Stratospheric Observatory for Infrared Astronomy SOFIA

1
Stratospheric Observatory for Infrared Astronomy
(SOFIA)

• by
• E. E. Becklina, A. G. G. M. Tielensb, R. D.
  Gehrzc,
• and
• H. H. S. Callisa

aUniversities Space Research Association, NASA
Ames Research Center bCode SST, NASA Ames
Research Center, Moffett Field, CA cDepartment
of Astronomy, University of Minnesota
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
Infrared Physics
IR 1 µm ? 1000 µm (yellow light 0.5 µm)
? 3K T 3000 K
4
Blackbody Physics and Infrared Astronomy
IR 1 µm ? 1000 µm ? 3K T 3000 K
5
Infrared Astronomy and the Chemical Evolution of
the Universe
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
The Advantages of SOFIA

• Above 99 of the water vapor
• Transmission at 14 km gt80 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

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 gt 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
• gt120 8-10 hour flights per year
• Built on NASA Lear/Kuiper Airborne Observatory
  Heritage

9
(No Transcript)
10
Nasmyth Optical Layout
11
The Un-Aluminized Primary Mirror Installed
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
SOFIAs 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
SOFIA Performance Spectral Resolution of the
First Generation Science Instruments

• FORCAST

• SPITZER IRS

MIPS
IRAC
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
Star and Planet Formation
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

• SOFIAs 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
17
Occultation astronomy with SOFIA
SOFIA will study stellar occultations
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.
• SOFIAs mobility also enables study of comets,
  supernovae and other serendipitous objects.

18
Resolving Star Formation Spitzer SOFIA
NASA/JPL-Caltech/V. Gorjian
NASA/JPL-Caltech/Z. Wang
Henize 206- LMC high mass star formation MIPS at
24 µm (80s, 20 x 20) HAWC at 53 / 89 µm
(mosaic)
Antennae Galaxies IRAC at 8 mm (red 160s, 4 x
4) FORCAST at 24 mm
19
Evolution of the Universe
SOFIA will study the deuterium abundance in the
galaxy, investigating the evolution of the
universe
Atmospheric transmission around the HD line at
40,000 feet
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.

• 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?

20
Classical Nova Explosions
21
Spitzer Spectra of Nova V382 Vel
R. D. Gehrz, et al. 2005, ApJ, in preparation
PID 124
H I
Ne II
Ne V
Ne III
O IV
Ne III
Ne V
IRS Long-High
IRS Short-High
IRS Short and Long-High Spectra Abundances and
Kinematics
22
Early Science with SOFIA

• 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

23
Preparations for Science Operations and
Community Task Force Activities

• 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.
• There will be community involvement in the Early
  Science Program.
• We will hold a SOFIAs 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

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
Summary

• SOFIA has unique spectral and temporal coverage
• Unique high-resolution spectroscopy 28 lt l lt 150
  µm
• (l/10 µm) arc-sec image quality, unique for 30 lt
  l lt 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
Appendices
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
SOFIAs 9 First Generation Instruments
4.5-28.3
Listed in approximate order of expected
in-flight commissioning Operational (August
2004)
Uses non-commercial
detector/receiver technology
Science
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
Current Activities of the SCTF

• Workshop during 6-8 December, 2007, at
  Caltech "SOFIAs
• 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.