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HII-CHI-mistry_UV derives oxygen and carbon abundances using the ultraviolet (UV) lines emitted by the gas phase ionized by massive stars. It provides the solution up to the second degree of the limb darkening law. It can also fit radial velocity curves and light curves via the implementation of the non-linear least squares method and also via Markov Chain Monte Carlo method.

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7 days, as well as the maximum radius amongst them (in Earth radii) and orbital period of the planet with maximum radius (in Earth days) in order to predict the probability of additional transiters in this system with period greater than 13. Any reference database (atomic or molecular) can also be used for line identification. NEAT uses a Monte Carlo technique to robustly propagate uncertainties from line flux measurements through to the derived abundances. PyCELP solves a set of statistical equilibrium equations in the spherical statistical tensor representation for a multi-level atom for the no-coherence case. StellaR accesses and manipulates publicly available stellar evolutionary tracks and isochrones from the Pisa low-mass database. However, it can also produce spectra well outside of the parameter space of the emulator. Elise jake malik and xiao each solved the same inequality theorem. 003) and FoF-Halo-finder (ascl:2107. MPI_XSTAR invokes XSTINITABLE from HEASoft to generate a job list of XSTAR commands for given physical parameters. LOTUS provides a fast optimizer for obtaining stellar parameters based on Differential Evolution algorithm, well constrained uncertainty of derived stellar parameters from slice-sampling MCMC from PyMC3 (ascl:1610. It can fit models of spectral ageing on small spatial scales, offers automatic selection of regions based on user parameters (e. signal to noise), and automatic determination of the best-fitting injection index.

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This translation operator is analogous to the Euclidean translation in harmonic space and exhibits some useful properties. The framework builds forward models, simulates instruments, and performs retrievals, and provides a rich library of classes for building additional programs and using new atmospheric parameters. SimulateSearch simulates high time-resolution data in radio astronomy. SOPIE (Sequential Off-Pulse Interval Estimation) provides functions to non-parametrically estimate the off-pulse interval of a source function originating from a pulsar. Allesfitter provides an inference framework that unites the versatile packages ellc (ascl:1603. Which is designed to be called from Python using the ctypes library; and 3. ) Menura simulates the interaction between a fully turbulent solar wind and various bodies of the solar system using a novel two-step approach. In comparing the synthetic and real data, observational errors and incompleteness are taken into account, and a rudimentary treatment of the effect of unresolved binaries is also implemented. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. Most of the code is based on a class called SingleImage, which provides methods and properties for image processing such as PSF determination. Larch provides a complete set of XAFS Analysis tools and has support for visualizing and analyzing XRF maps and spectra, and additional tools for X-ray spectral analysis, data handling, and general-purpose data modeling. StellarWakes uses stellar kinematic data to search for dark matter (DM) subhalos through their gravitational perturbations to the stellar phase-space distribution. Korg computes stellar spectra from 1D model atmospheres and linelists assuming local thermodynamic equilibrium and implements both plane-parallel and spherical radiative transfer. Written in Python, Corral features a Model-View-Controller design pattern on top of an SQL Relational Database capable of handling custom data models, processing stages, and communication alerts. A large cache of low ℓ, m, n modes is available for download and can be installed with a single function call and interpolated to provide good initial guess for root-polishing at new values of spin.

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A modernization of FISHPACK is available as FISHPACK90 (ascl:1609. Support is provided to add additional white noise and convolve with beam functions. The code returns, in addition to the optimal set of parameters, their error covariance, and the corresponding model prediction. Elise jake malik and xiao each solved the same inequality in set. The probabilistic mass-radius relationship (M-R relation) is evaluated within a Bayesian framework, which both quantifies this intrinsic dispersion and the uncertainties on the M-R relation parameters. In addition, it offers the ability to add source terms to the equations and is parallelized based on MPI. Parameter files control different details, such as the mixing-length parameter, the overshooting, and the damping of the lines.

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Each layer has a phase diagram with equations of state chosen for each phase. The PyGSM module provides visualization utilities, file output in FITS format, and the ability to generate observed skies for a given location and date. The program allows the two sets of coordinates to be related by a linear, quadratic, or cubic transformation. These simple models agree very well with those from SPH (smoothed particle hydrodynamics) calculations of stellar collisions, and the subsequent stellar evolution of these models also matches closely that of the more accurate hydrodynamic models. Elise jake malik and xiao each solved the same inequality in real life. The following criteria were used to select main belt asteroids for USNO/AE98: Diameter greater than 300 km, presumably among the most massive asteroids. The code is modular and allows comparison of the effect of multiple different brightness distributions for a dataset. 004) is a prerequisite for building. The latter is suited for modern cosmological application and relies heavily on the former to perform the Hankel transforms. All XMM products and fit results are read into an XGA source storage structure, thus avoiding the need to leave a Python environment at any point during the analysis. Triceratops (Tool for Rating Interesting Candidate Exoplanets and Reliability Analysis of Transits Originating from Proximate Stars) validates planet candidates from the Transiting Exoplanet Survey Satellite (TESS). Physical models, typically consisting of ordinary differential equations for stellar, orbital, tidal, rotational, atmospheric, internal, magnetic, climate, and galactic evolution, are coupled together to simulate evolution for the age of a system.

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TROVE is also general and can be used with any internal coordinates. It also includes functionality for fitting data measurements and finding the optimal model parameters, using both MCMC and nonlinear optimization techniques. UniDAM obtains a homogenized set of stellar parameters from spectrophotometric data of different surveys. Written in C, the package is modular; its main routine is as small as possible and calls other routines, which perform tasks such as reading input, choosing and setting (starting or injection) parameters, and handling noise. Among other physical processes, it can model continuum emission from stars, continuum and line-emission from ionized gas, attenuation from dust, and mid- and far-IR emission from dust and polycyclic aromatic hydrocarbons (PAHs). The halo is made of a dark matter component and a gas component, with the latter representing the ICM. 005) and frequency-dependent radiation transport is performed with the second order Monte Carlo code grmonty (ascl:1306. It includes several models for scattering and instrumental effects. Finally, it collates the retrieved information and draws conclusions; these include the accretion disk level inclination compared to the line of sight and the main disk and the first echo median. This may be of use for binning data to increase the signal to noise ratio, obtaining synthetic photometry, or resampling model spectra to match the sampling of observational data. The Julia library GRASS produces realistic stellar spectra with time-variable granulation signatures. The user can, for example, specify that only data products which are affected by a change in the input data are updated selectively, avoiding unnecessary computations. PyCCF emulates a Fortran program written by B. Peterson for use with reverberation mapping. LATTICEEASY creates lattice simulations of the evolution of interacting scalar fields in an expanding universe.

Unpopular is able to preserve sector-length astrophysical signals, allowing for the extraction of multi-sector light curves from the FFI data. MrMoose (Multi-Resolution Multi-Object/Origin Spectral Energy) fits user-defined models onto a set of multi-wavelength data using a Bayesian framework. 020) and Gadget-4 (ascl:2204. JWFront visualizes wavefronts and light cones in general relativity.