HIFI: Submm Workshop, 15 Aug, HIFI Heterodyne Instrument for the Far Infrared (The high resolution spectrometer for Herschel) Michel Fich

HIFI: Submm Workshop, 15 Aug, Outline HIFI science goals –Water! –Key Projects instrument characteristics –the Canadian instrument contribution: the LSU –how to use HIFI – observing modes, integration times proposing for HIFI time support for Canadian astronomers –the Canadian HIFI team –tools

HIFI: Submm Workshop, 15 Aug, 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: Submm Workshop, 15 Aug, HIFI Core Science Solar System: Water in Giant Planets Chemistry Martian atmosphere ISM in Galaxies: Normal galaxies Physical properties of star-forming ISM Dense cores and star-formation: Dynamics Role of Water Disks ISM in the Milky Way: Structure Dynamics (pressure) Composition (gradients) Late stages of stellar evolution: Winds Shells Asymmetries Composition

HIFI: Submm Workshop, 15 Aug, Science with HIFI – Water

HIFI: Submm Workshop, 15 Aug, Science with HIFI – Water SWAS result

HIFI: Submm Workshop, 15 Aug, Example – WATER in intermediate mass star forming region define intermediate mass as 100 – 1000 L sun spherical core, –1.5 power-law assumed water abundance H 2 –all frozen out at T < 20 K Monte Carlo solution to radiative transfer (RATRAN) –run until “lowest” 7 lines in HIFI bands converged with S/N=5 convolve to HIFI beam appropriate for line frequency –at centre of core sample spectra shown for 1000 L sun (left) and 100 L sun (right), 100 M sun (top) and 10 M sun (bottom)

HIFI: Submm Workshop, 15 Aug, GHz ortho (2-1) 61K

HIFI: Submm Workshop, 15 Aug, GHz ortho (3-1) 114K

HIFI: Submm Workshop, 15 Aug, GHz ortho (4-3) 194K

HIFI: Submm Workshop, 15 Aug, GHz ortho (7-6) 305K

HIFI: Submm Workshop, 15 Aug, Molecular Lines visible with HIFI H2OH2O20 lines O2O2 15 lines HDO40 lines H 2 18 O24 lines CO13 lines OH 6 lines OH + 4 lines Plus lines of HD, HD +, H 2 D, 6 LiH, 7 LiH, CH, CH +, NH, NH +, NeH +, HF, SH, SH +, HCl, FeH, SiH, SiH +, CH 2, NH 2, NH 3, … plus many lines from larger molecules

HIFI: Submm Workshop, 15 Aug, Science with HIFI – [CII] in distant galaxies

HIFI: Submm Workshop, 15 Aug, 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: Submm Workshop, 15 Aug, HIFI Instrument Characteristics HIFI Implementation: Heterodyne spectroscopy –single pixel on the sky –very high spectral resolution 7 dual-pol mixer bands – GHz (  m) 5x2 SIS mixers, IF 4-8 GHz – GHz(  m; 2x2 HEB mixers, IF GHz 14 LO sub-bands –LO source unit in common –LO multiplier chains 2 spectrometer systems; –for each polarisation - auto-correlator spectrometer - acousto-optical spectrometer HIFI designed for: - Spectral Scans and Spectral line surveys - Very high spectral resolution - Widest possible coverage in the unexplored FIR/Submm range 1.Frequency coverage: 480 – 1250 GHz ( m) 1410 – 1910 GHz ( m) 2. Sensitivity Near-quantum noise limit sensitivity IF bandwidth/Resolution: - 4 GHz (in 2 polarisations) – 280 kHz –0.5 and 1 MHz 3. Calibration Accuracy: 10% baseline; 3% goal

HIFI: Submm Workshop, 15 Aug, HIFI Design block diagram

HIFI: Submm Workshop, 15 Aug, HIFI Local Oscillator Source Unit (LSU) Flight Model assembled, undergoing tests. Due to be shipped to SRON first week of Sept the LSU dimensions are 265(H) x 424(L) x 286(W) mm. The Canadian Hardware Contribution to HIFI

HIFI: Submm Workshop, 15 Aug, Latest update LO chain performance: Bands 1-4 by RPG; Bands 5, 6L, 6H by JPL

HIFI: Submm Workshop, 15 Aug, HIFI Flight Mixer Performance at Unit level (open symbols) and after integration in the FPU

HIFI: Submm Workshop, 15 Aug, Band-3 SIS Noise Temperature as function of IF Band-6 HEB Noise Temperature as function of IF IN HIFI: ONE FREQUENCY Band is working at a time with 2 mixers; In orthogonal polarisation, also for redundancy. One LO band, with 2 sub-bands, match the corresponding mixer band

HIFI: Submm Workshop, 15 Aug, WBO FM with 1.1 MHz resolution and 4GHz bandwidth

HIFI: Submm Workshop, 15 Aug, HIFI-HRS (auto-correlator) FM Capabilities 2 HRS FM modules

HIFI: Submm Workshop, 15 Aug, HIFI Observing Modes Dual Beam Switch with internal copper and telescope nod Position Switch efficiency depending on off-position slew Frequency Switch with switching LSU Optimum AOT depends on stability of Telescope-Instrument System

HIFI: Submm Workshop, 15 Aug, HIFI Band Sensitivities Band Frequency Range (GHz) Tsys (K) Flux Limit (5 , 1hr, R=10 4 ) (Jy) Flux Limit (5 , 1hr, R=10 4 ) (mK) Line Flux limit (5 ,1hr, 10 4 ) ( Wm -2 ) Beamwidth (arcsec) Spectral Resolution (MHz) 0.14 – 0.28 – 1.00

HIFI: Submm Workshop, 15 Aug, Estimating integration times Time estimate recipe available on web at overheads not well known until after launch –slew times: large distances, scanning, small distances (beam- switching) –pointing/focus/calibration times –re-tuning times: within band and changing bands –data downloads and command uploads

HIFI: Submm Workshop, 15 Aug, Updated Herschel Observing Proposal AO Timeline AO KP (GT and OT) issue 1/02/2007 KP GT proposal deadline 5/04/2007 KP GT result official 5/07/2007 KP OT proposal deadline 1/11/2007 KP OT result official 28/02/2008 AO ‘regular’ GT cycle 1 issue 28/02/2008 AO ‘regular’ GT cycle 1 proposal deadline3/04/2008 GT result official 5/06/2008 AO OT issue 1/02/2009? AO = Announcement of OpportunityKP = Key Project GT = Guaranteed TimeOT = Open Time

HIFI: Submm Workshop, 15 Aug, Support for Canadian Astronomers 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 Canadian HIFI staff members of HIFI Instrument Control Centre (ICC) –Science support specialist (University of Waterloo): job available! –Instrument support specialist (SRON): Kevin Edwards

HIFI: Submm Workshop, 15 Aug, Tools for HIFI Observing tool is HSPOT (Herschel adaptation of Spitzer SPOT tool) Analysis tool is HICLASS (HIFI adaptation of CLASS) Tools based on Linux and Windows platforms but Canadian contribution is Mac OSX version – not fully functional because database not available for Macs may need to learn some Jython (Java/Python implementation) to write observing scripts, etc.

HIFI: Submm Workshop, 15 Aug, Canadian HIFI strategy is to maximize success rate on Open Time (OT) Proposals 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 mid-2009 observing assistance, data analysis advice and software support will be available