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Such plots are useful for seeing the parameter covariances along with the priors when fitting a model to data. Wsynphot provides a broad set of filters, including observation facility, instrument, and wavelength range, and functions for imaging stars to produce a filter curve showing the transmission of light for each wavelength value. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. Users can add effects from a list of pre-implemented astrophysical forces or contribute new ones. This Fortran wrapper for Python also includes modules for delensing and bi-spectrum calculations.

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It offers fast evaluation of likelihoods for NPTF analyses and has an easy-to-use interface for performing non-Poissonian (as well as standard Poissonian) template fits using MultiNest (ascl:1109. R(sigma) is numerically calculated and the code is valid for arbitrary eccentricities and inclinations, including retrograde orbits. Elise jake malik and xiao each solved the same inequality state supreme courts. 015) and Eigentools (ascl:2101. The code is derived from the Source Extractor code base (written in C) and aims to produce results compatible with Source Extractor whenever possible. It can also generate single turbulent realizations. In testing, PyIMRPhenomD is considerably faster than the C implementation.

It applies the methods of Implicit Monte Carlo (IMC) and Discrete Diffusion Monte Carlo (DDMC) for static or homologously expanding spatial grids. Used with the SNAD ZTF data releases object viewer (ascl:2106. LAPACK provides routines for solving systems of simultaneous linear equations, least-squares solutions of linear systems of equations, eigenvalue problems, and singular value problems. Elise jake malik and xiao each solved the same inequality in class. M2mcluster performs made-to-measure modeling of star clusters, and can fit target observations of a Galactic globular cluster's 3D density profile and individual kinematic properties, including proper motion velocity dispersion, and line of sight velocity dispersion. These three modules work independently and have different dependencies on other packages and libraries; failed dependencies met in one module will not influence the usage of another module. Isca provides a framework for the idealized modeling of the global circulation of planetary atmospheres at varying levels of complexity and realism.

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It incorporates the cosmological dependence of the bias beyond the mapping of halo mass to peak height. It can apply coordinate transformations between Galactic, Ecliptic and Equatorial reference frames, apply custom rotations either to vectors or full maps, and read and write HEALPix maps to disk in FITS format. AstroAccelerate processes time-domain radio astronomy data. Elise jake malik and xiao each solved the same inequality in one. Iminuit is a Jupyter-friendly Python interface for the Minuit2 C++ library maintained by CERN's ROOT team. Exocartographer solves the exo-cartography inverse problem.

UNICOR analyzes spectra using 1-d CCF. The code reads in frequency shift measurements and their associated sensitivity kernels and outputs two-dimensional slices of the subsurface flow field at a constant depth and (optionally) the associated averaging kernels. It is based on tools developed in scikit-learn, with some usage requiring also the H2O package. Users can run their own simulations (of LSST and other surveys) or download the galaxy catalog and simulation outputs to use with their own code. SIP (Systematics-Insensitive Periodograms) extends the generative model used to create traditional sine-fitting periodograms for finding the frequency of a sinusoid by including systematic trends based on a set of eigen light curves in the generative model in addition to using a sum of sine and cosine functions over a grid of frequencies, producing periodograms with vastly reduced systematic features. All fits include intrinsic scatter in the generative model orthogonal to the hyperplane. Derived from AIMS (ascl:1611. The code calculates the speed and velocity distributions of DM at various positions on the Earth and also helps with the calculation of the average scattering probabilities. This information is used in post-processing to compute calibrated shear estimates via metacalibration. Distlink computes the minimum orbital intersection distance (MOID), or global minimum of the distance between the points lying on two Keplerian ellipses by finding all stationary points of the distance function, based on solving an algebraic polynomial equation of 16th degree. MTNeedlet relies on Healpy (ascl:2008. 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. LSDCat is a conceptually simple but robust and efficient detection package for emission lines in wide-field integral-field spectroscopic datacubes.

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In the case where a heliocentric radial velocity is missing for the host star, the single host-star multivariate Gaussian model is replaced with a series of host star models and numerically marginalized over by taking the numerical sum of the host-star model probabilities. BOND determines oxygen and nitrogen abundances in giant H II regions by comparison with a large grid of photoionization models. It includes interfaces to the cosmological theory codes CAMB (ascl:1102. The active learning technique controls possible biases that may arise from training with synthetic spectra and extends the applicability of the method to features absent in this kind of spectra. Both baryonic and dark matter contribute to the gravitational field. With PyXspec loaded, a user can run Xspec with Python language scripts or interactively at a Python shell prompt; everything in PyXspec is accessible by importing the package xspec into your Python script. J plots classifies and quantifies a pixelated structure, based on its principal moments of inertia, thus enabling automatic detection and objective comparisons of centrally concentrated structures (cores), elongated structures (filaments) and hollow circular structures (bubbles) from the main population of slightly irregular blobs that make up most astronomical images.

The ASPIC collection of about 400 image-processing programs was written using the Starlink "interim" environment in the 1980; the software is now obsolete. The code is tailored to work well without much human interaction on optical and infrared spectra in a wide range of instrument setups and signal-to-noise regimes. 006), PolyChord (ascl:1502. 018) and CFITSIO (ascl:1010. HENDRICS, a rewrite and update to MaLTPyNT (ascl:1502. A particle can represent a binary or a body. ExoTETHyS models exoplanetary transits, eclipsing binaries, and related phenomena.

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2013); it is available in both C and Fortran. Pycola is a multithreaded Python/Cython N-body code, implementing the Comoving Lagrangian Acceleration (COLA) method in the temporal and spatial domains, which trades accuracy at small-scales to gain computational speed without sacrificing accuracy at large scales. POSYDON (POpulation SYnthesis with Detailed binary-evolution simulatiONs) incorporates full stellar structure and evolution modeling for single and binary-star population synthesis. OXAF provides a simplified model of Seyfert Active Galactic Nucleus (AGN) continuum emission designed for photoionization modeling. Arcmancer can be used to solve various problems in numerical geometry, such as solving the curve equation of motion using adaptive integration with configurable tolerances and differential equations along precomputed curves. It can be used similarly as a Lomb-Scargle periodogram, and retrieves a figure which has a similar aspect but has fewer peaks due to aliasing.

PINT has been developed and implemented completely independently from traditional pulsar timing software such as TEMPO (ascl:1509. The selection function can be determined for any desired sample cuts in signal-to-noise ratio, u-g, r-i, and E(B-V). ExoCross is also capable of working with the recently proposed method of super-lines. The primary reduction programs, 'line' (for spectral-line reduction) and 'condar' (for continuum reduction), used the People-Oriented Parsing Service (POPS) as the command line interpreter. The code first fixes C/O using ratios of appropriate emission lines and, in a second step, calculates O/H and the ionization parameter from carbon lines in the UV. Gramsci can run in serial, OpenMP, MPI and hybrid parallel schemes. PYSOLATOR removes the orbital modulation from a binary pulsar and/or its companion.

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In addition to direct usage of the package and command line UI, the program can be used through a web interface. For objects not significantly detected in the low‐resolution image, it provides useful and quantitative information for setting upper limits. LensQuEst forecasts the signal-to-noise of CMB lensing estimators (standard, shear-only, magnification-only), generates mock maps, lenses them, and applies various lensing estimators to them. The software is implemented as a Python module. The core of the algorithm follows the method developed in UPMASK but introducing several key enhancements that make it not only more general, they also improve its performance. It enables the user to predict the spectra of UHECR (and of their secondaries), their composition and arrival direction distribution. Site with collection of codes and fundamental references on mean motion resonances. MARGE (Machine learning Algorithm for Radiative transfer of Generated Exoplanets) generates exoplanet spectra across a defined parameter space, processes the output, and trains, validates, and tests machine learning models as a fast approximation to radiative transfer. All algorithms are parallel and run with Message Passing Interface (MPI); the code is designed to be deployed on large super-computing facilities.

PNICER also offers access to the well-established NICER technique in a simple unified interface and is capable of building extinction maps including the NICEST correction for cloud substructure. 012) infrastructure libraries. It is the central component of a pipeline for systematically identifying and analyzing eclipsing binaries within a large dataset of light curves; the results of DEBiL can be used to flag light curves of interest for follow-up analysis. Both real (time-domain) and complex (frequency-domain) Love numbers can be computed. The sources can be extended and/or embedded, and discrete and/or diffuse. It is geared towards optical astronomy, where scenes are composed of stars and galaxies, but it is straightforward to apply it to other imaging data. In particular, galfast-generated catalogs are used to derive the stellar component of "Universe Model" catalogs used by the LSST Project. The code is parallelized and also shows a high degree of vectorization; it works with line profiles such as Doppler, Lorentzian and Voigt and supports several broadening schemes.

CGS is based on van Albada's code (1982) and is distributed in the NEMO (ascl:1010. The core of MERA is a database framework. Journal 86 (4), 619). Available in R and Python, the simple analytic scheme NFWdist performs highly efficient and exact sampling of the Navarro, Frenk & White (NFW) profile as a true probability distribution function, with the only variable being the concentration.

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