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CMB mapping experiments: a designer's guide
Astrophysics · Submitted 24 May 1997
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Using these approximations, we discuss how to maximize the scientific return of CMB mapping experiments given the practical constraints at hand, and our main conclusions are as follows.
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The abstract, sentence by sentence
We apply state-of-the art data analysis methods to a number of fictitious CMB mapping experiments, including 1/f noise, distilling the cosmological information from time-ordered data to maps to power spectrum estimates, and find that in all cases, the resulting error bars can we well approximated by simple and intuitive analytic expressions. Using these approximations, we discuss how to maximize the scientific return of CMB mapping experiments given the practical constraints at hand, and our main conclusions are as follows. (1) For a given resolution and sensitivity, it is best to cover a sky area such that the signal-to-noise ratio per resolution element (pixel) is of order unity. (2) It is best to avoid excessively skinny observing regions, narrower than a few degrees. (3) The minimum-variance mapmaking method can reduce the effects of 1/f noise by a substantial factor, but only if the scan pattern is thoroughly interconnected. (4) 1/f noise produces a 1/l contribution to the angular power spectrum for well connected single-beam scanning, as compared to virtually white noise for a two-beam scan pattern such as that of the MAP satellite.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We apply state-of-the art data analysis methods to a number of fictitious CMB mapping experiments, including 1/f noise, distilling the cosmological information from time-ordered data to maps to power spectrum estimates, and find that in all cases, the resulting error bars can we well approximated by simple and intuitive analytic expressions. | contribution 0.57 | 0.95 | 0.11 | asserted 1.00 |
| s1 | Using these approximations, we discuss how to maximize the scientific return of CMB mapping experiments given the practical constraints at hand, and our main conclusions are as follows. | contribution 0.60 | 0.71 | 0.07 | asserted 0.68 |
| s2 | (1) For a given resolution and sensitivity, it is best to cover a sky area such that the signal-to-noise ratio per resolution element (pixel) is of order unity. | result 0.89 | 0.76 | 0.49 | asserted 1.00 |
| s3 | (2) It is best to avoid excessively skinny observing regions, narrower than a few degrees. | result 0.82 | 0.69 | 0.55 | asserted 1.00 |
| s4 | (3) The minimum-variance mapmaking method can reduce the effects of 1/f noise by a substantial factor, but only if the scan pattern is thoroughly interconnected. | result 0.98 | 0.77 | 0.51 | asserted 0.98 |
| s5 | (4) 1/f noise produces a 1/l contribution to the angular power spectrum for well connected single-beam scanning, as compared to virtually white noise for a two-beam scan pattern such as that of the MAP satellite. | result 0.98 | 0.74 | 0.28 | asserted 1.00 |
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The paper
Original abstract
We apply state-of-the art data analysis methods to a number of fictitious CMB mapping experiments, including 1/f noise, distilling the cosmological information from time-ordered data to maps to power spectrum estimates, and find that in all cases, the resulting error bars can we well approximated by simple and intuitive analytic expressions. Using these approximations, we discuss how to maximize the scientific return of CMB mapping experiments given the practical constraints at hand, and our main conclusions are as follows. (1) For a given resolution and sensitivity, it is best to cover a sky area such that the signal-to-noise ratio per resolution element (pixel) is of order unity. (2) It is best to avoid excessively skinny observing regions, narrower than a few degrees. (3) The minimum-variance mapmaking method can reduce the effects of 1/f noise by a substantial factor, but only if the scan pattern is thoroughly interconnected. (4) 1/f noise produces a 1/l contribution to the angular power spectrum for well connected single-beam scanning, as compared to virtually white noise for a two-beam scan pattern such as that of the MAP satellite.
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How the literature uses it
11 arXiv papers cite this in 14 sentences
Papers citing it · 9 sentences without a confident label
Uses its method or tool 5 papers
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For problems such as this where there are far more pixels than parameters for which we need to solve, the optimal solution to the above system of equations is [ref] [equation] with a covariance matrix [equation] Here $$ is the covariance matrix of the reconstructed $$.
Testing the statistical isotropy of large scale structure with multipole vectors · The Reconstruction Methodology · 0.96
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Assuming that the TOD are linearly dependent on an input map $m_p,in=[I_p,Q_p,U_p]^T$ of the sky, they can be described as [ref] [equation] where $y_p,t$ is a vector of samples from sky pixel $p$ at time $t$, $n_p,t$ is the noise associated with each sample and $P_p,t$ is the pointing matrix that contains information on which detectors are sampling pixel $p$ at time $t$ that maps an input map (Section [ref]) into TOD.
Spectral distortion and polarization of the cosmic microwave background: Measurement, challenges and perspectives · Simulations of TOD · 0.88
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For the IM experiments, in each redshift bin we model the noise in the style of a single-frequency CMB map [ref] .
Delensing Degree-Scale $B$-Mode Polarization with High-Redshift Line Intensity Mapping · Angular Power Spectra, Noise, and Correlation Coefficients · 0.97
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