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PyVO is a package providing access to remote data and services of the Virtual observatory (VO) using Python.
This package provides an alternative maintained fork of SEP python library with bug fixtures.
CalcMySky is a software package that simulates scattering of light by the atmosphere to render daytime and twilight skies (without stars). Its primary purpose is to enable realistic view of the sky in applications such as planetaria. Secondary objective is to make it possible to explore atmospheric effects such as glories, fogbows etc., as well as simulate unusual environments such as on Mars or an exoplanet orbiting a star with a non-solar spectrum of radiation.
This package consists of three parts:
calcmyskyutility that does the precomputation of the atmosphere model to enable rendering.libShowMySkylibrary that lets the applications render the atmosphere model.ShowMySkypreview GUI that makes it possible to preview the rendering of the atmosphere model and examine its properties.
This package provides a comprehensive framework for Massive Black Hole binary population synthesis. The framework includes modules to perform population synthesis using a variety of methodologies from semi-analytic models, to cosmological hydrodynamic simulations, and even observationally-derived galaxy merger catalogs.
This package provides an access to the JWST Science Calibration Pipeline processes data from all JWST instruments and observing modes by applying various science corrections sequentially, producing both fully-calibrated individual exposures and high-level data products (mosaics, extracted spectra, etc.).
CalcMySky is a software package that simulates scattering of light by the atmosphere to render daytime and twilight skies (without stars). Its primary purpose is to enable realistic view of the sky in applications such as planetaria. Secondary objective is to make it possible to explore atmospheric effects such as glories, fogbows etc., as well as simulate unusual environments such as on Mars or an exoplanet orbiting a star with a non-solar spectrum of radiation.
This package consists of three parts:
calcmyskyutility that does the precomputation of the atmosphere model to enable rendering.libShowMySkylibrary that lets the applications render the atmosphere model.ShowMySkypreview GUI that makes it possible to preview the rendering of the atmosphere model and examine its properties.
Baseband is a package for reading and writing VLBI and other radio baseband files, with the aim of simplifying and streamlining data conversion and standardization.
The BayesicFitting package is a python version of the the fitter classes in HCSS. HCSS was the all encompassing software system for the operations and analysis of the ESA satellite Herschel.
The CALCEPH Library is designed to access the binary planetary ephemeris files, such INPOPxx and JPL DExxx ephemeris files, (called original JPL binary or INPOP 2.0 or 3.0 binary ephemeris files in the next sections) and the SPICE kernel files (called SPICE ephemeris files in the next sections). At the moment, supported SPICE files are:
text Planetary Constants Kernel (KPL/PCK) files;
binary PCK (DAF/PCK) files;
binary SPK (DAF/SPK) files containing segments of type 1, 2, 3, 5, 8, 9, 12, 13, 17, 18, 19, 20, 21, 102, 103 and 120;
meta kernel (KPL/MK) files;
frame kernel (KPL/FK) files (only basic support).
The Python Satellite Data Analysis Toolkit (pysat) provides a simple and flexible interface for robust data analysis from beginning to end - including downloading, loading, cleaning, managing, processing, and analyzing data. Pysat's plug-in design allows analysis support for any data, including user provided data sets.
This package implements a functionality for calibration of science observations from the Nancy Grace Roman Space Telescope.
This package provides an way to compute dendrograms of observed or simulated Astronomical data in Python.
CFITSIO provides simple high-level routines for reading and writing Flexible Image Transport System files that insulate the programmer from the internal complexities of the FITS format. CFITSIO also provides many advanced features for manipulating and filtering the information in FITS files.
The FITS "World Coordinate System" (WCS) standard defines keywords and usage that provide for the description of astronomical coordinate systems in a FITS (Flexible Image Transport System) image header.
Ginga is a toolkit designed for building viewers for scientific image data in Python, visualizing 2D pixel data in numpy arrays. It can view astronomical data such as contained in files based on the FITS (Flexible Image Transport System) file format. It is written and is maintained by software engineers at the National Astronomical Observatory of Japan (NAOJ), the Space Telescope Science Institute (STScI), and other contributing entities.
The Ginga toolkit centers around an image display object which supports zooming and panning, color and intensity mapping, a choice of several automatic cut levels algorithms and canvases for plotting scalable geometric forms. In addition to this widget, a general purpose "reference" FITS viewer is provided, based on a plugin framework. A fairly complete set of standard plugins are provided for features that we expect from a modern FITS viewer: panning and zooming windows, star catalog access, cuts, star pick/FWHM, thumbnails, etc.
This package provides a Python wrapper for tempo2 - a high precision pulsar timing tool.
Tempo analyzes pulsar timing data. Pulse times of arrival (TOAs), pulsar model parameters, and coded instructions are read from one or more input files. The TOAs are fitted by a pulse timing model incorporating transformation to the solar-system barycenter, pulsar rotation and spin-down and, where necessary, one of several binary models. Program output includes parameter values and uncertainties, residual pulse arrival times, chi-squared statistics, and the covariance matrix of the model. In prediction mode,ephemerides of pulse phase behavior (in the form of polynomial expansions) are calculated from input timing models.
ASTROALIGN is a python module that will try to align two stellar astronomical images, especially when there is no WCS information available.
ImPPG performs Lucy-Richardson deconvolution, unsharp masking, brightness normalization and tone curve adjustment. It can also apply previously specified processing settings to multiple images. All operations are performed using 32-bit floating-point arithmetic.
Supported input formats: FITS, BMP, JPEG, PNG, TIFF (most of bit depths and compression methods), TGA and more. Images are processed in grayscale and can be saved as: BMP 8-bit; PNG 8-bit; TIFF 8-bit, 16-bit, 32-bit floating-point (no compression, LZW- or ZIP-compressed), FITS 8-bit, 16-bit, 32-bit floating-point.
SWarp is a program that resamples and co-adds together FITS images using any arbitrary astrometric projection defined in the WCS standard.
Stackistry implements the lucky imaging principle of astronomical imaging: creating a high-quality still image out of a series of many (possibly thousands) low quality ones (blurred, deformed, noisy). The resulting image stack typically requires post-processing, including sharpening (e.g. via deconvolution). Such post-processing is not performed by Stackistry.
This package implements functionality for simulating X-ray emission from astrophysical sources.
X-rays probe the high-energy universe, from hot galaxy clusters to compact objects such as neutron stars and black holes and many interesting sources in between. pyXSIM makes it possible to generate synthetic X-ray observations of these sources from a wide variety of models, whether from grid-based simulation codes such as FLASH, Enzo, and Athena, to particle-based codes such as Gadget and AREPO, and even from datasets that have been created 'by hand', such as from NumPy arrays. pyXSIM also provides facilities for manipulating the synthetic observations it produces in various ways, as well as ways to export the simulated X-ray events to other software packages to simulate the end products of specific X-ray observatories.
Hubble Space Telescope image combination using the drizzle algorithm to combine astronomical images, to model image distortion, to remove cosmic rays, and generally to improve the fidelity of data in the final image.
FITS/XISF image viewer with multithreaded image loading. It is intended primarily for viewing astro photos and images with support of following formats:
FITS 8, 16 bit integer and 32 bit float
XISF 8, 16 bit integer and 32 bit float
RAW CR2, DNG, NEF
JPEG, PNG, BMP, GIF, PBM, PGM, PPM and SVG images
Features:
using same stretch function as PixInsight
OpenGL accelerated drawing
index and search FITS XISF header data
quick mark images and then copy/move marked files
convert FITS <-> XISF
convert FITS/XISF -> JPEG/PNG
image statistics mean, media, min, max
support for WCS
thumbnails
convert CFA images to colour - debayer
color space aware