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The example input files provide a guide for the syntax and grammar of EqTide. The fragmentation code models fragmentation in collisions for the C version of REBOUND (ascl:1110. Elise jake malik and xiao each solved the same inequality in school. The pipeline is only CPU-based and can be easily and quickly deployed in computing nodes for testing purposes or data processes. Once the user obtains the original catalogs, running ETL pre-processing generates a sky zoning file. Written in IDL under Xwindows, PIA offers a full context sensitive graphical interface for retrieving, accessing and analyzing ISOPHOT data. Kd-match matches stellar catalogs for which the transformation between the coordinate systems of the two catalogs is unknown and might include shearing.

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The code provides a light-weighted API of a refined version of an algorithm originally implemented in lenstronomy (ascl:1804. Working in the range of 3, 650-10, 200 Angstroms, the automatic spectral typing algorithm compares important spectral lines to template spectra and determines the best matching spectral type, ranging from O to L type stars. Drive-casa provides a Python interface for scripting of CASA (ascl:1107. Elise jake malik and xiao each solved the same inequality in order. The algorithm is based on sparse regularization; adding a sparse penalty in the recovery leads to far better accuracy in terms of ellipticity error, especially at low S/N. 002) parameter inference code for cosmology offers new ingredients that improve the performance of Metropolis-Hastings sampling, speeding up convergence and offering significant time improvement in difficult runs.

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The IDL package reduces and analyzes radio astronomy data. SpaceHub uses unique algorithms for fast precise and accurate computations for few-body problems ranging from interacting black holes to planetary dynamics. RM-Tools is the core package for the pipelines used for the POlarized Sky Survey of the Universe's Magnetism (POSSUM) and the polarization component of the Very Large Array Sky Survey (VLASS). The first is potential_scale_reduction(chains... ), which estimates the potential scale reduction factor, also known as Rhat, for multiple scalar chains. To preserve all available small scale information, Glimpse avoids any binning of the irregularly sampled input shear and flexion fields and treats the mass-mapping problem as a general ill-posed inverse problem, regularized using a multi-scale wavelet sparsity prior. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. The Python code provides a class for the user to store measured attributes for each radio source, and to which model derived redshift probability density functions are returned. It can also isolate filaments embedded in a crowded position–position–velocity (PPV) space. The approximate sampling method is analytic and thus very fast, reproducing physically permissible samples in 97. LensingETC optimizes observing strategies for multi-filter imaging campaigns of galaxy-scale strong lensing systems. Radio astronomical observations are typically three dimensional and stored as data cubes.

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The framework rapidly and reliably localizes sources in optical images. 014), is an implementation of a flux-conservative Godunov-type algorithm for compressible magnetohydrodynamics. Elise jake malik and xiao each solved the same inequality in relation. These routines are neatly packaged in a graphical user interface, developed using tkinter, facilitating use. 001) for exoplanet modeling. 016) to produced physical properties derived from the MaNGA spectroscopy. It is a Python-based probabilistic programming language which composes and fits models using a range of Bayesian inference libraries, such as emcee (ascl:1303.

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Only 10-20 points per galaxy are needed to reconstruct both the individual PDFs and the ensemble redshift distribution, N(z), to an accuracy of 99. ExoData is a python interface for accessing and exploring the Open Exoplanet Catalogue. 063) software suites and allows different source extraction strategies to be chosen. 021), making that library's functionality more accessible through a Python interface; it also provides MCMC-based followup of promising candidates from wide-parameter-space searches. AstroStat is available in two versions with an identical interface and features: as a web service that can be run using any standard browser and as an offline application. Python-CPL is a framework to configure and execute pipeline recipes written with the Common Pipeline Library (CPL) (ascl:1402.

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The code fits the absorption line profiles within specified wavelength ranges and generates posterior distributions for the column density, Doppler parameter, and redshifts of the corresponding absorbers. PCCDPACK analyzes polarimetry data. Nbody6tt, based on Aarseth's nbody6 (ascl:1102. The code is written as a C++ library and wrapped as a Python package, and can be called from either C++ or Python. PROPER simulates the propagation of light through an optical system using Fourier transform algorithms (Fresnel, angular spectrum methods).

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Py-sdm (Support Distribution Machines) is a Python implementation of nonparametric nearest-neighbor-based estimators for divergences between distributions for machine learning on sets of data rather than individual data points. Fluid and radiation exchange four-momentum in an explicit first-order operator-split fashion. It was designed to be a data mining tool for finding high-quality stellar observations in the data archives of the National Virtual Observatory. JETGET accesses, visualizes, and analyses (magnetized-)fluid dynamics data stored in Hierarchical Data Format (HDF) and ASCII files. There are three key aspects to the cFS architecture: a dynamic run-time environment, layered software, and a component based design, making it suitable for reuse on NASA flight projects and/or embedded software systems. It uses telluric features to provide absolute wavelength calibration, and then cross-correlates with a standard star. This code comes with a GitHub tutorial on how to use the Min-CaLM package.

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Skylens++ implements a Layer-based raytracing framework particularly well-suited for realistic simulations of weak and strong gravitational lensing. The method has four tuning parameters, the number of predictor stars or pixels, the autoregressive window size, and two L2-regularization amplitudes for model components, and consistently produces low-noise light curves. Using nested sampling algorithms, it performs a thorough sampling of the parameter space and a model comparison via Bayesian evidences. RamsesGPU is a reimplementation of RAMSES (ascl:1011.

ZeldovichRecon computes the halo correlation function using the Zeldovich approximation. Pynucastro interfaces to the nuclear reaction rate databases, including the JINA Reaclib nuclear reactions database. Barcode (BAyesian Reconstruction of COsmic DEnsity fields) samples the primordial density fields compatible with a set of dark matter density tracers after cosmic evolution observed in redshift space. 024) simulations and plots the data. The DRP consists of two primary parts: the 2d stage that produces flux calibrated fiber spectra from raw individual exposures, and the 3d stage that combines multiple flux calibrated exposures with astrometric information to produce stacked data cubes. It generates MRP quantities with the MRP class, such as differential number counts and cumulative number counts, and offers various methods for generating normalizations. The KinMS (KINematic Molecular Simulation) package simulates observations of arbitrary molecular/atomic cold gas distributions from interferometers and line observations from integral field units. MHF is a Dark Matter halo finder that is based on the refinement grids of MLAPM. MixT accurately predicts T derived from a single-temperature fit for a multi-component thermal plasma. It has been used in the analysis of the Dark Energy Survey and to optimize the Large Synoptic Survey Telescope and the Wide-Field Infrared Survey Telescope, and is useful for innovative theory projects that test new concepts and methods to enhance the constraining power of cosmological analyses.

It works on any 3-column light curve that contains time, flux, and error. It provides an efficient, extendable, and accurate way of comparing theoretical inflationary predictions with cosmological data and supports many (~70) models of inflation. The Shape COnstraint REstoration algorithm (SCORE) is a proximal algorithm based on sparsity and shape constraints to restore images. It provides an efficient and robust numerical evaluation of the inflationary perturbation spectrum, and allows the free parameters in the inflationary potential to be estimated.

Line broadening cross sections for the broadening of spectral lines by collisions with neutral hydrogen atoms have been tabulated by Anstee & O'Mara (1995), Barklem & O'Mara (1997) and Barklem, O'Mara & Ross (1998) for s–p, p–s, p–d, d–p, d–f and f–d transitions. The simulations of matter density and 21 cm maps are performed with the code 21cmFAST (ascl:1102. Java and Fortran versions of the code are available. 010) and SME (ascl:1202. The Bayesian-based Gaussian Process model AsteroGaP (Asteroid Gaussian Processes) fits sparsely-sampled asteroid light curves. Given a timestream, with each point being the arrival times of a source, the software computes the estimated period. TAME measures the equivalent width (EWs) in high-resolution spectra. 008) and the galpy extension, which implements the fast calculation of the perturbed stream structure. It uses pseudo-spectral methods to compute the evolution of a complex scalar field governed by the Schrödinger-Poisson system of coupled differential equations. 011) and issues a PixelMap instance, which is a map from one 2d coordinate system ("pixel") to another ("world") 2d system. Observations of a standard star are included for convenience; the code also requires both the telluric and non-telluric-corrected spectra. Once the software environment is built, adding analysis steps is as easy as defining "Make" rules to allow parallelized operations, and not repeating operations that do not need to be recreated. It mainly applies on the spectroscopic data from high resolution spectral survey.

It creates plots and movies based on output from the MESA stellar evolution code (ascl:1010. The code accepts Numpy binary files or FITS as input, takes the observed (i. e. with PSF effects and noise) stack of galaxy images and a known PSF, and attempts to reconstruct the original images. PyWPF (Waterfall Principal Component Analysis Folding) finds periodicity in one-dimensional timestream data sets; it is particularly designed for very high noise situations where traditional methods may fail. The code merges the easy-to-use API of scikit-learn with the modularity of probabilistic modeling, including general mixture and hidden Markov models and Bayesian networks, to allow users to specify complicated models without the need to be concerned about implementation details. It is capable of reducing single or multi-extension fits files. BlaST (Blazar Synchrotron Tool) estimates the synchrotron peak of blazars given their spectral energy distribution. The library provides an API to open GSD files and read their contents.

PREVIS is a Python module that provides functions to help determine the observability of astronomical sources from long-baseline interferometers worldwide: VLTI (ESO, Chile) and CHARA (USA). The three components are: - a modular framework for nested sampling algorithms (nested_sampling) and their development; - a test framework to evaluate the performance and accuracy of algorithms (testsuite); and. It allows study of the evolution of the black-hole spins along their precession cycles, performs gravitational-wave-driven binary inspirals using both orbit-averaged and precession-averaged integrations, and predicts the properties of the merger remnant through fitting formulas obtained from numerical-relativity simulations. 002), which fits only SZ data. The code uses the autocorrelation function (ACF) to identify stellar rotation periods up to one-third the observational baseline of the data. Above a critical dark matter-nucleus scattering cross section, any terrestrial direct detection experiment loses sensitivity to dark matter, since the Earth crust, atmosphere, and potential shielding layers start to block off the dark matter particles. The main idea is to take each detected line and guess what line it could be (and thus the redshift of the object). Systematics due to events on fast timescales, such as thruster firings, are sometimes poorly corrected for many short-cadence targets. Though not a pipeline, pipelines for complex analysis can be built on top of it. The Planck simulation package does not only provide Planck-like data, it can also be easily adopted to mimic the properties of other existing and upcoming CMB experiments. It facilitates interactive work as well as the creation of publication-quality plots with a python-based workflow many astronomers are accustomed to. Limb-darkening laws include linear, quadratic, logarithmic, square-root and three-parameter laws. CUDAHM enables one to simultaneously sample the values of the characteristics and the parameters of their parent population from their joint posterior probability distribution.

C is callable by RAMSES (ascl:1011. Dense_basis implements the Dense Basis method tailored to SED fitting, in particular, the task of recovering accurate star formation history (SFH) information from galaxy spectral energy distributions (SEDs).

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