SIRMOS (Satellite for Infrared Multi-Object Spectroscopy) is a SMEX mission concept to map the universe in 3D over a cosmic volume of ~ 500 cubic gigaparsecs using 131 million H-alpha and [OIII] emission line galaxies (optimal for tracing cosmic large-scale structure) at 1 < z < 4. SIRMOS will probe the cosmic origin by placing unprecedented constraints on primordial non-Gaussianity, advance fundamental physics by precisely measuring the sum of neutrino masses, and definitively differentiate dark energy and modification of general relativity as the cause for the observed low-redshift cosmic acceleration. SIRMOS will measure galaxy evolution before and during the peak era of cosmic star formation over three orders of magnitude in environmental density, from cluster cores to cosmic filaments. SIRMOS has a 50 cm aperture telescope with 1.6 square degree FoV, and more than 4.4 million micromirrors on 2 digital micro-mirror devices (DMDs) to provide a programmable reflective slit mask allowing multi-slit spectroscopy at R~1300 over the wavelength range of 1.25 to 2.5 microns and a total survey area of 15,000 square degrees. The telescope is a modified Cassegrain followed by a prism mirror that splits the field toward 2 identical arms. Fore-optics reimage each subfield onto a DMD. The micro-mirrors in ON positions send the light to a spectrograph while those in OFF positions send the light to an imager which permits very precise measurements of the telescope pointing and everything not selected for spectroscopy.
In May 2024, the SOAR Adaptive-Module Optical Spectrograph (SAMOS) was installed at the SOAR 4.1 meter telescope in Cerro Pach´on, Chile. We discuss the instrument commissioning process, the integrated system performance, and first light results. SAMOS is a digital micromirror device (DMD)-based multi-object spectrograph and imager designed for use with the SOAR adaptive module ground-layer adaptive optics system. SAMOS covers 4000 Å to 9500 ˚A with a 3′ ×3′ field of view. The unique layout of the instrument allows for the spectroscopic and imaging channels to operate in parallel. While integrating spectral targets, the observer can simultaneously perform photometry on the remainder of the field, improving the spectro-photometric calibration compared to a conventional multi-object spectrograph. In SAMOS, the DMD is used as a reconfigurable slit mask that redistributes slits near-instantaneously. The spectrograph operates in a low resolution and high resolution mode with R∼2500 and R∼6500 respectively for a 0.33′′ slit width. We discuss the work completed during initial commissioning of the instrument and report the first light results.
We present a status update on SCORPIO, the next facility instrument for the Gemini South telescope at Cerro Pachon, Chile. SCORPIO is now in advanced Assembly, Integration and Verification phase at SWRI (San Antonio) and LICA (Madrid) in anticipation of shipment to Chile by Fall-2025.
SCORPIO (Spectrograph and Camera for the Observation of Rapid Phenomena in the Infrared and Optical) is a multiband instrument covering 0.385um to 2.35um in spectroscopy and 0.400um to 2.35um in imaging, currently under development for the Gemini Observatory. The instrument is intended to be deployed as a facility instrument at Gemini South in Chile to enable detailed follow-up observations of transients detected by the Vera C. Rubin Observatory. The instrument is designed with eight parallel channels corresponding to the standard g, r, i, z, Y, J, H, and Ks passbands. Here we present an update on the status of the instrument, the data reduction software, and the current path forward to completion.
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