Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: (Left) Simulated redshift slice of the area covered by the [C II] intensity mapping survey in the epoch of reionization (EoR), representing a small spectral bin (2.7 GHz wide, or Δ z = 0.07 at the adopted redshift) within the vast z = 3.5–8.0 redshift range covered by the EoR-Spec DSS [C II] measurements. (Right) Power spectrum of the [C II] emission, revealing the topology of reionization and the [C II] luminosity functions at redshifts of 3.7 to 7.5. The range of recent model predictions (solid lines; Silva et al. 2015; Serra et al. 2016; Dumitru et al. 2019; Chung et al. 2020) differs by factors of 10 to 50, and an ensemble of state-of-the-art models from C. Karoumpis et al. (2021, in preparation) spans an order of magnitude in power spectrum predictions at each redshift. Overlaid are our predicted EoR-Spec sensitivities. Our proposed survey is as much as 10× more sensitive than other proposed surveys (TIME; Crites et al. 2014; Sun et al. 2021; CONCERTO; Concerto Collaboration et al. 2020; raw sensitivities are shown for all experiments) leading to an expectation for detection of the intensity mapping signal at redshifts approaching 8 for most models. ALMA cannot make these measurements, since its field of view is smaller than a single pixel of EoR-Spec on FYST so that it requires enormous numbers of pointings to map the large spatial scales required for these measurements. Furthermore, an interferometer is insensitive to extended low surface brightness emission and individual faint sources below its point-source detection limit, which would be recovered by the intensity mapping signal.