Euclid 准备工作 LXXIX. 使用模拟低表面亮度矮星系探测 Euclid Wide Survey 的检测能力
星系天体物理
2025-11-17 v2 天体物理仪器与方法
摘要
局部宇宙矮星系可作为 cosmological 和质量组装探针。深层观测使我们能够研究这些对象下降到低表面亮度 (LSB) 领域。本文我们估算 Euclid 的矮星系检测能力以及其 MERge 处理函数 (MER 流程) 的限制，该流程负责生成堆叠马赛克和最终目录。为此，我们在实际的 Euclid Wide Survey (EWS) 场域中注入模拟矮星系，并将输入目录与最终 MER 目录进行比较。模拟矮星系使用带有结构参数（包括大小和表面亮度）从观测到的矮星系目录中抽取的简单 Sersic 模型生成。这些模拟代表一种理想化情形，即不考虑额外因素，如离心率、形态或拥挤。为描述检测到的矮星系，我们使用有效半径内的平均表面亮度 SB_e（单位为 mag arcsec^-2）。最终 MER 目录在 SB_e 位于 [21,24] 时的完整性达到 91%，在 SB_e 位于 [24,28] 时的完整性为 54%。这些数值未考虑可能的污染物，包括与矮星系位置的背景星系混淆。考虑到这些效应后，分别降低至 86% 和 38%。MER 流程采用小网格大小进行最终局部背景减除，导致 R_e > 10 arcsec 的星系发生通量损失。通过使用最终 MER 马赛克并重新注入该局部背景，我们获得的图像中可恢复位于弧分钟尺度下的可靠光度属性。因此，该背景重注入产品适用于研究局部宇宙矮星系。Euclid 的数据减法流程为其他深层观测提供了测试平台，尤其是关于背景减除方法，LSB 科学中的关键问题。
引用
@article{arxiv.2509.13163,
title = {Euclid preparation LXXIX. Using mock low surface brightness dwarf galaxies to probe Euclid Wide Survey detection capabilities},
author = {Euclid Collaboration and M. Urbano and P. -A. Duc and M. Poulain and A. A. Nucita and A. Venhola and O. Marchal and M. Kümmel and H. Kong and F. Soldano and E. Romelli and M. Walmsley and T. Saifollahi and K. Voggel and A. Lançon and F. R. Marleau and E. Sola and L. K. Hunt and J. Junais and D. Carollo and P. M. Sanchez-Alarcon and M. Baes and F. Buitrago and Michele Cantiello and J. -C. Cuillandre and H. Domínguez Sánchez and A. Ferré-Mateu and A. Franco and J. Gracia-Carpio and R. Habas and M. Hilker and E. Iodice and J. H. Knapen and M. N. Le and D. Martínez-Delgado and O. Müller and F. De Paolis and P. Papaderos and R. Ragusa and J. Román and E. Saremi and V. Testa and B. Altieri and L. Amendola and S. Andreon and N. Auricchio and C. Baccigalupi and M. Baldi and S. Bardelli and P. Battaglia and A. Biviano and E. Branchini and M. Brescia and S. Camera and G. Cañas-Herrera and V. Capobianco and C. Carbone and J. Carretero and S. Casas and M. Castellano and G. Castignani and S. Cavuoti and A. Cimatti and C. Colodro-Conde and G. Congedo and C. J. Conselice and L. Conversi and Y. Copin and F. Courbin and H. M. Courtois and M. Cropper and A. Da Silva and H. Degaudenzi and G. De Lucia and H. Dole and F. Dubath and C. A. J. Duncan and X. Dupac and S. Dusini and S. Escoffier and M. Farina and R. Farinelli and S. Ferriol and F. Finelli and M. Frailis and E. Franceschi and M. Fumana and S. Galeotta and K. George and B. Gillis and C. Giocoli and A. Grazian and F. Grupp and L. Guzzo and S. V. H. Haugan and W. Holmes and I. M. Hook and F. Hormuth and A. Hornstrup and K. Jahnke and M. Jhabvala and B. Joachimi and E. Keihänen and S. Kermiche and A. Kiessling and B. Kubik and M. Kunz and H. Kurki-Suonio and R. Laureijs and A. M. C. Le Brun and S. Ligori and P. B. Lilje and V. Lindholm and I. Lloro and G. Mainetti and D. Maino and E. Maiorano and O. Mansutti and O. Marggraf and M. Martinelli and N. Martinet and F. Marulli and R. J. Massey and E. Medinaceli and S. Mei and Y. Mellier and M. Meneghetti and E. Merlin and G. Meylan and A. Mora and M. Moresco and L. Moscardini and R. Nakajima and C. Neissner and S. -M. Niemi and C. Padilla and S. Paltani and F. Pasian and K. Pedersen and V. Pettorino and S. Pires and G. Polenta and M. Poncet and L. A. Popa and L. Pozzetti and F. Raison and R. Rebolo and A. Renzi and J. Rhodes and G. Riccio and M. Roncarelli and R. Saglia and Z. Sakr and D. Sapone and B. Sartoris and P. Schneider and T. Schrabback and A. Secroun and G. Seidel and S. Serrano and P. Simon and C. Sirignano and G. Sirri and L. Stanco and J. -L. Starck and J. Steinwagner and P. Tallada-Crespí and A. N. Taylor and H. I. Teplitz and I. Tereno and N. Tessore and S. Toft and R. Toledo-Moreo and F. Torradeflot and I. Tutusaus and L. Valenziano and J. Valiviita and T. Vassallo and G. Verdoes Kleijn and A. Veropalumbo and Y. Wang and J. Weller and G. Zamorani and I. A. Zinchenko and E. Zucca and M. Ballardini and M. Bolzonella and E. Bozzo and C. Burigana and R. Cabanac and A. Cappi and D. Di Ferdinando and J. A. Escartin Vigo and L. Gabarra and M. Huertas-Company and J. Martín-Fleitas and S. Matthew and N. Mauri and R. B. Metcalf and A. Pezzotta and M. Pöntinen and C. Porciani and I. Risso and V. Scottez and M. Sereno and M. Tenti and M. Viel and M. Wiesmann and Y. Akrami and I. T. Andika and S. Anselmi and M. Archidiacono and F. Atrio-Barandela and D. Bertacca and M. Bethermin and A. Blanchard and L. Blot and M. Bonici and S. Borgani and M. L. Brown and S. Bruton and A. Calabro and B. Camacho Quevedo and F. Caro and C. S. Carvalho and T. Castro and F. Cogato and S. Conseil and A. R. Cooray and O. Cucciati and S. Davini and G. Desprez and A. Díaz-Sánchez and J. J. Diaz and S. Di Domizio and J. M. Diego and M. Y. Elkhashab and A. Enia and Y. Fang and A. G. Ferrari and A. Finoguenov and K. Ganga and J. García-Bellido and T. Gasparetto and V. Gautard and E. Gaztanaga and F. Giacomini and F. Gianotti and G. Gozaliasl and M. Guidi and C. M. Gutierrez and A. Hall and H. Hildebrandt and J. Hjorth and J. J. E. Kajava and Y. Kang and V. Kansal and D. Karagiannis and K. Kiiveri and J. Kim and C. C. Kirkpatrick and S. Kruk and J. Le Graet and L. Legrand and M. Lembo and F. Lepori and G. Leroy and G. F. Lesci and J. Lesgourgues and L. Leuzzi and T. I. Liaudat and A. Loureiro and J. Macias-Perez and G. Maggio and M. Magliocchetti and F. Mannucci and R. Maoli and C. J. A. P. Martins and L. Maurin and M. Miluzio and P. Monaco and C. Moretti and G. Morgante and K. Naidoo and A. Navarro-Alsina and S. Nesseris and D. Paoletti and F. Passalacqua and K. Paterson and L. Patrizii and A. Pisani and D. Potter and S. Quai and M. Radovich and G. Rodighiero and S. Sacquegna and M. Sahlén and D. B. Sanders and E. Sarpa and A. Schneider and D. Sciotti and E. Sellentin and L. C. Smith and J. G. Sorce and K. Tanidis and C. Tao and G. Testera and R. Teyssier and S. Tosi and A. Troja and M. Tucci and C. Valieri and D. Vergani and G. Verza and P. Vielzeuf and N. A. Walton},
journal= {arXiv preprint arXiv:2509.13163},
year = {2025}
}
备注
Accepted for publication in Astronomy & Astrophysics (acceptance date: 30/10/2025). 22 pages, 19 figures, 7 tables