arXiv subjects

Francesco Chierici

Publications and source records attributed to Francesco Chierici.

2 recordsLinked to original sources

arXiv2023

On the seafloor horizontal displacement from cGPS and compass data in the Campi Flegrei caldera

Seafloor deformation monitoring is now performed in the marine sector of the Campi Flegrei volcanic area. MEDUSA infrastructure consists of 4 buoys at depths of 40-96m equipped with cGPS receivers, accelerometers and magnetic compasses to monitor buoy status and a seafloor module with a bottom pressure recorder. We study the seafloor deformation in the caldera. Previously we show that cGPS onland network and MEDUSA timeseries for the years 2017-2020 are in agreement with the deformation predicted by a Mogi model describing the observed deformation of an active volcano. Only for buoy A data differ significantly from model, at 6.9sigma and 23.7sigma for the horizontal speed (v) and direction. We devised a new method to reconstruct the sea bottom displacement including cGPS and compass data. The method, applied to buoy A and validated also on C, uses compass data to correct cGPS positions accounting for pole inclination. Including systematic errors, the internal consistency, within 3sigma (2sigma) for the speed (angle), between the results derived for different maximum inclinations of the buoy pole up to 3.5deg shows that the method allows to significantly reduce the impact of the pole inclination which can alter the estimation. We find good convergence of the velocity and deformation angle for increasing values of the buoy pole inclination. We found v=3.521+-0.039(stat)+-0.352(syst)cm/yr and an angle -115.159+-0.670(stat)+-7.630(syst)deg. The relative impact of potential systematics (statistical) effects increases (decreases) with cutoff. Our analysis gives v consistent with Mogi at 5.2sigma(stat) or 0.5sigma(stat and syst), and a deformation angle consistent at 4.3sigma(stat) or at 0.3sigma. The module of the vectorial difference between v from the data and Mogi diminishes by a factor 7.65+-1.23(stat) or +-5.78(stat+syst) compared with previous work. Potential improvements are discussed.

physics.geo-ph↗

arXiv2021

Effects of observer peculiar motion on the isotropic background frequency spectrum: from monopole to higher multipoles

The observer peculiar motion produces boosting effects in the background anisotropies with frequency spectral behaviours related to its spectrum. We study how the frequency spectrum of the background isotropic monopole emission is modified and transferred to the frequency spectra at higher multipoles, l. We perform the analysis in terms of spherical harmonic expansion up to a certain lmax, for various models from radio to far-IR. We derive a system of linear equations to obtain spherical harmonic coefficients and provide explicit solutions up to lmax=6 as linear combinations of the signals at N=lmax+1 colatitudes. The associated Legendre polynomials symmetry with respect to π/2 is used to separate the system into two subsystems, one for l=0 and even l, the other for odd l. This improves the solutions accuracy with respect to an arbitrary colatitudes choice. We apply the method to analytical or semi-analytical representions of monopole spectra, i.e. to four types of CMB distortions, four types of extragalactic backgrounds superimposed to the CMB Planckian spectrum and some combinations of them. We present our results in terms of spherical harmonic coefficients, relationships between the observed and intrinsic monopoles, maps, angular power spectra. We compare the method results with the ones obtained using more computationally demanding numerical integrations or map generation/inversion. The method is generalized to include the effect of the observer motion relative to the Sun. Its simplicity and efficiency can significantly alleviate the computational effort needed for accurate predictions and for the analysis of future data. We discuss the superposition of the CMB intrinsic anisotropies and of the effects induced by the observer motion, exploring for the possibility of constraining the intrinsic dipole embedded in the kinematic dipole, in the presence of CMB spectral distortions.

astro-ph.CO↗