IAS-LAB PUBLICATIONS
Euclid: Early Release Observations – The surface brightness and colour profiles of the far outskirts of galaxies in the Perseus cluster
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; MDH-6494-2025; CFE-6365-2022; DWB-0787-2022; FYQ-3698-2022; NAA-8765-2025; HZW-5449-2023; GBG-8291-2022; DXA-1243-2022; FZK-6500-2022; DVE-7652-2022; GBG-9412-2022; H-2913-2012; K-9464-2019; H-4394-2019; MQV-6996-2025; OVM-5938-2025; JYY-9592-2024; OAA-4277-2025; HRO-8503-2023; Z-4828-2019; EJM-8740-2022; FZO-1254-2022; FYJ-9637-2022; CEY-5520-2022; EKA-7986-2022; IUT-7926-2023; IUQ-9509-2023; AAO-6325-2021; L-8385-2017; JWI-9457-2024; LUN-9319-2024; HFL-6092-2022; E-2727-2014; IVA-4275-2023; EOV-3838-2022; B-4650-2017; IRQ-6937-2023; H-8587-2015; B-4348-2013; DVC-6323-2022; NHE-3385-2025; LEQ-1557-2024; AGZ-3259-2022; NKT-5952-2025; CNE-2384-2022; EUK-3820-2022; HPK-1894-2023; CPC-6980-2022; IBV-9243-2023; CQF-5798-2022; KLD-3528-2024; CQR-5759-2022; DWK-1716-2022; CSK-3817-2022; FBF-5584-2022; FBE-0351-2022; CTZ-4163-2022; GBH-2365-2022; DWQ-9372-2022; FBM-0217-2022; DWS-1040-2022; DXH-0671-2022; GEK-4486-2022; CYT-5449-2022; GWA-7849-2022; B-8502-2016; Q-5758-2017; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; HUJ-7899-2023; DFQ-7859-2022; V-6916-2017; GNG-7078-2022; FLD-9518-2022; DVP-3997-2022; KEK-6332-2024; DWT-4779-2022; HXJ-7641-2023; DKF-4281-2022; DWD-4131-2022; DLB-6897-2022; HTM-1531-2023; GBD-7573-2022; MTQ-2344-2025; FSY-2184-2022; DMX-5934-2022; ABC-8644-2021; K-4114-2015; DNW-6364-2022; DXL-4304-2022; DXO-8435-2022; NKY-6871-2025; IZJ-2041-2023; GWX-9207-2022; OWM-0849-2025; LGB-5701-2024; GDK-6495-2022; T-7378-2018; AAB-2503-2019; GCB-5227-2022; OAE-4195-2025; GCA-5567-2022; NZU-7226-2025; NHV-9369-2025; DZE-1995-2022; O-9396-2015; DTO-7937-2022; P-2194-2018; 59165454500; 6603023234; 7003267532; 55505051100; 57206423651; 6602409206; 55365150900; 57192921002; 8970939400; 35494536400; 8833942000; 10738797800; 36195346900; 55929371000; 58303888900; 57206536839; 56261663500; 57204700965; 58114843000; 7005317106; 6701390827; 14629998500; 56176939800; 57220414927; 6505819655; 57225389323; 35421870300; 7004185737; 6701447926; 7004168457; 7004279376; 56592859600; 8316050500; 24439181000; 55948641800; 54924573500; 56260193000; 37121732700; 7003910265; 6507398813; 55757270100; 8856476200; 59636105400; 7004529134; 6602521535; 6601991850; 24461026200; 56181792800; 24587025200; 9639653200; 36627225700; 36657273100; 8527480900; 14008117700; 6603519641; 7202555066; 16024707000; 6603380199; 55539553700; 35425530800; 55885669700; 35227493200; 6701865592; 55578049300; 56216916000; 6603602446; 56149076900; 6603205767; 6603770482; 56403356600; 36195926600; 14058603600; 10239419900; 14025617800; 57815020000; 6506385309; 56463558800; 14056466700; 55665939900; 14832846900; 7004208543; 7004629002; 14050522100; 58095754900; 55913343900; 57544565000; 7003604949; 57203250534; 15770290900; 57190439701; 7006538931; 8842216700; 55337191500; 57225899623; 57190443165; 7004160690; 57218941481; 14063887300; 55845420026; 6602208520; 58502049600; 58937209900; 17436196900; 57203391123; 57191960842; 6602565951; 57191419742; 59730206000; 7101771030; 7005350024; 9333441800; 6603819488; 56512377200
Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202554838
The Perseus field captured by Euclid as part of its Early Release Observations provides a unique opportunity to study cluster environment ranging from outskirts to dense regions. Leveraging unprecedented optical and near-infrared depths, we investigate the stellar structure of massive disc galaxies in this field. This study focuses on outer disc profiles, including simple exponential (Type I), down-bending break (Type II) and up-bending break (Type III) profiles, and their associated colour gradients, to trace late assembly processes across various environments. Type II profiles, though relatively rare in high dense environments, appear stabilised by internal mechanisms like bars and resonances, even within dense cluster cores. Simulations suggest that in dense environments, Type II profiles tend to evolve into Type I profiles over time. Type III profiles often exhibit small colour gradients beyond the break, hinting at older stellar populations, potentially due to radial migration or accretion events. We analyse correlations between galaxy mass, morphology, and profile types. Mass distributions show weak trends of decreasing mass from the centre to the outskirts of the Perseus cluster. Type III profiles become more prevalent, while Type I profiles decrease in lower-mass galaxies with cluster centric distance. Type I profiles dominate in spiral galaxies, while Type III profiles are more common in S0 galaxies. Type II profiles are consistently observed across all morphological types. While the limited sample size restricts statistical power, our findings shed light on the mechanisms shaping galaxy profiles in cluster environments. Future work should extend observations to the cluster outskirts to enhance statistical significance and explore looser environments. Additionally, 3D velocity maps are needed to achieve a non-projected view of galaxy positions, offering deeper insights into spatial distribution and dynamics.
Volume: 699
Keywords: galaxies: clusters: individual: Perseus; galaxies: evolution; galaxies: interactions; Galaxy: disk;
The Hera Space Mission in the Context of Small Near-Earth Asteroid Missions in the Past, Present and Future
Authors: Michel Patrick; Küppers Michael; Fitzsimmons Alan; Green Simon; Lazzarin Monica; Ulamec Stephan; Abell Paul; Sugita Seiji; Campo Bagatin Adriano; Carry Benoit; Charnoz Sébastien; de León Julia; Ferrari Fabio; Hérique Alain; Jutzi Martin; Karatekin Özgür; Kohout Tomas; Murdoch Naomi; Okada Tatsuaki; Palomba Ernesto; Pravec Petr; Raducan Sabina; Snodgrass Colin; Tortora Paolo; Vincent Jean-Baptiste; Wünnemann Kai
Journal: 28261
Published: 2025
DOI: 10.1007/s11214-025-01195-1
The Hera mission of the European Space Agency was launched successfully on October 7, 2024 and will perform the first rendezvous with a binary asteroid in fall 2026. It will measure in great detail the characteristics of the binary asteroid (65803) Didymos. This will include for the first time the interior of an asteroid, as well as the outcome of the impact of the NASA DART mission on the small moon, called Dimorphos; of the binary system. The first asteroid deflection test will thus be fully validated, enabling impact model extrapolations to other cases. Hera uses a unique architecture that includes for the first time a main spacecraft and two cubesats for deep space asteroid exploration. It takes place in the context of the golden age of asteroid exploration, with no less than 8 missions in development or already flying to asteroids and great successes of past missions, in particular the two recent asteroid sample return missions OSIRIS-REx by NASA and Hayabusa2 by JAXA. Up to now, all new asteroids visited by a spacecraft have generated great surprises, especially regarding their often counter-intuitive response to external actions, showing that we are still far from fully understanding the properties of these bodies in their low-gravity environment. By investigating and interacting with small asteroids, we should eventually be able to better understand and predict their properties as a function of common characteristics identified by ground-based observations. We are not there yet. In this paper, we present how Hera will contribute to this endeavor.
Volume: 221
Keywords: Asteroids; Binary asteroids; Planetary defense; Space mission;
Long-term effectiveness, safety, and liver stiffness dynamics of PBC treatment with obeticholic acid in real-world
Authors: AREA MIN. 06 - Scienze mediche; ITA; Goal 3: Good health and well-being###25122; EAE-4108-2022; AAB-7965-2019; GXH-0637-2022; ABA-7458-2022; AAM-5199-2020; GYG-3745-2022; DQA-3167-2022; EEZ-3131-2022; DWH-6622-2022; DJL-4541-2022; GDO-6870-2022; EPF-4015-2022; HXI-6162-2023; CER-4322-2022; EPL-8933-2022; CLX-8747-2022; R-6598-2016; CUO-7026-2022; CDG-6373-2022; EAA-0713-2022; CMD-8697-2022; HMC-6765-2023; DWO-5433-2022; EUY-7780-2022; OWZ-9517-2025; GJN-4882-2022; EPQ-0611-2022; CST-5700-2022; DGV-4842-2022; NOF-1514-2025; AAC-1949-2019; AAE-3161-2022; DVV-9362-2022; CFM-6817-2022; ELB-9576-2022; AAA-5759-2019; LFT-8668-2024; GNF-9719-2022; J-8600-2018; CEH-2506-2022; GDY-8839-2022; CGI-5783-2022; J-8463-2018; E-1120-2012; DBM-5248-2022; JHF-5645-2023; NCV-8425-2025; DTY-5484-2022; DXS-4726-2022; OUU-0112-2025; CJX-2082-2022; JCS-8414-2023; EPL-1215-2022; FSR-1611-2022; GVU-0673-2022; DWF-4268-2022; FIH-4311-2022; MUO-3257-2025; DPA-2383-2022; EQL-9934-2022; DQK-8599-2022; GBJ-7157-2022; GDZ-6667-2022; ORW-9434-2025; EQJ-1234-2022; FQB-6797-2022; MQU-5709-2025; K-4255-2019; FLO-9066-2022; ESJ-6426-2022; DKA-8928-2022; J-4394-2019; DZH-2825-2022; EIZ-6768-2022; DGZ-4325-2022; FUU-1830-2022; EMO-8688-2022; GPG-1122-2022; IAZ-8837-2023; AFM-2519-2022; PHG-8971-2026; KJQ-3800-2024; PFZ-5711-2026; GDC-3815-2022; JVS-9756-2024; DPL-3467-2022; CGZ-1469-2022; DTZ-5739-2022; LWM-3292-2024; DPL-0586-2022; GBB-8947-2022; GDJ-0380-2022; CDY-1662-2022; K-7706-2016; JCS-0572-2023; CEV-0715-2022; E-2565-2011; MYM-7264-2025; FQT-1261-2022; CWY-4285-2022; CFF-4678-2022; FZV-1726-2022; MNU-4399-2025; BBE-1333-2022
Journal: JHEP REPORTS
Published: 2025
DOI: 10.1016/j.jhepr.2025.101448
Volume: 7
The Economic Burden, Epidemiological Insights, and Treatment Patterns of Wilson’s Disease: A Real-World Study in Italy
Authors: Sciattella Paolo; Scortichini Matteo; Cazzagon Nora; Loudianos Georgios; Zuin Massimo; Battezzati Pier Maria; Maggiore Giuseppe; Grieco Antonio; Baglione Eugenio; Senzolo Marco; Mazza Silvia; Della Corte Claudia; Tortora Annalisa; Di Dato Fabiola; Matarazzo Margherita; Iorio Raffaele
Journal: DRUGS-REAL WORLD OUTCOMES
Published: 2025
DOI: 10.1007/s40801-025-00506-w
Volume: 12 Pages: 391-398
Euclid preparation: LXVIII. Extracting physical parameters from galaxies with machine learning
Authors: AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; KJS-6941-2024; PGU-9738-2026; C-9225-2017; KKS-3168-2024; JQO-3317-2023; ABB-9156-2021; HNI-9120-2023; O-9495-2015; H-4394-2019; MXW-4784-2025; B-4650-2017; B-4348-2013; AHB-3798-2022; GFK-2340-2022; FDK-8162-2022; AAY-1704-2020; Z-4828-2019; DVE-7652-2022; PCC-0635-2025; B-9633-2012; AAV-1857-2021; PHP-8037-2026; FXZ-5996-2022; GEH-7593-2022; OIQ-4966-2025; O-8727-2015; ETW-6961-2022; FZO-1254-2022; FYJ-9637-2022; CDR-2303-2022; CEY-5520-2022; C-4378-2014; IUT-7926-2023; IUQ-9509-2023; GBF-1843-2022; EKV-4052-2022; DVB-2560-2022; EOE-6462-2022; L-8385-2017; OBC-0525-2025; IAE-2305-2023; HWT-5982-2023; GBO-0318-2022; E-2727-2014; L-8237-2014; FZR-9687-2022; E-8021-2017; IVA-4275-2023; OZD-6988-2025; IRQ-6937-2023; HTG-8587-2023; H-8587-2015; DVC-6323-2022; NHE-3385-2025; PGG-2427-2026; AGZ-3259-2022; A-2693-2010; PCA-2324-2025; ERD-3189-2022; HLX-2021-2023; HKB-2933-2023; PWI-2374-2026; EUO-2530-2022; EUK-3820-2022; J-3686-2012; CNP-7538-2022; CPC-6980-2022; AAR-6622-2021; IBV-9243-2023; CQF-5798-2022; I-5515-2016; DXA-1952-2022; HPT-5858-2023; GBB-1832-2022; CQR-5759-2022; DWK-1716-2022; CTE-6775-2022; CSK-3817-2022; CUA-0149-2022; FBF-5584-2022; FBV-0790-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; DWQ-9372-2022; AAT-5867-2020; GZL-0460-2022; DWS-1040-2022; DXH-0671-2022; FFG-2233-2022; GEK-4486-2022; CYT-5449-2022; AAF-6025-2021; OOP-8239-2025; DUU-4676-2022; B-8502-2016; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLK-4707-2022; MTO-5925-2025; DWZ-6747-2022; HUJ-7899-2023; DFQ-7859-2022; DFY-8508-2022; U-7309-2018; MWK-2416-2025; AAX-3485-2021; D-1300-2016; GNG-7078-2022; FNC-4379-2022; DFC-8070-2022; FLD-9518-2022; MWC-3186-2025; DVP-3997-2022; FNA-5485-2022; KJY-7272-2024; DWT-4779-2022; FNB-0821-2022; ABB-2322-2020; C-3218-2017; HTJ-4919-2023; DWD-4131-2022; DLB-6897-2022; GBD-7573-2022; DMG-4306-2022; FVO-0175-2022; FSY-2184-2022; DMX-5934-2022; ABC-8644-2021; DNY-0415-2022; 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Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202453111
The Euclid mission is generating a vast amount of imaging data in four broadband filters at a high angular resolution. This data will allow for the detailed study of mass, metallicity, and stellar populations across galaxies that will constrain their formation and evolutionary pathways. Transforming the Euclid imaging for large samples of galaxies into maps of physical parameters in an efficient and reliable manner is an outstanding challenge. Here, we investigate the power and reliability of machine learning techniques to extract the distribution of physical parameters within well-resolved galaxies. We focus on estimating stellar mass surface density, mass-averaged stellar metallicity, and age. We generated noise-free synthetic high-resolution (100 pc × 100 pc) imaging data in the Euclid photometric bands for a set of 1154 galaxies from the TNG50 cosmological simulation. The images were generated with the SKIRT radiative transfer code, taking into account the complex 3D distribution of stellar populations and interstellar dust attenuation. We used a machine learning framework to map the idealised mock observational data to the physical parameters on a pixel-by-pixel basis. We find that stellar mass surface density can be accurately recovered with a ≤0.130 dex scatter. Conversely, stellar metallicity and age estimates are, as expected, less robust, but they still contain significant information that originates from underlying correlations at a sub-kiloparsec scales between stellar mass surface density and stellar population properties. As a corollary, we show that TNG50 follows a spatially resolved mass-metallicity relation that is consistent with observations. Due to its relatively low computational and time requirements, which has a time-frame of minutes without dedicated high performance computing infrastructure once it has been trained, our method allows for fast and robust estimates of the stellar mass surface density distributions of nearby galaxies from four-filter Euclid imaging data. Equivalent estimates of stellar population properties (stellar metallicity and age) are less robust but still hold value as first-order approximations across large samples.
Volume: 695
Keywords: Galaxies: general; Galaxies: photometry; Methods: statistical;
Euclid: The Early Release Observations Lens Search Experiment
Authors: Non assegn; AREA MIN. 02 - Scienze fisiche; ASTRONOMY & ASTROPHYSICS###0004-6361; CGD-2351-2022; JAX-2768-2023; CKU-5761-2022; H-4394-2019; DXZ-7810-2022; PGG-2427-2026; DWU-8294-2022; D-1237-2017; OMN-3792-2025; FYJ-4908-2022; EPI-1133-2022; AGZ-3259-2022; LHK-9354-2024; DVB-8405-2022; AFJ-2074-2022; MDG-9557-2025; GMD-3106-2022; ILM-3517-2023; GBU-8717-2022; DWQ-9372-2022; MYW-7907-2025; AAC-7835-2021; JBR-8488-2023; DUZ-7625-2022; MWC-3186-2025; F-3052-2014; PCC-0635-2025; LXV-7382-2024; HFV-0042-2022; GEI-1893-2022; FTV-5671-2022; DRO-1214-2022; FXH-0557-2022; AAN-1908-2021; IUS-5192-2023; DYG-8338-2022; GFN-8936-2022; NLB-5121-2025; GCJ-5104-2022; GCV-8309-2022; H-2913-2012; GCS-2631-2022; AAD-3011-2021; O-9495-2015; DWB-0787-2022; DXA-1243-2022; GEH-7593-2022; GBG-9412-2022; DYF-3433-2022; OTJ-2099-2025; FYH-4361-2022; L-2472-2017; FYH-7305-2022; MYL-2765-2025; NKL-3434-2025; MMS-5823-2025; FHL-5547-2022; DWN-4354-2022; MYS-2354-2025; JNB-1152-2023; IRI-1547-2023; EFH-6710-2022; GBC-8404-2022; FZO-1254-2022; FYJ-9637-2022; DUY-3094-2022; CEY-5520-2022; C-4378-2014; EKA-7986-2022; IUT-7926-2023; LXX-3952-2024; IUQ-9509-2023; GBF-1843-2022; DVB-2560-2022; L-8385-2017; OBC-0525-2025; LUN-9319-2024; CJD-7824-2022; HWT-5982-2023; CJL-9982-2022; GBO-0318-2022; E-2727-2014; L-8237-2014; FZR-9687-2022; IVA-4275-2023; OZD-6988-2025; B-4650-2017; IRQ-6937-2023; HTG-8587-2023; H-8587-2015; B-4348-2013; DVC-6323-2022; NHE-3385-2025; GBN-8818-2022; NKT-5952-2025; A-2693-2010; PCA-2324-2025; CNE-2384-2022; HKB-2933-2023; EUO-2530-2022; EUK-3820-2022; J-3686-2012; CPC-6980-2022; AAR-6622-2021; CQF-5798-2022; DXA-1952-2022; HPT-5858-2023; 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; FBF-5584-2022; HRW-8595-2023; FBV-0790-2022; S-8590-2017; CTZ-4163-2022; GBH-2365-2022; AAT-5867-2020; GZL-0460-2022; DWS-1040-2022; DXH-0671-2022; FFG-2233-2022; CYT-5449-2022; DUU-4676-2022; B-8502-2016; LYD-9061-2024; GFM-0308-2022; A-2699-2012; GAU-7672-2022; FIV-3763-2022; FLM-0394-2022; MTO-5925-2025; DWZ-6747-2022; HUJ-7899-2023; DFQ-7859-2022; U-7309-2018; MWK-2416-2025; AAX-3485-2021; D-1300-2016; GNG-7078-2022; DFC-8070-2022; FLD-9518-2022; DVP-3997-2022; FNA-5485-2022; KJY-7272-2024; DWT-4779-2022; KSI-9422-2024; KNP-2716-2024; DJO-8166-2022; MNN-0179-2025; FNB-0821-2022; ABB-2322-2020; 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; OYX-8116-2025; K-4114-2015; OON-3882-2025; DNW-6364-2022; DXL-4304-2022; GCA-5113-2022; GCT-2940-2022; DXO-8435-2022; JVJ-6571-2024; FXG-6905-2022; H-1761-2016; NKY-6871-2025; FZX-9985-2022; IZJ-2041-2023; GBV-4959-2022; GWX-9207-2022; FZJ-5145-2022; NGE-0152-2025; NES-1075-2025; EAA-4768-2022; LGB-5701-2024; L-8068-2014; PYK-2395-2026; MQB-6975-2025; Q-2220-2015; T-7378-2018; AAB-2503-2019; GCB-5227-2022; DYT-7473-2022; HNI-8187-2023; GCA-5567-2022; NLM-0551-2025; MTT-8732-2025; O-9396-2015; DTO-7937-2022; JMK-1133-2023; DYK-4428-2022; NLL-3428-2025; MNN-3541-2025; 58090912100; 57210265918; 55731742600; 55929371000; 58911394800; 8856476200; 7801607411; 7101983827; 58544914400; 57190942170; 6602458029; 59636105400; 59317606600; 55862177400; 55668778200; 59317261300; 57322480400; 57473067700; 7202097638; 55539553700; 57188806951; 36126412600; 57207846185; 57193489486; 7005525798; 6701593679; 56949991000; 6603351766; 56153006200; 57199319204; 55932248600; 22836264500; 57211567711; 7003485288; 13204971700; 12786945200; 7005244190; 7401938216; 55822387500; 57191290632; 10738797800; 8270263200; 57218513471; 6602409206; 7003267532; 57192921002; 57204700965; 8833942000; 57206423651; 57188639623; 57221950386; 55976971800; 57213830231; 7004666481; 57193558463; 57958980000; 57205730219; 6701685211; 58419113700; 58666622600; 58202351900; 57535859700; 6701409861; 14629998500; 56176939800; 8651648800; 57220414927; 24482926400; 6505819655; 57225389323; 58849865400; 35421870300; 7102960752; 6602293713; 6701447926; 7004168457; 7004279376; 55543112300; 35117442400; 26537052300; 56592859600; 8316050500; 57193414472; 57090221700; 24439181000; 55948641800; 54924573500; 56260193000; 55543336500; 37121732700; 7003910265; 6507398813; 55757270100; 56018146100; 7004529134; 26663174300; 6603213706; 6602521535; 57212263363; 6506323808; 6601991850; 6602678698; 56181792800; 57200514857; 9639653200; 6506341877; 56592156500; 14630273900; 56261365400; 57206536839; 8724245000; 36657273100; 8527480900; 57203599140; 9270789600; 14008117700; 9337191600; 6603519641; 7102513091; 7202555066; 7006022077; 16024707000; 6603380199; 35425530800; 23485209600; 55885669700; 35227493200; 37123976000; 55578049300; 7102120605; 6603602446; 6603623670; 6603205767; 6603770482; 56403356600; 36195926600; 35070066100; 10239419900; 14025617800; 57815020000; 6506385309; 56463558800; 55779479900; 13407562800; 7102174334; 14056466700; 36542679900; 55665939900; 14832846900; 7004208543; 35299820900; 7004629002; 55668172300; 8764087600; 35216145800; 7006833728; 14050522100; 56118600700; 58095754900; 57203234808; 55913343900; 57544565000; 7003604949; 57203250534; 15770290900; 6602930238; 57190439701; 7006538931; 8842216700; 6506955003; 36490343100; 55337191500; 7402364894; 57225899623; 57190443165; 8915699600; 6603819159; 7004160690; 57219119015; 56881732300; 15129157800; 57218941481; 13407890400; 14063887300; 54797318800; 55845420026; 6602208520; 6602315420; 35100980600; 14823864100; 58502049600; 57220082325; 54790157700; 55414427600; 58937209900; 17436196900; 57203391123; 57191960842; 6701439004; 6602565951; 57191419742; 10244106400; 7101771030; 9333441800; 6603819488; 56512377200; 7003963996; 7404952697; 25951796800
Journal: ASTRONOMY & ASTROPHYSICS
Published: 2025
DOI: 10.1051/0004-6361/202451868
We investigated the ability of the Euclid telescope to detect galaxy-scale gravitational lenses. To do so, we performed a systematic visual inspection of the 0.7 deg2 Euclid Early Release Observations data towards the Perseus cluster using both the high-resolution IE band and the lower-resolution YE, JE, and HE bands. Each extended source brighter than magnitude 23 in IE was inspected by 41 expert human classifiers. This amounts to 12 086 stamps of 1000 × 1000. We found 3 grade A and 13 grade B candidates. We assessed the validity of these 16 candidates by modelling them and checking that they are consistent with a single source lensed by a plausible mass distribution. Five of the candidates pass this check, five others are rejected by the modelling, and six are inconclusive. Extrapolating from the five successfully modelled candidates, we infer that the full 14 000 deg2 of the Euclid Wide Survey should contain 100 000+-7030000000 galaxy-galaxy lenses that are both discoverable through visual inspection and have valid lens models. This is consistent with theoretical forecasts of 170 000 discoverable galaxy-galaxy lenses in Euclid. Our five modelled lenses have Einstein radii in the range 000 . 68 < θE < 100 . 24, but their Einstein radius distribution is on the higher side when compared to theoretical forecasts. This suggests that our methodology is likely missing small-Einstein-radius systems. Whilst it is implausible to visually inspect the full Euclid dataset, our results corroborate the promise that Euclid will ultimately deliver a sample of around 105 galaxy-scale lenses.
Volume: 697
Keywords: galaxies: clusters: individual: Perseus; gravitational lensing: strong; methods: data analysis; methods: observational;
Accessible model predicts response in hormone receptor positive HER2 negative breast cancer receiving neoadjuvant chemotherapy
Authors: Mastrantoni Luca; Garufi Giovanna; Giordano Giulia; Maliziola Noemi; Di Monte Elena; Arcuri Giorgia; Frescura Valentina; Rotondi Angelachiara; Orlandi Armando; Carbognin Luisa; Palazzo Antonella; Miglietta Federica; Pontolillo Letizia; Fabi Alessandra; Gerratana Lorenzo; Pannunzio Sergio; Paris Ida; Pilotto Sara; Marazzi Fabio; Franco Antonio; Franceschini Gianluca; Dieci Maria Vittoria; Mazzeo Roberta; Puglisi Fabio; Guarneri Valentina; Milella Michele; Scambia Giovanni; Giannarelli Diana; Tortora Giampaolo; Bria Emilio
Journal: NPJ BREAST CANCER
Published: 2025
DOI: 10.1038/s41523-025-00727-w
Hormone receptor-positive/HER2-negative breast cancer (BC) is the most common subtype of BC and typically occurs as an early, operable disease. In patients receiving neoadjuvant chemotherapy (NACT), pathological complete response (pCR) is rare and multiple efforts have been made to predict disease recurrence. We developed a framework to predict pCR using clinicopathological characteristics widely available at diagnosis. The machine learning (ML) models were trained to predict pCR (n = 463), evaluated in an internal validation cohort (n = 109) and validated in an external validation cohort (n = 151). The best model was an Elastic Net, which achieved an area under the curve (AUC) of respectively 0.86 and 0.81. Our results highlight how simpler models using few input variables can be as valuable as more complex ML architectures. Our model is freely available and can be used to enhance the stratification of BC patients receiving NACT, providing a framework for the development of risk-adapted clinical trials.
Volume: 11
Conversion Ability of Immunotherapy in Hepatocellular Carcinoma: Insights from the International Converse Study
Authors: AREA MIN. 06 - Scienze mediche; Non assegn; AREA MIN. 03 - Scienze chimiche; LIVER CANCER###2235-1795; Goal 3: Good health and well-being###25122; NVU-1059-2025; ODU-4058-2025; JFA-3201-2023; AAA-6985-2022; NRG-7376-2025; N-4884-2016; E-4136-2016; K-9027-2016; ETI-8054-2022; DVX-2977-2022; OKL-0925-2025; JXN-9765-2024; GBI-3050-2022; ODT-3691-2025; MNP-2390-2025; EAA-0713-2022; CTC-6453-2022; GWQ-5807-2022; JLL-4417-2023; NBP-8708-2025; ACF-6633-2022; CIF-8523-2022; EKD-3321-2022; PCI-1657-2025; ABU-7442-2022; E-2873-2017; AAL-4707-2020; NVU-5037-2025; AAA-5966-2019; LRC-4609-2024; LJL-8863-2024; B-1253-2019; CDD-1531-2022; DZE-2417-2022; GAX-9838-2022; ONI-9192-2025; GFI-6538-2022; GBX-0618-2022; JAS-4656-2023; JAE-9905-2023; HDN-8476-2022; DYG-1391-2022; DXZ-0364-2022; FZO-1269-2022; DKZ-9331-2022; AAJ-1461-2020; AAI-3301-2021; AAB-9010-2019; DWE-5897-2022; DZG-2198-2022; LRB-6334-2024; GPG-4717-2022; MEC-3675-2025; EMW-3214-2022; GFJ-8359-2022; LSJ-1295-2024; CTL-8875-2022; K-1325-2018; IAZ-8837-2023; CMV-5205-2022; GLS-8971-2022; NNR-6045-2025; LQJ-8211-2024; DLZ-1607-2022; FZH-0936-2022; IAR-5511-2023; E-1120-2012; AAX-3013-2021; HXI-6162-2023; DVI-6747-2022; LKW-4755-2024; CFF-4678-2022; AAW-6583-2020; OKP-8212-2025; AAB-7784-2019; MZZ-5336-2025; DTK-9313-2022; FUU-1830-2022; DKU-9582-2022; HSM-5150-2023; ETY-6019-2022; FUX-0969-2022; CRN-8826-2022; AAC-1142-2022; C-5224-2017; DMO-7443-2022; KZP-1983-2024; ABD-2759-2021; JUF-2562-2023; MUO-2309-2025; CDW-1641-2022; LFV-9926-2024; IQR-8787-2023; PCH-8152-2025; 7103385675; 57192647681; 22978623500; 57205570340; 7003859199; 6602480388; 35316450500; 25642049500; 59664061700; 55533314700; 7409872158; 8664424100; 35399280200; 59722080200; 56068319400; 6602872506; 58450192500; 57223875522; 57223031784; 59507208500; 57203097714; 57323265500; 57217312225; 55405948300; 57201443418; 23479552000; 7006292400; 7101699492; 56516762300; 56494141600; 57217138368; 57045491200; 7202067754; 47961522200; 57202577641; 57203908984; 59743389500; 35339851600; 7005105898; 55338330900; 23991339200; 7003959009; 7004364046; 7004103098; 58676486300; 8888138300; 24778880000; 24079621100; 35180464500; 57209858034; 57223434900; 58161784700; 6602978959; 55853885600; 7005920149; 55312125500; 57246900700; 15923933100; 35378208900; 58554753100; 57192201029; 54788065400; 8619722900; 57237152900; 36854891300; 57196972311; 7101771483; 57204044185; 6603879680; 56348477100; 59557307700; 57117920800; 60126828300; 7004428252; 55839825600; 60127864400; 57194525584; 6507767839; 57204688931; 6506102320; 6603008052; 6603675919; 57224857907; 57126311200; 6701515092; 59454560300; 55280001900; 57193399387; 8621248500; 60127714400; 57211341552; 7003673653; 57218222462; 7004918276
Journal: LIVER CANCER
Published: 2025
DOI: 10.1159/000547792
Pages: 1-22
Keywords: Conversion; Hepatocellular carcinoma; Immunotherapy; Surgery;
Elliptical ejecta of asteroid Dimorphos is due to its surface curvature
Authors: Non assegn; AREA MIN. 02 - Scienze fisiche; CUU-8183-2022; HLR-3780-2023; GGW-7139-2022; GAH-5074-2022; ESD-3744-2022; QBH-6137-2026; HKN-0500-2023; HZI-2517-2023; P-6476-2015; I-4902-2012; HLK-1269-2023; CTM-4947-2022; DYN-1984-2022; IFG-8963-2023; ISQ-0634-2023; GHK-8431-2022; DWV-9440-2022; FWP-2241-2022; CFS-3628-2022; DYP-6030-2022; FZX-2971-2022; A-9759-2012; GCQ-2889-2022; GFF-8225-2022; DWN-9574-2022; FZZ-0535-2022; DDJ-7308-2022; FVV-6858-2022; DUQ-2065-2022; I-7475-2015; F-5384-2015; DWU-0981-2022; GDY-4101-2022; EUN-3723-2022; HUL-9562-2023; JCE-4157-2023; B-7744-2016; F-4568-2015; DUL-6195-2022; ENM-7589-2022; GDE-9626-2022; AAJ-3985-2021; DUL-3415-2022; DWP-0733-2022; HGD-4524-2022; GGD-2860-2022; FEG-0617-2022; CAJ-2883-2022; DVO-9054-2022; N-5574-2018; GDH-3986-2022; DKW-3609-2022; KIB-5109-2024; D-4408-2016; J-6191-2012; PEV-1372-2025; AAC-4090-2021; HNS-2166-2023; DTA-9438-2022; FAQ-9880-2022; AAN-2497-2020; I-7029-2015; AAS-8419-2020; MKD-3733-2025; HGV-4184-2022; FJY-5851-2022; HLS-6942-2023; HSK-4888-2023; JCM-2837-2023; DHC-3887-2022; GGB-5197-2022; L-9058-2014; F-9818-2010; GDD-3436-2022; GGN-2463-2022; AAO-5357-2020; NATURE COMMUNICATIONS###2041-1723; 55826845600; 57208445497; 7004318097; 7004640341; 57074031000; 57203736332; 7004011265; 6701831440; 55533357700; 8889572200; 57214791438; 37072319500; 36701832200; 7004189587; 57208049670; 58146735800; 6504168821; 57216933235; 25636752900; 55471974400; 55669241300; 23990264300; 57194858670; 24823039400; 57193622827; 23989081200; 55849158600; 55449295000; 7003331332; 36879186600; 6602709696; 7402075077; 7003564619; 8889756900; 24314530700; 55976970100; 7004387103; 23995780300; 23020214400; 57372292200; 6701612015; 6602999700; 6602330014; 8124291100; 56365949500; 57205446071; 56452875500; 55597712400; 16319102800; 54883873200; 35313993500; 9741589500; 57202131090; 55493499600; 35785529800; 58192237300; 55397558400; 57214805190; 57981671400; 6603871165; 59098028700; 38561464400; 56152199100; 7006528435; 57807063200; 55920339500; 57214806320; 7004712183; 58546708400; 8305008500; 57216737338; 6701471393; 57198080053; 57191593736; 56287163900; 12647223300
Journal: NATURE COMMUNICATIONS
Published: 2025
DOI: 10.1038/s41467-025-56010-w
Kinetic deflection is a planetary defense technique delivering spacecraft momentum to a small body to deviate its course from Earth. The deflection efficiency depends on the impactor and target. Among them, the contribution of global curvature was poorly understood. The ejecta plume created by NASA’s Double Asteroid Redirection Test impact on its target asteroid, Dimorphos, exhibited an elliptical shape almost aligned along its north-south direction. Here, we identify that this elliptical ejecta plume resulted from the target’s curvature, reducing the momentum transfer to 44 ± 10% along the orbit track compared to an equivalent impact on a flat target. We also find lower kinetic deflection of impacts on smaller near-Earth objects due to higher curvature. A solution to mitigate low deflection efficiency is to apply multiple low-energy impactors rather than a single high-energy impactor. Rapid reconnaissance to acquire a target’s properties before deflection enables determining the proper locations and timing of impacts.
Volume: 16
High-speed Boulders and the Debris Field in DART Ejecta
Authors: Farnham Tony L.; Sunshine Jessica M.; Hirabayashi Masatoshi; Ernst Carolyn M.; Daly R. Terik; Agrusa Harrison F.; Barnouin Olivier S.; Li Jian-Yang; Kumamoto Kathryn M.; Syal Megan Bruck; Wiggins Sean E.; Bjonnes Evan; Stickle Angela M.; Raducan Sabina D.; Cheng Andrew F.; Glenar David A.; Lolachi Ramin; Stubbs Timothy J.; Fahnstock Eugene G.; Amoroso Marilena; Bertini Ivano; Brucato John R.; Capannolo Andrea; Cremonese Gabriele; Dall'Ora Massimo; Della Corte Vincenzo; Deshapriya J. D. P.; Dotto Elisabetta; Gai Igor; Hasselmann Pedro H.; Ieva Simone; Impresario Gabriele; Ivanovski Stavro L.; Lavagna Michele; Lucchetti Alice; Marzari Francesco; Epifani Elena Mazzotta; Modenini Dario; Pajola Maurizio; Palumbo Pasquale; Pirrotta Simone; Poggiali Giovanni; Rossi Alessandro; Tortora Paolo; Zannoni Marco; Zanotti Giovanni; Zinzi Angelo; Dall’Ora Massimo; Deshapriya J.D.P.; Lavagna Michèle
Journal: PLANETARY SCIENCE JOURNAL
Published: 2025
DOI: 10.3847/PSJ/addd1a
On 2022 September 26 the Double Asteroid Redirection Test (DART) spacecraft collided with Dimorphos, the moon of the near-Earth asteroid 65803 Didymos, in a full-scale demonstration of a kinetic impactor concept. The companion Light Italian Cubesat for Imaging of Asteroids (LICIACube) spacecraft documented the aftermath, capturing images of the expansion and evolution of the ejecta from 29 to 243 s after the impact. We present results from our analyses of these observations, including an improved reduction of the data and new absolute calibration, an updated LICIACube trajectory, and a detailed description of the events and phenomena that were recorded throughout the flyby. One notable aspect of the ejecta was the existence of clusters of boulders, up to 3.6 m in radius, that were ejected at speeds of up to 52 m s−1. Our analysis of the spatial distribution of 104 of these boulders suggests that they are likely the remnants of larger boulders shattered by the DART spacecraft in the first stages of the impact. The amount of momentum contained in these boulders is more than 3 times that of the DART spacecraft, and it is directed primarily to the south, almost perpendicular to the DART trajectory. Recoil of Dimorphos from the ejection of these boulders has the potential to change its orbital plane by up to a degree and to impart a non-principal-axis component to its rotation state. Damping timescales for these phenomena are such that the Hera spacecraft, arriving at the system in 2026, should be able to measure these effects.
Volume: 6