Science Merit Function for the KEPLER Mission

TL;DR

This paper presents a merit function designed to optimize the Kepler Mission's design by balancing science goals, mission parameters, and resource constraints, thereby enhancing its scientific output.

Contribution

It introduces a comprehensive merit function model that predicts mission outcomes and guides design trade-offs for the Kepler space telescope.

Findings

The merit function effectively predicts the number of exoplanets detected.

It helps optimize mission parameters to maximize scientific return.

The model supports risk assessment and mission advocacy.

Abstract

The Kepler Mission was a NASA Discovery-class mission designed to continuously monitor the brightness of at least 100,000 stars to determine the frequency of Earth-size and larger planets orbiting other stars. Once the Kepler proposal was chosen for a flight opportunity, it was necessary to optimize the design to accomplish the ambitious goals specified in the proposal and still stay within the available resources. To maximize the science return from the mission, a merit function (MF) was constructed that relates the science value (as determined by the PI and the Science Team) to the chosen mission characteristics and to models of the planetary and stellar systems. This MF served several purposes; prediction of the science results of the proposed mission, effects of varying the values of the mission parameters to increase the science product or to reduce the mission costs, and assessment of risks. The Merit Function was also valuable for the purposes of advocating the Mission by illustrating its expected capability. Later, it was used to keep management informed of the changing mission capability as trade-offs and mission down-sizing occurred. The MF consisted of models of the stellar environment, assumed exoplanet characteristics and distributions, parameter values for the mission point-design, and equations that related the science value to the predicted number and distributions of detected exoplanets. A description of the MF model and representative results are presented.