1. The Stratospheric Observatory for Infrared Astronomy (SOFIA) B-G Andersson SOFIA Science Operations Manager Universities Space Research Association (USRA) Dust and Ice, March 30, 2010

2. March 30, 2010B-G Andersson 2 Outline This is SOFIA SOFIA Capabilities Science Highlights SOFIA for the professional Astronomer SOFIA Instrument Development/Asilomar 2010 workshop

3. March 30, 2010B-G Andersson 3 SOFIA Overview Stratospheric Observatory for Infrared Astronomy 2.5 (2.7)m telescope in a modified Boeing 747SP aircraft –Imaging and spectroscopy from 0.3  m to 1.6 mm –Emphasizes the obscured IR (30-300  m) Operational Altitude –39,000 to 45,000 feet (12 to 14 km) –Above > 99.8% of obscuring water vapor Joint Program between the US (80%) and Germany (20%) –First Light in 2010 –20 year design lifetime –can respond to changing technology –Ops: Science at NASA-Ames; Flight at Dryden FRC (Palmdale- Site 9) –Deployments to the Southern Hemisphere and elsewhere –>120 8-10 hour flights per year As is standard for NASA observatories – proposals open to US and non-US observers

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6. March 30, 2010B-G Andersson Dec. 1, 20096

7. March 30, 2010B-G Andersson 7 Primary Mirror M1 M2 M3-1 M3-2 f/19.6 Focal Plane Focal Plane Imager Pressure bulkhead Nasmyth tube Spherical Hydraulic Bearing Observers in pressurized cabin have ready access to the focal plane Nasmyth: Optical Layout

8. March 30, 2010B-G Andersson 8 Back End of the SOFIA Telescope SOFIA Science Vision Blue Ribbon Panel Review October 24, 2008

9. March 30, 2010B-G Andersson 9 The SOFIA Observatory open cavity (door not shown) TELESCOPE pressure bulkhead scientific instrument (1 of 9) scientist stations, telescope and instrument control, etc. Educators work station

10. March 30, 2010B-G Andersson 10 SOFIA Overview, cont. “Great Observatory” - like operations –User support –Data Analysis and Archive Usage grants (US based investigators) –Planning and observing tools –Comprehensive, on-line archive –Pipeline processing (being developed) Integrated Education and Public Outreach program –EPO staff to support users and educators –Airborne Ambassador program (flying with specific astronomers) –Planet Partners

11. March 30, 2010B-G Andersson 11 Why Air(Space)-borne Observatories for the IR? Even at the very best ground-based sites, the transmission in the mid- to far- infrared is poor or nonexistent Cool dust, light molecule rotation lines, atomic fine- structure lines etc., in this range provide unique tracers

12. March 30, 2010B-G Andersson 12 SOFIA Above 99.8% of the water vapor Transmission at 14 km >80% from 1 to 800 µm; emphasis on the obscured IR regions from 30 to 300 µm Instrumentation: wide variety, rapidly interchangeable, state-of- the art - Instrument suite to be regularly updated/upgraded Platform for testing technology and training observers Mobility: for transient events Twenty year design lifetime: enables long-term temporal studies Why SOFIA? Space vs. sub-orbital Aircraft +Replenish consumables +Technology upgrades +Cutting edge applications +Training of instrumentalists But: –“Human rated” –Fuel cost Spacecraft +Above all the atmosphere +Low stable background +More observing time per year But: –Launch cost –Mass and volume limitations –“Space qualified” technology –No “second chances” WIRE HST (-COSTAR/SM 1-4) ASTRO-E

13. March 30, 2010B-G Andersson 13 SOFIA Capabilities

14. March 30, 2010B-G Andersson 14 Already in 1:st gen.: wide complement of instruments

15. March 30, 2010B-G Andersson 15 SOFIA Photometric Sensitivity

16. March 30, 2010B-G Andersson 16 SOFIA Angular Resolution So, SOFIA is about as sensitive as ISO, and will increase effective sensitivity through future large-area arrays Easier mapping than Herschel SOFIA is diffraction limited beyond 25 µm and can produce sharper images than Spitzer

17. March 30, 2010B-G Andersson 17 Science Highlights

18. SOFIA Highlights Dust photometry Refractory and Ice Spectroscopy Polarimetry (second generation) –Magnetic fields of cores –Spectropolarimetry B-G AnderssonMarch 30, 2010 18

19. March 30, 2010B-G Andersson 19 Thermal Emission from ISM Gas and Dust SOFIA is the only mission in the next decade that is sensitive to the entire Far-IR SED of a galaxy that is dominated by emission from the ISM excited by radiation from massive stars and supernova shock waves The SED is dominated by PAH emission, thermal emission from dust grains, and by the main cooling lines of the neutral and ionized ISM NGC2024 Kandori, R., et al. 2007, PASJ, 59, 487 Spectral Energy Distribution (SED) of the entire LMC (courtesy of F. Galliano)

20. March 30, 2010B-G Andersson 20 Already in 1:st gen.: wide complement of instruments

21. March 30, 2010B-G Andersson 21 The Diversity of Stardust Kandori, R., et al. 2007, PASJ, 59, 487 ISO SWS Spectra: stardust is spectrally diverse in the regime covered by SOFIA Studies of stardust mineralogy Evaluation of stardust contributions from various stellar populations Implications for the lifecycle of gas and dust in galaxies Herbig AeBe Post-AGB and PNe Mixed chemistry post-AGB C-rich AGB O-rich AGB Mixed chemistry AGB Deeply embedded YSO HII region refection nebulae

22. Interstellar Ices Interstellar ices may –Contain significant reservoirs of some elements/species (O) –Allow for chemical evolution not possible in gas- phase reactions B-G AnderssonMarch 30, 2010 22

23. Resolving Power: Gas Phase vs. Solid State Examples of observed IR features: vibration-rotation bands of gaseous CO and pure vibrational features of solid CO and CO 2. [ISO SWS data; van Dishoeck et al.] Examples of observed IR features: vibration-rotation bands of gaseous CO and pure vibrational features of solid CO and CO 2. [ISO SWS data; van Dishoeck et al.] B-G AnderssonMarch 30, 2010 23 RESOLVING POWERS NEEDED TO EXTRACT ALL INHERENT INFORMATION RESOLVING POWERS NEEDED TO EXTRACT ALL INHERENT INFORMATION Feature R = /  Broad solid Features ~ 100 – 500 Narrow solid features + subfeatures ~ 500 – 2000 Gaseous vibration- rotation bands ≥ 10 4

24. March 30, 2010B-G Andersson 24 Already in 1:st gen.: wide complement of instruments

25. FIR Polarimetry (Instr. Gen. “1.5”): What’s the Role of Magnetic fields in Star Formation? B-G AnderssonMarch 30, 2010 25 SHARP SMA straight part of the hourglass seen by SHARP (Attard et al. ‘09) “waist” of the hourglass seen by SMA (Girart et al. ‘06) “…at [the Class 0 phase] magnetic fields dominate over turbulence as the key parameter to control the star formation process.”

26. FIR multi-band Polarimetry – Grain Alignment B-G AnderssonMarch 30, 2010 26 T A > T B, p A < p B,  A ~  B OR T A ~ T B, p A  B Tenuous Cloud 2.0 Radiative grain alignment model in starless clouds: Nearly all grains exposed to same ISRF Large grains are more efficiently Large grains cool more efficiently  Colder grains better aligned than warm grains Radiative torques in cores with embedded stars: Grains near stars aligned Grains far from stars not well-aligned  Warm grains better aligned than cool grains Vaillancourt et al.

27. B-G AnderssonMarch 30, 2010 27 Ices sublimate at characteristic depths H 2 O: A V ~3.5 mag. CO: A V ~5.5 mag. Measuring the polarization in the ice lines allow us to probe the magnetic field selectively “inside” these depths. Comparing opacity and polarization spectra can provide information on the refractory-to-ice volume ratio Whittet et al. 1989 Probing 3D Magnetic Fields Though Ice Line Polarimetry ( 2:nd Gen. Inst.)

28. March 30, 2010B-G Andersson 28 Nebulae and PDRs Fine structure lines from C II O I N II High-J lines of CO PAH lines

29. March 30, 2010B-G Andersson 29 PDR diagnostics adapted from Kaufman et al. 1999, ApJ, 527, 795

30. March 30, 2010B-G Andersson 30 Comets: Mineral Grains What can SOFIA observations of comets tell us about the origin of the Solar System? Comet dust mineralogy: amorphous, crystalline, and organic constituents Comparisons with IDPs and meteorites Comparisons with Stardust Only SOFIA can make these observations near perihelion The vertical lines mark features of crystalline Mg-rich crystalline olivine (forsterite) ISO Data Spitzer Data

31. SOFIA Occultation Studies of Objects in our Solar System SOFIA can probe the sizes, structures (rings), and atmospheres of solar system bodies by measuring how they occult background stars Toward Occulted Star Motion of Occulting Object Shadow of Occulting Object Earth Object SOFIA is uniquely suited for this because it can deploy over most of the Earth to be in the right place at the right time: Can pick from hundreds of events each year

32. March 30, 2010B-G Andersson 32 SOFIA Science Plus: All the great, smart, applications that we didn’t think of, but that YOU will!

33. March 30, 2010B-G Andersson 33 Early General Investigator Opportunities Open Door Flights began at Palmdale in late 2009 First light images are planned for April 2010 Short Science in 2010 with FORCAST (5-40 μm imager) and GREAT (Heterodyne 60 to 200 μm Spectrometer) –P–Proposals are in and teams have been selected –V–Very limited number of flights (~3) –G–GI’s will not fly Basic Science for GIs in 2011 with FORCAST and GREAT –D–Draft call was released in Jan 2009 –F–Final call to be released in April 2010, proposals due July 2 –L–Longer period (~15 Flights) Full science operations begin in 2014

34. March 30, 2010B-G Andersson 34 Instrument Development Second Generation Instruments are about to be solicited. –AO from NASA HQ likely to be issued in early 2011 –Open to all applications Watch for AO or contact Paul Hertz at NASA HQ. Workshop to discuss the community’s view to be held at Asilomar (Monterey peninsula, CA), June 6-8, 2010 Invited review talks Contributed posters –Large amounts of poster viewing time scheduled

35. March 30, 2010B-G Andersson 35 Please join us at Asilomar this June 6-8!

36. March 30, 2010B-G Andersson 36 Summary SOFIA is an airborne, major IR observatory Close to first light and first science Exciting Science, also in the Herschel/post-Spitzer era Many opportunities for involvement both for observers, instrument builders and educators.

37. March 30, 2010 Backup slides B-G Andersson 37

38. March 30, 2010B-G Andersson 38 Asilomar 2010 Logistics Asilomar is a former YMCA/YWCA retreat built in “Arts & Crafts” style Now a California state park Registration deadline April 2 No Registration Fee Lodging and Food (booked via the Asilomar web page): –Three meals a day included in –Several different lodging options available at Asilomar Asilomar is easily reached from the San Jose or San Francisco airports

39. Target features by instrument B-G AnderssonMarch 30, 2010 39 SOFIA Instrument Useful range R  Target features FLITECAM grism mode 2 – 5  m 2000N-bearing ices (ammonia, nitriles, cyanates) C–H stretch region (ices, organics) CO-bearing ices; 13CO/CO ratio FORECAST grism mode 5 – 40  m 200Water-ice bending mode Carbonyl features in kerogens and ices Other key ice features (CH3OH, NH3, etc.) Silicate dust FIFI-LS 40 – 80  m 3000Water-ice EXES 5 – 28  m 10 3 – 10 5 Fine structure in solid state features Gas phase abundances; gaseous CO survey of targets with solid CO detections

40. March 30, 2010B-G Andersson 40 Venus has not been thoroughly explored with broadband, high resolution spectroscopy -- Venus off-limits to Herschel D/H ratio indicates Venus lost an ocean -- Missing piece of evidence: where’s the O? -- Basic atmospheric chemical network not understood. Observations of atmospheric composition variability (esp. SO 2, SO) can constrain possibility of ongoing intermittent volcanic(?) activity Stratospheric super-rotation not understood GREAT Venus; Earth’s poorly understood “sister”

41. March 30, 2010B-G Andersson 41 SOFIA Observing for the community SOFIA Instruments come in three flavors: –Facility Class Science Instruments (FSI) Fully supported Based at the Science Center FLITECAM, FORCAST, HAWC (FIFI LS) –Principle Investigator Science Instruments (PSI) Based at builder’s institution Supported by PI Generally available without pre-proposal CASIMIR, EXES (GREAT) –Special Science Instruments (SSI) Requires collaboration with the instrument PI HIPO Full pipeline processing for FSI & PSI being developed

42. March 30, 2010B-G Andersson 42 SOFIA User Support Science Center at NASA Ames Tools for proposal development & preparation User Support scientists Part of the Edwin Hubble Fellowship program http://www.sofia.usra.edu

43. B-G AnderssonMarch 30, 2010 43 Example SOFIA Coverage: Orion contour: pointings where  (P) < 0.3% in 4 minutes with SOFIA KAO polarization map: Schleuning (1998)

44. March 30, 2010B-G Andersson 44 The Galactic Center Extremely high opacity region Opaque in Visual and NIR Harbors Super Massive Black Hole AGN? green 3.6 μm, blue 8.0 μm (IRAC) & red 24 μm (MIPS)

45. March 30, 2010B-G Andersson 45 Stellar of non-thermal heating in the GC? from Spaans & Meijerink 2008, ApJL, 678, L5

46. March 30, 2010B-G Andersson Dec. 1, 200946 SOFIA: First Generation Instruments InstrumentDescription λ range (μm) resolution (λ/Δλ) Institution PI FORCASTMid-IR camera and grism 5 - 40 R ~ 200 Cornell T. Herter GREATHeterodyne spectrometer 60 - 200 R = 10 6 - 10 8 MPIfR, Kosma R. Güsten FIFI LSImaging grating spectrometer 42 - 210 R = 1000 - 3750 MPE Garching A. Poglitsch HIPOPhotometer for occultation0.3 - 1.1 Lowell Obs. E. Dunham FLITECAMNear-IR camera and grism 1 - 5 R ~ 2000 UCLA I. McLean CASIMIRHeterodyne spectrometer 200 - 600 R = 3x10 4 - 6x10 6 Caltech J. Zmuidzinas HAWCFar-IR bolometer camera50 - 240 U. Chicago D. Harper EXESEchelon spectrometer 5 - 28 R = 10 5, 10 4, 3000 UT/UC Davis/Ames M. Richter

47. March 30, 2010B-G Andersson 47 Asilomar 2010 Topics and Invited Speakers Science Topics ISM Energetics & Magnetic FieldsEli Dwek (NASA GSFC) Dust, including PAH, Ices & MineralogyXander Tielens (Leiden U.) Molecular AstrophysicsDavid Neufeld (Johns Hopkins U.) The Galactic CenterPaul Ho (CfA) Extragalactic Star Formation/StarburstsEva Schinnerer (MPA) Line Diagnostics of the Intermediate-z UniverseGeorge Helou (IPAC) High-mass Star FormationJohn Bally (U. Colorado) Post-Main Sequence Stars, CSEsSun Kwok (U Hong Kong) ExoPlanetsDrake Deming (NASA GSFC) Solar System AstronomyDale Cruikshank (NASA ARC) Workshop SummarySteven Beckwith (U. California) Programmatic Topics NASA’s ViewJon Morse (NASA HQ) NASA 2nd Gen. SOFIA Inst. AOPaul Hertz (NASA HQ) Title TBDAlios Himmes (DLR) Welcome and SOFIA StatusErick Young (USRA) SOFIA 1st Generation InstrumentsEric Becklin (USRA)

48. March 30, 2010B-G Andersson Dec. 1, 200948 Orion region left: view at visual wavelengths right: far-infrared view An object can look radically different depending on the type of light collected from it: An object can look radically different depending on the type of light collected from it:

49. March 30, 2010B-G Andersson Dec. 1, 200949 Stellar Birth and Death Star Formation Late Stages of Stellar evolution

50. March 30, 2010B-G Andersson Dec. 1, 200950 Education Programs AAA = Airborne Astronomy Ambassadors Teams of formal & informal educators & select amateur astronomers Partnered by E&PO with consenting researcher teams, Involved in flight series w/ research partners Supported by E&PO after flights to enhance local education PP = Planet Partners Individuals or teams of educators Partnered by E&PO with SOFIA scientists in their local areas Not trained for flights SFW = Summer Faculty Workshops For college and university educators not involved in research Aimed especially at participants from institutions of under-served populations Can be coupled with REU program (below) REU = Research Experience for Undergraduates Summer fellowships at Ames (NSF-sponsored program) For select undergraduates Exposure to front-line science and engineering research

51. March 30, 2010B-G Andersson Dec. 1, 200951 SOFIA E&PO Components “Built in” to observatory from the very beginning Support for “Formal” (classroom) education Enrichment for educators Training and flights Partnerships with local SOFIA scientists summer workshops Production and dissemination of curricula Support for “Informal” education (museums, etc.) Science centers, Planetaria, etc. Public Outreach Public displays (e.g. air shows), conference displays, etc.

52. March 30, 2010B-G Andersson Dec. 1, 200952 It’s 3 AM onboard the KAO... Scientists Teachers Reporter Mission Director FOSTER Flight Staff Based/modeled on the KAO FOSTER flight program FOSTER = Flight Opportunities for Science Teacher EnRichment