LSST proposes to use an 8.4 meter telescope and a camera with a 9.6 square degree fieldof- view to image half the sky in six filters and at significantly greater depth than DES and other precursor surveys. It will provide an enormous dataset for dark energy measurements via gravitational lensing, Supernovae and other methods. If funded, LSST aims for first light around 2014. It is currently finalizing the design of the various instruments based on the science requirements; weak lensing places the most stringent requirements on its image quality specifications.

Bernstein, Jain and Jarvis have been involved with LSST lensing in the past three years. We have helped formulate the science requirements for the design of the LSST instruments. With M. Takada we have calculated the forecasts for dark energy measurements with LSST and helped with LSST presentations at conferences and white papers. Jarvis and Jain have examined the scaling of the PCA method to the enormous survey size of LSST. The computational issues in carrying out a global image analysis of the LSST dataset are challenging; we have made analytical estimates and begun the adaptation of the software for testing with LSST simulations. We have also begun to study the connection of photometric redshifts and lensing science goals;
this effort is in collaboration with A. Connolly (U. Washington) and is funded through an LSST subcontract.

Recently Jain has taken up the role of co-chair of the LSST weak lensing science collaboration. With co-chair Dave Wittman at UC Davis, he is setting up a series of studies to be carried out to prepare for lensing measurements with LSST. Bernstein will continue to contribute to LSST lensing as a member of its science collaboration, as well as to time-domain astronomy enabled by LSST. We will work together in our roles for LSST and SNAP to carry out a comprehensive analysis of the capabilities of these ambitious ground and space-based surveys.

LSST proposes to use an 8.4 meter telescope and a camera with a 9.6 square degree fieldof- view to image half the sky in six filters and at significantly greater depth than DES and other precursor surveys. It will provide an enormous dataset for dark energy measurements via gravitational lensing, Supernovae and other methods. LSST aims for first light around 2014. It is currently finalizing the design of the various instruments based on the science requirements; weak lensing places the most stringent requirements on its image quality specifications.

Bernstein, Jain and Jarvis have been involved with LSST lensing in the past three years. They have helped formulate the science requirements for the design of the LSST instruments. With M. Takada they have calculated the forecasts for dark energy measurements with LSST and helped with LSST presentations at conferences and white papers. Jarvis and Jain have examined the scaling of the PCA method to the enormous survey size of LSST. The computational issues in carrying out a global image analysis of the LSST dataset are challenging; the Penn group has made analytical estimates and begun the adaptation of the software for testing with LSST simulations. We have also begun to study the connection of photometric redshifts and lensing science goals; this effort is in collaboration with A. Connolly (U. Washington) and is funded through an LSST subcontract.