CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

被引：160

作者：

Abazajian, Kevork ^{[1
]}

Addison, Graeme E. ^{[2
]}

Adshead, Peter ^{[3
,4
]}

Ahmed, Zeeshan ^{[5
]}

Akerib, Daniel ^{[5
]}

Ali, Aamir ^{[6
]}

Allen, Steven W. ^{[7
]}

Alonso, David ^{[8
]}

Alvarez, Marcelo ^{[6
,9
]}

Amin, Mustafa A. ^{[10
]}

Anderson, Adam ^{[11
]}

Arnold, Kam S. ^{[12
]}

Ashton, Peter ^{[6
]}

Baccigalupi, Carlo ^{[13
,14
,15
]}

Bard, Debbie ^{[9
]}

Barkats, Denis ^{[16
]}

Barron, Darcy ^{[17
]}

Barry, Peter S. ^{[18
]}

Bartlett, James G. ^{[19
]}

Thakur, Ritoban Basu ^{[20
]}

Battaglia, Nicholas ^{[21
]}

Bean, Rachel ^{[21
]}

Bebek, Chris ^{[9
]}

Bender, Amy N. ^{[18
,22
]}

Benson, Bradford A. ^{[11
,22
,23
]}

Bianchini, Federico ^{[24
]}

Bischoff, Colin A. ^{[25
]}

Bleem, Lindsey ^{[18
,22
]}

Bock, James J. ^{[20
,26
]}

Bocquet, Sebastian ^{[27
]}

Boddy, Kimberly K. ^{[2
,28
]}

Bond, J. Richard ^{[29
]}

Borrill, Julian ^{[6
,9
]}

Bouchet, Francois R. ^{[30
,31
]}

Brinckmann, Thejs ^{[32
]}

Brown, Michael L. ^{[33
]}

Bryan, Sean ^{[34
]}

Buza, Victor ^{[16
,22
]}

Byrum, Karen ^{[18
]}

Caimapo, Carlos Hervias ^{[35
]}

Calabrese, Erminia ^{[36
]}

Calafut, Victoria ^{[21
]}

Caldwell, Robert ^{[37
]}

Carlstrom, John E. ^{[18
,22
,23
]}

Carron, Julien ^{[38
,39
,40
]}

Cecil, Thomas ^{[18
]}

Challinor, Anthony ^{[41
,42
,43
]}

Chang, Clarence L. ^{[18
,22
,23
]}

Chinone, Yuji ^{[44
]}

Cho, Hsiao-Mei Sherry ^{[5
]}

机构：

[1] Univ Calif Irvine, Irvine, CA 92697 USA

[2] Johns Hopkins Univ, Baltimore, MD 21218 USA

[3] Univ Illinois, Illinois Ctr Adv Studies Universe, Urbana, IL 61801 USA

[4] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

[5] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[6] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[7] Stanford Univ, Stanford, CA 94305 USA

[8] Univ Oxford, Oxford OX1 3RH, England

[9] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[10] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA

[11] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[12] Univ Calif San Diego, La Jolla, CA 92093 USA

[13] SISSA Int Sch Adv Studies, Via Bonomea, Trieste, Italy

[14] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

[15] Ist Nazl Fis Nucl, Natl Inst Nucl Phys, Via Valerio 2, I-34127 Trieste, Italy

[16] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[17] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[18] Argonne Natl Lab, Lemont, IL 60439 USA

[19] Univ Paris Diderot, CNRS IN2P3, Lab Astroparticule & Cosmol APC, F-75205 Paris 13, France

[20] CALTECH, Pasadena, CA 91125 USA

[21] Cornell Univ, Ithaca, NY 14853 USA

[22] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[23] Univ Chicago, Chicago, IL 60637 USA

[24] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[25] Univ Cincinnati, Cincinnati, OH 45221 USA

[26] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA

[27] Ludwig Maximilians Univ Munchen, D-81679 Munich, Germany

[28] Univ Texas Austin, Dept Phys, Theory Grp, Austin, TX 78712 USA

[29] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[30] CNRS, Inst Astrophys Paris IAP, Paris, France

[31] Sorbonne Univ, Paris, France

[32] SUNY Stony Brook, Stony Brook, NY 11794 USA

[33] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[34] Arizona State Univ, Tempe, AZ 85287 USA

[35] Florida State Univ, Tallahassee, FL 32306 USA

[36] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales

[37] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA

[38] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[39] Univ Geneva, CAP, CH-1211 Geneva 4, Switzerland

[40] Univ Sussex, Astron Ctr, Sch Math & Phys Sci, Brighton BN1 9QH, E Sussex, England

[41] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England

[42] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England

[43] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[44] Univ Tokyo, Kashiwa, Chiba 2778583, Japan

[45] Univ Groningen, Van Swinderen Inst Particle Phys & Grav, NL-9747 AG Groningen, Netherlands

[46] Univ Toronto, David A Dunlap Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[47] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[48] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan

[49] CEA Saclay DSM Irfu, Dept Astrophys, F-91191 Gif Sur Yvette, France

[50] Univ Sci & Technol China, Sch Phys Sci, Dept Astron, Hefei 230026, Anhui, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2022年 / 926卷 / 01期

基金：

美国国家科学基金会; 加拿大自然科学与工程研究理事会; 欧洲研究理事会; 澳大利亚研究理事会; 美国国家航空航天局;

关键词：

B-MODE POLARIZATION; INFLATIONARY UNIVERSE SCENARIO; 500 SQUARE DEGREES; PHASE-TRANSITION; GRAVITY-WAVES; MICROWAVE; SKY; FLUCTUATIONS; TEMPERATURE; COSMOLOGY;

D O I：

10.3847/1538-4357/ac1596

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 5 sigma, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.

引用

页数：23

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