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2019 IEEE Recent Advances in Geoscience and Remote Sensing: Technologies, Standards and Applications, TENGARSS 2019

作者： Misra, Indranil Sharma, Vivek Moorthi, S. Manthira Dhar, Debajyoti Optical Data Processing Division Signal and Image Processing Group Ahmedabad 380015 India

ISBN: (纸本)9781728140728

IRS-1C/1D remote sensing datasets from Indian Space Research organization (ISRO) is of significant importance till now for change detection analysis in the field of agriculture growth, wetland mapping, urban sprawl monitoring, snow/glacier studies and ingestion of historical digital sensor data in data cube framework for doing data analytics and generation of value added information. Currently, IRS-1C/1D georeferenced data products have system level location accuracy go up to 1 Km. In addition, the location error of IRS-1C/1D datasets are increased to many kilometers especially in hilly terrain scenes. Such higher location accuracy error makes legacy IRS-1C/1D data not directly usable for any kind of space borne applications. In this paper, an efficient approach is presented to improve the geo-location accuracy of IRS-1C/1D data by incorporating inflight geometric calibration exercises. The rigorous sensor model is fed with primary image, ancillary orbit and attitude data, digital elevation model (DEM) and a reference image to produce ortho-rectified product. The major challenge is to do automatic feature matching of IRS-1C/1D data with current RS-2A reference image database to achieve sub-pixel level geometric error. As datasets are more than two decades older, the number of outliers in matched feature points are more. Also geo-location error of 1C/1D is varying a lot which makes it difficult to set the search window radius for feature matching. To handle this scenario, mode seeking based pruning mechanism is added with robust SIFT feature matching technique which is independent of search window size. Additionally, SIFT parameters are also fine-tuned to get more stable feature points. The approach developed is tested in many multi temporal IRS-1C/1D LISS-3 datasets. The geo-location error of the products generated is at sub-pixel level accuracy with respect to the reference. The IRS-1C/1D data products generated with this new updated chain can be used directly as a

关键词： Location

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Is supervised learning with adversarial features provably better than sole supervision?

arXiv

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arXiv 2019年

作者： Rout, Litu Optical Data Processing Division Signal and Image Processing Group SAC ISRO Ahmedabad380015 India

Generative Adversarial Networks (GAN) have shown promising results on a wide variety of complex tasks. Recent experiments show adversarial training provides useful gradients to the generator that helps attain better performance. In this paper, we intend to theoretically analyze whether supervised learning with adversarial features can outperform sole supervision, or not. First, we show that supervised learning without adversarial features suffer from vanishing gradient issue in near optimal region. Second, we analyze how adversarial learning augmented with supervised signal mitigates this vanishing gradient issue. Finally, we prove our main result that shows supervised learning with adversarial features can be better than sole supervision (under some mild assumptions). We support our main result on two fronts (i) expected empirical risk and (ii) rate of convergence. Copyright © 2019, The Authors. All rights reserved.

关键词： Generative adversarial networks

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Enhancing Image Resolution: A Simulation Study and Sensitivity Analysis of System Parameters for Resourcesat-3S/3SA

arXiv

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arXiv 2024年

作者： Garg, Ankur Sarkar, Meenakshi Moorthi, S.M. Dhar, Debajyoti Optical Data Processing Group Signal and Image Processing Area Space Applications Centre Ahmedabad India

Resourcesat-3S/3SA, an upcoming Indian satellite, is designed with Aft andFore payloads capturing stereo images at look angles of -5deg and 26deg,respectively. Operating at 632.6 km altitude, it features a panchromatic (PAN)band offering a Ground Sampling Distance (GSD) of 1.25 meters and a 60 kmswath. To balance swath width and resolution, an Instantaneous Geometric Fieldof View (IGFOV) of 2.5 meters is maintained while ensuring a 1.25-meter GSDboth along and across track. Along-track sampling is achieved through precisetiming, while across-track accuracy is ensured by using two staggered pixelarrays. Signal-to-Noise Ratio (SNR) is enhanced through Time Delay andIntegration (TDI), employing two five-stage subarrays spaced 80 {\\mu}m apartalong the track, with a 4 {\\mu}m (0.5 pixel) stagger in the across-trackdirection to achieve 1.25-meter resolution. To further boost resolution, thesatellite employs super-resolution (SR), combining multiple low-resolutioncaptures using sub-pixel shifts to produce high-resolution images. Thistechnique, effective when images contain aliased high-frequency details,reconstructs full-resolution imagery using phase information from multipleobservations, and has been successfully applied in remote sensing missions likeSPOT-5, SkySat, and DubaiSat-1. A Monte Carlo simulation explores the factorsinfluencing the resolution in Resourcesat-3S/3SA, with sensitivity analysishighlighting key impacts. The simulation methodology is broadly applicable toother remote sensing missions, optimizing SR for enhanced image clarity andresolution in future satellite systems. Copyright © 2024, The Authors. All rights reserved.

关键词： Sensitivity analysis

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An Automated Feature Tracking Based Algorithm for Estimation of Ice Flow and Glacier Surface Velocity Using Resourcesat-2A data for Himalayan Terrain

An Automated Feature Tracking Based Algorithm for Estimation...

引用

International Conference on Image Information processing

作者： Yatharath Bhateja Indranil Misra Debajyoti Dhar Tushar Shukla Sampa Roy Optical Data Processing Division Signal Image Processing Group Space Applications Centre (ISRO) Ahmedabad India

Determination of ice flow and glacier surface velocity plays a pivotal role in the study of glacial geography, its sensitivity to climate change and its impact on water cycle of the region. This study becomes of utmost importance in case of Himalayan Cryosphere, which is a source of water to many areas in Asia. In this paper, we propose an algorithm for optical remote sensing multispectral data which can automatically calculate the ice flow velocity and further help other glacier related studies. An ortho-rectified image pair of Resourcesat - 2A LISS-3 (Linear Imaging and Self Scanning) sensor is taken as an input, which is further subjected to a cloud mask and snow feature enhancement technique to improve the visibility of the requisite area. This in turn is used as an input to the first level Principal component analysis (PCA). Further a common raster is extracted and then moving chip based sub-pixel correlation is performed to find the ice shift. Post processing steps are used to remove spurious matches and false positives. In the analysis we observe variations in velocities during the winter and summer season, further fluctuations were also observed in velocities for different zones of glaciers. Average glacier surface velocities ranging from 30my -1 to 110my -1 are observed. This study shows that optical image based correlation is suitable and efficient for measurement of ice flow in the fast moving glaciers of the Himalayas.

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ATR evaluation: Cautionary comments

ATR evaluation: Cautionary comments

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Infrared Systems and Components II 1988

作者： Kegelmeyer, W. Philip Webster, Dave Hughes Aircraft Company Electro-Optical Data Systems Group Image and Signal Processing Laboratory P.O. Box 902 EO/E52/D240 El SegundoCA90245 United States

Ambiguity in the use of the phrase "model-based" in the discussion of automatic target recognition (ATR) algorithms is identified. Some terminology designed to allow more precise discussion of model-based concepts is proposed, with the meaning of the terms delineated by discussion and example. © 1988 SPIE. All rights reserved.

关键词： Automatic target recognition

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DeepSWIR: A deep learning based approach for the synthesis of short-wave infrared band using multi-sensor concurrent datasets

arXiv

引用

arXiv 2019年

作者： Rout, Litu Bhateja, Yatharath Garg, Ankur Mishra, Indranil Moorthi, S. Manthira Dhar, Debjyoti Optical Data Processing Division Signal and Image Processing Group Space Applications Center Indian Space Research Organisation Ahmedabad380015 India

Convolutional Neural Network (CNN) is achieving remarkable progress in various computer vision tasks. In the past few years, the remote sensing community has observed Deep Neural Network (DNN) finally taking off in several challenging fields. In this study, we propose a DNN to generate a predefined High Resolution (HR) synthetic spectral band using an ensemble of concurrent Low Resolution (LR) bands and existing HR bands. Of particular interest, the proposed network, namely DeepSWIR, synthesizes Short-Wave InfraRed (SWIR) band at 5m Ground Sampling Distance (GSD) using Green (G), Red (R) and Near InfraRed (NIR) bands at both 24m and 5m GSD, and SWIR band at 24m GSD. To our knowledge, the highest spatial resolution of commercially deliverable SWIR band is at 7.5m GSD. Also, we propose a Gaussian feathering based image stitching approach in light of processing large satellite imagery. To experimentally validate the synthesized HR SWIR band, we critically analyse the qualitative and quantitative results produced by DeepSWIR using state-of-the-art evaluation metrics. Further, we convert the synthesized DN values to Top Of Atmosphere (TOA) reflectance and compare with the corresponding band of Sentinel-2B. Finally, we show one real world application of the synthesized band by using it to map wetland resources over our region of interest. Copyright © 2019, The Authors. All rights reserved.

关键词： Deep neural networks

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On-orbit measurements of the ISS atmosphere by the vehicle cabin atmosphere monitor

On-orbit measurements of the ISS atmosphere by the vehicle c...

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41st International Conference on Environmental Systems 2011, ICES 2011

作者： Darrach, M.R. Chutjian, A. Bornstein, B.J. Croonquist, A.P. Garkanian, V. Haemmerle, V.R. Hofman, J. Heinrichs, W.M. Karmon, D. Kenny, J. Kidd, R.D. Lee, S. MacAskill, J.A. Madzunkov, S.M. Mandrake, L. Rust, T.M. Schaefer, R.T. Thomas, J.L. Toomarian, N. Jet Propulsion Laboratory California Institute of Technology Pasadena CA 91109 United States Atomic and Molecular Physics Group JPL/Caltech United States Instrument Autonomy Group JPL/Caltech United States MicroDevices Group JPL/CalTech United States Optical Communications Group JPL/Caltech United States Processing Algorithms and Calibration Engineering JPL/Caltech United States Inst System Engineering JPL/Caltech United States Instruments and Science Data Systems JPL/Caltech United States Instrument Integration and Test JPL/Caltech United States Planetary Chemistry and Astrobiology JPL/Caltech United States High Capacity Computing and Modeling JPL/Caltech United States Machine Learning and Instrument Autonomy Group JPL/Caltech United States SpaceX 1 Rocket Rd Hawthorne CA 90250 United States Advanced Computer Systems and Technology JPL/Caltech United States Advanced Instrument Concepts JPL/Caltech United States

ISBN: (纸本)9781600869488

We report on trace gas and major atmospheric constituents results obtained by the Vehicle Cabin Atmosphere Monitor (VCAM) during operations aboard the International Space Station (ISS). VCAM is an autonomous environmental monitor based on a miniature gas chromatograph/mass spectrometer. It was flown to the ISS on shuttle mission STS-131 and commenced operations on 6/10/10. VCAM provides measurements of ppb-to-ppm levels of volatile trace-gas constituents, and of the atmospheric major constituents (nitrogen, oxygen, argon, and carbon dioxide) in a space vehicle or station. It is designed to operate autonomously and maintenance-free, approximately once per day, with a self-contained gas supply sufficient for a one-year lifetime. VCAM is designed to detect and identify 90% of the target compounds at their 180-day Spacecraft Maximum Allowable Concentration levels. © 2011 by the American Institute of Aeronautics and Astronautics, Inc.

关键词： Gases

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Ground-based and additional science support for SMILE

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Earth and Planetary Physics 2024年第1期8卷 275-298页

作者： J.A.Carter M.Dunlop C.Forsyth K.Oksavik E.Donovon A.Kavanagh S.E.Milan T.Sergienko R.C.Fear D.G.Sibeck M.Connors T.Yeoman X.Tan M.G.G.T.Taylor K.McWilliams J.Gjerloev R.Barnes D.D.Billet G.Chisham A.Dimmock M.P.Freeman D.-S.Han M.D.Hartinger S.-Y.W.Hsieh Z.-J.Hu M.K.James L.Juusola K.Kauristie E.A.Kronberg M.Lester J.Manuel J.Matzka I.McCrea Y.Miyoshi J.Rae L.Ren F.Sigernes E.Spanswick K.Sterne A.Steuwer T.Sun M.-T.Walach B.Walsh C.Wang J.Weygand J.Wild J.Yan J.Zhang Q.-H.Zhang Planetary Sciences Group School of Physics and AstronomyUniversity of LeicesterUniversity RoadLeicesterLE17RHUK Rutherford Appleton Laboratory Space Science Technology Facilities CouncilOxfordshireUK School of Space and Environment Beihang UniversityBeijing 100191China Key Laboratory of Space Environment Monitoring and Information Processing Ministry of Industry and Information TechnologyBeijing 100017China Department of Space and Climate Physics UCLMullard Space Science LaboratoryHolmbury St.MaryDorkingSurreyRH56NTUK Birkeland Centre for Space Science Department of Physics and Technology.University of BergenBergenNorway Department of Physics and Astronomy University of Calgary2500 University DriveCalgaryAlbertaCanada T2N 1N4 British Antarctic Survey CambridgeUK Swedish Institute of Space Physics KirunaSweden West Highfield Campus University of SouthamptonUniversity RoadSO171BJUK Goddard Space Flight Center NASAGreenbeltMarylandUSA Athabasca University AthabascaCanada ESTEC European Space AgencyNetherlands University of Saskatchewan SaskatoonCanada The Johns Hopkins University Applied Physics Laboratory LaurelMarylandUSA Swedish Institude of Space Physics UppsalaSE 75121Sweden Tongji University Shanghai 200092China Center for Space Plasma Physics Space Science Institute4765 Walnut Street Suite BBoulderColorado80301USA Polar Research Institute of China Shanghai 200136China Finnish Meteorological Institute(FMI) Finland Department of Earth and Environmental Sciences(Geophysics) Ludwig Maximilian University of Munich(LMU)MunichTheresienstr.41MunichD-80333Germany Canadian Space Agency MontrealCanada GFZ German Research Centre for Geosciences PotsdamGermany Nagoya University Institute for Space Earth Environment ResearchCenter for Integrated Data ScienceNagoyaAichiJP 464-8601 Northumbria University Newcastle upon TyneTyne and WearUK NE18ST National Space Science Center Chinese Academy SciencesBeijing 100190China Arctic Geophysics University Centre in Svalbard

The joint European Space Agency and Chinese Academy of Sciences Solar wind Magnetosphere Ionosphere Link Explorer(SMILE)mission will explore global dynamics of the magnetosphere under varying solar wind and interplanetary magnetic field conditions,and simultaneously monitor the auroral response of the Northern Hemisphere *** these large-scale responses with medium and fine-scale measurements at a variety of cadences by additional ground-based and space-based instruments will enable a much greater scientific impact beyond the original goals of the SMILE ***,we describe current community efforts to prepare for SMILE,and the benefits and context various experiments that have explicitly expressed support for SMILE can offer.A dedicated group of international scientists representing many different experiment types and geographical locations,the Ground-based and Additional Science Working group,is facilitating these *** include constructing an online SMILE data Fusion Facility,the discussion of particular or special modes for experiments such as coherent and incoherent scatter radar,and the consideration of particular observing strategies and spacecraft *** anticipate growing interest and community engagement with the SMILE mission,and we welcome novel ideas and insights from the solar-terrestrial community.

关键词： magnetosphere ionosphere magnetosphere-ionosphere coupling ground-based experimentation SMILE conjunctions missions

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Euclid: III. The NISP Instrument

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Astronomy and Astrophysics 2025年 697卷

作者： Euclid Collaboration Jahnke, K. Gillard, W. Schirmer, M. Ealet, A. Maciaszek, T. Prieto, E. Barbier, R. Bonoli, C. Corcione, L. Dusini, S. Grupp, F. Hormuth, F. Ligori, S. Martin, L. Morgante, G. Padilla, C. Toledo-Moreo, R. Trifoglio, M. Valenziano, L. Bender, R. Castander, F.J. Garilli, B. Lilje, P.B. Rix, H.-W. Andersen, M.I. Auricchio, N. Balestra, A. Barriere, J.-C. Battaglia, P. Berthe, M. Bodendorf, C. Boenke, T. Bon, W. Bonnefoi, A. Caillat, A. Capobianco, V. Carle, M. Casas, R. Cho, H. Costille, A. Ducret, F. Ferriol, S. Franceschi, E. Gimenez, J.-L. Holmes, W. Hornstrup, A. Jhabvala, M. Kohley, R. Kubik, B. Laureijs, R. Le Mignant, D. Lloro, I. Medinaceli, E. Mellier, Y. Polenta, G. Racca, G.D. Renzi, A. Salvignol, J.-C. Secroun, A. Seidel, G. Seiffert, M. Sirignano, C. Sirri, G. Strada, P. Smadja, G. Stanco, L. Wachter, S. Anselmi, S. Borsato, E. Caillat, L. Cogato, F. Colodro-Conde, C. Crouzet, P.-E. Conforti, V. DâÂ Â alessandro, M. Copin, Y. Cuillandre, J.-C. Davies, J.E. Davini, S. Derosa, A. Diaz, J.J. Di Domizio, S. Di Ferdinando, D. Farinelli, R. Ferrari, A.G. Fornari, F. Gabarra, L. Garcia, R. Gutierrez, C.M. Giacomini, F. Lagier, P. Gianotti, F. Krause, O. Madrid, F. Laudisio, F. Macias-Perez, J. Naletto, G. Niclas, M. Marpaud, J. Mauri, N. Da Silva, R. Passalacqua, F. Paterson, K. Patrizii, L. Risso, I. Solheim, B.G.B. Scodeggio, M. Stassi, P. Steinwagner, J. Tenti, M. Testera, G. Travaglini, R. Tosi, S. Troja, A. Tubio, O. Valieri, C. Vescovi, C. Ventura, S. Aghanim, N. Altieri, B. Amara, A. Amiaux, J. Andreon, S. Appleton, P.N. Aussel, H. Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany Aix-Marseille Université CNRS/IN2P3 CPPM Marseille France Université Claude Bernard Lyon 1 CNRS/IN2P3 IP2I Lyon UMR 5822 Villeurbanne69100 France Centre National d' Etudes Spatiales - Centre spatial de Toulouse 18 avenue Edouard Belin Toulouse31401 Cedex 9 France Aix-Marseille Université CNRS CNES LAM Marseille France INAF-Osservatorio Astronomico di Padova Via dell' Osservatorio 5 Padova35122 Italy Pino Torinese10025 Italy INFN-Padova Via Marzolo 8 Padova35131 Italy Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 Garching85748 Germany Universitäts-Sternwarte München Fakultät für Physik Ludwig-Maximilians-Universität München Scheinerstrasse 1 München81679 Germany Felix Hormuth Engineering Goethestr. 17 Leimen69181 Germany INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna40129 Italy Bellaterra08193 Spain Universidad Politécnica de Cartagena Departamento de Elec-trónica y Tecnología de Computadoras Plaza del Hospital 1 Cartagena30202 Spain INFN-Bologna Via Irnerio 46 Bologna40126 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Edifici RDIT Campus UPC Castelldefels Barcelona08860 Spain INAF-IASF Milano Via Alfonso Corti 12 Milano20133 Italy Institute of Theoretical Astrophysics University of Oslo PO Box 1029 Blindern Oslo0315 Norway Copenhagen Denmark IRFU CEA Université Paris-Saclay Gif-sur-Yvette91191 Cedex France CEA-Saclay DRF/IRFU Departement d' ingenierie des systemes bat472 Gif sur Yvette91191 cedex France Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-Yvette91191 France European Space Agency/ESTEC Keplerlaan 1 AZ Noordwijk2201 Netherlands Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Technical University of Denmark Elektrovej 327 Kgs. Lyngby2800 De

The Near-Infrared Spectrometer and Photometer (NISP) on board the Euclid satellite provides multiband photometry and R âÂ ³ 450 slitless grism spectroscopy in the 950- 2020 nm wavelength range. In this reference article, we illuminate the background of NISP' s functional and calibration requirements, describe the instrument' s integral components, and provide all its key properties. We also sketch the processes needed to understand how NISP operates and is calibrated as well as its technical potentials and limitations. Links to articles providing more details and the technical background are included. The NISP' s 16 HAWAII-2RG (H2RG) detectors with a plate scale of 03.3 pixel-1 deliver a field of view of 0.57 deg2. In photometric mode, NISP reaches a limiting magnitude of ~24.5 AB mag in three photometric exposures of about 100 s in exposure time for point sources and with a S/N of five. For spectroscopy, NISP' s pointsource sensitivity is a signal-to-noise ratio = 3.5 detection of an emission line with flux 2 10-16 erg s-1 cm-2 integrated over two resolution elements of 13.4 in 3-560 s grism exposures at 1.6 μm (redshifted Hα). Our calibration includes on-ground and in-flight characterisation and monitoring of the pixel-based detector baseline, dark current, non-linearity, and sensitivity to guarantee a relative photometric accuracy better than 1.5% and a relative spectrophotometry better than 0.7%. The wavelength calibration must be accurate to 5 or better. The NISP is the state-of-the-art instrument in the near-infrared for all science beyond small areas available from HST and JWST - and it represents an enormous advance from any existing instrumentation due to its combination of field size and high throughput of telescope and instrument. During Euclid' s six-year survey covering 14 000 deg2 of extragalactic sky, NISP will be the backbone in determining distances of more than a billion galaxies. Its near-infrared data will become a rich reference imaging and spec

关键词： Exposure meters

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Euclid preparation LXIX. The impact of relativistic redshift-space distortions on two-point clustering statistics from the Euclid wide spectroscopic survey

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Astronomy and Astrophysics 2025年 697卷

作者： Elkhashab, M.Y. Bertacca, D. Porciani, C. Salvalaggio, J. Aghanim, N. Amara, A. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Bardelli, S. Bodendorf, C. Bonino, D. Branchini, E. Brescia, M. Brinchmann, J. Camera, S. Capobianco, V. Carbone, C. Cardone, V.F. Carretero, J. Casas, R. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Cimatti, A. Colodro-Conde, C. Congedo, G. Conselice, C.J. Conversi, L. Copin, Y. Courbin, F. Courtois, H.M. Da Silva, A. Degaudenzi, H. Di Giorgio, A.M. Dinis, J. Douspis, M. Dubath, F. Duncan, C.A.J. Dupac, X. Dusini, S. Farina, M. Farrens, S. Ferriol, S. Fosalba, P. Frailis, M. Franceschi, E. Galeotta, S. Gillis, B. Giocoli, C. Gómez-Alvarez, P. Grazian, A. Grupp, F. Guzzo, L. Haugan, S.V.H. Holmes, W. Hormuth, F. Hornstrup, A. Jahnke, K. Jhabvala, M. Joachimi, B. Keihänen, E. Kermiche, S. Kiessling, A. Kilbinger, M. Kitching, T. Kubik, B. Kuijken, K. Kümmel, M. Kunz, M. Kurki-Suonio, H. Ligori, S. Lilje, P.B. Lindholm, V. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinet, N. Marulli, F. Massey, R. Medinaceli, E. Mei, S. Mellier, Y. Meneghetti, M. Meylan, G. Moresco, M. Moscardini, L. Niemi, S.-M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L.A. Pozzetti, L. Raison, F. Rebolo, R. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Saglia, R. Sakr, Z. Sánchez, A.G. Sapone, D. Schirmer, M. Schneider, P. Schrabback, T. Scodeggio, M. Secroun, A. Sefusatti, E. Seidel, G. Serrano, S. Sirignano, C. Sirri, G. Stanco, L. Steinwagner, J. Surace, C. Tallada-Crespí, P. Taylor, A.N. Tereno, I. Toledo-Moreo, R. Torradeflot, F. Tutusaus, I. Valenziano, L. Vassallo, T. Verdoes Kleijn, G. Veropalumbo, A. Wang, Y. Weller, J. Zamorani, G. Zucca, E. Biviano, A. Boucaud, A. Bozzo, E. Burigana, C. Calabrese, M. Di Ferdinando, D. Escartin Vigo, J.A. Farinelli, R. Finelli, F. Gracia-Carpio, J. Mauri, N. Pezzotta, A. Pöntinen, M. Scottez, V. Tenti, M. Viel, M. Wiesmann, M. Akrami, Y. Allevato, V. Anselmi, S INFN-Padova Via Marzolo 8 Padova 35131 Italy Dipartimento di Fisica e Astronomia “G. Galilei” Università di Padova Via Marzolo 8 Padova 35131 Italy INAF-Osservatorio Astronomico di Padova Via dell’Osservatorio 5 Padova 35122 Italy Universität Bonn Argelander-Institut für Astronomie Auf dem Hügel 71 Bonn 53121 Germany Dipartimento di Fisica – Sezione di Astronomia Università di Trieste Via Tiepolo 11 Trieste 34131 Italy INAF-Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 Trieste 34143 Italy IFPU Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste 34151 Italy INFN Sezione di Trieste Via Valerio 2 TS Trieste 34127 Italy Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay 91405 France School of Mathematics and Physics University of Surrey Guild-ford Surrey GU2 7XH United Kingdom INAF-Osservatorio Astronomico di Brera Via Brera 28 Milano 20122 Italy INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna 40129 Italy SISSA International School for Advanced Studies Via Bonomea 265 TS Trieste 34136 Italy Dipartimento di Fisica e Astronomia Università di Bologna Via Gobetti 93/2 Bologna 40129 Italy INFN-Sezione di Bologna Viale Berti Pichat 6/2 Bologna 40127 Italy Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 Garching 85748 Germany INAF-Osservatorio Astrofisico di Torino Via Osservatorio 20 (TO) Pino Torinese 10025 Italy Dipartimento di Fisica Università di Genova Via Dodecaneso 33 Genova 16146 Italy INFN-Sezione di Genova Via Dodecaneso 33 Genova 16146 Italy Department of Physics “E. Pancini” University Federico II Via Cinthia 6 Napoli 80126 Italy INAF-Osservatorio Astronomico di Capodimonte Via Moiariello 16 Napoli 80131 Italy INFN section of Naples Via Cinthia 6 Napoli 80126 Italy Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto PT4150-762 Portugal Diparti

Measurements of galaxy clustering are affected by redshift-space distortions (RSDs). Peculiar velocities, gravitational lensing, and other light-cone projection effects modify the observed redshifts, fluxes, and sky positions of distant light sources. We determined which of these effects leave a detectable imprint on several two-point clustering statistics to be extracted from the Euclid wide spectroscopic survey (EWSS) on large scales. We generated 140 mock galaxy catalogues with the survey geometry and selection function of the EWSS and made use of the LIGER (LIght cones with GEneral Relativity) method to account for a variable number of relativistic RSDs to linear order in the cosmological perturbations. We estimated different two-point clustering statistics from the mocks and used the likelihood-ratio test to calculate the statistical significance with which the EWSS could reject the null hypothesis that certain relativistic projection effects can be neglected in the theoretical models. We find that the combined effects of lensing magnification and convergence imprint characteristic signatures on several clustering observables. Their signal-to-noise ratio (S/N) ranges between 2.5 and 6 (depending on the adopted summary statistic) for the highest-redshift galaxies in the EWSS. The corresponding feature due to the peculiar velocity of the Sun is measured with a S/N of order one or two. The multipoles of the power spectrum from the catalogues that include all relativistic effects reject the null hypothesis that RSDs are only generated by the variation in the peculiar velocity along the line of sight with a significance of 2.9 standard deviations. As a by-product of our study, we demonstrate that the mixing-matrix formalism to model finite-volume effects in the multipole moments of the power spectrum can be robustly applied to surveys made of several disconnected patches. Our results indicate that relativistic RSDs, in particular the contribution from weak gravitati

关键词： galaxies: statistics large-scale structure of Universe methods: numerical

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