Alf d Alfred The Projekt The Projekt SOFIA - the Stratospheric Observatory For Infrared Astronomy is a project jointly dev SOFIA the Stratospheric Observatory For Infrared Astronomy is a project jointly dev operated by the German Aerospace Center (DLR) and the National Aeronautics and operated by the German Aerospace Center (DLR) and the National Aeronautics and Administration (NASA) SOFIA’s main scientific mission is the observation of the infra Administration (NASA). SOFIA’s main scientific mission is the observation of the infra f S near 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 cruising e approximately 14 km SOFIA will operate above 99 % of the atmospheres water vapo de approximately 14 km SOFIA will operate above 99 % of the atmospheres water vapo velocity of approximately 900 km/h and temperatures of approximately 50°C provide art. velocity of approximately 900 km/h, and temperatures of approximately -50 C provide f i t i l b ti ttga for precise astronomical observations. 9 stut ute 379 ni-s The Telescope titu art 623 .un The Telescope nst tga 31 rt – 6 dsi. The telescope was developed and built by the German Industry under the leadership A I tut g 3 gar 85 – @d The telescope was developed and built by the German Industry under the leadership dK Th d b d f th G A C t (DLR) It i td OFIA f S ring uttg 68 be@ and Kayser Threde by order of the German Aerospace Centre (DLR). It is supported SO y of aldr Stu 1 – abb bearing bearing and will float on a 50 µm thin oil fill in order to be decoupled from the an S sity nwa 69 S 711 Kra aircraft. The telescope can rotate ±3° about all three axes, its elevation is selectable b ma vers fen 056 07 ail: The Vibration Isolation System (VIS) decou Germ niv faff -70 el.: ma The Vibration Isolation System (VIS) decou from the vibration of the aircraft The VIS co 1 G Un Pf D- Te Em from the vibration of the aircraft. The VIS co ti ll tt hd ti i symmetrically attached pneumatic springs o axial and tangential direction each. The pri a final mass of about 800 kg and character coefficient of elasticity The secondary SiC coefficient of elasticity. The secondary SiC about both axes at a frequency up to 20 H about both axes at a frequency up to 20 H t d bt t th b k measurements and subtracts the backgrou translative corrections to center and focus t be used for the flexible body compensation oscillations onto the telesope introduced by oscillations onto the telesope introduced by Current Status Current Status Th N Si C t tk bl The New Science Case – to take away – see below In 2009 the news science vision for SOFIA was compiled Four major area in modern In 2009 the news science vision for SOFIA was compiled. Four major area in modern Galaxies and the Galactic Center SOFIA will investigate the strength and spatial SOFIA will investigate the strength and spatial distribution of star formation in the redshift range distribution of star formation in the redshift range bt 03> > 1 1 th t i i lf th between 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 complex galactic center to understand the complex mechanisms that proceed in this extreme mechanisms that proceed in this extreme i tE th [CII] 158 fi t t environment. E.g. the [CII] 158µm fine – structure transition, which is the most important cooling line of the cold Interstellar medium and therefore critical for its energy balance will be observed and therefore critical for its energy balance, will be observed. Th It t ll M di The Interstellar Medium SOFIA will probe the interstellar medium that is the record all generations of stars that belong to a the record all generations of stars that belong to a galaxy The physical processes on how stars galaxy. The physical processes on how stars interact with their environment the origin of dust interact with their environment, the origin of dust ll th l fl l b as well as the role of large complex carbon molecules will be explored. Hence SOFIA will take one of the deepest views in the regions where one of the deepest views in the regions where stars and eventually planets form stars, and eventually planets form. The Schedule for first science The Schedule for first science 2010: 2010: A il Fi tt hi l li ht ith FORCAST J April - First technical light with FORCAST June - call for basic science (Application from astronomical 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 FORCAST September - First science (Short science) with FORCAST ( bl th Gl ti C t ) (presumably on the Galactic Center) 2011 February - First science (Short science) with GREAT February First science (Short science) with GREAT March-June - Basic science with FORCAST GREAT March-June - Basic science with FORCAST, GREAT 2013 2013 J FLITECAM June - FLITECAM October - HIPO The First Science Instruments The First Science Instruments SOFIA ill h 9 fi t SOFIA will have 9 first gene 7 will be provided by the US by German teams. For the fi (3 US 2 German) instrumen (3 US, 2 German) instrumen SOFIA H hl SOFIA Herschel λλ [μm] 0,3 – 1600 60 – 670 Spiegel ø [m] 2,7 m 3,5 m S 2011 2009/10 Start 2011 2009/10 L f it [J h ] 20 3 Laufzeit [Jahre] 20 3 Ende 2034 /2013 1 Li Fl Li it i 1h i 3 10 18 W/ 2 tR 1 000 t 100 Ende 2034 /2013 1σ Line Flux Limit in 1h is ~3x10 -18 W/m 2 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; Germa SOFIA, the Stratospheric Observatory for Infrared Astronomy is a joint project of the Deutsches Zentrum für Luft und Raumfahrt e.V. (DLR; Germa Technology based on legislation by the German Parliament the state of Baden-Württemberg and the University of Stuttgart. Scientific operation for G the German Instruments is financed by the Max Planck Society (MPG) and the German Research Foundation (DFG). dK bb 1 Dö t M hl t 1 d Krabbe 1 , Dörte Mehlert 1 Platform: Boeing 747SP Platform: Boeing 747SP Telescope mass: 17 000 kg veloped and Telescope mass: 17.000 kg Main mirror diameter: 27m veloped and Space Main mirror diameter: 2,7 m Spectral range : 03 1600 µm Space ared universe from Spectral range : 0,3 - 1600 µm Pointing stability: 0 2 arcsec rms ared universe from f Pointing stability: 0,2 arcsec rms modified and in the g altitude of ur However a ur. However, a e harsh conditions e harsh conditions p of MT Aerospace p of MT-Aerospace b hd t ti by a hydrostatic rotation of the between 15º to 70°. Altitude: ~ 14 km Flights: ~ 160 / year uples the telescope Flights: 160 / year Science: ~ 8 h / night uples the telescope onsists out of 24 Science: 8 h / night Mission duration: 20 years onsists out of 24 h lf ti i Mission duration: 20 years one half acting in imary mirror is a lightweighted ZERODUR structure with rizes by a low coefficient of thermal expansion and a high ceramic mirror has a diameter of 35 cm and can be tilted ceramic mirror has a diameter of 35 cm and can be tilted z with a maximum angle of 8’ It is used for differential z with a maximum angle of 8 . It is used for differential d di ti f th i tifi bj t Additi ll it id nd 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 y the wind load y the wind load. IR Astronomy were identified to be the majorareas 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 Planets SOFIA will focus on the understanding how the most massive SOFIA will focus on the understanding how the most massive stars form These stars greatly impact large areas of the stars form. These stars greatly impact large areas of the l b th i di l hi ht t M galaxy 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 of stars of stars. Planetary Science Comets, near-Earth asteroids, atmosphere-bearing moons Comets, 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 on planets will be investigated with SOFIA and will give hints on h th t tf th t l f lif how the stage was set for the eventual appearance of life on our planet. First open door flight First open door flight D 18th 2009 Envelope expansion flights on Dec. 18th, 2009 - Envelope expansion flights - maintenance maintenance - instrument commission 2008 2009 2010 2011 2012 2013 2014 2015 C t Si T W l th I t t ti i t t Comments Science Type Wavelength- range [ µm] Instrument ration instruments. i lt At h di f l t I 03 06 HIPO range [ µm] partners, 2 are built - simultaneous mount with 2 - Atmospheres and rings of planets (solar system and exoplanets) I - 0,3-0,6 µm 04 1 1 µm HIPO NIR irst science 5 mount with 2. (solar system and exoplanets) - 0,4 – 1,1 µm NIR SP I nts will be available simultaneous T ti i lit I&S 1 5 5 µm FLITECAM SP-I nts will be available. - simultaneous mount with 1 - Testing image quality Spectroscopic complement HIPO I&S - 1 – 5,5 µm FLITECAM NIR mount with 1. - Spectroscopic complement – HIPO - stellar population in SF regions NIR F-I - 9 filters - Dust properties and ionisation sources in the I&S -5-8 µm FORCAST stellar population in SF regions F 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 & FORCAST MIR multi colour imaging galactic center; star formation regions, active galaxies, circum stellar dust envelopes 17 25 µm & 25-40 µm MIR F-I S it JWST - High - Fine structure transitions in ISM; cooling S 1,6 – 1,9 THz GREAT Spitzer JWST High resolution- Fine structure transitions in ISM; cooling processes; energy balance S 1,6 1,9 THz 2,4 – 2,7 THz GREAT FIR 3 – 180 0,6 – 28 submm spectr. - Deuterium abundance > SF history ~ 4.7 THz PI-I 0,85 m 6,5 m 2003 h 2014 [63 – 187 µm] 2003 nach 2014 3 [6] 5 10 -3D imaging! - SF & ISM in galaxies I&S 42 – 110 µm FIFI-LS 3 [6] 5-10 2009 2019 2024 - extragalactic > MW and others (e.g. dwarf; ULIRGs) 110 – 210 µm FIR 2009 2019-2024 > merging / interacting galaxies F-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 and 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 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