Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Analysis

A. Kogut; C. L. Bennett; D. N. Spergel; E. Komatsu; E. L. Wright; E. Wollack; G. Hinshaw; G. S. Tucker; H. V. Peiris; J. L. Weiland

REVIEW

Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Analysis

G. Hinshaw, M. R. Nolta, C. L. Bennett, R. Bean, O. Doré, M. R. Greason, M. Halpern, R. S. Hill

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N. Jarosik, A. Kogut, E. Komatsu, M. Limon, N. Odegard, S. S. Meyer, L. Page, H. V. Peiris, D. N. Spergel, G. S. Tucker, L. Verde, J. L. Weiland, E. Wollack, E. L. Wright

Astrophysics · Submitted 17 Mar 2006 · Published version · 22 references

Pith's verdict: WMAP three-year temperature analysis is a rigorous data release whose central claims hold up; the B-side beam scaling is the only real soft spot and it is a 1-2% normalization effect, not a load-bearing flaw.

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arXiv IDastro-ph/0603451 (version 2)

Pith ID7PYGCLOG, Pith's permanent record of this paper and its review

CitationA. Kogut, C. L. Bennett, D. N. Spergel, E. Komatsu, E. L. Wright, E. Wollack, G. Hinshaw, G. S. Tucker, H. V. Peiris, J. L. Weiland, L. Page, L. Verde, M. Halpern, M. Limon, M. R. Greason, M. R. Nolta, N. Jarosik, N. Odegard, O. Dor\'e, R. Bean, R. S. Hill, S. S. Meyer. "Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Analysis." arXiv:astro-ph/0603451 (2006). https://pith.science/paper/7PYGCLOG

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Editor's note

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The short version: this is the paper that made the three-year WMAP temperature maps and power spectrum the reference data set for precision cosmology, and it still reads as careful and honest. The central claims are solid. The spectrum is cosmic-variance limited to l=400 with S/N per mode above unity to l=850; the first two acoustic peaks are pinned at l=220.8±0.7 and 530.9±3.8; the rise to the third peak is unambiguous when combined with higher-resolution data. None of that is in real doubt.

What is genuinely new: the three-year maps in five bands, the 323-source catalog, the debiased ILC map with quantified residuals, the maximum-likelihood low-l spectrum, and the 153 independent cross-power spectra from V and W bands. The paper also does something rare in a big collaboration data paper: it states its own limitations plainly. It explicitly says the B-side beam model is not yet completed, so window-function uncertainties stay at first-year level; it explicitly says the ILC bias correction relies on a MEM galaxy model constrained by WMAP data; it explicitly revises the residual point-source amplitude downward after the original version. That is good scientific practice, and it makes the paper easier to trust, not harder.

The soft spots are real but proportionally minor. The B-side beam scaling could shift the l>50 normalization by roughly 1-2% if the scaled physical-optics model is off. That is an amplitude effect, not a shape or peak-position effect, and the paper already folds the uncertainty into the Fisher matrix. The ILC bias correction does involve some internal self-calibration, but the main spectrum comes from direct cross-power measurements with template subtraction, so the circularity burden is low. The low-l pseudo-Cl estimates disagree with the maximum-likelihood values at l=2,3,7 by about a factor of two; the authors adopt the ML values and show they are consistent with cut-sky full-sky checks. Worth noting as a live methodological issue, not a fatal one.

Who gets value from this: anyone using WMAP data for cosmological parameter estimation, foreground studies, or point-source work, and any reader who wants a model of how to write a defensible data-release paper. It deserves a serious referee, and in fact it got one. My own verdict: accept, with no demand for new analysis, just the standard request that the B-side beam model be completed and the window-function uncertainties updated when it is.

Referee report

Significance

If the result holds, this is a foundational data release and analysis that provides the most precise CMB temperature power spectrum of its time, with publicly available maps, spectra, likelihood code, and systematic-error assessments. The strengths of the paper are its use of 153 cross-power spectra to suppress noise bias, its detailed treatment of foregrounds, beams, point sources, and systematic errors, and its explicit comparisons with independent analyses (e.g., Eriksen et al., Huffenberger et al.). The central power-spectrum claims are direct cross-power measurements rather than derivations from a cosmological model, so the circularity burden is low. The main caveat, the B-side beam model scaling, is openly disclosed in Section 7.1.1 and affects only a 1-2% normalization at l > 50, which does not shift the acoustic peak locations or alter the cosmic-variance-limited sensitivity claims.

Minor objections (5)

[Section 9, item 9] The phrase "greatly reduced reduced" contains a duplicated word and should be corrected to "greatly reduced."
[Appendix A.1] The word "Guas sian" in the first sentence of Appendix A.1 is a typo and should read "Gaussian."
[Section 7.1.1 and Table 8] Because the B-side beam transfer functions are derived by scaling the A-side physical optics model, with window-function uncertainties held at the first-year level, the authors should state explicitly that the absolute amplitudes in Table 8 and the 1-2% normalization uncertainty do not affect the quoted peak locations or the cosmic-variance-limited claim; this would help readers who use Table 8 amplitudes for cosmological parameter extraction.
[Section 7.2] The revised point source amplitude, A = 0.014 +/- 0.003 microK^2 sr, is stated to encompass the earlier 0.017 value and the Huffenberger et al. estimate, but the text does not give the exact numerical impact on the final spectrum beyond "about 1%"; a brief quantitative statement of the shift in the high-l spectrum would be useful.
[References] The reference "Eriksen et al. 2004b" appears without a complete author list; it should be completed or replaced with the full citation so that readers can locate the work.

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The paper

The paper claims

The three-year WMAP temperature maps produce a cosmic-variance-limited CMB power spectrum out to l=400 and locate the first two acoustic peaks at l=220.8 and l=530.9.

The reading

The paper reports the three-year WMAP temperature analysis and aims to establish that the new full-sky maps, together with their derived angular power spectrum, provide a high signal-to-noise description of the CMB on angular scales from the full sky down to about a fifth of a degree. The spectrum is cosmic variance limited out to $l=400$—the error on those modes is set by the finite number of sky samples rather than by instrument noise—and the signal-to-noise ratio per $l$-mode exceeds unity to $l=850$. It locates the first two acoustic peaks at $l=220.8 \pm 0.7$ and $l=530.9 \pm 3.8$, and shows that, when combined with higher-resolution CMB measurements, the rise to a third peak is unambiguous. This matters because the CMB power spectrum is the main quantitative link between observations and cosmological parameters, so a public, well-characterized spectrum with improved gain and beam corrections directly sharpens what can be inferred about the composition and early-universe history.

What carries the argument

The load-bearing machine is the hybrid power-spectrum estimator. For $l \le 30$ it uses a pixel-space maximum-likelihood evaluation of the Gaussian likelihood, marginalizing over foreground templates; for $l > 30$ it uses a quadratic 'pseudo-$C_l$' cross-power estimator that forms products of maps from different receiver assemblies and different years so that uncorrelated noise cancels. The final spectrum averages 153 such independent V- and W-band channel-pair spectra, with the beam transfer functions $b_l$ supplied by a physical-optics model of the A-side optics scaled to the B side and by Jupiter beam measurements. Galactic emission is removed by fitting templates: a WMAP $K-Ka$ difference map traces synchrotron, an extinction-corrected H$\alpha$ map traces free-free, and a two-component dust model traces thermal dust. An updated Internal Linear Combination (ILC) map provides a foreground-minimized full-sky CMB map, bias-corrected through Monte Carlo simulations, and serves as a low-$l$ consistency check.

Extended reading notes

Core claim

The central discovery, stated on the paper's own terms, is that three years of WMAP observations yield a CMB temperature power spectrum that is close to the fundamental limit set by cosmic variance up to $l=400$, with signal-to-noise per mode above one through $l=850$. The best spectrum is built from 153 statistically independent V- and W-band cross-power spectra after foreground template subtraction and residual point-source correction; the first two acoustic peaks sit at $l=220.8 \pm 0.7$ and $l=530.9 \pm 3.8$, the first two troughs at $l=412.4 \pm 1.9$ and $l=675.1 \pm 11.1$, and the rise toward a third peak is unambiguous once WMAP is combined with higher-resolution CMB data. The three-year maps are consistent with the first-year maps but roughly $\sqrt{3}$ times more sensitive, with a corrected ILC map, an updated point-source catalog, and improved templates for synchrotron, free-free, and dust emission.

Load-bearing premise

The analysis assumes that one half of the telescope's beam is accurately described by rescaling a model built from the other half; if that scaling is wrong, the measured spectrum could be off by about 1–2% on small angular scales.

Editorial extensions

If this is right

The measured spectrum becomes the basis for tighter cosmological parameter constraints, including a reionization optical depth $\tau = 0.089 \pm 0.03$ and a scalar spectral index $n_s = 0.958 \pm 0.016$ from WMAP data alone.
Because the spectrum is cosmic variance limited to $l=400$, the first trough and the rise toward a third acoustic peak are measured rather than extrapolated, sharpening tests of baryon density and recombination physics.
The three-year maps, spectrum, and likelihood are public data products, so independent analyses can re-examine the foreground subtraction, the low-$l$ likelihood, and the reported large-scale anomalies.
The factor of about $\sqrt{3}$ lower noise and the $S/N > 1$ range to $l \approx 850$ extend the usable window for measuring the damping tail and for constraining residual point-source contamination.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

Beyond the paper, if a completed B-side beam model shifts the window functions by more than the first-year uncertainties, the spectrum normalization for $l \gtrsim 50$ would shift by roughly 1–2%, and that would propagate directly into cosmological parameters such as the scalar spectral index.
Beyond the paper, the 153-pair cross-power averaging strategy generalizes to other multifrequency CMB instruments: any experiment with many independent detector pairs can cancel noise bias the same way, provided its beam and calibration systematics are modeled at comparable accuracy.
Beyond the paper, the size of the ILC bias correction (about 41 $\mu$K$^2$ on the quadrupole) suggests that similar variance-minimization biases could affect other component-separation methods, and should be checked with Monte Carlo simulations before low-$l$ cosmological statements are made.

Original abstract

We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on the first three years of the WMAP sky survey. The new maps, which are consistent with the first-year maps and more sensitive, incorporate improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include refinements in the gain calibration and beam response models. We employ two forms of multi-frequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved 'Internal Linear Combination' map, based solely on WMAP data, by adding a bias correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission. The WMAP point source catalog is updated to include 115 new sources. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30. Our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l=400, and the signal-to-noise ratio per l-mode exceeds unity up to l=850. The first two acoustic peaks are seen at l=220.8 +- 0.7 and l=530.9 +- 3.8, respectively, while the first two troughs are seen at l=412.4 +- 1.9 and l=675.1 +- 11.1, respectively. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 9,098 input tokens.

What the abstract itself states, as probabilities: claims first 0.05 · states limitation 0.45 · human participants 0.02 · controlled comparison 0.13 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.94 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on the first three years of the WMAP sky survey. The new maps, which are consistent with the first-year maps and more sensitive, incorporate improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include refinements in the gain calibration and beam response models. We employ two forms of multi-frequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved 'Internal Linear Combination' map, based solely on WMAP data, by adding a bias correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission. The WMAP point source catalog is updated to include 115 new sources. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30. Our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l=400, and the signal-to-noise ratio per l-mode exceeds unity up to l=850. The first two acoustic peaks are seen at l=220.8 +- 0.7 and l=530.9 +- 3.8, respectively, while the first two troughs are seen at l=412.4 +- 1.9 and l=675.1 +- 11.1, respectively. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on the first three years of the WMAP sky survey.	contribution 0.99	0.96	0.10	asserted 1.00
s1	The new maps, which are consistent with the first-year maps and more sensitive, incorporate improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal.	contribution 0.78	0.82	0.07	asserted 0.65
s2	These include refinements in the gain calibration and beam response models.	method 0.95	0.62	0.02	asserted 0.95
s3	We employ two forms of multi-frequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses.	method 0.56	0.93	0.05	asserted 1.00
s4	First, we form an improved 'Internal Linear Combination' map, based solely on WMAP data, by adding a bias correction step and by quantifying residual uncertainties in the resulting map.	method 0.86	0.97	0.04	asserted 1.00
s5	Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission.	method 0.87	0.96	0.03	asserted 1.00
s6	The WMAP point source catalog is updated to include 115 new sources.	contribution 0.74	0.91	0.03	asserted 1.00
s7	We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30.	method 0.99	0.97	0.05	asserted 1.00
s8	Our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs.	method 0.96	0.97	0.07	asserted 1.00
s9	The combined spectrum is cosmic variance limited to l=400, and the signal-to-noise ratio per l-mode exceeds unity up to l=850.	result 0.98	0.94	0.11	asserted 1.00
s10	The first two acoustic peaks are seen at l=220.8 +- 0.7 and l=530.9 +- 3.8, respectively, while the first two troughs are seen at l=412.4 +- 1.9 and l=675.1 +- 11.1, respectively.	result 1.00	0.95	0.15	asserted 1.00
s11	The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established.	result 0.81	0.66	0.23	asserted 1.00

What kind of paper the classifier reports this is: empirical study 0.60 · evidence from analysis of existing data 0.66.

What was examined, and what was not

sources read

arXiv listing abstract v2

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

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S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** — Full-sky maps in Galactic coordinates smoothed wit

**Figure 2.** — The number of independent W-band observations per p

**Figure 3.** — Comparison of the three-year maps with the previous

**Figure 4.** — Results from the MEM foreground degeneracy analysi

**Figure 5.** — Galactic signal component maps from the Maximum Ent

**Figure 6.** — The mean Galaxy spectrum from 408 MHz to 94 GHz, based

**Figure 7.** — An overview of the microwave sky. The yellow, salmon

**Figure 8.** — top: Full-sky map color-coded to show the 12 regions that were used to generate the three-year ILC map (see §5.2). bottom: The mean ILC residual map from 100 Monte Carlo simulations of CMB signal, Galactic foreground signal and instrument noise. The CMB signal was drawn from a ΛCDM power spectrum that was modified to reproduce the power measured in the first-year spectrum at l = 2, 3. The first-year MEM foreground model was used to generate the (fixed) Galactic maps. In the simulations, systematic errors arose in the recovered ILC maps due to a combination of effects: (i) a…

**Figure 9.** — top: The first-year ILC map reproduced from Bennett et al. (2003c). middle: The three-year ILC map produced following the steps outlined in §5.2. bottom: The difference between the two (1-yr − 3-yr). The primary reason for the difference is the new bias correction (

**Figure 10.** — Galactic foreground removal with spatial templat

**Figure 11.** — Measurement of the source number count distributi

**Figure 12.** — The predicted Cl uncertainty (inverse Fisher matrix) at low l, in µK4 . The red curves show the result when pixel-pixel noise correlations are ignored. The smooth rise at low l reflects our approximate representation of 1/f noise in the noise bias model, equation (42). The black curves account for the full structure of the pixel-pixel inverse covariance matrix, including 1/f noise and map-making covariance. For the TT spectrum (left pair of curves in each panel), the noise is negligible compared to the signal, so this structure can be safely ignored. However, the TE analysis must…

**Figure 13.** — (top) Q-, V-, & W-band cross-power spectra before foreground subtraction, evaluated outside the Kp2 sky cut, relative to the final combined spectrum. (bottom) Same cross-power spectra after subtracting a template-based diffuse foreground model (§5.3) and the best-fit residual point source contamination (§7.2)

**Figure 14.** — Maps of power spectrum modes l = 2 − 8 computed from full-sky fits to the ILC map, shown at top left. Many authors note peculiar patterns in the phase of these modes, and many claim that the behavior is inconsistent with Gaussian random-phase fluctuations, as predicted by inflation. For example, the l = 5 mode appears strikingly symmetric (a non-random distribution of power in m), while the l = 2 and 3 modes appear unusually aligned. The significance of these a posteriori observations is being actively debated. See §8 for a more detailed discussion

**Figure 15.** — The posterior likelihood of l(l + 1)Cl/2π given the WMAP data, for l = 2 − 10. The curves are computed using data from the ILC map evaluated outside the Kp2 sky cut. The vertical blue lines show the values inferred using the pseudo-Cl estimate. These values are well within the posterior likelihood distribution, but there is a tendency for them to be lower than the peak, especially for l = 2, 3, 7. The vertical red lines show the predicted power spectrum from the best-fit ΛCDM model (fit to WMAP data). These points are well within the posterior likelihood in all cases; the faint…

**Figure 16.** — The binned three-year angular power spectrum (in b

**Figure 17.** — χ 2 vs. l for the full power spectrum relative to the best-fit ΛCDM model, fit to WMAP data only. The χ 2 per l has been averaged in l-bands of width ∆l = 15. The dark to light grey shading indicates the 1, 2, and 3σ confidence intervals for this distribution. The dashed line indicates the mode

**Figure 18.** — The WMAP three-year power spectrum (in black) compared to other recent measurements of the CMB angular power spectrum, including Boomerang (Jones et al. 2005), Acbar (Kuo et al. 2004), CBI (Readhead et al. 2004), and VSA (Dickinson et al. 2004). For clarity, the l < 600 data from Boomerang and VSA are omitted; as the measurements are consistent with WMAP, but with lower weight. These data impressively confirm the turnover in the 3rd acoustic peak and probe the onset of Silk damping. With improved sensitivity on sub-degree scales, the WMAP data are becoming an increasingly…

**Figure 19.** — Comparison of the three-year angular power spectr

**Figure 20.** — The unbinned three-year angular power spectrum (i

**Figure 21.** — Full-sky maps in ecliptic coordinates smoothed to

**Figure 22.** — Angular power spectra C T T l & C T E l from the three-year WMAP data. top: The TT data are as shown in

**Figure 23.** — An estimate of the multiplicative error introduce

Figures reproduced from arXiv:astro-ph/0603451 by the authors.

References

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The ﬁrst-year MEM foreground model was used to generate the (ﬁxed) Galactic maps. In the simulat ions, systematic errors arose in the recovered ILC maps due to a combination of eﬀects: (i) a tendency for the minimum variance method to exploit (anti) alignments between the CM B and foreground signal, and (ii) variations in the spectra of the foreground sig...

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3 PMN J2358-6054 aIndicates the source has multiple possible identiﬁcations . bSource J0322-3711 (Fornax A) is extended, and the ﬂuxes list ed were obtained by aperture photometry. cSource J0519-0540 is a blend of the Lynds Bright Nebulae LBN 2 07.65-23.11 and LBN 207.29-22.66. dSource J1357+7644 is outside of the declination range of the GB6 and PMN cata...

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The Tenerife values were obtained by taking the template cor relation coeﬃcients reported by de Oliveira-Costa et al. (2002) and de Oliveira-Costa et a l. (2004) (ﬁt to |b| > 20◦ data), scaling the templates to obtain model emission maps, then ev aluating the mean signal in the same way as with the WMAP and Haslam data. The Tenerife correlation with H α p...

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The vertical red lines show the predicted power spectrum from the best-ﬁt ΛCDM model (ﬁt to WMAP data). These points are well within the posterior likelihood in all cases; the faint dash ed lines indicate the 68% and 95% conﬁdence regions of the distribution (see §7.4). Note that the curves approach a Gaussian distribution as l increases. – 109 – Multipol...

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The dark to light grey shading indicates the 1, 2, and 3 σ conﬁdence intervals for this distribution. The dashed line indicates the mode. – 111 – Multipole moment l 10 100 500 1500 1000 l(l+1)Cl/2/ [+K2] Angular Scale 0 1000 2000 3000 4000 5000 6000 90° 2° 0.5° 0.2° WMAP Acbar Boomerang CBI VSA Fig. 18.— The WMAP three-year power spectrum (in black) compa...

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– 113 – Multipole moment l 100 200 300 400 0 l(l+1)Cl/2/ [+K2] 0 1000 2000 3000 4000 5000 6000 7000 Fig. 20.— The unbinned three-year angular power spectrum (i n black) from l = 2 − 400, where it provides a cosmic variance limited measurement of t he ﬁrst acoustic peak. The ﬁrst-year spectrum is shown in green for comparison. The red curve with the grey b...

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The feature is still visible in the three-year spectrum , but not prominently. We believe this feature was predominantly a no ise ﬂuctuation in the ﬁrst-year data. – 114 – +200 -200 T(+K) North South Fig. 21.— Full-sky maps in ecliptic coordinates smoothed to 1◦ resolution, shown in Lambert Azimuthal Equal Area projection. top: three-year ILC map, bottom:...

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Forward citations

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Recovering the Inflationary Potential and Primordial Power Spectrum With a Slow Roll Prior: Methodology and Application to WMAP 3 Year Data
astro-ph 2006-03 conditional novelty 7.0 of 10

A new Markov Chain Monte Carlo method that varies the Hubble slow roll parameters directly, using the inflationary flow equations, is applied to WMAP3 and SDSS data, yielding tight constraints on inflationary models a...
Polarization Observations of the Anomalous Microwave Emission in the Perseus Molecular Complex with the Cosmosomas Experiment
astro-ph 2006-03 conditional novelty 7.0 of 10

First polarization constraints on anomalous microwave emission show a low fraction (Π = 3.4^{+1.5}_{-1.9}% at 95% CL), supporting spinning dust over magnetic dipole emission.

Show 29 more citing papers

Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters
astro-ph.CO 2015-07 accept novelty 6.0 of 10

Planck 2015 temperature plus E-mode polarization gives tau = 0.078 +/- 0.019, confirms n_s < 1 at more than 5 sigma, and finds LambdaCDM an adequate fit, with high-multipole polarization flagged as not yet clean enoug...
The Atacama Cosmology Telescope: Cosmological Parameters from the 2008 Power Spectra
astro-ph.CO 2010-09 accept novelty 6.0 of 10

ACT's 148 and 218 GHz power spectra over 296 square degrees fit a lensed LCDM model plus SZ and point-source foregrounds, tightening limits on Neff, primordial helium, spectral running, the tensor-to-scalar ratio, and...
Oscillations in the CMB from Axion Monodromy Inflation
hep-th 2009-07 conditional novelty 6.0 of 10

Axion monodromy inflation produces a sinusoidally modulated scalar power spectrum whose amplitude and frequency can be bounded by CMB data, and detectable modulations arise in consistent string compactifications.
Duality Cascade in Brane Inflation
hep-th 2008-02 conditional novelty 6.0 of 10

Steps in a warped throat from the Seiberg duality cascade would produce small power-spectrum glitches but potentially large, distinctive non-Gaussianity in brane inflation, giving a possible CMB probe of string theory.
Likelihood Analysis of CMB Temperature and Polarization Power Spectra
astro-ph 2008-01 accept novelty 6.0 of 10

A new likelihood approximation for correlated CMB temperature and polarization power spectra is exact on the full sky and accurate enough for unbiased parameter estimation at multipoles above about 30.
Cosmological Constraints from the SDSS Luminous Red Galaxies
astro-ph 2006-08 accept novelty 6.0 of 10

A 58,000-galaxy power spectrum from SDSS luminous red galaxies, combined with WMAP, tightens the matter density to 0.24 +/- 0.02, curvature to 1.003 +/- 0.010, and dark energy to w = -0.94 +/- 0.09.
Cosmological parameters from combining the Lyman-alpha forest with CMB, galaxy clustering and SN constraints
astro-ph 2006-04 accept novelty 6.0 of 10

Adding Lyman-alpha forest power spectra to WMAP3, supernovae and galaxy clustering gives sum of neutrino masses below 0.17 eV at 95 percent confidence, no running of the spectral index, and an effective neutrino numbe...
Ghosts, Instabilities, and Superluminal Propagation in Modified Gravity Models
astro-ph 2006-04 conditional novelty 6.0 of 10

In the CDDETT modified gravity model, late-time accelerating attractor solutions generically have superluminal tensor or scalar propagation, even when fourth-order derivative ghosts are absent.
A Quintessentially Geometric Model
hep-ph 2006-03 conditional novelty 6.0 of 10

A D3-brane moving transverse to a ring of NS5 branes yields a cosh potential whose slow-roll inflation and late-time attractor can match the cosmological parameters allowed by 2006 observations.
Updating reionization scenarios after recent data
astro-ph 2006-03 conditional novelty 6.0 of 10

A model fit to WMAP3 and NICMOS data yields a reionization history that starts at z~15, is 90% complete by z~10, and finishes at z~6, requiring metal-free PopIII stars with efficiency >2%.
The impacts of dark matter particle annihilation on recombination and the anisotropies of the cosmic microwave background
astro-ph 2006-03 conditional novelty 6.0 of 10

Dark matter annihilation during recombination is constrained by WMAP three-year CMB data to F26<0.43 at 95% confidence, corresponding to a dark matter mass below roughly 8 MeV if annihilation explains the galactic pos...
CMB polarization features from inflation versus reionization
astro-ph.CO 2009-03 conditional novelty 5.0 of 10

Polarization from Planck should distinguish a step-inflation explanation of the WMAP l~20-40 temperature glitches from a smooth spectrum at about 3 sigma, rising to 5-8 sigma for a cosmic-variance-limited experiment.
Confronting Lemaitre-Tolman-Bondi models with Observational Cosmology
astro-ph 2008-02 conditional novelty 5.0 of 10

A Gpc-scale local void in an otherwise Einstein-de Sitter universe fits current supernova, CMB and BAO data about as well as flat LCDM, but Bayesian model comparison still mildly favours LCDM.
Combined analysis of the integrated Sachs-Wolfe effect and cosmological implications
astro-ph 2008-01 conditional novelty 5.0 of 10

A joint reanalysis of six galaxy catalogs against WMAP data detects the integrated Sachs-Wolfe effect at about 4.5 sigma and finds it consistent with a flat LCDM cosmology.
High resolution CMB power spectrum from the complete ACBAR data set
astro-ph 2008-01 accept novelty 5.0 of 10

The complete ACBAR 150 GHz data set yields a CMB power spectrum consistent with flat LambdaCDM, first detections of the fourth and fifth acoustic peaks, and a 1.1 sigma excess at multipoles above 2000 that is far smal...
Alignment tests for low CMB multipoles
astro-ph 2006-04 conditional novelty 5.0 of 10

Using multipole-vector statistics, the WMAP low-ℓ CMB maps are found to be in the ~10% least likely random realizations, confirming a quadrupole-octopole alignment and suggesting additional anomalies at ℓ=4 and ℓ=5.
The non-Gaussian Cold Spot in the 3-year WMAP data
astro-ph 2006-03 conditional novelty 5.0 of 10

The same 10-degree cold spot is detected in the 3-year WMAP data with a p-value around 1.85% after accounting for multiple scales, and it appears flat across frequencies, arguing against a foreground origin.
Testing Gaussian random hypothesis with the cosmic microwave background temperature anisotropies in the three-year WMAP data
astro-ph 2006-03 conditional novelty 5.0 of 10

Phase-based tests of the WMAP three-year DILC map find low-multipole extrema clustered at phi=180 degrees (0.45% significance), leading the authors to reject Gaussian randomness for l <= 10 and attribute the anomaly t...
Limits on Defects Formation and Hybrid Inflationary Models with Three-Year WMAP Observations
astro-ph 2006-03 conditional novelty 5.0 of 10

WMAP three-year data cannot distinguish hybrid inflation models with cosmic strings from plain ΛCDM, and the resulting upper bound on the string tension is Gμ ≤ 2.1e-7 at 68% confidence.
CMB statistical anisotropy, multipole vectors and the influence of the dipole
astro-ph 2006-03 conditional novelty 5.0 of 10

Low CMB multipole vectors, especially at l=2, 3, and 5, preferentially lie in the plane orthogonal to the kinematic dipole, and the paper attributes this to calibration nonlinearity.
Probing Inflation and Dark Energy with Current Cosmological Observations
astro-ph 2006-03 conditional novelty 5.0 of 10

Jointly fitting inflation parameters (spectral index, running, tensor ratio) and dark energy parameters (w0, w1) to WMAP1+SDSS+SNIa data broadens constraints and slightly increases preference for a running primordial ...
Blind component separation for polarized observations of the CMB
astro-ph 2006-03 conditional novelty 5.0 of 10

PolEMICA extends the SMICA spectral-matching algorithm to blindly separate polarized CMB and foreground components and recover temperature and polarization power spectra from multi-frequency maps.
KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions
astro-ph.CO 2026-05 conditional novelty 4.0 of 10

Bayesian hierarchical modeling of photometric redshifts in KiDS+VIKING-450 raises S8 to 0.756 ± 0.039 and reduces Planck tension to 1.9σ.
Bayesian foreground analysis with CMB data
astro-ph 2006-04 conditional novelty 4.0 of 10

A Bayesian parametric foreground separation method is reviewed and demonstrated on simulations, first-year WMAP data, and experiment design studies, with the central message that foreground uncertainties must be propa...
Observational constraints and cosmological parameters
astro-ph 2006-03 conditional novelty 4.0 of 10

WMAP 3-year data, analyzed with public MCMC methods, yields n_s < 1 only when the optical depth is pinned by polarization, and CMB lensing shifts n_s upward by an amount comparable to the Sunyaev-Zeldovich effect.
Cross-correlation of WMAP 3rd year and the SDSS DR4 galaxy survey: new evidence for Dark Energy
astro-ph 2006-03 conditional novelty 4.0 of 10

The WMAP3-SDSS DR4 cross-correlation detects the ISW effect at 4.7 sigma and favors Omega_L around 0.83, consistent with Lambda CDM.
An Accelerating Flat FLRW Model with Observation Constraints and Dynamic $\Lambda$
physics.gen-ph 2025-04 reject novelty 3.0 of 10

A four-parameter power-law FLRW model with a dynamic cosmological constant is fit to OHD, Union, Pantheon, and BAO data, giving dataset-dependent H0 values and a universe age around 21.7 billion years.
Planck 2015 results. I. Overview of products and scientific results
astro-ph.CO 2015-02 accept novelty 3.0 of 10

Planck's full-mission temperature and polarization data confirm a six-parameter flat LambdaCDM cosmology at percent-level precision, with no significant evidence for extensions.
Massive neutrinos and cosmology
astro-ph 2006-03 accept novelty 1.0 of 10

A detailed review of how cosmological observations bound the sum of neutrino masses through the free-streaming suppression of small-scale structure, and of future sensitivity forecasts.

How later papers used it

117 later papers cite it

Evidence: substantial. 103 of the citing papers share no author with it, and 32 of those carry a confident label from Pith's citation classifier.

Pith read 16 of the 175 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

6 later papers by other authors are listed below: 1 used its method or tool and 5 used its data or values.

Uses its method or tool 1 of 8 papers with this label

Considered the technique used by WMAP to identify and subtract radio point sources in this paper, along with the point source mask applied to the data, to evaluate the residual point source contribution to the estimated bispectrum in WMAP 3-year data.

Point Source Contamination in CMB Non-Gaussianity Analyses (2008) · 0.92 · paraphrased: the licence does not allow quoting

Uses its data or values 5 of 35 papers with this label

Fit to this paper's WMAP 3-year temperature-temperature, temperature-electric polarisation, and electric-electric polarisation spectra alone to avoid possible systematic problems from combining other CMB data sets.

Multiple inflation and the WMAP 'glitches' II. Data analysis and cosmological parameter extraction (2007) · 1.00 · paraphrased: the licence does not allow quoting
Found that this paper's 3-year WMAP CMB power spectrum constrains α to -0.005 ±0.040 at 95% confidence.

Does Planck mass run on the cosmological horizon scale? (2007) · 0.95 · paraphrased: the licence does not allow quoting
Constrained the radion evolution using this paper's three-year WMAP data and then the SNe Ia data.

Cosmological Constraints on Radion Evolution in the Universal Extra Dimension Model (2007) · 0.96 · paraphrased: the licence does not allow quoting
Used the co-added map of this paper's three-year data release to fit the texture profile to the cold spot.

Bianchi VII_h models and the cold spot texture (2007) · 0.99 · paraphrased: the licence does not allow quoting
Imposed that the resulting C2 does not exceed this paper's WMAP value of C2 ≃3·10^-11.

Gravity Waves Signatures from Anisotropic pre-Inflation (2008) · 0.99 · paraphrased: the licence does not allow quoting

How the literature uses it

89 arXiv papers cite this in 142 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 80 sentences without a confident label

Uses its method or tool 6 papers

The total log-likelihood is split in two, $-2 logL = L = L_0 + L_1$, where $L_0$ is due to cosmic variance, noise, and mask-induced mode coupling, and $L_1$ includes the uncertainty due to the point source and beam errors [ref] .

The scalar perturbation spectral index n_s: WMAP sensitivity to unresolved point sources · Source correction impact on spectral index · 0.90
In order to evaluate the residual point source contribution to the total estimated bispectrum in the WMAP–3yrs data, we must consider the technique used by WMAP to identify and substract radio point sources [ref] and the point source mask applied to the data.

Point Source Contamination in CMB Non-Gaussianity Analyses · Radio Point Sources · 0.92
The use of different frequency channels enable astrophysical foreground signals to be removed and the angular power spectra were calculated using both `pseudo-$C_ℓ$' and maximum likelihood based methods [ref] .

Multiple inflation and the WMAP 'glitches' II. Data analysis and cosmological parameter extraction · WMAP · 0.85

Uses its data or values 34 papers

For this purpose, we use the WMAP3 [ref] and 2dF [ref] data sets.

Primordial Neutrinos, Cosmological Perturbations in Interacting Dark-Energy Model: CMB and LSS · Constrains on the MaVaNs parameters · 1.00
For this purpose, we use the WMAP3 [ref] and 2dFGRS [ref] data sets.

Cosmological Signatures of the Interaction between Dark-Energy and Massive Neutrinos · Introduction · 1.00
For this purpose, we use the WMAP3 [ref] and 2dFGRS [ref] data sets.

Neutrino Masses from Cosmological Probes in Interacting Neutrino Dark-Energy Models · Neutrino Mass Bound in Neutrino-Dark Energy Model · 1.00

Compares with it 1 paper

In the figures the best fit solution for the CMB anisotropies are compared with the 3 year WMAP data [ref] and with the recent ACBAR results [ref] .

CMB anisotropies from acausal scaling seeds · Results · 0.93

Cites it as background 14 papers

A reduction in instrument noise produced spectra which are three times more sensitive in the noise limited region, independent years of data allow for cross-checks, the instrument calibration and response have been better characterised and a thorough analysis of the polarisation data has improved the understanding of the data [ref] .

Observational Constraints on Theories with a Blue Spectrum of Tensor Modes · Cosmic Microwave Background · 0.80
Most recently, the Wilkinson Microwave Anisotropy Probe (WMAP) experiment has generated high-resolution, all-sky maps of the CMB [ref] .

Correlation of CMB with large-scale structure: II. Weak lensing · Introduction · 0.87
In particular, since the release of the Wilkinson Microwave Anisotropy Probe (WMAP) data, observational constraints have been obtained, e.g., by [ref] for WMAP1 [ref] , by [ref] for WMAP3 [ref] and most recently for WMAP5 [ref] by [ref] , and by [ref] in the particular case of axion (uncorrelated, $=1$).

Constraints on primordial isocurvature perturbations and spatial curvature by Bayesian model selection · Introduction · 0.84

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [1]

Abele, H. et al. 2002, Phys. Rev. Lett., 88, 211801 Afshordi, N., Lin, Y.-T., & Sanderson, A. J. R. 2005, ApJ, 629 , 1 Afshordi, N., Loh, Y.-S., & Strauss, M. A. 2004, Phys. Rev., D 69, 083524 Arendt, R. et al. 1998, ApJ, 508, 74 Atrio-Barandela, F. & Muecket, J. P. 2006, ArXiv Astrophysi cs e-prints Barnes, C., Hill, R. S., Hinshaw, G., Page, L., Bennett...

View on Pith Pith review arXiv 2002

[2] [2]

725 K (Mather et al. 1999). cFull-width-at-half-maximum from radial proﬁle of A- and B- side average beams. Note: beams are not Gaussian. dNoise per observation for resolution 9 and 10 I, Q, & U maps, to ∼0.1% uncertainty. σ (p) = σ 0N −1/ 2 obs (p). eEﬀective frequency for synchrotron (s), free-free (ﬀ), and dust (d) emission, assuming spectral indices o...

View on Pith 1999

[3] [3]

The ﬁrst-year MEM foreground model was used to generate the (ﬁxed) Galactic maps. In the simulat ions, systematic errors arose in the recovered ILC maps due to a combination of eﬀects: (i) a tendency for the minimum variance method to exploit (anti) alignments between the CM B and foreground signal, and (ii) variations in the spectra of the foreground sig...

View on Pith 2004

[4] [4]

4 GB6 J0019+2021 00 25 26 −26 04 1 . 0 ±

View on Pith 2021

[5] [5]

5 PMN J0513-2016 05 13 58 −21 55 127 1 . 0 ±

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[6] [6]

3 PMN J0629-1959 06 33 47 −22 17 135 0 . 6 ±

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[7] [7]

4 PMN J0636-2041 a 06 39 46 73 26 087 0 . 8 ±

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[8] [8]

2 PMN J0836-2017 08 38 12 58 20 · · ·

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[9] [9]

1 GB6 J0854+2006 09 02 16 −14 14 1 . 1 ±

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[10] [10]

7 PMN J0907-2026 09 09 17 01 18 132 1 . 9 ±

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[11] [11]

5 PMN J1048-1909 10 58 28 01 34 149 4 . 5 ±

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[12] [12]

3 GB6 J1357+1919 13 57 04 76 44 0 . 7 ±

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[13] [13]

4 1Jy 2007+77 20 10 23 72 30 0 . 7 ±

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[14] [14]

6 PMN J2229-2049 22 32 38 11 44 047 3 . 0 ±

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[15] [15]

6 PMN J2256-2011 22 58 06 −27 57 012 6 . 7 ±

View on Pith 2011

[16] [16]

3 PMN J2358-6054 aIndicates the source has multiple possible identiﬁcations . bSource J0322-3711 (Fornax A) is extended, and the ﬂuxes list ed were obtained by aperture photometry. cSource J0519-0540 is a blend of the Lynds Bright Nebulae LBN 2 07.65-23.11 and LBN 207.29-22.66. dSource J1357+7644 is outside of the declination range of the GB6 and PMN cata...

View on Pith 2003

[17] [17]

The Tenerife values were obtained by taking the template cor relation coeﬃcients reported by de Oliveira-Costa et al. (2002) and de Oliveira-Costa et a l. (2004) (ﬁt to |b| > 20◦ data), scaling the templates to obtain model emission maps, then ev aluating the mean signal in the same way as with the WMAP and Haslam data. The Tenerife correlation with H α p...

View on Pith 2002

[18] [19]

The vertical red lines show the predicted power spectrum from the best-ﬁt ΛCDM model (ﬁt to WMAP data). These points are well within the posterior likelihood in all cases; the faint dash ed lines indicate the 68% and 95% conﬁdence regions of the distribution (see §7.4). Note that the curves approach a Gaussian distribution as l increases. – 109 – Multipol...

View on Pith 2000

[19] [20]

The dark to light grey shading indicates the 1, 2, and 3 σ conﬁdence intervals for this distribution. The dashed line indicates the mode. – 111 – Multipole moment l 10 100 500 1500 1000 l(l+1)Cl/2/ [+K2] Angular Scale 0 1000 2000 3000 4000 5000 6000 90° 2° 0.5° 0.2° WMAP Acbar Boomerang CBI VSA Fig. 18.— The WMAP three-year power spectrum (in black) compa...

View on Pith 2000

[20] [30]

– 113 – Multipole moment l 100 200 300 400 0 l(l+1)Cl/2/ [+K2] 0 1000 2000 3000 4000 5000 6000 7000 Fig. 20.— The unbinned three-year angular power spectrum (i n black) from l = 2 − 400, where it provides a cosmic variance limited measurement of t he ﬁrst acoustic peak. The ﬁrst-year spectrum is shown in green for comparison. The red curve with the grey b...

View on Pith 2000

[21] [208]

The feature is still visible in the three-year spectrum , but not prominently. We believe this feature was predominantly a no ise ﬂuctuation in the ﬁrst-year data. – 114 – +200 -200 T(+K) North South Fig. 21.— Full-sky maps in ecliptic coordinates smoothed to 1◦ resolution, shown in Lambert Azimuthal Equal Area projection. top: three-year ILC map, bottom:...

View on Pith 2000

[22] [2003]

Edited by G. Miele and G. Longo. World Scientiﬁc Publishing and Mainland Press, Sing apore, 217 Lewis, A., Challinor, A., & Lasenby, A. 2000, ApJ, 538, 473 Limon, M., Wollack, E., Bennett, C. L., Halpern, M., Hinshaw , G., Jarosik, N., Kogut, A., Meyer, S. S., Page, L., Spergel, D. N., Tucker, G. S., Wrig ht, E. L., Barnes, C., Greason, M., Hill, R., Koma...

View on Pith Pith review arXiv 2000