Experimental Astronomy最新文献

{"title":"An acoustic levitator design for suspending cosmic dust analogues and aerosol particles in light scattering experiments","authors":"A. Colin,&nbsp;O. Muñoz,&nbsp;F. J. García-Izquierdo,&nbsp;E. Frattin,&nbsp;J. Martikainen,&nbsp;Z. Gray,&nbsp;J. L. Ramos,&nbsp;J. Jiménez,&nbsp;A. Tobaruela,&nbsp;J. M. Gómez-López,&nbsp;I. Bustamante,&nbsp;J. C. Gómez,&nbsp;F. Moreno,&nbsp;A. Marzo","doi":"10.1007/s10686-025-09994-8","DOIUrl":"10.1007/s10686-025-09994-8","url":null,"abstract":"<div><p>We present a design of an acoustic levitator composed of 35 ultrasonic transducers operating at 40 <i>kHz</i> configured to form a spherical cavity. The acoustic radiation force measured experimentally in the center of the cavity is <span>({{varvec{F}}}_{rad}approx 9.6 mN)</span>, enough for levitating spheres as well as irregular particles of different materials of up to ~ 50 <i>mg</i>. Levitation tests have been performed with particles of different geometries and compositions, including liquid droplets and minerals relevant in studies of atmospheric aerosol and cosmic dust. This device has been deployed in the center of a polar nephelometer set-up to conduct studies of light scattering by irregular solid particles and liquid droplets. Test experiments have been carried out using a 1.5 <i>mm</i> diameter NBK- 7 glass sphere, for which three elements of the scattering matrix have been measured as functions of the scattering angle using a 647 <i>nm</i> diode laser. Mie theory calculations of the scattering matrix elements at this wavelength agree well with the measurements, demonstrating the functionality of the whole device.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09994-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143856494","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Research on the proton-induced radiation damage of pixelated CdZnTe detectors for space applications","authors":"Hao Chang,&nbsp;Ming Zeng,&nbsp;Di Wang,&nbsp;Hua Feng,&nbsp;Yang Tian,&nbsp;Ge Ma,&nbsp;Xiaofan Pan,&nbsp;Chen Li,&nbsp;Zhongming Wang,&nbsp;Xin Zhuo,&nbsp;Xutao Zheng,&nbsp;Yulan Li","doi":"10.1007/s10686-025-09998-4","DOIUrl":"10.1007/s10686-025-09998-4","url":null,"abstract":"<div><p>High-performance pixelated CZT detectors that achieve 3D position sensitivity are promising candidates for use in Compton imaging telescopes. We proposed to use pixelated CZT detectors in the MeV Astrophysical Spectroscopic Surveyor (MASS), which is a large area Compton telescope. Nevertheless, the presence of high-energy protons in space can lead to radiation damage in pixelated CZT detectors, causing their performance to degrade gradually. Using non-ionizing energy loss (NIEL), this study develops a method that quantitatively evaluates the radiation damage of detectors in space. To verify the method, this study irradiated two <span>(2times 2times 1text { cm}^3)</span> pixelated CZT detectors with 100 MeV protons at fluences ranging from <span>(3times 10^7text { p}^+/text {cm}^2)</span> to <span>( 3times 10^9text { p}^+/text {cm}^2)</span> under two bias sets. When the proton fluence reaches <span>(3 times 10^9 text { p}^+/text {cm}^2)</span>, the energy resolution of the detectors significantly deteriorates to <span>(3.8%)</span> at 511 keV (FWHM/E), even after post-correction. Finally, this study provides engineering considerations for their application in space.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143856493","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The PLATO mission","authors":"Heike Rauer,&nbsp;Conny Aerts,&nbsp;Juan Cabrera,&nbsp;Magali Deleuil,&nbsp;Anders Erikson,&nbsp;Laurent Gizon,&nbsp;Mariejo Goupil,&nbsp;Ana Heras,&nbsp;Thomas Walloschek,&nbsp;Jose Lorenzo-Alvarez,&nbsp;Filippo Marliani,&nbsp;César Martin-Garcia,&nbsp;J. Miguel Mas-Hesse,&nbsp;Laurence O’Rourke,&nbsp;Hugh Osborn,&nbsp;Isabella Pagano,&nbsp;Giampaolo Piotto,&nbsp;Don Pollacco,&nbsp;Roberto Ragazzoni,&nbsp;Gavin Ramsay,&nbsp;Stéphane Udry,&nbsp;Thierry Appourchaux,&nbsp;Willy Benz,&nbsp;Alexis Brandeker,&nbsp;Manuel Güdel,&nbsp;Eduardo Janot-Pacheco,&nbsp;Petr Kabath,&nbsp;Hans Kjeldsen,&nbsp;Michiel Min,&nbsp;Nuno Santos,&nbsp;Alan Smith,&nbsp;Juan-Carlos Suarez,&nbsp;Stephanie C. Werner,&nbsp;Alessio Aboudan,&nbsp;Manuel Abreu,&nbsp;Lorena Acuña,&nbsp;Moritz Adams,&nbsp;Vardan Adibekyan,&nbsp;Laura Affer,&nbsp;François Agneray,&nbsp;Craig Agnor,&nbsp;Victor Aguirre Børsen-Koch,&nbsp;Saad Ahmed,&nbsp;Suzanne Aigrain,&nbsp;Ashraf Al-Bahlawan,&nbsp;Ma de los Angeles Alcacera Gil,&nbsp;Eleonora Alei,&nbsp;Silvia Alencar,&nbsp;Richard Alexander,&nbsp;Julia Alfonso-Garzón,&nbsp;Yann Alibert,&nbsp;Carlos Allende Prieto,&nbsp;Leonardo Almeida,&nbsp;Roi Alonso Sobrino,&nbsp;Giuseppe Altavilla,&nbsp;Christian Althaus,&nbsp;Luis Alonso Alvarez Trujillo,&nbsp;Anish Amarsi,&nbsp;Matthias Ammler-von Eiff,&nbsp;Eduardo Amôres,&nbsp;Laerte Andrade,&nbsp;Alexandros Antoniadis-Karnavas,&nbsp;Carlos António,&nbsp;Beatriz Aparicio del Moral,&nbsp;Matteo Appolloni,&nbsp;Claudio Arena,&nbsp;David Armstrong,&nbsp;Jose Aroca Aliaga,&nbsp;Martin Asplund,&nbsp;Jeroen Audenaert,&nbsp;Natalia Auricchio,&nbsp;Pedro Avelino,&nbsp;Ann Baeke,&nbsp;Kevin Baillié,&nbsp;Ana Balado,&nbsp;Pau Ballber Balagueró,&nbsp;Andrea Balestra,&nbsp;Warrick Ball,&nbsp;Herve Ballans,&nbsp;Jerome Ballot,&nbsp;Caroline Barban,&nbsp;Gaële Barbary,&nbsp;Mauro Barbieri,&nbsp;Sebastià Barceló Forteza,&nbsp;Adrian Barker,&nbsp;Paul Barklem,&nbsp;Sydney Barnes,&nbsp;David Barrado Navascues,&nbsp;Oscar Barragan,&nbsp;Clément Baruteau,&nbsp;Sarbani Basu,&nbsp;Frederic Baudin,&nbsp;Philipp Baumeister,&nbsp;Daniel Bayliss,&nbsp;Michael Bazot,&nbsp;Paul G. Beck,&nbsp;Kevin Belkacem,&nbsp;Earl Bellinger,&nbsp;Serena Benatti,&nbsp;Othman Benomar,&nbsp;Diane Bérard,&nbsp;Maria Bergemann,&nbsp;Maria Bergomi,&nbsp;Pierre Bernardo,&nbsp;Katia Biazzo,&nbsp;Andrea Bignamini,&nbsp;Lionel Bigot,&nbsp;Nicolas Billot,&nbsp;Martin Binet,&nbsp;David Biondi,&nbsp;Federico Biondi,&nbsp;Aaron C. Birch,&nbsp;Bertram Bitsch,&nbsp;Paz Victoria Bluhm Ceballos,&nbsp;Attila Bódi,&nbsp;Zsófia Bognár,&nbsp;Isabelle Boisse,&nbsp;Emeline Bolmont,&nbsp;Alfio Bonanno,&nbsp;Mariangela Bonavita,&nbsp;Andrea Bonfanti,&nbsp;Xavier Bonfils,&nbsp;Rosaria Bonito,&nbsp;Aldo Stefano Bonomo,&nbsp;Anko Börner,&nbsp;Sudeshna Boro Saikia,&nbsp;Elisa Borreguero Martín,&nbsp;Francesco Borsa,&nbsp;Luca Borsato,&nbsp;Diego Bossini,&nbsp;Francois Bouchy,&nbsp;Gwenaël Boué,&nbsp;Rodrigo Boufleur,&nbsp;Patrick Boumier,&nbsp;Vincent Bourrier,&nbsp;Dominic M. Bowman,&nbsp;Enrico Bozzo,&nbsp;Louisa Bradley,&nbsp;John Bray,&nbsp;Alessandro Bressan,&nbsp;Sylvain Breton,&nbsp;Daniele Brienza,&nbsp;Ana Brito,&nbsp;Matteo Brogi,&nbsp;Beverly Brown,&nbsp;David J. A. Brown,&nbsp;Allan Sacha Brun,&nbsp;Giovanni Bruno,&nbsp;Michael Bruns,&nbsp;Lars A. Buchhave,&nbsp;Lisa Bugnet,&nbsp;Gaël Buldgen,&nbsp;Patrick Burgess,&nbsp;Andrea Busatta,&nbsp;Giorgia Busso,&nbsp;Derek Buzasi,&nbsp;José A. Caballero,&nbsp;Alexandre Cabral,&nbsp;Juan-Francisco Cabrero Gomez,&nbsp;Flavia Calderone,&nbsp;Robert Cameron,&nbsp;Andrew Cameron,&nbsp;Tiago Campante,&nbsp;Néstor Campos Gestal,&nbsp;Bruno Leonardo Canto Martins,&nbsp;Christophe Cara,&nbsp;Ludmila Carone,&nbsp;Josep Manel Carrasco,&nbsp;Luca Casagrande,&nbsp;Sarah L. Casewell,&nbsp;Santi Cassisi,&nbsp;Marco Castellani,&nbsp;Matthieu Castro,&nbsp;Claude Catala,&nbsp;Irene Catalán Fernández,&nbsp;Márcio Catelan,&nbsp;Heather Cegla,&nbsp;Chiara Cerruti,&nbsp;Virginie Cessa,&nbsp;Merieme Chadid,&nbsp;William Chaplin,&nbsp;Stephane Charpinet,&nbsp;Cristina Chiappini,&nbsp;Simone Chiarucci,&nbsp;Andrea Chiavassa,&nbsp;Simonetta Chinellato,&nbsp;Giovanni Chirulli,&nbsp;Jørgen Christensen-Dalsgaard,&nbsp;Ross Church,&nbsp;Antonio Claret,&nbsp;Cathie Clarke,&nbsp;Riccardo Claudi,&nbsp;Lionel Clermont,&nbsp;Hugo Coelho,&nbsp;Joao Coelho,&nbsp;Fabrizio Cogato,&nbsp;Josep Colomé,&nbsp;Mathieu Condamin,&nbsp;Fernando Conde García,&nbsp;Simon Conseil,&nbsp;Thierry Corbard,&nbsp;Alexandre C. M. Correia,&nbsp;Enrico Corsaro,&nbsp;Rosario Cosentino,&nbsp;Jean Costes,&nbsp;Andrea Cottinelli,&nbsp;Giovanni Covone,&nbsp;Orlagh L. Creevey,&nbsp;Aurelien Crida,&nbsp;Szilard Csizmadia,&nbsp;Margarida Cunha,&nbsp;Patrick Curry,&nbsp;Jefferson da Costa,&nbsp;Francys da Silva,&nbsp;Shweta Dalal,&nbsp;Mario Damasso,&nbsp;Cilia Damiani,&nbsp;Francesco Damiani,&nbsp;Maria Liduina das Chagas,&nbsp;Melvyn Davies,&nbsp;Guy Davies,&nbsp;Ben Davies,&nbsp;Gary Davison,&nbsp;Leandro de Almeida,&nbsp;Francesca de Angeli,&nbsp;Susana Cristina Cabral de Barros,&nbsp;Izan de CastroLeão,&nbsp;Daniel Brito de Freitas,&nbsp;Marcia Cristina de Freitas,&nbsp;Domitilla De Martino,&nbsp;José Renan de Medeiros,&nbsp;Luiz Alberto de Paula,&nbsp;Álvaro de Pedraza Gómez,&nbsp;Jelle de Plaa,&nbsp;Joris De Ridder,&nbsp;Morgan Deal,&nbsp;Leen Decin,&nbsp;Hans Deeg,&nbsp;Scilla Degl’Innocenti,&nbsp;Sebastien Deheuvels,&nbsp;Carlos del Burgo,&nbsp;Fabio Del Sordo,&nbsp;Elisa Delgado-Mena,&nbsp;Olivier Demangeon,&nbsp;Tilmann Denk,&nbsp;Aliz Derekas,&nbsp;Jean-Michel Desert,&nbsp;Silvano Desidera,&nbsp;Marc Dexet,&nbsp;Marcella Di Criscienzo,&nbsp;Anna Maria Di Giorgio,&nbsp;Maria Pia Di Mauro,&nbsp;Federico Jose Diaz Rial,&nbsp;José-Javier Díaz-García,&nbsp;Marco Dima,&nbsp;Giacomo Dinuzzi,&nbsp;Odysseas Dionatos,&nbsp;Elisa Distefano,&nbsp;Jose-Dias do Nascimento Jr.,&nbsp;Albert Domingo,&nbsp;Valentina D’Orazi,&nbsp;Caroline Dorn,&nbsp;Lauren Doyle,&nbsp;Elena Duarte,&nbsp;Florent Ducellier,&nbsp;Luc Dumaye,&nbsp;Xavier Dumusque,&nbsp;Marc-Antoine Dupret,&nbsp;Patrick Eggenberger,&nbsp;David Ehrenreich,&nbsp;Philipp Eigmüller,&nbsp;Johannes Eising,&nbsp;Marcelo Emilio,&nbsp;Kjell Eriksson,&nbsp;Marco Ermocida,&nbsp;Riano Isidoro Escate Giribaldi,&nbsp;Yoshi Eschen,&nbsp;Lucía Espinosa Yáñez,&nbsp;Inês Estrela,&nbsp;Dafydd Wyn Evans,&nbsp;Damian Fabbian,&nbsp;Michele Fabrizio,&nbsp;João Pedro Faria,&nbsp;Maria Farina,&nbsp;Jacopo Farinato,&nbsp;Dax Feliz,&nbsp;Sofia Feltzing,&nbsp;Thomas Fenouillet,&nbsp;Miguel Fernández,&nbsp;Lorenza Ferrari,&nbsp;Sylvio Ferraz-Mello,&nbsp;Fabio Fialho,&nbsp;Agnes Fienga,&nbsp;Pedro Figueira,&nbsp;Laura Fiori,&nbsp;Ettore Flaccomio,&nbsp;Mauro Focardi,&nbsp;Steve Foley,&nbsp;Jean Fontignie,&nbsp;Dominic Ford,&nbsp;Karin Fornazier,&nbsp;Thierry Forveille,&nbsp;Luca Fossati,&nbsp;Rodrigo de Marca Franca,&nbsp;Lucas Franco da Silva,&nbsp;Antonio Frasca,&nbsp;Malcolm Fridlund,&nbsp;Marco Furlan,&nbsp;Sarah-Maria Gabler,&nbsp;Marco Gaido,&nbsp;Andrew Gallagher,&nbsp;Paloma I. Gallego Sempere,&nbsp;Emanuele Galli,&nbsp;Rafael A. García,&nbsp;Antonio García Hernández,&nbsp;Antonio Garcia Munoz,&nbsp;Hugo García-Vázquez,&nbsp;Rafael Garrido Haba,&nbsp;Patrick Gaulme,&nbsp;Nicolas Gauthier,&nbsp;Charlotte Gehan,&nbsp;Matthew Gent,&nbsp;Iskra Georgieva,&nbsp;Mauro Ghigo,&nbsp;Edoardo Giana,&nbsp;Samuel Gill,&nbsp;Leo Girardi,&nbsp;Silvia Giuliatti Winter,&nbsp;Giovanni Giusi,&nbsp;João Gomes da Silva,&nbsp;Luis Jorge Gómez Zazo,&nbsp;Juan Manuel Gomez-Lopez,&nbsp;Jonay Isai González Hernández,&nbsp;Kevin Gonzalez Murillo,&nbsp;Alejandro Gonzalo Melchor,&nbsp;Nicolas Gorius,&nbsp;Pierre-Vincent Gouel,&nbsp;Duncan Goulty,&nbsp;Valentina Granata,&nbsp;John Lee Grenfell,&nbsp;Denis Grießbach,&nbsp;Emmanuel Grolleau,&nbsp;Salomé Grouffal,&nbsp;Sascha Grziwa,&nbsp;Mario Giuseppe Guarcello,&nbsp;Loïc Gueguen,&nbsp;Eike Wolf Guenther,&nbsp;Terrasa Guilhem,&nbsp;Lucas Guillerot,&nbsp;Tristan Guillot,&nbsp;Pierre Guiot,&nbsp;Pascal Guterman,&nbsp;Antonio Gutiérrez,&nbsp;Fernando Gutiérrez-Canales,&nbsp;Janis Hagelberg,&nbsp;Jonas Haldemann,&nbsp;Cassandra Hall,&nbsp;Rasmus Handberg,&nbsp;Ian Harrison,&nbsp;Diana L. Harrison,&nbsp;Johann Hasiba,&nbsp;Carole A. Haswell,&nbsp;Petra Hatalova,&nbsp;Artie Hatzes,&nbsp;Raphaelle Haywood,&nbsp;Guillaume Hébrard,&nbsp;Frank Heckes,&nbsp;Ulrike Heiter,&nbsp;Saskia Hekker,&nbsp;René Heller,&nbsp;Christiane Helling,&nbsp;Krzysztof Helminiak,&nbsp;Simon Hemsley,&nbsp;Kevin Heng,&nbsp;Konstantin Herbst ,&nbsp;Aline Hermans,&nbsp;JJ Hermes,&nbsp;Nadia Hidalgo Torres,&nbsp;Natalie Hinkel,&nbsp;David Hobbs,&nbsp;Simon Hodgkin,&nbsp;Karl Hofmann,&nbsp;Saeed Hojjatpanah,&nbsp;Günter Houdek,&nbsp;Daniel Huber,&nbsp;Joseph Huesler,&nbsp;Alain Hui-Bon-Hoa,&nbsp;Rik Huygen,&nbsp;Duc-Dat Huynh,&nbsp;Nicolas Iro,&nbsp;Jonathan Irwin,&nbsp;Mike Irwin,&nbsp;André Izidoro,&nbsp;Sophie Jacquinod,&nbsp;Nicholas Emborg Jannsen,&nbsp;Markus Janson,&nbsp;Harald Jeszenszky,&nbsp;Chen Jiang,&nbsp;Antonio José Jimenez Mancebo,&nbsp;Paula Jofre,&nbsp;Anders Johansen,&nbsp;Cole Johnston,&nbsp;Geraint Jones,&nbsp;Thomas Kallinger,&nbsp;Szilárd Kálmán,&nbsp;Thomas Kanitz,&nbsp;Marie Karjalainen,&nbsp;Raine Karjalainen,&nbsp;Christoffer Karoff,&nbsp;Steven Kawaler,&nbsp;Daisuke Kawata,&nbsp;Arnoud Keereman,&nbsp;David Keiderling,&nbsp;Tom Kennedy,&nbsp;Matthew Kenworthy,&nbsp;Franz Kerschbaum,&nbsp;Mark Kidger,&nbsp;Flavien Kiefer,&nbsp;Christian Kintziger,&nbsp;Kristina Kislyakova,&nbsp;László Kiss,&nbsp;Peter Klagyivik,&nbsp;Hubert Klahr,&nbsp;Jonas Klevas,&nbsp;Oleg Kochukhov,&nbsp;Ulrich Köhler,&nbsp;Ulrich Kolb,&nbsp;Alexander Koncz,&nbsp;Judith Korth,&nbsp;Nadiia Kostogryz,&nbsp;Gábor Kovács,&nbsp;József Kovács,&nbsp;Oleg Kozhura,&nbsp;Natalie Krivova,&nbsp;Arūnas Kuĉinskas,&nbsp;Ilyas Kuhlemann,&nbsp;Friedrich Kupka,&nbsp;Wouter Laauwen,&nbsp;Alvaro Labiano,&nbsp;Nadege Lagarde,&nbsp;Philippe Laget,&nbsp;Gunter Laky,&nbsp;Kristine Wai Fun Lam,&nbsp;Michiel Lambrechts,&nbsp;Helmut Lammer,&nbsp;Antonino Francesco Lanza,&nbsp;Alessandro Lanzafame,&nbsp;Mariel Lares Martiz,&nbsp;Jacques Laskar,&nbsp;Henrik Latter,&nbsp;Tony Lavanant,&nbsp;Alastair Lawrenson,&nbsp;Cecilia Lazzoni,&nbsp;Agnes Lebre,&nbsp;Yveline Lebreton,&nbsp;Alain Lecavelier des Etangs,&nbsp;Katherine Lee,&nbsp;Zoe Leinhardt,&nbsp;Adrien Leleu,&nbsp;Monika Lendl,&nbsp;Giuseppe Leto,&nbsp;Yves Levillain,&nbsp;Anne-Sophie Libert,&nbsp;Tim Lichtenberg,&nbsp;Roxanne Ligi,&nbsp;Francois Lignieres,&nbsp;Jorge Lillo-Box,&nbsp;Jeffrey Linsky,&nbsp;John Scige Liu,&nbsp;Dominik Loidolt,&nbsp;Yuying Longval,&nbsp;Ilídio Lopes,&nbsp;Andrea Lorenzani,&nbsp;Hans-Guenter Ludwig,&nbsp;Mikkel Lund,&nbsp;Mia Sloth Lundkvist,&nbsp;Xavier Luri,&nbsp;Carla Maceroni,&nbsp;Sean Madden,&nbsp;Nikku Madhusudhan,&nbsp;Antonio Maggio,&nbsp;Christian Magliano,&nbsp;Demetrio Magrin,&nbsp;Laurent Mahy,&nbsp;Olaf Maibaum,&nbsp;LeeRoy Malac-Allain,&nbsp;Jean-Christophe Malapert,&nbsp;Luca Malavolta,&nbsp;Jesus Maldonado,&nbsp;Elena Mamonova,&nbsp;Louis Manchon,&nbsp;Andres Manjón,&nbsp;Andrew Mann,&nbsp;Giacomo Mantovan,&nbsp;Luca Marafatto,&nbsp;Marcella Marconi,&nbsp;Rosemary Mardling,&nbsp;Paola Marigo,&nbsp;Silvia Marinoni,&nbsp;Rico Marques,&nbsp;Joao Pedro Marques,&nbsp;Paola Maria Marrese,&nbsp;Douglas Marshall,&nbsp;Silvia Martínez Perales,&nbsp;David Mary,&nbsp;Francesco Marzari,&nbsp;Eduard Masana,&nbsp;Andrina Mascher,&nbsp;Stéphane Mathis,&nbsp;Savita Mathur,&nbsp;Iris Martín Vodopivec,&nbsp;Ana Carolina Mattiuci Figueiredo,&nbsp;Pierre F. L. Maxted,&nbsp;Tsevi Mazeh,&nbsp;Stephane Mazevet,&nbsp;Francesco Mazzei,&nbsp;James McCormac,&nbsp;Paul McMillan,&nbsp;Lucas Menou,&nbsp;Thibault Merle,&nbsp;Farzana Meru,&nbsp;Dino Mesa,&nbsp;Sergio Messina,&nbsp;Szabolcs Mészáros,&nbsp;Nadége Meunier,&nbsp;Jean-Charles Meunier,&nbsp;Giuseppina Micela,&nbsp;Harald Michaelis,&nbsp;Eric Michel,&nbsp;Mathias Michielsen,&nbsp;Tatiana Michtchenko,&nbsp;Andrea Miglio,&nbsp;Yamila Miguel,&nbsp;David Milligan,&nbsp;Giovanni Mirouh,&nbsp;Morgan Mitchell,&nbsp;Nuno Moedas,&nbsp;Francesca Molendini,&nbsp;László Molnár,&nbsp;Joey Mombarg,&nbsp;Josefina Montalban,&nbsp;Marco Montalto,&nbsp;Mário J. P. F. G. Monteiro,&nbsp;Francisco Montoro Sánchez,&nbsp;Juan Carlos Morales,&nbsp;Maria Morales-Calderon,&nbsp;Alessandro Morbidelli,&nbsp;Christoph Mordasini,&nbsp;Chrystel Moreau,&nbsp;Thierry Morel,&nbsp;Giuseppe Morello,&nbsp;Julien Morin,&nbsp;Annelies Mortier,&nbsp;Benoît Mosser,&nbsp;Denis Mourard,&nbsp;Olivier Mousis,&nbsp;Claire Moutou,&nbsp;Nami Mowlavi,&nbsp;Andrés Moya,&nbsp;Prisca Muehlmann,&nbsp;Philip Muirhead,&nbsp;Matteo Munari,&nbsp;Ilaria Musella,&nbsp;Alexander James Mustill,&nbsp;Nicolas Nardetto,&nbsp;Domenico Nardiello,&nbsp;Norio Narita,&nbsp;Valerio Nascimbeni,&nbsp;Anna Nash,&nbsp;Coralie Neiner,&nbsp;Richard P. Nelson,&nbsp;Nadine Nettelmann,&nbsp;Gianalfredo Nicolini,&nbsp;Martin Nielsen,&nbsp;Sami-Matias Niemi,&nbsp;Lena Noack,&nbsp;Arlette Noels-Grotsch,&nbsp;Anthony Noll,&nbsp;Azib Norazman,&nbsp;Andrew J. Norton,&nbsp;Benard Nsamba,&nbsp;Aviv Ofir,&nbsp;Gordon Ogilvie,&nbsp;Terese Olander,&nbsp;Christian Olivetto,&nbsp;Göran Olofsson,&nbsp;Joel Ong,&nbsp;Sergio Ortolani,&nbsp;Mahmoudreza Oshagh,&nbsp;Harald Ottacher,&nbsp;Roland Ottensamer,&nbsp;Rhita-Maria Ouazzani,&nbsp;Sijme-Jan Paardekooper,&nbsp;Emanuele Pace,&nbsp;Miriam Pajas,&nbsp;Ana Palacios,&nbsp;Gaelle Palandri,&nbsp;Enric Palle,&nbsp;Carsten Paproth,&nbsp;Vanderlei Parro,&nbsp;Hannu Parviainen,&nbsp;Javier Pascual Granado,&nbsp;Vera Maria Passegger,&nbsp;Carmen Pastor-Morales,&nbsp;Martin Pätzold,&nbsp;May Gade Pedersen,&nbsp;David Pena Hidalgo,&nbsp;Francesco Pepe,&nbsp;Filipe Pereira,&nbsp;Carina M. Persson,&nbsp;Martin Pertenais,&nbsp;Gisbert Peter,&nbsp;Antoine C. Petit,&nbsp;Pascal Petit,&nbsp;Stefania Pezzuto,&nbsp;Gabriele Pichierri,&nbsp;Adriano Pietrinferni,&nbsp;Fernando Pinheiro,&nbsp;Marc Pinsonneault,&nbsp;Emese Plachy,&nbsp;Philippe Plasson,&nbsp;Bertrand Plez,&nbsp;Katja Poppenhaeger,&nbsp;Ennio Poretti,&nbsp;Elisa Portaluri,&nbsp;Jordi Portell,&nbsp;Gustavo Frederico Porto de Mello,&nbsp;Julien Poyatos,&nbsp;Francisco J. Pozuelos,&nbsp;Pier Giorgio Prada Moroni,&nbsp;Dumitru Pricopi,&nbsp;Loredana Prisinzano,&nbsp;Matthias Quade,&nbsp;Andreas Quirrenbach,&nbsp;Julio Arturo Rabanal Reina,&nbsp;Maria Cristina Rabello Soares,&nbsp;Gabriella Raimondo,&nbsp;Monica Rainer,&nbsp;Jose Ramón Rodón,&nbsp;Alejandro Ramón-Ballesta,&nbsp;Gonzalo Ramos Zapata,&nbsp;Stefanie Rätz,&nbsp;Christoph Rauterberg,&nbsp;Bob Redman,&nbsp;Ronald Redmer,&nbsp;Daniel Reese,&nbsp;Sara Regibo,&nbsp;Ansgar Reiners,&nbsp;Timo Reinhold,&nbsp;Christian Renie,&nbsp;Ignasi Ribas,&nbsp;Sergio Ribeiro,&nbsp;Thiago Pereira Ricciardi,&nbsp;Ken Rice,&nbsp;Olivier Richard,&nbsp;Marco Riello,&nbsp;Michel Rieutord,&nbsp;Vincenzo Ripepi,&nbsp;Guy Rixon,&nbsp;Steve Rockstein,&nbsp;José Ramón Rodón Ortiz,&nbsp;María Teresa Rodrigo Rodríguez,&nbsp;Alberto Rodríguez Amor,&nbsp;Luisa Fernanda Rodríguez Díaz,&nbsp;Juan Pablo Rodriguez Garcia,&nbsp;Julio Rodriguez-Gomez,&nbsp;Yannick Roehlly,&nbsp;Fernando Roig,&nbsp;Bárbara Rojas-Ayala,&nbsp;Tobias Rolf,&nbsp;Jakob Lysgaard Rørsted,&nbsp;Hugo Rosado,&nbsp;Giovanni Rosotti,&nbsp;Olivier Roth,&nbsp;Markus Roth,&nbsp;Alex Rousseau,&nbsp;Ian Roxburgh,&nbsp;Fabrice Roy,&nbsp;Pierre Royer,&nbsp;Kirk Ruane,&nbsp;Sergio Rufini Mastropasqua,&nbsp;Claudia Ruiz de Galarreta,&nbsp;Andrea Russi,&nbsp;Steven Saar,&nbsp;Melaine Saillenfest,&nbsp;Maurizio Salaris,&nbsp;Sebastien Salmon,&nbsp;Ippocratis Saltas,&nbsp;Réza Samadi,&nbsp;Aunia Samadi,&nbsp;Dominic Samra,&nbsp;Tiago Sanches da Silva,&nbsp;Miguel Andrés Sánchez Carrasco,&nbsp;Alexandre Santerne,&nbsp;Amaia Santiago Pé,&nbsp;Francesco Santoli,&nbsp;Ängela R. G. Santos,&nbsp;Rosario Sanz Mesa,&nbsp;Luis Manuel Sarro,&nbsp;Gaetano Scandariato,&nbsp;Martin Schäfer,&nbsp;Edward Schlafly,&nbsp;François-Xavier Schmider,&nbsp;Jean Schneider,&nbsp;Jesper Schou,&nbsp;Hannah Schunker,&nbsp;Gabriel Jörg Schwarzkopf,&nbsp;Aldo Serenelli,&nbsp;Dries Seynaeve,&nbsp;Yutong Shan,&nbsp;Alexander Shapiro,&nbsp;Russel Shipman,&nbsp;Daniela Sicilia,&nbsp;Maria Angeles Sierra sanmartin,&nbsp;Axelle Sigot,&nbsp;Kyle Silliman,&nbsp;Roberto Silvotti,&nbsp;Attila E. Simon,&nbsp;Ricardo Simoyama Napoli,&nbsp;Marek Skarka,&nbsp;Barry Smalley,&nbsp;Rodolfo Smiljanic,&nbsp;Samuel Smit,&nbsp;Alexis Smith,&nbsp;Leigh Smith,&nbsp;Ignas Snellen,&nbsp;Ádám Sódor,&nbsp;Frank Sohl,&nbsp;Sami K. Solanki,&nbsp;Francesca Sortino,&nbsp;Sérgio Sousa,&nbsp;John Southworth,&nbsp;Diogo Souto,&nbsp;Alessandro Sozzetti,&nbsp;Dimitris Stamatellos,&nbsp;Keivan Stassun,&nbsp;Manfred Steller,&nbsp;Dennis Stello,&nbsp;Beate Stelzer,&nbsp;Ulrike Stiebeler,&nbsp;Amalie Stokholm,&nbsp;Trude Storelvmo,&nbsp;Klaus Strassmeier,&nbsp;Paul Anthony Strøm,&nbsp;Antoine Strugarek,&nbsp;Sophia Sulis,&nbsp;Michal Švanda,&nbsp;László Szabados,&nbsp;Róbert Szabó,&nbsp;Gyula M. Szabó,&nbsp;Ewa Szuszkiewicz,&nbsp;Geert Jan Talens,&nbsp;Daniele Teti,&nbsp;Tom Theisen,&nbsp;Frédéric Thévenin,&nbsp;Anne Thoul,&nbsp;Didier Tiphene,&nbsp;Ruth Titz-Weider,&nbsp;Andrew Tkachenko,&nbsp;Daniel Tomecki,&nbsp;Jorge Tonfat,&nbsp;Nicola Tosi,&nbsp;Regner Trampedach,&nbsp;Gregor Traven,&nbsp;Amaury Triaud,&nbsp;Reidar Trønnes,&nbsp;Maria Tsantaki,&nbsp;Matthias Tschentscher,&nbsp;Arnaud Turin,&nbsp;Adam Tvaruzka,&nbsp;Bernd Ulmer,&nbsp;Solène Ulmer-Moll,&nbsp;Ceren Ulusoy,&nbsp;Gabriele Umbriaco,&nbsp;Diana Valencia,&nbsp;Marica Valentini,&nbsp;Adriana Valio,&nbsp;Ángel Luis Valverde Guijarro,&nbsp;Vincent Van Eylen,&nbsp;Valerie Van Grootel,&nbsp;Tim A. van Kempen,&nbsp;Timothy Van Reeth,&nbsp;Iris Van Zelst,&nbsp;Bart Vandenbussche,&nbsp;Konstantinos Vasiliou,&nbsp;Valeriy Vasilyev,&nbsp;David Vaz de Mascarenhas,&nbsp;Allona Vazan,&nbsp;Marina Vela Nunez,&nbsp;Eduardo Nunes Velloso,&nbsp;Rita Ventura,&nbsp;Paolo Ventura,&nbsp;Julia Venturini,&nbsp;Isabel Vera Trallero,&nbsp;Dimitri Veras,&nbsp;Eva Verdugo,&nbsp;Kuldeep Verma,&nbsp;Didier Vibert,&nbsp;Tobias Vicanek Martinez,&nbsp;Krisztián Vida,&nbsp;Arthur Vigan,&nbsp;Antonio Villacorta,&nbsp;Eva Villaver,&nbsp;Marcos Villaverde Aparicio,&nbsp;Valentina Viotto,&nbsp;Eduard Vorobyov,&nbsp;Sergey Vorontsov,&nbsp;Frank W. Wagner,&nbsp;Nicholas Walton,&nbsp;Dave Walton,&nbsp;Haiyang Wang,&nbsp;Rens Waters,&nbsp;Christopher Watson,&nbsp;Sven Wedemeyer,&nbsp;Angharad Weeks,&nbsp;Jörg Weingrill,&nbsp;Annita Weiss,&nbsp;Belinda Wendler,&nbsp;Richard West,&nbsp;Karsten Westerdorff,&nbsp;Pierre-Amaury Westphal,&nbsp;Peter Wheatley,&nbsp;Tim White,&nbsp;Amadou Whittaker,&nbsp;Kai Wickhusen,&nbsp;Thomas Wilson,&nbsp;James Windsor,&nbsp;Othon Winter,&nbsp;Mark Lykke Winther,&nbsp;Alistair Winton,&nbsp;Ulrike Witteck,&nbsp;Veronika Witzke,&nbsp;Peter Woitke,&nbsp;David Wolter,&nbsp;Günther Wuchterl,&nbsp;Mark Wyatt,&nbsp;Dan Yang,&nbsp;Jie Yu,&nbsp;Ricardo Zanmar Sanchez,&nbsp;María Rosa Zapatero Osorio,&nbsp;Mathias Zechmeister,&nbsp;Yixiao Zhou,&nbsp;Claas Ziemke,&nbsp;Konstanze Zwintz,&nbsp;Torsten Böhm,&nbsp;Léo Michel Dansac","doi":"10.1007/s10686-025-09985-9","DOIUrl":"10.1007/s10686-025-09985-9","url":null,"abstract":"<div><p>PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to &lt;2R<span>(_textrm{Earth})</span>) around bright stars (&lt;11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09985-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143852579","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A novel automated method for measuring spectral line indices of LAMOST-DR7 A-type stars","authors":"Fangyuan Chen,&nbsp;Liangping Tu,&nbsp;Hao Liu,&nbsp;Jian Zhao","doi":"10.1007/s10686-025-09996-6","DOIUrl":"10.1007/s10686-025-09996-6","url":null,"abstract":"<div><p>Stellar spectral line indices are key tools for studying stellar physical properties and evolutionary processes, playing a significant role in inferring important stellar attributes such as Teff, [Fe/H], and logg. This paper proposes an automated method for measuring stellar spectral line indices, specifically targeting LAMOST-DR7 A-type stellar spectra. The method involves several key steps: spectral preprocessing, continuum normalization, baseline correction, baseline fitting, spectral line fitting, and line index calculation, all aimed at achieving accurate spectral line index measurements. Traditional methods often encounter significant errors when dealing with complex spectral backgrounds. In contrast, the proposed method incorporates a series of optimizations and has been validated for robustness through Monte Carlo simulations. Our observational results indicate that this method is highly feasible from the comparisons to the line indices officially released by LAMOST and those in the Lick spectral library. Further testing with simulated data further demonstrates the reliability of this approach. This method provides a promising tool for future astronomical observations and stellar evolution studies and holds broad application potential. It not only helps improve the accuracy of research into stellar physical properties but also offers a practical technical approach for analyzing the composition and evolutionary patterns of stellar populations in galaxies.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809341","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Two complementary approaches of the periodicity detection in astronomical time series","authors":"Alexandru Pop,&nbsp;Maria Crăciun","doi":"10.1007/s10686-025-09995-7","DOIUrl":"10.1007/s10686-025-09995-7","url":null,"abstract":"<div><p>Estimation of the statistical significance of the peaks appearing in the spectra of various astronomical time series is essential for the detection of signals especially when they are contaminated by high levels of observational noise. In the present paper we consider a broader perspective which relies on two main aspects: (i) all the peaks have or may have significance and, therefore, (ii) we propose two complementary approaches to simultaneously supply estimates of the statistical significance of all the peaks of interest through Monte Carlo simulations. They are natural generalisations of the already used methods featured either by <i>specificity in frequency</i> or by <i>specificity in amplitude/power</i> of the peaks occurred in the spectrum. Three recently obtained radial velocity data on stars with orbiting exoplanets were used to illustrate these approaches: two G-type stars observed by the HARPS spectrograph (TOI-733, TOI-763) and an M-type star observed by the CARMENES spectrograph (Wolf 327). Some both interesting and useful features of the two considered statistical significances are also emphasised.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793217","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Machine learning applications to energy reconstruction of gamma-ray showers for the Tibet AS(gamma ) experiment","authors":"Y. Meng,&nbsp;J. Huang,&nbsp;D. Chen,&nbsp;K Y. Hu,&nbsp;Y. Zhang,&nbsp;L M. Zhai,&nbsp;Y H. Zou,&nbsp;Y L. Yu,&nbsp;Y Y. Li","doi":"10.1007/s10686-025-09993-9","DOIUrl":"10.1007/s10686-025-09993-9","url":null,"abstract":"<div><p>In order to improve the energy reconstruction accuracy of gamma-ray events observed by ground-based array experiments, this work propose a new energy estimator based on machine learning (ML) algorithm to determine the energies of gamma ray induced air showers in the energy range between 1 TeV and 10 PeV. We carry out a full Monte Carlo (MC) simulation using the Tibet air shower array and underground muon detector array, located at an altitude of 4,300 m above sea level. The MC simulated gamma-ray data are used to extract characteristic parameters depicting the air shower information, which are then fed into the ML model for training on both high-energy data sets (<span>(E &gt;sim 10)</span> TeV) and low-energy data sets (<span>(E &lt; 10)</span> TeV). In our simulation data tests, we found that the ML method showed significant advantages over traditional energy estimators (S50, <span>(N_e)</span>, and <span>(sum rho )</span>), with improved energy resolution for both low and high energy datasets. Compared to the traditional estimator, the energy resolution improves by approximately 30% for the inner array events and 55% for the outer array events at <span>(E &lt; 10)</span> TeV. At around 100 TeV, the energy resolution for large zenith angle events in the outer array improves by approximately 20%. This work also found that while the energy resolution of events falling the inside array can only be slightly improved, however, events outside array and at large zenith shower clear improvements. Moreover, it is particularly noteworthy that the ML method has little difference in the energy resolution of the inner and outer array events. The enhanced energy resolution achieved through the machine learning method for outer array events reduces the limitations imposed by the observation area, resulting in an approximately 30% improvement in statistical events. This method is suitable for ground-based array experiments in gamma-ray astronomy, and provides some technical support for further study of the primary gamma-ray energy reconstruction.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09993-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143740871","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Introduction to the SATech-01 satellite HEBS (GECAM-C)","authors":"Xinqiao Li,&nbsp;Xiangyang Wen,&nbsp;Shaolin Xiong,&nbsp;Zhenghua An,&nbsp;Yanbing Xu,&nbsp;Xiaohua Liang,&nbsp;Xiaojing Liu,&nbsp;Sheng Yang,&nbsp;Fan Zhang,&nbsp;Xilei Sun,&nbsp;Shuangnan Zhang,&nbsp;Min Gao,&nbsp;Jinzhou Wang,&nbsp;Dali Zhang,&nbsp;Ke Gong,&nbsp;Yaqing Liu,&nbsp;Xiaoyun Zhao,&nbsp;Zhenxia Zhang,&nbsp;Hong Lu,&nbsp;Wenxi Peng,&nbsp;Rui Qiao,&nbsp;Dongya Guo,&nbsp;Hui Wang,&nbsp;Yanguo Li,&nbsp;Chao Zheng,&nbsp;Chenwei Wang,&nbsp;Yanqiu Zhang,&nbsp;Lu Wang,&nbsp;Zhiqiang Ding,&nbsp;Xiaofeng Zhang","doi":"10.1007/s10686-025-09991-x","DOIUrl":"10.1007/s10686-025-09991-x","url":null,"abstract":"<div><p>The primary scientific objective of the High Energy Burst Searcher (HEBS) is to serve as a crucial component of the global space monitoring network for high-energy celestial burst sources. HEBS aims to monitor the high-energy electromagnetic counterparts of gravitational wave events, as well as the high-energy radiation from rapid radio bursts, gamma-ray bursts, magnetar flares, and other high-energy celestial phenomena across the entire sky. This effort will provide essential data support for related physical research, including energy spectra, light curves, and positional information. The probe is deployed on the Satech-01 satellite and operates in a 500 km solar-synchronous orbit. HEBS is equipped with two types of detectors: the Gamma Ray Detector (GRD) and the Charged Particle Detector (CPD). The GRD employs lanthanum bromide crystals coupled with silicon photomultiplier (SiPM) technology, as well as sodium iodide crystals paired with SiPM technology, to detect X-rays and gamma rays in the energy range of 6 keV to 5.9 MeV. It enables the localization of gamma-ray bursts and other high-energy events through the coordinated detection of multiple probes oriented in different directions. The CPD utilizes plastic scintillator technology coupled with SiPM to detect charged particles within the energy range of 150 keV to 5 MeV. When combined with the GRD, it effectively identifies and distinguishes space particle events from actual celestial phenomena. The payload processor (Electronics Box, EBOX) features onboard triggering and positioning capabilities, transmitting trigger times and positional data via Beidou short messaging in quasi-real time. This information will guide other telescopes in conducting follow-up observations.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143716949","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A novel optical design for wide-field imaging in X-ray astronomy","authors":"Neeraj K. Tiwari,&nbsp;Santosh V. Vadawale,&nbsp;N. P. S. Mithun","doi":"10.1007/s10686-025-09992-w","DOIUrl":"10.1007/s10686-025-09992-w","url":null,"abstract":"<div><p>Over the decades, astronomical X-ray telescopes have utilized the Wolter type-1 optical design, which provides stigmatic imaging in axial direction but suffers from coma and higher-order aberrations for off-axis sources. The Wolter-Schwarzschild design, with stigmatic imaging in the axial direction, while suffering from higher-order aberrations, is corrected for coma, thus performing better than the Wolter type-1. The Wolter type-1 and Wolter-Schwarzschild designs are optimized for on-axis but have reduced angular resolution when averaged over a wide field of view, with the averaging weighted by the area covered in the field of view. An optical design that maximizes angular resolution at the edge of the field of view rather than at the center is more suitable for wide-field X-ray telescopes required for deep-sky astronomical surveys or solar observations. A Hyperboloid-Hyperboloid optical design can compromise axial resolution to enhance field angle resolution, hence providing improved area-weighted average angular resolution over the Wolter-Schwarzschild design, but only for fields of view exceeding a specific size. Here, we introduce a new optical design that is free from coma aberration and capable of maximizing angular resolution at any desired field angle. This design consistently outperforms Wolter-1, Wolter-Schwarzschild, and Hyperboloid-Hyperboloid designs when averaged over any field of view size. The improvement in performance remains consistent across variations in other telescope parameters such as diameter, focal length, and mirror lengths. By utilizing this new optical design, we also present a design for a full-disk imaging solar X-ray telescope.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143612205","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Optical optimization of a dual-band sun-as-a-star extreme ultraviolet spectrograph for measuring the line-of-sight velocity of coronal mass ejections","authors":"Sifan Guo,&nbsp;Yufei Feng,&nbsp;Xianyong Bai,&nbsp;Hui Tian,&nbsp;Wei Duan,&nbsp;Xiaoming Zhu,&nbsp;Yajie Chen,&nbsp;Yuanyong Deng,&nbsp;Haiying Zhang,&nbsp;Zhiyong Zhang,&nbsp;Zhiwei Feng,&nbsp;Xiao Yang,&nbsp;Qi Yang,&nbsp;Mohamed Sedik","doi":"10.1007/s10686-025-09990-y","DOIUrl":"10.1007/s10686-025-09990-y","url":null,"abstract":"<div><p>The detection of Line-of-sight (LOS) velocity of coronal mass ejections (CMEs) is crucial for understanding and forecasting their propagation. The LOS velocity can be derived from the Sun-as-a-star extreme ultraviolet spectrograph based on the Doppler effect. However, the poor spectral resolution of existing instruments is not sufficient for detection. In the paper, we propose a dual-band Sun-as-a-star spectrograph with high spectral resolution for measuring the LOS velocity of CMEs. Based on a multilayer concave grating operating in a normal incident mode, we optimized the parameters of the spectrograph for the wavelength ranges of 18.3<span>( sim )</span>21.3 nm and 49.6<span>( sim )</span>52.9 nm. The spectral resolving power for these two ranges exceeds 1000 and 2000, respectively, which is about three times higher than that of the Extreme ultraviolet Variability Experiment onboard the Solar Dynamics Observatory. B<span>(_4)</span>C/Al and B<span>(_4)</span>C/Mo/Al multilayer structures were optimized to improve the diffraction efficiency across both bands simultaneously. We also evaluated the instrument performance by calculating the photon numbers. Additionally, we discussed the degradation of spectral resolution caused by the stability of satellite platform, determining that the stability should be better than ±7.2<span>(^{prime prime })</span>(<span>( pm )</span>0.002<span>(^circ )</span>) within the exposure time of 60 s. Our investigation provides a new way to observe Sun-as-a-star extreme ultraviolet spectrum.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143571107","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Simultaneous multi-spacecraft observations with VLBI radio telescopes to study the interplanetary phase scintillation","authors":"N. M. M. Said,&nbsp;G. Molera Calvés,&nbsp;P. Kummamuru,&nbsp;J. Edwards,&nbsp;M. Maoli,&nbsp;G. Cimo’","doi":"10.1007/s10686-025-09989-5","DOIUrl":"10.1007/s10686-025-09989-5","url":null,"abstract":"<div><p>Ground-based observations of spacecraft signals have been used to study space weather. However, single spacecraft measurements observed from the Earth have limitations in studying the structure and evolution of solar plasma as they are unable to differentiate spatial and temporal variations. To overcome this limitation and improve our understanding of interplanetary scintillation, we simultaneously observed radio signals transmitted by two co-orbiting spacecraft: the ESA Mars Express (MEX) and the Chinese National Space Administration Tianwen-1 (TIW-1). We conducted the observations from April to November 2021 using the University of Tasmania’s VLBI radio telescopes at 8.4 GHz. We employed the Planetary Radio Interferometer and Doppler Experiment (PRIDE) technique to determine the topocentric Doppler measurements and residual phase of the carrier signal. These observables were used to quantify the phase fluctuations of the spacecraft signals caused by solar wind and hydrodynamic turbulence in the interplanetary medium. The measured phase fluctuations RMS from both spacecraft show small differences which are caused by factors such as the spacecraft’s motion, onboard electronics, and variations in the uplink signal path through Earth’s ionosphere. These fluctuations decrease with solar elongation and correlate with solar radio flux at 10.7 cm (2800 MHz), indicating solar activity. The estimated total electron contents along MEX and TIW-1’s radio lines of sight are similar, with higher values at lower solar elongations. Simultaneous multi-spacecraft observations also enable RFI characterization, frequent spacecraft performance comparisons, and investigation of solar activity effects on spacecraft performance and scientific outcomes.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09989-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143564509","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}