1. HIFI: CASCA07 – lunch meeting 6 June, 2007 1 Herschel Lunch Meeting Agenda 1.HIFI overview (10 min) - Mike Fich instrument status, testing (5 min) Doug Johnstone key projects and other science (10 min.) Doug and perhaps other members of Science Team? user software and support(10 min.) Carolyn McCoey 2.SPIRE (30 min.) - David Naylor

2. HIFI: CASCA07 – lunch meeting 6 June, 2007 2 Canadian Participation in HIFI provide instrument subsystem –Local Oscillator Source Unit provide two people for Instrument Control Centre (ICC) –software development and support –one person (Kevin Edwards) located at ICC (Groningen) and one at U.Waterloo (Carolyn McCoey) four members of international Science Team significant involvement in at least one Key Project (1000-2000 hours observing time) Guaranteed Time in proportion to our investment one person on the international HIFI Steering Committee

3. HIFI: CASCA07 – lunch meeting 6 June, 2007 3 Top Level Requirements and Resulting Concept HIFI Implementation: Heterodyne spectroscopy –single pixel on the sky –very high spectral resolution 7 dual-pol mixer bands –480-1250 GHz (625-240  m) 5x2 SIS mixers, IF 4-8 GHz –1410-1910 GHz(212-157  m; 2x2 HEB mixers, IF 2.4-4.8 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 (625-240 m) 1410 – 1910 GHz (212-157 m) 2. Sensitivity Near-quantum noise limit sensitivity IF bandwidth/Resolution: - 4 GHz (in 2 polarisations) - 140 – 280 kHz –0.5 and 1 MHz 3. Calibration Accuracy: 10% baseline; 3% goal

4. HIFI: CASCA07 – lunch meeting 6 June, 2007 4 HIFI Band Sensitivities Band 123456 & 7 Frequency Range (GHz) 480-640640- 800 800- 960 960- 1120 1120- 1250 1410- 1910 Tsys (K) 16032048073020002500 Flux Limit (5 , 1hr, R=10 4 ) (Jy) 2.34.05.58.02022 Flux Limit (5 , 1hr, R=10 4 ) (mK) 5912174345 Line Flux limit (5 ,1hr, 10 4 ) (10 - 18 Wm -2 ) 1.33582434 Beamwidth (arcsec) 393025211913 Spectral Resolution (MHz) 0.14 – 0.28 – 1.00 testing currently underway - values may change

5. HIFI: CASCA07 – lunch meeting 6 June, 2007 5 HIFI-HRS (auto-correlator) FM Capabilities 2 HRS FM modules

6. HIFI: CASCA07 – lunch meeting 6 June, 2007 6 WBO (AOS) FM (one Polarisation) with 1.1 MHz resolution and 4GHz bandwidth

7. HIFI: CASCA07 – lunch meeting 6 June, 2007 7 HIFI Key Programs with possible Open time Key projects (*) OVERVIEW: (with coordinator’s name) 1. Water and Chemistry Studies in the Solar System (P. Hartogh and E. Lellouch) 2. The Star Formation Program 1.1 WATER (E. van Dishoeck) 1.2 Spectral Scans (C. Ceccarelli) 1.3 The Orion and Sgr B2 regions (T. Bergin) (1.4 Maps of the ORION region (J. Cernicharo))* (1.5 Molecular Oxygen (P. Goldsmith))* 3. ISM 2.1 The Warm ISM (V. Ossenkopf) 2.2 Hydrides and Molecular Carriers ( M. Gerin) 4. Late stages of Stellar Evolution (V. Bujarrabal) 3.1 WATER and CO observations of AGB envelopes, PPNe and PNe (3.2 HIFI frequency surveys of AGB, PPNe and PNe; coord. Pardo)* 5. Extragalactic Science (R. Guesten) 4.1 Physical and Chemical Conditions of the ISM in Galactic Nuclei 4.2 The Physics of the ISM in Low-Metallicity Environments*

8. HIFI: CASCA07 – lunch meeting 6 June, 2007 8 Updated Herschel Observing Proposal AO Timeline AO KP (GT and OT) issue 1 February 2007 KP GT proposal deadline 4 April 2007 KP GT result official 5 July 2007 KP OT proposal deadline 25 October 2007 KP OT result official 28 February 2008 AO ‘regular’ GT cycle 1 issue 28 February 2008 AO ‘regular’ GT cycle 1 deadline3 April 2008 GT result official 5 June 2008 Launch31 July 2008 OT cycle 1 issue1 February 2009 (?) OT cycle 1 deadline1 May 2009 (?) OT cycle 1 observing1 Aug 2009 (?)

9. HIFI: CASCA07 – lunch meeting 6 June, 2007 9 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 Other Canadians currently active in HIFI: Kevin Edwards (U.Waterloo/ICC), Carolyn McCoey (U.Waterloo), Martin Houde (U.Western Ontario), Li-Hong Xu (U.New Brunswick)

10. HIFI: CASCA07 – lunch meeting 6 June, 2007 10 Canadian HIFI strategy is to maximize success rate on Open Time Proposals Canadian staff and Science Team members available as a resource to all Canadian astronomers to help with – proposals preparation – observing assistance – data analysis advice – software support Canadian HIFI Workshop for potential users in 2007(?) http://astro.uwaterloo.ca/HIFI email: hifi@astro.uwaterloo.cahifi@astro.uwaterloo.ca

11. HIFI: CASCA07 – lunch meeting 6 June, 2007 11 Intermediate Mass Protostars (30 hrs) Doug Johnstone -> co-ordintator, prep. work, planning Mike Fich -> water line modeling Rene Plume -> chemistry, prep. work Asuncion Fuente-> prep. work, planning Ewine van Dishoeck -> prep. work, obs. planning Paola Caselli -> prep. work, obs planning others?

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15. HIFI: CASCA07 – lunch meeting 6 June, 2007 15

16. HIFI: CASCA07 – lunch meeting 6 June, 2007 16 Polarisation studies with Herschel/HIFI Each of the 7 bands have a pair of orthogonally linear polarised mixers (SIS or HEB) Three Stokes parameters (I,Q,U) can be evaluated with two (or three) measurements –Successive measurements can only be performed weeks apart –Different analysis techniques than commonly used

17. HIFI: CASCA07 – lunch meeting 6 June, 2007 17 Polarisation component orientations for each channel Courtesy W. Jellema

18. HIFI: CASCA07 – lunch meeting 6 June, 2007 18 Polarisation studies with Herschel/HIFI Team lead by M. Harwit (mission scientist), including M. Houde, W. Jellema, G. Melnick, K. Menten, and D. Neufeld Initial program will concentrate on masers –Potential for high linear polarisation levels –Many spectral lines (i.e., water) predicted If successful, expand to other types of observing programs Recruiting graduate student  talk to me! Martin Houde (houde@astro.uwo.ca)