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Demonstration of Science Observing Modes

Demonstration of Science Observing Modes. AOWG meeting Dec. 5, 2003 D. Le Mignant, A. Bouchez for the Keck AO team. Purpose: to demonstrate LGS-AO observing modes and disseminate accurate information on the performance of the system. We are

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Demonstration of Science Observing Modes

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  1. Demonstration of Science Observing Modes AOWG meetingDec. 5, 2003D. Le Mignant,A. Bouchez for the Keck AO team

  2. Purpose: to demonstrate LGS-AO observing modes and disseminate accurate information on the performance of the system. We are • Proposing a plan to demonstrate LGS-AO observing modes • Proposing a path to shared risk science observations in 2004B. • Soliciting and welcoming suggestions and ideas

  3. Science observing mode demonstration plan • Define most important observing modes • Focus on the observing modes for which the functionalities are in place • For these modes, engineering targets will be chosen by AO team. • Analysis of these engineering data may be done through collaborations, but tools and results should be made available to community. • Technical and performance results, techniques, and tools to be distributed to community.

  4. Risk levels • Demonstrating LGS-AO observing modes is closely related to • LGS-AO development priorities • LGS-AO characterization and performance effort Assign risk levels to various observing modes by Feb. deadline: • Low risk: demonstrated, some inefficiency. • Moderate risk: Functionalities in place, not yet demonstrated. • High risk: Functionalities not yet in place or pushing performance limits.

  5. Main criteriaand risk levels expected in Feb. 2004 • Low risk • TT star V < 16 • Dither with laser on optical axis • TT star < 30” from center of NIRC2 FOV • Integration up to 10 min. • Vertical Angle mode • Moderate risk • TT star V < 18 • laser kept on target during dither, throw <8” • Integration up to 20 min. • High pointing accuracy (~5-10milli-arcsec) • Position Angle mode • Elevation variation > 20deg. or fast rotating pupil • High risk • TT star V > 18 • Moving TT stars • Differential atmospheric refraction correction

  6. Example: AGN imaging and spectroscopy AGN mag. = 18.2; TT star = 16.4 @ 10 arcsec Many potential ways to observe this target.. Possible path to demonstrate both the feasibility and the performance: • closing loop on V= 16.4 star • off-axis observing with high accuracy TSS dither • PA mode with TSS dither • performance for 10min integration • TSS dither with LGS kept on target  then demonstrate the feasibility of observing an AGN using such setup and in parallel: • TT performance on extended/faint objects • on-axis observations with TSS dither while laser is kept on target

  7. Proposed strategy for 2004A (11 eng. nights) • Some fraction of each night reserved for subsystem testing, e.g. • Laser pointing. • Low-bandwidth wavefront sensor & tip-tilt sensor optimization. • LGS-AO characterization and performance • to be presented and discussed today • Observing mode demonstration • comes after sub-system testing and validation • Need backup programs for weather/laser contingency. • Could carry out observatory staff research programs. • Or, could call for NGS mini-proposals. • Web-based proposal, with very detailed list of observing parms • Service observing < 3 hours for each project • Which proposal is activated depends on conditions.

  8. LGS observing modes in 2004 B • LGS-AO engineering will continue in 04B • more functionalities/automation fed into the system • more characterization/performance • more demonstration of observing mode • Shared-risk science • We must commit to performance criteria in Feb. 2004. • Led by outside PIs, possible collaboration with LGS-AO team. • If something breaks, engineering is first priority. • How to optimize the return from shared-risk science? • Shall we decline high-risk science projects? • Shall we have NGS weather contingency proposals ranked by UC/CIT/UH TACs? • Shall we suggest a limit on the number of observing nights for both NGS and LGS in 2004B?

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