Next-generation active telescope for space astronomy

Abstract

We present a design for an active telescope for space astronomy. The telescope is capable of both exoplanet work and general astronomy over wavelengths from ∼100 nm up to 5 μm. The primary mirror is 6 m in diameter, formed by 16 mirror segments that are precisely phased and supported on rigid body actuators and with segment optical surface figures finetuned using surface figure actuators. The active primary forms a large deformable mirror (DM) with wavefront error (WFE) correction at the entrance pupil. Thus the largest source of WFE can be removed at the source and is corrected over the entire field of view. This enables diffraction-limited performance at 400 nm and a more efficient optical system over a broader wavelength range than could be achieved by a small DM at a downstream relayed pupil. The telescope is passively cooled to below 100 K at Sun-Earth L2, enabling astronomical-background-limited observations out to 5 μm. Launched on a SpaceX Starship or alternatively National Aeronautics and Space Administration's Space Launch System, the telescope requires minimal deployments. A 72-m-diameter starshade provides a contrast ratio better than 10 −10 for exoplanet science. Near the visible region, with a 108% working bandwidth from 300 to 1000 nm, a working distance of 120 Mm provides a 51-mas inner working angle (IWA). This band can be moved to shorter or longer wavelengths by adjusting the starshade range from the telescope. Our first-ever thermal analysis of such a starshade shows that a temperature below 100 K can be achieved over a broad range of observing directions, permitting the possibility of working into the infrared. We model the yield in exoplanets that can be observed. A starshade and associated spectrograph offer significant advantages for exoplanet characterization. They enable a much broader instantaneous spectral bandwidth (here 108%) than current coronagraphs (∼10% to 20% bandwidth), allow both polarizations to be observed simultaneously, and have higher throughput. The IWA is twice as small as can be achieved with a coronagraph and there is no outer working angle. These differences are particularly pronounced in the UV, where coronagraph performance would be strongly affected by throughput losses, wavefront aberrations, Fresnel polarization effects at surfaces, and thermal instability.

Approaches to lowering the cost of large space telescopes

“…Closely related to thermal control and observatory design is wavefront sensing and control techniques to maintain the alignment and prescription of optical surfaces and thereby preserve image quality. A range of scientific studies have investigated optimal wavefront sensing and control approaches for large space telescopes, including ultra-stable 6 m telescopes with active primary mirrors, 44 9.2 m space telescopes with formation-flying laser guide stars, [45][46][47] and active space telescopes with predictive thermal modeling. 48 There have been several research missions to test approaches to wavefront control and the TRL of these approaches for future missions.…”

Optimization design and implementation of eccentric tracking pendulum mirror for satellite-borne laser communication

“…At present, the pendulum mirror used on space products is mainly a center symmetrical layout, the rotation axis is in the center of the lens, in order to avoid the motion envelope, the height of the pendulum mirror bracket axis is more than half of the long axis of the pendulum mirror. The perimeter of the pendulum mirror is usually also designed with a semi-enveloping hood to block the influence of external heat flow [11][12] . All these measures cause the overall structure of the pendulum mirror to be too large in the altitude direction, resulting in a high launch envelope, which is not conducive to efficient utilization of the external height direction resources limited.…”

Characterization of Multilayer Piezoelectric Stacks Down to 100K

“…Piezoelectric stacks are used in a variety of applications including; Energy harvesting [1], Fuel injectors [2], Vibration control [3], Vibration generation [4], Ultrasonic horns [5], Motors [6] and Active Mirrors [7]. Piezoelectric materials are widely used in the generation of ultrasound because they are nominally linear, solid state, have a large power density and are relatively inexpensive.…”