fsue “lavochkin association” lebedev physical institute astro space center millimetron mision...

FSUE “Lavochkin Association”Lebedev Physical InstituteAstro Space Center

Millimetron mision sensitivities and Millimetron mision sensitivities and instrumentation conceptinstrumentation concept

A.M. Baryshev, W. Wild, G. Goltsman, N.S. KardashevA.M. Baryshev, W. Wild, G. Goltsman, N.S. Kardashev

Netherlands Institute for Space Research, NetherlandsNetherlands Institute for Space Research, NetherlandsAstro Space Center, Lebedev Physical Institute, RussiaAstro Space Center, Lebedev Physical Institute, Russia

ISSTT 2008, Groningen 2

OutlineOutline

• Main concept of “Millimetron” missionMain concept of “Millimetron” mission• Concept 12 m diameter deployable antenna of “Millimetron”Concept 12 m diameter deployable antenna of “Millimetron”• Astronomical instrumentsAstronomical instruments• SensitivitiesSensitivities• ConclusionsConclusions


Telescopes for Radio-astronomy Space MissionsTelescopes for Radio-astronomy Space Missions

• Main requirements and trendsMain requirements and trends• Driven by scientific objectiveDriven by scientific objective• Telescope size, diameter Telescope size, diameter

• Better sensitivity for compact sources ~DBetter sensitivity for compact sources ~D22

• Better spatial resolution ~DBetter spatial resolution ~D-1-1

• The larger the betterThe larger the better• Mirror accuracyMirror accuracy

• Tendency to observe frequencies, inaccessible from groundTendency to observe frequencies, inaccessible from ground• RF > 1 THzRF > 1 THz

• Telescope coolingTelescope cooling• Background radiation ~TBackground radiation ~T44

• Space environment allow for passive (50 K) and active coolingSpace environment allow for passive (50 K) and active cooling• 4 K dish is highly desired4 K dish is highly desired

• Large deployable apertures are neededLarge deployable apertures are needed• Ultimate mission: a free flying interferometer with large cold telescopes Ultimate mission: a free flying interferometer with large cold telescopes

(>6) (>6) FIRIFIRI• There are practicalities…There are practicalities…


Millimetron mission parameters and statusMillimetron mission parameters and status

• Frequency range: from mm wave to THz frequenciesFrequency range: from mm wave to THz frequencies• Two observing modesTwo observing modes

• Space earth VLBISpace earth VLBI• Single dish modeSingle dish mode

• Heterodyne and direct detection instruments (arrays)Heterodyne and direct detection instruments (arrays)• Aperture diameter 12 metersAperture diameter 12 meters

• ~4 m diameter central solid dish (~4 m diameter central solid dish (goalgoal 5 µm surface, 4 THz) 5 µm surface, 4 THz)• 12 m petal type deployable (12 m petal type deployable (goalgoal 10 µm RMS surface, 10 µm RMS surface,

1..2 THz)1..2 THz)• Passively cooled, 30..50 K (study active cooling possibilities)Passively cooled, 30..50 K (study active cooling possibilities)

• Mass < 4000 kgMass < 4000 kg• Orbit similar to Radioastron 300000 km apogee or L2Orbit similar to Radioastron 300000 km apogee or L2• Approved mission in Russia (Included in 10 year plan of RSA)Approved mission in Russia (Included in 10 year plan of RSA)• Now in conceptual phase, launch frame ~2017..18Now in conceptual phase, launch frame ~2017..18


Spacecraft conceptSpacecraft concept

“Navigator” spacecraft platform

Three layer deployable thermal shields

Deployable primary mirror Cold focal plane instruments (0.1…4 K)

Deployable truss


Space platform NavigatorSpace platform Navigator

Lavochkin association


Antenna optical parametersAntenna optical parameters

• Cassegrain schemeCassegrain scheme• Diameter 12 mDiameter 12 m• Secondary focus 4414.3Secondary focus 4414.3• Moveable secondary mirrorMoveable secondary mirror• Active main dish (concept) Active main dish (concept)

including laser petal position including laser petal position measurements and feed measurements and feed abck systemabck system


Radiosatron antenna construction (folded)Radiosatron antenna construction (folded)

Proton-MLauncher


Details openingDetails opening


Antenna deployment conceptAntenna deployment concept

Two 20:1 scalemodels are beingmade


Deploying sequenceDeploying sequence


Astronomical instrumentsAstronomical instruments

• Large format low spectral resolution camera (polarization Large format low spectral resolution camera (polarization sensitive)sensitive)

• Medium spectral resolution (R=1000..5000) imaging Medium spectral resolution (R=1000..5000) imaging spectrometer (similar to SPICA SAFARI)spectrometer (similar to SPICA SAFARI)

• High resolution spectrometer (similar to Herschel HIFI High resolution spectrometer (similar to Herschel HIFI instrument)instrument)

• SVLBI instruments (heterodyne, covering ALMA bands) SVLBI instruments (heterodyne, covering ALMA bands)


Low resolution spectrometerLow resolution spectrometer

• 1mm .. 0.15 mm wavelength, several channels1mm .. 0.15 mm wavelength, several channels• State of the art sensitivityState of the art sensitivity• Up to 10 kPixels for the shorter wavelength channelUp to 10 kPixels for the shorter wavelength channel• Use 12m diameter aperture up to 0.15 mm Use 12m diameter aperture up to 0.15 mm • Possibility to use central mirror for shorter wavelengthsPossibility to use central mirror for shorter wavelengths

• Specifically do not mention technologiesSpecifically do not mention technologies• NEP 10^-19 required depending on the achieved antenna NEP 10^-19 required depending on the achieved antenna

temperature temperature

• Cooling 100..300 mKCooling 100..300 mK


PhotometerPhotometer ( (SPIRE)SPIRE)


Sensitivity of photometer, 12m dish, 50KSensitivity of photometer, 12m dish, 50K


Photometer sensitivity 4m central dish, 50 KPhotometer sensitivity 4m central dish, 50 K


Photometer sensitivityPhotometer sensitivity


4K dish temperature (for reference)4K dish temperature (for reference)

1 1 0 1 0 0 1 0 0 0 1 0 40 .1

1

1 0

1 0 0

1 0 0 0

1 0 4

W a v e le ngth (m )

Det

ectio

nLi

mit

5–

1H

our(

Jy )

12 m dish , 10 m R M S, 50 K , R = 3

A L M A

JW ST M IR I

SP IC A M IR

H erschel SP IR EH erschel P A C S

SP IC A FIR SO AP

SP IC A FIR G OA L

M illim e tr o n

1 1 0 1 0 0 1 0 0 0 1 0 40 .1

1

1 0

1 0 0

1 0 0 0

1 0 4


Det

ectio

nLi

mit

5–

1H

our(

Jy )

12 m centra l dish , 10 m R M S , 4 K , R = 3

A L M A

JW ST M IR I

SP IC A M IR

H erschel SP IR EH erschel P A C S

SP IC A FIR SO AP

SP IC A FIR G OA L

M illim e tr o n


Medium resolution spectrometerMedium resolution spectrometer

• 1mm .. 0.15 mm wavelength, several channels1mm .. 0.15 mm wavelength, several channels• State of the art sensitivityState of the art sensitivity• Up to 5 kPixels for the shorter wavelength channelUp to 5 kPixels for the shorter wavelength channel• Use 12m diameter aperture up to 0.15 mm Use 12m diameter aperture up to 0.15 mm • Possibility to use central mirror for shorter wavelengthsPossibility to use central mirror for shorter wavelengths• R=1000..5000 (frequency dependent)R=1000..5000 (frequency dependent)• Technology TBDTechnology TBD

• NEP 10^-19 required depending on the achieved antenna NEP 10^-19 required depending on the achieved antenna temperature temperature

• Cooling 100…300mKCooling 100…300mK


FTSFTS ( (SPIRE)SPIRE)


Sensitivity of medium resolution spectrometerSensitivity of medium resolution spectrometer


4K dish for reference4K dish for reference

1 5 1 0 5 0 1 0 0 5 0 0 1 0 0 01 0 -2 1

1 0 -2 0

1 0 -1 9

1 0 -1 8

1 0 -1 7

1 0 -1 6


Det

ectio

nLi

mit

5–

1H

our(

Wm

-2)

12 m dish , 10 m R M S, 50 K , R = 1000

AL M A

JW ST M IR I

SP IC A M IR

Spitzer IR S

Herschel SP IR E

Herschel P AC S

SP IC A FIRSOA P

SP IC A FIR GO AL

M illim e tr o n

1 5 1 0 5 0 1 0 0 5 0 0 1 0 0 0

1 0 -2 1

1 0 -2 0

1 0 -1 9

1 0 -1 8

1 0 -1 7

1 0 -1 6


Det

ectio

nLi

mit

5–

1H

our(

Wm

-2)

12 m dish , 10 m R M S, 4 K , R = 1000

AL M A

JW ST M IR I

SP IC A M IR

Spitzer IR S

Herschel SP IR E

Herschel P AC S

SP IC A FIRSOA P

SP IC A FIR GO AL

M illim e tr o n


High resolution spectrometerHigh resolution spectrometer

• R > 10000R > 10000• Spot or continuous frequency bands 500-2000 THz for 12m Spot or continuous frequency bands 500-2000 THz for 12m

apertureaperture• Spot frequency bands up to 5 THz using central solid dishSpot frequency bands up to 5 THz using central solid dish• Small focal plane arrays for lower frequencies (LO power Small focal plane arrays for lower frequencies (LO power

limited)limited)• IF 4-12 GHzIF 4-12 GHz• Polarization !!!Polarization !!!• Conceptually based on Herschel HIFI instrumentConceptually based on Herschel HIFI instrument

• Cooling 4 KCooling 4 K


Herschel HIFIHerschel HIFI


Example of frequency distributionExample of frequency distribution

Millimetron Single-dish instrumentation

Instrument Frequency (GHz) or wavelength

Ang. res. ()

Spectral res.

Detector technology

Sensitivity TRL

Heterodyne receivers

HET-1 480 – 700 8…12 106 SIS 2x2 mixer array with multiplier LO

Tsys < 100 K 6

1100 – 1400 5…6 106 Tsys < 200 K 6

HET-2 1650 – 2000 ~3 106 HEB mixers with multiplier or QCL LO

Tsys < 500 K 6

2600 – 2700 ~2.5 106 Tsys < 700 K 4

4700 – 4800 4 (1) 106 Tsys < 1000 K 4

Far-Infrared imaging photometer/spectrometer

M-PACS 60 – 210 m 4 few 103 spectrom.

Photoconductor arrays

2 x 10-18 Wm-2 6


SensitivitiesSensitivities

0 .5 1 .0 1 .5 2 .0 2 .5 3 .0 3 .5 4 .0

1 0 -2 2

1 0 -2 1

1 0 -2 0

1 0 -1 9

1 0 -1 8

F r e q ue nc y ( T H z )

Det

ectio

nLi

mit

5–

1H

our(

Wm

-2)

R = 10000

5 quanta, 5 m R M S , 4 m5 quanta, 10 m R M S , 12 m1 quantum, 5 m R M S , 4 m1 quantum, 10 m R M S , 12 m


SVLBI instrumentsSVLBI instruments

• R > 10000R > 10000• Selected ALMA bands 500-1000 THz for 12m apertureSelected ALMA bands 500-1000 THz for 12m aperture• Spot frequency bands up to 5 THz using central solid dishSpot frequency bands up to 5 THz using central solid dish• On board data recorderOn board data recorder• On board stable referenceOn board stable reference• Fast data linkFast data link• IF 4-12 GHz (compatible to ALMA)IF 4-12 GHz (compatible to ALMA)

• Can be conceptually based on Herschel HIFI instrumentCan be conceptually based on Herschel HIFI instrument

• Cooling 4 KCooling 4 K


Instrument type

VLBI receiver

Heterodyne receiverscovering ALMA bands

Receiver VLBI-1 ALMA-1 ALMA-3 ALMA-6 ALMA-9

Frequency range

18 – 26 GHz

31.3 - 45 GHz

84-116 GHz 211-275 GHz

600-720 GHz

Detector technology

HEMT amplifier

SIS mixers, multiplier chain LO, dual pol.

Or HEMT




Sensitivity Tsys < 40 K < 17 K SSB < 37К SSB < 90 K SSB < 150 K DSB

TRL 6 6 6 6 6

fsue “lavochkin association” lebedev physical institute astro space center millimetron mision...

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