Volume Phase Holographic Gratings (VPHGs) have become a staple of astronomical spectrograph design over the last several decades. VPHGs commonly employ dichromated gelatin (DCG) as the index modulation medium which provides high efficiency, low stray light, robust environmental protection, and high index modulation – thereby enabling wide spectral bandwidths and angular tuning. However, wavefront performance can be a compromising factor in system design, even when gratings are polished after assembly using traditional polishing techniques. The final diffracted wavefront of a DCG-VPHG is a combination of several compounding factors: substrate homogeneity, surface flatness, holographically recorded wavefront, processing techniques, bowing of the glass during the capping process, and imprinted adhesive wavefront errors, some of which can be mitigated through careful process control. To address the remaining gap in wavefront error relative to other components, we propose custom magnetorheological finishing (MRF). In this paper, we demonstrate the wavefront improvement observed by applying custom MRF to a large diffraction grating (15 x 15 cm). The performance enhancements to be shown promise to improve grating wavefront performance considerably, thus improving overall system performance. The grating used in this study is part of a technology demonstration for the future HARMONI Spectrograph for ESO’s Extremely Large Telescope (ELT). The grating for this wavefront improvement project has been produced as a collaboration between University of Oxford researchers, Wasatch Photonics, and QED Technologies.
As part of our ongoing research and development activities for the Planetary Camera and Spectrograph (PCS) for ESO’s Extremely Large Telescope (ELT), we are comparing two types of integral field unit concepts—an image-slicer and a lenslet-array—for its integral field spectrograph and main science instrument. In our 2022 publication we described the design and manufacturing of the image-slicer used in this comparison, based on the concept of our twisted image slicer published in 2014; in this paper we present recent interferometric measurements of the mirrors of the image slicer, manufactured by Canon Inc. Using our 6-inch Fizeau interferometer we measured the spherical pupil mirrors, resulting in a typical peak-to-valley surface figure error of ≲ 160 nm, and an RMS error of ≲ 25 nm. Measuring the 0.3 mm×13.5 mm parabolic slicing mirrors was challenging, however, after removing low-order alignment errors our measurements indicate a surface error of RMS ≲ 70 nm. Based on these measurements we conclude that the surface quality of the mirrors is excellent and well suited for our experiment.
HARMONI is the first light, adaptive optics assisted, visible and near-infrared integral field spectrograph for the European Southern Observatory’s Extremely Large Telescope (ELT). As a ‘work-horse’ instrument, HARMONI will offer low, medium, and high spectral resolution volume phase diffraction gratings (VPH) across the I, z, J, H, and K-bands, operating at four spatial sampling scales including at the diffraction limit of the ELT. Consequently, understanding and controlling sources of wavefront error (WFE) is of critical importance to the instrument performance. We present a comprehensive overview of the WFE performance verification for the VPH element of the HARMONI infrared grating module. In collaboration with Wasatch Photonics, we compare the measured WFE at different test wavelengths to investigate the presence of any chromatic dependence or lack thereof. Finally, we discuss the origin of the observed wavefront error and the effectiveness of mitigation techniques such as magnetorheological finishing.
HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 470nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews. The diffraction gratings are the single biggest contributor to the instrument’s throughput loss. Additionally, the range of operating modes and configurations available to HARMONI users will result in a varying beam footprint at the grating surface. HARMONI’s four spectrographs will be equipped with 10 gratings each, requiring a bespoke automated test facility to qualify the transmission performance of all the HARMONI gratings. This paper describes the test bench, and presents transmission efficiency results for different HARMONI gratings.
With the ambitious goal of characterizing nearby Earth-like exoplanets, the Planetary Camera and Spectrograph for the Extremely Large Telescope (ELT-PCS) will need to push the boundaries of both high contrast coronagraphic imaging and integral field spectrograph technology. High contrast imaging spectrographs typically employ microlens array-based integral field units (IFU), which provide a large number of spaxels in exchange for short spectra and an inefficient use of detector pixels. In contrast, image slicers provide a high detector use efficiency with a broader spectral bandpass. We report on the progress of a trade study into IFU design choices for ELT-PCS using a modular integral field spectrograph test-bench. At the core of the experiment are two custom-built IFUs: a novel image slicer-based IFU manufactured by Canon Inc. and BIGRE-like microlens array IFU. We provide an overview of the experiment, the individual performances of the two IFUs, and outline future applications of the test-bench for the design of the integral field spectrograph sub-system of ELT-PCS.
HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450 nm to 2450 nm with resolving powers from 3500 to 18000 and spatial sampling from 60 mas to 4 mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews. HARMONI is a work-horse instrument that provides efficient, spatially resolved spectroscopy of extended objects or crowded fields of view. The gigantic leap in sensitivity and spatial resolution that HARMONI at the ELT will enable promises to transform the landscape in observational astrophysics in the coming decade. The project has undergone some key changes to the leadership and management structure over the last two years. We present the salient elements of the project restructuring, and modifications to the technical specifications. The instrument design is very mature in the lead up to the final design review. In this paper, we provide an overview of the instrument's capabilities, details of recent technical changes during the red flag period, and an update of sensitivities.
KEYWORDS: Point spread functions, Calibration, Education and training, Spectrographs, Deep learning, Data modeling, Equipment, Adaptive optics, Mathematical modeling, Device simulation
The detection and characterization of Earth-like planets in the solar neighborhood is a key scientific goal for the European Southern Observatory’s upcoming Extremely Large Telescope (ELT). A major limitation in achieving the high contrast ratios, i.e. 10−8–10−9, at the small inner working angles necessary to conduct these observations is the presence of Non-Common Path Aberrations (NCPAs), which arise from optical path differences between the adaptive optics system and the science instrument. NCPA calibration is therefore critical for improving the performance of several current and planned instruments including ELT-PCS and ELT-HARMONI, a first light instrument for the ELT. We present the development of an alternative approach to NCPA calibration using a deep learning model. The model is trained on both simulated image slicer images and real calibration data obtained from the recently commissioned ERIS integral field spectrograph at the VLT.
HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 470nm to 2450nm with resolving powers from 3300 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews. The integral field spectrograph is a key subsystem of HARMONI instrument, which forms the 2D spectral image and projects it onto the scientific detector. It has 40 operational modes with different platescales and gratings covering the band of 811-2450 nm with three resolution grades. In each of this configurations the as-built spectrograph wavefront error is strictly limited. We perform the sensitivity analysis for measurable and unknown errors and build the errors budget on this basis. Then we correct the values for the actual technological limits and perform a three-stage Monte-Carlo analysis combined with simulation of a few specific effect as the holographic grating wavefront error. Eventually, we show that it is possible to reach the target image quality in terms of the wavefront error and spectral resolution for the entire sub-system with practically feasible tolerances on design parameters.
HARMONI is the first light, adaptive optics assisted, visible and near-infrared integral field spectrograph for the European Southern Observatory’s Extremely Large Telescope (ELT). It covers a large spectral range from 450 nm to 2450 nm with spectral resolving powers R ≡ λ/δλ from 3300 to 17000 and spatial sampling from 60 mas to 4 mas. It contains four identical spectrograph modules that collimate, disperse, and image the long slit at the exit of the integral field unit onto the science detectors. The collimation optics comprises of a three mirror anastigmat, using off-axis, aspheric mirrors. Previously we simulated an iterative alignment procedure that uses interferometric wavefront measurements together with a numerical optical model to minimise the wavefront error by adjusting a set of compensators. In this paper we demonstrate the feasibility of this procedure with an off-axis parabolic mirror as a prototype collimator, that has the same number of compensators as the HARMONI collimators. We show that we achieve a sufficiently low wavefront error within a few iterations of alignment. We cooled the test setup in a cryostat and obtained preliminary wavefront measurements at a cryogenic temperature of 130 ˚K, demonstrating the athermal design of the prototype.
Integral fields units such as lenslet-arrays, fibre-bundles or image-slicers all suffer from inefficient over-sampling of the spatial PSF unless anamorphic magnifying optics are used, which adds optical aberrations, and reduces optical throughput. In 2014 we presented the novel twisted image slicer concept that produces fully Nyquist-sampled data cubes without the use of anamorphic optics; in this paper we present the opto-mechanical design of a prototype twisted image slicer, its nominal performance, and preliminary characterisation results. The image slicer, manufactured by Canon Inc., will be used with a test-bench integral field spectrograph as part of the R&D activities for the Planetary Camera and Spectrograph (PCS) for the Extremely Large Telescope (ELT). First interferometric measurements indicate a very good surface figure with a figure error smaller than 100 nm P-V. Preliminary spectra taken with the test-bench spectrograph suggest that the twisted slicer concept does indeed achieve Nyquist sampling in both spatial directions as well as along the spectral axis.
The Planetary Camera and Spectrograph (ELT-PCS) will provide an unprecedented combination of high contrast imaging and spectral resolving power to the Extremely Large Telescope (ELT) with the ambitious goal of characterizing nearby Earth-like exoplanets. We present the initial results of a laboratory experiment that aims to compare the performances of both a novel, high contrast image slicer-based integral field unit (IFU) and a traditional lenslet-based IFU for use in ELT-PCS. The slicer-based IFU mirrors are manufactured by Canon Inc. who recently developed a diamond machining technique to achieve an extremely low surface-roughness (≤1.5 nm). The experimental integral field spectrograph (IFS) is modular to operate with both custom IFUs and to ensure that differences in the optical performance are entirely driven by the IFU design. We provide an overview of the individual IFS subsystems, initial optical performance metrics, and outline the future objectives for the experiment.
We have recently commissioned a novel infrared (0:9-1:7 μm) integral field spectrograph (IFS) called the Wide Integral Field Infrared Spectrograph (WIFIS). WIFIS is a unique instrument that offers a very large field-of-view (5000 x 2000) on the 2.3-meter Bok telescope at Kitt Peak, USA for seeing-limited observations at moderate spectral resolving power. The measured spatial sampling scale is ~ 1 x 1" and its spectral resolving power is R ~ 2; 500 and 3; 000 in the zJ (0:9 - 1:35 μm) and Hshort (1:5 - 1:7 μm) modes, respectively. WIFIS's corresponding etendue is larger than existing near-infrared (NIR) IFSes, which are mostly designed to work with adaptive optics systems and therefore have very narrow fields. For this reason, this instrument is specifically suited for studying very extended objects in the near-infrared such as supernovae remnants, galactic star forming regions, and nearby galaxies, which are not easily accessible by other NIR IFSes. This enables scientific programs that were not originally possible, such as detailed surveys of a large number of nearby galaxies or a full accounting of nucleosynthetic yields of Milky Way supernova remnants. WIFIS is also designed to be easily adaptable to be used with larger telescopes. In this paper, we report on the overall performance characteristics of the instrument, which were measured during our commissioning runs in the second half of 2017. We present measurements of spectral resolving power, image quality, instrumental background, and overall efficiency and sensitivity of WIFIS and compare them with our design expectations. Finally, we present a few example observations that demonstrate WIFIS's full capability to carry out infrared imaging spectroscopy of extended objects, which is enabled by our custom data reduction pipeline.
We present the optomechanical design and development of the Wide Integral Field Infrared Spectrograph (WIFIS). WIFIS will provide an unrivalled integral field size of 20”×50” for a near-infrared (0.9-1.7 μm) integral-field spectrograph at the 2.3-meter Steward Bok telescope. Its main optomechanical system consists of two assemblies: a room-temperature bench housing the majority of the optical components and a cryostat for a field-flattening lens, thermal blocking filter, and detector. Two additional optical subsystems will provide calibration functionality, telescope guiding, and off-axis optical imaging. WIFIS will be a highly competitive instrument for seeing-limited astronomical investigations of the dynamics and chemistry of extended objects in the near-infrared wavebands. WIFIS is expected to be commissioned during the end of 2016 with scientific operations beginning in 2017.
We present an overview of the design of IRIS, an infrared (0.84 - 2.4 micron) integral field spectrograph and imaging
camera for the Thirty Meter Telescope (TMT). With extremely low wavefront error (<30 nm) and on-board wavefront
sensors, IRIS will take advantage of the high angular resolution of the narrow field infrared adaptive optics system
(NFIRAOS) to dissect the sky at the diffraction limit of the 30-meter aperture. With a primary spectral resolution of
4000 and spatial sampling starting at 4 milliarcseconds, the instrument will create an unparalleled ability to explore high
redshift galaxies, the Galactic center, star forming regions and virtually any astrophysical object. This paper summarizes
the entire design and basic capabilities. Among the design innovations is the combination of lenslet and slicer integral
field units, new 4Kx4k detectors, extremely precise atmospheric dispersion correction, infrared wavefront sensors, and a
very large vacuum cryogenic system.
Maximizing the grating efficiency is a key goal for the first light instrument IRIS (Infrared Imaging Spectrograph)
currently being designed to sample the diffraction limit of the TMT (Thirty Meter Telescope). Volume Phase
Holographic (VPH) gratings have been shown to offer extremely high efficiencies that approach 100% for high line
frequencies (i.e., 600 to 6000l/mm), which has been applicable for astronomical optical spectrographs. However, VPH
gratings have been less exploited in the near-infrared, particularly for gratings that have lower line frequencies. Given
their potential to offer high throughputs and low scattered light, VPH gratings are being explored for IRIS as a potential
dispersing element in the spectrograph. Our team has procured near-infrared gratings from two separate vendors. We
have two gratings with the specifications needed for IRIS current design: 1.51-1.82μm (H-band) to produce a spectral
resolution of 4000 and 1.19-1.37μm (J-band) to produce a spectral resolution of 8000. The center wavelengths for each
grating are 1.629μm and 1.27μm, and the groove densities are 177l/mm and 440l/mm for H-band R=4000 and J-band
R=8000, respectively. We directly measure the efficiencies in the lab and find that the peak efficiencies of these two
types of gratings are quite good with a peak efficiency of ~88% at the Bragg angle in both TM and TE modes at H-band,
and 90.23% in TM mode, 79.91% in TE mode at J-band for the best vendor. We determine the drop in efficiency off the
Bragg angle, with a 20-23% decrease in efficiency at H-band when 2.5° deviation from the Bragg angle, and 25%-28%
decrease at J-band when 5° deviation from the Bragg angle.
We present the efficiency of near-infrared reflective ruled diffraction gratings designed for the InfraRed Imaging
Spectrograph (IRIS). IRIS is a first light, integral field spectrograph and imager for the Thirty Meter Telescope
(TMT) and narrow field infrared adaptive optics system (NFIRAOS). IRIS will operate across the near-infrared
encompassing the ZYJHK bands (~0.84 - 2.4μm) with multiple spectral resolutions. We present our experimental
setup and analysis of the efficiency of selected reflective diffraction gratings. These measurements are used as a
comparison sample against selected candidate Volume Phase Holographic (VPH) gratings (see Chen et al., this
conference). We investigate the efficiencies of five ruled gratings designed for IRIS from two separate vendors.
Three of the gratings accept a bandpass of 1.19-1.37μm (J band) with ideal spectral resolutions of R=4000 and
R=8000, groove densities of 249 and 516 lines/mm, and blaze angles of 9.86° and 20.54° respectively. The other
two gratings accept a bandpass of 1.51-1.82μm (H Band) with an ideal spectral resolution of R=4000, groove
density of 141 lines/mm, and blaze angle of 9.86°. The fraction of flux in each diffraction mode was compared to
both a pure reflection mirror as well as the sum of the flux measured in all observable modes. We measure the
efficiencies off blaze angle for all gratings and the efficiencies between the polarization transverse magnetic (TM)
and transverse electric (TE) states. The peak reflective efficiencies are 98.90 ± 3.36% (TM) and 84.99 ± 2.74%
(TM) for the H-band R=4000 and J-band R=4000 respectively. The peak reflective efficiency for the J-band R=8000
grating is 78.78 ± 2.54% (TE). We find that these ruled gratings do not exhibit a wide dependency on incident angle
within ±3°. Our best-manufactured gratings were found to exhibit a dependency on the polarization state of the
incident beam with a ~10-20% deviation, consistent with the theoretical efficiency predictions. This work will
significantly contribute to the selection of the final grating type and vendor for the IRIS optical system, and are also
pertinent to current and future near-infrared astronomical spectrographs.
We are designing and constructing a new SETI (Search for Extraterrestrial Intelligence) instrument to search for direct
evidence of interstellar communications via pulsed laser signals at near-infrared wavelengths. The new instrument
design builds upon our past optical SETI experiences, and is the first step toward a new, more versatile and sophisticated
generation of very fast optical and near-infrared pulse search devices. We present our instrumental design by giving an
overview of the opto-mechanical design, detector selection and characterization, signal processing, and integration
procedure. This project makes use of near-infrared (950 - 1650 nm) discrete amplification Avalanche Photodiodes
(APD) that have > 1 GHz bandwidths with low noise characteristics and moderate gain (~104). We have investigated the
use of single versus multiple detectors in our instrument (see Maire et al., this conference), and have optimized the
system to have both high sensitivity and low false coincidence rates. Our design is optimized for use behind a 1m
telescope and includes an optical camera for acquisition and guiding. A goal is to make our instrument relatively
economical and easy to duplicate. We describe our observational setup and our initial search strategies for SETI targets,
and for potential interesting compact astrophysical objects.
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