1. 1 Stratospheric Observatory for Infrared Astronomy (SOFIA) by E. E. Becklin a, A. G. G. M. Tielens b, R. D. Gehrz c, and H. H. S. Callis a a Universities Space Research Association, NASA Ames Research Center b Code SST, NASA Ames Research Center, Moffett Field, CA c Department of Astronomy, University of Minnesota

2. 2 Outline Infrared (IR) Astronomy and SOFIA Science Objectives Description of the Observatory and Project Status Instrument Complement and Performance Characteristics Anticipated Science Highlights Summary

3. 3 Infrared Physics IR = 1 µm ≤ ≤ 1000 µm (yellow light = 0.5 µm)  3K ≤ T ≤ 3000 K

4. 4 Blackbody Physics and Infrared Astronomy IR = 1 µm ≤ ≤ 1000 µm  3K ≤ T ≤ 3000 K

5. 5 Infrared Astronomy and the Chemical Evolution of the Universe

6. 6 Key Science Topics How stars form in our galaxy and other nearby galaxies Chemistry, Mineralogy, and Biology Solar System studies Targets of Opportunity, for example: –Bright Comets –Eruptive variable stars –Galactic and LMC/SMC classical novae –Supernova in our galaxy or other nearby galaxies –Eclipses and Occultations in the Solar System

7. 7 Above 99% of the water vapor Transmission at 14 km >80% from 1 to 800 µm Instrumentation: wide variety, rapidly interchangeable, state-of-the art Mobility: anywhere, anytime Twenty year design lifetime A near-space observatory that comes home after every flight The Advantages of SOFIA

8. 8 SOFIA Overview 2.5 m (98 inch) telescope in a modified Boeing 747SP aircraft –Optical to millimeter-wavelengths –Emphasis on the obscured IR (30-300  m) Operating altitude –39,000 to 45,000 feet (12 to 14 km) –Above > 99% of obscuring water vapor Joint Program between the US (80%) and Germany (20%) First Light Science 2009 –20 year design lifetime –Science Ops at NASA-Ames and Flight Ops at NASA-Dryden –Deployments to the Southern Hemisphere and elsewhere –>120 8-10 hour flights per year –Built on NASA Lear/Kuiper Airborne Observatory Heritage

9. 9

10. 10 Primary Mirror M1 M2 M3-1 M3-2 Focal Plane Focal Plane Imager Pressure bulkhead Nasmyth tube Spherical Hydraulic Bearing Nasmyth: Optical Layout

11. 11 The Un-Aluminized Primary Mirror Installed

12. 12 Unique Science Capabilities 8 arcmin diameter FOV allows use of very large detector arrays Image size is diffraction limited beyond 15 µm, making images 3 times sharper than Spitzer Space Telescope Because of large aperture and better detectors, sensitivity for imaging and spectroscopy will be similar to the space observatory ISO Ability to adapt to new technologies Ability to track temporal events

13. 13 SOFIA’s Instrument Complement As an airborne mission, SOFIA supports a unique, expandable instrument suite SOFIA covers the full IR range with imagers and low, moderate, and high resolution spectrographs 4 instruments at IOC; 9 instruments at FOC SOFIA can take full advantage of improvements in instrument technology Both Facility and PI Instruments

14. 14 SOFIA Performance: Spectral Resolution of the First Generation Science Instruments FORCAST SPITZER IRS IRAC MIPS

15. 15 Four First Light Instruments Working/complete HIPO instrument in Waco on SOFIA during Aug 2004 Working/complete FLITECAM instrument at Lick in 2004/5 Working FORCAST instrument at Palomar in 2005 Successful lab demonstration of GREAT in July 2005

16. 16 Star and Planet Formation SOFIA’s unique high resolution spectrographs can determine the abundances and chemical routes of organic and pre-biotic molecules : The organic inventory of newly forming planetary systems The spatial distribution of water and the “snow-line” in proto- planetary systems NASA strategic sub-goal 3D.3 SOFIA will study the molecular composition of regions of star and planet formation Spectroscopy can reveal the presence of water, simple hydrocarbon molecules, and complex nitrogen-bearing organics

17. 17 Occultation astronomy with SOFIA Pluto occultation lightcurve observed on the KAO (1989) probes the atmosphere SOFIA can fly anywhere on the Earth, allowing it to position itself under the shadow of an occulting object. Occultation studies with SOFIA will probe the sizes, atmospheres, and possible satellites of Kuiper Belt Objects and newly discovered planet-like objects in the outer Solar System. The unique mobility of SOFIA opens up some hundred events per year for study compared to a handful for a fixed observatory. SOFIA’s mobility also enables study of comets, supernovae and other serendipitous objects. SOFIA will study stellar occultations

18. 18 Resolving Star Formation: Spitzer & SOFIA Antennae Galaxies IRAC at 8  m (red; 160s, 4’ x 4’) FORCAST at 24  m Henize 206- LMC high mass star formation MIPS at 24 µm (80s, 20’ x 20’) HAWC at 53 / 89 µm (mosaic) NASA/JPL-Caltech/Z. Wang NASA/JPL-Caltech/V. Gorjian

19. 19 Evolution of the Universe Atmospheric transmission around the HD line at 40,000 feet Only the high resolution spectrograph on SOFIA can measure the deuterium abundance throughout our galaxy and answer questions about: The abundance of deuterium and its variation with the local star formation rate in galaxies. What the deuterium abundance tells us about the Big Bang and about the star formation history of galaxies? Deuterium is created in the Big Bang, and the primordial deuterium abundance provides the best constraint on the mass density of baryons in the universe. However, the Big Bang deuterium record is modified by stellar nuclear burning. SOFIA will study the deuterium abundance in the galaxy, investigating the evolution of the universe

20. 20 Classical Nova Explosions

21. 21 R. D. Gehrz, et al. 2005, ApJ, in preparation [PID 124] Spitzer Spectra of Nova V382 Vel IRS Short-High IRS Long-High IRS Short and Long-High Spectra: Abundances and Kinematics H I [Ne II][Ne V][Ne III] [Ne V] [O IV][Ne III]

22. 22 The aircraft has flown in April 2007 and is now at NASA Dryden FRC for flight certification tests Early Science is expected to occur in 2009 Two instruments have been selected for Early Science - FORCAST: a US 5-40 μm imager - GREAT: a German heterodyne 60 to 200 μm Spectrometer - Both have been tested in the lab or on a telescope Early Science with SOFIA

23. 23 NASA Ames and USRA are ramping up for Observatory operations. Please visit the SOFIA booth or web site ( http://www.sofia.usra.edu/) for Job opportunities. http://www.sofia.usra.edu/ There will be community involvement in the Early Science Program. We will hold a “SOFIA’s 2020 Vision” Workshop at Caltech, December 6-8, 2007 – long term science We will hold a “SOFIA Early Science” Workshop at the January AAS meeting in Austin, TX, January 8, 2008 Preparations for Science Operations and Community Task Force Activities

24. 24 SOFIA Airborne! 26 April 2007, L-3 Communications, Waco Texas: SOFIA takes to the air for its first test flight after completion of modifications

25. 25 Summary SOFIA has unique spectral and temporal coverage –Unique high-resolution spectroscopy: 28 < l < 150 μm –(l/10 μm) arc-sec image quality, unique for 30 < l < ~60 μm –Unique ability to obtain coverage of transient events –Unique long operating lifetime SOFIA will increase its unique complement of capabilities in the future and will be a test-bed of technologies for future Far-IR missions –State-of-the-art large format IR detector arrays –Polarimeteric imaging and spectroscopy SOFIA is a hands-on Far-IR observatory –Will train future mission scientists and instrumentalists

26. 26 Appendices

27. 27 The Initial SOFIA Instrument Complement HIPO: High-speed Imaging Photometer for Occultation FLITECAM: First Light Infrared Test Experiment CAMera FORCAST: Faint Object InfraRed CAmera for the SOFIA Telescope GREAT: German Receiver for Astronomy at Terahetz Frequencies CASIMIR: CAltech Submillimeter Interstellar Medium Investigations Receiver FIFI-LS: Field Imaging Far-Infrared Line Spectrometer HAWC: High-resolution Airborne Wideband Camera EXES: Echelon-Cross -Echelle Spectrograph SAFIRE: Submillimeter And Far InfraRed Experiment

28. 28 SOFIA’s 9 First Generation Instruments * Listed in approximate order of expected in-flight commissioning % Operational (August 2004) § Uses non-commercial detector/receiver technology Science 4.5-28.3

29. 29 Science Objectives Major Science Programs for SOFIA: –Origin of stars and planetary systems –Planetary bodies that make up our Solar System –Life-cycle of dust and gas in galaxies –Composition of the molecular universe –Role of star formation and black hole activity in the energetics of luminous galaxies SOFIA has a unique suite of instruments that cover a wide range of wavelengths at a wide range of spectral resolution. SOFIA will be continuously upgraded with new instrumentation and will serve as an important technology development platform for future space missions. SOFIA is a highly visible icon for education and public outreach and will immerse educators in the scientific process.

30. 30 Current Activities of the SCTF Workshop during 6-8 December, 2007, at Caltech: "SOFIA’s 2020 Vision: Scientific and Technological Opportunities.” The LOC and SOC have been empanelled and are working. The first “SOFIA Community Task Force Workshop” will be held at the 211th AAS Meeting in Austin, TX on Tuesday January 8, 2008. Planning is underway. Formation of a subcommittee of general experts to advise the project on the contributions SOFIA can make to currently acknowledged outstanding scientific problems.