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Find_Orb takes a set of observations of an asteroid, comet, or natural or artificial satellite given in the MPC (Minor Planet Center) format, the ADES astrometric format, and/or the NEODyS or AstDyS formats, and finds the corresponding orbit. The code is not tied to a specific segmentation and can be used, for example, to detect radio frequency interference (RFI) in radio astronomy or galaxies and stars in widefield imaging data. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. The code implements a grid of MARCS model atmospheres and uses the MOOG radiative transfer code (ascl:1202. It has been primarily developed for VERITAS and CTA analysis. Exospheric temperature equations are developed to represent the thermospheric EUV and FUV heating. 014) psrflux function, a FITS file, or a pickle. 013) in addition to other common codes, and extensive documentation and tutorials are provided for the software.
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DNest3 is a C++ implementation of Diffusive Nested Sampling (ascl:1010. SPAMMS (Spectroscopic PAtch Model for Massive Stars), designed with geometrically deformed systems in mind, combines the eclipsing binary modelling code PHOEBE 2 (ascl:1106. PyROA models quasar light curves where the variability is described using a running optimal average (ROA), and parameters are sampled using Markov Chain Monte Carlo (MCMC) techniques using emcee (ascl:1303. JexoSim does not contain all known systematics for the various instruments, but is a good starting point to investigate the effects of systematics, and has the framework to incorporate more systematics in the future. The code uses the ratio of sides as the invariant under a coordinate transformation and searches for several triangles with similar transformations by building quadrilaterals from sets of four objects in each catalog and calculating the ratio of areas of the triangles that comprise the quadrilaterals. It also provides additional capabilities, including an automated best-fit background model selection, parallel processing, the ability to samples for further analyses, and an accessible and command-line friendly interface. The Pyxel framework, written in Python, provides basic image analysis tools, an input image generator, and a parametric mode to perform parametric and sensitivity analysis. Elise jake malik and xiao each solved the same inequality in two. PFANT has been optimized for speed, offers error reporting, and command-line configuration options. Automark models photon counts collected form observation of variable-intensity astronomical sources. Venice reads a mask file (DS9 or fits type) and a catalogue of objects (ascii or fits type) to create a pixelized mask, find objects inside/outside a mask, or generate a random catalogue of objects inside/outside a mask.
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An automated leap second management routine improves upon the one available in Astropy. Elise jake malik and xiao each solved the same inequality symbols. It is written in C and designed to work with the C edition of the Naval Observatory Vector Astrometry Software (NOVAS). SPHYNX uses an integral approach for estimating gradients, a flexible family of interpolators to suppress pairing instability, and incorporates volume elements to provides better partition of the unity. It carries out MCMC analyses of X-ray spectra in the X-ray spectral fitting program XSPEC (ascl:9910. The Difference-smoothing MATLAB code measures the time delay from the light curves of images of a gravitationally lendsed quasar.
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Swyft implements Truncated Marginal Neural Radio Estimation (TMNRE), a Bayesian parameter inference technique for complex simulation data. ART reconstructs log-probability distributions using Gaussian processes. EDRSX extends the Electronography Data Reduction System (EDRS, ascl:1512. Functions are additionally provided to plot the fitted spectral model with its confidence interval, and to derive the spectral age of the synchrotron emitting particles. 002) to explore the posterior probability distribution for the remaining fitted parameters and determine their best-fit values. Currently the data from a large number of instruments, including SMM (HXRBS, GRS Gamma, GRS X1, and GRS X2), Yohkoh (HXT, HXS, GRS, and SXT, ) CGRO (BATSE SPEC and BATSE LAD), WIND (TGRS), HIREX, and NEAR (PIN). CLUSTEREASY is a parallel programming extension of the simulation program LATTICEEASY (ascl:1911. EasyFermi provides a user-friendly graphical interface for basic to intermediate analysis of Fermi-LAT data in the framework of Fermipy (ascl:1812. The modules are available as separate downloads from SourceForge through the NASA cFS website. It uses (spin-)spherical harmonic representations of the (polarized) beam response and sky to generate simulated CMB detector signal timelines.
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Uses matplotlib to visualize multidimensional samples using a scatterplot matrix. It has been designed with particular emphasis for its scalability to large datasets and surveys. MORPHEUS (Manchester Omni-geometRical Program for Hydrodynamical EUlerian Simulations) is a 3D hydrodynamical code used to simulate astrophysical fluid flows. The wavelength calibration is primarily done using xwavecal (ascl:2212.
The radiation field affects material temperature but does not affect the motion of the fluid. The wavefront animations are available in 2D and 3D; the light cones are visualized using the coordinate systems (t, x, y) or (t, z, x). The radiative transfer is conducted in curved space-time near rotating black holes described by Kerr-Schild metric. Easyaccess facilitates access to astronomical catalogs stored in SQL Databases. Crowdsource removes a rough sky (the median), find the brighter peaks and fits these sources, computes centroids, and then computes an improved PSF. Ketu, written in Python, searches K2 light curves for evidence of exoplanets; the code simultaneously fits for systematic effects caused by small (few-pixel) drifts in the telescope pointing and other spacecraft issues and the transit signals of interest. EmpiriciSN generates realistic supernova parameters given photometric observations of a potential host galaxy, based entirely on empirical correlations measured from supernova datasets.