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Journal articles on the topic 'Euclid mission'

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Published: 1 April 2023

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1

de Teodoro, P., S. Nieto, and B. Altieri. "Data Management in the Euclid Science Archive System." Proceedings of the International Astronomical Union 12, S325 (2016): 385–88. http://dx.doi.org/10.1017/s1743921316012874.

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AbstractEuclid is the ESA M2 mission and a milestone in the understanding of the geometry of the Universe. In total Euclid will produce up to 26 PB per year of observations. The Science Archive Systems (SAS) belongs to the Euclid Archive System (EAS) that sits in the core of the Euclid Science Ground Segment (SGS). The SAS is being built at the ESAC Science Data Centre (ESDC), which is responsible for the development and operations of the scientific archives for the Astronomy, Planetary and Heliophysics missions of ESA. The SAS is focused on the needs of the scientific community and is intende

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Tereno, I., C. S. Carvalho, J. Dinis, et al. "Euclid Space Mission: building the sky survey." Proceedings of the International Astronomical Union 10, S306 (2014): 379–81. http://dx.doi.org/10.1017/s174392131401093x.

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AbstractThe Euclid space mission proposes to survey 15000 square degrees of the extragalactic sky during 6 years, with a step-and-stare technique. The scheduling of observation sequences is driven by the primary scientific objectives, spacecraft constraints, calibration requirements and physical properties of the sky. We present the current reference implementation of the Euclid survey and on-going work on survey optimization.

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Beaulieu, Jean-Philippe, David P. Bennett, Eamonn Kerins, and Matthew Penny. "Towards habitable Earths with EUCLID and WFIRST." Proceedings of the International Astronomical Union 6, S276 (2010): 349–53. http://dx.doi.org/10.1017/s1743921311020424.

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AbstractThe discovery of extrasolar planets is arguably the most exciting development in astrophysics during the past 15 years, rivalled only by the detection of dark energy. Two projects are now at the intersection of the two communities of exoplanet scientists and cosmologists: EUCLID, proposed as an ESA M-class mission; and WFIRST, the top-ranked large space mission for the next decade by the Astro 2010 Decadal Survey report. The missions are to have several important science programs: a dark energy survey using weak lensing, baryon acoustic oscillations, Type Ia supernova, a survey of exop

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Dubath, Pierre, Nikolaos Apostolakos, Andrea Bonchi, et al. "The Euclid Data Processing Challenges." Proceedings of the International Astronomical Union 12, S325 (2016): 73–82. http://dx.doi.org/10.1017/s1743921317001521.

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AbstractEuclid is a Europe-led cosmology space mission dedicated to a visible and near infrared survey of the entire extra-galactic sky. Its purpose is to deepen our knowledge of the dark content of our Universe. After an overview of the Euclid mission and science, this contribution describes how the community is getting organized to face the data analysis challenges, both in software development and in operational data processing matters. It ends with a more specific account of some of the main contributions of the Swiss Science Data Center (SDC-CH).

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Laureijs, René. "Observing the high redshift Universe with Euclid." Proceedings of the International Astronomical Union 12, S333 (2017): 238–41. http://dx.doi.org/10.1017/s1743921318000595.

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AbstractEuclid enables the exploration of large sky areas with diffraction limited resolution in the optical and near-infrared, and is sensitive enough to detect targets at cosmological distances. This combination of capabilities gives Euclid a clear advantage over telescope facilities with larger apertures, both on ground and in space. The decision to mount in the NISP instrument one extra grism for the wavelength range 0.92-1.3 μm with a spectral resolution of R ≈260 makes possible a rest-frame UV survey of the early Universe in the redshift range 6.5 < z < 9.7. Euclid’s standard imagi

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Martin, E. L. "Ultracool dwarf legacy science with ESA's Euclid mission." EPJ Web of Conferences 47 (2013): 15003. http://dx.doi.org/10.1051/epjconf/20134715003.

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Adam, R., M. Vannier, S. Maurogordato, et al. "Euclid preparation." Astronomy & Astrophysics 627 (June 26, 2019): A23. http://dx.doi.org/10.1051/0004-6361/201935088.

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Galaxy cluster counts in bins of mass and redshift have been shown to be a competitive probe to test cosmological models. This method requires an efficient blind detection of clusters from surveys with a well-known selection function and robust mass estimates, which is particularly challenging at high redshift. The Euclid wide survey will cover 15 000 deg2 of the sky, avoiding contamination by light from our Galaxy and our solar system in the optical and near-infrared bands, down to magnitude 24 in the H-band. The resulting data will make it possible to detect a large number of galaxy clusters

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Inserra, C., R. C. Nichol, D. Scovacricchi, et al. "Euclid: Superluminous supernovae in the Deep Survey." Astronomy & Astrophysics 609 (January 2018): A83. http://dx.doi.org/10.1051/0004-6361/201731758.

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Context. In the last decade, astronomers have found a new type of supernova called superluminous supernovae (SLSNe) due to their high peak luminosity and long light-curves. These hydrogen-free explosions (SLSNe-I) can be seen to z ~ 4 and therefore, offer the possibility of probing the distant Universe. Aims. We aim to investigate the possibility of detecting SLSNe-I using ESA’s Euclid satellite, scheduled for launch in 2020. In particular, we study the Euclid Deep Survey (EDS) which will provide a unique combination of area, depth and cadence over the mission. Methods. We estimated the redshi

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Scaramella, R., Y. Mellier, J. Amiaux, et al. "Euclid space mission: a cosmological challenge for the next 15 years." Proceedings of the International Astronomical Union 10, S306 (2014): 375–78. http://dx.doi.org/10.1017/s1743921314011089.

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AbstractEuclid is the next ESA mission devoted to cosmology. It aims at observing most of the extragalactic sky, studying both gravitational lensing and clustering over ~15,000 square degrees. The mission is expected to be launched in year 2020 and to last six years. The sheer amount of data of different kinds, the variety of (un)known systematic effects and the complexity of measures require efforts both in sophisticated simulations and techniques of data analysis. We review the mission main characteristics, some aspects of the the survey and highlight some of the areas of interest to this me

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Bretonnière, H., M. Huertas-Company, A. Boucaud, et al. "Euclid preparation." Astronomy & Astrophysics 657 (January 2022): A90. http://dx.doi.org/10.1051/0004-6361/202141393.

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We present a machine learning framework to simulate realistic galaxies for the Euclid Survey, producing more complex and realistic galaxies than the analytical simulations currently used in Euclid. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of 0.4 deg2 as it will be seen by the Euclid visible imager VIS, and we show that galaxy structural parameters are recovered to an accuracy similar to th

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Desprez, G., S. Paltani, J. Coupon, et al. "Euclid preparation." Astronomy & Astrophysics 644 (November 25, 2020): A31. http://dx.doi.org/10.1051/0004-6361/202039403.

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Forthcoming large photometric surveys for cosmology require precise and accurate photometric redshift (photo-z) measurements for the success of their main science objectives. However, to date, no method has been able to produce photo-zs at the required accuracy using only the broad-band photometry that those surveys will provide. An assessment of the strengths and weaknesses of current methods is a crucial step in the eventual development of an approach to meet this challenge. We report on the performance of 13 photometric redshift code single value redshift estimates and redshift probability

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Moneti, A., H. J. McCracken, M. Shuntov, et al. "Euclid preparation." Astronomy & Astrophysics 658 (February 2022): A126. http://dx.doi.org/10.1051/0004-6361/202142361.

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We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope’s Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg2 in the 3.6 and 4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and 8 μm bands. They reach at least 24

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Pöntinen, M., M. Granvik, A. A. Nucita, et al. "Euclid: Identification of asteroid streaks in simulated images using StreakDet software." Astronomy & Astrophysics 644 (November 25, 2020): A35. http://dx.doi.org/10.1051/0004-6361/202037765.

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Context. The ESA Euclid space telescope could observe up to 150 000 asteroids as a side product of its primary cosmological mission. Asteroids appear as trailed sources, that is streaks, in the images. Owing to the survey area of 15 000 square degrees and the number of sources, automated methods have to be used to find them. Euclid is equipped with a visible camera, VIS (VISual imager), and a near-infrared camera, NISP (Near-Infrared Spectrometer and Photometer), with three filters. Aims. We aim to develop a pipeline to detect fast-moving objects in Euclid images, with both high completeness a

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Carry, B. "Solar system science with ESA Euclid." Astronomy & Astrophysics 609 (January 2018): A113. http://dx.doi.org/10.1051/0004-6361/201730386.

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Context. The ESA Euclid mission has been designed to map the geometry of the dark Universe. Scheduled for launch in 2020, it will conduct a six-year visible and near-infrared imaging and spectroscopic survey over 15 000 deg2 down to VAB ~ 24.5. Although the survey will avoid ecliptic latitudes below 15°, the survey pattern in repeated sequences of four broadband filters seems well-adapted to detect and characterize solar system objects (SSOs). Aims. We aim at evaluating the capability of Euclid of discovering SSOs and of measuring their position, apparent magnitude, and spectral energy distrib

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Nesseris, S., D. Sapone, M. Martinelli та ін. "Euclid: Forecast constraints on consistency tests of the ΛCDM model". Astronomy & Astrophysics 660 (квітень 2022): A67. http://dx.doi.org/10.1051/0004-6361/202142503.

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Context. The standard cosmological model is based on the fundamental assumptions of a spatially homogeneous and isotropic universe on large scales. An observational detection of a violation of these assumptions at any redshift would immediately indicate the presence of new physics. Aims. We quantify the ability of the Euclid mission, together with contemporary surveys, to improve the current sensitivity of null tests of the canonical cosmological constant Λ and the cold dark matter (ΛCDM) model in the redshift range 0 < z < 1.8. Methods. We considered both currently available data and si

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Hook, Isobel. "Supernovæ and Transients with Euclid and the European ELT." Proceedings of the International Astronomical Union 7, S285 (2011): 63–66. http://dx.doi.org/10.1017/s1743921312000233.

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AbstractThe prospects are described for studies of large samples of supernovæ and other variable objects with two proposed future facilities: (1) the European Extremely Large Telescope, a general-purpose 40-m-class ground-based optical-IR telescope, and (2) Euclid, an M-class mission within ESA's Cosmic Vision programme, primarily for cosmology. The capabilities and status of the two facilities are briefly described. Their suitability for the study of time-varying objects in general, and of supernovæ in particular, is discussed. It is shown that Euclid has the potential for NIR imaging of a fe

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Kubik, Bogna, Remi Barbier, Eric Chabanat, et al. "A New Signal Estimator from the NIR Detectors of the Euclid Mission." Publications of the Astronomical Society of the Pacific 128, no. 968 (2016): 104504. http://dx.doi.org/10.1088/1538-3873/128/968/104504.

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Hook, I. M. "Supernovae and cosmology with future European facilities." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 371, no. 1992 (2013): 20120282. http://dx.doi.org/10.1098/rsta.2012.0282.

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Prospects for future supernova surveys are discussed, focusing on the European Space Agency’s Euclid mission and the European Extremely Large Telescope (E-ELT), both expected to be in operation around the turn of the decade. Euclid is a 1.2 m space survey telescope that will operate at visible and near-infrared wavelengths, and has the potential to find and obtain multi-band lightcurves for thousands of distant supernovae. The E-ELT is a planned, general-purpose ground-based, 40-m-class optical–infrared telescope with adaptive optics built in, which will be capable of obtaining spectra of type

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Holwerda, B. W., J. S. Bridge, R. Ryan, et al. "Substellar and low-mass dwarf identification with near-infrared imaging space observatories." Astronomy & Astrophysics 620 (December 2018): A132. http://dx.doi.org/10.1051/0004-6361/201832838.

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Aims. We aim to evaluate the near-infrared colors of brown dwarfs as observed with four major infrared imaging space observatories: the Hubble Space Telescope (HST), the James Webb Space Telescope (JWST), the Euclid mission, and the WFIRST telescope. Methods. We used the SPLAT SPEX/ISPEX spectroscopic library to map out the colors of the M-, L-, and T-type dwarfs. We have identified which color–color combination is optimal for identifying broad type and which single color is optimal to then identify the subtype (e.g., T0-9). We evaluated each observatory separately as well as the narrow-field

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Cagliari, M. S., B. R. Granett, L. Guzzo, et al. "Euclid: Constraining ensemble photometric redshift distributions with stacked spectroscopy." Astronomy & Astrophysics 660 (March 30, 2022): A9. http://dx.doi.org/10.1051/0004-6361/202142224.

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Context. The ESA Euclid mission will produce photometric galaxy samples over 15 000 square degrees of the sky that will be rich for clustering and weak lensing statistics. The accuracy of the cosmological constraints derived from these measurements will depend on the knowledge of the underlying redshift distributions based on photometric redshift calibrations. Aims. A new approach is proposed to use the stacked spectra from Euclid slitless spectroscopy to augment broad-band photometric information to constrain the redshift distribution with spectral energy distribution fitting. The high spectr

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Bisigello, L., U. Kuchner, C. J. Conselice, et al. "Euclid: the selection of quiescent and star-forming galaxies using observed colours." Monthly Notices of the Royal Astronomical Society 494, no. 2 (2020): 2337–54. http://dx.doi.org/10.1093/mnras/staa885.

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ABSTRACT The Euclid mission will observe well over a billion galaxies out to z ∼ 6 and beyond. This will offer an unrivalled opportunity to investigate several key questions for understanding galaxy formation and evolution. The first step for many of these studies will be the selection of a sample of quiescent and star-forming galaxies, as is often done in the literature by using well-known colour techniques such as the ‘UVJ’ diagram. However, given the limited number of filters available for the Euclid telescope, the recovery of such rest-frame colours will be challenging. We therefore invest

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Schmitz, M. A., J. L. Starck, F. Ngole Mboula, et al. "Euclid: Nonparametric point spread function field recovery through interpolation on a graph Laplacian." Astronomy & Astrophysics 636 (April 2020): A78. http://dx.doi.org/10.1051/0004-6361/201936094.

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Context. Future weak lensing surveys, such as the Euclid mission, will attempt to measure the shapes of billions of galaxies in order to derive cosmological information. These surveys will attain very low levels of statistical error, and systematic errors must be extremely well controlled. In particular, the point spread function (PSF) must be estimated using stars in the field, and recovered with high accuracy. Aims. The aims of this paper are twofold. Firstly, we took steps toward a nonparametric method to address the issue of recovering the PSF field, namely that of finding the correct PSF

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Jamal, S., V. Le Brun, O. Le Fèvre, et al. "Automated reliability assessment for spectroscopic redshift measurements." Astronomy & Astrophysics 611 (March 2018): A53. http://dx.doi.org/10.1051/0004-6361/201731305.

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Context. Future large-scale surveys, such as the ESA Euclid mission, will produce a large set of galaxy redshifts (≥106) that will require fully automated data-processing pipelines to analyze the data, extract crucial information and ensure that all requirements are met. A fundamental element in these pipelines is to associate to each galaxy redshift measurement a quality, or reliability, estimate.Aim. In this work, we introduce a new approach to automate the spectroscopic redshift reliability assessment based on machine learning (ML) and characteristics of the redshift probability density fun

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Penny, M. T., E. Kerins, N. Rattenbury, et al. "ExELS: an exoplanet legacy science proposal for the ESA Euclid mission – I. Cold exoplanets." Monthly Notices of the Royal Astronomical Society 434, no. 1 (2013): 2–22. http://dx.doi.org/10.1093/mnras/stt927.

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Tutusaus, I., M. Martinelli, V. F. Cardone, et al. "Euclid: The importance of galaxy clustering and weak lensing cross-correlations within the photometric Euclid survey." Astronomy & Astrophysics 643 (November 2020): A70. http://dx.doi.org/10.1051/0004-6361/202038313.

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Context. The data from the Euclid mission will enable the measurement of the angular positions and weak lensing shapes of over a billion galaxies, with their photometric redshifts obtained together with ground-based observations. This large dataset, with well-controlled systematic effects, will allow for cosmological analyses using the angular clustering of galaxies (GCph) and cosmic shear (WL). For Euclid, these two cosmological probes will not be independent because they will probe the same volume of the Universe. The cross-correlation (XC) between these probes can tighten constraints and is

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Knebe, Alexander, Daniel Lopez-Cano, Santiago Avila, et al. "UNITSIM-Galaxies: data release and clustering of emission-line galaxies." Monthly Notices of the Royal Astronomical Society 510, no. 4 (2022): 5392–407. http://dx.doi.org/10.1093/mnras/stac006.

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ABSTRACT New surveys such as European Space Agencys (ESA’s) Euclid mission are planned to map with unprecedented precision the large-scale structure of the Universe by measuring the 3D positions of tens of millions of galaxies. It is necessary to develop theoretically modelled galaxy catalogues to estimate the expected performance and to optimize the analysis strategy of these surveys. We populate two pairs of (1 h−1 Gpc)3 volume dark matter-only simulations from the UNIT project with galaxies using the Semi-Analytic Galaxy Evolution semi-analytic model of galaxy formation, coupled to the phot

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Solano, E., M. C. Gálvez-Ortiz, E. L. Martín, et al. "Ultracool dwarfs in deep extragalactic surveys using the virtual observatory: ALHAMBRA and COSMOS." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 281–90. http://dx.doi.org/10.1093/mnras/staa3423.

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ABSTRACT Ultracool dwarfs (UCDs) encompass a wide variety of compact stellar-like objects with spectra classified as late-M, L, T, and Y. Most of them have been discovered using wide-field imaging surveys. The Virtual Observatory (VO) has proven to be of great utility to efficiently exploit these astronomical resources. We aim to validate a VO methodology designed to discover and characterize UCDs in deep extragalactic surveys like Advance Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) and Cosmological Evolution Survey (COSMOS). Three complimentary searches based on parall

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Burgarella, Denis, Toru Yamada, Giovanni Fazio, and Marcin Sawicki. "Galaxies in 3D across the Universe." Proceedings of the International Astronomical Union 10, S309 (2014): 17–20. http://dx.doi.org/10.1017/s1743921314009235.

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AbstractWISH is a new space science mission concept whose primary goal is to study the first galaxies in the early universe. The primary science goal of the WISH mission is to push the high-redshift frontier beyond the epoch of reionization by utilizing its unique imaging and spectrocopic capabilities and the dedicated survey strategy. WISH will be a 1.5m telescope equipped with a 1000 arcmin2 wide-field Near-IR camera to conduct unique ultra-deep and wide-area sky imaging surveys in the wavelength range 1 - 5 μm. A spectroscopic mode (Integral-Field Unit) in the same Near-IR range and with a

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Skottfelt, Jesper, David J. Hall, Jason P. D. Gow, Neil J. Murray, Andrew D. Holland, and Thibaut Prod’homme. "Comparing simulations and test data of a radiation damaged charge-coupled device for the Euclid mission." Journal of Astronomical Telescopes, Instruments, and Systems 3, no. 2 (2017): 028001. http://dx.doi.org/10.1117/1.jatis.3.2.028001.

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McDonald, I., E. Kerins, M. Penny, et al. "ExELS: an exoplanet legacy science proposal for the ESA Euclid mission - II. Hot exoplanets and sub-stellar systems." Monthly Notices of the Royal Astronomical Society 445, no. 4 (2014): 4137–54. http://dx.doi.org/10.1093/mnras/stu2036.

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Martín, E. L., J. Y. Zhang, P. Esparza, et al. "Ammonia-methane ratios from H-band near-infrared spectra of late-T and Y dwarfs." Astronomy & Astrophysics 655 (November 2021): L3. http://dx.doi.org/10.1051/0004-6361/202142470.

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Aims. Our goals are to investigate the relative absorption strengths of ammonia and methane using low-resolution H-band (1.5−1.7 microns) spectra obtained in the laboratory and compared with observational spectra of late-T and Y dwarfs, and to estimate what can be expected from the wide-angle low-resolution near-infrared spectroscopic survey that will be provided by the upcoming Euclid space mission. Methods. Gas cells containing ammonia and methane at atmospheric pressure were custom-made in our chemical laboratory. Low-resolution near-infrared spectroscopy of these gas cells was collected in

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Jiménez Muñoz, A., J. F. Macías-Pérez, W. Cui, M. De Petris, A. Ferragamo, and G. Yepes. "The Three Hundred project: Contrasting clusters galaxy density in hydrodynamical and dark matter only simulations." EPJ Web of Conferences 257 (2022): 00022. http://dx.doi.org/10.1051/epjconf/202225700022.

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Cluster number count is a major cosmological probe for the next generation of cosmological large scale-structure surveys like the one expected from the Euclid satellite mission. Cosmological constraints will be mainly limited by the understanding of the selection function (SF), which characterize the probability of detecting a cluster of a given mass and redshift. The SF can be estimated by injecting realistic simulated clusters into the survey and re-applying the detection procedure. For this purpose we intend to use The Three Hundreds project, a 324 cluster sample simulated with full-physics

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MELCHIORRI, ALESSANDRO, FRANCESCO DE BERNARDIS, and ELOISA MENEGONI. "NEW LIMITS ON THE NEUTRINO MASS FROM COSMOLOGY." International Journal of Modern Physics: Conference Series 12 (January 2012): 368–79. http://dx.doi.org/10.1142/s2010194512006575.

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We place a nre upper limit on the sum of neutrino masses by using measurements of luminosity-dependent galaxy bias at several different redshifts, SDSS at z = 0.05, DEEP2 at z = 1 and LBGs at z = 3.8, combined with WMAP five-year cosmic microwave background anisotropy data and SDSS Red Luminous Galaxy survey three-dimensional clustering power spectrum. We obtain the upper limit of ∑ mν < 0.28 eV at the 95% confidence level for a ΛCDM + mν model, with a σ8 equal to σ8 = 0.759 ± 0.025 (1σ). When we allow the dark energy equation of state parameter w to vary we find w = -1.30 ± 0.19 for a gene

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Gouin, C., R. Gavazzi, S. Codis, C. Pichon, S. Peirani, and Y. Dubois. "Multipolar moments of weak lensing signal around clusters." Astronomy & Astrophysics 605 (September 2017): A27. http://dx.doi.org/10.1051/0004-6361/201730727.

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Context. Upcoming weak lensing surveys such as Euclid will provide an unprecedented opportunity to quantify the geometry and topology of the cosmic web, in particular in the vicinity of lensing clusters. Aims. Understanding the connectivity of the cosmic web with unbiased mass tracers, such as weak lensing, is of prime importance to probe the underlying cosmology, seek dynamical signatures of dark matter, and quantify environmental effects on galaxy formation. Methods. Mock catalogues of galaxy clusters are extracted from the N-body PLUS simulation. For each cluster, the aperture multipolar mo

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Dai, Ji-Ping, and Jun-Qing Xia. "Constraints on running of non-Gaussianity from large-scale structure probes." Monthly Notices of the Royal Astronomical Society: Letters 491, no. 1 (2019): L61—L65. http://dx.doi.org/10.1093/mnrasl/slz170.

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ABSTRACT In this letter, we present constraints on the scale-dependent ‘local’-type primordial non-Gaussianity, which is described by non-Gaussianity’s spectral index nNG, from the NRAO VLA Sky Survey and the quasar catalogue of the Sloan Digital Sky Survey (SDSS) Data Release 6, together with the SDSS Data Release 12 photo-z sample. Here, we use the autocorrelation analyses of these three probes and their cross-correlation analyses with the cosmic microwave background (CMB) temperature map, and obtain the tight constraint on the spectral index: $n_{\rm NG}=0.2 ^{+0.7}_{-1.0}$ ($1\sigma$ C.L.)

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Guglielmo, V., R. Saglia, F. J. Castander, et al. "Euclid preparation." Astronomy & Astrophysics 642 (October 2020): A192. http://dx.doi.org/10.1051/0004-6361/202038334.

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The Complete Calibration of the Colour–Redshift Relation survey (C3R2) is a spectroscopic effort involving ESO and Keck facilities designed specifically to empirically calibrate the galaxy colour–redshift relation – P(z|C) to the Euclid depth (iAB = 24.5) and is intimately linked to the success of upcoming Stage IV dark energy missions based on weak lensing cosmology. The aim is to build a spectroscopic calibration sample that is as representative as possible of the galaxies of the Euclid weak lensing sample. In order to minimise the number of spectroscopic observations necessary to fill the g

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Kannawadi, Arun, Erik Rosenberg, and Henk Hoekstra. "Mitigating the effects of undersampling in weak lensing shear estimation with metacalibration." Monthly Notices of the Royal Astronomical Society 502, no. 3 (2021): 4048–63. http://dx.doi.org/10.1093/mnras/stab211.

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ABSTRACT metacalibration is a state-of-the-art technique for measuring weak gravitational lensing shear from well-sampled galaxy images. We investigate the accuracy of shear measured with metacalibration from fitting elliptical Gaussians to undersampled galaxy images. In this case, metacalibration introduces aliasing effects leading to an ensemble multiplicative shear bias about 0.01 for Euclid and even larger for the Roman Space Telescope, well exceeding the missions’ requirements. We find that this aliasing bias can be mitigated by computing shapes from weighted moments with wider Gaussians

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Yanti, Yusma, and Septian Rahardiantoro. "ALTERNATIF PENGGEROMBOLAN DATA DERET WAKTU DENGAN KONDISI TERDAPAT DATA KOSONG." Indonesian Journal of Statistics and Its Applications 2, no. 1 (2018): 13–22. http://dx.doi.org/10.29244/ijsa.v2i1.55.

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Panel data describes a condition in which there are many observations with each observation observed periodically over a period of time. The observation clustering context based on this data is known as Clustering of Time Series Data. Many methods are developed based on fluctuating time series data conditions. However, missing data causes problems in this analysis. Missing data is the unavailability of data value on an observation because there is no information related to it. This study attempts to provide an alternative method of clustering observations on data with time series containing mi

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Reiman, David M., and Brett E. Göhre. "Deblending galaxy superpositions with branched generative adversarial networks." Monthly Notices of the Royal Astronomical Society 485, no. 2 (2019): 2617–27. http://dx.doi.org/10.1093/mnras/stz575.

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Abstract Near-future large galaxy surveys will encounter blended galaxy images at a fraction of up to 50 per cent in the densest regions of the Universe. Current deblending techniques may segment the foreground galaxy while leaving missing pixel intensities in the background galaxy flux. The problem is compounded by the diffuse nature of galaxies in their outer regions, making segmentation significantly more difficult than in traditional object segmentation applications. We propose a novel branched generative adversarial network to deblend overlapping galaxies, where the two branches produce i

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Borlaff, Alejandro, Ignacio Trujillo, Javier Román, et al. "The missing light of the Hubble Ultra Deep Field." Astronomy & Astrophysics 621 (January 2019): A133. http://dx.doi.org/10.1051/0004-6361/201834312.

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Context. The Hubble Ultra Deep field (HUDF) is the deepest region ever observed with the Hubble Space Telescope. With the main objective of unveiling the nature of galaxies up to z ∼ 7 − 8, the observing and reduction strategy have focused on the properties of small and unresolved objects, rather than the outskirts of the largest objects, which are usually over-subtracted. Aims. We aim to create a new set of WFC3 IR mosaics of the HUDF using novel techniques to preserve the properties of the low surface brightness regions. Methods. We created ABYSS: a pipeline that optimises the estimate and m

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Huertas-Company, M. "Galaxy morphologies in the era of big-data surveys." Proceedings of the International Astronomical Union 11, S319 (2015): 118–25. http://dx.doi.org/10.1017/s1743921315010911.

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AbstractGalaxy morphology is a first-order descriptor of a galaxy and a useful proxy to identify physical processes. The 100 years old Hubble fork describes the structural diversity of galaxies in the local universe. Unveiling the origins of this galaxy zoology is a key challenge in galaxy evolution. In this review talk, I first summarized some key advances in our understanding of the morphological evolution of galaxies from z ~ 0 to z ~ 3, thank you in particular to the SDSS and HST legacies. In the second part, I focused on the classification techniques. With the emergence in the last years

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Baronchelli, I., C. M. Scarlata, L. Rodríguez-Muñoz, et al. "Identification of Single Spectral Lines in Large Spectroscopic Surveys Using UMLAUT: an Unsupervised Machine-learning Algorithm Based on Unbiased Topology." Astrophysical Journal Supplement Series 257, no. 2 (2021): 67. http://dx.doi.org/10.3847/1538-4365/ac250c.

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Abstract The identification of an emission line is unambiguous when multiple spectral features are clearly visible in the same spectrum. However, in many cases, only one line is detected, making it difficult to correctly determine the redshift. We developed a freely available unsupervised machine-learning algorithm based on unbiased topology (UMLAUT) that can be used in a very wide variety of contexts, including the identification of single emission lines. To this purpose, the algorithm combines different sources of information, such as the apparent magnitude, size and color of the emitting so

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Habouzit, Mélanie, Marta Volonteri, Rachel S. Somerville, et al. "The diverse galaxy counts in the environment of high-redshift massive black holes in Horizon-AGN." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 1206–29. http://dx.doi.org/10.1093/mnras/stz2105.

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ABSTRACT High-redshift quasars are believed to reside in highly biased regions of the Universe, where black hole growth is sustained by an enhanced number of mergers and by being at the intersection of filaments bringing fresh gas. This assumption should be supported by an enhancement of the number counts of galaxies in the field of view of quasars. While the current observations of quasar environments do not lead to a consensus on a possible excess of galaxies, the future missions JWST, WFIRST, and Euclid will provide new insights on quasar environments, and will substantially increase the nu

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Gonzalez, Anthony H., Tyler George, Thomas Connor, et al. "Discovery of a possible splashback feature in the intracluster light of MACS J1149.5+2223." Monthly Notices of the Royal Astronomical Society 507, no. 1 (2021): 963–70. http://dx.doi.org/10.1093/mnras/stab2117.

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ABSTRACT We present an analysis of the intracluster light (ICL) in the Frontier Field Cluster MACS J1149.5+2223 (z = 0.544), which combines new and archival Hubble WFC3/IR imaging to provide continuous radial coverage out to 2.8 Mpc from the brightest cluster galaxy (BCG). Employing careful treatment of potential systematic biases and using data at the largest radii to determine the background sky level, we reconstruct the surface brightness profile out to a radius of 2 Mpc. This radius is the largest to which the ICL has been measured for an individual cluster. Within this radius, we measure

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Santos, Daryl Joe D., Tomotsugu Goto, Seong Jin Kim, et al. "Environmental effects on AGN activity via extinction-free mid-infrared census." Monthly Notices of the Royal Astronomical Society 507, no. 2 (2021): 3070–88. http://dx.doi.org/10.1093/mnras/stab2352.

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ABSTRACT How does the environment affect active galactic nucleus (AGN) activity? We investigated this question in an extinction-free way by selecting 1120 infrared (IR) galaxies in the AKARI North Ecliptic Pole Wide field at redshift z ≤ 1.2. A unique feature of the AKARI satellite is its continuous nine-band IR filter coverage, providing us with an unprecedentedly large sample of IR spectral energy distributions (SEDs) of galaxies. By taking advantage of this, for the first time, we explored the AGN activity derived from SED modelling as a function of redshift, luminosity, and environment. We

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Kim, Seong Jin, Nagisa Oi, Tomotsugu Goto, et al. "Identification of AKARI infrared sources by the Deep HSC Optical Survey: construction of a new band-merged catalogue in the North Ecliptic Pole Wide field." Monthly Notices of the Royal Astronomical Society 500, no. 3 (2020): 4078–94. http://dx.doi.org/10.1093/mnras/staa3359.

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ABSTRACT The North Ecliptic Pole field is a natural deep-field location for many satellite observations. It has been targeted many times since it was surveyed by the AKARI space telescope with its unique wavelength coverage from the near- to mid-infrared (mid-IR). Many follow-up observations have been carried out, making this field one of the most frequently observed areas with a variety of facilities, accumulating abundant panchromatic data from the X-ray to the radio wavelength range. Recently, a deep optical survey with the Hyper Suprime-Cam (HSC) at the Subaru telescope covered the NEP-Wid

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Chandra, Debabrata, and Supratik Pal. "Investigating the constraints on primordial features with future cosmic microwave background and galaxy surveys." Journal of Cosmology and Astroparticle Physics 2022, no. 09 (2022): 024. http://dx.doi.org/10.1088/1475-7516/2022/09/024.

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Abstract In this article, we do a thorough investigation of the competency of the forthcoming Cosmic Microwave Background (CMB) and Galaxy surveys in probing the features in the primordial power spectrum. Primordial features are specific model-dependent corrections on top of the standard power-law inflationary power spectrum; the functional form being given by different inflationary scenarios. Signature of any significant departure from the feature-less power spectrum will enable us to decipher the intricacies of the inflationary Universe. Here, we delve into three major yet distinct features,

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Shen, Yue, Hsiang-Chih Hwang, Masamune Oguri, et al. "Statistics of Galactic-scale Quasar Pairs at Cosmic Noon." Astrophysical Journal 943, no. 1 (2023): 38. http://dx.doi.org/10.3847/1538-4357/aca662.

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Abstract The statistics of galactic-scale quasar pairs can elucidate our understanding of the dynamical evolution of supermassive black hole (SMBH) pairs, the duty cycles of quasar activity in mergers, or even the nature of dark matter, but they have been challenging to measure at cosmic noon, the prime epoch of massive galaxy and SMBH formation. Here we measure a double quasar fraction of ∼6.2 ± 0.5 × 10−4 integrated over ∼0.″3–3″ separations (projected physical separations of ∼3–30 kpc at z ∼ 2) in luminous (L bol > 1045.8 erg s−1) unobscured quasars at 1.5 < z < 3.5 using Gaia EDR3

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Klypin, Anatoly, and Francisco Prada. "Effects of long-wavelength fluctuations in large galaxy surveys." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 1684–96. http://dx.doi.org/10.1093/mnras/stz2194.

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ABSTRACT In order to capture as much information as possible large galaxies surveys have been increasing their volume and redshift depth. To face this challenge theory has responded by making cosmological simulations of huge computational volumes with equally increasing numbers of dark matter particles and supercomputing resources. Thus, it is taken for granted that the ideal situation is when a single computational box encompasses the whole volume of the observational survey, e.g. $\sim 50\, h^{-3}\,{\rm Gpc}^3$ for the DESI and Euclid surveys. Here we study the effects of missing long waves

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"Euclid mission given go-ahead." Physics World 25, no. 07 (2012): 9. http://dx.doi.org/10.1088/2058-7058/25/07/17.

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