Samenvatting
CMB-S4 - the next-generation ground-based cosmic microwave background (CMB) experiment - is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2-3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5σ, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.
| Originele taal-2 | English |
|---|---|
| Artikelnummer | 54 |
| Tijdschrift | Astrophysical Journal |
| Volume | 926 |
| Nummer van het tijdschrift | 1 |
| DOI's | |
| Status | Published - 11-feb.-2022 |
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- 10.3847/1538-4357/ac1596Licentie: CC BY
- CMB-S4: Forecasting Constraints on Primordial Gravitational WavesFinal publisher's version, 2,18 MBLicentie: CC BY
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In: Astrophysical Journal, Vol. 926, Nr. 1, 54, 11.02.2022.
Onderzoeksoutput › Academic › peer review
TY - JOUR
T1 - CMB-S4
T2 - Forecasting Constraints on Primordial Gravitational Waves
AU - Abazajian, Kevork
AU - Addison, Graeme E.
AU - Adshead, Peter
AU - Ahmed, Zeeshan
AU - Akerib, Daniel
AU - Ali, Aamir
AU - Allen, Steven W.
AU - Alonso, David
AU - Alvarez, Marcelo
AU - Amin, Mustafa A.
AU - Anderson, Adam
AU - Arnold, Kam S.
AU - Ashton, Peter
AU - Baccigalupi, Carlo
AU - Bard, Debbie
AU - Barkats, Denis
AU - Barron, Darcy
AU - Barry, Peter S.
AU - Bartlett, James G.
AU - Basu Thakur, Ritoban
AU - Battaglia, Nicholas
AU - Bean, Rachel
AU - Bebek, Chris
AU - Bender, Amy N.
AU - Benson, Bradford A.
AU - Bianchini, Federico
AU - Bischoff, Colin A.
AU - Bleem, Lindsey
AU - Bock, James J.
AU - Bocquet, Sebastian
AU - Boddy, Kimberly K.
AU - Richard Bond, J.
AU - Borrill, Julian
AU - Bouchet, François R.
AU - Brinckmann, Thejs
AU - Brown, Michael L.
AU - Bryan, Sean
AU - Buza, Victor
AU - Byrum, Karen
AU - Hervias Caimapo, Carlos
AU - Calabrese, Erminia
AU - Calafut, Victoria
AU - Caldwell, Robert
AU - Carlstrom, John E.
AU - Carron, Julien
AU - Cecil, Thomas
AU - Challinor, Anthony
AU - Chang, Clarence L.
AU - Chinone, Yuji
AU - Sherry Cho, Hsiao Mei
AU - Cooray, Asantha
AU - Coulton, Will
AU - Crawford, Thomas M.
AU - Crites, Abigail
AU - Cukierman, Ari
AU - Cyr-Racine, Francis Yan
AU - De Haan, Tijmen
AU - Delabrouille, Jacques
AU - Devlin, Mark
AU - Di Valentino, Eleonora
AU - Dierickx, Marion
AU - Dobbs, Matt
AU - Duff, Shannon
AU - Dvorkin, Cora
AU - Eimer, Joseph
AU - Elleflot, Tucker
AU - Errard, Josquin
AU - Essinger-Hileman, Thomas
AU - Fabbian, Giulio
AU - Feng, Chang
AU - Ferraro, Simone
AU - Filippini, Jeffrey P.
AU - Flauger, Raphael
AU - Flaugher, Brenna
AU - Fraisse, Aurelien A.
AU - Frolov, Andrei
AU - Galitzki, Nicholas
AU - Gallardo, Patricio A.
AU - Galli, Silvia
AU - Ganga, Ken
AU - Gerbino, Martina
AU - Gluscevic, Vera
AU - Goeckner-Wald, Neil
AU - Green, Daniel
AU - Grin, Daniel
AU - Grohs, Evan
AU - Gualtieri, Riccardo
AU - Gudmundsson, Jon E.
AU - Gullett, Ian
AU - Gupta, Nikhel
AU - Habib, Salman
AU - Halpern, Mark
AU - Halverson, Nils W.
AU - Hanany, Shaul
AU - Harrington, Kathleen
AU - Hasegawa, Masaya
AU - Hasselfield, Matthew
AU - Hazumi, Masashi
AU - Heitmann, Katrin
AU - Henderson, Shawn
AU - Hensley, Brandon
AU - Hill, Charles
AU - Colin Hill, J.
AU - Hlozek, Renée
AU - Patty Ho, Shuay Pwu
AU - Hoang, Thuong
AU - Holder, Gil
AU - Holzapfel, William
AU - Hood, John
AU - Hubmayr, Johannes
AU - Huffenberger, Kevin M.
AU - Hui, Howard
AU - Irwin, Kent
AU - Jeong, Oliver
AU - Johnson, Bradley R.
AU - Jones, William C.
AU - Hwan Kang, Jae
AU - Karkare, Kirit S.
AU - Katayama, Nobuhiko
AU - Keskitalo, Reijo
AU - Kisner, Theodore
AU - Knox, Lloyd
AU - Koopman, Brian J.
AU - Kosowsky, Arthur
AU - Kovac, John
AU - Kovetz, Ely D.
AU - Kuhlmann, Steve
AU - Kuo, Chao Lin
AU - Kusaka, Akito
AU - Lähteenmäki, Anne
AU - Lawrence, Charles R.
AU - Lee, Adrian T.
AU - Lewis, Antony
AU - Li, Dale
AU - Linder, Eric
AU - Loverde, Marilena
AU - Lowitz, Amy
AU - Lubin, Phil
AU - Madhavacheril, Mathew S.
AU - Mantz, Adam
AU - Marques, Gabriela
AU - Matsuda, Frederick
AU - Mauskopf, Philip
AU - McCarrick, Heather
AU - McMahon, Jeffrey
AU - Daniel Meerburg, P.
AU - Melin, Jean Baptiste
AU - Menanteau, Felipe
AU - Meyers, Joel
AU - Millea, Marius
AU - Mohr, Joseph
AU - Moncelsi, Lorenzo
AU - Monzani, Maria
AU - Mroczkowski, Tony
AU - Mukherjee, Suvodip
AU - Nagy, Johanna
AU - Namikawa, Toshiya
AU - Nati, Federico
AU - Natoli, Tyler
AU - Newburgh, Laura
AU - Niemack, Michael D.
AU - Nishino, Haruki
AU - Nord, Brian
AU - Novosad, Valentine
AU - O'Brient, Roger
AU - Padin, Stephen
AU - Palladino, Steven
AU - Partridge, Bruce
AU - Petravick, Don
AU - Pierpaoli, Elena
AU - Pogosian, Levon
AU - Prabhu, Karthik
AU - Pryke, Clement
AU - Puglisi, Giuseppe
AU - Racine, Benjamin
AU - Rahlin, Alexandra
AU - Sathyanarayana Rao, Mayuri
AU - Raveri, Marco
AU - Reichardt, Christian L.
AU - Remazeilles, Mathieu
AU - Rocha, Graca
AU - Roe, Natalie A.
AU - Roy, Anirban
AU - Ruhl, John E.
AU - Salatino, Maria
AU - Saliwanchik, Benjamin
AU - Schaan, Emmanuel
AU - Schillaci, Alessandro
AU - Schmitt, Benjamin
AU - Schmittfull, Marcel M.
AU - Scott, Douglas
AU - Sehgal, Neelima
AU - Shandera, Sarah
AU - Sherwin, Blake D.
AU - Shirokoff, Erik
AU - Simon, Sara M.
AU - Slosar, Anze
AU - Spergel, David
AU - St. Germaine, Tyler
AU - Staggs, Suzanne T.
AU - Stark, Antony
AU - Starkman, Glenn D.
AU - Stompor, Radek
AU - Stoughton, Chris
AU - Suzuki, Aritoki
AU - Tajima, Osamu
AU - Teply, Grant P.
AU - Thompson, Keith
AU - Thorne, Ben
AU - Timbie, Peter
AU - Tomasi, Maurizio
AU - Tristram, Matthieu
AU - Tucker, Gregory
AU - Umiltà, Caterina
AU - Van Engelen, Alexander
AU - Vavagiakis, Eve M.
AU - Vieira, Joaquin D.
AU - Vieregg, Abigail G.
AU - Wagoner, Kasey
AU - Wallisch, Benjamin
AU - Wang, Gensheng
AU - Watson, Scott
AU - Westbrook, Ben
AU - Whitehorn, Nathan
AU - Wollack, Edward J.
AU - Kimmy Wu, W. L.
AU - Xu, Zhilei
AU - Eric Yang, H. Y.
AU - Yasini, Siavash
AU - Yefremenko, Volodymyr G.
AU - Won Yoon, Ki
AU - Young, Edward
AU - Yu, Cyndia
AU - Zonca, Andrea
N1 - Funding Information: The CMB-S4 collaboration ( https://cmb-s4.org/ ) is working to plan, construct, and operate a next-generation, multisite CMB experiment in the 2020s. The collaboration is led by an elected Governing Board, Spokespeople, Committee Chairs, and Executive Team. Funding for the CMB-S4 Integrated Project Office is provided by the Department of Energy’s Office of Science (project level CD-0) and by the National Science Foundation through the Mid-Scale Research Infrastructure-R1 award OPP-1935892. This research used resources of Argonne National Laboratory, a U.S. Department of Energy (DOE) Office of Science User Facility operated under Contract No. DE-AC02-06CH11357. This document was prepared by the CMB-S4 collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. Work at Lawrence Berkeley National Laboratory was supported by the Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Work at SLAC National Accelerator Laboratory is supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. In the United States, work on CMB-S4 by individual investigators has been supported by the National Science Foundation (awards 1248097, 1255358, 1815887, 1835865, 1852617, 2009469), the Department of Energy (awards DE-SC0009919, DE-SC0009946, DE-SC0010129, DE-SC0011784), and the National Aeronautics and Space Administration (award ATP-80NSSC20K0518). In Australia, the Melbourne authors acknowledge support from an Australian Research Council Future Fellowship (FT150100074). In Canada, R.H. is supported by the Discovery Grants program from NSERC, and acknowledges funding from CIFAR, the Sloan Foundation, and the Dunlap family. In Italy, C.B. acknowledges support under the ASI COSMOS and INFN INDARK programs. In the Netherlands, D.M. acknowledges NWO VIDI award number 639.042.730. In Switzerland, J.C. is supported by an SNSF Eccellenza Professorial Fellowship (No. 186879). In the United Kingdom, A.L., G.F., and J.C. are supported by the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC grant Agreement No. [616170]. A.L. also acknowledges STFC award ST/P000525/1. S.M. is supported by the research program Innovational Research Incentives Scheme (Vernieuwingsimpuls), which is financed by the Netherlands Organization for Scientific Research through the NWO VIDI grant No. 639.042.612-Nissanke and the Labex ILP (reference ANR-10-LABX-63) part of the Idex SUPER, received financial state aid managed by the Agence Nationale de la Recherche, as part of the program Investissements d’avenir under the reference ANR-11-IDEX-0004-02. Some computations in this paper were run on the Odyssey cluster, supported by the FAS Science Division Research Computing Group at Harvard University. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/2/11
Y1 - 2022/2/11
N2 - CMB-S4 - the next-generation ground-based cosmic microwave background (CMB) experiment - is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2-3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5σ, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.
AB - CMB-S4 - the next-generation ground-based cosmic microwave background (CMB) experiment - is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2-3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5σ, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.
UR - http://www.scopus.com/inward/record.url?scp=85125859842&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac1596
DO - 10.3847/1538-4357/ac1596
M3 - Article
AN - SCOPUS:85125859842
SN - 0004-637X
VL - 926
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 54
ER -