The Herschel The Herschel - - Heterodyne Instrument for the Far Heterodyne Instrument for the Far - - Infrared Infrared (HIFI): (HIFI): Instrument and Pre Instrument and Pre - - launch Testing launch Testing . . Thijs de Graauw Thijs de Graauw SRON and Leiden Observatory, NL SRON and Leiden Observatory, NL Joint ALMA Observatory, CL Joint ALMA Observatory, CL Acknowledgements: Space- and Science Funding Agencies and Institutes of all involved ESA countries; plus ESA, NASA and CSA, and Industries,
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The HerschelThe Herschel--Heterodyne Instrument for the FarHeterodyne Instrument for the Far--Infrared Infrared (HIFI):(HIFI): Instrument and PreInstrument and Pre--launch Testinglaunch Testing..
Thijs de GraauwThijs de GraauwSRON and Leiden Observatory, NLSRON and Leiden Observatory, NL
Joint ALMA Observatory, CLJoint ALMA Observatory, CL
Acknowledgements:Space- and Science Funding Agencies and Institutes of all involved ESA countries; plus ESA, NASA and CSA, and Industries,
The HerschelThe Herschel--Heterodyne Instrument for the FarHeterodyne Instrument for the Far--Infrared (HIFI):Infrared (HIFI):
Instrument and PreInstrument and Pre--launch Testinglaunch Testing..Thijs de Graauw Thijs de Graauw 1,2,31,2,3, Nick Whyborn, Nick Whyborn1,31,3, Frank Helmich, Frank Helmich11, Pieter Dieleman, Pieter Dieleman11, Peter , Peter
RoelfsemaRoelfsema11,, Emmanuel CauxEmmanuel Caux44, Tom Phillips, Tom Phillips55, Juergen Stutzki, Juergen Stutzki66, Douwe Beintema, Douwe Beintema11, , Arnold BenzArnold Benz77, Nicolas Biver, Nicolas Biver88, Adwin Boogert, Adwin Boogert99, Francois Boulanger, Francois Boulanger1010, Sergey , Sergey
CherednichenkoCherednichenko1919, Odile Coeur, Odile Coeur--JolyJoly44, Claudia Comito, Claudia Comito1111, Emmanuel Dartois, Emmanuel Dartois1010, , Albrecht de JongeAlbrecht de Jonge11, Gert de Lange, Gert de Lange11, Ian Delorme, Ian Delorme88, Anna DiGiorgio, Anna DiGiorgio1212, Luc , Luc
DubbeldamDubbeldam11, Kevin Edwards, Kevin Edwards1,131,13, Michael Fich, Michael Fich1313, Rolf G, Rolf Güüstensten1111, Fabrice Herpin, Fabrice Herpin1313, , Netty HoninghNetty Honingh66, Robert Huisman, Robert Huisman1, 1, Herman JacobsHerman Jacobs11, Willem Jellema, Willem Jellema11, Jon , Jon
KawamuraKawamura1414,Do Kester,Do Kester11, Teun Klapwijk, Teun Klapwijk2525, Thomas Klein, Thomas Klein1111, Jacob Kooi, Jacob Kooi5 5 , Jean, Jean--Michel KriegMichel Krieg88, Carsten Kramer, Carsten Kramer66, Bob Kruizenga, Bob Kruizenga2424, Wouter Laauwen, Wouter Laauwen11, Bengt , Bengt
LarssonLarsson1515, Christian Leinz, Christian Leinz1111, Rene Liseau, Rene Liseau1515, Steve Lord, Steve Lord88, Willem Luinge, Willem Luinge11, Anthony , Anthony MarstonMarston1,161,16, Harald Merkel, Harald Merkel1919, Rafael Moreno, Rafael Moreno88, Patrick Morris, Patrick Morris99, Anthony Murphy, Anthony Murphy2323, , Albert NaberAlbert Naber11, Pere Planesas, Pere Planesas3,173,17, Jesus Martin, Jesus Martin--PintadoPintado1818, Micheal Olberg, Micheal Olberg1,191,19, Piotr , Piotr
OrleanskiOrleanski2020, Volker Ossenkopf, Volker Ossenkopf1,61,6, John Pearson, John Pearson1414, Michel Perault, Michel Perault2121, Sabine Phillip, Sabine Phillip1111, , Mirek RatajMirek Rataj2020, Laurent Ravera, Laurent Ravera44, Paolo Saraceno, Paolo Saraceno1212, Rudolf Schieder, Rudolf Schieder66, Frank , Frank
SchmuellingSchmuelling6 6 , Ryszard Szczerba, Ryszard Szczerba2323, Russell Shipman, Russell Shipman11, David Teyssier, David Teyssier1,161,16, Charlotte , Charlotte VastelVastel44, Huib Visser, Huib Visser2424, Klaas Wildeman, Klaas Wildeman11,, Kees WafelbakkerKees Wafelbakker11, John Ward, John Ward1414, Roonan , Roonan
HigginsHiggins1,231,23, Henri Aarts, Henri Aarts11, Xander Tielens, Xander Tielens1,261,26, Peer Zaal, Peer Zaal1 1 ..
Acknowledgements:Space- and Science Funding Agencies and Institutes of all involved ESA countries; plus ESA, NASA and CSA, and Industries,
HIFI@SPIE2008 3
HerschelHerschel--HIFI ConsortiumHIFI Consortium
DemirmObservatoire de Paris
HIFI@SPIE2008 4
The Herschel Heterodyne Instrument for the Far-Infrared (HIFI)
FPUFPU--FM integrated (1235) and started testingFM integrated (1235) and started testing•• 2006 ++FPU2006 ++FPU--FM fully integrated and testing ongoing; FM fully integrated and testing ongoing;
++ Final Instrument Level tests, including calibration ++ Final Instrument Level tests, including calibration and characterisation, started December till July 2007.and characterisation, started December till July 2007.
•• 2007mid2007mid——2008 Integration in Satellite and system tests2008 Integration in Satellite and system tests
HIFI FPU-FM
5
HIFI main Science:HIFI main Science:Life Cycle of Gas and Dust in OurLife Cycle of Gas and Dust in Our-- and Nearby and Nearby
Galaxies:Galaxies:
ISM in Galaxies• Star formation• Dynamics• Physical conditions
Star formation• Physical conditions• Chemistry• Energetics• Dynamics• Role of Water
ISM in the Milky Way• Physical conditions• Chemistry• Energetics• Dynamics• Isotopic gradients
Stellar evolution• Mass loss• Composition• Dynamics
Seen through Molecular Lines
To achieve the scientific objectivesHIFI was designed with 3 main Challenges:
1) very high spectral resolution; velocity discrimination 0.1-1 Km/s
2) highest possible sensitivity
3) widest possible wavelength/frequency coveragewidest possible instantaneous coverage: velocity span
HIFI@SPIE2008 6
HerschelHerschel--HIFI Science: Life Cycle of Gas and DustHIFI Science: Life Cycle of Gas and DustStar Formation & EvolutionStar Formation & Evolution
Solar System:• Water in GiantPlanets• Atmospheric chemistry• Water activity and
composition of comets
ISM in Galaxies:• Normal galaxies• Physical properties
of star-forming ISM
Dense cores and star-formation:• Temperature, density
structure• Dust properties• Stellar IMF
ISM in the Milky Way:• Structure• Dynamics (pressure)• Composition(gradients)
Late stages of stellar evolution:• Winds• Shells• Asymmetries• Composition
HIFI@SPIE2008 7
0.800.850.900.951.001.05
5.4 5.6 5.8 6 6.2 6.4 6.6 6.8 7
Observations
nten
sity
Herschel Unique Science: Herschel Unique Science: Water abundant from SWAS, ODIN, ISO, Spitzer, etcWater abundant from SWAS, ODIN, ISO, Spitzer, etc
HIFI has coverage for variety of densities and excitation conditHIFI has coverage for variety of densities and excitation conditionsions
-100 0 100Velocity (km/s)
1.9E-16
1.8E-16
1.7E-16
1.6E-16
1.5E-16
W c
m-2
μm
-1
o-H2O 221-110
relative warm H2O
ISO-SWSISO- LWS
SWAS
HIFI@SPIE2008 8
Role Water as chemical and physical probeRole Water as chemical and physical probe
•• HH22O abundance shows large variations in SF regions: O abundance shows large variations in SF regions: <10<10--88 –– 3. 103. 10--44 => unique probe of different physical regimes=> unique probe of different physical regimes
•• Traces basic processes of freezeTraces basic processes of freeze--out onto grains and out onto grains and evaporation, which characterize different stages of evolutionevaporation, which characterize different stages of evolution
•• HH22OO’’s role in the thermal balance: when and where does Hs role in the thermal balance: when and where does H22O O become dominant heating or cooling agent?become dominant heating or cooling agent?
•• HH22O as a dynamical probe of high density gas: infall (?), O as a dynamical probe of high density gas: infall (?), outflow, quiescent gas, mixing, outflow, quiescent gas, mixing, ……
•• HDO/HHDO/H22O: determined by gasO: determined by gas--phase or grainphase or grain--surface surface processes? Relation with comets?processes? Relation with comets?
Santiago 5 November 2007 9
14.5”
Chemistry Chemistry -- as diagnostic toolas diagnostic tool
Ph.D. Thesis, Boonman (2003)
HIFI@SPIE2008 10
HIFI Instrument: HIFI Instrument: Top Level Requirements and Resulting ConceptTop Level Requirements and Resulting Concept
•• Heterodyne spectroscopyHeterodyne spectroscopy•• single pixel on the skysingle pixel on the sky•• very high spectral resolutionvery high spectral resolution
BandBand--6 HEB Noise Temperature6 HEB Noise Temperatureas function of IFas function of IF
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•• LOU with 7 LO assemblies LOU with 7 LO assemblies •• each with 2 LO chains each with 2 LO chains
(10%)(10%)
Local Oscillator Scheme: A common source LSU; 2×7 multiplication chains in 7
assemblies, located opposite the FPU outside the cryostat
MPIfRA/NASA-JPL/SRC-Poland/Canada
HIFI@lesHouches2007 17
HIFI LO HIFI LO frequency multiplication scheme with frequency multiplication scheme with allall--planar devices and no mechanical tunersplanar devices and no mechanical tuners
LOU with 7 LO assemblies LOU with 7 LO assemblies each with 2 LO chainseach with 2 LO chains
LO Assemblywith two chains
To FPU
LSU
LOUWaveguides
HIFI Consortium @ 6 June 2007 1
External DeExternal De--icing baffleicing baffleto be used for attenuator to be used for attenuator
HIFI@SPIE2008 19
WBO FM (one Polarisation)WBO FM (one Polarisation)with 1.1 MHz resolution and 4GHz bandwidthwith 1.1 MHz resolution and 4GHz bandwidth
Sourcemodule
Bragg-cell
Imagingoptics
Cyl.lens
CCD
IF Processor
HIFI@SPIE2008 20
HIFIHIFI--HRS (autoHRS (auto--correlator) FM Capabilities correlator) FM Capabilities
2 HRS FM modules
Hersch
el Press
Event –Friedric
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HIFI 7 months of testing: HIFI 7 months of testing: demonstrated readiness for flightdemonstrated readiness for flight
with good performance, as planned.with good performance, as planned.
With WBS: Methanol at 1016 GHz
With HRS: SO2 at 1696 GHz
Simulatingobservingmolecules in space
1
Gas cell tests Band 1Gas cell tests Band 1
HIFI Stability: Allan Variance numbersHIFI Stability: Allan Variance numbers
HIFI@SPIE2008 23
1
From Table to Observing Modes IFrom Table to Observing Modes I
•• Continuum stability = Continuum observations with Continuum stability = Continuum observations with OTF/MappingOTF/Mapping
•• Spectroscopic stability= Spectroscopy with OTF/Mapping Spectroscopic stability= Spectroscopy with OTF/Mapping
•• Diff. Load Chop Spectroscopy = Double Beam Switch Diff. Load Chop Spectroscopy = Double Beam Switch spectroscopy spectroscopy
Note: Not all Observations with same Obs Mode have same Note: Not all Observations with same Obs Mode have same requirements (Xrequirements (X--Gal Obs)Gal Obs)
HIFI@SPIE2008 25
Expected HIFI sensitivitiesExpected HIFI sensitivitiesderived from ILT testsderived from ILT tests
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HIFI Instrument Summary:HIFI Instrument Summary:
Heterodyne Heterodyne spectroscopy; spectroscopy;
at the time in operation:at the time in operation:-- One single pixel on the One single pixel on the
skysky-- One frequency band;One frequency band;
-- 7 dual7 dual--pol mixer bandspol mixer bands-- 14 LO sub14 LO sub--bandsbands
-- 2 spectrometer systems 2 spectrometer systems in common;in common;
125 K 1.5-15K 300K
HIFI@SPIE2008 27
HIFI Observing Modes and AOT summaryHIFI Observing Modes and AOT summary
• Dual Beam Switch with internal copper and telescope nod• Position Switch efficiency depending on off-position slew• Frequency Switch with switching LSU• Optimum AOT depending on stability Telescope-Instrument System
11. The Star Formation Program. The Star Formation Program1.1 WATER (E. van Dishoeck)1.1 WATER (E. van Dishoeck)1.2 Spectral Scans (C. Ceccarelli)1.2 Spectral Scans (C. Ceccarelli)1.3 The Orion and Sgr B2 regions (T. Bergin)1.3 The Orion and Sgr B2 regions (T. Bergin)
2. ISM2. ISM2.1 The Warm ISM (V. Ossenkopf)2.1 The Warm ISM (V. Ossenkopf)2.2 Hydrides and Molecular Carriers ( M. Gerin)2.2 Hydrides and Molecular Carriers ( M. Gerin)
3. Late stages of Stellar Evolution 3. Late stages of Stellar Evolution (coordinator V. Bujarrabal)(coordinator V. Bujarrabal)3.1 WATER and CO observations of AGB envelopes, PPNe and PNe3.1 WATER and CO observations of AGB envelopes, PPNe and PNe
4. Extragalactic Science 4. Extragalactic Science (R. Guesten)(R. Guesten)4.1 Physical and Chemical Conditions of the ISM in Galactic Nucl4.1 Physical and Chemical Conditions of the ISM in Galactic Nucleiei
5. Water and Chemistry Studies in the Solar System 5. Water and Chemistry Studies in the Solar System (P. Hartogh and E. (P. Hartogh and E. Lellouch)Lellouch)
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25 Years FIRST / Herschel 25 Years FIRST / Herschel Proposal Preparatory WorkshopProposal Preparatory Workshop