PAPER / ARXIV:2609.05155
Euclid Collaboration : I. Risso (1 and 2 and 3), B. R. Granett (3), E. Branchini (1 and 2 and 3), A. Veropalumbo (3 and 2 and 1), B. Kubik (4), P. Monaco (5 and 6 and 7 and 8), J. Comparat (9), A. Hall (10), N. Aghanim (11), B. Altieri (12), A. Amara (13), S. Andreon (3), N. Auricchio (14), C. Baccigalupi (8 and 6 and 7 and 15), M. Baldi (16 and 14 and 17), A. Balestra (18), S. Bardelli (14), P. Battaglia (14), A. Biviano (6 and 8), M. Bolzonella (14), M. Brescia (19 and 20), S. Camera (21 and 22 and 23), G. Cañas-Herrera (24), V. Capobianco (23), C. Carbone (25), J. Carretero (26 and 27), F. J. Castander (28 and 29), M. Castellano (30), G. Castignani (14), S. Cavuoti (20 and 31), A. Cimatti (32), C. Colodro-Conde (33), G. Congedo (10), L. Conversi (34 and 12), Y. Copin (4), F. Courbin (35 and 36 and 37), H. M. Courtois (38), H. Degaudenzi (39), S. de la Torre (40), G. De Lucia (6), H. Dole (11), F. Dubath (39), X. Dupac (12), S. Dusini (41), S. Escoffier (42), M. Farina (43), R. Farinelli (14), S. Ferriol (4), F. Finelli (14 and 44), N. Fourmanoit (42), M. Frailis (6), E. Franceschi (14), M. Fumana (25), L. Gabarra (45), S. Galeotta (6), K. George (46), W. Gillard (42), B. Gillis (10), C. Giocoli (14 and 17), J. Gracia-Carpio (47), A. Grazian (18), F. Grupp (47 and 48), L. Guzzo (49 and 3 and 50), S. V. H. Haugan (51), S. Hemmati (52), W. Holmes (53), F. Hormuth (54), A. Hornstrup (55 and 56), K. Jahnke (57), M. Jhabvala (58), B. Joachimi (59), S. Kermiche (42), A. Kiessling (53), M. Kümmel (48), M. Kunz (60), H. Kurki-Suonio (61 and 62), A. M. C. Le Brun (63), S. Ligori (23), P. B. Lilje (51), V. Lindholm (61 and 62), I. Lloro (64), M. Magliocchetti (43), G. Mainetti (65), O. Mansutti (6), O. Marggraf (66), M. Martinelli (30 and 67), N. Martinet (40), F. Marulli (68 and 14 and 17), R. J. Massey (69), N. Mauri (32 and 17), E. Medinaceli (14), M. Melchior (70), M. Meneghetti (14 and 17), E. Merlin (18), G. Meylan (71), A. Mora (72), M. Moresco (68 and 14), C. Moretti (6 and 8 and 7), L. Moscardini
RESUMO
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.
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