Euclid：一种用于诊断Euclid光谱巡天中恒星相关系统误差的两点相关方法

Euclid. A two-point correlation approach to diagnosing star-related systematics in the Euclid spectroscopic survey

Euclid Collaboration, I. Risso, B. R. Granett, E. Branchini, A. Veropalumbo, B. Kubik, P. Monaco, J. Comparat, A. Hall, N. Aghanim, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, P. Battaglia, A. Biviano, M. Bolzonella, M. Brescia, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, F. J. Castander, M. Castellano, G. Castignani, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, L. Conversi, Y. Copin, F. Courbin, H. M. Courtois, H. Degaudenzi, S. de la Torre, G. De Lucia, H. Dole, F. Dubath, X. Dupac, S. Dusini, S. Escoffier, M. Farina, R. Farinelli, S. Ferriol, F. Finelli, N. Fourmanoit, M. Frailis, E. Franceschi, M. Fumana, L. Gabarra, S. Galeotta, K. George, W. Gillard, B. Gillis, C. Giocoli, J. Gracia-Carpio, A. Grazian, F. Grupp, L. Guzzo, S. V. H. Haugan, S. Hemmati, W. Holmes, F. Hormuth, A. Hornstrup, K. Jahnke, M. Jhabvala, B. Joachimi, S. Kermiche, A. Kiessling, M. Kümmel, M. Kunz, H. Kurki-Suonio, A. M. C. Le Brun, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, M. Magliocchetti, G. Mainetti, O. Mansutti, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R. J. Massey, N. Mauri, E. Medinaceli, M. Melchior, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, C. Moretti, L. Moscardini, R. Nakajima, C. Neissner, S. -M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, W. J. Percival, V. Pettorino, A. Pezzotta, S. Pires, G. Polenta, M. Poncet, L. A. Popa, F. Raison, A. Renzi, J. Rhodes, G. Riccio, F. Rizzo, E. Romelli, M. Roncarelli, B. Rusholme, R. Saglia, Z. Sakr, A. G. Sánchez, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, M. Scodeggio, A. Secroun, E. Sihvola, C. Sirignano, G. Sirri, L. Stanco, P. Tallada-Crespí, A. N. Taylor, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, J. Valiviita, T. Vassallo, Y. Wang, J. Weller, G. Zamorani, F. M. Zerbi, E. Zucca, M. Ballardini, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, A. Cappi, F. Caro, T. Castro, J. A. Escartin Vigo, J. García-Bellido, T. Gasparetto, J. Macias-Perez, R. Maoli, R. B. Metcalf, A. A. Nucita, M. Pöntinen, E. Sarpa, V. Scottez, M. Sereno, M. Tenti, M. Tucci, M. Viel, M. Wiesmann, J. A. Acevedo Barroso, Y. Akrami, I. T. Andika, S. Anselmi, M. Archidiacono, G. Aricò, F. Atrio-Barandela, M. Baes, L. Bazzanini, J. Bel, D. Bertacca, M. Bethermin, F. Beutler, L. Blot, M. Bonici, M. L. Brown, S. Bruton, B. Camacho Quevedo, P. Carrilho, C. S. Carvalho, F. Cogato, T. E. Collett, S. Conseil, S. Contarini, A. R. Cooray, P. Corcho-Caballero, B. Csizi, O. Cucciati, S. Davini, T. de Boer, F. De Paolis, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J. M. Diego, V. Duret, A. Enia, Y. Fang, A. Farina, A. Finoguenov, A. Franco, Y. Fu, K. Ganga, E. Gaztanaga, Z. Ghaffari, F. Giacomini, F. Gianotti, G. Gozaliasl, A. Gruppuso, M. Guidi, C. M. Gutierrez, H. Hildebrandt, J. Hjorth, M. Jauzac, J. J. E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, J. Kim, C. C. Kirkpatrick, A. Kovács, I. Kovačić, K. Koyama, S. Kruk, M. C. Lam, F. Leclercq, L. Legrand, M. Lembo, G. Leroy, G. F. Lesci, J. Lesgourgues, T. I. Liaudat, L. Linke, S. J. Liu, F. Mannucci, F. R. Marleau, C. J. A. P. Martins, M. Miluzio, G. Morgante, S. Nadathur, K. Naidoo, A. Navarro-Alsina, S. Nesseris, L. Nicastro, F. Oppizzi, F. Pace, D. Paoletti, G. Parimbelli, F. Passalacqua, K. Paterson, L. Patrizii, C. Pattison, R. Paviot, A. Pisani, D. Potter, G. W. Pratt, S. Quai, M. Radovich, G. Rodighiero, W. Roster, S. Sacquegna, M. Sahlén, D. B. Sanders, A. Schneider, D. Sciotti, E. Sellentin, S. Serjeant, L. C. Smith, J. G. Sorce, I. Szapudi, M. Talia, K. Tanidis, C. Tao, F. Tarsitano, G. Testera, R. Teyssier, S. Tosi, A. Troja, C. Uhlemann, C. Valieri, A. Venhola, D. Vergani, G. Verza, S. Vinciguerra, M. von Wietersheim-Kramsta, N. A. Walton, L. Wang, A. H. Wright

arXiv 2609.05155首次发表：2026-09-07更新：2026-09-07

发表机构

Università di Genova; INFN-Sezione di Genova; INAF-Osservatorio Astronomico di Brera; Université Claude Bernard Lyon 1; Dipartimento di Fisica - Sezione di Astronomia, Università di Trieste; INAF-Osservatorio Astronomico di Trieste; INFN, Sezione di Trieste; IFPU, Institute for Fundamental Physics of the Universe; Univ. Grenoble Alpes（热那亚大学; 意大利国家核物理研究所热那亚分部; 意大利国家天体物理研究所布雷拉天文台; 里昂第一大学; 的里雅斯特大学物理系天文学部; 意大利国家天体物理研究所的里雅斯特天文台; 意大利国家核物理研究所的里雅斯特分部; 宇宙基础物理研究所; 格勒诺布尔阿尔卑斯大学）

机构由 AI 辅助整理，请以论文原文为准。

AI 中文总结

该研究提出一种两点相关方法，利用EuclidLargeMocks等星表，分析光度余辉和恒星掩膜不匹配对Euclid光谱巡天星系成团性的影响，发现恒星-星系互相关可检测低至10%的残余光度余辉。

AI 中文摘要

Euclid光谱巡天将以前所未有的精度测量星系成团性，这需要严格控制观测和仪器系统误差。恒星相关效应可能通过光度余辉和恒星的不完美掩膜污染光谱图像。我们表征了它们对星系成团性分析的影响，重点关注数据中可识别的角特征。我们使用角和空间自相关及互相关统计量。对于星系，我们使用了来自EuclidLargeMocks的模拟光谱星表，覆盖Euclid宽巡天（EWS）的330平方度区域；对于恒星，我们使用了同一区域的Gaia和2MASS星表。为模拟光度余辉，我们实现了一个基于光谱测量校准的简化探测器级模型，并改变其强度以引入不同的干扰天体比例。对于恒星掩膜，我们对应用于数据的掩膜与应用于随机星表的掩膜之间的不一致进行了建模。我们使用Landy–Szalay估计器测量了恒星-恒星、星系-星系和恒星-星系角相关函数，并量化了与预期零恒星-星系相关性的偏差。我们还通过三维两点相关函数（2PCF）评估了此类系统误差的大尺度影响。光度余辉在约100角秒尺度的恒星-星系角互相关中产生了对应于Euclid抖动模式和棱镜色散几何的特征，以及一个高达1°的近似恒定的虚假正信号。恒星-星系互相关可以在数据发布1（Data Release 1）光谱星表中检测到低至10%污染水平的残余光度余辉。相比之下，在现实的EWS条件下，恒星掩膜不匹配会产生强烈的小尺度角特征，但对大尺度2PCF的影响可忽略不计。

英文摘要

The Euclid spectroscopic survey will measure galaxy clustering with unprecedented precision, requiring stringent control of observational and instrumental systematics. Star-related effects may contaminate spectroscopic images through photometric persistence and imperfect masking of stars. We characterized their impact on galaxy clustering analyses, focusing on angular features identifiable in the data. We used angular and spatial auto- and cross-correlation statistics. For galaxies, we used mock spectroscopic catalogues from the EuclidLargeMocks in a 330 deg2 region of the Euclid Wide Survey (EWS). For stars, we used Gaia and 2MASS catalogues in the same area. To simulate photometric persistence, we implemented a simplified detector-level model calibrated on spectroscopic measurements and varied its strength to introduce different interloper fractions. For stellar masking, we modelled inconsistencies between the mask applied to the data and to the random catalogue. We measured star-star, galaxy-galaxy, and star-galaxy angular correlation functions using the Landy--Szalay estimator, and quantified deviations from the expected null star-galaxy correlation. We also evaluated the large-scale impact of such systematics through the three-dimensional two-point correlation function (2PCF). Photometric persistence produces a characteristic feature in the star-galaxy angular cross-correlation at scales of order 100", corresponding to the Euclid dithering pattern and grism dispersion geometry, and a spurious positive signal approximately constant up to 1°. Star-galaxy cross-correlation can detect residual persistence at contamination levels as low as 10% in a Data Release 1 spectroscopic catalogue. In contrast, stellar-mask mismatches produce strong small-scale angular signatures but have negligible impact on the large-scale 2PCF under realistic EWS conditions.

论文原文

arXiv 摘要页 · PDF 原文 · HTML 原文