interventions and too observations with the large binocular telescope
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Interventions and ToO Observations with the Large Binocular Telescope. R. Mark Wagner Research & Instrumentation Scientist LBTO/OSU. LBT Project Partners. Arizona – 25% The University of Arizona Arizona State University Northern Arizona University Germany – 25% - PowerPoint PPT PresentationTRANSCRIPT
Interventions and ToO Observations with the
Large Binocular Telescope
R. Mark Wagner
Research & Instrumentation Scientist
LBTO/OSU
LBT Project Partners• Research Corporation – 12.5%
– The Ohio State University– University of Notre Dame– University of Minnesota– University of Virginia
• Italy – 25% Istituto Nazionale di Astrofisica (INAF)
– Osservatorio Astrofisico di Arcetri– Osservatorio Astronomico di
Bologna– Osservatorio Astronomico di Roma– Osservatorio Astronomico di Padova– Osservatorio Astronomico di Brera– Other Italian Observatories and
Universities• The Ohio State University – 12.5%
• Arizona – 25%– The University of Arizona– Arizona State University– Northern Arizona University
• Germany – 25% LBT Beteiligungsgesellschaft
(LBTB)– Max-Planck-Institut fur Astronomie
(Heidelberg)– Landessternwarte (Heidelberg)– Astrophysikalisches Institut
Potsdam– Max-Plank-Institut fur
Extraterrestriche Physik (Munich)– Max-Plank-Institut fur
Radioastronomie (Bonn)
LBT Enclosure on Mt. Graham
The Large Binocular Telescope• Binocular 8.4 m apertures• 11.8 m equivalent aperture• Baseline of 22.8 m• Alt-azimuth mounting• Integrated adaptive optics• F/15 Gregorian and F/1.1 prime foci• Six focal station pairs• “Rapid” telescope reconfiguration
Second Primary Mirror installed in telescope
First Light Image – NGC 891
LBCFPA
&
FullMoon
overN891
LBT Instruments• Facility instruments
– Large Binocular Camera (LBC)– MultiObject Double Spectrograph (MODS)– Near-IR Imager/Spectrograph (LUCIFER)
• Strategic instruments– LBT Interferometer (LBTI)– Near-IR/Visible Adaptive Camera and
Interferometer (LINC/NIRVANA)• PI and Visitor instruments
– Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI)
LBT Instrument ParametersInstrument Focal
StationModes Spectral
Coverage(m)
Spectral Resolution
Field of View
Pixel Scale(arcsec/pixel)
LBC-BlueLBC-Red
Prime Direct CCD U, BV, R, I
4-50 27' × 27' 0.228
MODS-BlueMODS-Red
Direct F/15 Imager, Longslit, MOS
0.32 - 0.600.60 - 1.0
2,000 - 8,000 6' × 6' 0.15
LUCIFER Front-Bent Imager, Longslit, MOS
AO
Z, J, H, K
J, H, K
5,000 - 10,000
~30,000
4' × 4'
30″ × 30″
0.12 - 0.25
0.015
LBTI Center-Bent Nulling InterfShort FizeauLong Fizeau
8 – 133-5
8-25
2 - 30 25″ 0.1
LINCNIRVANA
Rear-Bent Fizeau Interferometer
J, H, K' 5 - 20 10″ - 20″ 0.006
PEPSI Rear-BentDirect F/15
SpectroscopySpecPol
0.39 - 1.1 40,000 to300,000
0.5″ - 1.4″ 0.165
Draft LBT Operations Model• LBT will be scheduled in partner blocks of
7-10 nights.• Partners will send only experienced
observing teams to the LBT.• Observing teams will queue observe
partner’s programs.• Telescope reconfigurations, including AO,
are permitted. Number/night is TBD.• LBTO will provide daytime and nighttime
technical support, LTO, and IQ Specialist.
Interventions and ToO with the LBT
• No policy currently in place.
• Discussed by Science Advisory Committee (SAC) in May 2002.
• Some partners may be interested in receiving notifications and acting on them.
• Consortium-wide agreements may be difficult to achieve.
• Models from similar partnerships may be helpful in formulating a LBTO policy.