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The VIRUS2 instrument is a new fiber-fed multiplexed integral field spectrograph consisting of 6 units, each with 4 spectral channels, to provide large on-sky area coverage coupled with broad spectral coverage. VIRUS2 will be a new facility instrument on the McDonald Observatory 2.7 m Harlan J Smith Telescope. The instrument employs a novel beam-switch module within the fiber feed to split the light into the 4 spectral channels covering 370-930 nm at R~2000, while achieving a very compact and highly stable instrument. The design of VIRUS2 emphasizes stability and careful calibration, with scrambling in the beam-switch module, compact spectrograph format, and tight thermal control. This is the first time such measures have been employed at moderate spectral resolution. In this paper, we provide an overview of the instrument and the build status of the 24 spectrographs, dete ield units. VIRUS2 is funded by NSF and deployment is planned in the second half of 2021.

We present observations of the stellar kinematics of the centre of the core collapsed globular cluster M15 obtained with the MUSE integral field spectrograph on the Very Large Telescope operating in narrow field mode. Thanks to the use of adaptive optics, we obtain a spatial resolution of 0.1 arcsec and are able to reliably measure the radial velocities of 864 stars within 8 arcsec of the centre of M15, thus providing the largest sample of radial velocities ever obtained for the innermost regions of this system. Combined with previous observations of M15 using MUSE in wide field mode and literature data, we find that the central kinematics of M15 are complex with the rotation axis of the core of M15 offset from the rotation axis of the bulk of the cluster. While this complexity has been suggested by previous work, we confirm it at higher significance and in more detail., CU acknowledges the support of the Swedish Research Council, Vetenskapsrådet. SK gratefully acknowledges funding from UKRI in the form of a Future Leaders Fellowship (grant no. MR/T022868/1) and financial support from the European Research Council (ERC-CoG-646928, Multi-Pop). MG acknowledges support from the Ministry of Science and Innovation through a Europa Excelencia grant (EUR2020-112157). VHB acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) through grant RGPIN-2020-05990. EB acknowledges financial support from a Vici grant by the Netherlands Organisation for Scientific Research (NWO).

The 2 m-aperture Survey Space Telescope (also known as the China Space Station Telescope, CSST) is a major science project of China Manned Space Program. It is expected to start science operations around 2024 and has a nominal mission lifetime of 10 years. During observations, CSST will fly independently in the same orbit as the space station while maintaining a large distance apart. It can dock with the space station for refueling and servicing as scheduled or as needed. With a Cook-type three-mirror anastigmat design, CSST can achieve superior image quality within a large field of view (FoV), which gives it an advantage for survey observations. Being an off-axis telescope without any obstruction, its point spread function (PSF) is not affected by diffraction of mirror support structures and is thus helpful for weak-lensing shear measurements. The radius encircling 80% energy of the PSF within CSST’s central 1.1 square degrees of FoV is required to be no more than 0.15″, including all wavefront errors in the optics and instruments and dynamical effects such as the telescope’s attitude control and vibration. CSST will be launched with 5 first-generation instruments including a survey camera, a terahertz receiver, a multichannel imager, an integral field spectrograph, and a cool planet imaging coronagraph. The survey camera is equipped with 30 9k×9k detectors for science observations, each with a filter or grating mounted above, a defocused 9k×9k detector for flux calibration in r band, 8 640×512 near-infrared detectors, fine guide sensors, and wavefront sensors. The primary task of CSST is to carry out a high-resolution large-area multiband imaging and slitless spectroscopy survey covering the wavelength range of 255–1000 nm. Precision cosmology is the main science driver of the survey, and, therefore, the main area of sky selected for observation is at median-to-high galactic latitude and median-to-high ecliptic latitude. It will take the survey camera roughly 7 years of operation accumulated over 10 years of orbital time to image roughly 17500 square degrees of the sky in NUV, u, g, r, i, z, and y bands and take slitless spectroscopy of the same sky in 3 bands. The point-source 5σ limiting magnitudes in g and r bands can reach 26 (AB mag) or higher. The spectral resolution ( R = λ /Δ λ ) of the slitless spectrograph is specified to be on average no less than 200, and the wide-band-equivalent limiting magnitudes in GV (400–620 nm) and GI (620–1000 nm) bands will reach 23 or higher. In addition, a number of deep fields will be selected for more observations to reach at least one magnitude deeper than the wide-area survey. The combined advantage of its angular resolution, depth, wavelength range, capability of both imaging and spectroscopy and large-area sky coverage makes the CSST survey highly competitive, and, at the same time, its observations are also highly complementary with other large projects of its time, such as Vera Rubin Observatory, Euclid, and Roman Space Telescope. These projects will provide extremely rich datasets for potential breakthroughs in studies from the solar system to cosmology and beyond.

We investigated the interstellar medium (ISM) properties in the central regions of nearby Seyfert galaxies characterised by prominent conical or bi-conical outflows belonging to the MAGNUM survey by exploiting the unprecedented sensitivity, spatial and spectral coverage of the integral field spectrograph MUSE at the Very Large Telescope. We developed a novel approach based on the gas and stars kinematics to disentangle high-velocity gas in the outflow from gas in the disc to spatially track the differences in their ISM properties. This allowed us to reveal the presence of an ionisation structure within the extended outflows that can be interpreted with different photoionisation and shock conditions, and to trace tentative evidence of outflow-induced star formation (''positive'' feedback) in a galaxy of the sample, Centaurus A., 5 pages, 3 figures. To appear in Proceedings of IAU Symposium 359 (T. Storchi-Bergmann, R. Overzier, W. Forman & R. Riffel, eds.)

The DIVING3D Survey (Deep Integral Field Spectrograph View of Nuclei of Galaxies) aims to observe, with high signal/noise and high spatial resolution, a statistically complete sample of southern galaxies brighter than B = 12.0 The main objectives of this survey are to study: 1) the nuclear emission line properties; 2) the circumnuclear emission line properties; 3) the central stellar kinematics and 4) the central stellar archaeology. Preliminary results of individual or small groups of galaxies have been published in 18 papers.

We investigate the processes of active galactic nuclei (AGN) feeding and feedback in the narrow line regions (NLRs) and host galaxies of nearby AGN through spatially resolved spectroscopy with the Gemini Near-Infrared Integral Field Spectrograph (NIFS) and the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS). We examine the connection between nuclear and galactic inflows and outflows by adding long-slit spectra of the host galaxies from Apache Point Observatory. We demonstrate that nearby AGN can be fueled by a variety of mechanisms. We find that the NLR kinematics can often be explained by in situ ionization and radiative acceleration of ambient gas, often in the form of dusty molecular spirals that may be the fueling flow to the AGN.

I report the discovery of a transient broad-Hα point source in the outskirts of the giant elliptical galaxy NGC 1404, discovered in archival observations taken with the Multi-Unit Spectroscopic Explorer (MUSE) integral field spectrograph. The Hα line width of 1950 km s−1 full width at half-maximum, and luminosity of (4.1 ± 0.1) × 1036 erg s−1, are consistent with a nova outburst, and the source is not visible in MUSE data obtained 9 months later. A transient soft X-ray source was detected at the same position (within

KIDSpec, the Kinetic Inductance Detector Spectrograph, is a concept for a highly sensitive, medium-spectral-resolution optical through near-IR spectrograph. It uses the intrinsic-energy-resolving capability of an array of optical/IR-sensitive MKIDs to distinguish multiple orders from a low-resolution grating. By acting as an ‘order resolver,’ the MKID array replaces the cross-disperser in an echelle spectrograph. This greatly simplifies the optical layout of the spectrograph and enables longer slits than are possible with cross-dispersed instruments (to improve sky subtraction). KIDSpec would have similar capabilities to ESO’s highly successful X-shooter instrument. It would provide an R = 4000–10,000 spectrum covering the optical and near-IR spectral range (0.4–1.5 µm). As well as a ‘long-slit’ mode, the IFU would provide a small ($$\sim 50\hbox { spaxel}$$∼50spaxel) field of view for spatially resolved sources. In addition, the photon-counting operation of MKIDs and their photon-energy-resolving ability enable a read-noise-free spectrum with perfect cosmic ray removal. The spectral resolution would be sufficient to remove the bright night-sky lines without the additional pixel noise, making the instrument more sensitive than an equivalent semiconductor-based instrument. KIDSpec would enhance many existing high-profile science cases, including transient (GRB, SNe, etc.) follow-up, redshift determination of faint objects and transit spectroscopy of exoplanets. In addition, it will enable unique science cases, such as dynamical mass estimates of the compact objects in ultra-compact binaries.

We present an exposure time calculator (ETC) developed for polarimetric observing modes for two next-generation high-contrast direct imaging instruments planned for the W. M. Keck Observatory: SCALES1 (Santa Cruz Array of Lenslets for Exoplanet Spectroscopy), a low-resolution mid-infrared integral field spectrograph; and a future polarimetric observing mode for NIRC2, the near-infrared adaptive optics (AO) supported high-contrast direct imager currently on the Keck Observatory. In addition to producing estimates of companion signal-to-noise ratios (SNR, see Fig. 2a), the ETC calculates the polarization fraction that would be detected with a user-specific SNR in a given exposure time (see Fig. 2b). The ETC includes a graphical user interface and is packaged as a polarimetry add-on to the PSI-Red thermal imaging module of PSISim, an instrument performance simulation tool for the Planetary Systems Imager2 - a modular suite of AO-supported instruments planned for the Thirty Meter Telescope

We present preliminary laboratory cryogenic test results for the Coronagraph Slide mechanism, which allows observers the choice of up to 4 coronagraphic focal plane masks when using SCALES (Santa Cruz Array of Lenslets for Exoplanet Spectroscopy). SCALES is a 2-5 micron high-contrast lenslet integral field spectrograph currently undergoing preliminary design for the W. M. Keck Observatory. When deployed behind the Keck Adaptive Optics system, SCALES will be used to detect and characterize a wide variety of exoplanets. To minimize thermal emission, all optical and mechanical components of SCALES are fully cryogenic. The Coronagraph Slide is the first fully cryogenic mechanism for SCALES designed, built, and tested in-house at UCSC with mostly off-the-shelf components.

To directly detect exoplanets and protoplanetary disks, the development of high accuracy wavefront sensing and control (WFS&C) technologies is essential, especially for ground-based Extremely Large Telescopes (ELTs). The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a high-contrast imaging platform to discover and characterize exoplanets and protoplanetary disks. It also serves as a testbed to validate and deploy new concepts or algorithms for high-contrast imaging approaches for ELTs, using the latest hardware and software technologies on an 8-meter class telescope. SCExAO is a multi-band instrument, using light from 600 to 2500 nm, and delivering a high Strehl ratio (>80% in median seeing in H-band) downstream of a low-order correction provided by the facility AO188. Science observations are performed with coronagraphs, an integral field spectrograph, or single aperture interferometers. The SCExAO project continuously reaches out to the community for development and upgrades. Existing operating testbeds such as the SCExAO are also unique opportunities to test and deploy the new technologies for future ELTs. We present and show a live demonstration of the SCExAO capabilities (Real-time predictive AO control, Focal plane WFS&C, etc) as a host testbed for the remote collaborators to test and deploy the new WFS&C concepts or algorithms. We also present several high-contrast imaging technologies that are under development or that have already been demonstrated on-sky., 13 pages, 8 figures, 2021 SPIE Optics+Photonics

We present first results from a new exoplanet direct imaging survey being carried out with the Subaru Coronagraphic Extreme Adaptive Optics project coupled with the CHARIS integral field spectrograph. Our survey targeting stars showing evidence for a statistically significant astrometric acceleration from the Hipparcos and Gaia satellites implying the existence of substellar or planetary companions at sub-arcsecond separations.. JHK low-resolution spectra from CHARIS constrain newly-discovered companion spectral types, temperatures, and gravities. Relative astrometry of companions from SCExAO/CHARIS and absolute astrometry of the star from Hipparcos and Gaia together yield direct dynamical mass constraints, circumventing usual challenges in inferring the masses of imaged planets from luminosity evolution models. Even in its infancy, our survey has already yielded multiple discoveries, including at least one likely jovian planet at a moderate orbital separation and multiple other substellar companions. We describe how our small nascent survey is yielding a far higher detection rate than large blind surveys from GPI and SPHERE and the path forward for imaging and characterizing planets at lower masses and smaller orbital separations than previously possible.

The Ultraviolet Micromirror Imaging Spectrograph (UMIS) will be the first UV integral field spectrograph (IFS) to use micro-electro-mechanical systems (MEMS) micromirrors, specifically in the form of two-axis analog micromirror arrays (AMAs). This novel application of AMAs will increase both the flexibility and spectral multiplexing efficiency of UMIS relative to currently available instruments. AMAs are already a widely used technology in telecommunications; this study investigated and proved their suitability for high performance scientific instrumentation. Suitability was determined through evaluation of the individual micromirror component on a custom optical bench set up. The following metrics were evaluated: temporal stability, thermal drift and stability, large-scale linear response and pointing precision. The tests demonstrated that under conditions of 20C - 40C the micromirror's temporal stability, thermal stability, large-scale linear response and pointing precision were stable within the required range. The micromirror's performance, as measured in this experiment, meets the requirements specified in UMIS design and indicates feasibility for future flight instruments. We present the experiment test setup and results in the context of the development of the UMIS testbed instrument.

The INtegral Field Ultraviolet Spectroscopic Experiment (INFUSE), a sounding rocket payload under development at the University of Colorado Laboratory for Atmospheric and Space Physics, will be the first far ultraviolet (1000 - 2000 A° ) integral field spectrograph (IFS) in space. With access to part of the Lyman ultraviolet (1000 - 1216 A° ), INFUSE will study spectral emission lines such as O VI in extended objects at greater spatial resolution and grasp than has previously been possible. An F/16, 0.49 m Cassegrain telescope feeds the instrument. A 26-element image slicer provided by Canon Inc. forms the basis for the IFS. Each reflective slice acts as a long-slit, creating 26 different channels. Each channel is re-focused and dispersed by one of 26 identical holographic gratings supplied by Horiba JY onto the same 94 x 94 mm cross-strip (XS) microchannel plate detector (MCP). This MCP, provided by Sensor Sciences, will be the largest MCP of its type ever flown in space and will be advancing high event rate photon-counting detector technology for future NASA missions. We discuss the process of aligning the instrument, with a focus on the method by which the 26 gratings are aligned with the image slicer. Additionally, we examine the challenges presented by mounting and coating the large primary mirror and the steps taken to ensure that the mirror remains stable in flight. The first flight of INFUSE is projected for Spring 2023 when it will spectroscopically image the XA region of the Cygnus Loop at the interface between the supernova and the ambient ISM, studying shock fronts in the supernova remnant.

We describe a new high-contrast imaging capability well suited for studying planet-forming disks: near-infrared (NIR) high-contrast spectropolarimetric imaging with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) integral field spectrograph (IFS). The advent of extreme adaptive optics (AO) systems, like SCExAO, has enabled recovery of planet-mass companions at the expected locations of gas-giant formation in young disks alongside disk structures (such as gaps or spirals) that may indicate protoplanet formation. In combination with SCExAO, the CHARIS IFS in polarimetry mode allows characterization of these systems at wavelengths spanning the NIR J, H, and K bands ($1.1-2.4$ $\mu m$, $R\sim20$) and at angular separations as small as 0.04". By comparing the resulting images with forward-modeled scattered light or 3D radiative-transfer models, the likely origins of any observed features can be assessed. Utilization of swift optimization algorithms, such as differential evolution (DE), to identify model parameters that best reproduce the observations allows plausible disk geometries to be explored efficiently. The recent addition of CHARIS's unique integral field spectropolarimetry mode has further facilitated the study of planet-forming disks -- aiding in the confirmation of candidate protoplanets, the diagnosis of disk structures, and the characterization of dust grain populations. We summarize preliminary results for two young planet-forming disk systems based on observations with the novel integral field spectropolarimetry mode for SCExAO/CHARIS., Comment: 20 pages, 8 figures

We report the direct imaging discovery of a low-mass companion to the nearby accelerating A star, HIP 109427, with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument coupled with the MKID Exoplanet Camera (MEC) and CHARIS integral field spectrograph. CHARIS data reduced with reference star PSF subtraction yield 1.1-2.4 $\mu$m spectra. MEC reveals the companion in $Y$ and $J$ band at a comparable signal-to-noise ratio using stochastic speckle discrimination, with no PSF subtraction techniques. Combined with complementary follow-up $L_{\rm p}$ photometry from Keck/NIRC2, the SCExAO data favors a spectral type, effective temperature, and luminosity of M4-M5.5, 3000-3200 $K$, and $\log_{10}(L/L_{\rm \odot}) = -2.28^{+0.04}_{-0.04}$, respectively. Relative astrometry of HIP 109427 B from SCExAO/CHARIS and Keck/NIRC2, and complementary Gaia-Hipparcos absolute astrometry of the primary favor a semimajor axis of $6.55^{+3.0}_{-0.48}$ au, an eccentricity of $0.54^{+0.28}_{-0.15}$, an inclination of $66.7^{+8.5}_{-14}$ degrees, and a dynamical mass of $0.280^{+0.18}_{-0.059}$ $M_{\odot}$. This work shows the potential for extreme AO systems to utilize speckle statistics in addition to widely-used post-processing methods to directly image faint companions to nearby stars near the telescope diffraction limit., Comment: 13 pages, 7 figures, 3 tables

HARMONI is the first light visible and near-infrared (NIR) integral field spectrograph for the Extremely Large Telescope(ELT). The HARMONI spectrograph will have four near-infrared cameras and two visible, both with seven lenses of various materials and diameters ranging from 286 to 152 mm. The lens mounts design has been optimized for each lens material to compensate for thermal stresses and maintain lens alignment at the operational temperature of 130 K. We discuss their design and mounting concept, as well as assembly and verification steps. We show initial results from two prototypes and outline improvements in the mounting procedures to reach tighter lens alignments. To conclude, we present a description of our future work to measure the decentering of the lenses when cooled down and settled.

Integral field spectrographs (IFS) have transformed studies of low-redshift spatially resolved galaxies as they provide simultaneous spectral coverage over contiguous spatial regions. IFS surveys of galaxies have allowed for observations of the spatially varying physical diagnostics of galaxy disks. Though IFS instruments have been traditionally limited to small fields of view (FOV), on the order of 100 square arcseconds, constraining the extent to which IFS studies can map the most nearby galaxies. Small FOV have also restricted IFS studies of large galaxy samples to pre-selected targets. Scaling up the fields of IFS instruments is challenging due to the limited number of spatial elements that can be imaged on a single CCD. To cost effectively scale up IFS capability in order to observe larger fields, the Visible Integral-field Replicable Unit Spectrograph (VIRUS) utilizes massive replication on an unprecedented 100-fold scale to be able to image ∼35,000 fibers over a ∼22 arcminute FOV with a single observation. VIRUS consists of up to 78 replicable units, each with two integral field spectrograph channels. The VIRUS design takes advantage of large-scale replication of simple units to significantly reduce engineering and production costs of building a facility instrument of this scale. With VIRUS being 156 realizations of the same spectrograph and the first to be replicated on this massive scale, I present analysis that uncovers the statistical variations in performance of these units along with an assessment of cost/tolerance trade offs of scaling up instrument capabilities through massively replicated designs. The VIRUS instrument was designed to conduct the Hobby Eberly Telescope Dark Energy Experiment (HETDEX) which intends to build a sample of nearly a million Lyα emitting galaxies (LAEs) from 1.9

This thesis is focused on the development and testing of a new instrument capable of finding and characterizing recently-formed Jupiter-sized planets orbiting other stars. To observe these planets, I present the design, construction and testing of the Gemini Planet Imager (GPI) Integral Field Spectrograph (IFS). GPI is a facility class instrument for the Gemini Observatory with the primary goal of directly detecting young Jovian planets. The GPI IFS utilizes an infrared transmissive lenslet array to sample a rectangular 2.7 × 2.7 arcsecond field of view and provide low-resolution spectra across five bands between 1 and 2.5 μm. The dispersing element can be replaced with a Wollaston prism to provide broadband polarimetry across the same five filter bands. The IFS construction was based at the University of California, Los Angeles in collaboration with the Université de Montréal, Immervision and Lawrence Livermore National Laboratory.I will present performance results, from in-lab testing, of the Integral Field Spectrograph (IFS) for the Gemini Planet Imager (GPI). The IFS is a large, complex, cryogenic, optical system requiring several years of development and testing. I will present the design and integration of the mechanical and optical performance of the spectrograph optics. The IFS passed its pre-ship review in 2011 and was shipped to University of California, Santa Cruz for integration with the remaining sub-systems of GPI. The UCLA built GPI IFS was integrated with the rest of GPI and is delivering high quality spectral datacubes of GPI's coronagraphic field.Using the NIRC2 instrument located at the Keck Observatory, my collaborators and I observed the planetary companion to beta Pictoris in L' (3.5--4.1μm). Observations taken in the fall of 2009 and 2012 are used to find the location and inclination of the planet relative to the massive debris disk orbiting beta Pictoris. We find that the planet's orbit has a position angle on the sky of 211.9±0.4 degrees, making the planet misaligned by 2.9±0.5 degrees from the main disk, consistent with other observations that β Pic b is misaligned with the main disk, and part of the misaligned inner disk. In 2009 & 2012 we find a projected orbital separation of 312.8 ± 18.3 and 466.35 ± 8.4 milliarcseconds consistent with an orbital period of ∼ 20 years, and a semi-major axis of ∼ 9 AU as found by Macintosh et al. (2014).During the first commissioning observations with the Gemini Planet Imager (GPI), my collaborators and I took the first H-band spectrum of the planetary companion to the nearby young star beta Pictoris. The spectrum has a resolving power of ∼ 45 and demonstrates the distinctive triangular shape of a cool substellar object with low surface gravity. Using atmospheric models, we find an effective temperature of 1650 ± 50K and a surface gravity of log(g) = 4.0 ± 0.25 (cgs units). These values agree well with predictions from planetary evolution models for a gas giant with mass between 10 and 12 MJup and age between 10 and 20 Myrs. The spectrum is very similar to a known low mass field brown dwarf but has more flux at the long wavelength end of the filters compared to models. Given the very high signal-to-noise of our spectrum this likely indicates additional physics such as patchy clouds that need to be included in the model.

The IRIS Exposure Time Calculator (ETC) was designed to be a publicly available aid to the astronomical community in the development of science cases for the Infrared Imaging Spectrograph (IRIS) and future proposal planning. The IRIS ETC is developed from the IRIS simulator in which the signal-to-noise calculation is done pixel-by-pixel for 2D and 3D data. The IRIS ETC makes use of simulated Narrow Field InfraRed Adaptive Optics System (NFIRAOS) point spread functions sampling the performance at key positions across the focal plane of the IRIS imager and Integral Field Spectrograph, with varying adaptive optics performances and atmospheric conditions. Like the IRIS simulator, we model the near-infrared background with variable OH emission lines and thermal emission from the atmosphere to provide accurate noise estimates. The IRIS ETC is designed to work with the hundreds of modes given the combination of filters and grating selection. The framework, developed in Python and making use of Astropy and Photutils, can handle any 2D or 3D data input and therefore can be easily adapted for any current or future near-infrared instrument.

BlueMUSE (Blue Multi Unit Spectroscopic Explorer) is a blue-optimised, medium spectral resolution, panoramic integral field spectrograph proposed for the Very Large Telescope (VLT) and based on the MUSE concept. BlueMUSE will open up a new range of galactic and extragalactic science cases allowed by its specific capabilities in the 350 - 580 nm range: an optimised end-to-end transmission down to 350 nm, a larger FoV (up to $1.4 \times 1.4$ arcmin$^2$) sampled at 0.3 arcsec, and a higher spectral resolution ($\lambda/\Delta \lambda \sim 3500$) compared to MUSE. To our knowledge, achieving such capabilities with a comparable mechanical footprint and an identical detector format ($4\text{k} \times 4\text{k}$, 15 $\mathrm{\mu m}$ CCD) would not be possible with a conventional spectrograph design. In this paper, we present the optomechanical architecture and design of BlueMUSE at pre-phase A level, with a particular attention to some original aspects such as the use of curved detectors.

NGC 7469 is a well-known luminous infrared galaxy, with a circumnuclear star formation ring ∼830 pc radius) surrounding a Seyfert 1 active galactic nucleus (AGN). Nuclear unresolved winds were previously detected in X-rays and ultraviolet, as well as an extended biconical outflow in infrared coronal lines. We search for extended outflows by measuring the kinematics of the Hβ and [O III] λ5007 optical emission lines, in data of the Very Large Telescope/Multi-unit Spectroscopic Explorer integral field spectrograph. We find evidence of two outflow kinematic regimes: One slower regime extending across most of the star formation (SF) ring-possibly driven by the massive SF-and a faster regime (with a maximum velocity of -715 km s-1), only observed in [O III], in the western region between the AGN and the massive star-forming regions of the ring, likely AGN-driven. This work shows a case where combined AGN/SF feedback can be effectively spatially resolved, opening up a promising path toward a deeper understanding of feedback processes in the central kiloparsec of AGN, Support from CONACyT (Mexico) grant CB-2016-01-286316 is acknowledged. J.P.T.P. acknowledges DAIP-UGto (Mexico) for granted support (0173/2019). Y.A. acknowledges support from project PID2019-107408GB-C42 (Ministerio de Ciencia e Innovación, Spain). S.F.S. thanks the support of CONACYT grants CB-285080 and FC-2016-01- 1916, and funding from the PAPIIT-DGAPA-IN100519 (UNAM) project. L.G. was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). E.B acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. This research has been partially funded by the Spanish State Research Agency (AEI) Project MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC)

Combining high-contrast imaging with medium-resolution spectroscopy has been shown to significantly boost the direct detection of exoplanets. HARMONI, one of the first-light instruments to be mounted on ESO's ELT, will be equipped with a single-conjugated adaptive optics system to reach the diffraction limit of the ELT in H and K bands, a high-contrast module dedicated to exoplanet imaging, and a medium-resolution (up to R = 17 000) optical and near-infrared integral field spectrograph. Combined together, these systems will provide unprecedented contrast limits at separations between 50 and 400 mas. In this paper, we estimate the capabilities of the HARMONI high-contrast module for the direct detection of young giant exoplanets. We use an end-to-end model of the instrument to simulate observations based on realistic observing scenarios and conditions. We analyze these data with the so-called "molecule mapping" technique combined to a matched-filter approach, in order to disentangle the companions from the host star and tellurics, and increase the S/N of the planetary signal. We detect planets above 5-sigma at contrasts up to 16 mag and separations down to 75 mas in several spectral configurations of the instrument. We show that molecule mapping allows the detection of companions up to 2.5 mag fainter compared to state-of-the-art high-contrast imaging techniques based on angular differential imaging. We also demonstrate that the performance is not strongly affected by the spectral type of the host star, and that we reach close sensitivities for the best three quartiles of observing conditions at Armazones, which means that HARMONI could be used in near-critical observations during 60 to 70% of telescope time at the ELT. Finally, we simulate planets from population synthesis models to further explore the parameter space that HARMONI and its high-contrast module will soon open., Accepted for publication in A&A (14 pages, 9 figures)

We present the design and lab performance of a prototype lenslet-slicer hybrid integral field spectrograph (IFS), validating the concept for use in future instruments like SCALES/PSI-Red. By imaging extrasolar planets with IFS, it is possible to measure their chemical compositions, temperatures and masses. Many exoplanet-focused instruments use a lenslet IFS to make datacubes with spatial and spectral information used to extract spectral information of imaged exoplanets. Lenslet IFS architecture results in very short spectra and thus low spectral resolution. Slicer IFSs can obtain higher spectral resolution but at the cost of increased optical aberrations that propagate through the down-stream spectrograph and degrade the spatial information we can extract. We have designed a lenslet/slicer hybrid that combines the minimal aberrations of the lenslet IFS with the high spectral resolution of the slicer IFS. The slicer output f/\# matches the lenslet f/\# requiring only additional gratings., Comment: 8 pages, 9 figures, SPIE Optical Engineering + Applications 2021

Context. In recent decades, direct imaging has confirmed the existence of substellar companions (exoplanets or brown dwarfs) on wide orbits (>10 au) around their host stars. In striving to understand their formation and evolution mechanisms, in 2015 we initiated the SPHERE infrared survey for exoplanets (SHINE), a systematic direct imaging survey of young, nearby stars that is targeted at exploring their demographics. Aims. We aim to detect and characterize the population of giant planets and brown dwarfs beyond the snow line around young, nearby stars. Combined with the survey completeness, our observations offer the opportunity to constrain the statistical properties (occurrence, mass and orbital distributions, dependency on the stellar mass) of these young giant planets. Methods. In this study, we present the observing and data analysis strategy, the ranking process of the detected candidates, and the survey performances for a subsample of 150 stars that are representative of the full SHINE sample. Observations were conducted in a homogeneous way between February 2015 and February 2017 with the dedicated ground-based VLT/SPHERE instrument equipped with the IFS integral field spectrograph and the IRDIS dual-band imager, covering a spectral range between 0.9 and 2.3 μm. We used coronographic, angular, and spectral differential imaging techniques to achieve the best detection performances for this study, down to the planetary mass regime. Results. We processed, in a uniform manner, more than 300 SHINE observations and datasets to assess the survey typical sensitivity as a function of the host star and of the observing conditions. The median detection performance reached 5σ-contrasts of 13 mag at 200 mas and 14.2 mag at 800 mas with the IFS (YJ and YJH bands), and of 11.8 mag at 200 mas, 13.1 mag at 800 mas, and 15.8 mag at 3 as with IRDIS in H band, delivering one of the deepest sensitivity surveys thus far for young, nearby stars. A total of sixteen substellar companions were imaged in this first part of SHINE: seven brown dwarf companions and ten planetary-mass companions.These include two new discoveries, HIP 65426 b and HIP 64892 B, but not the planets around PDS70 that had not been originally selected for the SHINE core sample. A total of 1483 candidates were detected, mainly in the large field of view that characterizes IRDIS. The color-magnitude diagrams, low-resolution spectrum (when available with IFS), and follow-up observations enabled us to identify the nature (background contaminant or comoving companion) of about 86% of our subsample. The remaining cases are often connected to crowded-field follow-up observations that were missing. Finally, even though SHINE was not initially designed for disk searches, we imaged twelve circumstellar disks, including three new detections around the HIP 73145, HIP 86598, and HD 106906 systems. Conclusions. Nowadays, direct imaging provides a unique opportunity to probe the outer part of exoplanetary systems beyond 10 au to explore planetary architectures, as highlighted by the discoveries of: one new exoplanet, one new brown dwarf companion, and three new debris disks during this early phase of SHINE. It also offers the opportunity to explore and revisit the physical and orbital properties of these young, giant planets and brown dwarf companions (relative position, photometry, and low-resolution spectrum in near-infrared, predicted masses, and contrast in order to search for additional companions). Finally, these results highlight the importance of finalizing the SHINE systematic observation of about 500 young, nearby stars for a full exploration of their outer part to explore the demographics of young giant planets beyond 10 au and to identify the most interesting systems for the next generation of high-contrast imagers on very large and extremely large telescopes. © M. Langlois et al. 2021. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zürich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European CommissionSixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012) and grant number 312430 for FP7 (2013-2016). This paper is based on observations collected at the European Southern Observatory under ESO programmes 198.C-0209, 097.C-0865, 095.C-0298, 095.C-0309,096.C-0241. This work has made use of the SPHERE Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and Observatoire de Lyon (OSUL/CRAL). This work is supported by the French National Research Agency in the framework of the Investissements d’Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life” project of the Univ. Grenoble-Alpes. This work is jointly supported by the French National Programms (PNP and PNPS) and by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES. We also thank the anonymous referee for her/his careful reading of the manuscript as well as her/his insightful comments and suggestions. AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). A.-M.L. acknowledges funding from French National Research Agency (GIPSE project). C.P. acknowledges financial support from Fondecyt (grant 3190691) and financial support from the ICM (Iniciativa Científica Milenio) via the Núcleo Milenio de Formación Planetaria grant, from the Universidad de Valparaíso. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 832428.

We present recent results from our MAGNUM survey of nearby active galactic nuclei (AGN), which exploits observations from the optical/near-IR integral field spectrograph MUSE at VLT. We detect strongly enhanced line widths in emission line maps of four galaxies perpendicularly to their low-power jets and AGN ionisation cones, indicative of turbulent/outflowing material. The observation of a similar phenomenon in other works suggests that it originates from an interaction mechanism between the jet and the galaxy disc through which it propagates.

The advantage of having a high-fidelity instrument simulation tool developed in tandem with novel instrumentation is having the ability to investigate, in isolation and in combination, the wide parameter space set by the instrument design. SCALES, the third generation thermal-infrared diffraction limited imager and low/med-resolution integral field spectrograph being designed for Keck, is an instrument unique in design in order to optimize for its driving science case of direct detection and characterization of thermal emission from cold exoplanets. This warranted an end-to-end simulation tool that systematically produces realistic mock data from SCALES to probe the recovery of injected signals under changes in instrument design parameters. In this paper, we quantify optomechanical tolerance and detector electronic requirements set by the fiducial science cases using information content analysis, and test the consequences of updates to the design of the instrument on meeting these requirements., Comment: 7 pages, 4 figures, SPIE Optical Engineering and Applications 2021

IRIS (Infrared Imaging Spectrograph) is the near-infrared (0.84 to 2.4 micron) diffraction-limited imager and Integral Field Spectrograph (IFS) designed for the Thirty Meter Telescope (TMT) and the Narrow-Field Infrared Adaptive Optics System ( NFIRAOS ). The imager will have a 34 arcsec x 34 arcsec field of view with 4 milliarcseconds (mas) pixels. The IFS consists of a lenslet array and slicer, enabling four plate scales from 4 mas to 50 mas, with multiple gratings and filters. We will report the progress on the development of the IRIS Data Reduction System ( DRS ) in the final design phase. The IRIS DRS is being developed in Python with the software architecture based on the James Webb Space Telescope science calibration pipeline. We are developing a library of algorithms as individual Python classes that can be configured independently and bundled into pipelines. We will interface this with the observatory software to run online during observations and we will release the package publicly for scientists to develop custom analyses. It also includes a C library for readout processing to be used for both in real-time processing (e.g., up-the-ramp, MCDS) as well the ability for astronomers to use for offline reduction. Lastly, we will also discuss the development of the IRIS simulation packages that simulate raw spectra and image readout-data from the Hawaii-4RG detectors, which helps in developing reduction algorithms during this design phase., Software and Cyberinfrastructure for Astronomy VI, December 14-18, 2020, Online Only, United States, Series: Proceedings of SPIE

HARMONI is the first light visible and near-infrared integral field spectrograph for the Extremely Large Telescope. It covers a broad spectral range from 450 nm to 2450 nm with resolving powers from R (≡λ/Δλ)3500 to 18000 and spatial sampling from 60 mas to 4 mas. The HARMONI optical design is predominantly reflective, with approximately 25 mirrors in the science path. We, therefore, want to maximise the instrument transmission by procuring the best reflective coatings for our optics. Reflective dielectric coatings offer better performance than metallic coatings but are challenging for our wide wavelength range. We discussed with several companies and purchased from Asahi Spectra and Optics Balzers. On average, the theoretical reflectance of the provided coatings is higher than 99% with features. To ensure the applicability of the coatings for HARMONI, we tested the coating survivability of the procured samples considering their adherence, cryogenic cycling endurance, and cleaning ease. We report reflectance measurements for one of our AOI design ranges. We also discuss which of HARMONI's many reflective surfaces we could coat considering their optics size and surface shape.

We present recent results obtained with the VLT/MUSE Integral Field Spectrograph fed by the 4LGSF and its laser tomography adaptive optics module GALACSI. While this so-called narrow-field mode of MUSE was not designed to perform directly imaging of exoplanets and outflows, we show that it can be a game changer to detect and characterize young exoplanets with a prominent emission lines (i.e Hα, tracer of accretion), at moderate contrasts. These performances are achieved thanks to the combo of a near-diffraction limited PSF and a medium resolution spectrograph and a cross-correlation approach in post-processing . We discuss this in the context of ground and space, infrared and visible wavelengths, preparing for missions like JWST and WFIRST in great synergy and as pathfinder for future ELT/GSMT (Extremely Large and/or Giant Segmented Mirror Telescopes) instruments.

HARMONI is the first light visible and near-infrared (450 – 2450 nm, λ/Δλ = 3,000 – 17,000) integral field spectrograph for the European Southern Observatory’s Extremely Large Telescope. The path for scientific light includes pre-optics to set the field of view (4 – 60 mas), an integral field unit to reformat the rectangular field into four 540 mm long slits, and four spectrographs which collimate, disperse, and image the light. The spectrographs collimate the input slits using a system of three off-axis, aspheric mirrors which lack a common optical axis. We have demonstrated the alignment procedure of this three-mirror anastigmat in numerical simulations. We will initially align the collimator mirrors by measuring reference features with a coordinate measuring machine (CMM). We will then use an interferometer to measure the wavefront error (WFE) at positions along the input slit. These WFE measurements will be entered into a numerical model to optimize available compensators, and the corresponding adjustments will be applied to the collimator. This process of measuring WFE, using a model to determine optimal compensator adjustments, and applying the adjustments will be repeated until the performance has converged. As an initial demonstration of this method, we have simulated the full alignment procedure. The modelled systems include manufacturing errors, account for the uncertainty of values reported by mirror manufacturers, and simulate the CMM and interferometer alignment steps. Nearly all of 1000 instances meet our requirements after two iterations of the optical alignment, and all were found to satisfy our requirements after five iterations.

The Paranal Instrumentation Programme is responsible for planning and delivering the instruments and the associated infrastructures needed to keep the VLT and La Silla Observatories at the forefront of ground-based astronomy. With the completion of commissioning of the AOF, ESPRESSO, the AO system for the four VLTI Auxiliary Telescopes (NAOMI) and the two VLTI instruments GRAVITY, MATISSE, Gravity for Matisse fringe tracking, all second generation VLT instruments are now offered to the users. CRIRES upgrade is currently in full commissioning at VLT and the exo-planet science instrument NIRPS spectrograph is on its way to the 3.6 m telescope at La Silla. By keeping the foreseen roadmap (start one new instrument or upgrade every year), the programme is now completing the AO imager and IFU ERIS, an upgrade of AOF narrow field mode: IRLOS and is integrating the two MOS Instruments MOONS and 4MOST. A dedicated La Silla NTT instrument to transient science SOXS is also in construction. Ph

The MCAO Assisted Visible Imager and Spectrograph (MAVIS) is a facility-grade visible MCAO instrument, currently under development for the Adaptive Optics Facility at the VLT. The adaptive optics system will feed both an imager and an integral field spectrograph, with unprecedented sky coverage of 50% at the Galactic Pole. The imager will deliver diffraction-limited image quality in the V band, cover a 30" x 30" field of view, with imaging from U to z bands. The conceptual design for the spectrograph has a selectable field-of-view of 2.5" x 3.6", or 5" x 7.2", with a spatial sampling of 25 or 50 mas respectively. It will deliver a spectral resolving power of R=5,000 to R=15,000, covering a wavelength range from 380 - 950 nm. The combined angular resolution and sensitivity of MAVIS fill a unique parameter space at optical wavelengths, that is highly complementary to that of future next-generation facilities like JWST and ELTs, optimised for infrared wavelengths. MAVIS will facilitate a broad range of science, including monitoring solar system bodies in support of space missions; resolving protoplanetary- and accretion-disk mechanisms around stars; combining radial velocities and proper motions to detect intermediate-mass black holes; characterising resolved stellar populations in galaxies beyond the local group; resolving galaxies spectrally and spatially on parsec scales out to 50 Mpc; tracing the role of star clusters across cosmic time; and characterising the first globular clusters in formation via gravitational lensing. We describe the science cases and the concept designs for the imager and spectrograph.

HARMONI is the adaptive optics assisted, near-infrared and visible light integral field spectrograph for the Extremely Large Telescope (ELT). A first light instrument, it provides the work-horse spectroscopic capability for the ELT. As the project approaches its Final Design Review milestone, the design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument's capabilities from a user perspective, provide a summary of the instrument's design, including plans for operations and calibrations, and provide a brief glimpse of the predicted performance for a specific observing scenario. The paper also provides some details of the consortium composition and its evolution since the project commenced in 2015.

We are building an image slicer integral field unit (IFU) to go on the IMACS wide-field imaging spectrograph on the Magellan Baade Telescope at Las Campanas Observatory, the Reformatting Optically-Sensitive IMACS Enhancement IFU, or ROSIE IFU. The 50.4" x 53.5" field of view will be pre-sliced into four 12.6" x 53.5" subfields, and then each subfield will be divided into 21 0.6" x 53.5" slices. The four main image slicers will produce four pseudo-slits spaced six arcminutes apart across the IMACS f/2 camera field of view, providing a wavelength coverage of 1800 Angstroms at a spectral resolution of 2000. Optics are in-hand, the first image slicer is being aluminized, mounts are being designed and fabricated, and software is being written. This IFU will enable the efficient mapping of extended objects such as nebulae, galaxies, or outflows, making it a powerful addition to IMACS., 12 pages, 9 figures, 2 tables, submitted to SPIE

The Gemini Planet Imager (GPI) is a dedicated high-contrast imaging facility designed for the direct detection and characterization of young Jupiter mass exoplanets. After six yrs of operation at Gemini South, GPI has helped establish that Jovian planets are rare at wide separations, but have higher occurrence rates at small separations. This motivates an upgrade of GPI to achieve deeper contrasts, especially at small inner working angles, while leveraging its current capabilities. GPI has been funded to undergo a major science-driven upgrade as part of a relocation to Gemini North (GN). Gemini plans to remove GPI at the end of 2020A. We present the status of the proposed upgrades to GPI including a EMCCD-based pyramid wavefront sensor, broadband low spectral resolution prisms and new apodized-pupil Lyot coronagraph designs. We discuss the expected performance improvements in the context of GPI 2.0's enhanced science capabilities which are scheduled to be made available at GN in 2022., SPIE Astronomical Telescopes + Instrumentation, December 14-18, 2020, Online Only, United States, Series: Proceedings of SPIE

HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from R (≡λ/Δλ) 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 instrument uses a field splitter and image slicer to divide the field into 4 sub-units, each providing an input slit to one of four nearly identical spectrographs. This proceeding presents the final opto- mechanical design and the AIV plan of the spectrograph units.

BlueMUSE is a blue-optimised, medium spectral resolution, panoramic integral field spectrograph based on the MUSE concept and proposed for the Very Large Telescope. With an optimised transmission down to 350 nm, a larger FoV (1.4 × 1.4 arcmin2) and a higher spectral resolution (λ/Δλ ~ 4000) compared to MUSE, BlueMUSE will open up a new range of galactic and extragalactic science cases allowed by its specific capabilities in the 350-580nm range, beyond those possible with MUSE. In this paper, we present the optomechanical architecture and design of BlueMUSE at pre-phase A level, with a particular attention to some original aspects such as the use of curved detectors.

The InfraRed Imaging Spectrograph (IRIS) is a first-light instrument for the Thirty Meter Telescope (TMT) that will be used to sample the corrected adaptive optics field by the Narrow-Field Infrared Adaptive Optics System (NFIRAOS) with a near-infrared (0.8 - 2.4 µm) imaging camera and integral field spectrograph. To better understand IRIS science specifications we use the IRIS data simulator to characterize relative photometric precision and accuracy across the IRIS imaging camera 34”x34” field of view. Because the Point Spread Function (PSF) varies due to the effects of anisoplanatism, we use the Anisoplanatic and Instrumental Reconstruction of Off-axis PSFs for AO (AIROPA) software package to conduct photometric measurements on simulated frames using PSF-fitting as the PSF varies in single-source, binary, and crowded field use cases. We report photometric performance of the imaging camera as a function of the instrumental noise properties including dark current and read noise. Using the same methods, we conduct comparisons of photometric performance with reconstructed PSFs, in order to test the veracity of the current PSF-Reconstruction algorithms for IRIS/TMT., Ground-based and Airborne Instrumentation for Astronomy VIII, December 14-18, 2020, Online Only, United States, Series: Proceedings of SPIE

We will present the status of the next generation near-infrared (0.84 - 2.45 micron) imager and integral field spectrograph (IFS) instrument, Liger, that is being designed for the W. M. Keck Observatory. The Liger imager and IFS operates concurrently on-sky and are optimized to sample the Keck All-sky Precision Adaptive optics (KAPA) system. The Liger IFS design is able to offer new science capabilities by extending to bluer wavelength coverage, larger field of views, and range of spectral resolving powers. We will discuss the overall Liger technical design, science requirements, and implementation plans for the entire program.

HARMONI is the first-light visible and near-IR integral field spectrograph for the E-ELT. Non-Common Path Aberrations between the Adaptive Optics channel and the science path are the main limitation for direct imaging of exoplanets. The next generation of Extremely Large Telescopes will require advanced techniques for NCPA calibration to exploit their full capabilities and open up a new era of exoplanet discoveries. Calibrating these aberrations with conventional techniques like Phase Diversity can become problematic when the instrument contains an image slicer (such as HARMONI and PCS for the E-ELT). In this context, we have characterised the impact of image slicers on the PSF, and developed an alternative approach to NCPA calibration based on Machine Learning, which can discriminate between intrinsic slicer effects and aberrations features in the PSF.

Liger is a next-generation near-infrared imager and integral field spectrograph (IFS) for the W.M. Keck Observatory designed to take advantage of the Keck All-Sky Precision Adaptive Optics (KAPA) upgrade. Liger will operate at spectral resolving powers between R$\sim$4,000 - 10,000 over a wavelength range of 0.8-2.4$\mu$m. Liger takes advantage of a sequential imager and spectrograph design that allows for simultaneous observations between the two channels using the same filter wheel and cold pupil stop. We present the design for the filter wheels and pupil mask and their location and tolerances in the optical design. The filter mechanism is a multi-wheel design drawing from the heritage of the current Keck/OSIRIS imager single wheel design. The Liger multi-wheel configuration is designed to allow future upgrades to the number and range of filters throughout the life of the instrument. The pupil mechanism is designed to be similarly upgradeable with the option to add multiple pupil mask options. A smaller wheel mechanism allows the user to select the desired pupil mask with open slots being designed in for future upgrade capabilities. An ideal pupil would match the shape of the image formed of the primary and would track its rotation. For different pupil shapes without tracking we model the additional exposure time needed to achieve the same signal to noise of an ideal pupil and determine that a set of fixed masks of different shapes provides a mechanically simpler system with little compromise in performance., Comment: 9 pages, 7 figures, 1 table

VIRUS2 is a new NSF-funded facility instrument on the McDonald Observatory Harlan J Smith 2.7m Telescope. The instrument is a fiber-fed multiplexed integral field spectrograph consisting of 6 units, each with 4 spectral channels, to provide large on-sky area coverage coupled with broad spectral coverage. A novel beam switch module is implemented in the fiber feed which separates light into the pass bands of the four spectral channels. This paper details the mechanical design of the spectrograph, cryostat, and the beam switch module. A unique method for precise six degree of freedom positioning of the CCD detectors is presented, along with process for determination of required adjustments. Results from prototype testing and first article production is included.

HARMONI is the first light visible and near-infrared (450 - 2450 nm,λ/Δλ = 3500 - 18000) integral field spectrograph (IFS) for the European Southern Observatory's Extremely Large Telescope (ELT). Spectroscopic observations from ground-based telescopes in these wavelengths are contaminated by emission from molecules in the Earth's atmosphere, called skylines. Conventional means of removing these skylines requires spending up to half of the telescope time on observing blank sky exposures. Observations with IFS can circumvent this inefficiency by making use of sky models from science exposure themselves to remove the background, called on- IFU sky-subtraction. However, this has not been achieved in practice as it requires an accurate knowledge on the Line Spread Function (LSF) of the spectrograph. The information on the LSF is also useful in telluric calibration of science observations, especially in case of telluric standards that underfill the slits. In this manuscript, we present a tunable Fabry-perot design which will be used to characterise the LSF of HARMONI. The Fabry- perot etalon will operate over HARMONI's entire wavelength range and spectral resolving powers. The design presented in this manuscript has the potential to be adapted for any spectroscopic instrument in the future, and fundamentally change the way we have been observing with IFS instruments.