Snowmass 2021 CMB-S4 White Paper

Abazajian, Kevork N.; Abdulghafour, Arwa; Addison, Graeme E.; Adshead, Peter; Ahmed, Zeeshan; Ajello, M.; Akerib, D. S.; Allen, Steven W.; Alonso, David; Alvarez, Marcelo A.; Amin, Mustafa A.; Amiri, M.; Anderson, Adam W.; Ansarinejad, Behzad; Archipley, Melanie; Arnold, K.; Ashby, M. L. N.; Aung, Han H.; Baccigalupi, C.; Carina, Baker,; Abhishek, Bakshi,; Bard, Debbie; Barkats, D.; Barron, Darcy; Barry, P. S.; Bartlett, J. G.; Barton, Paul; Thakur, R. Basu; Battaglia, Nicholas; Beall, Jim; Bean, Rachel; Beck, Dominic; Belkner, Sebastian; Benabed, K.; Bender, A. N.; Benson, B. A.; Besuner, Bobby; Béthermin, M.; Bhimani, Sanah; Bianchini, F.; Biquard, Simon; Birdwell, Ian; Bischoff, C. A.; Bleem, L. E.; Bocaz, Paulina; Bock, J. J.; Bocquet, S.; Boddy, Kimberly K.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brinckmann, Thejs; Brown, Michael L.; Bryan, Sean; Buza, V.; Byrum, K.; Calabrese, E.; Calafut, Victoria; Caldwell, Robert W.; Carlstrom, J. E.; Carron, Julien; Cecil, Thomas E.; Challinor, A.; Chan, Victor; Chang, C. L.; Chapman, Scott; Charles, E.; Chauvin, E.; Cheng, Cheng; Chesmore, Grace E.; Cheung, K.; Chinone, Yuji; Chluba, Jens; Cho, Hsiao-Mei Sherry; Choi, Steve K.; Clancy, J; Clark, Susan; Cooray, Asantha; Coppi, Gabriele; Corlett, J.; Coulton, Will; Crawford, T. M.; Crites, A. T.; Cukierman, A.; Cyr-Racine, Francis-Yan; Dai, Wei‐Min; Daley, C.; Dart, Eli; Daues, Gregorg; Haan, T. de; Deaconu, C.; Delabrouille, J.; Derylo, G.; Devlin, Mark J.; Valentino, Eleonora Di; Dierickx, M.; Dober, B.; Doriese, W. B.; Duff, Shannon M.; Dutcher, D.; Dvorkin, Cora; Dünner, Rolando; Eftekhari, T.; Eimer, Joseph; Bouhargani, Hamza El; Elleflot, T.; Emerson, Nick; Errard, Josquin; Essinger-Hileman, Thomas; Fabbian, Giulio; Fanfani, Valentina; Fasano, A.; Chen, Feng; Ferraro, Simone; Filippini, J. P.; Flauger, Raphael; Flaugher, B.; Fraisse, A. A.; Frisch, J.; Frolov, A.; Galitzki, Nicholas; Gallardo, Patricio A.; Galli, S.; Ganga, K.; Gerbino, Martina; Giannakopoulos, Christos; Gilchriese, M.; Gluscevic, Vera; Goeckner-Wald, N.; Goldfinger, D. C.; Green, Daniel; Grimes, Paul W.; Grin, Daniel; Grohs, Evan; Gualtieri, R.; Guarino, V.; Gudmundsson, J. E.; Gullett, Ian; Guns, S.; Habib, Salman; Haller, G.; Halpern, M.; Halverson, N. W.; Hanany, Shaul; Hand, Emma; Harrington, Kathleen; Hasegawa, M.; Hasselfield, Matthew; Hazumi, M.; Heitmann, Katrin; Henderson, S.; Hensley, Brandon; Herbst, R.; Hervías-Caimapo, Carlos; Hill, J. Colin; Hills, R. E.; Hivon, E.; Hložek, Renée; Ho, Anna Y. Q.; Holder, G. P.; Hollister, M. I.; Holzapfel, W. L.; Hood, John; Hotinli, Selim C.; Hryciuk, Alec; Hubmayr, Johannes; Huffenberger, K. M.; Hui, H.; nez, Roberto Ibá; Ibitoye, Ayodeji; Ikape, Margaret; Irwin, K. D.; Jacobus, Cooper; Jeong, O.; Johnson, Bradley R.; Johnstone, Doug; Jones, William C.; Joseph, J.; Jost, Baptiste; Kang, J.; Kaplan, Ari; Karkare, K. S.; Katayama, N.; Keskitalo, R.; King, Cesiley; Kisner, T. S.; Klein, Matthias; Knox, L.; Koopman, Brian J.; Kosowsky, Arthur; Kovac, J. M.; Kovetz, Ely D.; Krolewski, Alex; Kubik, D.; Kuhlmann, S.; Kuo, Chao-Lin; Kusaka, A.; Lähteenmäki, A.; Lau, Kenny; Lawrence, C. R.; Lee, Adrian T.; Legrand, Louis; Leitner, M.; Leloup, C.; Lewis, Antony; Li, Dale; Linder, Eric V.; Liodakis, Ioannis; Liu, Jia; Long, Kevin Nicholas; Louis, Thibaut; Loverde, Marilena; Lowry, Lindsay; Lu, Chunyu; Lubin, P. M.; Ma, Yin-Zhe; Maccarone, Thomas J.; Madhavacheril, Mathew S.; Maldonado, Felipe; Mantz, Adam; Marques, Gabriela Moreno; Matsuda, Frederick; Mauskopf, Philip Daniel; May, Jared; McCarrick, Heather; McCracken, K. G.; McMahon, Jeffrey; Meerburg, P. Daniel; Melin, Jean-Baptiste; Menanteau, F.; Meyers, Joel; Millea, M.; Miranda, V.; Mitchell, Donald G.; Mohr, J. J.; Moncelsi, L.; Monzani, M. E.; Moshed, Magdy; Mroczkowski, Tony; Mukherjee, Suvodip; Münchmeyer, Moritz; Nagai, Daisuke; Nagarajappa, Chandan; Nagy, Johanna; Namikawa, Toshiya; Nati, F.; Natoli, T.; Nerval, S.; Newburgh, Laura; Nguyen, H. H.; Nichols, Erik; Nicola, Andrina; Niemack, Michael D.; Nord, B.; Novosad, V.; O’Brient, R.; Omori, Y.; Orlando, Giorgio; Osherson, B.; Osten, Rachel A.; Padin, S.; Paine, Scott; Partridge, B.; Patil, S. L.; Petravick, Don; Petroff, Matthew A.; Pierpaoli, E.; Pilleux, Mauricio; Pogosian, Levon; Prabhu, K.; Pryke, C.; Puglisi, Giuseppe; Racine, B.; Raghunathan, Srinivasan; Rahlin, A.; Raveri, Marco; Reese, Ben; Reichardt, Christian; Remazeilles, M.; Rizzieri, Arianna; Rocha, G.; Roe, Natalie A.; Rotermund, K. M.; Roy, Anirban; Ruhl, J. E.; Saba, Joe; Sailer, Noah; Salatino, Maria; Saliwanchik, B. R.; Sapozhnikov, L.; Rao, Mayuri Sathyanarayana; Saunders, Lauren; Schaan, Emmanuel; Schillaci, A.; Sliwa, Benjamin; Scott, Douglas; Sehgal, Neelima; Shandera, Sarah; Sherwin, Blake D.; Shirokoff, E.; Shiu, C.; Simon, Sara M.; Singari, Baibhav; Slosar, Anže; Spergel, David N.; Germaine, T. St.; Staggs, Suzanne T.; Stark, A. A.; Starkman, Glenn D.; Steinbach, B.; Stompor, R.; Stoughton, Chris; Suzuki, Aritoki; Tajima, O.; Tandoi, Chris; Teply, G. P.; Thayer, Gregg; Thompson, K. L.; Thorne, Ben; Timbie, Peter; Tomasi, M.; Trendafilova, Cynthia; Tristram, M.; Tucker, C.; Tucker, G. E.; Umiltà, Caterina; Engelen, Alexander van; Marrewijk, J. van; Vavagiakis, Eve M.; Vergès, Clara; Vieira, J. D.; Vieregg, A. G.; Wagoner, Kasey; Wallisch, Benjamin; Wang, Gensheng; Wang, Guojian; Watson, Scott; Watts, Duncan J.; Weaver, Chris; Wenzl, Lukas; Westbrook, Ben; White, M. J.; Whitehorn, N.; Wiedlea, Andrew; Williams, Paul; Wilson, R. G.; Winch, Harrison; Wollack, Edward J.; Wu, W. L. Kimmy; Xu, Zhisheng; Yefremenko, V.; Yu, Cyndia; Zegeye, David; Zivick, Jeff; Zonca, A.

doi:10.48550/arxiv.2203.08024

Cited by 26 publications

(29 citation statements)

References 8 publications

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“…Beyond the massive clusters, the level of 𝑦 signals in this work are not detectable in an individual tSZ image in any current data, or even future data, due to the noise levels. The appendix provides some examples of what 𝑦 maps from the simulations would look like given forecasted noise for the upcoming Simons Observatory (SO, Ade et al 2019) and CMB-Stage 4 (CMB-S4, Abazajian et al 2022). Stacking is necessary to increase the SNR sufficiently to measure the unbound gas.…”

Section: Discussionmentioning

confidence: 99%

Boundless baryons: how diffuse gas contributes to anisotropic tSZ signal around simulated Three Hundred clusters

Lokken¹,

Cui²,

Bond³

et al. 2022

Preprint

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Upcoming advances in galaxy surveys and cosmic microwave background data will enable measurements of the anisotropic distribution of diffuse gas in filaments and superclusters at redshift 𝑧 = 1 and beyond, observed through the thermal Sunyaev-Zel'dovich (tSZ) effect. These measurements will help distinguish between different astrophysical feedback models, account for baryons that appear to be 'missing' from the cosmic census, and present opportunities for using locally-anisotropic tSZ statistics as cosmological probes. This study seeks to guide such future measurements by analysing whether diffuse intergalactic gas is a major contributor to anisotropic tSZ signal in T T H G -S hydrodynamic simulations. Various definitions are applied to divide concentrated from diffuse gas at 𝑧 = 1 and create mock Compton-𝑦 maps for the separate components. The maps from 98 simulation snapshots are centred on massive galaxy clusters, oriented by the most prominent galaxy filament axis, and stacked. Results vary significantly depending on the definition used for diffuse gas, indicating that assumptions should be clearly defined when claiming observations of the warm-hot intergalactic medium. In all cases, the diffuse gas is important, contributing 25-60% of the tSZ signal in the far field (> 4ℎ −1 comoving Mpc) from the stacked clusters. The gas 1-2 virial radii from halo centres is especially key. Oriented stacking and environmental selections help to amplify the signal from the warm-hot intergalactic medium, which is aligned but less concentrated along the filament axis than the hot halo gas.

show abstract

Section: Discussionmentioning

confidence: 99%

Boundless baryons: how diffuse gas contributes to anisotropic tSZ signal around simulated Three Hundred clusters

Lokken¹,

Cui²,

Bond³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…8 as red and blue bands. The future CMB-S4 experiment [31,32] is expected to reach a much better sensitivity in determining N eff which will put stronger constraints on models predicting extra light relics. The projected sensitivity of CMB-S4 is shown as the dashed blue line in Fig.…”

Section: Dark Radiation From Hidden Sectorsmentioning

confidence: 99%

A tower of hidden sectors: a general treatment and physics implications

Aboubrahim¹,

Nath²

2022

Preprint

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An analysis of a tower of hidden sectors coupled to each other, with one of these hidden sectors coupled to the visible sector, is given and the implications of such couplings on physics in the visible sector are investigated. Thus the analysis considers n number of hidden sectors where the visible sector couples only to hidden sector 1, while the latter couples also to hidden sector 2, and the hidden sector 2 couples to hidden sector 3 and so on. A set of successively feeble couplings of the hidden sectors to the visible sector are generated in such a set up. In general each of these sectors live in a different heat bath. We develop a closed form set of coupled Boltzmann equations for the correlated evolution of the temperatures and number densities of each of the heat baths. We then apply the formalism to a simplified model with scalar portals between the different sectors. Predictions related to dark matter direct detection experiments and future CMB probes of dark radiation are made.

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“…This is significant if we consider the relative error values for optimistic and even for moderate foregrounds in Table II. Note that, the relative errors in Table III provide an error floor, which can be minimised only with more precise measurements of the cosmological parameters, which is possible with the next generation of experiments, like CMB stage-4 [116], EUCLID galaxy survey [117], etc.…”

Section: Modelmentioning

confidence: 99%

Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

Sarkar¹,

Kovetz²

2022

Preprint

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The fluctuations in the dark matter-baryon relative velocity field are imprinted as acoustic oscillations in the 21-cm power spectrum during cosmic dawn (CD). These velocity acoustic oscillations (VAOs) keep the imprints of the comoving sound horizon scale. In a previous work by Muñoz, it has been demonstrated that these VAOs can be treated as standard rulers to measure the cosmic expansion rate at high redshifts by considering a variety of Lyman-Werner feedback strengths and foreground contamination scenarios. Here we extend that analysis by using a modified version of the public code 21cmFAST. We use this code to simulate the VAOs in 21-cm power spectrum and forecast the potential to constrain H(z) with the HERA radio telescope, taking into account the effects of Lyman-α heating, Lyman-Werner feedback and foregrounds, the dependence on various astrophysical parameters, and the degeneracy with cosmological parameters. We find that H(z) can be measured with HERA at ∼ 0.3 − 6% relative accuracy in the range 11 < z < 20, under different astrophysical and foreground scenarios, with uncertainties in the Planck cosmological parameters setting a ∼ 0.08 − 0.2% relative-error floor in the measurement. This accuracy is on par with most low-redshift measurements and can be helpful in testing various cosmological scenarios motivated by the ongoing "Hubble Tension".

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Snowmass 2021 CMB-S4 White Paper

Cited by 26 publications

References 8 publications

Boundless baryons: how diffuse gas contributes to anisotropic tSZ signal around simulated Three Hundred clusters

Boundless baryons: how diffuse gas contributes to anisotropic tSZ signal around simulated Three Hundred clusters

A tower of hidden sectors: a general treatment and physics implications

Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

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