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Jackie Davidson Jackie Davidson
(USRA SOFIA Project Scientist)(USRA SOFIA Project Scientist)
http://sofia.arc.nasa.gov
SOFIAStratospheric Observatory for Infrared Astronomy
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SOFIA Characteristics• Wavelength range: UV - Radio (0.3µm - 1600µm) as defined by
the atmosphere above flight altitude.
Traub & Stier (1976)
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SOFIA Characteristics• Wavelength range: UV - Radio (0.3µm - 1600µm) as defined by the
atmosphere above flight altitude.
• Platform & Operating Altitude: Boeing 747SP; @ 37,000 - 45,000 ft
• Optical configuration: Bent Cassegrain with oscillating secondary mirror and flat folding tertiary mirror.
• Primary Mirror Ø: 2.7m (Aperture 2.5 m)
• Telecope emissivity: < 10% @ 10 µm (without dichroic tertiary)– Optical transmission: > 90% (without dichroic tertiary)
• Operating temperature: 240 K
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Observatory LayObservatory Lay--outout
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SOFIA Cavity - Waco January 2003
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Telescope in Aircraft
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Suspension Assembly (SUA) of
Telescope -Augsburg May 2002
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Installation of SUA - Waco February 2003
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Installing the Telescope Metering Structure-Waco May 2003
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Representative Chet Edwards - June 2003
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Primary Mirror Cell Installation - Waco July 2003
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Primary Mirror - France 2002
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Science Instrument Mounting Flange Installation - April 2003Cabling - ongoing; Photo ~ September 2003
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Clean SOFIA after Pressure Proof Test of the Aircraft Fuselage - Waco April 2004
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Cavity Door - Being assembled at Ames
Shear Layer Control
Flex Skirt
Cavity Door
Rigid ExternalDoor
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SOFIA Characteristics• Wavelength range: UV - Radio (0.3µm - 1600µm) as defined by the
atmosphere above flight altitude.
• Platform & Operating Altitude: Boeing 747SP; @ 37,000 - 45,000 ft
• Optical configuration: Bent Cassegrain with oscillating secondary mirror and flat folding tertiary mirror.
• Primary Mirror Ø: 2.7m (Aperture 2.5 m)
• Telecope emissivity: < 10% @ 10 µm (without dichroic tertiary)– Optical transmission: > 90% (without dichroic tertiary)
• Operating temperature: 240 K
• Visible image quality*: 80% energy within 5.3 arcseconds (first year)
80% energy within 1.6 arcseconds (by third year)
* Includes the effects of pointing jitter but not shear-layer seeing
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1
10
100
1 10 100 1000
Angular ResolutionD
iam
eter
(arc
sec)
Wavelength (µm)
SOFIA
KAO
ISO
IRAS
SIRTF
Herschel
SOFIA will open a new regime of FarSOFIA will open a new regime of Far--IR angular resolutionIR angular resolution
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Information on SOFIA Science Instruments:http://sofia.arc.nasa.gov
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SOFIA First-Light Science Instrumentshttp://sofia.arc.nasa.gov
10 0
10 1
10 2
10 3
10 4
10 5
10 6
10 7
10 8
1 10 100 1000Wavelength [µm]
Spec
tral
res
olut
ion
HIPO (
FLITECAM
FORCAST
EXES
HAWC
SAFIREFIFI LS
GREAT
CASIMIR
102410242225625622
12x3212x321024102422
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SOFIA Performance:
Herschel
10 -5
10 -4
10 -3
10 -2
10 -1
10 0
10 1
10 2
10 3
0. 1 10 100 1000
Photometric Sensitivity
Phot
omet
ric
Sens
itivi
ty1
Sigm
a, 1
hr,
Flu
x D
ensi
ty (m
Jy)
Wavelength (µm)
SOFIA
KAO SIRTF
ISO
IRAS
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SOFIA naturally complements Spitzer
• Spitzer observes faint sources only– Detectors too sensitive for bright sources
• SOFIA covers the bright sources– With good spatial resolution– With great spectral resolution
• i.e., matched to the object being observed
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HAWC
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Circumstellar Disks: Vega
Size of Solar System
SCUBA Beam Size
FORCAST Beam size
HAWC (60)
MIPS-70MIPS (24)
SCUBA 850 µm: rdisk~20" (160AU) ⇒ Tdust~ 80 K⇒ λpeak ~ 35 µm
ISO observed λpeak~35 µm ⇒little dust at r < 160 AU ⇒
hole in distribution
38 µm
Flux
(Jy)
Wavelength (µm)
Heinrichsen et al.1998 FORCAST: Resolve disk and hole ⇒ distribution of dust…
and planets?
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Protostellar/Stellar Detectability with FORCAST
0.0001
0.001
0.01
0.1
1
10 100 1000 10000
Temperature (K)
L/L_
sun
5.6127.68819.5330.6837.65 - 928 - 38
Wavelength
d = 140 pcS/N = 5 in 3600 sec0.63" image quality
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SOFIA First-Light Science Instruments
10 0
10 1
10 2
10 3
10 4
10 5
10 6
10 7
10 8
1 10 100 1000Wavelength [µm]
Spec
tral
res
olut
ion
HIPO
FLITECAM
FORCAST
EXES
HAWC
SAFIREFIFI LS
GREAT
CASIMIR
For R=1000, at 100 um, 1For R=1000, at 100 um, 1--sigma, sigma, 1 hr limit is ~ 3x101 hr limit is ~ 3x10--1818 W/mW/m22
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SOFIA First-Light Science Instruments
10 0
10 1
10 2
10 3
10 4
10 5
10 6
10 7
10 8
1 10 100 1000Wavelength [µm]
Spec
tral
res
olut
ion
HIPO
FLITECAM
FORCAST
EXES
HAWC
SAFIREFIFI LS
GREAT
CASIMIR
Planetary AtmospheresPlanetary Atmospheres
Planetary AtmospheresPlanetary AtmospheresChemistry of the cold ISMChemistry of the cold ISM
Comet MoleculesComet Molecules Dynamics of the Galactic CenterDynamics of the Galactic Center
Dynamics of collapsing Dynamics of collapsing protostarsprotostars
Velocity structure and gas composition in Velocity structure and gas composition in disks and outflows ofdisks and outflows of YSOsYSOs
Composition/dynamics/physics of the Composition/dynamics/physics of the ISM in external galaxiesISM in external galaxiesPAH & organic moleculesPAH & organic molecules
Nuclear synthesis in supernovae in nearby galaxiesNuclear synthesis in supernovae in nearby galaxies
Composition of interstellar grainsComposition of interstellar grains
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Low-Mass Star Formation
SOFIA farSOFIA far--IRIRbeam diameterbeam diameter
for Taurus for Taurus
Hollenbach, Ceccarelli, Neufeld, and Teilens (1995)
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GREAT - CO(J>13) lines in inner most regions of circumstellar envelopes
(R=λ/∆λ ~ 104) Mrate =10-5 Mo /yr
OH OH (accretion shock)(accretion shock)
High-J CO lines -> measure acceleration ofinfalling gas
Hollenbach, Ceccarelli, Neufeld, and Teilens (1995)
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Spectroscopic Capabilities, 2003 - 2025
10 0
10 1
10 2
10 3
10 4
10 5
10 6
10 7
10 8
1 10 100 1000Wavelength [µm]
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
SOFIA SOFIA -- 2006, 20072006, 2007
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Spectroscopic Capabilities, 2003 - 2025
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
SpitzerSpitzer
SOFIA SOFIA -- 2006, 20072006, 2007Spitzer Spitzer -- 2003 to 20082003 to 2008
10 8
10 7
10 6
10 5
10 1
10 0
1 100 100010Wavelength [µm]
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Spectroscopic Capabilities, 2003 - 2025
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
SpitzerSpitzerAstroAstro--FF
SOFIA SOFIA -- 2006, 20072006, 2007Spitzer Spitzer -- 2003 to 20082003 to 2008AstroAstro_F _F -- 2004 to 20062004 to 2006
10 8
10 7
10 6
10 5
10 1
10 0
1 100 100010Wavelength [µm]
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Spectroscopic Capabilities, 2003 - 2025
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
HerschelHerschel
SpitzerSpitzerAstroAstro--FF
SOFIA SOFIA -- 2006, 20072006, 2007Spitzer Spitzer -- 2003 to 20082003 to 2008AstroAstro_F _F -- 2004 to 20062004 to 2006Herschel Herschel -- 2007 to 20102007 to 2010
HerschelHerschel
10 8
10 7
10 6
10 5
HerschelHerschel
10 1
10 0
1 100 100010Wavelength [µm]
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Spectroscopic Capabilities, 2003 - 2025
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
HerschelHerschel
SpitzerSpitzer
JWSTJWST
AstroAstro--FF
SOFIA SOFIA -- 2006, 20072006, 2007Spitzer Spitzer -- 2003 to 20082003 to 2008AstroAstro_F _F -- 2004 to 20062004 to 2006Herschel Herschel -- 2007 to 20102007 to 2010JWST(JWST(NGSTNGST) ) -- >2010>2010
HerschelHerschel
10 8
10 7
10 6
10 5
HerschelHerschel
10 1
10 0
1 100 100010Wavelength [µm]
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SOFIA complements Herschel
• Herschel can’t do the whole sky in three years!– Must be selective
• Herschel is a natural for surveys– especially of faint sources (e.g., distant galaxy)
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Blank Field Surveys
100≤160Spitzer (2004)100170-500Herschel (2007)
3200HAWC/SOFIA (2005)0.1350SHARC II/CSO0.31300MAMBO/IRAM0.2850SCUBA/JCMT
galaxies/hour (5σ)λ (µm)Facility
A. Blain
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SOFIA complements Herschel
• Herschel is a natural for lines obscured by Earth’s atmosphere above the tropopause
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Sub-mm on SOFIA
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SOFIA complements Herschel
• SOFIA is a natural for in-depth studies of particular targets– With increased spectral coverage– With increased science instrument capabilities
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Spectroscopic Capabilities
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
HerschelHerschel
SOFIA SOFIA -- 2006, 20072006, 2007Herschel Herschel -- 2007 to 20102007 to 2010
HerschelHerschel
10 8
10 7
10 6
10 5
HerschelHerschel
10 1
10 0
1 100 100010Wavelength [µm]
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Nearby Face-on Spiral Galaxies: M83
6” Resolution CO (1-0) Map overlayed on false-color HI (Rand,
Lord, & Higdon 1999)
SOFIA (& Herschel) will resolve Far-IR Lines and Far-IR continuum Emission from Spiral Arms ⇔ Star Formation and Spiral Density Waves
SOFIA
Visible Image of M83
FORCAST 38 µm beam: 75 pc
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Far-IR Spectral Lines • A host of Far-IR fine-structure and molecular-transition lines, accessible to
SOFIA at optimum spectral resolutions, can probe the physical properties of the ISM of the Milky Way and other galaxies:
• [OI]*, [SiII] lines probe the physical conditions of gas in PDRs.• [NIII], [SIII], and [OIII]* line pairs are excellent probes of HII region
densities.• [NII]* lines trace the warm ionized medium.• [CII]* line traces PDRs, atomic clouds, and warm ionized medium. • [NII]*/[NIII], [SIII]/[OIII]*, [NeIII]/[OIV]/[NeV] ratios give the effective
temperature of stellar or AGN UV radiation fields.• [SI], [SiI]*, [SiII] and [FeI] lines indicate the presence of dissociative J-
shocks.• High J CO* rotational lines trace shocked gas found in warm dense gas of
PDRs.• OH* lines trace shocked gas in cool dense gas.• H2 rotational lines probe the mass of warm molecular clouds.• OH*, CH*, and NH3* together constrain molecular cloud chemistry.
• Lines with “*” are observable from Herschel as well. Herschel cannot observe all of the SOFIA lines. Stacey Stacey
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Watson 1985Watson 1985
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Spectroscopic Capabilities
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
HerschelHerschel
SOFIA SOFIA -- 2006, 20072006, 2007Herschel Herschel -- 2007 to 20102007 to 2010
HerschelHerschel
10 8
10 7
10 6
10 5
HerschelHerschel
10 1
10 0
1 100 100010Wavelength [µm]
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Spectroscopic Capabilities
10 2
10 3
10 4
Spec
tral
res
olut
ion
HIPO
FLITECAM
EXES
SAFIREFIFI LS
GREAT
CASIMIR
HerschelHerschel
SOFIA SOFIA -- 2006, 20072006, 2007Herschel Herschel -- 2007 to 20102007 to 2010SOFIA SOFIA -- 2008 to 20252008 to 2025 HerschelHerschel
FORCASTFORCAST
10 8
10 7
10 6
10 5
HerschelHerschel
10 1
10 0
1 100 100010Wavelength [µm]
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Increasing High Resolution Spectral Capabilities on SOFIA
• Finish SAFIRE (TES array, Fabry-Perot Spectrometer)
• EXES (Echelon Spectrometer)– Increase detector array size from 2562to 10242 Si:As array
• FORCAST (mid-IR camera)– Add Grism to allow for R=2,000 spectroscopy
• GREAT & CASIMIR (heterodyne spectrometers)– HEB mixers and new type of LOs for coverage <200 um– Heterodyne arrays
• Develop R~104 -105 spectral resolving capability spanning from 40 um to 200 um in one spectrometer.
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Increasing other Capabilities on SOFIA
• Use Occultation Cameras (HIPO & FLITECAM)• Add Polarimeters• Expand Wide Field FIR Cameras
– At 100 um, an 8’x 8’ fully sampled array is an 128x128 array
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Detector Array Capabilities
Wolf 2002Wolf 2002
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SOFIA supports the larger IR/SMM Technology Development Community
http://www.sofia.usra.edu/det_workshop/
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Beyond Spitzer & Herschel….• Hopefully new IR/SMM space missions
• BUT also, until the mid- 2020s, a vibrant IR/SMM airborne program (SOFIA) providing– Easy access to the IR/SMM Universe – State-of-the-art IR/SMM science instruments– A source of resources for new IR/SMM technology development– An advocate for the IR/SMM community
• SOFIA is the far-IR community’s “ground-based” observatory with many space-based type capabilities
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So how & when can the community use SOFIA?
• SOFIA will have an annual observing cycle– Call for Proposals will be issued by USRA annually
• Observing will start in January 2006
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Jackie Davidson Jackie Davidson
(USRA SOFIA Project Scientist)(USRA SOFIA Project Scientist)
http://sofia.arc.nasa.gov
SOFIAStratospheric Observatory for Infrared Astronomy