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!!! - science - the mission HIFI
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 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 km/s and km/s coverage or imaging with two 25x16 arrays at and μm simultaneously
HIFI: very high spectral resolution heterodyne spectroscopy spanning and 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 (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
H2O
20 lines O2
15 lines
HDO
40 lines
H218O
24 lines CO
13 lines OH
6 lines
OH+
4 lines
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. Herschel Meeting: 12:00 – 13:30 Friday, Esqumalt Room
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
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!
Meeting Thursday after the CASCA Business Meeting
HIFI: CASCA08, 23 May, 2008

15. The Far-IR Spatial Resolution Gap
~ arcsecs with few K sensitivity
~ 10 arcsec with micro-K sensitivity
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