MASTER of the Cosmic Microwave Background Anisotropy Power Spectrum: A Fast Method for Statistical Analysis of Large and Complex Cosmic Microwave Background Data Sets

By E. Hivon, K. G'orski, C. Netterfield, B. Crill, S. Prunet, F. Hansen. 2001

707 citations recorded by the source corpus.

We describe a fast and accurate method for estimation of the cosmic microwave background (CMB) anisotropy angular power spectrum—Monte Carlo Apodized Spherical Transform Estimator (MASTER). Originally devised for use in the interpretation of the BOOMERANG experimental data, MASTER is both a computationally efficient method suitable for use with the currently available CMB data sets (already large in size, despite covering small fractions of the sky, and affected by inhomogeneous and correlated noise) and a very promising application for the analysis of very large future CMB satellite mission products.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e275c70b5625b34581b470770f22f80e73d5a82c

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In Astronomy and Astrophysics

Citations in the corpus

Evidence of Vorticity and Shear at Large Angular Scales in the WMAP Data: A Violation of Cosmological Isotropy? (2005, methodology): “In Figure 2 we compare the power spectra of the original and the Bianchi-corrected V+W linear combination map10, as computed by the MASTER algorithm (Hivon et al. 2002) for the Kp2 sky coverage.”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, methodology): “However, instead of using the Monte Carlo Apodised Spherical Transform EstimatoR (MASTER) estimate (Hivon et al. 2002) for the l > 32 TT spectrum, we now use an optimally-estimated power spectrum and errors based on the quadratic estimator from Tegmark (1997), as discussed in detail in Bennett et…”
Fast estimation of polarization power spectra using correlation functions (2003, methodology): “2, centred on the true spectrum smoothed with a 10-arcmin beam, encloses the ±σ error region based on the rule of thumb (generalised from Hivon et al. 2002 for the temperature case) ∆CEl ≈ √ 2 νl (CEl +Nl).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “(A15) The factor w22/w4 represents the loss of modes due to pixel weighting, where wk is the k-th moment of the weight (Hivon et al. 2002) given by wk = 1 Ωsky ∫ dθW k(θ).”
A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG (2005, methodology): “Both IT and NA power spectra estimation pipelines are based on the MASTER method (Hivon et al. 2002) that computes the pseudo-aℓm on a fraction of the sphere defined by the function W (n̂) that takes into account weighting and sky coverage.”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION POWER SPECTRUM AT SUB-DEGREE SCALES WITH POLARBEAR (2014, methodology): “We estimate angular power spectra using a pseudospectrum technique, based on the MASTER algorithm (Hivon et al. 2002).”
Planck intermediate results. XLVI. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth (2016, positive): “Two versions of the PCL cross-spectra were produced, using Xpol (Tristram et al. 2005) and Spice, a MASTER-like code (Hivon et al. 2002).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: POWER SPECTRA AND WMAP-DERIVED PARAMETERS (2010, methodology): “For high-l (l > 32) TT we use the MASTER pseudo-Cl quadratic estimator (Hivon et al. 2002).”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND DAMPING TAIL FROM THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2012, methodology): “For each field, we calculate the transfer function by comparing the average power spectrum of these simulated maps to the known input spectrum using an iterative scheme (Hivon et al. 2002).”
A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG (2005, methodology): “Power Spectrum Estimation Both the NA and IT analysis pipelines employ variations of the pseudo-Cℓ Monte Carlo approach to power spectrum estimation introduced in Hivon et al. (2002).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP ) OBSERVATIONS: ARE THERE COSMIC MICROWAVE BACKGROUND ANOMALIES? (2010, methodology): “Our analysis is limited to 33 ≤ ℓ < 600, which is the part of the power spectrum that is flat-weighted on the sky and where the Monte Carlo Apodised Spherical Transform EstimatoR (Hivon et al. 2002) pseudo-spectrum is used.”
Three Year Wilkinson Microwave Anistropy Probe (WMAP) Observations: Polarization Analysis (2006, methodology): “The first method is based directly on the MASTER spectrum (Hivon et al. 2002, and Appendix B) of EE data and serves as a simple check of the other two.”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, neutral): “[552].”