A5071856444- Galaxies: Formation, Evolution, Phenomena
- Astronomy and Astrophysical Research
- Cosmology and Gravitation Theories
- Astrophysical Phenomena and Observations
- Astrophysics and Cosmic Phenomena
- Neuroscience and Neuropharmacology Research
- Memory and Neural Mechanisms
- Gamma-ray bursts and supernovae
- Scientific Research and Discoveries
- Neural dynamics and brain function
- Radio Astronomy Observations and Technology
- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- CCD and CMOS Imaging Sensors
- Neurobiology and Insect Physiology Research
- Remote Sensing in Agriculture
- Computational Physics and Python Applications
- Neuroendocrine regulation and behavior
- Plant Water Relations and Carbon Dynamics
- Black Holes and Theoretical Physics
- Breast Cancer Treatment Studies
- Photoreceptor and optogenetics research
- Pulsars and Gravitational Waves Research
- Radiomics and Machine Learning in Medical Imaging
- Aerogels and thermal insulation
Icahn School of Medicine at Mount Sinai
2019-2025
Capital Medical University
2015-2025
Allen Institute for Brain Science
2025
Shandong University of Finance and Economics
2024
Université de Technologie de Troyes
2024
University of California, Berkeley
2007-2023
Ningxia Medical University General Hospital
2023
Ningxia Medical University
2023
Beijing Tongren Hospital
2021-2022
Ministry of Industry and Information Technology
2021-2022
(Abridged for arXiv)We investigate the properties of halos, galaxies and blackholes to z=0 in high resolution hydrodynamical simulation MassiveBlack-II (MBII) which evolves a LCDM cosmology comoving volume Vbox=100(Mpc/h)^3. MBII is highest this size includes self-consistent model star formation, black hole accretion associated feedback. We provide browser web application enables interactive search tagging subhalos their publicly release our galaxy catalogs. Our analysis halo mass function...
We present nbodykit, an open-source, massively parallel Python toolkit for analyzing large-scale structure (LSS) data. Using bindings of the Message Passing Interface (MPI), we provide implementations many commonly used algorithms in LSS. nbodykit is both interactive and scalable piece scientific software, performing well a supercomputing environment while still taking advantage tools provided by ecosystem. Existing functionality includes estimators power spectrum, 2 3-point correlation...
Matter evolved under the influence of gravity from minuscule density fluctuations. Nonperturbative structure formed hierarchically over all scales and developed non-Gaussian features in Universe, known as cosmic web. To fully understand formation Universe is one holy grails modern astrophysics. Astrophysicists survey large volumes use a ensemble computer simulations to compare with observed data extract full information our own Universe. However, evolve billions particles years, even...
We introduce FastPM, a highly scalable approximated particle mesh (PM) N-body solver, which implements the PM scheme enforcing correct linear displacement (1LPT) evolution via modified kick and drift factors. Employing two-dimensional domain decomposing scheme, FastPM scales extremely well with very large number of CPUs. In contrast to Comoving-Lagrangian (COLA) approach, we do not require split force or track separately 2LPT solution, reducing code complexity memory requirements. compare...
Abstract Tracking animal behavior by video is one of the most common tasks in life sciences. Although commercial software exists for executing this task, they often present enormous cost to researcher and can entail purchasing hardware that expensive lacks adaptability. Additionally, underlying code proprietary. Alternatively, available open-source options frequently require model training be challenging those inexperienced with programming. Here we an platform independent set analysis...
Observations of the most distant bright quasars imply that billion solar mass supermassive black holes (SMBHs) have to be assembled within first 800 million years. Under our standard galaxy formation scenario such fast growth implies large gas densities providing sustained accretion at critical or supercritical rates onto an initial hole seed. It has been a long standing question whether and how high can achieved centers early galaxies. Here we use new MassiveBlack cosmological hydrodynamic...
We introduce the BlueTides simulation and report initial results for luminosity functions of first galaxies AGN, their contribution to reionization. was run on BlueWaters cluster at NCSA from $z=99$ $z=8.0$ includes 2$\times$7040$^3$ particles in a $400$Mpc/h per side box, making it largest hydrodynamic ever performed high redshift. pressure-entropy formulation smoothed particle hydrodynamics, gas cooling, star formation (including molecular hydrogen), black hole growth models stellar AGN...
Many scientists have devoted themselves to the study of interaction between subwavelength structures and electromagnetic waves. These are commonly composed regular arrays protuberances, which can be artificially designed. However, extending from 2D periodic patterns 3D disordered has not been studied yet. In this study, we total diffuse reflectivity carbon aerogels with various networks randomly oriented particle-like nanostructures by using normally incident visible light (430-675 nm). We...
One of the main unsolved problems cosmology is how to maximize extraction information from nonlinear data. If data are usual approach employ a sequence statistics (N-point statistics, counting clusters, density peaks or voids etc.), along with corresponding covariance matrices. However, this computationally prohibitive and has not been shown be exhaustive in terms content. Here we instead develop hierarchical Bayesian approach, expanding likelihood around maximum posterior linear modes,...
The growth of the most massive black holes in early Universe, consistent with detection highly luminous quasars at z > 6 implies sustained, critical accretion material to grow and power them. Given a hole (BH) seed scenario, it is still uncertain which conditions Universe allow fastest BH growth. Large-scale hydrodynamical cosmological simulations structure formation us explore conducive earliest supermassive BHs. We use hydrodynamic simulation BlueTides, incorporates variety baryon physics...
Miniature microscopes have gained considerable traction for in vivo calcium imaging freely behaving animals. However, extracting signals from raw videos is a computationally complex problem and remains bottleneck many researchers utilizing single-photon imaging. Despite the existence of powerful analysis packages designed to detect extract dynamics, most either key parameters that are hard-coded or insufficient step-by-step guidance validations help users choose best parameters. This makes...
The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well being an interesting signature formation and evolution (albeit one that difficult predict theoretically). Here we investigate relative orientations stars dark matter haloes subhaloes (central satellite) extracted from MassiveBlack-II simulation, state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar active galactic nucleus...
As galaxy surveys begin to measure the imprint of baryonic acoustic oscillations (BAO) on large-scale structure at sub-percent level, reconstruction techniques that reduce contamination from nonlinear clustering become increasingly important. Inverting continuity equation, we propose an Eulerian growth-shift algorithm does not require displacement any objects, which is needed for standard Lagrangian BAO algorithm. In real-space DM-only simulations yields 95% signal-to-noise obtained...
We present the UNIT $N$-body cosmological simulations project, designed to provide precise predictions for nonlinear statistics of galaxy distribution. focus on characterizing relevant emission line and luminous red galaxies in current upcoming generation surveys. use a suite particle mesh (FastPM) as well with full calculations mass resolution $\sim 1.2\times10^9\,h^{-1}$M$_{\odot}$ investigate recently suggested technique Angulo & Pontzen 2016 suppress variance study redshift space...
The intrinsic alignment of galaxies with the large-scale density field is an important astrophysical contaminant in upcoming weak lensing surveys. We present detailed measurements galaxy alignments and associated ellipticity–direction (ED) projected shape (wg+) correlation functions for cosmological hydrodynamic MassiveBlack-II simulation. carefully assess effects on shapes, misalignment stellar component dark matter two-point statistics iterative weighted (by mass luminosity) definitions...
We employ the very large cosmological hydrodynamical simulation BlueTides to investigate predicted properties of galaxy population during epoch reionization (z > 8). has a resolution and volume ((400/h ≈ 577)3 cMpc3) providing galaxies that is well matched depth area current observational surveys targeting high-redshift Universe. At z = 8, includes almost 160 000 with stellar masses >108 M⊙. The by closely matches constraints on both mass function far-UV (150 nm) luminosity function....
We present a method to reconstruct the initial conditions of universe using observed galaxy positions and luminosities under assumption that can be calibrated with weak lensing give mean halo mass. Our relies on following gradients forward model since standard way identify halos is non-differentiable results in discrete sample objects, we propose framework position mass field starting from non-linear matter Neural Networks. evaluate performance our multiple metrics. more than $95\%$...
We present an efficient and accurate method for simulating massive neutrinos in cosmological structure formation simulations, together with easy to use public implementation. Our builds on our earlier implementation of the linear response approximation (LRA) neutrinos, coupled N-body code cold dark matter particles. The LRA's good behaviour at early times regime is preserved, while better following non-linear clustering small scales. Massive are split into initially "fast" "slow" components....
The Quijote simulations are a set of 44,100 full N-body spanning more than 7,000 cosmological models in the $\{\Omega_{\rm m}, \Omega_{\rm b}, h, n_s, \sigma_8, M_\nu, w \}$ hyperplane. At single redshift contain 8.5 trillions particles over combined volume $(h^{-1}{\rm Gpc})^3$; each simulation follow evolution $256^3$, $512^3$ or $1024^3$ box $1~h^{-1}{\rm Gpc}$ length. Billions dark matter halos and cosmic voids have been identified simulations, whose runs required 35 million core hours....
In this work we establish and test methods for implementing dynamical friction massive black hole pairs that form in large volume cosmological hydrodynamical simulations which include galaxy formation growth. We verify our models parameters both individual dynamics the population volumes. Using model of (DF) from collisionless particles, holes can effectively sink close to center, provided hole's mass is at least twice lowest resolution particles simulation. Gas drag also plays a role...
The observed UV continuum slope of star-forming galaxies is strongly affected by the presence dust. Its observation then a potentially valuable diagnostic dust attenuation, particularly at high redshift where other diagnostics are currently inaccessible. Interpreting in context attenuation often achieved assuming empirically calibrated Meurer et al. relation. Implicit this relation assumption an intrinsic (β = −2.23). However, results from numerical simulations suggest that slopes...
We use the high-resolution simulation MassiveBlackII to examine scaling relations between black hole (BH) mass and host galaxy properties (σ, total M* LV), finding good agreement with recent observational data, especially at high-mass end. find Gaussian intrinsic scatter (∼half observed scatter) about all three relations, except among most massive objects. Below z ∼ 2 slope of remain roughly z-independent, only steepen by 50 per cent 4. The normalization σ, LV evolve 0.3, 0.43 dex, while...