A5068659338- Galaxies: Formation, Evolution, Phenomena
- Astrophysics and Cosmic Phenomena
- Radio Astronomy Observations and Technology
- Astrophysics and Star Formation Studies
- Cosmology and Gravitation Theories
- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Geophysics and Gravity Measurements
- Astrophysical Phenomena and Observations
- Gamma-ray bursts and supernovae
- Scientific Research and Discoveries
- Superconducting and THz Device Technology
- Pulsars and Gravitational Waves Research
- Solar and Space Plasma Dynamics
- Dark Matter and Cosmic Phenomena
- GNSS positioning and interference
- Algebraic and Geometric Analysis
- Nonlinear Waves and Solitons
- Remote Sensing in Agriculture
- Calibration and Measurement Techniques
- Adaptive optics and wavefront sensing
- Fractal and DNA sequence analysis
- Meteorological Phenomena and Simulations
- Molecular Spectroscopy and Structure
- Particle Accelerators and Free-Electron Lasers
University of Cambridge
2000-2023
Cavendish Hospital
1998
In this paper, we present Q-U-I JOint Tenerife Experiment (QUIJOTE) 10–20 GHz observations (194 h in total over ≈250 deg2) intensity and polarisation of G159.6-18.5, one the most widely studied regions harbouring anomalous microwave emission (AME). By combining with other publicly available data, achieve precise spectrum AME measured to date an individual region, 13 independent data points between 10 50 being dominated by emission. The four QUIJOTE provide first confirmation downturn at low...
We present a method for fast optimal estimation of the temperature angular power spectrum from observations cosmic microwave background. employ Hamiltonian Monte Carlo (HMC) sampler to obtain samples posterior probability distribution all coefficients given set observations. compare properties HMC and related Gibbs sampling approach on low-resolution simulations. The correlation lengths produced by are generally comparable. At very high signal-to-noise (≳10) outperforms while intermediate...
We introduce the Bayesian Global Sky Model (B-GSM), a novel data-driven approach to modelling radio foregrounds at frequencies <400~MHz. B-GSM aims address limitations of previous models by incorporating robust error quantification and calibration. Using nested sampling, we compute evidence posterior distributions for spectral behaviour spatial amplitudes diffuse emission components. model comparison is used determine optimal number components their parametrisation. Posterior sky predictions...
A harmonic-space maximum-entropy method (MEM) is presented for separating the emission from different physical components in all-sky observations by forthcoming Planck satellite. The analysis performed at full resolution, with a pixel size of 1.7 arcmin, which corresponds to ℓmax≈ 6000. simulated data include cosmic microwave background (CMB), kinetic and thermal Sunyaev–Zel'dovich (SZ) effects galaxy clusters, as well Galactic dust, free–free synchrotron emission. Our simulations also...
Anomalous Microwave Emission (AME) is a significant component of Galactic diffuse emission in the frequency range $10$-$60\,$GHz and new window into properties sub-nanometre-sized grains interstellar medium. We investigate morphology AME $\approx10^{\circ}$ diameter $\lambda$ Orionis ring by combining intensity data from QUIJOTE experiment at $11$, $13$, $17$ $19\,$GHz C-Band All Sky Survey (C-BASS) $4.76\,$GHz, together with 19 ancillary datasets between $1.42$ $3000\,$GHz. Maps physical...
We present observations and analysis of a sample 123 galaxy clusters from the 2013 Planck catalogue Sunyaev-Zel'dovich sources with Arcminute Microkelvin Imager (AMI), ground-based radio interferometer. AMI provides an independent measurement higher angular resolution, 3 arcmin compared to beams 5-10 arcmin. The thus provide validation cluster detections, improved positional estimates, consistency check on fitted 'size' ($\theta_{s}$) 'flux' ($Y_{\rm tot}$) parameters in Generalised Navarro,...
Anomalous Microwave Emission (AME) is an important emission component between 10 and 60 GHz that not yet fully understood. It seems to be ubiquituous in our Galaxy observed at a broad range of angular scales. Here we use the new QUIJOTE-MFI wide survey data 11, 13, 17 19 constrain AME Galactic plane ($|b|<10^\circ$) on degree We built spectral energy distribution 0.408 3000 for each 5309 0.9$^\circ$ pixels plane, fitted parametric model by considering five components: synchrotron, free-free,...
We discuss all-sky convolution of the instrument beam with sky signal in polarimetry experiments, such as Planck mission which will map temperature anisotropy and polarization cosmic microwave background (CMB). To account properly for stray light (from e.g. galaxy, sun, planets) far side-lobes an experiment, it is necessary to perform over full sky. this process multipole space arbitrary response, fully including effects asymmetry cross polarization. The form that Wandelt-G\'orski fast...