* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download PPT - University of Waterloo
Survey
Document related concepts
Nebular hypothesis wikipedia , lookup
Aquarius (constellation) wikipedia , lookup
Formation and evolution of the Solar System wikipedia , lookup
Extraterrestrial life wikipedia , lookup
Advanced Composition Explorer wikipedia , lookup
Corvus (constellation) wikipedia , lookup
James Webb Space Telescope wikipedia , lookup
Astrophotography wikipedia , lookup
Spitzer Space Telescope wikipedia , lookup
International Ultraviolet Explorer wikipedia , lookup
Star formation wikipedia , lookup
Hubble Deep Field wikipedia , lookup
Timeline of astronomy wikipedia , lookup
Transcript
HIFI Heterodyne Instrument for the Far Infrared (The high resolution spectrometer for Herschel) Michel Fich HIFI: CASCA08, 23 May, 2008 1 Outline Herschel - science - the mission HIFI - the instrument - science - the Canadian HIFI team • what comes after Herschel? HIFI: CASCA08, 23 May, 2008 2 Herschel Main Scientific Objectives Formation and evolution of galaxies and clusters in the early universe Star formation rates, bolometric luminosities, AGN structure Evolution of chemical elements Formation of stars & planets and physics of the interstellar medium Tracers of structure, kinematics, chemistry in star forming regions Circulation/enrichment of the interstellar medium Astrochemistry – WATER Detailed studies of nearby resolvable galaxies Cometary, planetary, and satellite atmospheres History of the solar system Pristine material in comets Water activity HIFI: CASCA08, 23 May, 2008 3 Herschel: The Mission • facility-class far-infrared/submm space observatory – 1/3 Guaranteed Time, 2/3 Open Time with annual calls for proposals • 3.5 m Ritchey-Chrétien telescope that will passively cool to around 70K • have an operational lifetime of at least three years • incorporates an ISO-type liquid helium cryostat • launched by an Ariane 5 in late 2008 (with Planck) • operate from an orbit around the L2 point in the Sun/Earth system located approximately 1.5 million km away from the Earth in the anti-sunward direction HIFI: CASCA08, 23 May, 2008 late 4 Herschel: The Instruments • SPIRE: simultaneously imaging at 250, 350, 500 μm with 322, 242, and 162 pixels in same 4'x4' FOV or low to medium resolution spectroscopy in 2'x2' • PACS: spectroscopy with velocity resolution of 100-250 km/s and 1300-3000 km/s coverage or imaging with two 25x16 arrays at 80-130 and 130-210 μm simultaneously • HIFI: very high spectral resolution heterodyne spectroscopy spanning 480-1250 and 1410-1910 GHz with wide and narrow band spectrometers operating in parallel HIFI: CASCA08, 23 May, 2008 5 HIFI Design block diagram f rom telescope LOU FPU Housing Radiator 7 LO Assemblies with 7x2 LO chains and power amplifiers Common Optics Calibration source Chopper mechanism 7 M ixer Assemblies each with 2 mixers IF amplifiers LSU LCU Control Control M aster oscillator M ultiplier bias Synthesizer Power amplifier Ref. distribution bias FCU HRS-v HRS-h WBS-v WBS-h Control M ixer bias Amplifier bias M echanism control IF processor Sub-band division IF processor Sub-band division IF processor Sub-band division IF processor Sub-band division f~1GHz f variable f~1GHz f variable f 4 GHz f 1 M Hz f 4 GHz f 1 M Hz Instrument Control Unit spacecraf t OB DH HIFI: CASCA08, 23 May, 2008 6 HIFI Local Oscillator Source Unit (LSU) The Canadian Hardware Contribution to HIFI • • built by COMDEV performing extremely well in tests • the LSU dimensions are 265(H) x 424(L) x 286(W) mm. HIFI: CASCA08, 23 May, 2008 7 HIFI Core Science ISM in Galaxies: • Normal galaxies • Physical properties •of star-forming ISM ISM in the Milky Way: • Structure • Dynamics (pressure) • Composition (gradients) Dense cores and star-formation: • Dynamics • Role of Water • Disks Late stages of stellar evolution: • Winds • Shells • Asymmetries • Composition Solar System: • Water in Giant Planets • Chemistry Martian atmosphere HIFI: CASCA08, 23 May, 2008 8 Molecular Lines visible with HIFI H 2O 20 lines O2 15 lines HDO 40 lines H218O 24 lines CO 13 lines OH 6 lines OH+ 4 lines Plus lines of HD, HD+, H2D, 6LiH, 7LiH, CH, CH+, NH, NH+, NeH+, HF, SH, SH+, HCl, FeH, SiH, SiH+, CH2, NH2, NH3, … plus many lines from larger molecules HIFI: CASCA08, 23 May, 2008 9 Science with HIFI – Water SWAS result HIFI: CASCA08, 23 May, 2008 10 HIFI Key Projects (Guaranteed Time) • water in star forming regions – low mass: pre-stellar, Class 0, Class 1, outflows – intermediate mass: embedded (led by Doug Johnstone) – high mass: pre-stellar, hot cores, maps – disks – hydrides • Ori B maps and spectral surveys – Ori KL, Ori-South (led by Rene Plume), bar maps • warm ISM – PDRs, diffuse, shocks, low-UV, hydrides, C-clusters (Peter Martin on team) • Solar System – comets, mars, outer solar system • evolved stars • extragalactic – galactic centre, star bursts, ultra-luminous, AGNs, Cen A, metal-poor HIFI: CASCA08, 23 May, 2008 11 Canadian HIFI Steering Committee • • • • • • Michel Fich* (University of Waterloo) Canadian Lead Co-Investigator Doug Johnstone* (NRC/HIA) Peter Martin* (University of Toronto) Henry Matthews (NRC/HIA/DAO/DRAO) Bill McCutcheon (University of British Columbia) Rene Plume* (University of Calgary) * “Astronomy Co-Investigator” - member of the international HIFI Science Team HIFI: CASCA08, 23 May, 2008 12 Canadian HIFI strategy is to maximize success rate on Open Time Proposals •we expect a call for OT proposals due no sooner than May 2009 •Canadian staff and Science Team members available as a resource to all Canadian astronomers to help with proposals •Canadian HIFI Workshop for potential users in 2009 (perhaps with CASCA meeting) •observing assistance, data analysis advice and software support will be available http://astro.uwaterloo.ca/HIFI email: [email protected] Herschel Meeting: 12:00 – 13:30 Friday, Esqumalt Room HIFI: CASCA08, 23 May, 2008 13 What comes after Herschel? • cold telescopes (SPICA) • larger telescopes (10 meter diameter) • Interferometers Join the Far InfraRed Discipline Working Group (FIRDWG) to learn more! http://astro.uwaterloo.ca/~firdwg Meeting Thursday after the CASCA Business Meeting HIFI: CASCA08, 23 May, 2008 14 The Far-IR Spatial Resolution Gap ~ 10 arcsec with micro-K sensitivity ~ 0.005 arcsecs with few K sensitivity UofW Astro-lunch 29 Nov. 2006 15 Interferometers: Heterodyne vs. Direct Detection Heterodyne – detect the signals at each antenna and then combine electronically Direct Detection – combine beams, then detect signal • sensitivity • resolution • technology challenges (cost and schedule) UofW Astro-lunch 29 Nov. 2006 16 Dave Leisawitz NASA Based largely on the NASA-sponsored study of the Space Infrared Interferometric Telescope (SPIRIT), a candidate Origins Probe mission UofW Astro-lunch 29 Nov. 2006 17