1. D. Measurement Approach Phil Hinz Principal Investigator

2. Measurement and Analysis Compliance This presentation discusses the approach to measuring and analyzing HOSTS observations and demonstrates performance Relationship to ORR Success Criteria: The presentation demonstrates that the 12- zodi sensitivity is satisfied Concerns: None Liens: None D-2 1.a LBTI demonstrates 12-zodi sensitivity (1 , single star measurement, PLRA zodi model) Green

3. A Quick Tour of the LBT D-3 Adaptive Secondary (M2) Prime Focus Camera (stowed) Swing Arm Tertiary (M3) DX (right) Primary (M1) Multi-Object Double Spectrograph (MODS) C-Ring Azimuth Bearing LBTI Bent Gregorian Focal Station SX (left) Primary (M1) Uprights Wind Bracing ARGOS Laser Launch Telescope Dynamic Balance Element Rear View of LBT DX Mirror Cell All telescope optics outfitted with seismic accelerometer to completely define their motion in all 6 DOF at 1 kHz

4. Key Parameters of the LBT Sensitivity Wavefront precision Simple, cryogenic beam-combination D-4 LBT AO Secondary High-Strehl AO-corrected image in J-Band

5. LBTI Layout D-5 Beam-combiner optics are at 80 K

6. Nulling Optical Path D-6 Nulling Optics are at 80 K Phase sensing is completely common-path

7. Control System Three main loops: – Left AO system – Right AO system – Phasing system All coordinated by the science camera (NOMIC) D-7 Manual Set-Point Adjustment

8. Phase Sensing Approach Pupil image is formed at 2.2 µm wavelength – Wedge in the beamsplitter creates a tilt at K band for overlapped 11-µm images – Argument from Fourier Transform gives phase error signal at 1 kHz – Group delay is encoded in the visibility of the fringes across the pupil PID and discrete vibration filtering used for closed loop control – Feed-forward from accelerometers gives error signal at 1 kHz D-8 1 kHz 1 Hz Accelerometer Inputs

9. Overall Observing Sequence The HOSTS observing sequence for each science object is set up as follows: D-9

10. Acquisition Process (Once per Pointing) Each pointing requires – Object acquisition – AO setup – Fringe acquisition – Phase sensor setup – Null acquisition D-10 Set-point adjustment will be automated during SV

11. Offset Process (Once per Nod) Each offset requires – Telescope offset command – AO pause and resume – Manual phase-loop closing D-11 Phase-loop automated pause and resume will be implemented during SV

12. Survey Optimization Why not observe, say, 150 stars? – The sample of “good” stars for LBTI’s observational parameters are 50- 100. Detectability drops off for additional stars – The Mission Success Analysis, suggests sensitivity is preferred to number of stars (although both help) So, why not observe 20 stars more deeply? – Improvements using very long exposures may not be realizable Have you considered more/less dwell time per nod? – This is set by an attempt to balance efficiency and low frequency background effects – Less would be preferable and will be explored during SVP Have you considered more/less dwell time per pointing? – This is set by an attempt to measure slow drifts – No drifts are seen in data. Could perhaps be lengthened D-12