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Cosmic Microwave Background Anisotropies
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▪ Abstract Cosmic microwave background (CMB) temperature anisotropies have and will continue to revolutionize our understanding of cosmology. The recent discovery of the previously predicted acoustic peaks in the power spectrum has established a working cosmological model: a critical density universe consisting of mainly dark matter and dark energy, which formed its structure through gravitational instability from quantum fluctuations during an inflationary epoch. Future observations should test this model and measure its key cosmological parameters with unprecedented precision. The phenomenology and cosmological implications of the acoustic peaks are developed in detail. Beyond the peaks, the yet to be detected secondary anisotropies and polarization present opportunities to study the physics of inflation and the dark energy. The analysis techniques devised to extract cosmological information from voluminous CMB data sets are outlined, given their increasing importance in experimental cosmology as a whole.
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“Analysis of the WMAP data puts very strongly pressure on the simple monomial w ( χ ) = G 4 χ 4 at the 3 σ level[18, 40]”
From Phase Transitions in the Early and Present Universe (2006) · cites this paper as [40]
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Massimo Giovannini, A. (2007) · International Journal of Modern Physics A · doi:10.1142/s0217751x07036919 · Cited by 9
Non-circular beam correction to the CMB power spectrum
Souradeep, T., Mitra, S., Sengupta, A. S., Ray, S., & Saha, R. (2006) · New Astronomy Reviews · doi:10.1016/j.newar.2006.09.011 · Cited by 9
A model-independent precision test of General Relativity using LISA bright standard sirens
Afroz, S., & Mukherjee, S. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/10/100 · Cited by 8
Barron, D. R., Mitchell, K., Groh, J. C., Arnold, K., Elleflot, T., Howe, L. A., Ito, J., Lee, A. T.-J., Lowry, L. N., Anderson, A. J., et al. (2021) · IEEE Transactions on Applied Superconductivity · doi:10.1109/tasc.2021.3067190 · Cited by 8
“B-mode polarization in the CMB is also generated at the arcminute scale in the later universe by gravitational lensing by large-scale structure [1].”
BackgroundMehta, H., & Mukherjee, S. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/09/037 · Cited by 8
“We follow the derivation given by [19, 20].”
Observational constraints on running vacuum model
Zhang, J.-J., Lee, C.-C., & Geng, C.-Q. (2019) · Chinese Physics C · doi:10.1088/1674-1137/43/2/025102 · Cited by 8
Cosmic microwave background and first molecules in the early universe
Signore, M., & Puy, D. (2008) · The European Physical Journal C · doi:10.1140/epjc/s10052-008-0807-z · Cited by 9
Cosmic Reionization and the First Nonlinear Structures in the Universe
Haiman, Z. (2015) · Astrophysics and space science library · doi:10.1007/978-3-319-21957-8_1 · Cited by 8
“IGM is not dense and hot enoughto changethe spectrum of the CMB, elastic Thomsonscatteringby free electrons changes the patterns of both the temperature and polarization power spectra (see reviews by [8, 9, 10]). Scattering a fraction τe of the CMB photons out of each sightline translates into a suppression of the pri…”
BackgroundScientific Realism and Primordial Cosmology
Azhar, F., & Butterfield, J. (2017) · Routledge eBooks · doi:10.4324/9780203712498-25 · Cited by 15
“The basic observable associated with the CMB is the intensity of radiation as a function of frequency and direction in the sky (Hu and Dodelson 2002).”
BackgroundCosmic Microwave Background experiments — past, present and future
Richards, P. L. (2007) · International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) · doi:10.1109/icimw.2007.4516378 · Cited by 8
“This standard cosmological model has been discussed in many hundreds of publications [1], [2].”
BackgroundD’Ascenzo, N. (2009) · DESY Publication Database (PUBDB) (Deutsches Elektronen-Synchrotron) · doi:10.3204/desy-thesis-2009-004 · Cited by 8
“A more precise quantification of the Dark Matter content of the universe is recently made with the detection and analysis of the Cosmic Microwave Background (CMB) Anisotropies [72].”
MethodForecast of Foreground Cleaning Strategies for AliCPT-1
Zhang, J., Ghosh, S., Dou, J., Liu, Y., Li, S., Chen, J., Wang, J., Zhang, Z., Delabrouille, J., Remazeilles, M., et al. (2024) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad5c63 · Cited by 7
“…of B-mode polarization patterns on large angular scales is particularly compelling, as it can reveal horizon-scale primordial gravitational waves ( Kamionkowski et al. 1997; Zaldarriaga & Seljak 1997; Hu & Dodelson 2002 ) and provide new insights into the in fl ationary epoch of our Universe.”
Strange stars admixed with dark matter: Equiparticle model in a two fluid approach
Marzola, I., Rodrigues, É. H., Coelho, A. F., & Lourenço, O. (2025) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.111.063076 · Cited by 7
Dai, X., Yang, Y., Wang, Y., Qu, Y., Yi, S., & Wang, F. W. F. (2026) · Physical review. D/Physical review. D. · doi:10.1103/zg3l-yt32 · Cited by 7
Tachyonic vs quintessence dark energy: linear perturbations and CMB data
Rajvanshi, M. P., Singh, A., Jassal, H. K., & Bagla, J. S. (2021) · Classical and Quantum Gravity · doi:10.1088/1361-6382/ac1b49 · Cited by 7
A diffused background from axion-like particles in the microwave sky
Mehta, H., & Mukherjee, S. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/07/084 · Cited by 7
“We follow the derivation given in [1, 70].”
The design, implementation, and performance of the LZ calibration systems
Aalbers, J., Akerib, D. S., Musalhi, A. K. A., Alder, F., Amarasinghe, C. S., Ames, A., Anderson, T., Angelides, N., Araújo, H. M., Armstrong, J. E., et al. (2024) · Journal of Instrumentation · doi:10.1088/1748-0221/19/08/p08027 · Cited by 7
“Despite multiple astronomical and cosmological observations indicating that dark matter constitutes ∼ 85% of the total mass in the universe [1–5], it has not been directly detected so far.”
Mahmoudifard, M., Salehi, A., & Sepahvand, R. (2024) · The European Physical Journal C · doi:10.1140/epjc/s10052-024-13466-2 · Cited by 7
Chou, T.-L., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Balkenhol, L., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., et al. (2025) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.111.123513 · Cited by 7
Confronting dark fermion with a doubly charged Higgs in the left–right symmetric model
Dey, S., Ghosh, P., & Kumar, S. (2022) · The European Physical Journal C · doi:10.1140/epjc/s10052-022-10778-z · Cited by 7
Entanglement masquerading in the CMB
Adil, A., Albrecht, A., Baunach, R., Holman, R., Ribeiro, R. H., & Richard, B. J. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/06/024 · Cited by 7
“where S(k, η) contains all the cosmological hydrodynamics while the spherical Bessel function j`[k(η0 − η)] acts as a window function encoding the geometric effect of projecting onto the CMB surface [43].”
BackgroundFIMP dark matter from flavon portals
Babu, K. S., Chakdar, S., Das, N., Ghosh, D. K., & Ghosh, P. (2023) · Journal of High Energy Physics · doi:10.1007/jhep07(2023)143 · Cited by 7
Status of CMB polarization measurements from DASI and other experiments
Carlstrom, J. E., Kovac, J. M., Leitch, E. M., & Pryke, C. (2003) · New Astronomy Reviews · doi:10.1016/j.newar.2003.09.007 · Cited by 7
“However, at these angular scales, corresponding to multipoles ∼ 5000, the level of the primary CMB anisotropy is strongly damped and secondary effects due to interactions with large-scale structure in the universe are expected to dominate (Hu & Dodelson 2002).”
BackgroundRocher, J., Benabed, K., & Bouchet, F. R. (2007) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2007/05/013 · Cited by 7
“The polarization sky pattern essentially maps the local quadrupolar temperature anisotropies on the last scattering surface and at the linear order, the scalar metric perturbations can only produce an E polarization [21].”
BackgroundHigher order terms in the inflaton potential and the lower bound on the tensor to scalar ratio r
Destri, C., de Vega, H. J., & Sanchez, N. G. (2010) · Annals of Physics · doi:10.1016/j.aop.2010.11.019 · Cited by 7
Non-Gaussianity in the cosmic microwave background induced by dipolar dark matter
Luc Blanchet, A., Langlois, D., Tiec, A. L., & Marsat, S. (2013) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2013/02/022 · Cited by 7
“(5.18b) Present observations of the CMB temperature fluctuations require g to be small enough, typically g .”
InfluentialDrake, K. P., & Wright, G. B. (2020) · Journal of Computational Physics · doi:10.1016/j.jcp.2020.109544 · Cited by 7
“For example, the confirmation of the first peak in the temperature angular power spectrum affirmed that the universe is spatially flat [15].”
BackgroundBarrentine, E. M., Timbie, P. T., Stevenson, T. R., Ali, S. T., Chervenak, J. A., Wollack, E. J., Moseley, S. H., Allen, C. A., Hseih, W.-T., Miller, T. M., et al. (2008) · Journal of Low Temperature Physics · doi:10.1007/s10909-007-9615-3 · Cited by 7
Cosmological Implications of the BIMA 30 GHz Sunyaev‐Zeldovich Effect Galaxy Cluster Survey
Lin, Y., & Mohr, J. J. (2003) · The Astrophysical Journal · doi:10.1086/344749 · Cited by 7
“On angular scales of 50 and smaller, the thermal SZE contribution to the CMB anisotropy can dominate that of the primary CMB anisotropy (see, e.g., Holzapfel et al. 2000a; Refregier, Spergel, & Herbig 2000; Hu & Dodelson 2002; Springel, White, & Hernquist 2001; Bond et al. 2002).”
BackgroundThe current status of observational cosmology
Ostriker, J. P., & Souradeep, T. (2004) · CERN Document Server (European Organization for Nuclear Research) · Cited by 7
Cosmic Red Shift, Microwave Background, And New ParticlesPreprint
Fedosın, S. G. (2012) · viXra · doi:10.5281/zenodo.890805 · Cited by 7
The Intrinsic Bispectrum of the Cosmic Microwave Background
Pettinari, G. W., Fidler, C., Crittenden, R., Koyama, K., & Wands, D. (2013) · Springer theses · doi:10.1007/978-3-319-21882-3 · Cited by 65
Metadata
- Authors
- Hu, W., & Dodelson, S.
- Affiliations
- Fermi National Accelerator Laboratory (US)
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 2002-09
- Volume
- 40
- Issue
- 1
- Pages
- 171-216
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2123864481
- Cited by
- 745
- References
- 208
- Citations by year
- 2026: 35 · 2025: 38 · 2024: 38 · 2023: 28 · 2022: 34 · 2021: 27 · 2020: 37 · 2019: 58 · 2018: 25 · 2017: 25 · 2016: 24 · 2015: 29 · 2014: 26 · 2013: 29 · 2012: 18
- FWCI
- 3.64
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Annual Review of Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- cosmic microwave background, temperature anisotropy, acoustic peaks, power spectrum, inflation (cosmology), dark energy, dark matter, gravitational instability, quantum fluctuations, secondary anisotropies, CMB polarization, cosmological parameters, structure formation
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