Ningfeng Zhu
A5063844151- Radio Astronomy Observations and Technology
- Superconducting and THz Device Technology
- Cosmology and Gravitation Theories
- Quantum Computing Algorithms and Architecture
- Quantum Information and Cryptography
- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Quantum many-body systems
- Quantum and electron transport phenomena
- Advancements in Semiconductor Devices and Circuit Design
- Astrophysics and Cosmic Phenomena
- Neural Networks and Reservoir Computing
- Geophysics and Gravity Measurements
- Adaptive optics and wavefront sensing
- Stellar, planetary, and galactic studies
- Semiconductor materials and devices
- Spacecraft and Cryogenic Technologies
- Quantum optics and atomic interactions
- Gamma-ray bursts and supernovae
- Quantum Mechanics and Applications
- Astrophysics and Star Formation Studies
- Microwave Engineering and Waveguides
- Advanced Data Storage Technologies
- Computational Physics and Python Applications
- Advanced Thermodynamic Systems and Engines
Google (United States)
2022-2025
Henan Agricultural University
2025
Mudanjiang Normal University
2024
California University of Pennsylvania
2018-2023
University of Pennsylvania
2019-2022
University of California, Riverside
2022
Philadelphia University
2019
Lawrence Berkeley National Laboratory
2018
Cornell University
2018
Princeton University
2018
We demonstrate a high dynamic range Josephson parametric amplifier (JPA) in which the active nonlinear element is implemented using an array of rf-SQUIDs. The device matched to 50 Ω environment with Klopfenstein-taper impedance transformer and achieves bandwidth 250–300 MHz input saturation powers up −95 dBm at 20 dB gain. A 54-qubit Sycamore processor was used benchmark these devices, providing calibration for readout power, estimation added noise, platform comparison against standard...
The Simons Observatory (SO) will make precise temperature and polarization measurements of the cosmic microwave background (CMB) using a set telescopes which cover angular scales between 1 arcminute tens degrees, contain over 60,000 detectors, observe at frequencies 27 270 GHz. SO consist 6 m aperture telescope coupled to 30,000 transition-edge sensor bolometers along with three 42 cm refractive telescopes, an additional 30,000+ all be located in Atacama Desert altitude 5190 m. powerful...
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 introduce and validate a delensing framework for the Simons Observatory (SO), which will be used to improve constraints on inflationary gravitational waves by reducing lensing noise in measurements of $B$ modes CMB polarization. SO initially observe using three small aperture telescopes one large-aperture telescope. While polarization maps from small-aperture constrain waves, internal delens reconstructed data Since obtained dominated subdegree scales, constructs template lensing-induced...
Background Prostate cancer (PCa) is one of the prevalent malignant tumors among men. It can progress to castration-resistant prostate (CRPC), which significantly more challenging treat. Saikosaponin A (SSA), a triterpenoid saponin extracted from genus Bupleurum, exerts numerous pharmacological effects, including anti-inflammatory and anti-tumorigenic effects. However, mechanism underlying effects SSA in treatment remains elusive. Methods In this study, network pharmacology approach was...
An understanding of astrophysical feedback is important for constraining models galaxy formation and extracting cosmological information from current future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect, quantified via the Compton-$y$ parameter, a powerful tool studying feedback, because it directly probes pressure hot, ionized gas residing in dark matter halos. Cross-correlations between galaxies maps obtained cosmic microwave background surveys are sensitive to redshift...
Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised address many questions Galactic astrophysics addition its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for range science cases. We find that SO can: constrain spectrum polarized dust emission at level $\Delta\beta_d \lesssim 0.01$ and thus test models composition predict $\beta_d$ polarization differs...
New telescopes are being built to measure the Cosmic Microwave Background (CMB) with unprecedented sensitivity, including Simons Observatory (SO), CCAT-prime, BICEP Array, SPT-3G, and CMB Stage-4. We present observing strategies for located in Chile that informed by tools used develop recent Atacama Cosmology Telescope (ACT) Polarbear surveys. As ACT Polarbear, these composed of scans sweep azimuth at constant elevation. explore both small (0.42 m) aperture (SAT) a large (6 telescope (LAT)....
The Simons Observatory (SO) is an upcoming experiment that will study temperature and polarization fluctuations in the cosmic microwave background (CMB) from Atacama Desert Chile. SO field both a large aperture telescope (LAT) array of small telescopes (SATs) observe six bands with center frequencies spanning 27 to 270~GHz. Key considerations during design phase are vast, including number cameras per telescope, focal plane magnification pixel density, in-band optical power camera throughput,...
The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series telescopes which cover angular scales between one arcminute tens degrees sample frequencies 27 270 GHz. Here we present current design large aperture telescope receiver (LATR), 2.4m diameter cryostat that be mounted on SO 6m largest CMB to date. size was chosen take advantage focal plane area having high Strehl ratios, is inherent Cross-Dragone...
The Simons Observatory (SO) will measure the cosmic microwave background (CMB) in both temperature and polarization over a wide range of angular scales frequencies from 27-270 GHz with unprecedented sensitivity. One technology for coupling light onto ~50 detector wafers that SO field is spline-profiled feedhorns, which offer tunability between efficiency control beam leakage effects. We present efforts to scale up feedhorn production their viability future CMB experiments, including...
The Simons Observatory (SO) is a cosmic microwave background (CMB) experiment from the Atacama Desert in Chile comprising three small-aperture telescopes (SATs) and one large-aperture telescope (LAT). In total, SO will field over 60,000 transition-edge sensor (TES) bolometers six spectral bands centered between 27 280 GHz order to achieve sensitivity necessary measure or constrain numerous cosmological quantities. this work, we focus on SATs which are optimized search for primordial...
In this proceeding, we present studies of instrumental systematic effects for the Simons Obsevatory (SO) that are associated with detector system and its interaction full SO experimental systems. will measure Cosmic Microwave Background (CMB) temperature polarization anisotropies over a wide range angular scales in six bands bandcenters spanning from 27 GHz to 270 GHz. We explore including intensity-to-polarization leakage due coupling optics, bolometer nonlinearity, uncalibrated gain...
The Simons Observatory (SO) will observe the temperature and polarization anisotropies of cosmic microwave background (CMB) over a wide range frequencies (27 to 270 GHz) angular scales by using both small (0.5 m) large (6 aperture telescopes. SO telescopes target degree where primordial B-mode signal is expected peak. incoming be modulated cryogenic, continuously-rotating half-wave plate (CRHWP) mitigate systematic effects arising from slowly varying noise detector pair-differencing. In this...
The Simons Observatory will consist of a single large (6 m diameter) telescope and number smaller (∼0.5 refracting telescopes designed to measure the polarization Cosmic Microwave Background unprecedented accuracy. aperture is same design as CCAT-prime telescope, modified Crossed Dragone with field-of-view over 7.8 degrees diameter at 90 GHz. This paper presents an overview cold reimaging optics for this what drove our choice 350–400 mm silicon lenses in 2.4 cryostat other possibilities. We...
The Simons Observatory (SO) will provide precision polarimetry of the cosmic microwave background (CMB) using a series telescopes which cover angular scales from arc-minutes to tens degrees, contain over 60,000 detectors, and observe in frequency bands between 27 GHz 270 GHz. SO consist six-meter-aperture telescope initially coupled roughly 35,000 detectors along with an array half-meter aperture refractive cameras, additional 30,000+ detectors. large receiver (LATR) is six-meter crossed...
The Simons Observatory (SO) is a new experiment that aims to measure the cosmic microwave background (CMB) in temperature and polarization. SO will polarized sky over large range of frequencies angular scales using combination small ($\sim0.5 \, \rm m$) ($\sim 6\, m $) aperture telescopes be located Atacama Desert Chile. This work part series papers studying calibration, sensitivity, systematic errors for SO. In this paper, we discuss current efforts model optical effects, how these have...
While Type Ia Supernovae (SNe Ia) are one of the most mature cosmological probes, next era promises to be extremely exciting in number different ways SNe used measure various parameters. Here we review experiments 2020s that will yield orders magnitudes more Ia, and new understandings capabilities constrain systematic uncertainties at a level match these statistics. We then discuss five probes with Ia: conventional Hubble diagram for measuring dark energy properties, distance ladder...
Abstract The Simons Observatory is a Cosmic Microwave Background experiment to observe the microwave sky in six frequency bands from 30 290 GHz. Observatory—at ∼5200 m altitude—comprises three Small Aperture Telescopes and one Large Telescope (LAT) at Atacama Desert, Chile. This research note describes design current status of LAT along with its future timeline.
Context. Galaxy clusters are an important tool for cosmology, and their detection characterization key goals current future surveys. Using data from the Wide-field Infrared Survey Explorer (WISE), Massive Distant Clusters of WISE (MaDCoWS) located 2839 significant galaxy overdensities at redshifts 0.7 ≲ z 1.5, which included extensive follow-up imaging Spitzer Space Telescope to determine cluster richnesses. Concurrently, Atacama Cosmology (ACT) has produced large area millimeter-wave maps...
The Simons Observatory (SO) is a set of cosmic microwave background instruments that will be deployed in the Atacama Desert Chile. key science goals include setting new constraints on inflation, measuring large scale structure with gravitational lensing, and constraining neutrino masses. Meeting these SO requires high sensitivity improved calibration techniques. In this paper, we highlight few most important instrument calibrations, including spectral response, gain stability, polarization...
The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which observe from the Atacama Desert in Chile. In total, SO field over 60,000 transition-edge sensor (TES) bolometers six spectral bands centered between 27 280 GHz order to achieve sensitivity necessary measure or constrain numerous cosmological quantities, as outlined Collaboration et al. (2019). These require 33 highly...
The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series telescopes which cover angular scales between one arcminute tens degrees, contain over 60,000 detectors, sample frequencies 27 270 GHz. SO consist six-meter-aperture telescope coupled to 30,000 detectors along with an array half-meter aperture refractive cameras, together couple additional 30,000+ detectors. measure fundamental cosmological...