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: Contiguous wide-area multiwavelength Prime-Cam surveys will measure the dust-obscured star formation properties of hundreds of thousands of galaxies out to z ∼ 6 with high precision. This will greatly enhance our picture of cosmic galaxy evolution, probing 2–3 times lower luminosities than Herschel-SPIRE at z > 1 (due to source confusion; see insets in upper left panel) while sampling large-scale environments (voids, average density regions, groups, and clusters) over 100 times larger areas than feasible to map with ALMA (the field of view of ALMA is a fraction of a single Prime-Cam pixel) and providing more accurate dust-obscured star formation measurements than current or future millimeter-only surveys. Upper left: sky coverage of the CIB-Mid survey (i.e., ∼100 deg2) compared to the dark matter distribution at z ∼ 1.4 from the Millennium simulation (Springel et al. 2018). Insets illustrate how the improved angular resolution of Prime-Cam helps going deeper into the source confusion than was possible with the Herschel 3.5 m telescope. Lower left: survey area needed to detect at least one halo of mass, M h, at a redshift, z, within a redshift bin, Δz = 0.1 × z, as inferred using the halo mass function of Murray et al. (2013). Different lines correspond to different halo masses. This plot only includes structures that will likely be within our field of view, not which ones would be detectable, as that depends on the occupation of these structures by DSFGs. These structure will by identified by other means (e.g., X-ray, optical) and studied by Prime-Cam through either direct detection or stacking analysis. Upper right: simulated Prime-Cam survey luminosity limits, compared to surveys feasible with existing instrumentation covering the 250–500 μm wavelength range, which is critical to measure accurately the infrared luminosity of 1 ≲ z ≲ 6 galaxies. Prime-Cam will probe up to 2–3 times deeper than Herschel-SPIRE, while sampling luminosities inaccessible to small (e.g., ALMA) surveys because of the rarity of luminous objects. These limits are illustrated by the gray and black areas, i.e., there will be less than 10 galaxies more luminous than these limits within a redshift bin, ﹩{\rm{\Delta }}z=\max (0.15\times z,0.5)﹩ in a survey of 2 or 100 deg2, as inferred using the model of Béthermin et al. (2017). Lower right: predicted reliability (16th to 84th percentiles) of FIR luminosity measurements, highlighting the vast improvements with the short submillimeter-wavelength Prime-Cam 350 μm (850 GHz) band and wide spectral coverage. These reliabilities were inferred by fitting (or renormalizing) single modified blackbody function with β = 1.5 and T dust ∈ [20–50 K] (e.g., Magnelli et al. 2012) to the variety of SEDs from the Draine & Li (2007) template library. See text for detailed description of this procedure. At all redshifts, we use the same set of SEDs—we assume no redshift evolution in LIR. Errors improve at higher redshift because we probe closer to the SED peak, and thus any dust temperature dependency becomes less problematic (see also Figure 9 of Schreiber et al. 2015).