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1. [CII] luminosity models and large-scale image cubes based on COSMOS 2020 and ALPINE-ALMA [CII] data back to the epoch of reionisation

   https://doi.org/10.1051/0004-6361/202450300  

   Clarke, J; Karoumpis, C; Riechers, D; Magnelli, B; Okada, Y; Dev, A; Nikola, T; Bertoldi, F (September 2024, Astronomy & Astrophysics)

   Aims.We have implemented a novel method to create simulated [CII] emission line intensity mapping (LIM) data cubes using COSMOS 2020 galaxy catalogue data. It allows us to provide solid lower limits for previous simulation-based model predictions and the expected signal strength of upcoming surveys. Methods.We applied [CII]158 μm luminosity models to COSMOS 2020 to create LIM cubes covering a 1.2 × 1.2deg²sky area. These models were derived using galaxy bulk property data from the ALPINE-ALMA survey over the redshift range of 4.4 < z < 5.9, while additional models were taken from the literature. The LIM cubes cover 3.42 < z < 3.87, 4.14 < z < 4.76, 5.34 < z < 6.31, and 6.75 < z < 8.27, matched to planned observations from the EoR-Spec module of the Prime-Cam instrument in the Fred Young Submillimeter Telescope (FYST). We also created predictions including additional galaxies below current detection limits by ‘extrapolating’ from the faint end of the COSMOS 2020 luminosity function, comparing these to predictions from the literature. In addition, we computed the signal-to-noise (S/N) ratios for the power spectra, using parameters from the planned FYST survey with predicted instrumental noise levels. Results.We find lower limits for the expected power spectrum using the likely incomplete empirical data: when normalised by 2π², the amplitudes atk = 1 Mpc⁻¹are 3.06 × 10⁷, 1.43 × 10⁷, 9.80 × 10⁵, 2.77 × 10⁵ (Jy sr⁻¹)²for the aforementioned redshift ranges. For the extrapolated sample, the power spectra are consistent with prior predictions, indicating that extrapolation is a viable method for creating mock LIM cubes. In this case, we expect a result of S/N> 1 when using FYST parameters. However, our high-redshift results remain inconclusive because of the poor completeness of COSMOS 2020 atz > 6.3. These predictions will be improved on the basis of future JWST data. 

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2. CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope

   https://doi.org/10.3847/1538-4365/ac9838  

   CCAT-Prime Collaboration; Aravena, Manuel; Austermann, Jason E.; Basu, Kaustuv; Battaglia, Nicholas; Beringue, Benjamin; Bertoldi, Frank; Bigiel, Frank; Bond, J. Richard; Breysse, Patrick C.; et al (December 2022, The Astrophysical Journal Supplement Series)

   Abstract We present a detailed overview of the science goals and predictions for the Prime-Cam direct-detection camera–spectrometer being constructed by the CCAT-prime collaboration for dedicated use on the Fred Young Submillimeter Telescope (FYST). The FYST is a wide-field, 6 m aperture submillimeter telescope being built (first light in late 2023) by an international consortium of institutions led by Cornell University and sited at more than 5600 m on Cerro Chajnantor in northern Chile. Prime-Cam is one of two instruments planned for FYST and will provide unprecedented spectroscopic and broadband measurement capabilities to address important astrophysical questions ranging from Big Bang cosmology through reionization and the formation of the first galaxies to star formation within our own Milky Way. Prime-Cam on the FYST will have a mapping speed that is over 10 times greater than existing and near-term facilities for high-redshift science and broadband polarimetric imaging at frequencies above 300 GHz. We describe details of the science program enabled by this system and our preliminary survey strategies. 

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3. Design of the SPT-SLIM Focal Plane: A Spectroscopic Imaging Array for the South Pole Telescope

   https://doi.org/10.1007/s10909-022-02843-4  

   Barry, P. S.; Anderson, A.; Benson, B.; Carlstrom, J. E.; Cecil, T.; Chang, C.; Dobbs, M.; Hollister, M.; Karkare, K. S.; Keating, G. K.; et al (September 2022, Journal of Low Temperature Physics)

   Abstract The Summertime Line Intensity Mapper (SLIM) is a mm-wave line-intensity mapping (mm-LIM) experiment for the South Pole Telescope (SPT). The goal of SPT-SLIM is to serve as a technical and scientific pathfinder for the demonstration of the suitability and in-field performance of multi-pixel superconducting filterbank spectrometers for future mm-LIM experiments. Scheduled to deploy in the 2023-24 austral summer, the SPT-SLIM focal plane will include 18 dual-polarisation pixels, each coupled to an$$R = \lambda / \Delta \lambda = 300$$ $R=\lambda /\Delta \lambda =300$thin-film microstrip filterbank spectrometer that spans the 2 mm atmospheric window (120–180 GHz). Each individual spectral channel feeds a microstrip-coupled lumped-element kinetic inductance detector, which provides the highly multiplexed readout for the 10k detectors needed for SPT-SLIM. Here, we present an overview of the preliminary design of key aspects of the SPT-SLIM focal plane array, a description of the detector architecture and predicted performance, and initial test results that will be used to inform the final design of the SPT-SLIM spectrometer array. 

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4. Characterization and performance of the upgraded NIRSPEC on the W. M. Keck Telescope

   https://doi.org/10.1117/12.2563075  

   Lopez, Ronald A.; Hoffman, Erika; Doppmann, Gregory; Fitzgerald, Michael P.; Johnson, Chris; Kassis, Marc; Lanclos, Kyle; Lyke, Jim; Martin, Emily C.; McLean, Ian; et al (December 2020, SPIE Astronomical Telescopes & Instrumentation 2020 Proceedings)

   Evans, Christopher J.; Bryant, Julia J.; Motohara, Kentaro (Ed.)

   NIRSPEC is a high-resolution near-infrared echelle spectrograph on the Keck II telescope that was commissioned in 1999 and upgraded in 2018. This recent upgrade was aimed at improving the sensitivity and longevity of the instrument through the replacement of the spectrometer science detector (SPEC) and slit-viewing camera (SCAM). Commissioning began in 2018 December, producing the first on-sky images used in the characterization of the upgraded system. Through the use of photometry and spectroscopy of standard stars and internal calibration lamps, we assess the performance of the upgraded SPEC and SCAM detectors. First, we evaluate the gain, readnoise, dark current, and the charge persistence of the spec detector. We then characterize the newly upgraded spectrometer and the resulting improvements in sensitivity, including spectroscopic zero points, pixel scale, and resolving power across the spectrometer detector field. Finally, for SCAM, we present zero points, pixel scale, and provide a map of the geometric distortion of the camera. 

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5. A Water Vapor Radiometer for the CO Mapping Array Project (COMAP)

   https://doi.org/10.23919/USNC-URSINRSM57470.2023.10043109  

   Kim, Junhan; Cleary, Kieran A.; O’Neill, Sandra; Lamb, James W.; Woody, David P.; Harris, Andrew I.; Dunne, Delaney A.; Catha, Morgan; Hobbs, Richard; Kocz, Jonathon; et al (January 2023, 2023 United States National Committee of URSI National Radio Science Meeting (USNC-URSI NRSM))

   The CO Mapping Array Project (COMAP) is a carbon monoxide (CO) line intensity mapping experiment using a 19-feed 26–34 GHz focal plane spectrometer array on a 10.4 m dish at the Owens Valley Radio Observatory. We are developing a water vapor radiometer (WVR) that continuously measures the temporal variability of the atmosphere’s water vapor content along the telescope’s line of sight to better calibrate the COMAP science data. The WVR is designed to monitor the rotational transition line of water vapor around 22.2 GHz, with a spectral measurement between 18 and 26 GHz and a measurement of continuum at 28–30 GHz. Here we describe the COMAP WVR instrument system. 

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