Not all primary mirror segments are made equal. Additionally, obscuration from the secondary mirror structure on the inner ring of mirror segments and the secondary mirror surface figure error can make for challenging warping solutions. Presented in this paper is the latest technique developed at the W. M. Keck Observatory for calculating the optimal warping solution for unwarped segments in the telescopes called BAMM!. The new technique has been in operation for the last 3 years. BAMM! is built upon earlier work using Damped Least Squares or Tikhonov regularization. The solver modifies the LaGrange multiplier for each column vector of the influence function based on the ability of a single column vector to correct the surface figure in slope space with limitations on the maximum allowable force for each leaf spring. Results from this new solver are presented along with the limitations of this approach. The paper will also discuss why the warping solver needed to evolve due to of surface figure measurement creep. This creep resulted from how the secondary mirror position is calculated when unwarped segments are present during the telescope alignment, prior to primary mirror surface error measurements.
The first scientific observations with adaptive optics (AO) at W. M. Keck Observatory (WMKO) began in 1999. Through 2023, over 1200 refereed science papers have been published using data from the WMKO AO systems. The scientific competitiveness of AO at WMKO has been maintained through a continuous series of AO and instrument upgrades and additions. This tradition continues with AO being a centerpiece of WMKO’s scientific strategic plan for 2035. We will provide an overview of the current and planned AO projects from the context of this strategic plan. The current projects include implementation of new real-time controllers, the KAPA laser tomography system and the HAKA high-order deformable mirror system, the development of multiple advanced wavefront sensing and control techniques, the ORCAS space-based guide star project, and three new AO science instruments. We will also summarize steps toward the future strategic directions which are centered on ground-layer, visible and high-contrast AO.
The Veloce spectrograph is a high resolution (R > 75000), compact, highly-stabilised, and hyper-calibrated echelle spectrograph to obtain Doppler velocities for Sun-like and M-dwarf at < 1 ms−1. This spectrograph was built utilising multiple innovations to provide a “just -enough-stabilisation” platform, compensating the science observations with simultaneous collected data from an ultra-stabilised calibration source. The spectrograph consists of three spectral arms, one of which has been in operation while the additional two arms were undergoing construction. The first arm of the spectrograph, the Rosso arm, has a wavelength coverage of 580-930 nm was installed at the Anglo-Australian Telescope (AAT) and saw first light in September 2018. The Verde, 434-593 nm, and Azzurro, 378-437 nm, spectral arms passed the final design review in February of 2021 and were installed May and June of 2023 with first light occurring in early July 2023. This paper presents a review of the upgrade project along with discussions on the mechanical and optical designs in terms of procurement and manufacturability. We discuss the changes to the instrument driven from the lessons learned during the construction of the first arm of the spectrograph including detector electronics, optical mounts, and infrastructure, also the provisional acceptance of the installed instrument. We also include a discussion on the determination of the very tight slope error tolerances for the aspheric lenses in order to limit the influence of the mid-spatial frequencies on the spectra presented to the detector.
The Orbiting Configurable Artificial Star (ORCAS) mission in collaboration with the W. M. Keck Observatory (WMKO) is poised to deliver near diffraction limited observations in visible light. The ability to conduct such observations will enable significant scientific discoveries in fields related to Active Galactic Nuclei (AGN), Dark Energy, Flux Calibration, the High Redshift Universe, Exoplanets, and the Solar System. The ORCAS team has successfully completed three primary mission development goals to enable such observations. The performance demonstration with the ORCAS Keck Instrument Demonstrator (ORKID) captured arguably the highest resolution image at visible wavelengths from a large (10 meter) segmented telescope on the ground to date. High resolution AO imaging of the galaxy UGC 4729 in Natural Guide Star (NGS) mode was performed by locking onto a foreground asteroid passing nearby, which simulated an observation with a moving guide star validating post processing capabilities and demonstrating how regions unreachable by NGS and LGS could be explored. Additionally, the ORCAS team has successfully locked onto a laser source onboard the Laser Communications Relay Demonstration (LCRD) and closed the adaptive optics loop to perform near diffraction limited imaging at 1550 nm with the Keck 10 meter, the first demonstration of such capability with a large segmented telescope. All of these results validate the feasibility of the ORCAS mission. Following these accomplishments, ORCAS will be strongly positioned to propose a full-scale mission to upcoming opportunities.
We present the status and plans for the Keck All sky Precision Adaptive optics (KAPA) program. KAPA includes (1) an upgrade to the Keck I laser guide star adaptive optics (AO) facility to improve image quality and sky coverage, (2) the inclusion of AO telemetry-based point spread function estimates with all science exposures, (3) four key science programs, and (4) an educational component focused on broadening the participation of women and underrepresented groups in instrumentation. For this conference we focus on the KAPA upgrades since the 2020 SPIE proceedings1 including implementation of a laser asterism generator, wavefront sensor, real-time controller, asterism and turbulence simulators, the laser tomography system itself along with new operations software and science tools, and modifications to an existing near-infrared tip-tilt sensor to support multiple natural guide star and focus measurements. We will also report on the results of daytime and on-sky calibrations and testing.
The success of the Keck telescopes’ segmented mirror technology provided a basis for the development of other large and extremely large telescopes. We investigate ways to optimize the performance of the segmented mirror telescope further to (1) take on the challenges of high contrast imaging to characterize habitable zone exoplanets, (2) enable visible adaptive optics (AO), and (3) fully benefit from recent extreme AO developments. The current status of Keck telescope phasing using the phasing camera system (PCS) is briefly presented. A phase retrieval technique is presented that uses AO science instrument images to improve the phasing of the telescope primary mirror. The technique was tested on the Keck telescopes, and the first experimental results are presented along with the limitations of this approach. The static, semi-static, and dynamic nature of the residual segment piston errors are discussed, along with possible elevation-dependent residual segment piston errors. We propose that the technique be periodically used at Keck observatory to monitor and improve telescope phasing. We discuss the significance of the technique for AO observations with the existing and future large aperture optical telescopes. The ultimate goal is to push large aperture ground-based telescopes to their performance limits and make them competitive with space telescopes in terms of PSF stability to enable breakthrough science.
MAROON-X is a fiber-fed, red-optical, high precision radial velocity spectrograph recently commissioned at the Gemini North telescope on Mauna Kea, Hawai’i. With a resolving power of 85,000 and a wavelength coverage of 500–920 nm, it delivers radial velocity measurements for late K and M dwarfs with sub-50 cm s−1 precision. MAROON-X is currently the only optical EPRV spectrograph on a 8 m-class telescope in the northern hemisphere and the only EPRV instrument on a large telescope with full access by the entire US comm report here on the results of the commissioning campaign in December 2019 and early science results.
The Keck Planet Finder (KPF) is a fiber-fed, high-resolution, high-stability spectrometer in development at the UC Berkeley Space Sciences Laboratory for the W.M. Keck Observatory. KPF is designed to characterize exoplanets via Doppler spectroscopy with a goal of a single measurement precision of 0.3 m s-1 or better, however its resolution and stability will enable a wide variety of astrophysical pursuits. Here we provide post-preliminary design review design updates for several subsystems, including: the main spectrometer, the fabrication of the Zerodur optical bench; the data reduction pipeline; fiber agitator; fiber cable design; fiber scrambler; VPH testing results and the exposure meter.
We present the status and plans for the Keck All sky Precision Adaptive optics (KAPA) program. KAPA includes four key science programs, an upgrade to the Keck I laser guide star (LGS) adaptive optics (AO) facility to improve image quality and sky coverage, AO telemetry based point spread function (PSF) estimates for all science exposures, and an educational component focused on broadening the participation of women and underrepresented groups in instrumentation. For the purpose of this conference we will focus on the AO facility upgrade which includes implementation of a new laser, wavefront sensor and real-time controller to support laser tomography, the laser tomography system itself, and modifications to an existing near-infrared tip-tilt sensor to support multiple natural guide star (NGS) and focus measurements.
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