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)

LayLay--out Presentation:out Presentation:Scientific motivationScientific motivation•• HIFI consortium HIFI consortium •• Instrument designInstrument design•• First ILT resultsFirst ILT results•• Instrument CapabilitiesInstrument Capabilities

HIFI Programmatic Status:HIFI Programmatic Status:•• 2004 CQM delivered2004 CQM delivered•• 2005 CQM successfully tested/ 2005 CQM successfully tested/

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

prepre--stellar cores stellar cores ¬¬> YSO> YSO’’s s ¬¬> disks > disks ¬¬> comets> comets

•• 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

•• 7 dual7 dual--pol mixer bandspol mixer bands•• 480480--1250 GHz (6251250 GHz (625--240 240 μμm) m)

5x2 SIS mixers, 5x2 SIS mixers, IF 4IF 4--8 GHz8 GHz

•• 14101410--1910 GHz(2121910 GHz(212--157 157 μμm; m; 2x2 HEB mixers, 2x2 HEB mixers, IF 2.4IF 2.4--4.8 GHz4.8 GHz

•• 14 LO sub14 LO sub--bandsbands•• LO source unit in commonLO source unit in common•• LO multiplier chainsLO multiplier chains

•• 2 spectrometer systems;2 spectrometer systems;•• for each polarisationfor each polarisation

-- autoauto--correlator spectrometercorrelator spectrometer-- acoustoacousto--optical spectrometeroptical spectrometer

Angular Resolution (with Herschel): 12”- 40”

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 μm)

1410 – 1910 GHz (212-157 μm)

2. SensitivityNear-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

11

2) To cover wide frequency range:2) To cover wide frequency range:HIFI consists of 7 receiversHIFI consists of 7 receivers

Spectralresolution

Backendspectrometers

mixer

IF amp

FrequencyDependencyand range

7 Mixers/amps

2×2 Spectrometers(common)

2×7 LO bands

Basic receiver elements 7 Mixer bands and 7×2 LO’s

3) High Sensitivitywith superconducting mixers

(SIS and HEB)

LO

HIFI@SPIE2008 12

HIFI Block DiagramHIFI Block Diagram

fromtelescope

Common OpticsCalibration sourceChopper mechanism7 Mixer Assemblies each with 2 mixersIF amplifiers

FPU

ControlMixer biasAmplifier biasMechanism control

FCU

LOUHousing7 LO Assemblies with 7x2 LO chains and power amplifiers

LCUControlMultiplier biasPower amplifier

biasSec Power for

LSU

LSUMaster oscillatorSynthesizerRef. distribution

Instrument Control UnitInstrument Controller Power Conditioning (for FCU only)Command Interface Data Interface

spacecraftCDMS

Band 6 up-converter3 dB coupler

IFH

Band 6 up-converter3 dB coupler

IFV

Δf~1GHzδf variable

HRS-hIF processorSub-band division

Δf~1GHzδf variable

HRS-vIF processorSub-band division

Δf 4 GHzδf 1 MHz

WBS-vIF processorSub-band division

Δf 4 GHzδf 1 MHz

WBS-hIF processorSub-band division

From Telescope

In Service Module

HIFI@SPIE2008 13

HIFI FPU FM with mixer bands HIFI FPU FM with mixer bands 1,2,3,5 and complete1,2,3,5 and complete

Common Optics Asembly

HIFI@SPIE2008 14

HIFI Signal Chain: Mixers and AmplifiersHIFI Signal Chain: Mixers and AmplifiersHIFI Dual IF System - one polarisation

N. D. Whyborn, 021016

N.B. There is an identical arrangement for the other polarisation.

min. level:

IF gain:

max. level:

-128 dBm/MHz

-118 dBm/MHz

HRS-V

WBS-V

-108 dBm/MHz

-98 dBm/MHz

-95 dBm/MHz

-85 dBm/MHz

-100 dBm/MHz

-90 dBm/MHz

-3 dB -2 dB-5 dB25 dB-1 dB +21 dB -8 dB

6H

6L

5

4

3

2

1

2.4

- 4.8

GH

z IF

4 - 8

GH

z IF

10.4 GHz

2.4 - 4.8GHz

8 - 5.6GHz

min. level:

max. level:

-128 dBm/MHz

-118 dBm/MHz

-103 dBm/MHz

-93 dBm/MHz

-79 dBm/MHz

-69 dBm/MHz

-100 dBm/MHz

-90 dBm/MHz

mixer &isolator IF up-converter spectrometerscryoharness

290 K (SVM)

warmharness

leveltrimming

15 K level4 Klevel

IF-1amplifier

2 K level

IF-2assembly

IF gain: -16 dB -3 dB -2 dB-3 dB29 dB-1 dB +30 dB -6 dB

(+31 dB) (-10 dB)

1

3/4

6

2

5

3/4

1

IF-1IF-2

HIFI@SPIE2008 15

BandBand--3 SIS Noise Temperature 3 SIS Noise Temperature as function of IFas function of IF

FM 12, Band6 High, 2005-07-14, S32-82, 4.2K ;LO: 1-- 1.63 THz; 16--1.89 THz

700900

110013001500170019002100230025002700

2.4 2.9 3.4 3.9 4.4 4.9IF, GHz

DSB

Tr,

K, c

orre

cted

for o

ptic

al lo

ss

FM12-IF-1 Band6H-1.6THzFM12-IF-16 Band6H-1.9THzBand6H-1.8THz

LO:1.63 THz

LO:1.89 THz

BandBand--6 HEB Noise Temperature6 HEB Noise Temperatureas function of IFas function of IF

16

•• 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

21

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

•• Diff. Internal Load Continuum = Double Beam Switch Diff. Internal Load Continuum = Double Beam Switch Continuum Continuum

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

26

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

HIFI@SPIE2008 28

HIFI Key ProgramsHIFI Key ProgramsOVERVIEW: (with coordinatorOVERVIEW: (with coordinator’’s name)s name)

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)

29

25 Years FIRST / Herschel 25 Years FIRST / Herschel Proposal Preparatory WorkshopProposal Preparatory Workshop

Noordwijkerhout, NLNoordwijkerhout, NLMay 1983May 1983