Download - Astronomers Returns to the Stratosphere
Presenter: Name 1
NASA ARC - AIAASeptember 14, 2010
Moffett Field, CA
Presented BySean C Casey
Universities Space Research [email protected]
Stratospheric Observatory forInfrared Astronomy (SOFIA)
Presenter: Sean C. Casey 2
Talk Outline
• Introduction on Airborne Astronomy• Construction of the observatory• SOFIA’s expected science return• Summary
Presenter: Sean C. Casey 3
Astronomy in the Infrared
• Astronomical observatories throughout the EM spectrum• Wavelength is indicative of the energetics
Optical
Presenter: Sean C. Casey 4
Friedrich Wilhelm Herschel 1738 - 1822
The 18th Century Discovery of Infrared Radiation (IR)
Discovered theplanet Uranus!
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21st Century Imaging in the Optical and Infrared
Optical
(What your eye does see.)
Infrared
(What your eye does not see.)
A Collard Lizard
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Astronomy in the Optical and Infrared
Cooled gas and dust emission at T = 10’s – 100’s K
Presenter: Sean C. Casey 7
Interstellar Dust
Carbonaceous and Silicate condensates of the ISM.Particle size produces selective extinction (s+a).
Presenter: Sean C. Casey 8
Looking toward the center of our GalaxyOptical Image
Near-Infrared
Far-Infrared
• Imaging at longer wavelengths– Optical shows only cloud surfaces– Infrared provides diagnostics of obscured environments
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Lifecycle of the ISM
X. Tielens 2006
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Atmospheric Absorption
0.0
0.2
0.4
0.6
0.8
1.0
145 150 155 160 165
C+
R ~ 10,000Observations within the 30 – 300 micron window are only possible from the stratosphere and above.
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Previous and Existing IR Observatories
Ground-based Sub-orbital
IRAS COBE ISO SIRTF
Space-based
KAOMauna Kea
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Kuiper Airborne Observatory : 1974 - 1995>300 investigators, ~50 PhDs, ~40 instruments, ~9000 observing
hours
Important Science results:- Life cycle of gas and dust in the ISM- Recognition of photo-dissociation regions- Numerous far-IR lines OI, CII, FeIV
- PAH emission characteristics- Far-Infrared polarization- Ring of Uranus
Set the scientific stage for the infrared missions: IRAS, ISO, and Spitzer
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Typical instrumentation aboard KAO
Pre-flight checkoutof FIFI on the KAOby A. Poglitsch andTeam (Genzel et al.).
Successful developmentand use of stressed/unstressed germanium photo-conductors in far-IR.
Successful Internationalparticipation
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Astronomy aboard an Airplane
A. Krabbe and H-P. Roeser 1999 “SOFIA Astronomy and Technology in the 21st Century”
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Flight Profiles – Start at 37,000 Feet
• Some research flights may reach duration of 10.5 Science Hours
START, TAXI, TAKEOFFGW 648.0
CRUISE108,000 LBS. FUELF.F. 22,520 LBS/HR4.6 HRS.
37,000 FT.GW 628.0
CRUISE40,000 LBS. FUELF.F. 19,480 LBS/HR.1.9 HRS.
CRUISE40,000 LBS FUELF.F. 18,380 LBS/HR.2.05 HRS.
CRUISE35,000 LBS. FUELF.F. 16,920 LBS/HR.2.05 HRS.
TOTAL FUEL USED – 268,000 LBS.TOTAL CRUISE TIME – 10.6 HRS.
TOTAL FLIGHT TIME – 11.9 HRS.
ASSUMPTIONS
ZFW 380,000 LBS.20,000 LBS. FUEL TO FIRST LEVEL OFFCLIMB TO FIRST LEVEL-OFF AT MAX CRUISE WTSTAY AT ALT. UNTIL FUEL FLOW IS LESS AT STEP CLIMB ALT.1 HRS.FOR EACH STEP CLIMBLANDING WITH 20,000 LBS. FUELBASED ON 747 SP FLIGHT MANUAL TABULATED DATASTANDARD DAY PLUS 10 DEGREES CSPEED-MACH .84
39,000 FT.GW 520.0
41,000 FT.GW 480.0
43,000 FT.GW 440.0
DESCENTGW 405.0
5,000 LBS. FUEL
.5 HRS.
LANDINGGW 400.0
CLIMB.5 HRS.
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Stratospheric Observatory For Infrared Astronomy
747-SP “Clipper Lindbergh”
Aircraft flight tests, circa 1997/8
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SOFIA Attributes
- Wavelength range: “UV to Radio”: 0.3 – 1600 µm
- Mobility: “anywhere, any time”: all sky, ephemeral events
- Primary Mirror: 2.7 m diameter (Aperture 2.5 m)
- Operating Altitude: 12 – 14 km (37,000 - 45,000 feet)
- Design Lifetime: 20 years
- Observing Program: flexible; annual proposal opportunities
- Science Instruments: wide variety, hands-on in-flight, late
latest technologies in new instruments
- Young researchers’ opportunities: scientists and instrumentalists
- Education/Public Outreach: teachers/media/publicSOFIA will be a mobile modern observatory
in the lower stratosphere.
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Angular resolution of SOFIA
HST in optical KAO at 60 µm
SOFIA: KAO Comparison - almost 9 SOFIA beams for every 1 KAO beam
Orion in Optical and Far-infrared
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Education & Public Outreach Section
Mission Control & Science Operation Section
Pressure Bulkhead
Telescope Cavity Door
ScienceInstrument
Cavity Environmental Control System
Telescope 2.7m
SOFIA’s Interior Layout
Open Port Cavity
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SOFIA’s Optical Layout
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Photometric Sensitivity and Angular resolution
SOFIA is diffraction limited beyond 25 µm (θmin ~ λ/10 in arcseconds) and can produce images three times sharper than those made by Spitzer
SOFIA is as
sensitive as ISO
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SOFIA’s Operational Phase Space
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10 0
10 1
10 2
10 3
10 4
10 5
10 6
10 7
10 8
1 10 100 1000Wavelength [µm]
Sp
ectr
al r
esol
uti
on
HIPO
FLITECAM
FORCAST
EXES
HAWC
SAFIREFIFI LS
GREAT
CASIMIR
Planetary AtmospheresPlanetary Atmospheres
Planetary AtmospheresPlanetary Atmospheres
Chemistry of the cold ISMChemistry of the cold ISM
Comet MoleculesComet Molecules Dynamics of the Galactic CenterDynamics of the Galactic Center
Dynamics of collapsing protostarsDynamics of collapsing protostars
Velocity structure and gas composition in Velocity structure and gas composition in disks and outflows of YSOsdisks and outflows of YSOs
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
KBOs, Planet TransitsKBOs, Planet TransitsDebris Disk StructureDebris Disk Structure
Luminosity and Morphology of Star Formation Galactic Luminosity and Morphology of Star Formation Galactic and Extra-Galactic Regionsand Extra-Galactic Regions
SOFIA Science is broadly based
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Current Instruments
Early Science SIs
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SOFIA Instruments
#1
#2
Working/complete HIPO instrument at Lowell Obs. Aug 2004
Working/complete FLITECAM instrument atLick in 2004/5
Working FORCAST instrument at Palomar in 2005
Successful lab demonstration of GREAT in Oct 2005
HAWC flight cryostat testing at Yerkes in 2005
Early science instruments:FORCAST/GREAT
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FORCAST: Mid-IR Imager
PI: T. Herter (Cornell Univ.) [email protected]
Detectors: Dual channel 256 x 256 arrays; 5 – 25 m (Si:As) 20 – 40 m (Si:Sb)
Field of View: 3.2’ x 3.2’
Science: Thermal and narrow band imaging
Targets: Circumstellar disks, Galactic Center,Galactic and extragalactic star formation
NB: Diffraction Limited > 15 microns; Grism upgrade funded (Ennico 2005)
Working FORCAST instrument at Palomar in 2006
Presenter: Sean C. Casey 27
GREAT: Heterodyne Spectrometer
PI: R. Guesten, Max-Planck Institut, [email protected]
R= 106 -> 108
Detector: dual channel mixer (HEB);60 – 200 m (2 – 5 THz)
Science: Spectroscopy of CII (158 m), and HD (112 m)
Targets: Galactic and extragalactic ISM, circumstellar shells
Successful lab demonstration of GREAT in Oct 2005
NB: TA ~ 2500 K at 158 m
High frequency upgrade at 4.7 THz expected for OI (63 m).
Field of View: single element
Presenter: Sean C. Casey 28
SOFIA Aircraft: 747 SP #21441 as proposed by USRA
Christened the “Clipper Lindbergh”by Anne Morrow Lindberghin May 1977 on the 50th anniversary of Lindbergh’s flight across the Atlantic.
Juan Trippe andCharles Lindberghwith Pan Am inmid-1930’s.
Summer ‘97
Observatory Hardware
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2.7 M
Primary Mirror, f/1.28 at SAGEM, circa 2000
RMS = 280 nm
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Aircraft pressure bulk head ’01 (assembly) ’02 (installation)
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Build-up of the DLR telescope components in Germany.
Complete telescope assembly (TA) run with closed-loop servo control using the hydrostatic bearing and gyroscopic control.
Telescope metering structureScience Instrument end of TA
March ‘02
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Telescope arrives in Waco, TX Sept. ‘02
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July ’03 – primary mirror installed
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August ’03 – Telescope installation complete
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March ’04 – Proof pressure test
SOFIA passes test!
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February ‘05 – Test of landing gear
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February ‘06 – Aircraft aperture door complete
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SOFIA Instrument Flange
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SOFIA’s Interior
Aircraft interior Sept. 06
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SOFIA with NASA colors
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SOFIA is Airborne in 2007
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SOFIA at ARC in 2007
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SOFIA at NASA Dryden
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Uncoated Telescope/Incomplete Door
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Finishing the Door
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A coated primary mirror
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Optical telescope tests with HIPO team
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SOFIA Line-Op
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Telescope Testing
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Telescope Close-up
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Telescope for Test Flights
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FORCAST on SOFIA
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SOFIA First Light - Jupiter
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Will SOFIA reveal debris disks @ 37 m?
Wilner et al. model of Vega predicts resolved structure when convolved with SOFIA resolution @ =37 m (LEFT), but Spitzer finds Fomalhaut (RIGHT) and Vega (not shown) amorphous at =24 m. Due to small grains or small inner disk radius?? - ask SOFIA!
?
Vega model SOFIA @37 m Fomalhaut Spitzer MIPS @24 m
72"
FORCAST beam size at 37 m
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Malfait et al. 1998Debris Disk Evolution
VegaFomalhaut Beta Pic
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Segregation of gas & ices around protostars
van Dishoeck & Hogerheijde 1999
W33AGibb et al. 2000
R~2000 FLITECAM and FORCAST (with grisms) observations can reveal constituents & chemistry of protostellar envelopes (except for CO2).
Presenter: Sean C. Casey 57
Occultation astronomy with SOFIA
Pluto occultation lightcurve observed on the KAO (1984) 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 measure stellar occultations
Presenter: Sean C. Casey 58
Transits of Extrasolar Planets
• SOFIA will fly above the scintillating components of the atmosphere and will be the most sensitive freely pointing observatory for extrasolar planetary transits after HST.
• SOFIA will be able to detect weak transit signals with high signal-to-noise, conclusively determining the status of candidate extrasolar planets discovered by transit surveys: long life needed!
HD 209458 artist’s concept (left) and HST STIS data (below)
Presenter: Sean C. Casey 59
The ground-based infrared spectrum of Mars is dominated by broad lines in the Earth atmosphere. A weak feature on the wing of the strong terrestrial methane line may be the Doppler-shifted methane line in the Mars atmosphere. If true, the methane abundance is very high and may reflect biogenic activity.
The high resolution spectrograph on SOFIA can probe between the much narrower terrestrial lines at airborne altitudes and uniquely address:
• Is there methane in the Martian atmosphere?
• If so, where does it come from? What is it global distribution? How does it vary with the seasons on Mars?
SOFIA will study planetary atmospheres
Planetary Atmospheres
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Phillips 1988
Astrochemistry
• Most molecular lines in IR or submillimeter– Need high spectral resolution
throughout the submillimeter
• As sensitive as CSO, but complete wavelength range is accessible– H2, C2H2,CH4 only in IR
• The fullerene, C60, has 4 IR lines in SOFIA’s bands
• Light molecules: Hydrogen, water, other hydrides in IR and submillimeter
• HD at 112 microns
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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:
• What is the abundance of deuterium and how does it vary with the local star formation rate in galaxies?
• What does that tell us about the Big Bang and about the star formation history of galaxies?
Deuterium in the universe is created in the Big Bang and the primordial deuterium abundance provides the best constraints on the mass density of baryons in the universe. However, this Big Bang record is subsequently modified by stellar nuclear burning as material cycles from stars to the interstellar medium and back to stars.
SOFIA will study the deuterium abundance in the galaxy, investigating the evolution of the universe
Presenter: Sean C. Casey 62
SOFIA’s Next Steps
• Short Science Flights– FORCAST – Oct 2010 (3 flights)– GREAT – Feb 2010 (3 flights)
• Basic Science Program (50+ proposals)– Shared risk flights with FORCAST & GREAT– Summer 2011 (20 flights)
• Completion of observatory updated– 2011 – 2012 (down time)
• Full Operating Capabilities– 2013 & beyond (working to 100+ flights/year)
Presenter: Sean C. Casey 63
Science and Instruments
• SOFIA offers unique capabilities within NASA– Serving two communities
• Instrument developers – offers a robust instrument program
• General Investigators – access to latest technologies
– Capable sub-orbital platform• Daily, weekly, monthly, yearly access to observatory• Ready access to science instruments• Track record for new technologies
• Science instrument development is an essential element of successful SOFIA operations.
Presenter: Sean C. Casey 64
Summary of SOFIA Goals
• Science: Provide high angular and
spectral resolution imaging through-out
the infrared and sub-millimeter.
• Technology: Provide a well calibrated
and understood platform for state-of-
the-art infrared and sub-millimeter
instrumentation.
• Education: Provide readily accessible
educational and public forums which
encourage the study of astronomy.
http://sofia.arc.nasa.gov
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Additional Material
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1988 Kuiper Airborne Obs.6 x 6 Bolometer Camera
1994 South Pole128 x 128 Si:Sb BIB Spectrometer
1997 Apache Point Obs.1024 x 1024 InSb Camera
Historical photos
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Organic Growth & Chemistry in the ISM
Formation Processing Fossil / Delivery
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Telescope for Astronomy
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SOFIA First Light – M82
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SOFIA Science is broadly based
• Star formation, dynamics and chemical content of other galaxies:
• Interstellar cloud chemistry and dynamics, and star and planet formation in our galaxy:
• The dynamic activity in the center of our own galaxy:
• Origin and evolution of biogenic materials in the interstellar medium and in proto-planetary disks:
• Comets, planet atmospheres and rings in our solar system:
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GREAT: Heterodyne Spectrometer
PI: R. Guesten, Max-Planck Institut, [email protected]
R= 106 -> 108
Detector: dual channel mixer (HEB);60 – 200 m (1.4 - 5THz)
60 - 300 µm
Science: Spectroscopy of CII (158 m), and HD (112 m)
Targets: Galactic and extragalactic ISM, circumstellar shells
Successful lab demonstration at 1.9 THz of GREAT in July 2005
NB: TA < 2500 K at 158 m High frequency upgrade at 4.7 THz expected for OI (63 m).
Field of View: single element
Presenter: Sean C. Casey 73
Science Capabilities
• Sensitivity– Telescope
Emissivity ~ 0.1
Temperature ~ 240 K
– 40 to 300 m• ~ ISO point source (both
imaging and spectroscopy)
– 5 to 40 m• ~ 8 meter ground-based
telescope at 20m
• FOV 8 arcmin diameter• Image Size
– > 15 m: diffraction limited: 3 times better than Spitzer
(FWHM) ~ (m) / 10”
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SOFIA, Herschel, and JWST
2008-2012
2014-2019
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HIPO: High Speed Imager
PI: T. Dunham (Lowell Observatory) [email protected]
Detector: Dual channel 1Kx1K CCDs
Field of View: 5.6’ x 5.6’#1
#2
Working/complete HIPO instrument atLowell Obs. Aug 2004
Science: Occultations
Targets: Pluto, Triton, KBOs.
NB: Co-mounts w. FLITECAM
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August ’04 – Optical telescope tests with HIPO team
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NASA technology readiness level (TRL)
• Technology readiness defined– NASA/DOD– 9 levels
• Technology migration is an issue– Science enabling technologies are
essential to future NASA missions– Diminishing funds at the lowest and
highest levels create the “mid-TRL desert”
• Mitigation of new technology risks– Missions invest in critical technologies
• Spitzer - IRAC bridge chips• JWST - micro shutters arrays• Herschel - mixers/local oscillators
– System level integration is an issue• Converting photons into published results
Presenter: Sean C. Casey 78
SOFIA Instrument Definitions
• Principal Investigator Science Instruments (PSI)– Cutting edge technologies (low-TRL)– Developed and operated by PI teams– General investigators work with PI teams
• Facility Science Instrument (FSI)– Mature technologies (mid-TRL) when possible– Developed and delivered by PI teams– General investigators work with Observatory staff
• SOFIA must balance PSI and FSI programs– New SI, existing SI upgrades, & focused technology
development
Presenter: Sean C. Casey 79
HIPO: High Speed ImagerPI: T. Dunham (Lowell Observatory)
Detector: Dual channel 1Kx1K CCDs
Field of View: 5.6’ x 5.6’ #1
#2
Working/complete HIPO instrument atLowell Obs. Aug 2004
Pluto occultation from KAO (Elliot, et al. 1989)
Science: Occultations
Targets: Pluto, Triton, KBOs.
NB: Co-mounts w. FLITECAM
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FLITECAM: Near-IR Imager
PI: I. McLean (UCLA) [email protected]
Detector: Single 1K x 1K array; 1-5 m (InSb)
Field of View: 8.2’ x 8.2’
Science: Imaging, Spectroscopy,Occultations
Targets: Galactic, extragalactic
Grism observations from Lick of NGC 7027
NB: SOFIA seeing limits (129.01)
Working/complete FLITECAM instrument atLick in 2004/5
R ~ 2000