The CCAT-Prime Submillimeter Observatory

Aravena, M.; Austermann, J.; Basu, Kaustuv; Battaglia, Nicholas; Beringue, Benjamin; Bertoldi, F.; Bond, J. R.; Breysse, Patrick C.; Bustos, R.; Chapman, Scott; Choi, Steve K.; Chung, Dongwoo T.; Cothard, Nicholas F.; Dober, Bradley; Duell, Cody J.; Duff, Shannon M.; Dünner, Rolando; Erler, Jens; Fich, M.; Fissel, Laura M.; Foreman, Simon; Gallardo, Patricio A.; Gao, Jiansong; Giovanelli, Riccardo; Graf, U. U.; Haynes, Martha P.; Herter, T.; Hilton, G. C.; Hložek, Renée; Hubmayr, Johannes; Johnstone, D.; Keating, Laura C.; Komatsu, Eiichiro; Magnelli, B.; Mauskopf, Phil; McMahon, Jeffrey; Meerburg, P. Daniel; Meyers, Joel; Murray, N.; Niemack, Michael D.; Nikola, Thomas; Nolta, Michael R.; Parshley, Stephen C.; Puddu, Roberto; Riechers, Dominik A.; Rosolowsky, Erik; Simon, Sara M.; Stacey, G. J.; Stevens, Jason R.; Stutzki, J.; Engelen, Alexander van; Vavagiakis, Eve M.; Viero, Marco P.; Vissers, Michael; Walker, Samantha; Zou, Bugao

doi:10.48550/arxiv.1909.02587

Cited by 16 publications

(20 citation statements)

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“…In terms of future wide-field surveys that will provide valuable information on CMB "secondaries", there is AdvACT and SPT-3G, with Simons Observatory (SO Collab., 2019) being an ambitious ground-based program that is currently under construction, and then there is the even more ambitious CMB-Stage 4 (CMB-S4 Science Case, 2019) project that is in the planning stages. Large cameras on single-dish mm and submm telescopes (like IRAM or the LMT) perform surveys that are effectively like CMB mapping at higher angular resolutionopportunities here include a new detector array for JCMT, the CCAT-prime project (Aravena et al, 2019) and plans for ATLAST (Klaassen et al, 2019). There are also ideas for surveys from balloons (which can go to even higher frequencies), like BFORE (Bryan et al, 2018).…”

Section: Cmb Experimentsmentioning

confidence: 99%

Cosmology in front of the background: studying the growth of structure at CMB wavelengths

Scott,

Bond,

Chapman

et al. 2019

Preprint

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Canada has thriving communities in CMB (cosmic microwave background) studies, cosmology and submillimetre (submm) astronomy, with involvement in many facilities that featured prominently in previous Astronomy Long Range Plans. The standard cosmological model continues to be well fit using a small number of parameters. No one expects this model to be complete and so we need to continue to challenge it with data; moreover, it does not explain how galaxies and other structures form. So, how do we improve the precision of our understanding of structure formation within this model?Wavelengths from the microwave to the submm will be particularly fruitful for answering this question. That's because, in addition to the CMB anisotropies, there are other signals that can be extracted from large maps at these wavelengths -particularly the cosmic infrared and submm backgrounds, the thermal and kinetic Sunyaev-Zeldovich effects, and CMB lensing. Such signals carry a wealth of information about the cosmological model, as well as how dust, gas and star-formation evolve within dark-matter halos. Cross-correlations between these signals and those coming from the radio, optical and X-ray surveys, will provide even more information.Canadians are already members of teams for several related facilities and are working to be involved in others. In order for Canada to be fully engaged in exploiting the detailed information coming from these cosmological signatures, it is crucial that we find the resources to participate competitively in a combination of projects currently being planned. Examples include CMB-S4, CCAT-prime, AtLAST, a new camera for JCMT, balloon projects such as BFORE and a future ambitious CMB satellite.

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Section: Cmb Experimentsmentioning

confidence: 99%

Cosmology in front of the background: studying the growth of structure at CMB wavelengths

Scott,

Bond,

Chapman

et al. 2019

Preprint

Self Cite

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“…Tentative recent detections of CO intensity shot power spectrum by COPSS [27][28][29] and mmIME [30] surveys, and [CII] emission via cross-correlation between Planck and SDSS quasars [12] have further amplified the growing observational and theoretical interest in LIM. Looking ahead, in addition to several 21-cm surveys, a wide range of ground-and space-based experiments (e.g., COMAP [10], TIME [31], CONCERTO [32], CCAT-prime [33] EXCLAIM [34], SPHEREx [3] and CDIM [35]) will provide higher-fidelity detection of line intensity fluctuations at different redshifts from several emission lines 1 . Success of these surveys will pave the way for next generation wide-field LIM surveys (e.g., [36,37]), capable of providing precision cosmological constraints.…”

Section: Introductionmentioning

confidence: 99%

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

Dizgah,

Nikakhtar,

Keating

et al. 2021

Preprint

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Line intensity mapping (LIM) is an emerging technique with a unique potential to probe a wide range of scales and redshifts. Realizing the full potential of LIM, however, relies on accurate modeling of the signal. We introduce an extended halo model for the power spectrum of intensity fluctuations of CO rotational lines and [CII] fine transition line in real space, modeling nonlinearities in matter fluctuations and biasing relation between the line intensity fluctuations and the underlying dark matter distribution. We also compute the stochastic contributions beyond the Poisson approximation using the halo model framework. To establish the accuracy of the model, we create the first cosmological-scale simulations of CO and [CII] intensity maps, MithraLIMSims, at redshifts 0.5 ≤ z ≤ 6, using halo catalogs from Hidden-Valley simulations, and painting halos according to mass-redshift-luminosity relations for each line. We show that at z = 1 on scales k max 0.8 Mpc −1 h, the model predictions of clustering power (with only two free parameters) are in agreement with the measured power spectrum at better than 5%. At higher redshift of z = 4.5, this remarkable agreement extends to smaller scale of k max 2 Mpc −1 h. Furthermore, we show that on large scales, the stochastic contributions to CO and CII power spectra are non-Poissonian, with amplitudes reproduced reasonably well by the halo model prescription. Lastly, we assess the performance of the theoretical model of the baryon acoustic oscillations (BAO) and show that hypothetical LIM surveys probing CO lines at z = 1, that can be deployed within this decade, will be able to make a high significance measurement of the BAO. On a longer time scale, a space-based mission probing [CII] line can uniquely measure the BAO on a wide range of redshifts at an unprecedented precision.

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“…The rapidly growing instantaneous bandwidth [1][2][3][4][5] and field-of-view [6][7][8] of millimeter-submillimeter (mm-submm) astronomical instruments and telescopes are advantageous not only for collecting more astronomical signal, but also for characterizing and removing the foreground emission of the Earth's atmosphere. 9 Even at the best sites for submm astronomy on ground, the brightness temperature of the Earth's atmosphere in the submm range is ≥20 K, which can be ∼10 3 -10 5 times stronger than the astronomical signal (see Fig.…”

Section: Introductionmentioning

confidence: 99%

“…The requirements for applying such techniques are expected to drive the design of future telescopes and focal-plane instrument systems. [6][7][8] Here we present TiEMPO, the Time-dependent End-to-end Model for Post-process Optimization of the DESHIMA spectrometer. TiEMPO is a numerical model for simulating wideband submm astronomical observations through the Earth's atmosphere, and produces timestream data that can be fed to data-analysis software 11 as if they were taken with a real instrument operated on a telescope.…”

Section: Introductionmentioning

confidence: 99%

TiEMPO: Open-source time-dependent end-to-end model for simulating ground-based submillimeter astronomical observations

Huijten,

Roelvink,

Brackenhoff

et al. 2021

Preprint

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The next technological breakthrough in millimeter-submillimeter astronomy is 3D imaging spectrometry with wide instantaneous spectral bandwidths and wide fields of view. The total optimization of the focal-plane instrument, the telescope, the observing strategy, and the signal-processing software must enable efficient removal of foreground emission from the Earth's atmosphere, which is time-dependent and highly nonlinear in frequency.Here we present TiEMPO : Time-dependent End-to-end Model for Post-process Optimization of the DESHIMA spectrometer. TiEMPO utilizes a dynamical model of the atmosphere and parametrized models of the astronomical source, the telescope, the instrument, and the detector. The output of TiEMPO is a timestream of sky brightness temperature and detected power, which can be analyzed by standard signal-processing software.We first compare TiEMPO simulations with an on-sky measurement by the wideband DESHIMA spectrometer, and find good agreement in the noise power spectral density and sensitivity. We then use TiEMPO to simulate the detection of the line emission spectrum of a high-redshift galaxy using the DESHIMA 2.0 spectrometer in development. The TiEMPO model is open source. Its modular and parametrized design enables users to adapt it to design and optimize the end-to-end performance of spectroscopic and photometric instruments on existing and future telescopes.

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The CCAT-Prime Submillimeter Observatory

Cited by 16 publications

References 0 publications

Cosmology in front of the background: studying the growth of structure at CMB wavelengths

Cosmology in front of the background: studying the growth of structure at CMB wavelengths

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

TiEMPO: Open-source time-dependent end-to-end model for simulating ground-based submillimeter astronomical observations

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