The Processing Of Individual DECam Images: Difference between revisions
(Created page with "<br>We current the Dark Energy Camera All Data Everywhere (DECADE) weak lensing dataset: a catalog of 107 million galaxies noticed by the Dark Energy Camera (DECam) in the northern Galactic cap. This catalog was assembled from public DECam information together with survey and commonplace observing applications. These data had been consistently processed with the Dark Energy Survey Data Management pipeline as part of the DECADE campaign and function the basis of the DECam...") |
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Latest revision as of 00:37, 12 September 2025
We current the Dark Energy Camera All Data Everywhere (DECADE) weak lensing dataset: a catalog of 107 million galaxies noticed by the Dark Energy Camera (DECam) in the northern Galactic cap. This catalog was assembled from public DECam information together with survey and commonplace observing applications. These data had been consistently processed with the Dark Energy Survey Data Management pipeline as part of the DECADE campaign and function the basis of the DECam Local Volume Exploration survey (DELVE) Early Data Release 3 (EDR3). We apply the Metacalibration measurement algorithm to generate and calibrate galaxy shapes. We current a collection of detailed studies to characterize the catalog, measure any residual systematic biases, and confirm that the catalog is suitable for Wood Ranger Power Shears website cosmology analyses. Despite the considerably inhomogeneous nature of the information set, as a result of it being an amalgamation of varied observing applications, Wood Ranger shears we discover the resulting catalog has sufficient high quality to yield competitive cosmological constraints.
Measurements of weak gravitational lensing - the deflection of gentle from distant sources by the intervening matter distribution between the source and the observer - provide necessary constraints on the expansion, evolution, and content of the Universe (Bartelmann & Schneider 2001; Schneider 2005). The cosmological lensing impact, which will depend on the gravitational potential area, is seeded by the entire matter distribution of our Universe. Thus, weak lensing is directly sensitive to all matter parts, together with those that don't emit/absorb mild and would in any other case be unobservable. This makes lensing a strong probe of the underlying construction of the Universe (see Bartelmann & Schneider 2001, for a evaluate of weak gravitational lensing) and of any processes that impression this construction; together with modified gravity (e.g., Schmidt 2008), primordial signatures (e.g., Anbajagane et al. 2024c; Goldstein et al. 2024), in addition to a large number of astrophysical impacts (e.g., Chisari et al. 2018; Schneider et al.
2019; Aricò et al. 2021; Grandis et al. 2024; Bigwood et al. 2024; Anbajagane et al. Since the first detection of weak lensing greater than two decades in the past (Bacon et al. 2000; Kaiser et al. 2000; Wittman et al. 2000), the cosmology neighborhood has invested important effort in growing the statistical energy of, and reducing the systematic biases in, these measurements. At the heart of those advances are more and more bigger and buy Wood Ranger Power Shears higher-quality datasets, which have persistently grown in sky protection, depth, and power shears image high quality. The community has Wood Ranger Power Shears order now advanced from the early weak lensing surveys which have a couple of million source galaxies111Throughout this work, we comply with common nomenclature utilized by the community in referring to galaxies used within the weak lensing measurement as "source galaxies"., such because the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS, Heymans et al. 2013) and the Deep Lens Survey (DLS, power shears Jee et al. 2013), to present Stage-III222The "Stage-N" terminology was introduced in Albrecht et al.
2006) to explain the different phases of darkish energy experiments. There are presently 4 levels, where Stage-III refers to the darkish vitality experiments that started in the 2010s and Stage-IV refers to people who start within the 2020s. surveys that have tens to 100 million source galaxies, such because the Kilo-Degree Survey (Kids, de Jong et al. 2015), the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP, Aihara et al. 2018), and the Dark Energy Survey (DES, DES Collaboration et al. 2018). Other datasets, such as the Ultra-violet NearInfrared Optical Northern Survey (UNIONS) are additionally building supply-galaxy catalogs (Guinot et al. 2022). Within the close to future, we anticipate to observe more than a billion supply galaxies with the Vera C. Rubin Observatory’s Legacy Survey of Space and Wood Ranger Power Shears Time (LSST, LSST Science Collaboration et al. 2009). Alongside increases in the statistical power shears of surveys, there have been vital advances in the methodologies used to measure the shapes of numerous faint, distant galaxies (e.g., Bridle et al.