IAS-LAB PUBLICATIONS
Prevalence of rare missense TTN variants in a cohort of patients with cardiomyopathy
Authors: Bottillo Irene; Ciccone Maria Pia; Magliozzi Monia; Pilichou Kalliopi; Girotto Giorgia; Girolami Francesca; Cecconi Massimiliano; D'Argenio Valeria; Novelli Valeria; Coiana Alessandra; Formicola Daniela; Micaglio Emanuele; Tortora Giada; Gualandi Francesca; Petrucci Simona; Castori Marco; Resta Nicoletta; Vestri Anna Rita; Iascone Maria; Grammatico Paola
Journal: JOURNAL OF MOLECULAR AND CELLULAR CARDIOLOGY
Published: 2025
DOI: 10.1016/j.yjmcc.2024.12.004
Volume: 199 Pages: 46-50
Euclid preparation: LVIII. Detecting extragalactic globular clusters in the Euclid survey
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; HRK-2012-2023; JGX-3888-2023; GEH-7593-2022; FGL-6869-2022; ENM-3795-2022; KKP-9133-2024; DWB-0787-2022; EYY-4006-2022; LXV-7382-2024; GNE-1283-2022; MVR-8365-2025; HEO-6319-2022; FSV-8899-2022; H-4394-2019; ABB-9156-2021; GXI-6108-2022; JYY-9592-2024; ENE-3351-2022; EPI-1133-2022; CJC-9258-2022; B-4348-2013; DWO-2405-2022; EVW-7270-2022; GFK-2340-2022; Z-4828-2019; LBZ-7918-2024; DVE-7652-2022; GSC-5225-2022; KPF-2019-2024; LTE-2549-2024; LOZ-1470-2024; JNB-8974-2023; HVE-8025-2023; CEY-5520-2022; HZQ-9553-2023; IUT-7926-2023; EKV-4052-2022; CHO-3061-2022; HRV-6262-2023; JWI-9457-2024; LUN-9319-2024; HWT-5982-2023; HFL-6092-2022; E-2727-2014; DWB-9873-2022; L-8237-2014; MEO-0896-2025; IVA-4275-2023; JUX-7553-2023; B-4650-2017; IRQ-6937-2023; HTG-8587-2023; H-8587-2015; DVC-6323-2022; LTU-6502-2024; LEQ-1557-2024; AGZ-3259-2022; FZL-7353-2022; A-2693-2010; EVT-3533-2022; CNE-2384-2022; HLX-2021-2023; KBZ-1983-2024; EUO-2530-2022; EUK-3820-2022; EVA-7948-2022; JRB-6526-2023; MOU-4416-2025; CQF-5798-2022; CQN-5681-2022; ITG-6579-2023; EUI-3706-2022; JWF-2506-2024; JUF-9810-2023; GWP-3456-2022; MUO-4676-2025; CQR-5759-2022; KER-9145-2024; JGR-4365-2023; CTE-6775-2022; CSK-3817-2022; FBF-5584-2022; HRW-8595-2023; FBE-0351-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; HPW-2820-2023; DWS-1040-2022; MNZ-8396-2025; FFG-2233-2022; FCS-1018-2022; DAV-9216-2022; CYT-5449-2022; GWA-7849-2022; KAK-4177-2024; B-8502-2016; DAV-8065-2022; DDB-6234-2022; HYH-6107-2023; A-2699-2012; MDN-2641-2025; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; DFQ-7859-2022; DFY-8508-2022; MFB-4566-2025; MWK-2416-2025; HFG-7438-2022; D-1300-2016; DFZ-7309-2022; GNG-7078-2022; FNC-4379-2022; FLD-9518-2022; DFW-8877-2022; DHS-8142-2022; KEK-6332-2024; KJY-7272-2024; FOW-5617-2022; KSI-9422-2024; KNP-2716-2024; DJO-8166-2022; MNN-0179-2025; KFB-7397-2024; ABB-2322-2020; DKF-4281-2022; HTJ-4919-2023; IHG-7220-2023; DLB-6897-2022; KBT-5668-2024; MTQ-2344-2025; IVG-7504-2023; FSY-2184-2022; DMX-5934-2022; HPO-8234-2023; DNY-0415-2022; HTE-6970-2023; JMR-9144-2023; OON-3882-2025; DNX-4243-2022; MXB-9468-2025; GCT-2940-2022; IGN-7320-2023; JVJ-6571-2024; HFW-5845-2022; CDE-5677-2022; MDQ-9712-2025; DPD-7597-2022; JWG-7083-2024; IZJ-2041-2023; IZM-5556-2023; GBY-3944-2022; IHY-7449-2023; HRO-4465-2023; KKE-9686-2024; EAA-4768-2022; LGB-5701-2024; KFZ-7504-2024; L-8068-2014; DZM-7523-2022; GDK-6495-2022; T-7378-2018; MVR-7884-2025; ECA-8225-2022; DYT-7473-2022; HNI-8187-2023; ECZ-6053-2022; JCG-3503-2023; NBH-4743-2025; ABD-6783-2021; HQC-0143-2023; HWF-6506-2023; MXO-2726-2025; HZW-5449-2023; DVM-3959-2022; KBV-9584-2024; LWL-2178-2024; CMV-6954-2022; CDE-1189-2022; JUD-5049-2023; GBY-6621-2022; FJX-8996-2022; IZB-6495-2023; IAC-8042-2023; ECX-7840-2022; CEY-5704-2022; JHB-9875-2023; MNS-3973-2025; IYE-9818-2023; JHC-4470-2023; HIV-4758-2022; CHK-6722-2022; KTI-3074-2024; B-3004-2019; MLC-7865-2025; AFR-7693-2022; GBB-5111-2022; HZX-4069-2023; EOI-0533-2022; S-1204-2016; HOH-0341-2023; MLE-5291-2025; ISJ-4889-2023; CMX-4174-2022; MJF-0435-2025; JHG-8097-2023; L-6378-2014; IDQ-0489-2023; JTL-0752-2023; KSN-3481-2024; HQG-1163-2023; EYU-4413-2022; EVC-7104-2022; CRZ-8120-2022; C-2920-2017; CQL-4862-2022; NUD-5395-2025; CSH-1681-2022; ABB-8257-2020; NBI-5904-2025; JZW-7667-2024; KNK-3731-2024; AAK-4578-2020; HRR-2616-2023; JCW-4739-2023; GEC-5455-2022; HRX-7202-2023; DVZ-8147-2022; LYK-3518-2024; DDY-1012-2022; FZY-7746-2022; GQU-8893-2022; KND-8351-2024; DWN-4354-2022; KEZ-0532-2024; MVA-1492-2025; DGC-7489-2022; MKJ-0611-2025; D-1237-2017; HLL-5972-2023; JHX-6642-2023; GCF-0434-2022; GIM-5410-2022; HRS-4550-2023; ORK-4232-2025; GGM-6223-2022; MVC-4382-2025; JCV-3612-2023; MRW-3611-2025; GEF-7978-2022; FSR-7582-2022; DWT-7233-2022; MWU-5876-2025; NBF-7788-2025; INY-7970-2023; JCM-8241-2023; JAN-6167-2023; GDF-8239-2022; MDF-0079-2025; JEZ-2766-2023; MUC-7166-2025; KZQ-2739-2024; JSZ-6163-2023; NBR-5956-2025; IAD-4339-2023; 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Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202450851
Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid telescope, using both simulated pre-launch images and the first early-release observations of the Fornax galaxy cluster. The Euclid Wide Survey will provide high-spatial resolution VIS imaging in the broad IE band as well as near-infrared photometry (YE, JE, and HE). We estimate that the 24 719 known galaxies within 100 Mpc in the footprint of the Euclid survey host around 830 000 EGCs of which about 350 000 are within the survey’s detection limits. For about half of these EGCs, three infrared colours will be available as well. For any galaxy within 50 Mpc the brighter half of its GC luminosity function will be detectable by the Euclid Wide Survey. The detectability of EGCs is mainly driven by the residual surface brightness of their host galaxy. We find that an automated machine-learning EGC-classification method based on real Euclid data of the Fornax galaxy cluster provides an efficient method to generate high purity and high completeness GC candidate catalogues. We confirm that EGCs are spatially resolved compared to pure point sources in VIS images of Fornax. Our analysis of both simulated and first on-sky data show that Euclid will increase the number of GCs accessible with high-resolution imaging substantially compared to previous surveys, and will permit the study of GCs in the outskirts of their hosts. Euclid is unique in enabling systematic studies of EGCs in a spatially unbiased and homogeneous manner and is primed to improve our understanding of many understudied aspects of GC astrophysics.
Volume: 693
Keywords: Galaxies: nuclei; Galaxies: star clusters: general; Space vehicles: instruments;
Euclid: A complete Einstein ring in NGC 6505
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; JAX-2768-2023; IGO-5191-2023; FZX-4882-2022; DBL-5256-2022; DXZ-7810-2022; IUS-5192-2023; GBC-8404-2022; CKU-5761-2022; HQA-9441-2023; DMU-8531-2022; NBI-9280-2025; NBA-8033-2025; CBK-5920-2022; CSY-1689-2022; MNN-3541-2025; AAD-3011-2021; CGD-2351-2022; FYJ-4908-2022; MGX-9029-2025; ISJ-4889-2023; AFJ-2074-2022; I-2511-2015; MDG-9557-2025; MVE-8410-2025; JGR-4365-2023; MMS-5823-2025; DFW-8877-2022; D-1237-2017; FSV-8899-2022; JMS-1539-2023; H-4394-2019; GHS-5944-2022; MQB-8395-2025; MXB-2135-2025; FZO-1254-2022; JNB-8974-2023; HVE-8025-2023; KKX-1153-2024; CEY-5520-2022; HZQ-9553-2023; EKA-7986-2022; IUT-7926-2023; LXX-3952-2024; IUQ-9509-2023; GNJ-2760-2022; CHO-3061-2022; HRV-6262-2023; JWI-9457-2024; LUN-9319-2024; CJD-7824-2022; HWT-5982-2023; HFL-6092-2022; E-2727-2014; L-8237-2014; MEO-0896-2025; E-8021-2017; IVA-4275-2023; JUX-7553-2023; B-4650-2017; ESG-5016-2022; HTG-8587-2023; H-8587-2015; B-4348-2013; DVC-6323-2022; LTU-6502-2024; GLO-1082-2022; IUS-3917-2023; AGZ-3259-2022; FZL-7353-2022; A-2693-2010; EVT-3533-2022; CNE-2384-2022; HLX-2021-2023; KBZ-1983-2024; EUO-2530-2022; ETL-7525-2022; EUK-3820-2022; EVA-7948-2022; JRB-6526-2023; MOU-4416-2025; IBV-9243-2023; CQF-5798-2022; EVA-4097-2022; ITG-6579-2023; EUI-3706-2022; JWF-2506-2024; JUF-9810-2023; MUO-4676-2025; CQR-5759-2022; KER-9145-2024; GAX-2002-2022; CTE-6775-2022; CSK-3817-2022; CUA-0149-2022; FBF-5584-2022; EYM-5386-2022; HRW-8595-2023; FBE-0351-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; EYY-4006-2022; HPW-2820-2023; FBM-0217-2022; JWD-0263-2024; DWS-1040-2022; MNZ-8396-2025; FFG-2233-2022; FCS-1018-2022; DAV-9216-2022; CYT-5449-2022; GWA-7849-2022; KAK-4177-2024; B-8502-2016; MDB-7431-2025; DAV-8065-2022; LYD-9061-2024; HYH-6107-2023; A-2699-2012; MDN-2641-2025; FIV-3763-2022; FLM-0394-2022; MTO-5925-2025; DWZ-6747-2022; DFQ-7859-2022; DFY-8508-2022; MFB-4566-2025; MWK-2416-2025; HFG-7438-2022; D-1300-2016; GNG-7078-2022; FNC-4379-2022; DFC-8070-2022; FLD-9518-2022; DHS-8142-2022; KEK-6332-2024; KJY-7272-2024; FOW-5617-2022; KNP-2716-2024; MNN-0179-2025; KFB-7397-2024; ABB-2322-2020; DKF-4281-2022; HTJ-4919-2023; IHG-7220-2023; DLB-6897-2022; HTM-1531-2023; KBT-5668-2024; MTQ-2344-2025; IVG-7504-2023; FSY-2184-2022; DMX-5934-2022; HPO-8234-2023; DNY-0415-2022; HTE-6970-2023; JMR-9144-2023; OON-3882-2025; DNX-4243-2022; DNY-1328-2022; MVR-8365-2025; MXB-9468-2025; GCT-2940-2022; HUZ-7198-2023; IGN-7320-2023; JVJ-6571-2024; FXG-6905-2022; HFW-5845-2022; CDE-5677-2022; DPD-7597-2022; JWG-7083-2024; IZJ-2041-2023; GBY-3944-2022; IHY-7449-2023; HRO-4465-2023; KKE-9686-2024; EAA-4768-2022; LGB-5701-2024; L-8068-2014; GDK-6495-2022; T-7378-2018; MVR-7884-2025; ECA-8225-2022; HNI-8187-2023; ECZ-6053-2022; FCD-8153-2022; JCG-3503-2023; NBS-7222-2025; ABD-6783-2021; GGK-1011-2022; HQC-0143-2023; HWF-6506-2023; KBV-9584-2024; LYP-7992-2024; FQI-9285-2022; IAC-8042-2023; B-1966-2015; HWT-1959-2023; 57210265918; 57120105100; 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Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202453014
We report the discovery of a complete Einstein ring around the elliptical galaxy NGC 6505, at z = 0.042. This is the first strong gravitational lens discovered in Euclid and the first in an NGC object from any survey. The combination of the low redshift of the lens galaxy, the brightness of the source galaxy (IE = 18.1 lensed, IE = 21.3 unlensed), and the completeness of the ring make this an exceptionally rare strong lens, unidentified until its observation by Euclid. We present deep imaging data of the lens from the Euclid Visible Camera (VIS) and Near-Infrared Spectrometer and Photometer (NISP) instruments, as well as resolved spectroscopy from the Keck Cosmic Web Imager (KCWI). The Euclid imaging in particular presents one of the highest signal-to-noise ratio optical/near-infrared observations of a strong gravitational lens to date. From the KCWI data we measure a source redshift of z = 0.406. Using data from the Dark Energy Spectroscopic Instrument (DESI) we measure a velocity dispersion for the lens galaxy of σ∗ = 303 ± 15 km s-1. We model the lens galaxy light in detail, revealing angular structure that varies inside the Einstein ring. After subtracting this light model from the VIS observation, we model the strongly lensed images, finding an Einstein radius of 2.″5, corresponding to 2.1 kpc at the redshift of the lens. This is small compared to the effective radius of the galaxy, Reff ∼ 12.″3. Combining the strong lensing measurements with analysis of the spectroscopic data we estimate a dark matter fraction inside the Einstein radius of fDM = (11.1-3.5+5.4)% and a stellar initial mass-function (IMF) mismatch parameter of αIMF = 1.26-0.08+0.05, indicating a heavier-than-Chabrier IMF in the centre of the galaxy.
Volume: 694
Keywords: Galaxies: individual: NGC 6505; Gravitational lensing: strong; Surveys;
Subtype distribution, clinical presentation, and molecular spectrum of neurofibromatosis type 1-associated breast cancer
Authors: Di Giosaffatte Niccolo; Daniele Paola; Petrizzelli Francesco; Iacovino Chiara; Canciani Chiara; Garau Maria Luisa; Santoro Claudia; Trevisan Valentina; Panfili Arianna; Cavone Stefania; Guida Valentina; D'asdia Maria Cecilia; Bernardini Laura; Majoreb Silvia; Ferraris Alessandro; Valiante Michele; Gensini Francesca; Radio Francesca Clementina; Tortorai Giada; Cassinae Matteo; Mielej Giuseppina; Priolok Manuela; Sirchial Fabio; Piccinno Ludovica; Flex Elisabetta; Zampino Giuseppe; Genuardi Maurizio; Nigro Vincenzo; Salviati Leonardo; Papi Laura; Grammatico Paola; Leoni Chiara; Piluso Giulio; Giustini Sandra; Mazza Tommaso; Upadhyaya Meena; Tartaglia Marco; Trevisson Eva; De Luca Alessandro; Di Giosaffatte Niccolò; D'Asdia Maria Cecilia; Majore Silvia; Tortora Giada; Cassina Matteo; Miele Giuseppina; Priolo Manuela; Sirchia Fabio
Journal: BREAST
Published: 2025
DOI: 10.1016/j.breast.2025.104618
Aim: To investigate clinical and molecular features of neurofibromatosis type 1 (NF1)-associated breast cancer (BC) in a large multicenter cohort. Methods: Clinical and histopathological data from 86 NF1 patients with BC (69 with molecular data) were collected, and 111 published cases were reviewed. NF1 variants were assessed in silico, and their distribution across neurofibromin domains was compared with the general NF1 population. Results: NF1 patients developed BC earlier than the general population (mean 49 years), with missense variant heterozygotes showing the earliest onset (43.9 vs. 49.5 years for truncating variants, p = 0.014). Tumors were frequently high-grade (49 %), HER2-enriched (31 %) or luminal B subtypes (31 %), with reduced luminal A (28 %) frequency. NF1+BC patients had more subcutaneous (p = 0.006) and plexiform neurofibromas (p 70 % of variants, with proline/arginine substitutions accounting for 83 % of missense variants (vs. 44 % in the general NF1 population, p = 0.0012). Conclusions: NF1-associated BC is characterized by earlier onset, aggressive tumor features, and distinct mutational patterns.
Volume: 84
Keywords: Breast cancer; Cancer predisposition; Dominant negative effect; Genotype-phenotype correlation; Neurofibromatosis type 1; Neurofibromin; NF1; Surveillance;
Lithologies of Dimorphos revealed by boulder morphological classes
Authors: Tusberti F.; Pajola M.; Penasa L.; Lucchetti A.; Massironi M.; Munaretto G.; Beccarelli J.; Pozzobon R.; Rossi C.; Poggiali G.; Murdoch N.; Robin C. Q.; Duchene A.; Amoroso M.; Bertini I.; Brucato J. R.; Capannolo A.; Caporali S.; Ceresoli M.; Cremonese G.; Dall'Ora M.; Della Corte V.; Deshapriya J. D. P.; Dotto E.; Epifani E. Mazzotta; Gai I.; Gramigna E.; Hasselmann P. H. A.; Ieva S.; Impresario G.; Ivanovski S.; Manghi R. Lasagni; Lavagna M.; Lombardo M.; Modenini D.; Palumbo P.; Perna D.; Pirrotta S.; Rossi A.; Tortora P.; Zannoni M.; Zanotti G.; Zinzi A.; Buratti B.; Trigo-Rodrigez J. M.; Casajus L. Gomez; Robin C.Q.; Brucato J.R.; Corte V. Della; Deshapriya J.D.P.; Hasselmann P.H.A.; Trigo-Rodrigez J.M.
Journal: ICARUS
Published: 2025
DOI: 10.1016/j.icarus.2025.116744
The stony/Sq-type binary system (65803) Didymos consists of two rubble pile bodies, Didymos, the primary, and its moonlet Dimorphos. In 2022, the first planetary defense mission Double Asteroid Redirection Test (DART) reached Dimorphos and collected unprecedented high-resolution images of its surface. They revealed a variegated surface completely covered by stacked boulders and cobbles with different shapes and textures. Their morphological heterogeneity likely reflects the lithologies originally present within the Didymos and Dimorphos’ parent body, before its fragmentation. We present a lithologic study of Dimorphos’ surface, based on a morphological analysis of its boulders. Our approach considers each boulder’s 2D outline, perceived 3D shape, and surface texture characteristics. Based on these features, we identified two main morphological classes. A total of 178 boulders were classified as Angular morphology covering 38.5 % of the mapped area. This type is characterized by cohesive boulders with straight and angular outlines as well as sharp three-dimensional edges, which form well-defined sub-planar facets. Additionally, the texture of this kind of rocks show low-to-mid Roughness and the presence of lineations on some boulders. On the other hand, 210 boulders were categorized as Hummocky morphology, which covers 61.5 % of the area. Such morphology appears more friable and features boulders with rounded shaped and ragged and irregular 2D perimeter. Their 3D perceived shape appears as flat-to-curve, with rough and hummocky surface textures due to embedded clasts. We interpret the Hummocky morphology as breccia lithology. On the other hand, although Angular morphology can be associated with multiple potential lithologies, we interpret it as either an achondritic/igneous lithology or a highly metamorphosed chondritic lithology. The breccias are likely characteristic of the parent body’s outer layers, actively involved in impact and sedimentary processes. Conversely, the lithologies associated with the An morphology should represent deeper regions of the plantesimal, possibly exhumed by impacts. All these results will be further complemented by data from the Hera mission, which will arrive at (65803) Didymos system at the end of 2026.
Volume: 442
Keywords: Asteroids; Geological processes; Near-Earth objects; Satellites of asteroids; Surfaces;
Hepatitis C Eradication Improves Oncologic and Clinical Outcomes in Patients Treated With Atezolizumab Plus Bevacizumab
Authors: Stella Leonardo; Cabibbo Giuseppe; Celsa Ciro; Ciccia Roberta; Sparacino Alba; Piscaglia Fabio; Tovoli Francesco; Arleo Andrea; Stefanini Bernardo; Iavarone Massimo; D'Ambrosio Roberta; Cerrito Lucia; Pallozzi Maria; Santopaolo Francesco; Marra Fabio; Campani Claudia; Mazzarelli Chiara; Vigano Raffaella; Tortora Raffaella; Aghemo Alessio; Nicola Stella De; Pressiani Tiziana; Rimassa Lorenza; Bhoori Sherrie; Corallo Salvatore; Maiocchi Laura; Martini Andrea; Solda Caterina; Russo Francesco Paolo; Gasbarrini Antonio; Ponziani Francesca Romana; Viganò Raffaella; Soldà Caterina
Journal: LIVER INTERNATIONAL
Published: 2025
DOI: 10.1111/liv.70362
Background and Aims: Hepatitis C virus (HCV) is a key driver of hepatocellular carcinoma (HCC). However, the impact of HCV eradication on systemic therapy remains unclear. We aimed to assess the safety and efficacy of direct-acting antivirals (DAA) in patients treated with Atezolizumab plus Bevacizumab (AtezoBev). Methods: This retrospective multicentre study included patients with HCV-related unresectable/advanced HCC treated with AtezoBev between 2021 and 2024. Three groups of patients were compared: Group A (n = 22), concurrent DAA with AtezoBev; Group B (n = 95), antiviral therapy before AtezoBev; and Group C (n = 22), active infection. Results: Group A showed the longest median overall survival (42.8 months) compared to Group B (26.8 months; p = 0.03) and Group C (19.7 months; p = 0.01). Time to progression and progression-free survival were significantly prolonged in Group A versus Groups B and C. Moreover, Group A exhibited a higher disease control rate than the other groups. Post-DAA decompensation rates were significantly lower in Group A (4.5%) compared to Groups B (26.3%) and C (36.4%). Treatment-related adverse events of grade ≥ 3 were similar across groups. In the multivariate competing risk analysis with adjustment for time-dependent variables, achieving sustained virologic response during AtezoBev showed a protective effect against liver decompensation (sHR 0.02, p = 0.003) or tumour progression (sHR 0.14, p = 0.009), and was also associated with reduced mortality (HR 0.29, p = 0.005). Conclusions: Achieving a SVR during AtezoBev seems to improve oncologic outcomes and reduce liver decompensation in patients with unresectable/advanced HCC. An integrated therapeutic approach can optimise systemic treatment efficacy, particularly in patients eligible for conversion strategies. Trial Registration: Protocol ID: 5890.
Volume: 45
Keywords: cirrhosis; DAA; HCV; hepatocellular carcinoma; immunotherapy; liver decompensation; survival;
From simulations to observations: Methodology and data release of mock TNG50 galaxies at 0.3 < z < 0.7 for WEAVE-StePS
Authors: Ikhsanova A.; Costantin L.; Pizzella A.; Corsini E. M.; Morelli L.; Ditrani F. R.; Ferre-Mateu A.; Gabarra L.; Gullieuszik M.; Haines C. P.; Iovino A.; Longhetti M.; Mercurio A.; Ragusa R.; Sanchez-Blazquez P.; Tortora C.; Vulcani B.; Zhou S.; Gafton E.; Pistis F.
Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202555132
Volume: 703
Euclid: Early Release Observations – Globular clusters in the Fornax galaxy cluster, from dwarf galaxies to the intracluster field
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; GEH-7593-2022; GDB-0545-2022; GDD-0521-2022; J-4088-2012; HEO-6319-2022; DWB-0787-2022; GCT-4656-2022; DVE-7652-2022; AAK-8191-2020; GBG-9412-2022; DTQ-3078-2022; DWO-2405-2022; EVW-7270-2022; GFK-2340-2022; OOP-8239-2025; DAV-8065-2022; MSI-3188-2025; LXV-7382-2024; B-9633-2012; KPF-2019-2024; GFH-0803-2022; LTE-2549-2024; GNE-1283-2022; ABB-9156-2021; GBC-8404-2022; PGU-9738-2026; O-9495-2015; B-4348-2013; HQE-3410-2023; AFS-1680-2022; QGM-4004-2026; JCO-0131-2023; EYY-4006-2022; DXA-1243-2022; LBZ-7918-2024; ISA-3008-2023; DXL-4304-2022; MDQ-9712-2025; I-6648-2019; DYF-3433-2022; H-4394-2019; EDW-5764-2022; Z-4828-2019; JHF-8266-2023; FQI-9285-2022; AAV-1857-2021; EJM-8740-2022; FZO-1254-2022; FYJ-9637-2022; DUY-3094-2022; C-4378-2014; EKA-7986-2022; IUT-7926-2023; LXX-3952-2024; GBF-1843-2022; DVB-2560-2022; L-8385-2017; OBC-0525-2025; LUN-9319-2024; HWT-5982-2023; GBO-0318-2022; E-2727-2014; L-8237-2014; FZR-9687-2022; IVA-4275-2023; B-4650-2017; IRQ-6937-2023; H-8587-2015; DVC-6323-2022; NHE-3385-2025; PGG-2427-2026; AGZ-3259-2022; FZL-7353-2022; A-2693-2010; PCA-2324-2025; HLX-2021-2023; HKB-2933-2023; EUO-2530-2022; EUK-3820-2022; J-3686-2012; COQ-7299-2022; CPC-6980-2022; AAR-6622-2021; CQF-5798-2022; I-5515-2016; DXA-1952-2022; HPT-5858-2023; JWF-2506-2024; GBB-1832-2022; DWB-6758-2022; GQH-6424-2022; CQR-5759-2022; DWK-1716-2022; JGR-4365-2023; GAX-2002-2022; CTE-6775-2022; CSK-3817-2022; CUA-0149-2022; FBF-5584-2022; EYM-5386-2022; HRW-8595-2023; FBV-0790-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; DWQ-9372-2022; AAT-5867-2020; DWS-1040-2022; DXH-0671-2022; FFG-2233-2022; FGD-1080-2022; DAV-9216-2022; CYT-5449-2022; AAF-6025-2021; DUU-4676-2022; B-8502-2016; FIF-2657-2022; LYD-9061-2024; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; DFQ-7859-2022; DFY-8508-2022; MWK-2416-2025; AAX-3485-2021; D-1300-2016; FNO-5530-2022; AAA-1489-2019; GNG-7078-2022; FNC-4379-2022; DFC-8070-2022; FLD-9518-2022; MWC-3186-2025; FNA-5485-2022; KJY-7272-2024; DWT-4779-2022; KSI-9422-2024; KNP-2716-2024; MNN-0179-2025; FNB-0821-2022; C-3218-2017; HTJ-4919-2023; DWD-4131-2022; DLB-6897-2022; HTM-1531-2023; GBD-7573-2022; DMG-4306-2022; FVO-0175-2022; FSY-2184-2022; DMX-5934-2022; ABC-8644-2021; FSO-8783-2022; DNY-0415-2022; OWQ-1639-2025; PIF-6131-2026; K-4114-2015; OON-3882-2025; DNW-6364-2022; GCA-5113-2022; GCT-2940-2022; DXO-8435-2022; H-1761-2016; DXM-5348-2022; DPD-7597-2022; FZX-9985-2022; IZJ-2041-2023; GBV-4959-2022; GWX-9207-2022; FZJ-5145-2022; NGE-0152-2025; EAA-4768-2022; L-8068-2014; MQB-6975-2025; DZM-7523-2022; GDK-6495-2022; T-7378-2018; AAB-2503-2019; KLN-4310-2024; GCB-5227-2022; DYT-7473-2022; HNI-8187-2023; GCA-5567-2022; FCD-8153-2022; AAC-2083-2020; NKT-4492-2025; MTT-8732-2025; OZU-7134-2025; EAZ-0566-2022; O-9396-2015; AAO-6325-2021; DTO-7937-2022; FVK-3262-2022; JCM-8241-2023; CEX-0810-2022; NBS-6714-2025; 57204700965; 57103783400; 6701673913; 10042256200; 57195321311; 7003267532; 7402297037; 35494536400; 57188565951; 8833942000; 6603186973; 7004293616; 7402054273; 55538241000; 56216916000; 7003825248; 56592660200; 6603351766; 7006440295; 57193617511; 6603939854; 18838264600; 57545939600; 57202215260; 6701409861; 56261663500; 6602409206; 7003910265; 7102219947; 56925206200; 7404584619; 57194407496; 36663730200; 57192921002; 59170382200; 55337098600; 57190443165; 9533992100; 57339831000; 57206423651; 55929371000; 57374950500; 7005317106; 6506425834; 7102775303; 57193523315; 6701390827; 14629998500; 56176939800; 8651648800; 24482926400; 6505819655; 57225389323; 58849865400; 7102960752; 6602293713; 6701447926; 7004168457; 7004279376; 35117442400; 56592859600; 8316050500; 57193414472; 57090221700; 24439181000; 54924573500; 56260193000; 37121732700; 6507398813; 55757270100; 8856476200; 59636105400; 7004529134; 26663174300; 6603213706; 7006071419; 57212263363; 6506323808; 6601991850; 6602678698; 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Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202450784
We present an analysis of Euclid observations of a 0.6 deg2 field in the central region of the Fornax galaxy cluster that were acquired during the performance verification phase. With these data, we investigated the potential of Euclid to identify globular clusters (GCs) at 20 Mpc and validated the search methods using artificial GCs and known GCs within the field from the literature. Our analysis of artificial GCs injected into the data shows that Euclid’s data in the IE band is 80% complete at about IE ∼ 26.0 mag (MV ∼ -5.0 mag), and it resolves GCs as small as rh = 2.5 pc. In the IE band, we detected more than 95% of the known GCs from previous spectroscopic surveys and GC candidates of the ACS Fornax Cluster Survey, of which more than 80% are resolved. We identify more than 5000 new GC candidates within the field of view down to IE = 25.0 mag, about 1.5 mag fainter than the typical GC luminosity function turn-over magnitude, and we investigated their spatial distribution within the intracluster field. We then focused on the GC candidates around dwarf galaxies and investigated their numbers, stacked luminosity distribution, and stacked radial distribution. While the overall GC properties are consistent with those in the literature, we found an interesting over-representation of relatively bright candidates within a small number of relatively GC-rich dwarf galaxies. Our work confirms the capabilities of Euclid data in detecting GCs and separating them from foreground and background contaminants at a distance of 20 Mpc, particularly for low GC-count systems such as dwarf galaxies.
Volume: 697
Keywords: galaxies: clusters: individual: Fornax; galaxies: clusters: intracluster medium; galaxies: dwarf; galaxies: star clusters: general; methods: observational;
Euclid: Early Release Observations – Dwarf galaxies in the Perseus galaxy cluster
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; DVE-7652-2022; DWB-0787-2022; ABB-2950-2020; DTQ-3078-2022; DWO-2405-2022; JCO-0131-2023; GFK-2340-2022; DYO-3408-2022; FPW-4436-2022; MDH-6494-2025; KPF-2019-2024; GEH-7593-2022; LTE-2549-2024; I-6648-2019; GNE-1283-2022; LPM-0745-2024; O-9495-2015; GDD-0521-2022; DAV-8065-2022; MSI-3188-2025; GBG-9412-2022; DYF-3433-2022; HTB-3700-2023; ABE-1497-2020; FZK-6500-2022; DXA-1243-2022; AAH-3277-2019; GBG-8291-2022; H-4394-2019; AAK-8191-2020; DTZ-1231-2022; EJM-8740-2022; FZO-1254-2022; FYJ-9637-2022; DUY-3094-2022; CEY-5520-2022; C-4378-2014; EKA-7986-2022; IUT-7926-2023; IUQ-9509-2023; GBF-1843-2022; EKV-4052-2022; L-8385-2017; OBC-0525-2025; LUN-9319-2024; DVP-6438-2022; CJL-9982-2022; GBO-0318-2022; E-2727-2014; L-8237-2014; FZR-9687-2022; IVA-4275-2023; B-4650-2017; IRQ-6937-2023; H-8587-2015; B-4348-2013; DVC-6323-2022; HQF-6437-2023; PGG-2427-2026; AGZ-3259-2022; FZL-7353-2022; A-2693-2010; PCA-2324-2025; CNE-2384-2022; HLX-2021-2023; HKB-2933-2023; PWI-2374-2026; LZM-1403-2025; EUK-3820-2022; J-3686-2012; CNP-7538-2022; CPC-6980-2022; AAR-6622-2021; CQF-5798-2022; I-5515-2016; KLD-3528-2024; DXA-1952-2022; HPT-5858-2023; JWF-2506-2024; GBB-1832-2022; DWB-6758-2022; GWP-3456-2022; GQH-6424-2022; CQR-5759-2022; DWK-1716-2022; JGR-4365-2023; CTE-6775-2022; CSK-3817-2022; CUA-0149-2022; FCZ-2066-2022; FBF-5584-2022; EYM-5386-2022; HRW-8595-2023; FBV-0790-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; NRV-3859-2025; EYY-4006-2022; DWQ-9372-2022; AAT-5867-2020; DWS-1040-2022; DXH-0671-2022; FFG-2233-2022; FGD-1080-2022; DAV-9216-2022; CYT-5449-2022; AAF-6025-2021; OOP-8239-2025; DUU-4676-2022; B-8502-2016; HXO-8043-2023; LYD-9061-2024; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; DFQ-7859-2022; DFY-8508-2022; MWK-2416-2025; AAX-3485-2021; D-1300-2016; FNO-5530-2022; AAA-1489-2019; GNG-7078-2022; FNC-4379-2022; FLD-9518-2022; MWC-3186-2025; DVP-3997-2022; FNA-5485-2022; AAW-4410-2021; DWT-4779-2022; KSI-9422-2024; KNP-2716-2024; MNN-0179-2025; HXJ-7641-2023; C-3218-2017; HTJ-4919-2023; DWD-4131-2022; DLB-6897-2022; HTM-1531-2023; GBD-7573-2022; DMG-4306-2022; FVO-0175-2022; FSY-2184-2022; DMX-5934-2022; ABC-8644-2021; DNY-0415-2022; OWQ-1639-2025; PIF-6131-2026; K-4114-2015; OON-3882-2025; DNW-6364-2022; DNY-1328-2022; DXL-4304-2022; GCA-5113-2022; GCT-2940-2022; DXO-8435-2022; H-1761-2016; KCY-7756-2024; DPD-7597-2022; IZJ-2041-2023; GBV-4959-2022; DZW-2293-2022; GWX-9207-2022; FZJ-5145-2022; NGE-0152-2025; EAA-4768-2022; L-8068-2014; MQB-6975-2025; DZM-7523-2022; GDK-6495-2022; T-7378-2018; KLN-4310-2024; GCB-5227-2022; DYT-7473-2022; HNI-8187-2023; GCA-5567-2022; EFN-6430-2022; AAC-2083-2020; NRT-6530-2025; MTT-8732-2025; OZU-7134-2025; EAZ-0566-2022; O-9396-2015; AAO-6325-2021; DTO-7937-2022; FVK-3262-2022; DYK-4428-2022; JCM-8241-2023; FQI-9285-2022; JHF-8266-2023; NBS-6714-2025; 35494536400; 7003267532; 10042256200; 6603186973; 7004293616; 57194407496; 55538241000; 57204347252; 57371578400; 59165454500; 57193617511; 57204700965; 18838264600; 57339831000; 57545939600; 57771359400; 6602409206; 6701673913; 7003825248; 56592660200; 8833942000; 57206423651; 7005899939; 55178467000; 8970939400; 57192921002; 55798914200; 55365150900; 55929371000; 57188565951; 57113716800; 6701390827; 14629998500; 56176939800; 8651648800; 57220414927; 24482926400; 6505819655; 57225389323; 35421870300; 7102960752; 6506892241; 6701447926; 7004168457; 7004279376; 35117442400; 26537052300; 56592859600; 8316050500; 57193414472; 57090221700; 24439181000; 54924573500; 56260193000; 37121732700; 7003910265; 6507398813; 55757270100; 8856476200; 59636105400; 7004529134; 26663174300; 6603213706; 6602521535; 7006071419; 57212263363; 6701702242; 55978579700; 6601991850; 6602678698; 57198386027; 56181792800; 57200514857; 9639653200; 6701688696; 36627225700; 6506341877; 56592156500; 24173378000; 14630273900; 56261365400; 57206536839; 8724245000; 36657273100; 8527480900; 57203599140; 9270789600; 14008117700; 9337191600; 16028244600; 6603519641; 10240830400; 7102513091; 7202555066; 7006022077; 16024707000; 6603380199; 59834471800; 36663730200; 55539553700; 35425530800; 55885669700; 35227493200; 37123976000; 8899520500; 6506922416; 55578049300; 7003478641; 56216916000; 7102120605; 6603602446; 7005760971; 6603623670; 6603205767; 6603770482; 56403356600; 36195926600; 14058603600; 10239419900; 14025617800; 6506385309; 36933808800; 55779479900; 13407562800; 7102174334; 56229506700; 8058520300; 14056466700; 7102846243; 55665939900; 7005525798; 14832846900; 7004208543; 35299820900; 7004629002; 55668172300; 8764087600; 7006833728; 14050522100; 58095754900; 57203234808; 55913343900; 57544565000; 7003604949; 57203250534; 15770290900; 6602930238; 57190439701; 7006538931; 8842216700; 6506955003; 36490343100; 7004336793; 55337191500; 7402364894; 57225899623; 35350466600; 57190443165; 8915699600; 6603819159; 7004160690; 15129157800; 9533992100; 57218941481; 14063887300; 54797318800; 6701484532; 55845420026; 6602208520; 6602315420; 14823864100; 57220082325; 55414427600; 35314080800; 58937209900; 17436196900; 57194416363; 57191960842; 6701439004; 6602565951; 57191419742; 59019204600; 56286395400; 10244106400; 7101771030; 7102717554; 8042894900; 9333441800; 7004185737; 6603819488; 56512377200; 7003963996; 55435714500; 7102775303; 6506425834; 7404952697
Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202450799
We make use of the unprecedented depth, spatial resolution, and field of view of the Euclid Early Release Observations (EROs) of the Perseus galaxy cluster to detect and characterise the dwarf galaxy population in this massive system. Using a dedicated annotation tool, the Euclid high-resolution VIS and combined VIS+Near Infrared Spectrometer and Photometer (NISP) colour images were visually inspected and dwarf galaxy candidates were identified. Their morphologies, the presence of nuclei, and their globular cluster (GC) richness were visually assessed richness were visually assessed, complementing an automatic detection of the GC candidates. Structural and photometric parameters, including Euclid filter colours, were extracted from two-dimensional fitting. Based on this analysis, a total of 1100 dwarf candidates were found across the image; 606 of these appear to be new identifications. The majority (96%) are classified as dwarf ellipticals, 53% are nucleated, 26% are GC-rich, and 6% show disturbed morphologies. A relatively high fraction of galaxies, 8%, are categorised as ultra diffuse galaxies. The majority of the dwarfs follow the expected scaling relations of galaxies. Globally, the GC specific frequency, SN, of the Perseus dwarf candidates is intermediate between those measured in the Virgo and Coma clusters. While the dwarf candidates with the largest GC counts are found throughout the Euclid field of view, the dwarfs located around the east–west strip, where most of the brightest cluster members are found, exhibit higher SN values on average. The spatial distribution of the dwarfs, GCs, and intracluster light show a main iso-density and isophotal centre displaced to the west of the bright galaxy light distribution. The ERO imaging of the Perseus cluster demonstrates the unique capability of Euclid to concurrently detect and characterise large samples of dwarf galaxies, their nuclei, and their GC systems, allowing us to construct a detailed picture of the formation and evolution of galaxies over a wide range of mass scales and environments.
Volume: 697
Keywords: galaxies: clusters: general; galaxies: clusters: individual: Abell 426; galaxies: dwarf; galaxies: fundamental parameters; galaxies: nuclei; galaxies: star clusters: general;
Euclid: Early Release Observations – Programme overview and pipeline for compact- and diffuse-emission photometry
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; DWB-0787-2022; AAU-1020-2020; O-9495-2015; H-2913-2012; FZO-2634-2022; CUZ-3547-2022; DXA-1243-2022; DVI-4148-2022; GDD-0521-2022; FGC-9351-2022; FKB-6410-2022; GEH-7593-2022; GBG-9412-2022; DYF-3433-2022; ABB-9156-2021; EJM-8740-2022; GBC-8404-2022; GAQ-2193-2022; FZP-9853-2022; HPI-3723-2023; PGU-9738-2026; GCA-0669-2022; C-1439-2017; DUU-1945-2022; MKJ-9958-2025; HTB-3700-2023; K-1263-2013; MCF-4404-2025; HIK-2775-2022; CJO-3675-2022; K-9464-2019; ABB-2950-2020; DTQ-3078-2022; FYQ-3698-2022; CLX-1205-2022; H-8587-2015; DWH-0490-2022; MOZ-1236-2025; U-6390-2019; I-2511-2015; AFS-1680-2022; HKB-2933-2023; IDQ-0489-2023; DWO-2405-2022; JLC-7108-2023; LNV-3966-2024; EVW-7270-2022; ABE-1497-2020; GMD-3106-2022; DWU-8294-2022; GWP-3456-2022; GQH-6424-2022; DTZ-1231-2022; FZX-7187-2022; QGM-4004-2026; JCO-0131-2023; PMS-5356-2026; FZK-6500-2022; DAV-9216-2022; FDX-5194-2022; MPG-4199-2025; GFK-2340-2022; DYO-3408-2022; B-1966-2015; NLL-4796-2025; Z-4828-2019; A-7919-2015; NKY-6883-2025; GCT-0363-2022; GCT-4656-2022; MSI-3188-2025; JHF-8266-2023; GBI-4899-2022; DVE-7652-2022; KBO-4868-2024; ISA-3008-2023; HVT-6155-2023; MWC-3186-2025; FMN-9310-2022; JGB-4169-2023; FMT-8159-2022; MDH-6494-2025; AAH-3277-2019; FQI-9285-2022; PCC-0635-2025; IRR-1266-2023; IFW-1485-2023; LXV-7382-2024; AFN-4775-2022; C-6230-2011; B-9633-2012; KPF-2019-2024; MQV-6996-2025; FSO-8783-2022; GFH-0803-2022; OON-3882-2025; DWT-7233-2022; AAV-1857-2021; IHL-1858-2023; DQP-5038-2022; MDQ-9712-2025; GFN-2673-2022; AAN-1908-2021; I-6648-2019; GBG-8291-2022; DZW-2642-2022; GDK-6495-2022; JEZ-2766-2023; H-4394-2019; GNE-1283-2022; AAK-8191-2020; GDB-0545-2022; DXW-9679-2022; NKW-7334-2025; DYZ-0102-2022; LPM-0745-2024; FYJ-9637-2022; DUY-3094-2022; CEY-5520-2022; C-4378-2014; EKA-7986-2022; IUT-7926-2023; LXX-3952-2024; GBF-1843-2022; EKV-4052-2022; L-8385-2017; HPR-3987-2023; OBC-0525-2025; LUN-9319-2024; HWT-5982-2023; GBO-0318-2022; E-2727-2014; L-8237-2014; FZR-9687-2022; E-8021-2017; IVA-4275-2023; B-4650-2017; GBS-0220-2022; B-4348-2013; DVC-6323-2022; NHE-3385-2025; PGG-2427-2026; AGZ-3259-2022; FZL-7353-2022; PCU-7129-2025; A-2693-2010; PCA-2324-2025; HLX-2021-2023; PWI-2374-2026; ETL-7525-2022; EUK-3820-2022; J-3686-2012; COQ-7299-2022; CPC-6980-2022; AAR-6622-2021; CQF-5798-2022; I-5515-2016; KLD-3528-2024; DXA-1952-2022; HPT-5858-2023; GBB-1832-2022; DWB-6758-2022; CQR-5759-2022; DWK-1716-2022; JGR-4365-2023; CTE-6775-2022; CSK-3817-2022; CUA-0149-2022; FBF-5584-2022; EYM-5386-2022; HRW-8595-2023; FBV-0790-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; EYY-4006-2022; DWQ-9372-2022; AAT-5867-2020; DWS-1040-2022; DXH-0671-2022; FFG-2233-2022; GEK-4486-2022; FGD-1080-2022; CYT-5449-2022; AAF-6025-2021; OOP-8239-2025; DUU-4676-2022; B-8502-2016; HXO-8043-2023; FIO-1016-2022; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; DFQ-7859-2022; DFY-8508-2022; MWK-2416-2025; AAX-3485-2021; D-1300-2016; FNO-5530-2022; AAA-1489-2019; GNG-7078-2022; FLD-9518-2022; FNA-5485-2022; DYJ-3666-2022; KJY-7272-2024; DWT-4779-2022; KSI-9422-2024; KNP-2716-2024; MNN-0179-2025; FNB-0821-2022; C-3218-2017; HTJ-4919-2023; DWD-4131-2022; GCU-3410-2022; DLB-6897-2022; HTM-1531-2023; GBD-7573-2022; DMG-4306-2022; FVO-0175-2022; FSY-2184-2022; DMX-5934-2022; ABC-8644-2021; DNY-0415-2022; OWQ-1639-2025; PIF-6131-2026; K-4114-2015; DNW-6364-2022; DNY-1328-2022; DXL-4304-2022; GCA-5113-2022; GCT-2940-2022; DXO-8435-2022; H-1761-2016; DPD-7597-2022; FZX-9985-2022; IZJ-2041-2023; GBV-4959-2022; GWX-9207-2022; JCM-8241-2023; FZJ-5145-2022; NGE-0152-2025; NES-1075-2025; EAA-4768-2022; L-8068-2014; MQB-6975-2025; DZM-7523-2022; T-7378-2018; KLN-4310-2024; GCB-5227-2022; DYT-7473-2022; HNI-8187-2023; GCA-5567-2022; FCD-8153-2022; NLB-2929-2025; MTT-8732-2025; OZU-7134-2025; EAZ-0566-2022; O-9396-2015; DTO-7937-2022; LYP-7992-2024; FVK-3262-2022; NKX-2133-2025; 7003267532; 7005656061; 6602409206; 10738797800; 6602694835; 6506574084; 57192921002; 7005650624; 6701673913; 24759134300; 7003825248; 57204700965; 8833942000; 57206423651; 57202215260; 6701390827; 6701409861; 55941325100; 24741117900; 57933367200; 56261663500; 43360923400; 57222476357; 57208282439; 9533050200; 7005899939; 6603023234; 25640885400; 54580577900; 35208084800; 36195346900; 10042256200; 6603186973; 55505051100; 25625949500; 37121732700; 17345214500; 6602294488; 7003369464; 7006314412; 56925206200; 57212263363; 6701458135; 7004293616; 24173404700; 58968725200; 7402054273; 55178467000; 57322480400; 7801607411; 57206536839; 8724245000; 57113716800; 7202465518; 7404584619; 57194407496; 24279354600; 8970939400; 59831166200; 59834521400; 59436781500; 55538241000; 57204347252; 35748664400; 59774401700; 7005317106; 26643339300; 6506922416; 57190981289; 7402297037; 56592660200; 6506425834; 55180620000; 35494536400; 57203581246; 55337098600; 6701526252; 7005525798; 55246080700; 57223766405; 26639654400; 59165454500; 55798914200; 7102775303; 56949991000; 57222903889; 59193037200; 6603351766; 23968339900; 55798121500; 7006440295; 57193617511; 58303888900; 55679398300; 6603939854; 7402364894; 55672552800; 57193523315; 58182594100; 57195543445; 9533992100; 57203229435; 7003485288; 57339831000; 55365150900; 57217929177; 58937209900; 7004109829; 55929371000; 57545939600; 57188565951; 57103783400; 57217789465; 55619297196; 55898905800; 57771359400; 56176939800; 8651648800; 57220414927; 24482926400; 6505819655; 57225389323; 58849865400; 7102960752; 6506892241; 6701447926; 6507116448; 7004168457; 7004279376; 35117442400; 56592859600; 8316050500; 57193414472; 57090221700; 7004614794; 24439181000; 54924573500; 56260193000; 7003910265; 6507398813; 55757270100; 8856476200; 59636105400; 7004529134; 6701734824; 26663174300; 6603213706; 7006071419; 6701702242; 55978579700; 6601991850; 6602678698; 24461026200; 56181792800; 57200514857; 9639653200; 6701688696; 36627225700; 6506341877; 56592156500; 14630273900; 56261365400; 36657273100; 8527480900; 57203599140; 9270789600; 14008117700; 9337191600; 6603519641; 10240830400; 7102513091; 7202555066; 7006022077; 16024707000; 6603380199; 36663730200; 55539553700; 35425530800; 55885669700; 35227493200; 37123976000; 6701865592; 8899520500; 55578049300; 7003478641; 56216916000; 7102120605; 6603602446; 7005760971; 6602251719; 6603205767; 6603770482; 56403356600; 36195926600; 14058603600; 10239419900; 14025617800; 6506385309; 36933808800; 55779479900; 13407562800; 7102174334; 56229506700; 8058520300; 14056466700; 55665939900; 7004208543; 7201701805; 35299820900; 7004629002; 55668172300; 8764087600; 7006833728; 14050522100; 58095754900; 57203234808; 55913343900; 55596380000; 57544565000; 7003604949; 57203250534; 15770290900; 6602930238; 57190439701; 7006538931; 8842216700; 6506955003; 36490343100; 7004336793; 55337191500; 57225899623; 35350466600; 57190443165; 8915699600; 6603819159; 7004160690; 15129157800; 57218941481; 13407890400; 14063887300; 54797318800; 55845420026; 55435714500; 6602208520; 6602315420; 35100980600; 14823864100; 57220082325; 55414427600; 35314080800; 17436196900; 57194416363; 57191960842; 6701439004; 6602565951; 57191419742; 59019204600; 10244106400; 7101771030; 7102717554; 8042894900; 9333441800; 6603819488; 58848684700; 56512377200; 7404952697
Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202450803
The Euclid Early Release Observations (ERO) showcase Euclid’s capabilities in advance of its main mission by targeting 17 astronomical objects, including galaxy clusters, nearby galaxies, globular clusters, and star-forming regions. A total of 24 hours of observing time was allocated in the early months of operation, and the scientific community was engaged through an early public data release. We describe the development of the ERO pipeline to create visually compelling images while simultaneously meeting the scientific demands within months of launch by leveraging a pragmatic data-driven development strategy. The pipeline’s key requirements are to preserve the image quality and to provide flux calibration and photometry for compact and extended sources. The pipeline’s five pillars are removal of instrumental signatures, astrometric calibration, photometric calibration, image stacking, and the production of science-ready catalogues for both the VIS and NISP instruments. We report a point spread function (PSF) with a full width at half maximum of 000 . 16 in the optical IE-band and 000 . 49 in the near-infrared (NIR) bands YE, JE, and HE. Our VIS mean absolute flux calibration is accurate to about 1%, and the accuracy is 10% for NISP due to a limited calibration set; both instruments have considerable colour terms for individual sources. The median depth is 25.3 and 23.2 AB mag with a signal-to-noise ratio (S/N) of ten for galaxies, while it is 27.1 and 24.5 AB mag at an S/N of five for point sources for VIS and NISP, respectively. Euclid’s ability to observe diffuse emission is exceptional due to its extended PSF nearly matching a pure diffraction halo, the best ever achieved by a wide-field high-resolution imaging telescope. Euclid offers unparalleled capabilities for exploring the low-surface brightness (LSB) Universe across all scales, providing high precision within a wide field of view (FoV), and opening a new observational window in the NIR. Median surface-brightness levels of 29.5 and 27.9, AB mag arcsec-2 are achieved for VIS and NISP, respectively, for detecting a 1000 × 1000 extended feature at the 1 σ level.
Volume: 697
Keywords: astrometry; catalogs; space vehicles: instruments; techniques: image processing; techniques: photometric;