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

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Presentation transcript:

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 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

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.

Risk levels 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. Demonstrating LGS-AO observing modes is closely related to LGS -AO development priorities LGS-AO characterization and performance effort

Main criteria and risk levels expected in Feb 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 2.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 3.High risk TT star V > 18 Moving TT stars Differential atmospheric refraction correction

Example: AGN imaging and spectroscopy AGN mag. = 18.2; TT star = 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

Proposed strategy for 2004A (11 eng. nights) 1.Some fraction of each night reserved for subsystem testing, e.g. Laser pointing. Low-bandwidth wavefront sensor & tip-tilt sensor optimization. 2.LGS-AO characterization and performance to be presented and discussed today 3.Observing mode demonstration comes after sub-system testing and validation 4.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.

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 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?