Telescope T. Cavalié1,2, B. Benmahi1, N. Biver2, M. Dobrijevic1, K. Bermudez-Diaz3, E. Lellouch2, P. Hartogh4, Aa. Sandqvist5, A. Lecacheux2, Å. Hjalmarson6, U. Frisk7, M. Olberg8, and The Odin Team. (1) LAB – CNRS – Univ. Bordeaux, Pessac, France ([email protected]), (2) LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, France (3) Université Paris Diderot, France, (4) Max Planck Institute for Solar System Research, Göttingen, Germany, (5) Stockholm Observatory, Sweden, (6) Onsala Space Observatory, Sweden, (7) Omnisys Instruments, Gothenburg, Sweden, (8) Chalmers University, Gothenburg, Sweden. Abstract References Water vapor and CO2 have been detected in the Burgdorf et al. 2006. Icarus 184, 634–637. stratospheres of the giant planets and Titan Cavalié et al. 2013. Astron. Astrophys. 553, A21. (Feuchtgruber et al. 1997, Coustenis et al. 1998, Coustenis et al. 1998. Astron. Astrophys. 336, L85– Burgdorf et al. 2006). The presence of the atmospheric L89. cold trap implies an external origin for H2O, and the Feuchtgruber et al. 1997. Nature 389, 159–162. possible sources are: interplanetary dust particles Lellouch et al. 1995. Nature 373, 592–595. (IDP), icy rings and/or satellites, and large comet Nordh et al. 2003. Astron. Astrophys. 402, L21-L25. impacts. In July 1994, the Shoemaker-Levy 9 comet (SL9) spectacularly impacted Jupiter near 44°S. On the long term, Jupiter was left with a variety of new species in its stratosphere, including CO, HCN, CS, etc (Lellouch et al.
    [Show full text]
  • Exoplanetary Atmospheres: from Hot Jupiters to Habitable Planets
    Observing Planetary Systems II – Santiago, Chile, March 5-8, 2012 Exoplanetary atmospheres: from hot Jupiters to habitable planets! Michaël Gillon [email protected] Overview! " From solar to extrasolar planetary atmospheres ! " Phase curves of non-transiting planets! " Transiting planets ! !Transit transmission spectrophotometry ! !Occultation emission spectrophotometry ! !Phase curves ! !2D emission maps! " Direct spectroscopy of extrasolar planets ! " Conclusions ! Before extrasolar planets:# solar planets atmosphere observations! XIXth century: imagery and photometry establish the existence of an atmosphere for several planets! !* Occultation of stars are gradual! !* Variable features incompatible with surface origin! From 1920s: spectroscopic studies of planets, e.g.! !* No O2 in Venus$ atmosphere (Webster 1927)! !* CH4 in the atmosphere of giant planets (Adel & Slipher, 1934) !* CO2 in the atmosphere of terrestrial planets (Adel 1937) !* Detection of the atmosphere of Titan (Kuiper 1944)! Second half of XXth century to now: in situ measurements with probes (orbiters & landers)! Accurate thermal profiles & composition (e.g. Seiff et al. 1998) The planetary atmospheres zoo: theoretical expectations! Seager & Deming (2010) " Primordial atmospheres captured from the protostellar nebula and dominated by H and He in cosmic proportions (giant planets)! " Outgassed atmospheres rich in H (up to 50%) around planets in the 10 to 30 Earth masses range, massive enough to retain H. No He.! " Outgassed atmospheres dominated by CO2 (Venus,
    [Show full text]
  • The Two-Colour EMCCD Instrument for the Danish 1.54 M Telescope and SONG?
    A&A 574, A54 (2015) Astronomy DOI: 10.1051/0004-6361/201425260 & c ESO 2015 Astrophysics The two-colour EMCCD instrument for the Danish 1.54 m telescope and SONG? J. Skottfelt1;2, D. M. Bramich3, M. Hundertmark1, U. G. Jørgensen1;2, N. Michaelsen1, P. Kjærgaard1, J. Southworth4, A. N. Sørensen1, M. F. Andersen5, M. I. Andersen1, J. Christensen-Dalsgaard5, S. Frandsen5, F. Grundahl5, K. B. W. Harpsøe1;2, H. Kjeldsen5, and P. L. Pallé6;7 1 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark e-mail: [email protected] 2 Centre for Star and Planet Formation, Natural History Museum, University of Copenhagen, Østervoldgade 5–7, 1350 København K, Denmark 3 Qatar Environment and Energy Research Institute, Qatar Foundation, PO Box 5825, Doha, Qatar 4 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 5 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 6 Instituto de Astrofísica de Canarias (IAC), 38200 La Laguna, Tenerife, Spain 7 Dept. Astrofísica, Universidad de La Laguna (ULL), 38206 Tenerife, Spain Received 1 November 2014 / Accepted 27 November 2014 ABSTRACT We report on the implemented design of a two-colour instrument based on electron-multiplying CCD (EMCCD) detectors. This instrument is currently installed at the Danish 1.54 m telescope at ESO’s La Silla Observatory in Chile, and will be available at the SONG (Stellar Observations Network Group) 1m telescope node at Tenerife and at other SONG nodes as well. We present the software system for controlling the two-colour instrument and calibrating the high frame-rate imaging data delivered by the EMCCD cameras.
    [Show full text]
  • Herschel Space Observatory-An ESA Facility for Far-Infrared And
    Astronomy & Astrophysics manuscript no. 14759glp c ESO 2018 October 22, 2018 Letter to the Editor Herschel Space Observatory? An ESA facility for far-infrared and submillimetre astronomy G.L. Pilbratt1;??, J.R. Riedinger2;???, T. Passvogel3, G. Crone3, D. Doyle3, U. Gageur3, A.M. Heras1, C. Jewell3, L. Metcalfe4, S. Ott2, and M. Schmidt5 1 ESA Research and Scientific Support Department, ESTEC/SRE-SA, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands e-mail: [email protected] 2 ESA Science Operations Department, ESTEC/SRE-OA, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands 3 ESA Scientific Projects Department, ESTEC/SRE-P, Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands 4 ESA Science Operations Department, ESAC/SRE-OA, P.O. Box 78, E-28691 Villanueva de la Canada,˜ Madrid, Spain 5 ESA Mission Operations Department, ESOC/OPS-OAH, Robert-Bosch-Strasse 5, D-64293 Darmstadt, Germany Received 9 April 2010; accepted 10 May 2010 ABSTRACT Herschel was launched on 14 May 2009, and is now an operational ESA space observatory offering unprecedented observational capabilities in the far-infrared and submillimetre spectral range 55−671 µm. Herschel carries a 3.5 metre diameter passively cooled Cassegrain telescope, which is the largest of its kind and utilises a novel silicon carbide technology. The science payload comprises three instruments: two direct detection cameras/medium resolution spectrometers, PACS and SPIRE, and a very high-resolution heterodyne spectrometer, HIFI, whose focal plane units are housed inside a superfluid helium cryostat. Herschel is an observatory facility operated in partnership among ESA, the instrument consortia, and NASA. The mission lifetime is determined by the cryostat hold time.
    [Show full text]
  • 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.
    [Show full text]