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It uses parameterizations of a detector's fiducial area or volume, selection efficiency, energy resolution, angular resolution, and event classification efficiency to convert (surface) neutrino fluxes into mean event rates in bins of observable space. ECCSAMPLES solves the inverse cumulative density function (CDF) of a Beta distribution, sometimes called the IDF or inverse transform sampling. 022) to read in simulation datasets and extends it to provide realistic synthetic observations appropriate for studies of the interstellar, circumgalactic, and intergalactic media.

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010) and provides useful information on the viability of mergers of white dwarfs as a progenitor for Type Ia supernovae. NRPy+ uses SymPy as its computer algebra system backend. MixT accurately predicts T derived from a single-temperature fit for a multi-component thermal plasma. It is based on a modern machine learning technique (feed-forward artificial neural network) by supervising a large data pool obtained from the IRBEM library, which is the traditional source for numerically calculating the L* values. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. A self-organizing map (SOM) can be used to identify planetary candidates from Kepler and K2 datasets with accuracies near 90% in distinguishing known Kepler planets from false positives. The statistical framework comprises algorithms which define likelihood functions, minimization, Monte Carlo, Fisher Matrix and profile likelihood methods. The pipeline organizes the raw data, creates SOF and configuration files, runs the calibration and science recipes, and creates plots of the images and extracted spectra. IRSFRINGE is available as a stand-alone package and is also part of the Spectroscopic Modeling, Analysis and Reduction Tool (SMART, ascl:1210.

The FFTLog algorithm can be thought of as the Fast Fourier Transform (FFT) of a logarithmically spaced periodic sequence (= Hankel Transform). It uses an integration algorithm for models that cannot be quickly calculated analytically, and in typical use, the batman Python package can calculate a million model light curves in well under ten minutes for any limb darkening profile. BELLAMY is a cross-matching algorithm designed primarily for radio images, that aims to match all sources in the supplied target catalogue to sources in a reference catalogue by calculating the probability of a match. Potential uses of the DDPM include accurate in-painting of occluded data, such as satellite trails, and domain transfer, where new input images can be processed to mimic the properties of the DDPM training set. Source positions and fluxes are then loaded into a SQL database for association and variability detection. 013) and AstroPy (ascl:1304. Elise jake malik and xiao each solved the same inequality in america. QSFit performs automatic analysis of Active Galactic Nuclei (AGN) optical spectra. It is similar to Markov Chain Monte Carlo (MCMC) in that it generates samples that can be used to estimate the posterior probability distribution. This library works for 1D, 2D, and 3D data files and for any amount of nested-grid levels. Curvit is available on PyPI.

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CaTffs predicts the strength of calcium triplet indices (CaT*, PaT and CaT) on the basis of empirical fitting functions and performs required interpolations between the different local functions. It also corrects the radiation flux for relativistic effects, and assesses the impact of this on the wind velocity. Fourierdimredn (Fourier dimensionality reduction) implements Fourier-based dimensionality reduction of interferometric data. It uses chemical networks downloaded from the KInetic Database for Astrochemistry (KIDA) but the model can be adapted to any network. Trilogy determines the intensity scaling automatically and independently in each channel to display faint features without saturating bright features. GWToolbox simulates gravitational wave observations for various detectors. C from Numerical Recipes in C (Press et al. Elise jake malik and xiao each solved the same inequality in math. This code requires RADEX to be installed locally.

It implements plotting functionality, handles MS tables with spectral windows with different number of channels, and can import visibilities from ASCII to MS Table. This model of instance segmentation also performs image segmentation at the pixel level, and has shown a Mean Average Precision (mAP) of 0. Written in Python, it calculates light curves for any radially symmetric stellar limb darkening law, and where planets are modeled as two semi-circles of different radii. 002) and, in particular, it precludes the use of fv (ascl:1205. In these visualizations, each one- and two-dimensional projection of the sample is plotted to reveal covariances. Driven by a plain text input file, the pipeline is modular and can be run in stages. The particles occupy a coordinate frame that is enforced to be consistent, such that particles loaded on-the-fly will match e. rotations and translations of particles already in memory. PMOIRED models astronomical spectro-interferometric data stored in the OIFITS format. It is a fast, distributed-memory, planar-parallel code.

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The pipeline's design allows for fast startup and easy implementation; the package offers a suite of robust default and optional tools for surface brightness profile extractions and related methods. The solver computes the chemical evolution of gas-phase species at a fixed temperature and density and can be used in one dimension (1D) if a grid of temperature, density, and visual extinction is provided. E-field Parallel Imaging Correlator (EPIC), a highly parallelized Object Oriented Python package, implements the Modular Optimal Frequency Fourier (MOFF) imaging technique. ATHOS can be configured to run in parallel in an arbitrary number of threads, thus enabling the fast and efficient analysis of huge datasets. The parameterization is similar to that in Halofit (ascl:1402.

However, the development of this package is part of the LSST Science Pipeline; the meas_deblender package contains a wrapper to implement the algorithms here for the LSST stack. If one image is supplied, then the pixels are binned by fractional error on the intensity. SENR (Simple, Efficient Numerical Relativity) provides the algorithmic framework that combines the C codes generated by NRPy+ (ascl:1807. Fringes that originate from the detector subtrates are observed in the IRS Short-High (SH) and Long-High (LH) modules.

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WzBinned extracts binned and uncorrelated estimates of dark energy equation of state w(z) using Type Ia supernovae Hubble diagram and other cosmological probes and priors. The z -transformed discrete correlation function (ZDCF) is a method for estimating the CCF of sparse, unevenly sampled light curves. The models consist of plane-parallel slabs standing vertically above the solar surface. Such particle realizations are useful for Monte Carlo experiments and provide consistent initial conditions for cosmological N-body simulations.

The algorithm described by this code was incorporated into the tclean task within CASA as auto-multithresh. Walter was written with the expectation that such calculations will be very useful for planning surveys with the Nancy Grace Roman Space Telescope (RST, formerly WFIRST). The package contains two main modules: BackgroundSolver solves the background equations, and the MsSolver module solves and analyses the MS equations. LORENE classes implement basic structures such as arrays and matrices, but also abstract mathematical objects, such as tensors, and astrophysical objects, such as stars and black holes. Vortex performs a Helmholtz-Hodge decomposition on vector fields defined on AMR grids, decomposing a vector field in its solenoidal (divergence-less) and compressive (curl-less) parts. 083) evolutionary tracks for single, non-interacting, and interacting binaries organized in grids. In its basic set-up, the GIST pipeline extracts stellar kinematics, performs an emission-line analysis, and derives stellar population properties from full spectral fitting and via the measurement of absorption line-strength indices by exploiting pPXF (ascl:1210. Later releases added new astronomy-specific applications to this sound framework. Q-transforms of the data windows that triggered TOF detections. Output is a summary of void properties in plain ASCII; a Python API is provided for analysis tasks, including loading and manipulating void catalogs and particle members, filtering, plotting, computing clustering statistics, stacking, comparing catalogs, and fitting density profiles. The modeled results are saved and can be directly passed to a Python dictionary for analysis and plotting.

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All ixpeobssim simulation and analysis tools are fully configurable via the command line. Interpolates particle data onto either a Cartesian (uniform) grid or an adaptive mesh refinement (AMR) grid where each cell contains no more than one particle. Molsoft operates, monitors and schedules observations, both through predetermined schedule files and fully dynamically, at the refurbished Molonglo Observatory Synthesis Radio Telescope (MOST). They also provide information about stellar processes and the evolution of the galactic disk. 008), part of the HEASARC's HEAsoft (ascl:1408. PDFchem models the cold ISM at moderate and large scales using functions connecting the quantities of the local and the observed visual extinctions and the local number density with probability density functions. CMC is parallelized using the Message Passing Interface (MPI), and is pinned to the COSMIC (ascl:2108. Smoothed Particle Hydrodynamics (SPH) is a Lagrangian particle method that approximates a continuous fluid as discrete nodes, each carrying various parameters such as mass, position, velocity, pressure, and temperature. ORIGIN performs blind detection of faint emitters in MUSE datacubes. The approximate sampling method is analytic and thus very fast, reproducing physically permissible samples in 97. LP-VIcode computes variational chaos indicators (CIs) quickly and easily. 013) for its MCMC; its forward model is a neural network surrogate model trained by MARGE (ascl:2003. CMasher provides a curated collection of scientific colormaps that are perceptually uniform sequential using the viscm package (ascl:2102. The pipeline is controlled by simple parameter files and can either be invoked on the command line or interactively through a modern graphical user interface.

BoxRemap remaps the cubical domain of a cosmological simulation into simple non-cubical shapes. Two-point correlations may be auto-correlations or cross-correlations, including any combination of shear, kappa, and counts. Based around the cygrid package from Benjamin Winkel and Daniel Lenz. It is written in Python and is started from the command-line. In addition, the evolution includes the transfer of angular momentum between the stellar convective and radiative zones, effect of the stellar evolution on the tidal dissipation efficiency, and stellar core and envelope spins and loss of stellar convective zone angular momentum to a magnetically launched wind.

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So_noise_models is the N(ell) noise curve projection code for the Simons Observatory. There is also a GUI to overlay star catalogs on an image and an option to download them directly from the Vizier server. Tempo is the basis for the Tempo2 (ascl:1210. Python notebooks are provided to demonstrate using Citlalicue for both functions. IFSRED also contains additional software specific to reducing data from GMOS and the Gemini Near-Infrared Integral Field Spectrograph (NIFS). The second data release (DR2) of the archive contains over 3. It is accurate on a single timestep and stable over many iterations with decreased accuracy, though performs less well at low visual extinctions. 015); running the program in parallel greatly extends the range of scales and times that can be simulated. Galaxy modelling with ProFit, using the previously determined PSF and user-specified models. It is based on the Particle Mesh (PM) technique.

It takes advantage of Starlink's (ascl:1110. The disk is assumed to be in Keplerian rotation at a radius lower than the centrifugal radius (which can be set to a large value, for a purely Keplerian disk), and in infall with rotation beyond the centrifugal radius. The input file contains a list of options that can be set, as well as output parameters that print to a file during an integration. The code can be extended to other models (physical or empirical), to incorporate data from other experiments, or to use alternative Monte-Carlo sampling engines as required. The code first calculates a magnetic potential using a modified Green's function method and then uses a finite differencing scheme to calculate the magnetic field from the potential. Its basic form can run a baryonic group finder to identify galaxies and a halo finder to identify dark matter halos; it can also assign said galaxies to their respective halos, calculate halo & galaxy global properties, and iterate through previous time steps to identify the most-massive progenitors of each halo and galaxy. LiSA can analyze input data cubes of any size with pipelines that automatically decompose data into different domains for parallel distributed analysis.