We present first on-sky performance results of KalAO, the natural guide star adaptive optics imager on the 1.2m Swiss telescope in La Silla, Chile. It is designed to reach at least 30% Strehl in order to detect stellar companions as close as the 150mas in visible-light, at diffraction limit. KalAO was built to search for binarity in planet hosting stars by following-up planet candidates primarily from the TESS satellite survey. The optical design is optimised for the 450 to 900nm wavelength range and is fitted with SDSS griz filters. Wavefront control works down to I-magnitude 10 stars in order to probe the same parameter space as radial velocity instruments such as HARPS and NIRPS. The system first closed the loop on sky in November 2023 and reached diffraction limit imaging in February 2024. It can carry out AO corrected observation of up to 500 targets in one night, with a Strehl ratio of ≈30%.
The Gemini North Adaptive Optics (GNAO) facility is the upcoming Adaptive Optics (AO) facility for Gemini North providing a state-of-the-art AO system for surveys and time domain science in the era of James Webb Space Telescope (JWST) and Rubin operations. GNAO will be optimized to feed the Gemini Infrared Multi Object Spectrograph (GIRMOS).
The GNAO project includes the development of a new laser guide star facility which will consist of four side launched laser beams supporting the two primary AO modes of GNAO: a wide-field mode providing an improved image quality over natural seeing for a 2-arcminute circular field-of-view using Ground Layer AO (GLAO) and a narrow-field mode providing near diffraction-limited performance over a 20 × 20 arcsecond square field-of-view using Laser Tomography AO (LTAO).
After a competitive phase A study among three teams for the conceptual design of the AO bench, one team has been selected to complete the design, build and commissioning it at the telescope. We will be presenting the overall GNAO facility design, including specifics related to the AO bench and its architectural design. We will provide updates on all subsystems of the facility.
Multi-Object Adaptive Optics (MOAO) proves to be an innovative technique, presenting distinct advantages for both multiplexing and adaptive optics (AO)-assisted integral field spectroscopy. This work presents an examination of MOAO performance designed for the Thirty Meter Telescope (TMT). Inspired by the design principles of GNAO-GIRMOS for the Gemini North Telescope, we propose a two-stage AO system. Leveraging the experience from GIRMOS, our approach incorporates NFIRAOS as the initial stage carrying out the Ground Layer Adaptive Optics (GLAO) correction. Subsequently, we introduce a MOAO module to achieve an additional correction at specific positions within a two arcminutes field of view, using the wavefront sensor telemetry provided by NFIRAOS. Through extensive numerical simulations, we explore the MOAO system order parameters, leading us to converge on a baseline design. This study provides insights into the performance metrics extracted from our simulations and concludes with a promising outlook for the transformative impact of a two-stage AO system on TMT observations and scientific productivity.
We are presenting in this work, the final design of the Multi-Object Adaptive Optics system for the Gemini InfraRed Multi Object Spectrograph (GIRMOS). This report outlines key modifications made during the critical design phase as we progress towards the manufacturing assembly integration and testing stage. Our adjustments include in particular, the wavefront sensor subassembly through the selection of a new camera and by optimizing the number of sub-apertures and pixels. Additionally, recent advancements in the Gemini North Adaptive Optics (GNAO) design prompt a reassessment of Ground Layer Adaptive Optics (GLAO) and tomographic performance, thus influencing both multi-Objects Adaptive Optics (MOAO) and the GIRMOS imager. The final optical and mechanical design of the MOAO subsystem as well as the revisited performance is discussed. Since the beginning of the project, we have identified some risks associated to the MOAO system and developed mitigation strategies and activities. We report the progress made towards the mitigation of identified risks such as open-loop calibration and control, go-to errors, quasi-static errors, etc. A primary objective driving the development of GIRMOS is the survey of a substantial sample of high-redshift galaxies. Using AO observations of z~2 galaxies, as seen with SINFONI at the Very Large Telescope, and employing image processing techniques with various GIRMOS simulated point spread functions (PSFs), we methodically explore the GIRMOS ability to detect and characterize star-forming clumps within high-redshift galaxies. This analysis provides valuable insights into optimal target selection based on their positioning in the field of view, on the observing conditions (such as seeing, zenith angle, etc.), and the intended scientific objectives.
The Research, Experiment and Validation of adaptive Optics on a Legacy Telescope (REVOLT) project is an on-sky AO technology research platform which was commissioned at the Dominion Astrophysical Observatory’s (DAO) 1.2m telescope in Victoria, Canada in June 2022. The goal of the project is to provide a flexible and expandable AO system to test a wide variety of technologies and control strategies with rapid deployment to sky. To date, REVOLT has enabled the first on-sky use of the Herzberg Extensible Adaptive Realtime Toolkit (HEART), a realtime controller software package developed at the National Research Council of Canada’s Herzberg Astronomy and Astrophysics (NRC-HAA) research centre, slated to be deployed on multiple future AO instruments. REVOLT has provided the first on-sky demonstration of First Light Imaging’s C-Blue-One CMOS camera as a Shack-Hartmann Wavefront Sensor (SH-WFS), and demonstrated injection of the science PSF into a single mode fiber to feed experimental Spectral Correlation Sensor technology being developed to detect gas signatures in planetary atmospheres. Since its initial commissioning as a Single Conjugate AO (SCAO) system, an open loop arm, the GIRMOS Open Loop Demonstration (GOLD) arm, has been added to test OL calibration and control, and a Pyramid WFS (PWFS) arm has been added with the goal first of testing the Gemini Planet Imager 2 (GPI-2) HEART pipeline, as well as provide an on going test platform for PWFS research. This paper provides a full description of the current REVOLT system, summarizes the performance of each experiment conducted to date, highlights future plans and openly invites proposals for collaboration from the AO community.
The Gemini Infrared Multi-Object Spectrograph (GIRMOS) is a new facility instrument being designed in close partnership with the upcoming facility adaptive optics (AO) system at Gemini-North observatory called GNAO. GIRMOS will carry out high angular resolution (0.83 – 2.4 µm) imaging and multi-object integral field (0.95 – 2.35 µm) spectroscopy within GNAO’s two arcminute field-of-regard. GIRMOS consists of an imager and four identical deployable integral field spectrographs with a multi-object AO system that provides an additional image quality improvement for each spectrograph over GNAO across the full field. We present the final design overview of GIRMOS, which will be entering the construction phase in 2024 with an expected delivery in 2027. GIRMOS is a pathfinder for future extremely large telescope instrumentation that requires high angular resolution, highly multiplexed spectroscopy.
NIRPS is a fiber-fed AO nIR spectrograph working simultaneously with HARPS at the La Silla-ESO 3.6m telescope. The cryogenic spectrograph operating at 75K employs a cross-dispersed echelle grating (R4), covering a wavelength range of 0.98-1.80 microns in a single image using a Teledyne Hawaii-4RG infrared detector. In early 2022, the NIRPS spectrograph was transported to Chile by plane with all the optical elements mechanically attached to the optical bench inside the vaccum vessel. To ensure the safety of the spectrograph, dedicated work was performed on the shipping crate design, which could survive up to 7g shocks. In La Silla, the vacuum vessel was re-integrated on its support structure and the spectrograph alignment was verified with the H4RG and the injection module. Given the optical design, the alignment phase was performed using a metrology arm and a few optical tests, which minimize the time required for this critical phase. From the validation/technical phase results, two major modifications were required. Firstly, the original grating element was replaced by a new etched crystalline silicon component made by the Fraunhofer Institute for Applied Optics and Precision Engineering. A novel technique was developed to verify the alignment at a warm temperature with the H4RG detector. Secondly, a thermal enclosure was added around the vacuum vessel to optimize thermal stability. Since then, the long-term thermal stability has been better than 0.2mK over 20 days. In this paper, we will review the final spectrograph performances, prior to shipping, and describe the novel techniques developed to minimize shipping costs, AITV phase duration, and grating replacement at the observatory. Additionally, we will discuss the thermal enclosure design to achieve the sub-mK thermal stability.
The Near-InfraRed Planet Searcher or NIRPS is a precision radial velocity spectrograph developed through collaborative efforts among laboratories in Switzerland, Canada, Brazil, France, Portugal and Spain. NIRPS extends to the 0.98-1.8 μm domain of the pioneering HARPS instrument at the La Silla 3.6-m telescope in Chile and it has achieved unparalleled precision, measuring stellar radial velocities in the infrared with accuracy better than 1 m/s. NIRPS can be used either standalone, or simultaneously with HARPS. Commissioned in late 2022 and early 2023, NIRPS embarked on a 5-year Guaranteed Time Observation (GTO) program in April 2023, spanning 720 observing nights. This program focuses on planetary systems around M dwarfs, encompassing both the immediate solar vicinity and transit follow-ups, alongside transit and emission spectroscopy observations. We highlight NIRPS’s current performances and the insights gained during its deployment at the telescope. The lessons learned and successes achieved contribute to the ongoing advancement of precision radial velocity measurements and high spectral fidelity, further solidifying NIRPS’ role in the forefront of the field of exoplanets.
GIRMOS is an integral field spectrograph designed to operate behind the Gemini North Adaptive Optics system. Its four arms will run in open-loop mode, using the telemetry received from GNAO to reconstruct tomographically the turbulence along each direction. The application of open-loop correction has been shown to be challenging on other instruments, because of the inability to monitor in real time its effect on the observed target. To reduce the risks associated to the use of open-loop adaptive optics with GIRMOS, we test our calibration procedures on sky using REVOLT, the adaptive optics bench and imager for the 1.2m telescope at the Dominion Astrophysical Observatory in Victoria, Canada.
The Gemini Infra-Red Multi-Object Spectrograph (GIRMOS) is a four-arm, Multi-Object Adaptive Optics (MOAO) IFU spectrograph being built for Gemini (commissioning in 2024). GIRMOS is being planned to interface with the new Gemini-North Adaptive Optics (GNAO) system, and is base lined with a requirement of 50% EE within a 0.100 spaxel at H-band. We present a design and forecast the error budget and performance of GIRMOS-MOAO working behind GNAO. The MOAO system will patrol the 20 field of regard of GNAO, utilizing closed loop GLAO or MCAO for lower order correction. GIRMOS MOAA will perform tomographic reconstruction of the turbulence using the GNAO WFS, and utilize order 16x16 actuator DMs operating in open loop to perform an additional correction from the Pseudo Open Loop (POL) slopes, achieving close to diffraction limited performance from the combined GNAO+MOAO correction. This high performance AO spectrograph will have the broadest impact in the study of the formation and evolution of galaxies, but will also have broad reach in fields such as star and planet formation within our Milky Way and supermassive black holes in nearby galaxies.
We present the last developments of the Multi-Object Adaptive Optics (MOAO) demonstrator for the Gemini Infra-Red Multi-Object Spectrograph (GIRMOS). The GIRMOS MOAO system will able to deliver an image quality close to the diffraction-limit in the near-infrared (1.0-2.4μm) by taking advantage of the GLAO corrected wavefront delivered by the future Gemini North Adaptive Optics (GNAO) facility and performing an additional MOAO correction. MOAO is particularly challenging and risky because the DM is controlled in open-loop and usually subject to the so-called DM go-to-error which are difficult to model and manage. Therefore, as part of the preliminary design phase of the instrument, we decided to build a one-to-one scale demonstrator to mitigate some risks, exercise MOAO calibration techniques between two AO systems (GNAO and GIRMOS) and characterize of the MOAO performance. GIRMOS is a complex AO instrument and to circumvent the cost and complexity of such a system we are using a spatial light modulator (SLM) allowing the generation of turbulence in specific directions in the field without the need of pick-off system. In this paper, we present the status of the GIRMOS MOAO prototype. We exercised MOAO calibration and characterized the open-loop error and the GIRMOS MOAO performance in laboratory. We found, thanks to the GLAO- MOAO design, a very small open-loop error of about 60 nm rms. In addition, the GIRMOS MOAO design includes a figure source to compensate the DM accuracy errors. Using the figure source in laboratory, we compensated about 37 nm rms of go-to errors reducing the open-loop error down to 44 nm rms.
NIRPS (Near Infra-Red Planet Searcher) is an AO-assisted and fiber-fed spectrograph for high precision radial velocity measurements in the YJH-bands. NIRPS also has the specificity to be an SCAO assisted instrument, enabling the use of few-mode fibers for the first time. This choice offers an excellent trade-off by allowing to design a compact cryogenic spectrograph, while maintaining a high coupling efficiency under bad seeing conditions and for faint stars. The main drawback resides in a much more important modal-noise, a problem that has to be tackled for allowing 1m/s precision radial velocity measurements. In this paper, we present the NIRPS Front-End: an overview of its design (opto-mechanics, control), its performance on-sky, as well as a few lessons learned along the way.
The Gemini Infra-Red Multi-Object Spectrograph (GIRMOS) is a four-arm, Multi-Object Adaptive Optics (MOAO) IFU spectrograph being built for Gemini (commissioning in 2024). GIRMOS is being planned to interface with the new Gemini-North Adaptive Optics (GNAO) system, and is base lined with a requirement of 50% EE within a 0.100 spaxel at H-band. We present a design and forecast the error budget and performance of GIRMOS-MOAO working behind GNAO. The MOAO system will patrol the 20 field of regard of GNAO, utilizing closed loop GLAO or MCAO for lower order correction. GIRMOS MOAA will perform tomographic reconstruction of the turbulence using the GNAO WFS, and utilize order 16x16 actuator DMs operating in open loop to perform an additional correction from the Pseudo Open Loop (POL) slopes, achieving close to diffraction limited performance from the combined GNAO+MOAO correction. This high performance AO spectrograph will have the broadest impact in the study of the formation and evolution of galaxies, but will also have broad reach in fields such as star and planet formation within our Milky Way and supermassive black holes in nearby galaxies.
We present our development of the Multi-Object Adaptive Optics (MOAO) system for the Gemini Infra-Red Multi-Object Spectrograph (GIRMOS). The GIRMOS MOAO system consists of four identical arms patrolling over a large field-ofregard (2 arcmin) and able to deliver an image quality close to the diffraction-limit in the near-infrared. The AO system of GIRMOS will performed MOAO correction on top of the wavefront delivered by the Gemini North AO (GNAO) system. We are currently prototyping one arm in the laboratory in order to validate the simulated performances and characterize the hardware as well as different MOAO control strategies. GIRMOS MOAO is a complex AO system and a complete lab characterization would require a full GNAO simulator with a pick-off system and multiple wavefront sensors (WFS), light sources, etc. To circumvent the cost and complexity of such a system we are using a spatial light modulator (SLM) allowing the generation of residual turbulences in specific directions in the field without the need of pick-off system. Coupled with a numerical end-to-end model of the system, our bench is focused on open-loop control rather than tomography. In this paper, we review the GIRMOS MOAO preliminary design of the system, the baseline performances and the status of the testbed.
GIRMOS is a multi-object adaptive optics spectrograph in the near-infrared currently being designed for the Gemini North telescope. It will allow to observe with high-quality adaptive optics correction multiple targets selected from a large field. To increase the efficiency of the nightly observations, it is important to provide a feedback in real time to operators and observers on the quality of the point-spread function, using intuitive metrics such as the full width at half maximum, the Strehl ratio and the encircled energy. We present a set of simple analytical expressions derived from other works that use the measurement of the wavefront residuals. We then compare the results to an end-to-end AO simulation of GIRMOS. We show that this approach works well with the estimation of the full width at half maximum and the Strehl ratio, while it is less successful with the encircled energy.
KEYWORDS: Spectrographs, Telescopes, Lanthanum, Planets, Spectroscopes, Exoplanets, Aerospace engineering, Space operations, James Webb Space Telescope
NIRPS is a near-infrared (YJH bands), fiber-fed, high-resolution precision radial velocity (pRV) spectrograph currently under construction for deployment at the ESO 3.6-m telescope in La Silla, Chile. Through the use of a dichroic, NIRPS will be operated simultaneously with the optical HARPS pRV spectrograph and will be used to conduct ambitious planet-search and characterization surveys through a 720-night of guaranteed time allocation. NIRPS aims at detecting and characterizing Earth-like planets in the habitable zone of low-mass dwarfs and obtain high-accuracy transit spectroscopy of exoplanets. Here we present a summary of the full performances obtained in laboratory tests conducted at Université Laval (Canada), and the first results of the on-going on-sky commissioning of the front-end. Science operations of NIRPS is expected to start in late-2020, enabling significant synergies with major space and ground instruments such as the JWST, TESS, ALMA, PLATO and the ELT.
NIRPS (Near Infra Red Planet Searcher) is a new ultra-stable infrared ( YJH) fiber-fed spectrograph that will be installed on ESO’s 3.6-m telescope in La Silla, Chile. Aiming at achieving a precision of 1 m/s, NIRPS is designed to find rocky planets orbiting M dwarfs, and will operate together with HARPS (High Accuracy Radial velocity Planet Searcher). In this paper we describe NIRPS science cases, present its main technical characteristics and its development status.
Since 1st light in 2002, HARPS has been setting the standard in the exo-planet detection by radial velocity (RV) measurements[1]. Based on this experience, our consortium is developing a high accuracy near-infrared RV spectrograph covering YJH bands to detect and characterize low-mass planets in the habitable zone of M dwarfs. It will allow RV measurements at the 1-m/s level and will look for habitable planets around M- type stars by following up the candidates found by the upcoming space missions TESS, CHEOPS and later PLATO. NIRPS and HARPS, working simultaneously on the ESO 3.6m are bound to become a single powerful high-resolution, high-fidelity spectrograph covering from 0.4 to 1.8 micron. NIRPS will complement HARPS in validating earth-like planets found around G and K-type stars whose signal is at the same order of magnitude than the stellar noise. Because at equal resolving power the overall dimensions of a spectrograph vary linearly with the input beam étendue, spectrograph designed for seeing-limited observations are large and expensive. NIRPS will use a high order adaptive optics system to couple the starlight into a fiber corresponding to 0.4” on the sky as efficiently or better than HARPS or ESPRESSO couple the light 0.9” fiber. This allows the spectrograph to be very compact, more thermally stable and less costly. Using a custom tan(θ)=4 dispersion grating in combination with a start-of-the-art Hawaii4RG detector makes NIRPS very efficient with complete coverage of the YJH bands at 110’000 resolution. NIRPS works in a regime that is in-between the usual multi-mode (MM) where 1000’s of modes propagates in the fiber and the single mode well suited for perfect optical systems. This regime called few-modes regime is prone to modal noise- Results from a significant R and D effort made to characterize and circumvent the modal noise show that this contribution to the performance budget shall not preclude the RV performance to be achieved.
Radial velocity instruments require high spectral resolution and extreme thermo-mechanical stability, even more difficult to achieve in near-infra red (NIR) where the spectrograph has to be cooled down. For a seeing-limited spectrograph, the price of high spectral resolution is an increased instrument volume, proportional to the diameter of the primary mirror. A way to control the size, cost, and stability of radial velocity spectrographs is to reduce the beam optical etendue thanks to an Adaptive Optics (AO) system. While AO has revolutionized the field of high angular resolution and high contrast imaging during the last 20 years, it has not yet been (successfully) used as a way to control spectrographs size, especially in the field of radial velocities.
In this work we present the AO module of the future NIRPS spectrograph for the ESO 3.6 m telescope, that will be feed with multi-mode fibers. We converge to an AO system using a Shack-Hartmann wavefront sensor with 14x14 subapertures, able to feed 50% of the energy into a 0.4" fiber in the range of 0.98 to 1.8 μm for M-type stars as faint as I=12.
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