In this paper, we describe the wide-field spectroscopic survey telescope (WST) project. WST is a 12-metre wide-field spectroscopic survey telescope with simultaneous operation of a large field-of-view (3 sq. degree), high-multiplex (20,000) multi-object spectrograph (MOS), with both a low and high-resolution modes, and a giant 3×3 arcmin2 integral field spectrograph (IFS). In scientific capability, these specifications place WST far ahead of existing and planned facilities. In only 5 years of operation, the MOS would target 250 million galaxies and 25 million stars at low spectral resolution, plus 2 million stars at high resolution. Without need for pre-imaged targets, the IFS would deliver 4 billion spectra offering many serendipitous discoveries. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work in synergy with future ground and space-based facilities. We show how it can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; the origin of stars and planets; and time domain and multi-messenger astrophysics. WST’s uniquely rich dataset may yield unforeseen discoveries in many of these areas. The telescope and instruments are designed as an integrated system and will mostly use existing technology, with the aim to minimise the carbon footprint and environmental impact. We will propose WST as the next European Southern Observatory (ESO) project after completion of the 39-metre ELT.
A six-night optical turbulence monitoring campaign has been carried at Cerro Paranal observatory in February and March, 2023 to facilitate the development and characterisation of two novel atmospheric site monitoring instruments - the ring-image next generation scintillation sensor (RINGSS) and 24-hour Shack Hartmann image motion monitor (24hSHIMM) in the context of providing optical turbulence monitoring support for upcoming 20-40m class telescopes. Both instruments offer the potential to replace the outdated MASS-DIMM, utilising new technologies to produce detailed, real-time characterisation of optical turbulence conditions at a site. In addition, the well-characterised Stereo-SCIDAR and 2016-MASS-DIMM were both active throughout the campaign providing further data for comparison. Contemporaneous measurements of both the integrated turbulence parameters - including seeing, free atmosphere seeing, coherence time and angle – and the vertical optical turbulence profile are examined along with the first 24-hour, day and night turbulence measurements at the site.
In this contribution we report the on-going progresses of the project FATE, an operational automatic forecast system conceived to deliver forecasts of a set of astroclimatic and atmospheric parameters having the aim to support the science operations (i.e. the Service Mode) at the Very Large Telescope. The project has been selected at conclusion of an international open call for tender opened by ESO and it fits with precise technical specifications. In this contribution we will present the ultimate goals of this service once it will be integrated in the VLT operations, the forecasts performances at present time and the state of the art of the project. FATE is supposed to draw the roadmap towards the optical turbulence forecast for the ELT.
The efficiency of science observation Short-Term Scheduling (STS) can be defined as being a function of how many highly ranked observations are completed per unit time. Current STS at ESO’s Paranal observatory is achieved through filtering and ranking observations via well-defined algorithms, leading to a proposed observation at time t. This Paranal STS model has been successfully employed for more than a decade. Here, we summarize the current VLT(I) STS model and outline ongoing efforts of optimizing the scientific return of both the VLT(I) and future ELT. We describe the STS simulator we have built that enables us to evaluate how changes in model assumptions affect STS effectiveness. Such changes include: using short-term predictions of atmospheric parameters instead of assuming their constant time evolution; assessing how the ranking weights on different observation parameters can be changed to optimize the scheduling; changing STS to be more ‘dynamic’ to consider medium-term scheduling constraints. We present specific results comparing how machine learning predictions of the seeing can improve STS efficiency when compared to the current model of using the last 10 min median of the measured seeing for observation selection.
The transition from construction to operations of the Thirty-Meter-Telescope (TMT) will happen over a phase of "early-operations” that will last several years to encompass the technical and science commissioning of its main systems, and will conclude when the facility enters "steady-state operations” (early 2030s according to the current schedule).
In this talk, we will present the current plan for technical and scientific operations of the Thirty-Meter-Telescope, including a description of its organizational structure, staffing and day-to-day activities. TMT's science operations model will be aimed at optimizing the science impact of the TMT and its operations efficiency, while providing a high-level of support to TMT users over all phases (submission, implementation and (post-)execution) of their science programs.
Optical turbulence affects significantly the quality of ground-based astronomical observations. An accurate and reliable forecast of optical turbulence can help to optimize the scheduling of the science observations and to improve both the quality of the data and the scientific productivity of the observatory. However, forecasts of the turbulence to a level of accuracy which is useful in the operations of large observatories are notoriously difficult to obtain. Several routes have been investigated, from detailed physical modelling of the atmosphere to empirical data-driven approaches. Here, we present an empirical approach exploiting spatial diversity and based on simultaneous measurements between two nearby sites, Cerro Paranal, host of the Very Large Telescope (VLT), and Cerro Armazones, future host of the Extremely Large Telescope (ELT) in Chile. We study the correlation between the high-altitude turbulence as measured between those two sites. This is part of the on-going efforts initiated by the European Southern Observatory (ESO), to obtain short-term forecasts of the turbulence to facilitate the operations of the VLT and prepare the ELT mode of operations.
How much light from the astronomical object actually reaches the focal plane of a telescope? To what extent the sensitivity can be extended to both ends of the visible wavelengths – ultraviolet (UV) and infrared (IR) – as much as possible from the ground? And how to maintain good throughput of the telescope optics? In this report, we make a simplified model to show effect in the reflectivity change of the telescope mirror from the recoating and cleaning versus degradation focusing on a segmented primary mirror of a telescope. The better understandings and monitoring of these competing factors will help fine tune the scheduling of the in-situ cleaning such as CO2 cleaning. By maintaining the high throughput of the optics, it becomes more feasible to catch rare atmospheric condition whenever it becomes available for very sensitive UV or IR observations during Moon’s dark and bright phases, respectively. The degradation not recoverable by the cleaning is reset by replacing dirty segments with freshly coated ones. The importance of regular in-situ cleaning is evident when it takes long time to replace the large number of freshly coated segments. It is important to clean the entire aperture as much as possible when a wet condition is forecast; for once the contamination settles on the surface, CO2 cleaning alone won’t be able to recover good surface characteristics of reflectivity, scattering, and emissivity.
The Keck II Laser Guide Star (LGS) Adaptive Optics (AO) System was upgraded from a dye laser to a TOPTICA/MPBC Raman-Fibre Amplification (RFA) laser in December 2015. The W. M. Keck Observatory (WMKO) has been operating its AO system with a LGS for science since 2004 using a first generation 15 W dye laser. Using the latest diode pump laser technology, Raman amplification, and a well-tuned second harmonic generator (SHG), this Next Generation Laser (NGL) is able to produce a highly stable 589 nm laser beam with the required power, wavelength and mode quality. The beam’s linear polarization and continuous wave format along with optical back pumping are designed to improve the sodium atom coupling efficiency over previously operated sodium-wavelength lasers. The efficiency and operability of the new laser has also been improved by reducing its required input power and cooling, size, and the manpower to operate and maintain it.
The new laser has been implemented on the telescope’s elevation ring with its electronics installed on a new Nasmyth sub-platform, with the capacity to support up to three laser systems for future upgrades. The laser is projected from behind the telescope’s secondary mirror using the recently implemented center launch system (CLS) to reduce LGS spot size. We will present the new laser system and its performance with respect to power, stability, wavelength, spot size, optical repumping, polarization, efficiency, and its return with respect to pointing alignment to the magnetic field. Preliminary LGSAO performance is presented with the system returning to science operations. We will also provide an update on current and future upgrades at the WMKO.
Significantly reducing weather and climate prediction uncertainty requires global observations with substantially higher information content than present observations provide. While GPS occultations have provided a major advance, GPS observations of the atmosphere are limited by wavelengths chosen specifically to minimize interaction with the atmosphere. Significantly more information can be obtained via satellite to satellite occultations made at wavelengths chosen specifically to characterize the atmosphere. Here we describe such a system that will probe cm- and mmwavelength water vapor absorption lines called the Active Temperature, Ozone and Moisture Microwave Spectrometer (ATOMMS). Profiling both the speed and absorption of light enables ATOMMS to profile temperature, pressure and humidity simultaneously, which GPS occultations cannot do, as well as profile clouds and turbulence. We summarize the ATOMMS concept and its theoretical performance. We describe field measurements made with a prototype ATOMMS instrument and several important capabilities demonstrated with those ground based measurements including retrieving temporal variations in path-averaged water vapor to 1%, in clear, cloudy and rainy conditions, up to optical depths of 17, remotely sensing turbulence and determining rain rates. We conclude with a vision of a future ATOMMS low Earth orbiting satellite constellation designed to take advantage of synergies between observational needs for weather and climate, ATOMMS unprecedented orbital remote sensing capabilities and recent cubesat technological innovations that enable a constellation of dozens of very small spacecraft to achieve many critical, but as yet unfulfilled, monitoring and forecasting needs.
The design of adaptive optics systems is driven by the local characteristics of the atmospheric turbulence. Site
characterization campaigns utilizing a variety of atmospheric monitoring equipment provides a statistical description of
parameters such integrated seeing, vertical distribution of turbulence strength as well as the coherent time of the
turbulence. Modeling work, intended to understand the operation bandwidth of adaptive optics systems make use of
Kolmogorov turbulence theory as well as time series of atmospheric parameters obtained from regression analysis based
on site characterization data. However, most of the time, even in the more detailed studies, one parameter though
important is not measured and monitored with the same attention than the other turbulence parameters, namely, the outer
scale of the turbulence.
The image quality in large aperture telescopes has been shown to have an important dependence on the instantaneous
magnitude of the outer scale of the turbulence. In general terms, the shorter the outer scale of the turbulence, the lower
the wavefront variance over the aperture of the imaging system and consequently the higher the image quality.
This study focuses in using reconstructed open loop wavefront sensor data observed simultaneously by the two apertures
of the Large Binocular Telescope (LBT) to compute and monitor the outer scale of the turbulence.
In 2013, a serial sky test has been held on 1.8 meter telescope in Yunnan observation site after 2011-2012 Laser guide star photon return test. In this test, the long-pulsed sodium laser and the launch telescope have been upgraded, a smaller and brighter beacon has been observed. During the test, a sodium column density lidar and atmospheric coherence length measurement equipment were working at the same time. The coupling efficiency test result with the sky test layout, data processing, sodium beacon spot size analysis, sodium profile data will be presented in this paper.
The TMT first light Adaptive Optics (AO) facility consists of the Narrow Field Infra-Red AO System (NFIRAOS) and the associated Laser Guide Star Facility (LGSF). NFIRAOS is a 60 × 60 laser guide star (LGS) multi-conjugate AO (MCAO) system, which provides uniform, diffraction-limited performance in the J, H, and K bands over 17-30 arc sec diameter fields with 50 per cent sky coverage at the galactic pole, as required to support the TMT science cases. NFIRAOS includes two deformable mirrors, six laser guide star wavefront sensors, and three low-order, infrared, natural guide star wavefront sensors within each client instrument. The first light LGSF system includes six sodium lasers required to generate the NFIRAOS laser guide stars. In this paper, we will provide an update on the progress in designing, modeling and validating the TMT first light AO systems and their components over the last two years. This will include pre-final design and prototyping activities for NFIRAOS, preliminary design and prototyping activities for the LGSF, design and prototyping for the deformable mirrors, fabrication and tests for the visible detectors, benchmarking and comparison of different algorithms and processing architecture for the Real Time Controller (RTC) and development and tests of prototype candidate lasers. Comprehensive and detailed AO modeling is continuing to support the design and development of the first light AO facility. Main modeling topics studied during the last two years include further studies in the area of wavefront error budget, sky coverage, high precision astrometry for the galactic center and other observations, high contrast imaging with NFIRAOS and its first light instruments, Point Spread Function (PSF) reconstruction for LGS MCAO, LGS photon return and sophisticated low order mode temporal filtering.
The TMT first light Adaptive Optics (AO) facility consists of the Narrow Field Infra-Red AO System (NFIRAOS) and the associated Laser Guide Star Facility (LGSF). NFIRAOS is a 60 × 60 laser guide star (LGS) multi-conjugate AO (MCAO) system, which provides uniform, diffraction-limited performance in the J, H, and K bands over 17-30 arc sec diameter fields with 50 per cent sky coverage at the galactic pole, as required to support the TMT science cases. NFIRAOS includes two deformable mirrors, six laser guide star wavefront sensors, and three low-order, infrared, natural guide star wavefront sensors within each client instrument. The first light LGSF system includes six sodium lasers required to generate the NFIRAOS laser guide stars. In this paper, we will provide an update on the progress in designing, modeling and validating the TMT first light AO systems and their components over the last two years. This will include pre-final design and prototyping activities for NFIRAOS, preliminary design and prototyping activities for the LGSF, design and prototyping for the deformable mirrors, fabrication and tests for the visible detectors, benchmarking and comparison of different algorithms and processing architecture for the Real Time Controller (RTC) and development and tests of prototype candidate lasers. Comprehensive and detailed AO modeling is continuing to support the design and development of the first light AO facility. Main modeling topics studied during the last two years include further studies in the area of wavefront error budget, sky coverage, high precision astrometry for the galactic center and other observations, high contrast imaging with NFIRAOS and its first light instruments, Point Spread Function (PSF) reconstruction for LGS MCAO, LGS photon return and sophisticated low order mode temporal filtering.
Dome and mirror seeing are critical effects influencing the optical performance of ground-based telescopes.
Computational Fluid Dynamics (CFD) can be used to obtain the refractive index field along a given optical path and
calculate the corresponding image quality utilizing optical modeling tools. This procedure is validated using
measurements from the Keck II and CFHT telescopes.
CFD models of Keck II and CFHT observatories on the Mauna Kea summit have been developed. The detailed models
resolve all components that can influence the flow pattern through turbulence generation or heat release. Unsteady
simulations generate time records of velocity and temperature fields from which the refractive index field at a given
wavelength and turbulence parameters are obtained.
At Keck II the Cn2 and l0 (inner scale of turbulence) were monitored along a 63m path sensitive primarily to turbulence
around the top ring of the telescope tube. For validation, these parameters were derived from temperature and velocity
fluctuations obtained from CFD simulations.
At CFHT dome seeing has been inferred from their database that includes telescope delivered Image Quality (IQ). For
this case CFD simulations were run for specific orientations of the telescope respect to incoming wind, wind speeds and
outside air temperature. For validation, temperature fluctuations along the optical beam from the CFD are turned to
refractive index variations and corresponding Optical Path Differences (OPD) then to Point Spread Functions (PSF) that
are ultimately compared to the record of IQ.
Atmospheric optical turbulence is the main driver of wavefront distortions which affect optical telescope performance.
Therefore, many techniques have been developed to measure the optical turbulence strength along the line of sight.
Based on data collected with the MASS (Multi Aperture Scintillation Sensor), we show that a large sample of such
measurements can be used to assess the average three dimensional turbulence distribution above ground.
The use of, and a more sophisticated instrumental setup for, such turbulence tomography will be discussed.
Laser beams projected from the ground to form laser guide stars (LGS) experience scattering and absorption
that reduce their intensity as they propagate through the atmosphere. Some fraction of the scattered light will
be collected by the other LGS wavefront sensors and causes additional background in parts of the pupil. This
cross-talk is referred to as the fratricide effect. In this paper we quantify the magnitude of four different sources
of scattering/absorption and back scattering, and evaluate their impact on performance with various zenith
angles and turbulence profiles for the Thirty Meter Telescope (TMT) MCAO system, NFIRAOS. The resulting
wavefront error is on the order of 5 to 20 nm RMS, provided that the mean background from the fratricide can
be calibrated and subtracted with an accuracy of 80%. We have also found that the impact of fratricide is a
weak function of LGS asterism radius.
With the development of increasingly larger and more complex telescopes and instrumentation, site testing and
characterization efforts also increase in both magnitude and complexity. This happens because the investment
into larger observatories is higher and because new technologies, such as adaptive optics, require knowledge about
parameters that did not matter previously, such as the vertical distribution of turbulence. We present examples
of remaining questions which, to date, are not generally addressed by "standard" site characterization efforts,
either because they are technically not (yet) feasible or because they are impractical. We center our observations
around the experience gained during the Thirty Meter Telescope (TMT) site testing effort with an emphasis
on turbulence measurements, but our findings are applicable in general to other current and future projects as
well.
The Thirty Meter Telescope (TMT) project has been collecting data on five candidate sites since 2003. This paper
describes the site testing portion of the TMT site selection program and the process and standards employed
by it. This includes descriptions of the candidate sites, the process by which they were identified, the site
characterization instrument suite and its calibration and the available results, which will be published shortly.
Periodic vortex shedding from a 12-m parabola antenna has been found in the wind of 9 m s-1 and an attack angle of 26
degrees. The measurements have been made at the NRAO VLA site. The periodic yaw motion of an elevation axis has
been detected with linear gauges mounted on a reference structure that was built in each side of the yoke. It has also been
observed in the angle difference of two encoders installed at both ends of the elevation axis. The frequency of yaw
motion was 0.15 Hz. The same periodicities have been found in both the wind direction and wind velocity measured with
an ultrasonic anemometer in the wake downstream of the antenna. Such periodicities have been seen in neither common
displacement of the bearing housings nor rotation of the elevation axis. The Reynolds number of the flow was 6 x 106
(hypercritical), suggesting the vortex shedding be periodic, which is consistent with our observations. The Strouhal
number of parabola has been found to be 0.19 that is comparable to those of cylinder, inverse triangle, and other similar
geometric shapes. The coefficient for oscillatory lateral force exerted on the antenna by shedding vortices has been
estimated to be about 1.
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