The Herschel-Heterodyne Instrument for the Far-Infrared

"Developments in microwave technologies for HIFI"

HIFI Consortium (1)

•• ThijsThijs de de GraauwGraauw 1,2,31,2,3, Nick Whyborn, Nick Whyborn1,31,3, Frank Helmich, Frank Helmich11, Pieter Dieleman, Pieter Dieleman11, , Peter RoelfsemaPeter Roelfsema11,, Emmanuel CauxEmmanuel Caux44, Tom Phillips, Tom Phillips55, , JuergenJuergen StutzkiStutzki66, , DouweDouwe BeintemaBeintema11, Arnold Benz, Arnold Benz77, Nicolas Biver, Nicolas Biver88, , AdwinAdwin BoogertBoogert99, Francois , Francois BoulangerBoulanger1010, Sergey Cherednichenko, Sergey Cherednichenko1919, , OdileOdile CoeurCoeur--JolyJoly44, Claudia , Claudia ComitoComito1111, Emmanuel Dartois, Emmanuel Dartois1010, Albrecht de Jonge, Albrecht de Jonge11, , GertGert de Langede Lange11, Ian , Ian DelormeDelorme88, Anna DiGiorgio, Anna DiGiorgio1212, Luc Dubbeldam, Luc Dubbeldam11, Kevin Edwards, Kevin Edwards1,131,13, Michael , Michael FichFich1313, Rolf G, Rolf Güüstensten1111, , FabriceFabrice HerpinHerpin1313, , NettyNetty HoninghHoningh66, Robert Huisman, Robert Huisman1, 1,

Herman JacobsHerman Jacobs11, Willem Jellema, Willem Jellema11, Jon Kawamura, Jon Kawamura1414,Do Kester,Do Kester11, , TeunTeunKlapwijkKlapwijk2525, Thomas Klein, Thomas Klein1111, Jacob Kooi, Jacob Kooi5 5 , Jean, Jean--Michel KriegMichel Krieg88, , CarstenCarstenKramerKramer66, Bob Kruizenga, Bob Kruizenga2424, , WouterWouter LaauwenLaauwen11, , BengtBengt LarssonLarsson1515, Christian , Christian LeinzLeinz1111, Rene Liseau, Rene Liseau1515, Steve Lord, Steve Lord88, Willem Luinge, Willem Luinge11, Anthony Marston, Anthony Marston1,161,16, , HaraldHarald MerkelMerkel1919, Rafael Moreno, Rafael Moreno88, Patrick Morris, Patrick Morris99, Anthony Murphy, Anthony Murphy2323, Albert , Albert NaberNaber11, , PerePere PlanesasPlanesas3,173,17, Jesus Martin, Jesus Martin--PintadoPintado1818, , MichealMicheal OlbergOlberg1,191,19, , PiotrPiotrOrleanskiOrleanski2020, Volker Ossenkopf, Volker Ossenkopf1,61,6, John Pearson, John Pearson1414, Michel Perault, Michel Perault2121, Sabine , Sabine PhillipPhillip1111, , MirekMirek RatajRataj2020, Laurent Ravera, Laurent Ravera44, Paolo Saraceno, Paolo Saraceno1212, Rudolf , Rudolf SchiederSchieder66, Frank Schmuelling, Frank Schmuelling6 6 , , RyszardRyszard SzczerbaSzczerba2323, Russell Shipman, Russell Shipman11, , David TeyssierDavid Teyssier1,161,16, Charlotte Vastel, Charlotte Vastel44, , HuibHuib VisserVisser2424, , KlaasKlaas WildemanWildeman11,, KeesKeesWafelbakkerWafelbakker11, John Ward, John Ward1414, Ronan Higgins, Ronan Higgins1,231,23, Henri Aarts, Henri Aarts11, , XanderXanderTielensTielens1,261,26, Peer Zaal, Peer Zaal1 1 ..

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HerschelHerschel--HIFI Consortium:HIFI Consortium:11 countries/23 Institutes11 countries/23 Institutesdeveloped and constructed HIFI (15+10 yrsdeveloped and constructed HIFI (15+10 yrs))

DemirmObservatoire de Paris

The Herschel Mission

•• ESA 4ESA 4thth cornerstone Horizon2000 cornerstone Horizon2000 observatoryobservatory–– instruments instruments ‘‘nationallynationally’’ funded, funded,

with intwith int’’l l -- NASA, CSA, Poland NASA, CSA, Poland ––collaborationcollaboration

–– ~1/3 guaranteed time, ~2/3 open ~1/3 guaranteed time, ~2/3 open

•• FIR (57 FIR (57 -- 670 670 μμm) space facilitym) space facility–– large (3.5 m) monolithic low large (3.5 m) monolithic low

emissivity passively cooled emissivity passively cooled telescope, with stable backgroundtelescope, with stable background

–– 3 focal plane science instruments3 focal plane science instruments–– 3 years routine operational 3 years routine operational

lifetime (>+0.5)lifetime (>+0.5)–– full spectral access full spectral access

•• Planned launch in 2008Planned launch in 2008

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FarInfrared/SubMillimeterFarInfrared/SubMillimeter Wavelength RangeWavelength Rangedomain of Cool and Cold Universedomain of Cool and Cold Universe

•• But also very rich with fine details of crucial information But also very rich with fine details of crucial information

•• Molecular(130) Emission and Absorption linesMolecular(130) Emission and Absorption lines

•• Atomic and Ionic lines, and in particularAtomic and Ionic lines, and in particular

•• Simple molecules with Hydrogen and one or two other atoms Simple molecules with Hydrogen and one or two other atoms like Water like Water (H(H22O), OH, etc..O), OH, etc..

This spectral survey is a ground-based (Hawaii) example (330GHz) what HIFI will see at higher frequencies (>480 GHz)

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Bring Comets water on new planets?Comet soup

Origin of water on Earth

Hale-Bopp

Meet HDO/H2O!

7

>141 molecules detected (2006)>141 molecules detected (2006)

8

FIR observations from Space?FIR observations from Space?Limitations from AtmosphereLimitations from Atmosphere

9

Why longer (IRWhy longer (IR--Submm)wavelengthsSubmm)wavelengths??

4.5 8.0 24 μm1.2 1.6 1 mm contours

Such obscured star-forming regions can be probed directlyat FIR/mm wavelengths

10

(F)IR Missions in Perspective(F)IR Missions in Perspective

(Survey)

IRAS

SPITZERAKARI

JWST-MIRIHerschel

SPICA

1983

2009;SOFIA

1983

1995

2008

2004

2013

SWASOdin

2007

survey

Spectral Survey

2017

ISO

Mmtron

LRS

2017

> 2020

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~ 0.005 arcsecs with few K sensitivity

~ 10 arcsec with micro-K sensitivity

Closing the FIR Spatial Resolution Gap

Herschel

300-30 µm

FIRIESPRIT

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Herschel spacecraft dataHerschel spacecraft data

•• telescope diameter 3.5 mtelescope diameter 3.5 m

•• telescope WFE < 6 telescope WFE < 6 μμmm

•• telescope temp < 90 Ktelescope temp < 90 K

•• telescope emissivity < 4%telescope emissivity < 4%

•• abs/abs/relrel pointgpointg (68%) < 3.7(68%) < 3.7”” / 0.3/ 0.3””

•• science instruments 3science instruments 3

•• science data rate science data rate 130 kbps130 kbps

•• cryostat lifetime 4.0cryostat lifetime 4.0±±0.4 years 0.4 years

•• height / widthheight / width ~ 7.5 / 4 m~ 7.5 / 4 m

•• launch masslaunch mass ~ 3200 kg~ 3200 kg

•• power power ~ 1500 W~ 1500 W

•• orbit orbit ‘‘largelarge’’ LissajousLissajous around L2around L2

•• solar aspect angle 60solar aspect angle 60--120 deg120 deg

•• launcher (w Planck) launcher (w Planck) ArianeAriane 5 ECA5 ECA

Introduction - the Herschel Spacecraft

Launch late 2008 shared with Planck on Arianne V

Sun-Earth L2 orbit

Far-infrared/submmSpace Observatory

Credits ESA/AstriumCredits ESA/Astrium

Herschel and Planck in an Sun-Earth L2 Orbit; 2008

Introduction - the Herschel Telescope

• Largest telescope ever put into space

• 3.5 meter Cassegrain telescope

• Stable and light-weight SiC technology

Credits ESA/Astrium Credits ESA/Astrium

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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--polpol mixer bandsmixer bands–– 480480--1250 GHz (6251250 GHz (625--240 240 μμm) 5x2 m) 5x2

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

–– 14101410--1910 GHz(2121910 GHz(212--157 157 μμm; 2x2 m; 2x2 HEB mixers, 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--correlatorcorrelator spectrometerspectrometer-- acoustoacousto--optical spectrometeroptical spectrometer

Angular Resolution 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

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HIFI uses Heterodyne DetectionA radio technique invented in 1918

Two signals with different frequencies are combined onto a detector-mixer, e.g.1) broad band signal from the sky + 2) oscillator (single frequency) inside the instrumentlocal oscillator LOto produce difference signal (IF= intermediate

frequency signal)

Mixer needs non-linear element (diode, SIS junction)

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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 FM Focal Plan Unit (1)

MSA’s

IF box

HIFI FM Focal Plane Unit (2)

Pickoff mirror M3

ADCSA

HIFI FM Focal Plane Unit (3)

LO ports

MSA’s

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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

23

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

2

3/4

56

3/4

1

IF-1IF-2

Focal Plane Optics – Mixer Units

Waveguide mixer (band 3)Horn antenna

Quasi-optical mixer (band 5)Integrated Lens-Antenna

25

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

HIFI@lesHouches2007 26

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

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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

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WBO FM (WBO FM (oneone Polarisation)Polarisation)withwith 1.1 MHz 1.1 MHz resolutionresolution and 4GHz and 4GHz bandwidthbandwidth

Sourcemodule

Bragg-cell

Imagingoptics

Cyl.lens

CCD

IF Processor

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HIFIHIFI--HRS (autoHRS (auto--correlatorcorrelator) FM Capabilities ) 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 flightwith good performance, as planned.with good performance, as planned.

With WBS: Methanol at 1016 GHz

With HRS: SO2 at 1696 GHz

Simulatingobservingmolecules in space

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Expected HIFI sensitivitiesExpected HIFI sensitivitiesderived from ILT testsderived from ILT tests

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Summary:Summary:

•• New techniques allow a major step in FIR/New techniques allow a major step in FIR/SubMMSubMMAstronomyAstronomy–– In spectral resolutionIn spectral resolution–– In angular resolutionIn angular resolution

•• In next 5 years 2 new worldIn next 5 years 2 new world--class facilities class facilities (Herschel/ALMA)(Herschel/ALMA)–– Detailed studies will advance knowledge of galaxy Detailed studies will advance knowledge of galaxy

evolution and star/planet system formationevolution and star/planet system formation