The family of directly detected exoplanets includes HR 8799 b, c, d, e ( Marois et al. The direct imaging technique is biased towards high-temperature gas giant planets at an early age (≲100 Myr) because contraction of their atmospheric envelope makes these objects bright at near-infrared (NIR) wavelengths (e.g., Burrows et al. 2016), directly imaged planets are key targets for atmospheric characterization (e.g., Barman et al. Although the occurrence rate of gas giant exoplanets on long-period orbits is low, as reflected by the numerous nondetections of large-scale surveys (e.g., Biller et al. High-contrast imaging is a powerful technique to study the population of planetary and substellar companions at orbital radii beyond ∼5–10 au (e.g., Oppenheimer & Hinkley 2009 Bowler 2016). National Center of Competence in Research “PlanetS” ( ). As an example, we processed archival VLT/NACO L′ and M′ data of β Pic b and reassessed the brightness and position of the planet with a Markov chain Monte Carlo analysis we also provide a derivation of the photometric error budget. The pipeline package enables end-to-end data reduction of pupil-stabilized data and supports classical dithering and coronagraphic data sets. Modules have been implemented for dedicated processing and analysis steps, including background subtraction, frame registration, PSF subtraction, photometric and astrometric measurements, and estimation of detection limits. ![]() The architecture of PynPoint has been redesigned with the core functionalities decoupled from the pipeline modules. The current version of PynPoint has evolved from an earlier version that was developed as a PSF-subtraction tool based on principal component analysis (PCA). ![]() ![]() PynPoint is written in Python 2.7 and applies various image-processing techniques, as well as statistical tools for analyzing the data, building on open-source Python packages. The package should be scalable and robust for future implementations and particularly suitable for the 3–5 μm wavelength range where typically thousands of frames have to be processed and an accurate subtraction of the thermal background emission is critical. We aim at developing a generic and modular data-reduction pipeline for processing and analysis of high-contrast imaging data obtained with pupil-stabilized observations. In addition, improvements in data reduction and point spread function (PSF)-subtraction algorithms are equally relevant for maximizing the scientific yield, both from new and archival data sets.Īims. ![]() Dedicated high-contrast imaging instruments deliver unprecedented sensitivity, enabling detailed insights into the atmospheres of young low-mass companions. The direct detection and characterization of planetary and substellar companions at small angular separations is a rapidly advancing field. Institute for Particle Physics and Astrophysics, ETH Zurich, Wolfgang-Pauli-StraZurich, SwitzerlandĮ-mail: Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The NetherlandsĬontext. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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