The SCALES instrument is a high-contrast imager and integral field spectrograph that operates in the infrared wavelength and is intended to be utilized behind W.M. Keck Observatory’s adaptive optics system. The instrument operates over a broad wavelength range from 1.0 to 5.0 μm. The instrument includes a microlens array-based integral field spectrograph that is used with slicer optics and allows for low (R ∼ 35 - 250) and moderate (R ∼ 2000 - 6500) spectral resolution spectroscopy. We have implemented end-to-end modeling of the SCALES instrument optics using both geometric optics and physical optics. This analysis has been useful to understand the spectral formats, spectral resolution, and point spread functions. We have also modeled the geometric PSF from lenslets and combined it with the diffraction effects to model the crosstalk between the closely spaced lenslet spectra. The psf modeling are being integrated with the SCALES simulator to simulate realistic data products that are being used to develop the SCALES data pipeline.
The Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES) is a 2 μm to 5 μm, high-contrast Integral Field Spectrograph (IFS) currently being built for Keck Observatory. With both low (R ≲ 250) and medium (R approximately 3500 to 7000) spectral resolution IFS modes, SCALES will detect and characterize significantly colder exoplanets than those accessible with near-infrared (approximately 1 μm to 2 μm) high-contrast spectrographs. This will lead to new progress in exoplanet atmospheric studies, including detailed characterization of benchmark systems that will advance the state of the art of atmospheric modeling. SCALES’ unique modes, while designed specifically for direct exoplanet characterization, will enable a broader range of novel (exo)planetary observations as well as galactic and extragalactic studies. Here we present the science cases that drive the design of SCALES. We describe an end-to-end instrument simulator that we use to track requirements and show simulations of expected science yields for each driving science case. We conclude with a discussion of preparations for early science when the instrument sees first light in approximately 2025.
Hanle echelle spectrograph (HESP) is a high resolution, bench mounted, fiber-fed spectrograph at visible wavelengths. The instrument was recently installed at the 2m Himalayan Chandra Telescope (HCT), located at Indian Astronomical Observatory (IAO), Hanle at an altitude of 4500m. The telescope and the spectrograph are operated remotely from Bangalore,(∼ 3200km from Hanle), through a dedicated satellite link. HESP was designed and built by Kiwi Star Optics, Callaghan Innovation, New Zealand. The spectrograph has two spectral resolution modes (R=30000 and 60000). The low resolution mode uses a 100 micron fiber as a input slit and the high resolution mode is achieved using an image slicer. An R2 echelle grating, along with two cross dispersing prisms provide a continuous wavelength coverage between 350-1000nm. The spectrograph is enclosed in a thermally controlled environment and provides a stability of 200m/s during a night. A simultaneous thorium-argon calibration provides a radial velocity precision of 20m/s. Here, we present a design overview, performance and commissioning of the spectrograph.
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