The Lazuli Space Observatory: Architecture and Capabilities

Abstract

The Lazuli Space Observatory is a 3 m aperture astronomical facility designed for rapid-response observations and precision astrophysics across visible to near-IR wavelengths (400–1700 nm bandpass). An off-axis, freeform telescope delivers diffraction-limited image quality (Strehl >0.8 at 633 nm) to three instruments across a wide, flat focal plane. The three instruments provide complementary capabilities; the Wide-field Context Camera (WCC) delivers multiband imaging over a 35′×12′ footprint with high-cadence photometry; the Integral-field Spectrograph (IFS) provides continuous 400–1700 nm spectroscopy at R ∼ 100–500 for stable spectrophotometry; and the ExtraSolar Coronagraph (ESC) enables high-contrast imaging expected to reach raw contrasts of 10−8 and postprocessed contrasts approaching 10−9. Operating from a 3:1 lunar-resonant orbit, Lazuli will respond to targets of opportunity in under four hours—a programmatic requirement designed to enable routine temporal responsiveness that is unprecedented for a space telescope of this size. Lazuli’s technical capabilities are shaped around three broad science areas: (1) time-domain and multimessenger astronomy, (2) stars and planets, and (3) cosmology. These capabilities enable a potent mix of science spanning gravitational-wave counterpart characterization, fast-evolving transients, Type Ia supernova cosmology, high-contrast exoplanet imaging, and spectroscopy of exoplanet atmospheres. While these areas guide the observatory design, Lazuli is conceived as a general-purpose facility with open time for the global community. We describe the observatory architecture and capabilities in the preliminary design phase, with science operations anticipated following a rapid development cycle from concept to launch; quoted performance specifications reflect current design requirements and modeling predictions, pending on-orbit verification.