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HIFI H eterodyne I nstrument for the F ar I nfrared

HIFI H eterodyne I nstrument for the F ar I nfrared (The high resolution spectrometer for Herschel). Michel Fich. Outline. Visit the HIFI booth!!!. Herschel - science - the mission HIFI the instrument science the Canadian HIFI team what comes after Herschel?.

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HIFI H eterodyne I nstrument for the F ar I nfrared

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  1. HIFI Heterodyne Instrument for the Far Infrared (The high resolution spectrometer for Herschel) Michel Fich HIFI: CASCA08, 23 May, 2008

  2. Outline Visit the HIFI booth!!! • Herschel - science - the mission • HIFI • the instrument • science • the Canadian HIFI team • what comes after Herschel? HIFI: CASCA08, 23 May, 2008

  3. 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

  4. 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 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

  5. 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

  6. HIFI Design block diagram HIFI: CASCA08, 23 May, 2008

  7. 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

  8. 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

  9. Molecular Lines visible with HIFI 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

  10. Science with HIFI – Water SWAS result HIFI: CASCA08, 23 May, 2008

  11. 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

  12. 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

  13. 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: hifi@astro.uwaterloo.ca • Herschel Meeting: 12:00 – 13:30 Friday, Esqumalt Room HIFI: CASCA08, 23 May, 2008

  14. 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

  15. ~ 10 arcsec with micro-K sensitivity ~ 0.005 arcsecs with few K sensitivity The Far-IR Spatial Resolution Gap JWST UofW Astro-lunch 29 Nov. 2006

  16. 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

  17. Direct Detection Far-IR Interferometry 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

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