FITS Files Research Articles

Adaptive optics telemetry standard

Context. The amount of adaptive optics (AO) telemetry generated by visible/near-infrared ground-based observatories is ever greater, leading to a growing need for a standardised data exchange format to support performance analysis, AO research, and development activities that involve large-scale telemetry mining, processing, and curation. Aims. This paper introduces the Adaptive Optics Telemetry (AOT) data exchange format as a standard for sharing AO telemetry from visible/infrared ground-based observatories. AOT is based on the flexible image transport system (FITS) and aims to provide unambiguous and consistent data access across various systems and configurations, including natural and single- or multiple-laser guide-star AO systems. Methods. We designed AOT with a focus on two key use cases: atmospheric turbulence parameter estimation and point-spread function reconstruction. We prototyped and tested the design using existing AO telemetry datasets from multiple systems: single conjugate with natural and laser guide stars, tomographic systems with multi-channel wavefront sensors, and single- and multi-wavefront correctors in systems featuring either a Shack-Hartmann or Pyramid as the main wavefront sensor. Results. The AOT file structure has been thoroughly defined, with specified data fields, descriptions, data types, units, and expected dimensions. To support this format, we have developed a Python package that enables the data conversion, reading, writing, and exploration of AOT files; it has been made publicly available and is compatible with a general-purpose Python package manager. We have demonstrated the flexibility of the AOT format by packaging data from five different instruments, installed on different telescopes.

ВИРАЖАЛЬНИЙ ПОТЕНЦІАЛ СЛОВА В ЛІТЕРАТУРІ ФОРМАЛЬНИХ ОБМЕЖЕНЬ

Formal constraints are inherent to literature since its beginnings. Every author has to solve the problem of choosing the fi tting lexical options from the multitude of lexical and semantical variants. Focusing on a certain topic or the desire to express thoughts and emotions of a certain directivity immediately shape the necessity of con-straints for the author. Creative freedom and the perceived constraints form a dialectic pair and paradoxically contribute to the true enrichment of the literary genre. The key focus of the advocates of Oulipo are theory and practice of constraint. The received results of the creative work allow to intensify the observations of word and language as objects of boundless attention. Through lingual experiments and ver-bal discoveries, it has been possible to approach the understanding of the world and the person in it oftentimes in the form of play.The work on language and its potential inventory continues since the founding of Oulipo and till today. The authors strive to research spoken word and written word graphics resources. Through combining seemingly incompatible things (poetry and mathematics, the funny and the serious, strenuous work and lighthearted play), the collision of diff erent contexts and senses occurs. Totally new senses that manifest the limitlessness of literary art are born and burst.The interest in formal structures and verbal experiments is most often seen on the col-lision point of diff erent literary phenomena or epochs. The following conditions are crucial for the functioning of constrained writing: 1) the presence of the original (preferably but not necessarily precedent) text; 2) architectonic and semantic transformation of the initial text; 3) experimental and creative nature of contemporary author’s work; 4) intensifi cation of intellectual communicative game; 5) cultivation of appendant and additional complexities.

Analyzing Earth's Position based on the Anisotropic Characteristics of Cosmic Microwave Background Radiation

This paper elaborates on the results of an exhaustive study regarding the Earth's position in the universe based on the Cosmic Microwave Background (CMB) radiation map, which is the latest discovery in modern astronomy. CMB radiation provides crucial insights into the early distribution of mass and energy in the universe. The aim of this research is to understand the theory and mechanisms behind the formation of polarity structures in the CMB and analyze their correlation with Earth's position in the overall structure of the universe. Intensity measurement data of CMB radiation published by COBE, WMAP, and Planck present temperature distribution data in coordinates in FITS (Flexible Image Transport System) format files. Subsequently, a spherical harmonic transformation is performed to obtain spherical harmonic coefficients a_lm as equations that represent dipole, quadrupole, octupole models, and various other multipole models. The analysis of the correlation in the temperature distribution of CMB radiation involves detailing various patterns found in the dipole, quadrupole, and octopole models, demonstrating quasi-symmetry characteristics with Earth at its center. An analysis of anisotropic CMB data yields an interesting hypothesis that the Earth's position plays a role in shaping the structure of the universe on a certain scale. Even more extremely, it can be said that Earth is at the center of the universe. This finding prompts profound contemplation about Earth's position in the structure of the cosmos, opening the door for further research in this field.

The correction of a hyperopic astigmatism with full-toric orthokeratology lenses. Clinical case

Orthokeratology has gained widespread clinical application in the last decade due to accumulated scientifi c data confi rming its effectiveness in inhibiting progressive myopia in children and adolescents. In cases of correction of other refractive errors, such as hypermetropia, mixed astigmatism, specialists inform patients about the possibilities of orthokeratology lenses (OKL) not often. This clinical case demonstrates the possibilities of customized, full-toric OKL to correct complex hyperopic astigmatism in an 11-year-old child. The patient was observed for several years with complex hyperopic astigmatism in ophthalmological clinics and followed the recommendations of specialists to use eyeglass correction. At the stage of transition from preschool to primary school, the child became shy of glasses and refused to wear them. In search of an alternative method of correction, parents sought advice in the special contact lens practice. The patient underwent a complete ophthalmological examination, including corneal topography. Taking into account the features of refraction and the shape of the cornea, the wishes of the child and parents, we have chosen customized orthokeratology lenses (OKL) with a fully toric design (full-toric) as method of correction. The OKL parameters were calculated by using the RGP Designer program. The lenses were made by OKVision Laboratory (Moscow). The fi tting of customized OKL allowed us to solve several tasks at once: the correction of complex hyperopic astigmatism and the freedom from using correction tools in the daytime. Despite the fact that orthokeratology is not the fi rst-line choice for optical correction of hyperopia, in some cases the method may become the only alternative to glasses and soft contact lenses

Venkovská usedlost čp. 5 v Kohoutovicích: poznatky z průzkumu patrového roubeného domu na Českodubsku

The article summarizes the documentation of house No. 5 in Kohoutovice, which was managed to be documented as part of a survey of the oldest representatives of vernacular architecture in Český Dub area and Jizera river area. This is a historic homestead in an extremely authentic structural form, important for understanding the development of a multi-storey country house. The documentation of house No. 5 was motivated by an effort to supplement and update older surveys, ranking the object among the representatives of the oldest surviving layer of a timber house in the region. The dendrochronological analysis placed the age of this house up to the fi rst third of the 19th century, and this conclusion can thus serve to complete the timeline of the development of the one-story timber house in the region. House No. 5, despite the overall maintenance, shows partial failures of the wooden structures, which may require more extensive replacements in the future. The house is protected as a cultural monument, so even its repairs should be carried out in accordance with monument principles. Apart from the partial modernization of the living area, the homestead has been preserved in an extremely authentic state with a number of valuable elements - for example, a set of historic door panels including fi ttings. It is a valuable representative of the wealthy farmstead in the researched area.

Astronomical Data and its Visualization

Abstract: The Crab Nebula has been the subject of several studies because to its significance in understanding star formation, supernova remnants, and high-energy astrophysics. In this paper, we present a complete study of astronomical fitting file photos of the Crab Nebula using SAO DS9, a powerful and scalable software tool. Images, spectroscopy, luminosity values, catalogue data, and color mapping techniques are all employed in our investigation. The primary purpose of this research was to employ astrometric and spectroscopic techniques to analyze the intricate details and features of the Crab Nebula. We used SAO DS9 to analyze fits file pictures to reveal the nebula's morphological characteristics, intricate structures, and fine-scale features. I enhanced the nebula's visualization by employing numerous color maps, allowing us to acquire a better understanding of its emission properties and dynamic behavior. As part of our analysis, I also collected spectroscopic data from the fits files. These spectroscopic discoveries shed information on the nebula's physical properties and dynamics, as well as its origins and development. I retrieved and incorporated data from many scientific catalogues to widen the scope of our inquiry

Automatic detection of sunspots on solar continuum HMI images blending local–global threshold

A huge collection of solar images to visualize sunspot are acquired by various solar observatories spread across the globe. This necessitates efficient tools for detecting and analyzing the sunspots encompassing diverse solar features. One such contribution is delivered in this work by exploiting the intrinsic intensity variations of solar images associated with sunspots and their attributes. The presented mechanism initially, pre-processes the acquired solar images by correcting the intensity variations introduced while profiling from the sun center to the limb followed by smoothening using a localized window. The resultant is then differenced from the global threshold that is obtained as a result of the statistical analysis computed over the probability distribution function of the input image. This arrangement offers higher discerning variations concerned with the local contextual structures related to sunspot, umbra, and penumbra. Also, it captures the major gradient variation between these regions that adds to the pixel heterogeneity surrounding them to finally render an automatic sunspot detection mechanism distinguishing the diverse solar regions. Receiver Operating Characteristics (ROC) investigation on annual solar images in Flexible Image Transport System (FITS) format reveals the presented method’s efficacy. Also, Pearson correlation analysis of the evaluated sunspot numbers from the detected sunspots with the solar catalog reveals the scheme’s detection closeness. Moreover, the model’s simplicity analyzed along the time and space dimensions affirms its extension to real-time analysis

New tool in python for spectroscopic data analysis: Application to variable stars data from the Oukaimden and OHP observatories

Recently we have carried out a campaign of measurements of variable star spectra at the Oukaimeden observatory since 2013. To analyze thousands of spectra, we developed a graphical interface using Python.The spectroscopic study of variable stars is based on the acquisition of data in the observatory, and their storage in Fits files. We treat this data digitally to make them exploitable and graphically representable, for this purpose we use special software or scripts developed by astrophysicists. To facilitate analysis and meet our needs, we developed a graphical interface using Python and used the Tkinter module to represent our spectroscopic data graphically. This interface can plot figures of our spectra in 1D curve, and as a superposition in 1D and 2D. Thus, this interface can determine the necessary parameters in the spectroscopic study of short-period variable stars; such as the pulsation phases, the Blazhko phase, the correction for the heliocentric velocity, etc. Moreover, we can use this interface to convert the pre-treated Fits files into text files as well as to create Excel tables containing the calculated parameters. This interface is easy and fast to use and can provide high-quality figures.By exploiting the potential of this graphical interface, we were able to carry out a study of the influence of the Blazhko effect on the Van Hoof effect which occurs between the metallic lines FeIλ4920.509 Å and FeIIλ4923.921 Å in RR Lyr.

INTELLIGENT COMPUTING PARADIGM FOR SECOND-GRADE FLUID IN A ROTATING FRAME IN A FRACTAL POROUS MEDIUM

The numerical methods such as the artificial neural networks with greater probability and nonlinear configurations are more suitable for estimation and modeling of the problem parameters. The numerical methods are easy to use in applications as these methods do not require costly and time-consuming tests like the experimental study. In this study, we use the Levenberg–Marquardt-based backpropagation Process (LMP) to create a computing paradigm that makes use of the strength of artificial neural networks (ANN), known as (ANN-LMP). Here we use the ANN-LMP to obtain the solution of the second-grade fluid in a rotating frame in a porous material with the impact of a transverse magnetic field. The 1000 data set points in the interval [Formula: see text] are used for the network training to determine the effect of various physical parameters of the flow problem under consideration. The experiment is executed of six scenarios with different physical paramaters. ANN-LMP is used for evaluating the mean square errors (MSE), training (TR), validation (VL), testing (TT), performance (PF) and fitting (FT) of the data. The problem has been verified by error histograms (EH) and regression (RG) measurements, which show high consistency with observed solutions with accuracy ranging from E-5 to E-8. Characteristics of various concerned parameters on the velocity and temperature profiles are studied.

The Near Infrared Imager and Slitless Spectrograph for JWST. V. Kernel Phase Imaging and Data Analysis

Kernel phase imaging (KPI) enables the direct detection of substellar companions and circumstellar dust close to and below the classical (Rayleigh) diffraction limit. The high-Strehl full pupil images provided by the James Webb Space Telescope (JWST) are ideal for application of the KPI technique. We present a kernel phase analysis of JWST NIRISS full pupil images taken during the instrument commissioning and compare the performance to closely related NIRISS aperture masking interferometry (AMI) observations. For this purpose, we develop and make publicly available the custom Kpi3Pipeline data reduction pipeline enabling the extraction of kernel phase observables from JWST images. The extracted observables are saved into a new and versatile kernel phase FITS file data exchange format. Furthermore, we present our new and publicly available fouriever toolkit which can be used to search for companions and derive detection limits from KPI, AMI, and long-baseline interferometry observations while accounting for correlated uncertainties in the model fitting process. Among the four KPI targets that were observed during NIRISS instrument commissioning, we discover a low-contrast (∼1:5) close-in (∼1 λ/D) companion candidate around CPD-66 562 and a new high-contrast (∼1:170) detection separated by ∼1.5 λ/D from 2MASS J062802.01-663738.0. The 5σ companion detection limits around the other two targets reach ∼6.5 mag at ∼200 mas and ∼7 mag at ∼400 mas. Comparing these limits to those obtained from the NIRISS AMI commissioning observations, we find that KPI and AMI perform similar in the same amount of observing time. Due to its 5.6 times higher throughput if compared to AMI, KPI is beneficial for observing faint targets and superior to AMI at separations ≳325 mas. At very small separations (≲100 mas) and between ∼250 and 325 mas, AMI slightly outperforms KPI which suffers from increased photon noise from the core and the first Airy ring of the point-spread function.

Properties of Flare-imminent versus Flare-quiet Active Regions from the Chromosphere through the Corona. I. Introduction of the AIA Active Region Patches (AARPs)

We begin here a series of papers examining the chromospheric and coronal properties of solar active regions. This first paper describes an extensive data set of images from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory curated for large-sample analysis of this topic. Based on (and constructed to coordinate with) the “Active Region Patches” as identified by the pipeline data analysis system for the Helioseismic and Magnetic Imager on the same mission (the “HARPs”), the “AIA Active Region Patches” (AARPs), described herein, comprise an unbiased multiwavelength set of FITS files downsampled spatially only by way of HARP-centered patch extractions (full spatial sampling is retained), and downsampled in the temporal domain but still able to describe both short-lived kinematics and longer-term trends. The AARPs database enables physics-informed parameterization and analysis using nonparametric discriminant analysis in Paper II of this series, and is validated for analysis using differential emission measure techniques. The AARP data set presently covers mid-2010 through 2018 December, is ≈9 TB in size, and is available through the Solar Data Analysis Center.

Eureka!: An End-to-End Pipeline for JWST Time-Series Observations

$\texttt{Eureka!}$ is a data reduction and analysis pipeline for exoplanet time-series observations, with a particular focus on JWST data. Over the next 1-2 decades, JWST will pursue four main science themes: Early Universe, Galaxies Over Time, Star Lifecycle, and Other Worlds. Our focus is on providing the astronomy community with an open source tool for the reduction and analysis of time-series observations of exoplanets in pursuit of the fourth of these themes, Other Worlds. The goal of $\texttt{Eureka!}$ is to provide an end-to-end pipeline that starts with uncalibrated FITS files and ultimately yields precise exoplanet spectra. The pipeline has a modular structure with six stages, and each stage uses a "Eureka! Control File" (ECF) to allow for easy control of the pipeline's behavior. Stage 5 also uses a "Eureka! Parameter File" (EPF) to control the fitted parameters. We provide template ECFs for the MIRI, NIRCam, NIRISS, and NIRSpec instruments on JWST and the WFC3 instrument on the Hubble Space Telescope (HST). These templates give users a good starting point for their analyses, but $\texttt{Eureka!}$ is not intended to be used as a black box tool, and users should expect to fine-tune some settings for each observation in order to achieve optimal results. At each stage, the pipeline creates intermediate figures and outputs that allow users to compare $\texttt{Eureka!}$'s performance using different parameter settings or to compare $\texttt{Eureka!}$ with an independent pipeline. The ECF used to run each stage is also copied into the output folder from each stage to enhance reproducibility. Finally, while $\texttt{Eureka!}$ has been optimized for exoplanet observations (especially the latter stages of the code), much of the core functionality could also be repurposed for JWST time-series observations in other research domains thanks to $\texttt{Eureka!}$'s modularity.

A Novel Deep Learning-Based Relabeling Architecture for Space Objects Detection from Partially Annotated Astronomical Images

Space Surveillance and Tracking is a task that requires the development of systems that can accurately discriminate between natural and man-made objects that orbit around Earth. To manage the discrimination between these objects, it is required to analyze a large amount of partially annotated astronomical images collected using a network of on-ground and potentially space-based optical telescopes. Thus, the main objective of this article is to propose a novel architecture that improves the automatic annotation of astronomical images. To achieve this objective, we present a new method for automatic detection and classification of space objects (point-like and streaks) in a supervised manner, given real-world partially annotated images in the FITS (Flexible Image Transport System) format. Results are strongly dependent on the preprocessing techniques applied to the images. Therefore, different techniques were tested including our method for object filtering and bounding box extraction. Based on our relabeling pipeline, we can easily follow how the number of detected objects is gradually increasing after each iteration, achieving a mean average precision of 98%.

FERIA: Flat Envelope Model with Rotation and Infall under Angular Momentum Conservation

Radio observations of low-mass star formation in molecular spectral lines have rapidly progressed since the advent of the Atacama Large Millimeter/submillimeter Array (ALMA). The gas distribution and its kinematics within a few hundreds of astronomical unit scale around a Class 0–I protostar are spatially resolved, and the region where a protostellar disk is being formed is now revealed in detail. In such studies, it is essential to characterize the complex physical structure around a protostar consisting of an infalling envelope, a rotationally supported disk, and an outflow. For this purpose, we have developed a general-purpose computer code “FERIA” (Flat Envelope model with Rotation and Infall under Angular momentum conservation) to generate the image data cube based on the infalling-rotating envelope model and the Keplerian disk model, both of which are often used in observational studies. In this paper, we present the description and the user manual of FERIA and summarize caveats in actual applications. This program outputs cube FITS files, which can be used for direct comparison with observations. It can also be used to generate mock data for machine/deep learning. Examples of these applications are described and discussed to demonstrate how the model analyses work with actual observational data.

Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager

We present the complete sample of protoplanetary disks from the Gemini- Large Imaging with the Gemini Planet Imager Herbig/T Tauri Survey, which observed bright Herbig Ae/Be stars and T Tauri stars in near-infrared polarized light to search for signatures of disk evolution and ongoing planet formation. The 44 targets were chosen based on their near- and mid-infrared colors, with roughly equal numbers of transitional, pre-transitional, and full disks. Our approach explicitly did not favor well-known, “famous” disks or those observed by the Atacama Large Millimeter/submillimeter Array, resulting in a less-biased sample suitable to probe the major stages of disk evolution during planet formation. Our optimized data reduction allowed polarized flux as low as 0.002% of the stellar light to be detected, and we report polarized scattered light around 80% of our targets. We detected point-like companions for 47% of the targets, including three brown dwarfs (two confirmed, one new), and a new super-Jupiter-mass candidate around V1295 Aql. We searched for correlations between the polarized flux and system parameters, finding a few clear trends: the presence of a companion drastically reduces the polarized flux levels, far-IR excess correlates with polarized flux for nonbinary systems, and systems hosting disks with ring structures have stellar masses <3 M⊙. Our sample also included four hot, dusty “FS CMa” systems, and we detected large-scale ( >100 au) scattered light around each, signs of extreme youth for these enigmatic systems. Science-ready images are publicly available through multiple distribution channels using a new FITS file standard that has been jointly developed with members of the Very Large Telescope Spectro-polarimetric High-contrast Exoplanet Research team.

TSCat: data model and storage engine for AI-based light-curve analysis

ABSTRACT Light-curve data are one of the most important data sources in time domain astronomy research. With the advancement of observation facilities and the continuous accumulation of observation data, and considering the analysis needs of large sample data sets, software or tools based on new technologies, especially artificial intelligence (AI), will be indispensable for light-curve analysis. The light-curve analysis tool designed by an individual will follow its own defined data structure, which will make the tools designed and developed by different individuals incompatible. A unified light-curve data model will be able to solve this compatibility problem, similar to the traditional flexible image transport system (FITS) file format. This paper proposes a light-curve data model named TSCat, designs and implements a data storage engine. The TSCat data model defines the basic metadata and format required for storing optical curve data following the international virtual observatory alliance (IVOA) data format specification system. The TSCat storage engine implements basic operations such as importing, storing, and accessing light-curve data. The function and performance of the TSCat storage engine are evaluated through the actual observation data. The experimental results show that the TSCat data model is complete enough to support the analysis of light curves. TSCat will help support the standardization of the data access level of software and tools in the field of light-curve analysis, and provide a new reference for the specification system of astronomical scientific data formats.

Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy

HEALPix—the Hierarchical Equal Area isoLatitude Pixelization—has become a standard in high-energy and gravitational wave astronomy. Originally developed to improve the efficiency of all-sky Fourier analyses, it is now also utilized to share sky localization information. When used for this purpose the need for a homogeneous all-sky grid represents a limitation that hinders a broader community adoption. This work presents mhealpy, a Python library able to create, handle and analyze multiresolution maps, a solution to this problem. It supports efficient pixel querying, arithmetic operations between maps, adaptive mesh refinement, plotting, and serialization into FITS—Flexible Image Transport System—files. This HEALPix extension makes it suitable to represent highly resolved region, resulting in a convenient common format to share spatial information for joint multiwavelength and multimessenger analyses.

DBSP_DRP: A Python package for automated spectroscopic data reduction of DBSP data

DBSP_DRP is a python package that provides fully automated data reduction of data taken by the Double Spectrograph (DBSP) at the 200-inch Hale Telescope at Palomar Observatory (Oke & Gunn, 1982). The underlying data reduction functionality to extract 1D spectra, perform flux calibration and correction for atmospheric absorption, and coadd spectra together is provided by PypeIt (Prochaska et al., 2020). The new functionality that DBSP_DRP brings is in orchestrating the complex data reduction process by making smart decisions so that no user input is required after verifying the correctness of the metadata in the raw FITS files in a table-like GUI. Though the primary function of DBSP_DRP is to automatically reduce an entire night of data without user input, it has the flexibility for astronomers to fine-tune the data reduction with GUIs for manually identifying the faintest objects, as well as exposing the full set of PypeIt parameters to be tweaked for users with particular science needs. DBSP_DRP also handles some of the occasional quirks specific to DBSP, such as swapping FITS header cards, adding (an) extra null byte/s to FITS files making them not conform to the FITS specification, and not writing the coordinates of the observation to file. Additionally, DBSP_DRP contains a quicklook script for making real-time decisions during an observing run, and can open a GUI displaying a minimally reduced exposure in under 15 seconds. Docker containers are available for ease of deploying DBSP_DRP in its quicklook configuration (without some large atmospheric model files) or in its full configuration.

Spatio-temporal bands of coronal bright points and their relation to solar torsional oscillations

ABSTRACT Using automatic processing of daily fits files from SOHO_EIT, we studied the temporal evolution of the latitudinal distribution of bright coronal points from 1995 to 2020. The study revealed homogeneous and inhomogeneous components of the latitudinal distribution. The homogeneous component has cyclical variations with a significant phase shift compared to the number of sunspots. The residual inhomogeneous component manifests itself as migration of the centre of increased density from high to low latitudes. The bands of the residual density of coronal bright points (CBP) reflect solar torsional oscillations. It should be associated with the strengthening of the local alpha-omega dynamo. However, the cyclical nature of the number of CBP is explained by the diffusion of large-scale magnetic fluxes.

SSTRED: Data- and metadata-processing pipeline for CHROMIS and CRISP

Context. Data from ground-based, high-resolution solar telescopes can only be used for science with calibrations and processing, which requires detailed knowledge about the instrumentation. Space-based solar telescopes provide science-ready data, which are easier to work with for researchers whose expertise is in the interpretation of data. Recently, data-processing pipelines for ground-based instruments have been constructed. Aims. We aim to provide observers with a user-friendly data pipeline for data from the Swedish 1-meter Solar Telescope (SST) that delivers science-ready data together with the metadata needed for proper interpretation and archiving. Methods. We briefly describe the CHROMospheric Imaging Spectrometer (CHROMIS) instrument, including its (pre)filters, as well as recent upgrades to the CRisp Imaging SpectroPolarimeter (CRISP) prefilters and polarization optics. We summarize the processing steps from raw data to science-ready data cubes in FITS files. We report calibrations and compensations for data imperfections in detail. Misalignment of Ca II data due to wavelength-dependent dispersion is identified, characterized, and compensated for. We describe intensity calibrations that remove or reduce the effects of filter transmission profiles as well as solar elevation changes. We present REDUX, a new version of the MOMFBD image restoration code, with multiple enhancements and new features. It uses projective transforms for the registration of multiple detectors. We describe how image restoration is used with CRISP and CHROMIS data. The science-ready output is delivered in FITS files, with metadata compliant with the SOLARNET recommendations. Data cube coordinates are specified within the World Coordinate System (WCS). Cavity errors are specified as distortions of the WCS wavelength coordinate with an extension of existing WCS notation. We establish notation for specifying the reference system for Stokes vectors with reference to WCS coordinate directions. The CRIsp SPectral EXplorer (CRISPEX) data-cube browser has been extended to accept SSTRED output and to take advantage of the SOLARNET metadata. Results. SSTRED is a mature data-processing pipeline for imaging instruments, developed and used for the SST/CHROMIS imaging spectrometer and the SST/CRISP spectropolarimeter. SSTRED delivers well-characterized, science-ready, archival-quality FITS files with well-defined metadata. The SSTRED code, as well as REDUX and CRISPEX, is freely available through git repositories.