The DOI matches its Crossref record; 209 of the 209 references it cites were found in a registry or an index.
Cosmic Microwave Background Anisotropies
Open accessAbstract
▪ 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.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
The check wasn’t confident either way, so it gives no verdict — never disputed.
In the citing paper
“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]
Experimental — accuracy not yet measured
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
Riess, A. G., Filippenko, A. V., Challis, P., Clocchiatti, A., Diercks, A., Garnavich, P. M., Gilliland, R. L., Hogan, C. J., Jha, S., Kirshner, R. P., et al. (1998) · The Astronomical Journal · doi:10.1086/300499 · Cited by 19,704
Measurements of Ω and Λ from 42 High‐Redshift Supernovae
Perlmutter, S., Aldering, G., Goldhaber, G., Knop, R. A., Nugent, P., Castro, P. G., Deustua, S., Fabbro, S., Goobar, A., Groom, D. E., et al. (1999) · The Astrophysical Journal · doi:10.1086/307221 · Cited by 18,062
Cosmological Imprint of an Energy Component with General Equation of State
Caldwell, R. R., Dave, R., & Steinhardt, P. J. (1998) · Physical Review Letters · doi:10.1103/physrevlett.80.1582 · Cited by 3,697
Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant
Freedman, W. L., Madore, B. F., Gibson, B. K., Ferrarese, L., Kelson, D. D., Sakai, S., Mould, J. R., Robert C. Kennicutt, Jr., Ford, H. C., Graham, J. A., et al. (2001) · The Astrophysical Journal · doi:10.1086/320638 · Cited by 3,543
A flat Universe from high-resolution maps of the cosmic microwave background radiation
de Bernardis, P., Ade, P. A. R., Bock, J. J., Bond, J. R., Borrill, J., Boscaleri, A., Coble, K., Crill, B. P., de Gasperis, G., Farese, P. C., et al. (2000) · Nature · doi:10.1038/35010035 · Cited by 2,614
A Measurement of Excess Antenna Temperature at 4080 Mc/s.
Penzias, A. A., & Wilson, R. W. (1965) · The Astrophysical Journal · doi:10.1086/148307 · Cited by 2,606
Structure in the COBE differential microwave radiometer first-year maps
Smoot, G. F., Bennett, C. L., Kogut, A., WRIGHT, E. L., Aymon, J., Boggess, N. W., Cheng, E. S., Amici, G. D., Gulkis, S. L., Hauser, M. G., et al. (1992) · The Astrophysical Journal · doi:10.1086/186504 · Cited by 2,595
Gauge-invariant cosmological perturbations
Bardeen, J. M. (1980) · Physical Review D · doi:10.1103/physrevd.22.1882 · Cited by 2,393
Baryonic Features in the Matter Transfer Function
Eisenstein, D. J., & Hu, W. (1998) · The Astrophysical Journal · doi:10.1086/305424 · Cited by 2,250
Self-citationSpontaneous creation of almost scale-free density perturbations in an inflationary universe
Bardeen, J. M., Steinhardt, P. J., & Turner, M. S. (1983) · Physical Review D · doi:10.1103/physrevd.28.679 · Cited by 2,073
Research works printed but not linked: 22
- Aghanim N, 1996, Astron. Astrophys., 311, 1
- Aghanim N, 1999, Astron. Astrophys., 347, 409
- Bernardeau F, 1997, Astron. Astrophys., 324, 15
- Bernardeau F, 1998, Astron. Astrophys., 338, 767
- Blanchard A, 1987, Astron. Astrophys., 184, 1
- Bond JR, 1997, MNRAS, 291, L33
- Carlstrom J, 2001, IAP Conf.
- Doroshkevich AG, 1978, Sov. Astron., 22, 523
- Halverson NW, 2001, Ap. J.
- Kofman LA, 1985, Sov. Astron. Lett., 11, 271
- Netterfield C, 2001, Ap. J.
- Polnarev AG, 1985, Sov. Astron., 29, 607
- Pryke C, 2001, Ap. J.
- Starobinskii A, 1985, Sov. Astron. Lett., 11, 133
- Stompor R, 2001, Ap. J.
- Sunyaev R, 1972, Comments Astrophys. Space Phys., 4, 173
- Tegmark M, 2001, Phys. Rev., 63, 043007
- Theureau G, 1997, Astron. Astrophys., 322, 730
- Wandelt B, 2001, Phys. Rev. D
- Wang X, 2001, Phys. Rev. D
- White M, 1997, Astron. Astrophys., 321, 8
- Zel'dovich Y, 1969, Sov. Phys.–JETP, 28, 146
Cited by
Sorted by citations
Items 401–500 of 742
Toda, Y., & Seto, O. (2026) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2026/02/019 · Cited by 6
“Although this original model nowadays suffers from the formation of topological defects, modifications to avoid this problem without altering the prediction is also possible [81].”
Burke, B. F., Smith, F. G., & Wilkinson, P. N. (2019) · Cambridge University Press eBooks · doi:10.1017/9781316987506.006 · Cited by 6
Single-step first order phase transition and gravitational waves in a SIMP dark matter scenario
Chakrabarty, N., Roy, H., & Srivastava, T. (2023) · Nuclear Physics B · doi:10.1016/j.nuclphysb.2023.116392 · Cited by 6
Vector dark matter with Higgs portal in type II seesaw framework
Das, N., Jha, T., & Nanda, D. (2024) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.109.115020 · Cited by 6
Progress on ANL/KICP Bolometers for SPTpol
Crites, A. T., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Datesman, A., Divan, R. N. S., George, E. M., Holzapfel, W. L., Lee, A. T.-J., et al. (2010) · IEEE Transactions on Applied Superconductivity · doi:10.1109/tasc.2010.2094990 · Cited by 6
Testing the analytical blind separation method in simulated CMB polarization maps
Santos, L. C. O., Yao, J., Zhang, L., Ghosh, S., Zhang, P., Zhao, W. K., Thyrso Villela, H., Chen, J., & Delabrouille, J. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936546 · Cited by 6
Xiao, S., Renzini, A. I., & Weinstein, A. J. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.107.122002 · Cited by 6
Mapping speed for an array of corrugated horns
Padin, S. (2010) · Applied Optics · doi:10.1364/ao.49.000479 · Cited by 6
“Measurements of CMB polarization anisotropy provide an important window on the early universe [2,3].”
BackgroundBaryogenesis and asymmetric dark matter from the left–right mirror symmetric model
Yang, W.-M. (2014) · Nuclear Physics B · doi:10.1016/j.nuclphysb.2014.06.002 · Cited by 6
Filtering Problems for Periodically Correlated Isotropic Random Fields
Dubovets’ka, I., Masyutka, O., & Moklyachuk, M. (2014) · Mathematics and Statistics · doi:10.13189/ms.2014.020402 · Cited by 6
“[2] W. Hu, S. Dodelson.”
BackgroundDependent Component Analysis for Cosmology: A Case Study
Kuruoğlu, E. E. (2010) · Lecture notes in computer science · doi:10.1007/978-3-642-15995-4_67 · Cited by 6
Xu, L. (2016) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2016/08/059 · Cited by 6
“J C A P 0 8 ( 2 0 1 6 ) 0 5 9 CMB photons [10].”
BackgroundGravitational lensing of the cosmic neutrino background
Lin, J. Y.-Y., & Holder, G. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/04/054 · Cited by 6
Understanding Galaxy Formation and Evolution
Avila-Reese, V. (2007) · Springer eBooks · doi:10.1007/978-1-4020-5575-1_4 · Cited by 6
Contemporary Millimeter- and Submillimeter-Wave Astronomy
Зинченко, И. И. (2003) · Radiophysics and Quantum Electronics · doi:10.1023/b:raqe.0000024989.12653.a0 · Cited by 6
Modern cosmology: Interactive computer simulations that use recent observational surveys
Moldenhauer, J., Engelhardt, L., Stone, K., & Shuler, E. (2013) · American Journal of Physics · doi:10.1119/1.4798490 · Cited by 6
Rivera, J. D., Moraes, B., Merson, A. I., Jouvel, S., Abdalla, F. B., & Abdalla, M. C. B. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty880 · Cited by 6
“…cosmological probes, including measure- E-mail: josedavidr@ift.unesp.br (JDR); fba@star.ucl.ac.uk (FBA) ments of Baryon Acoustic Oscillations (BAO, Hu & Dodelson 2002; Eisenstein et al. 2005; Percival et al. 2007; Blake et al. 2011; Anderson et al. 2014), the weak lensing of galaxies…”
BackgroundCosmological Implications of the BIMA 30 Ghz Sunyaev-Zel'dovich Effect Galaxy Cluster Survey
Lin, Y. T., & Mohr, J. J. (2002) · CERN Document Server (European Organization for Nuclear Research) · Cited by 6
Carroll, S. M. (2003) · Nature · doi:10.1038/422026a · Cited by 6
Diffuse source separation in CMB observationsPreprint
Delabrouille, J., & Cardoso, J.-F. (2007) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0702198 · Cited by 6
“Eriksen and collaborators have developed a method based on a refined modelling of the astrophysical components and fitted this model to the data to obtain estimates of foreground parameters (Eriksen et al. [ 21 ]).”
BackgroundMethodStatus of CMB Polarization Measurements from DASI and Other ExperimentsPreprint
Carlstrom, J. E., Kovac, J. M., Leitch, E. M., & Pryke, C. L. (2013) · Cited by 6
Dark matter cooling during early matter-domination boosts sub-earth halos
Banerjee, A., Chowdhury, D., Hait, A., & Islam, M. S. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/03/030 · Cited by 5
“Several astrophysical [1, 3–7] and cosmological [2] observations substantiate the claim for the existence of DM, leveraging its gravitational interaction.”
Constraints on running vacuum models with the baryon-to-photon ratio
Yu, H., Yang, K., & Li, J. (2022) · The European Physical Journal C · doi:10.1140/epjc/s10052-022-10164-9 · Cited by 7
SYSTEMATIC EFFECTS IN INTERFEROMETRIC OBSERVATIONS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION
Karakci, A., Zhang, L., Sutter, P. M., Bunn, E. F., Korotkov, A. L., Timbie, P. T., Tucker, G. S., & Wandelt, B. D. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/207/1/14 · Cited by 5
“A detection of these signals would probe the epoch of inflation and place an important constraint on the inflationary energy scale (Hu & Dodelson 2002).”
Zhang, L., Karakci, A., Sutter, P. M., Bunn, E. F., Korotkov, A. L., Timbie, P. T., Tucker, G. S., & Wandelt, B. D. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/206/2/24 · Cited by 5
“The primordial B-modes can probe horizon-scale primordial gravitational waves and play a major role in understanding the inflationary epoch (Hu & Dodelson 2002), while the secondary lensing-induced B-mode signals (Zaldarriaga & Seljak 1998) promise to provide a wealth of information about the…”
BackgroundPartial CMB maps: bias removal and optimal binning of the angular power spectrum
Ansari, R., & Magneville, C. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16561.x · Cited by 5
“An overview of the physical mechanisms responsible for the CMB anisotropies and the effect of the cosmological parameters on the power spectrum shape can be found in (Zaldarriaga et al 1997) and (Hu & Dodelson 2002).”
BackgroundSimulating instrumental systematics of Cosmic Microwave Background experiments with s4cmb
Fabbian, G., & Peloton, J. (2021) · The Journal of Open Source Software · doi:10.21105/joss.03022 · Cited by 5
“The observation of cosmic microwave background (CMB) anisotropies is one of the key probes of the standard cosmological model (Hu & Dodelson, 2002).”
BackgroundModel of four generation fermions and cold dark matter and matter-antimatter asymmetry
Yang, W.-M. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.87.095003 · Cited by 5
Constraints on the composite photon theory
Low, L. F. (2016) · Modern Physics Letters A · doi:10.1142/s021773231675002x · Cited by 5
Parameters and pitfalls in dark energy models with time varying equation of statePreprint
Biswas, R., & Wandelt, B. D. (2009) · arXiv (Cornell University) · doi:10.48550/arxiv.0903.2532 · Cited by 5
“For example, many features of CMB power spectra depend on the cosmological parameters through very specific functions of the these parameters (Hu et al. 2001; Hu & Dodelson 2002; Doran et al. 2001a; Doran & Lilley 2002).”
BackgroundBianchi, M. (2025) · Journal of Applied Mathematics and Physics · doi:10.4236/jamp.2025.1312240 · Cited by 4
Bianchi, M. (2026) · Journal of Applied Mathematics and Physics · doi:10.4236/jamp.2026.144077 · Cited by 4
Dark Universe inspired by the Kaluza-Klein gravity and impact on primordial gravitational waves
Jusufi, K., Luciano, G. G., Sheykhi, A., & Samart, D. (2025) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2025.100373 · Cited by 4
Matter dipole and Hubble tension due to large wavelength perturbations
Kashyap, G., Singh, N. K., & Jain, P. (2025) · Physical review. D/Physical review. D. · doi:10.1103/ftk4-6zmz · Cited by 4
Cuzinatto, R. R., Medeiros, L. G., de Morais, E. M., & Brandenberger, R. (2018) · Astroparticle Physics · doi:10.1016/j.astropartphys.2018.07.005 · Cited by 4
“[5, 6] and [7, 8] for textbook discussions).”
A measure of cosmological distance using the C IV Baldwin effect in quasars
Huang, L., Wang, H., Gao, Z., Zeng, X., & Chang, Z. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244644 · Cited by 4
Direct Optimal Mapping Image Power Spectrum and its Window Functions
Xu, Z. L., Kim, H., Hewitt, J. N., Chen, K.-F., Kern, N. S., Rath, E., Byrne, R. L., Gorce, A., Pascua, R., Martinot, Z. E., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad528c · Cited by 4
“The cosmic microwave background (CMB) measures the early universe at redshift ∼ 1100 (Fixsen et al. 1996; Hu & Dodelson 2002; Staggs et al. 2018); the late universe measurement gives statistical properties of the universe below redshift 10 (Anderson et al. 2014; Alam et al. 2017; Abbott et al.…”
BackgroundYamamoto, K. (2003) · International Journal of Modern Physics A · doi:10.1142/s0217751x03015295 · Cited by 4
CMB spectral distortions during the recombination of the primeval plasma in the early Universe
Kurt, V. G., & Shakhvorostova, N. N. (2014) · Uspekhi Fizicheskih Nauk · doi:10.3367/ufnr.0184.201404f.0423 · Cited by 4
Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves
Kumar, S. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acf618 · Cited by 4
“…the Big Bang, when the temperature of the Universe dropped to a level such that the electrons and protons could combine to form hydrogen atoms, the photons were set free, known as the cosmic microwave background ( CMB ) , and the sound waves were frozen ( Hu & Dodelson 2002; Aghanim et al. 2020 ) .”
BackgroundThe Reconstruction of Dark Energy with the Ridge Regression Approach
Huang, L., Yang, X., & Liu, X. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abf64a · Cited by 4
Living in a non-flat universe: theoretical formalism
Baumgartner, S., & Yoo, J. (2022) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2022/08/077 · Cited by 4
“Given the large level arm, the effects of a non-zero spatial curvature have been well studied [21–28] for cosmic microwave background (CMB) anisotropies (see, [27, 28] for review).”
BackgroundForeground removal from WMAP 7 yr polarization maps using an MLP neural network
Nørgaard-Nielsen, H. U. (2012) · Astrophysics and Space Science · doi:10.1007/s10509-012-1047-0 · Cited by 4
Geometrical Constraints on Dark Energy Models
Lazkoz, R., Carbajal, M., Montaño, L. M., Rosas-Ortiz, Ó., Velazquez, S. A. T., & Miranda, O. (2007) · AIP conference proceedings · doi:10.1063/1.2825127 · Cited by 4
Coherent phenomena at the last scattering in the CMB light
Bershadskii, A. (2007) · Physics Letters A · doi:10.1016/j.physleta.2007.12.041 · Cited by 4
Gangui, A. (2003) · Science · doi:10.1126/science.1082423 · Cited by 4
Gravitational waves from galaxy encounters
Quilis, V., González-García, A. C., Sáez, D., & Font, J. A. (2007) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.75.104008 · Cited by 4
A Direct Dark Matter Search with the MAJORANA Low-Background Broad Energy Germanium Detector
Finnerty, P. (2019) · Carolina Digital Repository (University of North Carolina at Chapel Hill) · doi:10.17615/hj0v-8263 · Cited by 4
Ansari, R., Bargot, S., Bourrachot, A., Couchot, F., Haïssinski, J., Versillé, S., Meur, G. L., Perdereau, O., Piat, M., Plaszczynski, S., et al. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06694.x · Cited by 4
“The set ofCℓ coefficients completely characterizes the CMB anisotropies in the case of uncorrelated Gaussian inhomogeneities (Hu & Dodelson 2002, Bond & Efstathiou 1987).”
BackgroundUnderstanding Galaxy Formation and EvolutionPreprint
Ávila-Reese, V. (2006) · Cited by 4
Cosmic Microwave Background anisotropies: the power spectrum and beyondPreprint
Martínez-González, E. (2006) · Cited by 4
The atmosphere above Mauna Kea at mid-infrared wavelengths
Chapman, I. M. (2002) · Open ULeth Scholarship (OPUS) (University of Lethbridge) · Cited by 4
AstroMLab 1: Who wins astronomy jeopardy!?
Ting, Y.-S., Nguyen, T. D., Ghosal, T., Pan, R., Arora, H., Sun, Z., de Haan, T., Ramachandra, N., Wells, A., Madireddy, S., et al. (2024) · Astronomy and Computing · doi:10.1016/j.ascom.2024.100893 · Cited by 9
Jiang, J.-Y., Jiao, K., & Zhang, T.-J. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/11/065 · Cited by 3
“This early-Universe constraint anchors the geometric measurements from BAO and SNe, ensuring consistency with the physics of the early Universe at z ∼ 1100 [29].”
Cosmic Microwave Background without Expansion
Cody, M. (2026) · Journal of Modern Physics · doi:10.4236/jmp.2026.171003 · Cited by 3
A singlet scalar assisted $$N_{2}$$ leptogenesis and pseudo-scalar dark matter
Ghosh, D. K., Ghosh, P., Mukherjee, K., & Narendra, N. (2025) · The European Physical Journal C · doi:10.1140/epjc/s10052-025-14937-w · Cited by 3
“Analysis of anisotropies in CMB data reveals that approximately one-fourth of the Universe consists of DM, which is non-baryonic and non-luminous [17].”
Detectors for the Atacama B-mode Search experiment
Appel, J. W. (2012) · Cited by 5
Cosmology with the Cosmic Microwave Background
Souradeep, T. (2014) · Springer handbooks · doi:10.1007/978-3-642-41992-8_32 · Cited by 3
MiCASA is a new method for quantifying cellular organization
Sornborger, A. T., Li, J., Timmons, C., Lupu, F. I., Eggenschwiler, J. T., Takahama, Y., & Manley, N. R. (2017) · Nature Communications · doi:10.1038/ncomms15619 · Cited by 3
“Similar analytical methods are commonly used in cosmology to describe and quantify structure in the distribution of galaxies throughout the universe 8–10 .”
ISW-galaxy cross-correlation in K-mouflage
Benevento, G., Bartolo, N., & Liguori, M. (2018) · Journal of Physics Conference Series · doi:10.1088/1742-6596/956/1/012001 · Cited by 3
Cylindrically symmetric and plane-symmetric solutions in f(R) theory via Noether symmetries
Öz, I. B., & Bamba, K. (2022) · The European Physical Journal C · doi:10.1140/epjc/s10052-022-10316-x · Cited by 3
Eigenmode analysis of perturbations in the primordial medium at and before recombination
Nelson, A. H. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039978 · Cited by 3
A cosmological distance measure using radio-loud quasars
Huang, L., & Chang, Z. X. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1451 · Cited by 3
Big Bang Nucleosynthesis: Nuclear Physics in the Early Universe
Fields, B. D. (2023) · Springer eBooks · doi:10.1007/978-981-19-6345-2_111 · Cited by 3
Thin tubes of a massless scalar field as a possible source of dark energy
Lelyakov, A. P., & Lelyakov, S. A. (2023) · Classical and Quantum Gravity · doi:10.1088/1361-6382/ad1710 · Cited by 3
Yao, J., Krachmalnicoff, N., Foschi, M., Puglisi, G., & Baccigalupi, C. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449827 · Cited by 3
Mehta, H., & Mukherjee, S. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/02/050 · Cited by 3
“7255 K and intensity given as [22, 24]: CMB cosmology involves the study of its anisotropies (spatial fluctuations in temperature or polarization) [91] and spectral distortions (deviations from blackbody spectrum), which are caused due to various photon interactions in early, as well as in late…”
Ghaffarnejad, H. (2019) · Journal of Physics Conference Series · doi:10.1088/1742-6596/1391/1/012028 · Cited by 3
The cosmic microwave background: from discovery to precision cosmology
Partridge, R. B. (2019) · Oxford University Press eBooks · doi:10.1093/oxfordhb/9780198817666.013.8 · Cited by 3
Circular polarisation of gamma rays as a probe of dark matter interactions with cosmic ray electrons
Cermeño, M., Degrande, C. C., & Mantani, L. (2021) · Physics of the Dark Universe · doi:10.1016/j.dark.2021.100909 · Cited by 3
Measuring CMB Polarisation with the Planck Mission
Delabrouille, J. (2004) · Springer eBooks · doi:10.1007/978-94-017-0559-2_7 · Cited by 3
An Absorber-coupled TES Bolometer for Measuring CMB Polarization
Wang, G., Yefremenko, V. G., Novosad, V., Pearson, J. E., Divan, R. N. S., Chang, C. L., Bleem, L. E., Crites, A. T., Mehl, J., Benson, B. A., et al. (2012) · Physics Procedia · doi:10.1016/j.phpro.2012.02.468 · Cited by 3
Predicting the polarization of the microwave background from the WMAP temperature maps
Jaffe, A. H. (2003) · New Astronomy Reviews · doi:10.1016/j.newar.2003.09.030 · Cited by 3
“…correlations: the correlated component of the polarization and temperature is due in large part to correlations between density and velocity perturbations on the surface of last scattering (Kamionkowski et al., 1997; Zaldarriaga and Seljak, 1997; Jaffe et al., 2000; Hu and Dodelson, 2002).”
BackgroundCosmology with galaxy correlations
Nichol, R. C. (2007) · General Relativity and Gravitation · doi:10.1007/s10714-007-0546-8 · Cited by 3
Bambi, C., & Dolgov, A. D. (2015) · UNITEXT for physics · doi:10.1007/978-3-662-48078-6_10 · Cited by 3
Alternative cosmological theories
Kragh, H. (2019) · Oxford University Press eBooks · doi:10.1093/oxfordhb/9780198817666.013.4 · Cited by 3
Philosophical aspects of cosmology
Smeenk, C. (2019) · Oxford University Press eBooks · doi:10.1093/oxfordhb/9780198817666.013.13 · Cited by 4
THE COSMIC MICROWAVE BACKGROUND ANISOTROPIES: OPEN PROBLEMS
Martínez-González, E., & Vielva, P. (2006) · Springer eBooks · doi:10.1007/1-4020-4526-3_1 · Cited by 3
“…more detailed discussions the reader is r fereed to the many good reviews written in the literature, some of themmore oriented to the theory (e.g. Hu and Dodelson 2002, Challinor 2004, 2005, Cabella and Kamionkowski 2004) and others to the experiments (e.g. Barreiro 2000, Bersanelli, Maino and…”
Zaldarriaga, M. (2002) · Nature · doi:10.1038/420747a · Cited by 3
A 145-GHz Interferometer for Measuring the Anisotropy of the Cosmic Microwave Background
Doriese, W. B. (2016) · Cited by 3
Observational Constraints on Models with an Interaction between Dark Energy and Dark Matter
Costa, A. A. (2014) · doi:10.11606/t.43.2014.tde-20012015-123002 · Cited by 3
Measuring CMB polarisation with the Planck mission
Delabrouille, J. (2004) · Astrophysics and Space Science · doi:10.1023/b:astr.0000022166.34602.c7 · Cited by 3
“Science with Planck Predictions of the accuracy on temperature and polarisation spectra with Planck are shown in figure 3 (adapted from (Hu & Dodelson, 2002)).”
Catch 'em all: Effective Leptophilic WIMPs at the $e^+\,e^-$ ColliderPreprint
Barman, B., Bhattacharya, S., Girmohanta, S., & Jahedi, S. (2021) · arXiv (Cornell University) · Cited by 3
Interacting Dark Energy and Its Implications for Unified Dark Sector
Pradosh Keshav, M. V., & Arun, K. (2024) · International Journal of Theoretical Physics · doi:10.1007/s10773-024-05794-6 · Cited by 2
“:3) anomaly, one approach is to introduce a dark energy component that can interact with matter or to modify the theory of gravity [3].”
Cosmic strings-induced CMB anisotropies in light of weighted morphology
Afzal, A., Alakhras, M., Kanafi, M. H. J., & Movahed, M. S. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf1110 · Cited by 3
Samandar, A., Duque, J. C., Copi, C. J., Barandiaran, M. M., Mihaylov, D. P., Starkman, G. D., Akrami, Y., Anselmi, S., Cornet-Gomez, F., Eskilt, J. R., et al. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/08/015 · Cited by 2
Foidl, H., & Rindler-Daller, T. (2025) · Frontiers in Astronomy and Space Sciences · doi:10.3389/fspas.2025.1627777 · Cited by 2
Bianchi, M. (2026) · Journal of Applied Mathematics and Physics · doi:10.4236/jamp.2026.147137 · Cited by 2
Wallisch, B. (2019) · Springer theses · doi:10.1007/978-3-030-31098-1_2 · Cited by 2
Observational constraint on dark energy from quantum uncertainty *
Huang, L., Yang, X., & Liu, X. (2021) · Chinese Physics C · doi:10.1088/1674-1137/ac2946 · Cited by 2
Mehta, H., & Mukherjee, S. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/05/051 · Cited by 2
Revisiting the temperature evolution law of the CMB with Gaussian processes
Avila, F., Rivera, A. B., Nunes, R. C., Holanda, R. F. L., & Bernui, A. (2025) · Physics Letters B · doi:10.1016/j.physletb.2025.139606 · Cited by 2
A cosmological Bragg law: interpreting the CMB as a diffractogram of foliated spacetime
Izabel, D. (2025) · The European Physical Journal Plus · doi:10.1140/epjp/s13360-025-06956-z · Cited by 2
“However, due to the asymmetric shape of the peak—caused by Silk damping, projection effects, and plasma composition—the true spectral centroid lies closer to (cid:6) ≈ 304 ± 4, as shown in [56].”
Braibant, S., Giacomelli, G., & Spurio, M. (2011) · Undergraduate lecture notes in physics · doi:10.1007/978-94-007-2464-8_13 · Cited by 2
Cosmic strings and natural inflation
Panotopoulos, G. (2007) · Journal of High Energy Physics · doi:10.1088/1126-6708/2007/06/080 · Cited by 2
Kamionkowski, M. (2003) · Nuclear Physics B - Proceedings Supplements · doi:10.1016/s0920-5632(03)01426-9 · Cited by 2
Cosmological constraints on radion evolution in the universal extra dimension model
Chan, K. C., & Chu, M. C. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.063525 · Cited by 2
E 3 Modeling and Simulation at the Exascale for Energy and the Environment
Simon, H. D. (2007) · Cited by 2
Minimax-robust filtering of functionals from periodically correlated random fields
Golichenko, I., Masyutka, O., & Moklyachuk, M. (2015) · Cogent Mathematics · doi:10.1080/23311835.2015.1074327 · Cited by 2
“These data include cosmic microwave background anisotropies (Adshead & Hu, 2012; Bartlett, 1999; Hu & Dodelson, 2002; Kogo & Komatsu, 2006; Okamoto & Hu, 2002), medical imaging (Kakarala, 2012), global and land-based temperature data (Jones, 1994; Subba Rao & Terdik, 2006), gravitational and…”
BackgroundFluctuations in the Cosmic Microwave Background
Jaffe, A. H. (2005) · Springer eBooks · doi:10.1007/1-4020-3057-6_10 · Cited by 2
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
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
