Alf dAlfredThe ProjektThe ProjektjSOFIA - the Stratospheric Observatory For Infrared Astronomy is a project jointly devSOFIA the Stratospheric Observatory For Infrared Astronomy is a project jointly devoperated by the German Aerospace Center (DLR) and the National Aeronautics andoperated by the German Aerospace Center (DLR) and the National Aeronautics and Administration (NASA) SOFIA’s main scientific mission is the observation of the infraAdministration (NASA). SOFIA’s main scientific mission is the observation of the infra

f Snear infrared to submm wavelengths. For this purpose a Boeing 747 SP was heavily back portion of the plane a 2.7 m telescope weighing 17 tons was installed. A cruisinge p p p g g gapproximately 14 km SOFIA will operate above 99 % of the atmospheres water vapode approximately 14 km SOFIA will operate above 99 % of the atmospheres water vapovelocity of approximately 900 km/h and temperatures of approximately 50°C providear

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t d bt t th b kmeasurements and subtracts the backgroutranslative corrections to center and focus tbe used for the flexible body compensationy poscillations onto the telesope introduced byoscillations onto the telesope introduced by

Current StatusCurrent StatusTh N S i C t t k b lThe New Science Case – to take away – see belowyIn 2009 the news science vision for SOFIA was compiled Four major area in modernIn 2009 the news science vision for SOFIA was compiled. Four major area in modern

Galaxies and the Galactic CenterSOFIA will investigate the strength and spatialSOFIA will investigate the strength and spatial distribution of star formation in the redshift rangedistribution of star formation in the redshift range b t 0 3 > > 1 1 th t i i l f thbetween 0,3 > z > 1,1 that is crucial for the understanding of the star formation history of the universe. Moreover SOFIA will observe the galactic center to understand the complexgalactic center to understand the complex mechanisms that proceed in this extrememechanisms that proceed in this extreme

i t E th [CII] 158 fi t tenvironment. E.g. the [CII] 158µm fine – structuretransition, which is the most important cooling line of the cold Interstellar medium , p gand therefore critical for its energy balance will be observedand therefore critical for its energy balance, will be observed.

Th I t t ll M diThe Interstellar MediumSOFIA will probe the interstellar medium that is pthe record all generations of stars that belong to athe record all generations of stars that belong to a galaxy The physical processes on how starsgalaxy. The physical processes on how starsinteract with their environment the origin of dustinteract with their environment, the origin of dust

ll th l f l l bas well as the role of large complex carbon molecules will be explored. Hence SOFIA will take pone of the deepest views in the regions whereone of the deepest views in the regions where stars and eventually planets formstars, and eventually planets form.

The Schedule for first scienceThe Schedule for first science2010:2010:A il Fi t t h i l li ht ith FORCAST JApril - First technical light with FORCAST June

- call for basic science (Application from( ppastronomical community – limited)astronomical community limited)

July - Call for next generation instruments (US)July - Call for next generation instruments (US)September First science (Short science) with FORCASTSeptember - First science (Short science) with FORCAST

( bl th G l ti C t )(presumably on the Galactic Center)2011February - First science (Short science) with GREATFebruary First science (Short science) with GREATMarch-June - Basic science with FORCAST GREATMarch-June - Basic science with FORCAST, GREAT20132013J FLITECAMJune - FLITECAMOctober - HIPO

The First Science InstrumentsThe First Science InstrumentsSOFIA ill h 9 fi tSOFIA will have 9 first gene7 will be provided by the USby German teams. For the fiy(3 US 2 German) instrumen(3 US, 2 German) instrumen

SOFIA H h lSOFIA Herschel

λλ [μm] 0,3 – 1600 60 – 670Spiegel ø [m] 2,7 m 3,5 mS 2011 2009/10Start 2011 2009/10L f it [J h ] 20 3Laufzeit [Jahre] 20 3 Ende 2034 /2013

1 Li Fl Li it i 1h i 3 10 18 W/ 2 t R 1 000 t 100

Ende 2034 /20131σ Line Flux Limit in 1h is ~3x10-18 W/m2 at R ≈ 1,000 at 100µm

SOFIA the "Stratospheric Observatory for Infrared Astronomy" is a joint project of the Deutsches Zentrum für Luft- und Raumfahrt e V (DLR; GermaSOFIA, the Stratospheric Observatory for Infrared Astronomy is a joint project of the Deutsches Zentrum für Luft und Raumfahrt e.V. (DLR; GermaTechnology based on legislation by the German Parliament the state of Baden-Württemberg and the University of Stuttgart. Scientific operation for Gthe German Instruments is financed by the Max Planck Society (MPG) and the German Research Foundation (DFG).

d K bb 1 Dö t M hl t1d Krabbe1, Dörte Mehlert1,Platform: Boeing 747SPPlatform: Boeing 747SPTelescope mass: 17 000 kg

veloped andTelescope mass: 17.000 kgMain mirror diameter: 2 7 mveloped and

SpaceMain mirror diameter: 2,7 mSpectral range : 0 3 1600 µmSpace

ared universe fromSpectral range : 0,3 - 1600 µm Pointing stability: 0 2 arcsec rmsared universe from

fPointing stability: 0,2 arcsec rms

modified and in the g altitude of gur However aur. However, a e harsh conditionse harsh conditions

p of MT Aerospacep of MT-Aerospace b h d t tiby a hydrostatic rotation of the

between 15º to 70°. Altitude: ~ 14 kmFlights: ~ 160 / yearuples the telescope Flights: 160 / yearScience: ~ 8 h / night

uples the telescope onsists out of 24 Science: 8 h / night

Mission duration: 20 yearsonsists out of 24

h lf ti i Mission duration: 20 yearsone half acting in imary mirror is a lightweighted ZERODUR structure with rizes by a low coefficient of thermal expansion and a high y p gceramic mirror has a diameter of 35 cm and can be tiltedceramic mirror has a diameter of 35 cm and can be tilted z with a maximum angle of 8’ It is used for differentialz with a maximum angle of 8 . It is used for differential

d di ti f th i tifi bj t Additi ll it idnd radiation from the scientific object. Additionally it provides the collected light beam. The secondary mirror is also planned to n during Observation, which will compensate the natural g , py the wind loady the wind load.

IR Astronomy were identified to be the major areas that will be investigated with SOFIA:IR Astronomy were identified to be the major areas that will be investigated with SOFIA:The Formation of Stars and PlanetsSOFIA will focus on the understanding how the most massiveSOFIA will focus on the understanding how the most massive stars form These stars greatly impact large areas of thestars form. These stars greatly impact large areas of the

l b th i di l hi h t t Mgalaxy by their exceedingly high temperatures. Moreover SOFIA will be able to trace the formation, distribution an evolution of water from the ISM into the planet bearing disks p gof starsof stars.

Planetary ScienceyComets, near-Earth asteroids, atmosphere-bearing moonsComets, near Earth asteroids, atmosphere bearing moons (such as Titan) and planets (e g Venus) as well as Exo-(such as Titan), and planets (e.g. Venus) as well as Exo-planets will be investigated with SOFIA and will give hints onplanets will be investigated with SOFIA and will give hints on h th t t f th t l f lifhow the stage was set for the eventual appearance of life on our planet.p

First open door flightFirst open door flight D 18th 2009

Envelope expansion flightson Dec. 18th, 2009

- Envelope expansion flights- maintenancemaintenance- instrument commission

2008 2009 2010 2011 2012 2013 2014 2015

C tS iTW l thI t tti i t t CommentsScienceTypeWavelength-range [ µm]

Instrumentration instruments.

i ltAt h d i f l tI0 3 0 6HIPOrange [ µm] partners, 2 are built

- simultaneous mount with 2

- Atmospheres and rings of planets (solar system and exoplanets)

I- 0,3-0,6 µm0 4 1 1 µm

HIPONIRirst science 5 mount with 2.(solar system and exoplanets)- 0,4 – 1,1 µmNIRSP Ints will be available

simultaneousT ti i litI&S1 5 5 µmFLITECAMSP-Ints will be available.

- simultaneous mount with 1

- Testing image qualitySpectroscopic complement HIPO

I&S- 1 – 5,5 µmFLITECAMNIR mount with 1.- Spectroscopic complement – HIPO

- stellar population in SF regionsNIRF-I

- 9 filters- Dust properties and ionisation sources in theI&S-5-8 µmFORCASTstellar population in SF regionsF I

- 9 filters- multi colour

- Dust properties and ionisation sources in the galactic center; star formation regions, active

I&S-5-8 µm-17-25 µm &

FORCASTMIR multi colour

imaginggalactic center; star formation regions, active galaxies, circum stellar dust envelopes

17 25 µm & 25-40 µm

MIRF-I

S it JWST - High- Fine structure transitions in ISM; coolingS1,6 – 1,9 THzGREATg gg , pµ

Spitzer JWST High resolution-

Fine structure transitions in ISM; cooling processes; energy balance

S1,6 1,9 THz2,4 – 2,7 THz

GREATFIR

3 – 180 0,6 – 28 submm spectr. p ; gy

- Deuterium abundance > SF history, ,

~ 4.7 THzPI-I0,85 m 6,5 m2003 h 2014

[63 – 187 µm] 2003 nach 20143 [6] 5 10

-3D imaging!- SF & ISM in galaxies I&S42 – 110 µmFIFI-LS3 [6] 5-102009 2019 2024

- extragalactic> MW and others (e.g. dwarf; ULIRGs)110 – 210 µm FIR 2009 2019-2024 > merging / interacting galaxiesF-I

I – imaging; S – spectroscopy SP-, F-, PI-I: Special Purpose, Facility & Principal Investigator Instrument

n Aerospace Centre grant: 50OK0901) and the National Aeronautics and Space Administration (NASA) It is funded on behalf of DLR by the Federal Ministry of Economics andn Aerospace Centre, grant: 50OK0901) and the National Aeronautics and Space Administration (NASA). It is funded on behalf of DLR by the Federal Ministry of Economics and ermany is coordinated by the German SOFIA-Institute (DSI) of the Universität Stuttgart, in the USA by the Universities Space Research Association (USRA). The development of