R. Sudiwala
A5105096482- Superconducting and THz Device Technology
- Radio Astronomy Observations and Technology
- Cosmology and Gravitation Theories
- Molecular Junctions and Nanostructures
- Astronomy and Astrophysical Research
- Porphyrin and Phthalocyanine Chemistry
- Polydiacetylene-based materials and applications
- Dark Matter and Cosmic Phenomena
- Lipid Membrane Structure and Behavior
- Galaxies: Formation, Evolution, Phenomena
- Spectroscopy and Quantum Chemical Studies
- Precipitation Measurement and Analysis
- Scientific Research and Discoveries
- Spacecraft and Cryogenic Technologies
- Thermal Radiation and Cooling Technologies
- Ocular Surface and Contact Lens
- Physics of Superconductivity and Magnetism
- Meteorological Phenomena and Simulations
- Adaptive optics and wavefront sensing
- Astrophysics and Cosmic Phenomena
- Geophysics and Gravity Measurements
- Calibration and Measurement Techniques
- Atmospheric Ozone and Climate
- Photoreceptor and optogenetics research
- Climate variability and models
Cardiff University
2011-2024
University of Wales
2005-2012
California Institute of Technology
2009-2011
Princeton University
2009
Jet Propulsion Laboratory
2009
Stanford University
2009
Queen Mary University of London
1991-1998
Laboratoire de Chimie Moléculaire
1996
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
1996
CEA Paris-Saclay
1996
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 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,...
The Bicep2 telescope is designed to measure the polarization of cosmic microwave background on angular scales near 2-4 degrees, expected peak B-mode signal induced by primordial gravitational waves from inflation. follows success Bicep, which has set most sensitive current limits B-modes degree scales. experiment adopts a new detector design in beam-defining slot antennas are coupled TES detectors photolithographically patterned same silicon wafer, with multiplexing SQUID readout. takes...
Bicep2 deployed to the South Pole during 2009-2010 austral summer, and is now mapping polarization of cosmic microwave background (CMB), searching for evidence inflationary cosmology. belongs a new class telescopes including Keck (ground-based) Spider (balloon-borne) that follow on Bicep's strategy employing small, cold, on-axis refracting optics. This common design provides key advantages ideal targeting signature from inflation, including: (i) A large field view, allowing substantial light...
The Bicep2 and Keck Array experiments are designed to measure the polarization of cosmic microwave background (CMB) on angular scales 2-4 degrees (ℓ = 50–100). This is region in which <i>B</i>-mode signal, a signature prediction inflation, expected peak. was deployed South Pole at end 2009 middle its third year observing with 500 polarization-sensitive detectors 150 GHz. 2010, initially three receivers—each similar Bicep2. An additional two receivers have been added during 2011-12 summer. We...
Between the BICEP2 and Keck Array experiments, we have deployed over 1500 dual polarized antenna coupled bolometers to map Cosmic Microwave Background's polarization. We been able rapidly deploy these detectors because they are completely planar with an integrated phased-array antenna. Through our experience in learned of several challenges this technology- specifically beam synthesis antenna- paper report on how modified designs mitigate challenges. In particular, discus differential...
ADVERTISEMENT RETURN TO ISSUEPREVArticleNEXTFabrication of thin-film dielectrics from an amphiphilic two-ring phthalocyanineJoel D. Shutt, Daniel A. Batzel, Rashmikant V. Sudiwala, Scott E. Rickert, and Malcolm KenneyCite this: Langmuir 1988, 4, 6, 1240–1247Publication Date (Print):November 1, 1988Publication History Published online1 May 2002Published inissue 1 November 1988https://pubs.acs.org/doi/10.1021/la00084a004https://doi.org/10.1021/la00084a004research-articleACS PublicationsRequest...
The BICEP and Keck Array experiments are a suite of small-aperture refracting telescopes observing the microwave sky from South Pole. They target degree-scale B-mode polarization signal imprinted in Cosmic Microwave Background (CMB) by primordial gravitational waves. Such measurement would shed light on physics very early universe. While BICEP2 observed for first time at 150 GHz, higher frequencies Planck satellite showed that it could be entirely due to polarized emission Galactic dust,...
Anisotropic Langmuir–Blodgett films of phthalocyanine derivatives have been patterned using an atomic force microscope to scan the surface film at high rate (≳100 μm/s). The depth periodic grooved lines, width down 50 nm, formed perpendicular fast direction can be controlled monolayer level through effect load (a few nanonewtons) applied tip. It is shown that patterning results from oscillation in feedback loop resulting a modulation nanonewtons along each line. Using same principle, we show...
We describe the transition-edge-sensor (TES) focal plane arrays used for three cosmic microwave background (CMB) polarimetry projects. The first is BICEP2. array BICEP2 has been delivered and instrument now taking data at South Pole. Second Keck Array. planes will be nearly identical to those of BICEP2, but cover multiples frequencies (96, 150 225 GHz). scheduled deployment late 2010. Finally, there Spider, a high-altitude balloon observatory, which also 96, 150, GHz deployed in 2012. goal...
The upcoming Cosmic Microwave Background (CMB) experiments BICEP2/Keck and SPIDER will be using planar arrays of polarization sensitive antenna-coupled TES bolometers, operating at frequencies between 96GEIZ 220 GEIz.At 145 GlTz each array consists 64 polarimeters (128 sensors) four these are assembled together to make a focal plane.The detector integrated with time-domain SQUID multiplexer developed NIST read out the Multi-Channel Electronics (MCE) University British Columbia.We present our...
We describe the objectives, design and predicted performance of Clover, which is a ground-based experiment to measure faint ``B-mode'' polarisation pattern in cosmic microwave background (CMB). To achieve this goal, clover will make polarimetric observations approximately 1000 deg^2 sky spectral bands centred on 97, 150 225 GHz. The be made with two-mirror compact range antenna fed by profiled corrugated horns. telescope beam sizes for each band are 7.5, 5.5 arcmin, respectively. measured...
The Keck Array is a cosmic microwave background (CMB) polarimeter that will begin observing from the South Pole in late 2010. initial deployment consist of three telescopes similar to BICEP2 housed ultra-compact, pulse tube cooled cryostats. Two more receivers be added following year. In these proceedings we report on design and performance cryostat. We also some results antenna-coupled TES detectors operating presence tube. find not seriously impacted by replacement BICEP2's liquid helium...
Measurements of B-mode polarization in the CMB sourced from primordial gravitational waves would provide information on energy scale inflation and its potential form. To achieve these goals, one must carefully characterize Galactic foregrounds, which can be distinguished by conducting measurements at multiple frequencies. BICEP Array is latest-generation multi-frequency instrument BICEP/Keck program, specifically targets degree-scale B-modes CMB. In final configuration, this telescope will...