A. Schillaci
A5106466463- Superconducting and THz Device Technology
- Radio Astronomy Observations and Technology
- Cosmology and Gravitation Theories
- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Geophysics and Gravity Measurements
- Dark Matter and Cosmic Phenomena
- Astrophysics and Cosmic Phenomena
- Astrophysics and Star Formation Studies
- Physics of Superconductivity and Magnetism
- Advanced Thermodynamic Systems and Engines
- Stellar, planetary, and galactic studies
- Scientific Research and Discoveries
- Computational Physics and Python Applications
- Astronomical Observations and Instrumentation
- Spacecraft and Cryogenic Technologies
- Calibration and Measurement Techniques
- Superconducting Materials and Applications
- Advanced Frequency and Time Standards
- Microwave Engineering and Waveguides
- Particle Accelerators and Free-Electron Lasers
- Pulsars and Gravitational Waves Research
- Particle Detector Development and Performance
- Solar and Space Plasma Dynamics
- Soil Moisture and Remote Sensing
California Institute of Technology
2017-2024
Instituto Argentino de Radioastronomía
2024
Consejo Nacional de Investigaciones Científicas y Técnicas
2020-2024
Sapienza University of Rome
2011-2022
Istituto Nazionale di Fisica Nucleare, Sezione di Roma I
2010-2022
Hanoi University of Science and Technology
2018-2022
Harvard University
2022
Fermi National Accelerator Laboratory
2022
University of Chicago
2022
Brookhaven National Laboratory
2022
We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to including 2018 observing season. add additional Array observations at 220 GHz 95 previous 95/150/220 dataset. The Q/U maps now reach depths 2.8, 8.8 μK_{CMB} arcmin 95, 150, GHz, respectively, over effective area ≈600 square degrees ≈400 150 GHz. achieve a signal-to-noise ratio on polarized dust emission exceeding that Planck 353 take auto- cross-spectra between...
We present results from an analysis of all data taken by the bicep2/Keck CMB polarization experiments up to and including 2015 observing season. This includes first Keck Array observations at 220 GHz additional 95 150 GHz. The Q U maps reach depths 5.2, 2.9, 26 μKCMB arcmin 95, 150, GHz, respectively, over effective area ≈400 square degrees. achieve a signal noise on polarized dust emission approximately equal that Planck 353 take auto cross spectra between these publicly available WMAP...
The imprint left on the cosmic microwave background (CMB) from CMB photons scattering off high-energy electrons in galaxies and clusters is known as Sunyaev-Zel'dovich (SZ) effect subject of these two papers Atacama Cosmology Telescope (ACT). ACT measurements combined with those Planck BOSS are shown to provide a rich picture electron gas thermodynamics galactic cluster medium. This can be used test improve cosmological simulations relevant for upcoming experiments.
The early dark energy (EDE) scenario aims to increase the value of Hubble constant (${H}_{0}$) inferred from cosmic microwave background (CMB) data over that found in standard cosmological model ($\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$), via introduction a new form density Universe. EDE component briefly accelerates expansion just prior recombination, which reduces physical size sound horizon imprinted CMB. Previous work has nonzero is not preferred by Planck CMB power spectrum alone,...
The Atacama Cosmology Telescope (ACT) is designed to make high angular resolution measurements of anisotropies in the Cosmic Microwave Background (CMB) at millimeter wavelengths. We describe ACTPol, an upgraded receiver for ACT, which uses feedhorn-coupled, polarization-sensitive detector arrays, a 3 degree field view, 100 mK cryogenics with continuous cooling, and meta material anti-reflection coatings. ACTPol comprises three arrays separate cryogenic optics: two central frequency 148 GHz...
The thermal and kinematic Sunyaev-Zel'dovich effects (tSZ, kSZ) probe the thermodynamic properties of circumgalactic intracluster medium (CGM ICM) galaxies, groups, clusters, since they are proportional, respectively, to integrated electron pressure momentum along line-of-sight. We present constraints on gas thermodynamics CMASS galaxies in Baryon Oscillation Spectroscopic Survey (BOSS) using new measurements kSZ tSZ signals obtained a companion paper. Combining measurements, we measure...
We construct cosmic microwave background lensing mass maps using data from the 2014 and 2015 seasons of observations with Atacama Cosmology Telescope (ACT). These cover 2100 square degrees sky overlap a wide variety optical surveys. The are signal dominated on large scales have fidelity such that their correlation infrared is clearly visible by eye. also create thermal Sunyaev-Zel'dovich contamination removed novel cleaning procedure only slightly degrades signal-to-noise ratio....
Optimal analyses of many signals in the cosmic microwave background (CMB) require map-level extraction individual components sky, rather than measurements at power spectrum level alone. To date, nearly all component separation CMB has been performed exclusively using satellite data. In this paper, we implement a method based on internal linear combination (ILC) approach which have designed to optimally account for anisotropic noise (in 2D Fourier domain) often found ground-based experiments....
This paper presents a maximum-likelihood algorithm for combining sky maps with disparate coverage, angular resolution and spatially varying anisotropic noise into single map of the sky. We use this to merge hundreds individual covering 2008-2018 ACT observing seasons, resulting in by far deepest released so far. also combine full Planck maps, that have best features both ACT: Planck's nearly white on intermediate large scales ACT's high-resolution sensitivity small scales. The cover over...
We report on the design and performance of BICEP3 instrument its first three-year data set collected from 2016 to 2018. is a 52cm aperture, refracting telescope designed observe polarization cosmic microwave background (CMB) degree angular scales at 95GHz. It started science observation South Pole in with 2400 antenna-coupled transition-edge sensor (TES) bolometers. The receiver demonstrated new technologies such as large-diameter alumina optics, Zotefoam infrared filters, flux-activated...
Bicep Array is the newest multi-frequency instrument in Bicep/Keck program. It comprised of four 550mm aperture refractive telescopes observing polarization cosmic microwave background (CMB) at 30/40, 95, 150 and 220/270 GHz with over 30,000 detectors. We present an overview receiver, detailing optics, thermal, mechanical, magnetic shielding design. follows Bicep3's modular focal plane concept, upgrades to 6" wafer reduce fabrication higher detector count per module. The first receiver...
We present new constraints on anisotropic birefringence of the cosmic microwave background polarization using two seasons data from Atacama Cosmology Telescope covering 456 square degrees sky. The power spectrum, measured a curved-sky quadratic estimator, is consistent with zero. Our results provide tightest current constraint over range angular scales between 5 arc minutes and 9\ifmmode^\circ\else\textdegree\fi{}. improve previous upper limits amplitude scale-invariant spectrum by factor 2...
Our current understanding of the Universe is established through pristine measurements structure in cosmic microwave background (CMB) and distribution shapes galaxies tracing large scale (LSS) Universe. One key ingredient that underlies cosmological observables field sources observed assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps most robust theoretical prediction models explain Universe; itis necessarily present even...
We present estimates of line-of-sight distortion fields derived from the 95 GHz and 150 data taken by BICEP2, BICEP3, Keck Array up to 2018 observing season, leading cosmological constraints a study instrumental astrophysical systematics. Cosmological are three concerning gravitational lensing large-scale structure, polarization rotation magnetic or an axion-like field, screening effect patchy reionization. measure amplitude power spectrum $A_L^{\phi\phi}=0.95 \pm 0.20$. constrain rotation,...
We present the strongest constraints to date on anisotropies of cosmic microwave background (CMB) polarization rotation derived from 150 GHz data taken by BICEP2 Keck Array CMB experiments up and including 2014 observing season (BK14). The definition angle in BK14 maps has gone through self-calibration which overall is adjusted minimize observed $TB$ $EB$ power spectra. After this procedure, $QU$ lose sensitivity a uniform but are still sensitive rotation. This analysis places rotation,...
We present a $5.4\ensuremath{\sigma}$ detection of the pairwise kinematic Sunyaev-Zeldovich (kSZ) effect using Atacama Cosmology Telescope (ACT) and Planck CMB observations in combination with Luminous Red Galaxy samples from Sloan Digital Sky Survey (SDSS) DR15 catalog. Results are obtained three ACT maps: co-added 150 98 GHz maps, combining 2008--2018 (ACT DR5), which overlap SDSS over 3,700 sq. deg., component-separated map night-time only 2014--2015 DR4), overlapping 2,089 deg....
We measure the projected number density profiles of galaxies and splashback feature in clusters selected by Sunyaev--Zeldovich (SZ) effect from Advanced Atacama Cosmology Telescope (AdvACT) survey using observed Dark Energy Survey (DES). The radius for complete galaxy sample is consistent with theoretical measurements CDM-only simulations, located at $2.4^{+0.3}_{-0.4}$ Mpc $h^{-1}$. split based on color find significant differences profile shapes. Red those green valley show a...
We present ΛCDM cosmological parameter constraints obtained from delensed microwave background power spectra. Lensing maps a subset of DR4 data the Atacama Cosmology Telescope (ACT) are used to undo lensing effect in ACT spectra observed at 150 and 98 GHz. At GHz, we remove distortion with an effective efficiency 30% (TT), (EE), 26% (TE) 20% (BB); this results detections delensing 8.7σ 5.1σ 2.6σ (TE), 2.4σ (BB) significance. The combination GHz TT, EE, TE is well fit by standard model. also...
Abstract We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H i ) observations. Dust is important for both our understanding of astrophysical processes in the interstellar medium (ISM) search primordial gravitational waves cosmic microwave background (CMB). In diffuse ISM, H strongly correlated partly organized into that are aligned local magnetic field. analyze deep at 95, 150, 220 GHz, over...
The LSPE is a balloon-borne mission aimed at measuring the polarization of Cosmic Microwave Background (CMB) large angular scales, and in particular to constrain curl component CMB (B-modes) produced by tensor perturbations generated during cosmic inflation, very early universe. Its primary target improve limit on ratio scalar amplitudes down r = 0.03, 99.7% confidence. A second produce wide maps foreground our Galaxy synchrotron emission interstellar dust emission. These will be important...
The balloon-borne LSPE mission is optimized to measure the linear polarization of Cosmic Microwave Background at large angular scales. Short Wavelength Instrument for Polarization Explorer (SWIPE) composed 3 arrays multi-mode bolometers cooled 0.3K , with optical components and filters cryogenically below 4K reduce background on detectors. Polarimetry achieved by means rotating half-wave plates wire-grid polarizers in front arrays. modulator first component chain, reducing significantly...
A detection of curl-type (B-mode) polarization the primary CMB would be direct evidence for inflationary paradigm origin Universe. The Bicep/Keck Array (BK) program targets degree angular scales, where power from primordial B-mode is expected to peak, with ever-increasing sensitivity and has published most stringent constraints on inflation date. Bicep (BA) Stage-3 instrument BK will comprise four Bicep3-class receivers observing at 30/40, 95, 150 220/270 GHz a combined 32,000+ detectors;...