Solar-MACH is available as a Python package; a Streamlit-enabled tool that runs in a browser is also available (). Period04 statistically analyzes large astronomical time series containing gaps. Dsigma analyzes galaxy-galaxy lensing.
LSC (LINEAR Supervised Classification) trains a number of classifiers, including random forest and K-nearest neighbor, to classify variable stars and compares the results to determine which classifier is most successful. Elise, Jake, Malik, and Xiao each solved the same - Gauthmath. It uses the NDF data format and the ADAM libraries for parameters and messaging. The pycs package defines a collection of classes and high level functions, that you can script in a flexible way. It can handle the standard species (cdm, baryons, photons), and two neutrino mass eigenstates (1 light, 1 heavy).
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. The central component of CAMELOT is a database summarizing the properties of observational data and simulations in the literature through pertinent metadata. Elise jake malik and xiao each solved the same inequality in class. 005) and CUTE (ascl:1505. In addition, there are routines to calculate magnetic observables to compare with RV variations and determine what is driving Solar activity. SEDPY performs a variety of tasks for astronomical spectral energy distributions. The O'TRAIN package identifies transients in astronomical images based on a Convolutional Neural Network (CNN).
PPMAP provides column density mapping with extra dimensions (temperature and dust opacity index); it generate image cubes of differential column density as a function of (x, y) sky position and temperature for diffuse dusty structures. Default values for these parameters (0. It can train either a recurrent neural network or random forest to classify light-curves using only photometric information. It goes through visibilities in time order and contains standard operations like averaging, phase-shifting and flagging bad stations. MCFOST also includes a non-LTE line transfer module, and NLTE level population are obtained via iterations between Monte Carlo radiative transfer calculations and statistical equilibrium. Elise jake malik and xiao each solved the same inequality using. The code can also be incorporated into a Moment Network to enable high-dimensional likelihood-free inference. The MCMC technique is used for the cluster quantities (the first six items listed above) and numerical integration is used for the stellar quantities (the last three items in the above list). 008) is also required. 011) is a parallelized version of 2DFFT. There are also simpler versions of the most general model and utilities to generate mock clusters and mock observations. It does this without resorting to χ2 or rebinning, which can lose high-resolution information.
018) and is part of the NuGrid Python Chemical Evolution Environment (NuPyCEE, ascl:1610. Drive-casa provides a Python interface for scripting of CASA (ascl:1107. Both functions remove the field interlopers by using a 3-sigma clipping algorithm. The density is not mapped on to a grid, and therefore the calculation is performed at exactly the same resolution as the hydrodynamics. The ODEPACK solvers are written in standard Fortran and there are separate double and single precision versions. The code enables large scale analyses of sub-kilometer scale cratering rates and refinement of both scaling laws and the luminous efficiency. Elise jake malik and xiao each solved the same inequality calculator. MCCD (Multi-CCD) generates a Point Spread Function (PSF) model based on stars observations in the field of view. The code approximates the merger process (including shock heating, hydrodynamic mixing, mass ejection, and angular momentum transfer) with simple algorithms based on conservation laws and a basic qualitative understanding of the hydrodynamics. Along with core sampling functionality, PyMC includes methods for summarizing output, plotting, goodness-of-fit and convergence diagnostics. Functionality is provided to compute the induced fluctuations on the sphere directly in either real or harmonic space. Written as a standalone Fortran90 module that can be implemented in existing codes, NICIL is fully parameterizable, allowing the user to choose which processes to include and decide the values of the free parameters. It is tailored for fiber-fed multi-order spectrographs, both in optical and near-infrared (up to 2.
CALCEPH accesses binary planetary ephemeris files, including INPOPxx, JPL DExxx, and SPICE ephemeris files. For univariate time series, users can apply the Welch's power spectrum estimator or compute a nonuniform fast Fourier transform-based periodogram. Host limb darkening can be fitted either independently ("uncoupled") for each filter or combined ("coupled") using prior conditioning from the PHOENIX stellar atmosphere models. It has been used for real-time image reduction of MITSuME observational data, and can be used with data from other observatories. The mutiple fields can be generated tomographically in an arbitrary number of redshift slices and all their statistical properties (including cross-correlations) are determined by the angular power spectra supplied as input and the multivariate lognormal (or Gaussian) distribution assumed for the fields. Submission scripts for slurm and PBS job schedulers are automatically generated where necessary, catering for HPC facilities that are commonly used for processing MeerKAT data. PROPER simulates the propagation of light through an optical system using Fourier transform algorithms (Fresnel, angular spectrum methods). MonoTools detects, vets, and models transiting exoplanets, with a specific emphasis on monotransiting planets and those with unknown periods.
The code can also be run on images that are not spatially flat, assuming that there is some model of the signal on the CCD that can be used to produce a residual image. AstroPoP reduces almost any CCD photometry and image polarimetry data. The code then generates a survey by adopting a beam pattern using various survey parameters, among them telescope gain, sampling time, receiver temperature, central frequency, channel bandwidth, number of polarizations, and survey region limits. It requires CFITSIO (ascl:1010. In the most general model, the stars can be a mixture of background (contamination) and the cluster, for which the (3, 3) velocity dispersion matrix and velocity gradient (i. e., dv_x/dx and dv_y/dx) are included. PRISM stores results in HDF5-files and can be executed in serial or MPI on any number of processes. The library is written in C++, and solves a wide variety of problems. Pixmappy provides a Python interface to gbdes pixel map (astrometry) solutions. Covdisc computes the disconnected part of the covariance matrix of 2-point functions in large-scale structure studies, accounting for the survey window effect. Supplied with the latitudes, longitudes, and radii of spots and the stellar inclinations from which each star is viewed, fleck takes advantage of efficient array broadcasting with numpy to return approximate light curves. The main package is PostCactus, which provides a high-level Python interface to the various data formats in a simulation folder.
The creation of the ray-tracing simulations requires less computing time than N-body runs and the results is in good agreement with full N-body simulations. The solutions calculated are the perturbations to the velocity, v and to the magnetic field, b. The standard output of pipelines constructed with CERES is a FITS cube with the optimally extracted, wavelength calibrated and instrumental drift-corrected spectrum for each of the science images. SFQEDtoolkit implements strong-field QED (SFQED) processes in existing particle-in-cell (PIC) and Monte Carlo codes to determine the dynamics of particles and plasmas in extreme electromagnetic fields, such as those present in the vicinity of compact astrophysical objects. The code can simulate optical observations from simulation snapshots in which positions and magnitudes of objects are known. FastPM solves the gravity Possion equation with a boosted particle mesh. It is a key component of the Starlink software collection (ascl:1110. The code requires only the two-dimensional plane of galactic longitude and latitude as input.
The model is trained and tested on labeled LSBGs and artifacts from the Dark Energy Survey and demonstrates that CNNs offer a promising path in the quest to study the low-surface-brightness universe. This set of Python interfaces enables interactive exploration of rates and collection of rates (networks) in Jupyter notebooks and easy creation of the righthand side routines for reaction network integration (the ODEs) for use in simulation codes. Bulge + disc + Halo; and 3. ) KERTAP computes the strong lensing effects of Kerr black holes, including the effects on polarization. CAESAR extracts and parameterizes both compact and extended sources from astronomical radio interferometric maps. Bilby can also be used to do population studies using hierarchical Bayesian modelling. LPF (Live Pulse Finder) provides real-time automated analysis of the radio image data stream at multiple frequencies. CMacIonize simulates the self-consistent evolution of HII regions surrounding young O and B stars, or other sources of ionizing radiation. A sensitivity analysis was conducted to determine the required accuracy in terms of input parameters. DaMaSCUS-CRUST is a modified version of DaMaSCUS (ascl:1706. By known galaxies' redshifts or cosmic age, stellar masses, and star formation enhancement to galaxies' star-forming main sequence (Delta MS), the gas scaling functions predict their stellar mass ratio (gas fraction) and gas depletion time. 004) to fit multiple stars in the field simultaneously; and. It treats points of sets of data as samples from some unknown probability distribution and then statistically estimates the distance between those distributions, such as the KL divergence, the closely related Rényi divergence, L2 distance, or other similar distances.
SolTrack is derived from the Fortran library libTheSky (ascl:2209. EVEREST (EPIC Variability Extraction and Removal for Exoplanet Science Targets) removes instrumental noise from light curves with pixel level decorrelation and Gaussian processes. SOFA (Standards Of Fundamental Astronomy) is a collection of subprograms, in source-code form, that implement official IAU algorithms for fundamental astronomy computations. LRGS extends an algorithm by Kelly (2007) that used Gibbs sampling for performing linear regression in fairly general cases in two ways: generalizing the procedure for multiple response variables, and modeling the prior distribution of covariates using a Dirichlet process. Additional potential applications include other types of spectra, such as unresolved stellar clusters or supernovae spectra.
Pwv_kpno provides models for the atmospheric transmission due to precipitable water vapor (PWV) at user specified sites. 023) and supports the same cleaning and data selections options that WSClean offers in normal mode (such as cotton-schwab, multi-frequency multi-scale cleaning, and auto-masking). The computational time grows with the square of the number of objects to be correlated; technology provides multiple means to massively parallelize this problem and CUTE is specifically designed for these kind of calculations. Lastly, the platform provides a visualization tool that illustrates associations between primary bursts and repeaters, complementing basic repeater information provided by the Transient Name Server. LgrbWorldModel is written in Fortran 90 and attempts to model the population distribution of the Long-duration class of Gamma-Ray Bursts (LGRBs) as detected by the NASA's now-defunct Burst And Transient Source Experiment (BATSE) onboard the Compton Gamma Ray Observatory (CGRO). 014) offers interactive control to set up and combine multiple spectral models to fully fit the spectrum of choice. ADAM does not require boundary contour extraction for reconstruction and can be run in parallel. Kepler-K2 Cadence Events can be used to visualize and manipulate light curve files and target pixel files from the Kepler, K2, and TESS missions.
Given a timestream, with each point being the arrival times of a source, the software computes the estimated period. Observational time and filter fluxes are used as inputs; since the inputs are agnostic, additional data such as host galaxy information can also be included. Brutifus is modular, in that the order in which the post-processing routines are run is entirely customizable. 006) software, although it can be "fooled" into running on other data as well. The first two components follow an exponential density profile, and the last two a Dehnen density profile with gamma=1 by default, corresponding to a Hernquist profile. The nested sampling algorithm is then used to compute the marginal likelihood or evidence. The escape model interpolates the BaSTI luminosity evolution grid to the observed mass and luminosity of the host star.