Prediction of CFRP and NSM-Wrapped Composite Column Capacities Using Experimentation and an Ensemble Machine-Learning Approach with SHAP Interpretation
Carbon fiber-reinforced polymer wrapping; Column capacity; Composite columns; Extreme gradient boost; Machine learning in structural engineering; Near-surface mounted wrapping; Shapley additive explanations
Column capacity is an essential parameter in structural design, and its accurate determination is critical for a safe load-Transfer mechanism in structures. Also, experimental and accurate model-based assessments are critical to the column capacity evaluation. The main objective of this study is to experimentally and analytically investigate near-surface mounted (NSM) wrapped columns of different configurations and compare their capacity enhancements with the capacity enhancements of carbon fiber-reinforced polymer (CFRP). The study is also focused on developing a statistical regression model and extreme gradient boost (XG Boost), an ensemble machine-learning (ML) approach-based model, and examining both models developed for the experimental results by Shapley additive explanations (SHAP) interpretations. Therefore, the study experimentally reviewed the behavior of 24 composite columns to gain insights into experimental and code-recommended column capacities, stress-strain responses, axial stiffness, ductility factors, and failure modes. NSM-wrapped columns gained 10% strength increments, and, in comparison, the full-wrapped CFRP columns achieved 22% strength enhancement. The structural columns in a structure typically require various levels or types of strengthening, depending on their loading conditions, geometry, and material properties. With a 10% increment, the NSM technique suits columns needing lesser strength enhancements. Therefore, a key finding of the study is that the contribution of NSM longitudinal wrapping to column capacity is significant and cannot be ignored. A statistical regression model is developed for column capacity with four key parameters: percentage steel reinforcement, the extent of epoxy adhesion, the weight of the specimen, and the concrete clear cover. A model based on XG Boost, an ensemble ML approach, is also developed for the same four key parameters. The models developed are evaluated by SHAP interpretations. The SHAP analysis technique interpreted this improved model for various input-output features. The XG Boost machine-learning algorithm, developed with a coefficient of determination of 0.99, is found to be a refined regression model. Also, the study establishes that the ensemble ML approach used in tandem with SHAP analysis is a robust prediction and model interpretation tool, highlighting the significance of the percentage of steel reinforcement and the extent of epoxy adhesion over the other variables for the experimental dataset. 2026 American Society of Civil Engineers.
Journal of Structural Design and Construction Practice;Volume;31;Issue;3;Article No.;4026046;
American Society of Civil Engineers (ASCE)
Restricted Access; Hardcopy may be available in the library
https://doi.org/10.1061/JSDCCC.SCENG-2094 https://www.scopus.com/pages/publications/105035086761?origin=resultslist
Sudhir M.R., Dept. of Civil Engineering, School of Engineering and Technology, Christ (Deemed to Be Univ.), Bangalore, Karnataka, 560074, India; Beulah M., Dept. of Civil Engineering, School of Engineering and Technology, Christ (Deemed to Be Univ.), Bangalore, Karnataka, 560074, India
Hybrid Analytical-Machine Learning Framework for SH-Wave Dispersion in Piezo-Flexoelectric Layered Structures with Imperfect Interfaces
Imperfect interfaces; Machine learning surrogates; Physics-informed neural networks; Piezo-flexoelectricity; Shear-horizontal waves; Surface acoustic wave (SAW)/micro-electro-mechanical systems (MEMS) applications
This study presents a hybrid analytical-machine learning (ML) framework for modeling shear-horizontal (SH) wave propagation in piezo-flexoelectric (PFE) layered structures with imperfect interfacial bonding. The governing dispersion relations were derived using mechanical, electrical, and flexoelectric continuity conditions, establishing explicit links among phase velocity, wave number, layer thickness ratio, and flexoelectric coefficients. Analytical results revealed that nanoscale flexoelectricity and interfacial imperfections significantly influence wave behavior: electrically open (EO) boundaries amplify electromechanical coupling and enhance dispersion, whereas electrically shorted (ES) conditions suppress these effects, leading to reduced phase velocities. To address the computational cost associated with evaluating high-dimensional parametric spaces, ML surrogate models were incorporated. Convolutional neural network (CNN) and k-nearest neighbor (KNN) regressors accurately reproduced analytical dispersion surfaces with errors below 3% and drastically reduced computation time by more than two orders of magnitude. Classification models provided >90% accuracy in distinguishing EO and ES boundary-condition regimes, and generative artificial intelligence (AI) variational autoencoder/generative adversarial network (VAE/GAN) architectures successfully synthesized dispersion surfaces for previously unseen flexoelectric parameter ranges. The proposed hybrid framework combines the physical rigor of analytical modeling with the efficiency of modern ML surrogates, enabling rapid parametric exploration and high-fidelity prediction of SH-wave characteristics. The outcomes support accelerated design of advanced surface acoustic wave (SAW) devices, micro-electro-mechanical systems (MEMS) components, and nanoscale electromechanical systems. Future work will extend the approach to experimental validation and uncertainty-aware modeling for real-world applications. 2026 American Society of Civil Engineers.
Journal of Engineering Mechanics;Volume;152;Issue;6;Article No.;4026020;
https://doi.org/10.1061/JENMDT.EMENG-8884 https://www.scopus.com/pages/publications/105035391118?origin=resultslist
Seema, Dept. of Mathematics, Christ Univ., Bengaluru, Karnataka, 560029, India; Singhal A., Dept. of Mathematics, Christ Univ., Bengaluru, Karnataka, 560029, India
Generative AI: fuelling e-commerce revenue growth
Dynamic capabilities; GenAI; PLS-SEM; Socio-technical system
Generative AI (GenAI) is a novel technology that has transformed businesses across various industries. E-commerce companies are increasingly using cutting-edge technologies, such as GenAI, that could drive revenue growth. This study leverages the lens of social-technical systems and dynamic capabilities theories to examine how e-commerce companies adopt GenAI and its subsequent impact on their revenue generation capabilities. This study investigated the factors influencing the adoption of GenAI in e-commerce companies. This study considers both Social factorstop management support, organizational readiness, competitive pressure, and vendor support) and Technical factors (security concerns, technological readiness, and AI explainability). Further, it investigates how the use of GenAI affects the development of technological capabilities and leads to financial performance, particularly in sales growth, revenue generation, profitability, and cost reduction. To validate the proposed model, we surveyed e-commerce company managers and analyzed the collected data using PLS-SEM. These findings offer valuable insights for e-commerce companies and their managers, enabling them to leverage GenAI for revenue generation. This novel study makes a significant contribution to the academic understanding of GenAI adoption and how it can be adopted for successful revenue generation. The Author(s), under exclusive licence to Springer Nature Limited 2025.
Journal of Revenue and Pricing Management;Volume;25;Issue;1;pp.93-108
https://doi.org/10.1057/s41272-025-00554-5 https://www.scopus.com/pages/publications/105012844995?origin=resultslist
Sivathanu B., School of Business and Management, Christ University, Karnataka, Bangalore, India; Pillai R., Chandragupt Institute of Management Patna, Bihar, Patna, India
Examining humanized bot interaction for the retail revenue growth
Chatbot; Continuous purchase; Price; Revenue; Trust
The increasing popularity of conversational artificial intelligence (chatbot) in retail has fuelled consumer purchase decisions. The present study measures humanbot interaction through anthropomorphism, social presence, personalization, media richness, and its role in customer engagement and continuous purchase intention for retail revenue growth. Data were collected from 366 respondents and analyzed using PLS-SEM-ANN integrated approach. To overcome the limitation of establishing only the linear relationship among variables for prediction, the study deploys nonlinear complex artificial neural network (ANN) models to determine the relative importance of the significant predictors identified through structural equation modeling (PLS-SEM). The findings of the study confirm the role of anthropomorphism, personalization, and media richness in customer engagement and customer engagement leading to continuous purchase intention. Furthermore, Chatbots in the electronic commerce space strengthen involvement, but trust and price fairness also play a positive moderating influence in shaping consumer purchase intentions. Study implications highlight the role of anthropomorphic design in the desired social presence for sustained engagement and its contribution to revenue. This study enriches the AI literature and guides organizations leveraging chatbots to create more natural and personalized interactions so retailers can better meet customer needs, foster loyalty, and stay competitive in an increasingly digital marketplace. The Author(s), under exclusive licence to Springer Nature Limited 2025.
Kumar, Nishant; Garg, Pratibha; Gupta, Neha; Upreti, Kamal
Journal of Revenue and Pricing Management;Volume;25;Issue;1;pp.25-40
https://doi.org/10.1057/s41272-025-00549-2 https://www.scopus.com/pages/publications/105012379316?origin=resultslist
Kumar N., School of Business and Management, CHRIST University, Bangalore, India; Garg P., Amity School of Business, Amity University, Noida, India; Gupta N., Amity School of Business, Amity University, Noida, India; Upreti K., Department of Computer Science, CHRIST University, Delhi NCR, Ghaziabad, India
Probing the formation of megaparsec-scale giant radio galaxies II. Continuum and polarization behavior from magneto-hydrodynamic simulations
galaxies: active; galaxies: groups: general; galaxies: jets; magnetohydrodynamics (MHD); methods: numerical
Context. The persistence of radiative signatures in giant radio galaxies (GRGs & 700 kpc) remains a frontier topic of research, with contemporary telescopes revealing intricate features that require investigation. Aims. This study aims to examine the emission characteristics of simulated GRGs, and correlate them with their underlying three-dimensional dynamical properties. Methods. Sky-projected continuum and polarization maps at 1 GHz were computed from five 3D relativistic magnetohydrodynamical (RMHD) simulations by integrating the synthesized emissivity data along the line of sight, with the integration path chosen to reflect the GRG evolution in the sky plane. The emissivities were derived from these RMHD simulations, featuring FR-I and FR-II jets injected at different locations of the large-scale environment and with propagation along varying jet frustration paths. Results. Morphologies, such as widened lobes from low-power jets and collimated flows from high-power jets, are strongly shaped by the triaxiality of the environment, resulting in features such as wings and asymmetric cocoons, thereby making morphology a crucial indicator of GRG formation mechanisms. The decollimation of the bulk flow in GRG jets gives rise to intricate cocoon features, most notably filamentary structuresmagnetically dominated threads with lifespans of a few mega-year. High jet power cases frequently display enhanced emission zones at mid-cocoon distances (alongside warmspots around the jet head), contradicting the interpretations of the GRG as a restarting source. In such cases, examining the lateral intensity variation of the cocoon may reveal the sources state, with a gradual decrease in emission suggesting a low active stage. This study highlights that applying a simple radio powerjet power relation to a statistical GRG sample is unfeasible, as it depends on growth conditions of individual GRGs. Effects such as inverse-Compton cooling due to cosmic microwave background photons and matter entrainment significantly impact the long-term emission persistence of GRGs. The diminishing fractional polarization with GRG evolution reflects increasing turbulence, underscoring the importance of modeling this characteristic further, particularly for even larger-scaled sources. The Authors 2025.
Giri, Gourab; Fendt, Christian; Bagchi, Joydeep; Thorat, Kshitij; Saikia, Dhruba J.; Deane, Roger P.; Delhaize, Jacinta
Astronomy and Astrophysics;Volume;703;Issue;;Article No.;A214;
https://doi.org/10.1051/0004-6361/202554872 https://www.scopus.com/pages/publications/105022885217?origin=resultslist
Giri G., Istituto Nazionale di Astrofisica (INAF), Istituto di Radioastronomia (IRA), via Gobetti 101, Bologna, 40129, Italy, Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa; Fendt C., Max Planck Institute for Astronomy, Kigstuhl 17, Heidelberg, D-69117, Germany; Bagchi J., Department of Physics and Electronics, Christ University, Hosur Road, Bangalore, 560029, India; Thorat K., Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa; Saikia D.J., Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Pune, 411007, India; Deane R.P., Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa, Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Johannesburg, 2000, South Africa; Delhaize J., Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch, 7701, South Africa
Euclid: Early Release Observations of ram-pressure stripping in the Perseus cluster: Detection of parsec-scale star formation within the low surface brightness stripped tails of UGC 2665 and MCG +07-07-070
Galaxies: clusters: intracluster medium; Galaxies: evolution; Galaxies: spiral; Galaxies: star formation
Euclid is delivering optical and near-infrared imaging data over 14 000 deg2 on the sky at spatial resolution and surface brightness levels that can be used to understand the morphological transformation of galaxies within groups and clusters. Using the Early Release Observations (ERO) of the Perseus cluster, we demonstrate the capability offered by Euclid in studying the nature of perturbations for galaxies in clusters. Filamentary structures are observed along the discs of two spiral galaxies, UGC 2665 and MCG +07-07-070, with no extended diffuse emission expected from tidal interactions at surface brightness levels of a30 mag arcseca 2. The detected features exhibit a good correspondence in morphology between optical and near-infrared wavelengths, with a surface brightness of a25 mag arcseca 2, and the knots within the features have sizes of a 100 pc, as observed through IE imaging. Using the Euclid, CFHT, UVIT, and LOFAR 144 MHz radio continuum observations, we conducted a detailed analysis to understand the origin of the detected features. We constructed the Euclid IEaYE, YEaHE, and CFHT u ar, g ai colour-colour plane and show that these features contain recent star formation events, which are also indicated by their H? and NUV emissions. Euclid colours alone are insufficient for studying stellar population ages in unresolved star-forming regions, which require multi-wavelength optical imaging data. There are features with red colours that can be explained by dust being stripped along with the gas in these regions. The morphological shape, orientation, and mean age of the stellar population, combined with the presence of extended radio continuum cometary tails can be consistently explained if these features formed during a recent ram-pressure stripping event. This result further confirms the exceptional qualities of Euclid in the study of galaxy evolution in dense environments. 2025 EDP Sciences. All rights reserved.
George, K.; Boselli, A.; Cuillandre, J.-C.; Kmel, M.; Lann, A.; Bellhouse, C.; Saifollahi, T.; Mondelin, M.; Bolzonella, M.; Joseph, P.; Roberts, I.D.; Van Weeren, R.J.; Liu, Q.; Sola, E.; Urbano, M.; Baes, M.; Peletier, R.F.; Klein, M.; Davies, C.T.; Zinchenko, I.A.; Sorce, J.G.; Poulain, M.; Aghanim, N.; Altieri, B.; Amara, A.; Andreon, S.; Auricchio, N.; Baccigalupi, C.; Baldi, M.; Balestra, A.; Bardelli, S.; Battaglia, P.; Biviano, A.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Cas-Herrera, G.; Capobianco, V.; Carbone, C.; Carretero, J.; Casas, S.; Castellano, M.; Castignani, G.; Cavuoti, S.; Chambers, K.C.; Cimatti, A.; Colodro-Conde, C.; Congedo, G.; Conselice, C.J.; Conversi, L.; Copin, Y.; Courbin, F.; Courtois, H.M.; Cropper, M.; Da Silva, A.; Degaudenzi, H.; De Lucia, G.; Di Giorgio, A.M.; Dole, H.; Douspis, M.; Dubath, F.; Dupac, X.; Dusini, S.; Escoffier, S.; Farina, M.; Faustini, F.; Ferriol, S.; Fotopoulou, S.; Frailis, M.; Franceschi, E.; Galeotta, S.; Gillis, B.; Giocoli, C.; Gracia-Carpio, J.; Grazian, A.; Grupp, F.; Haugan, S.V.H.; Holmes, W.; Hook, I.M.; Hormuth, F.; Hornstrup, A.; Hudelot, P.; Jahnke, K.; Jhabvala, M.; Keihen, E.; Kermiche, S.; Kiessling, A.; Kubik, B.; Kunz, M.; Kurki-Suonio, H.; Le Brun, A.M.C.; Le Mignant, D.; Ligori, S.; Lilje, P.B.; Lindholm, V.; Lloro, I.; Mainetti, G.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Maurogordato, S.; Medinaceli, E.; Mei, S.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mohr, J.J.; Mora, A.; Moresco, M.; Moscardini, L.; Nakajima, R.; Neissner, C.; Nichol, R.C.; Niemi, S.-M.; Nightingale, J.W.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W.J.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.; Popa, L.A.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Sakr, Z.; Sapone, D.; Sartoris, B.; Schewtschenko, J.A.; Schirmer, M.; Schneider, P.; Secroun, A.; Seidel, G.; Seiffert, M.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.; Steinwagner, J.; Tallada-Cresp P.; Taylor, A.N.; Tereno, I.; Toft, S.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valentijn, E.A.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Verdoes Kleijn, G.; Veropalumbo, A.; Wang, Y.; Weller, J.; Zamorani, G.; Zerbi, F.M.; Zucca, E.; Burigana, C.; Gabarra, L.; Mart-Fleitas, J.; Scottez, V.
Astronomy and Astrophysics;Volume;701;Issue;;Article No.;A40;
All Open Access; Gold Open Access; Green Open Access
https://doi.org/10.1051/0004-6361/202554836 https://www.scopus.com/pages/publications/105015302152?origin=resultslist
George K., University Observatory, LMU, Faculty of Physics, Scheinerstrasse 1, Munich, 81679, Germany; Boselli A., Aix-Marseille Universite, CNRS, CNES, LAM, Marseille, France; Cuillandre J.-C., UniversitParis-Saclay, UniversitParis Cite, CEA, CNRS, AIM, Gif-sur-Yvette, 91191, France; Kmel M., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany; Lann A., Universitde Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, Strasbourg, 67000, France; Bellhouse C., School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD, United Kingdom; Saifollahi T., Universitde Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, Strasbourg, 67000, France; Mondelin M., UniversitParis-Saclay, UniversitParis Cite, CEA, CNRS, AIM, Gif-sur-Yvette, 91191, France; Bolzonella M., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Joseph P., Indian Institute of Astrophysics, Koramangala II Block, Bangalore, 560034, India, Department of Physics and Electronics, CHRIST (Deemed to Be University), Bangalore, 560029, India; Roberts I.D., Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, N2L 3G1, ON, Canada; Van Weeren R.J., Leiden Observatory, Leiden University, Einsteinweg 55, Leiden, 2333 CC, Netherlands; Liu Q., Leiden Observatory, Leiden University, Einsteinweg 55, Leiden, 2333 CC, Netherlands; Sola E., Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom; Urbano M., Universitde Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, Strasbourg, 67000, France; Baes M., Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, Gent, 9000, Belgium; Peletier R.F., Kapteyn Astronomical Institute, University of Groningen, PO Box 800, Groningen, 9700 AV, Netherlands; Klein M., Ludwig-Maximilians-University, Schellingstrasse 4, Munich, 80799, Germany; Davies C.T., Ludwig-Maximilians-University, Schellingstrasse 4, Munich, 80799, Germany; Zinchenko I.A., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany; Sorce J.G., Univ. Lille, CNRS, Centrale Lille, UMR 9189, CRIStAL, Lille, 59000, France, UniversitParis-Saclay, CNRS, Institut da Astrophysique Spatiale, Orsay, 91405, France; Poulain M., Space Physics and Astronomy Research Unit, University of Oulu, Pentti Kaiteran katu 1, Oulu, FI-90014, Finland; Aghanim N., UniversitParis-Saclay, CNRS, Institut da Astrophysique Spatiale, Orsay, 91405, France; Altieri B., ESAC/ESA, Camino Bajo Del Castillo, s/n., Urb. Villafranca del Castillo, Villanueva de la Cada, Madrid, 28692, Spain; Amara A., School of Mathematics and Physics, University of Surrey, Guildford, Surrey, GU2 7XH, United Kingdom; Andreon S., INAF, Osservatorio Astronomico di Brera, Via Brera 28, Milano, 20122, Italy; Auricchio N., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Baccigalupi C., IFPU, Institute for Fundamental Physics of the Universe, Via Beirut 2, Trieste, 34151, Italy, INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy, INFN, Sezione di Trieste, Via Valerio 2, TS, Trieste, 34127, Italy, SISSA, International School for Advanced Studies, Via Bonomea 265, TS, Trieste, 34136, Italy; Baldi M., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, Dipartimento di Fisica e Astronomia, Universitdi Bologna, Via Gobetti 93/2, Bologna, 40129, Italy, INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy; Balestra A., INAF-Osservatorio Astronomico di Padova, Via della Osservatorio 5, Padova, 35122, Italy; Bardelli S., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Battaglia P., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Biviano A., IFPU, Institute for Fundamental Physics of the Universe, Via Beirut 2, Trieste, 34151, Italy, INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Bonino D., INAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20 (TO), Pino Torinese, 10025, Italy; Branchini E., INAF, Osservatorio Astronomico di Brera, Via Brera 28, Milano, 20122, Italy, Dipartimento di Fisica, Universitdi Genova, Via Dodecaneso 33, Genova, 16146, Italy, INFN-Sezione di Genova, Via Dodecaneso 33, Genova, 16146, Italy; Brescia M., Department of Physics E. Pancini, University Federico II, Via Cinthia 6, Napoli, 80126, Italy, INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli, 80131, Italy; Brinchmann J., Instituto de Astrofica e Ciencias Do Espa, Universidade Do Porto, CAUP, Rua das Estrelas PT4150-762, Porto, Portugal, Faculdade de Ciencias, Universidade Do Porto, Rua do Campo de Alegre, Porto, 4150-007, Portugal; Camera S., INAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20 (TO), Pino Torinese, 10025, Italy, Dipartimento di Fisica, UniversitDegli Studi di Torino, Via P. Giuria 1, Torino, 10125, Italy, INFN-Sezione di Torino, Via P. Giuria 1, Torino, 10125, Italy; Cas-Herrera G., Leiden Observatory, Leiden University, Einsteinweg 55, Leiden, 2333 CC, Netherlands, European Space Agency, ESTEC, Keplerlaan 1, Noordwijk, 2201 AZ, Netherlands, Institute Lorentz, Leiden University, Niels Bohrweg 2, Leiden, 2333 CA, Netherlands; Capobianco V., INAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20 (TO), Pino Torinese, 10025, Italy; Carbone C., INAF-IASF Milano, Via Alfonso Corti 12, Milano, 20133, Italy; Carretero J., Centro de Investigaciones Energicas, Medioambientales y Tecnolicas (CIEMAT), Avenida Complutense 40, Madrid, 28040, Spain, Port da InformaciCientica, Campus UAB, C. Albareda s/n, Bellaterra, Barcelona, 08193, Spain; Casas S., Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH, Aachen University, Aachen, 52056, Germany; Castellano M., INAF-Osservatorio Astronomico di Roma, Via Frascati 33, Monteporzio Catone, 00078, Italy; Castignani G., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Cavuoti S., INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli, 80131, Italy, INFN Section of Naples, Via Cinthia 6, Napoli, 80126, Italy; Chambers K.C., Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, 96822, HI, United States; Cimatti A., Dipartimento di Fisica e Astronomia Augusto Righi, Alma Mater Studiorum Universita di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy; Colodro-Conde C., Instituto de Astrofica de Canarias, Via Ltea, La Laguna, Tenerife, 38205, Spain; Congedo G., Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom; Conselice C.J., Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom; Conversi L., ESAC/ESA, Camino Bajo Del Castillo, s/n., Urb. Villafranca del Castillo, Villanueva de la Cada, Madrid, 28692, Spain, European Space Agency, ESRIN, Largo Galileo Galilei 1, Frascati, Roma, 00044, Italy; Copin Y., UniversitClaude Bernard Lyon 1, CNRS, IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, F-69100, France; Courbin F., Institut de Cicies Del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Marti Franqu 1, Barcelona, 08028, Spain, InstituciCatalana de Recerca i Estudis Avants (ICREA), Passeig de Llu Companys 23, Barcelona, 08010, Spain; Courtois H.M., UCB Lyon 1, CNRS, IN2P3, IUF, IP2I Lyon, 4 rue Enrico Fermi, Villeurbanne, 69622, France; Cropper M., Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey, RH5 6NT, United Kingdom; Da Silva A., Departamento de Fica, Faculdade de Ciencias, Universidade de Lisboa, Edifio C8, Campo Grande, Lisboa, PT1749-016, Portugal, Instituto de Astrofica e Ciencias Do Espa, Faculdade de Ciencias, Universidade de Lisboa, Campo Grande, Lisboa, 1749-016, Portugal; Degaudenzi H., Department of Astronomy, University of Geneva, ch. da Ecogia 16, Versoix, 1290, Switzerland; De Lucia G., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Di Giorgio A.M., INAF, Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere, 100, Roma, 00100, Italy; Dole H., UniversitParis-Saclay, CNRS, Institut da Astrophysique Spatiale, Orsay, 91405, France; Douspis M., UniversitParis-Saclay, CNRS, Institut da Astrophysique Spatiale, Orsay, 91405, France; Dubath F., Department of Astronomy, University of Geneva, ch. da Ecogia 16, Versoix, 1290, Switzerland; Dupac X., ESAC/ESA, Camino Bajo Del Castillo, s/n., Urb. Villafranca del Castillo, Villanueva de la Cada, Madrid, 28692, Spain; Dusini S., INFN-Padova, Via Marzolo 8, Padova, 35131, Italy; Escoffier S., Aix-Marseille Universite, CNRS, IN2P3, CPPM, Marseille, France; Farina M., INAF, Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere, 100, Roma, 00100, Italy; Faustini F., INAF-Osservatorio Astronomico di Roma, Via Frascati 33, Monteporzio Catone, 00078, Italy, Space Science Data Center, Italian Space Agency, Via del Politecnico snc, Roma, 00133, Italy; Ferriol S., UniversitClaude Bernard Lyon 1, CNRS, IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, F-69100, France; Fotopoulou S., School of Physics, HH Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol, BS8 1TL, United Kingdom; Frailis M., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Franceschi E., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Galeotta S., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Gillis B., Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom; Giocoli C., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy; Gracia-Carpio J., Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Grazian A., INAF-Osservatorio Astronomico di Padova, Via della Osservatorio 5, Padova, 35122, Italy; Grupp F., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Haugan S.V.H., Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, Oslo, 0315, Norway; Holmes W., Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109, CA, United States; Hook I.M., Department of Physics, Lancaster University, Lancaster, LA1 4YB, United Kingdom; Hormuth F., Felix Hormuth Engineering, Goethestr. 17, Leimen, 69181, Germany; Hornstrup A., Technical University of Denmark, Elektrovej 327, Kgs. Lyngby, 2800, Denmark, Cosmic Dawn Center (DAWN), Denmark; Hudelot P., Institut da Astrophysique de Paris, UMR 7095, CNRS, Sorbonne Universite, 98 bis boulevard Arago, Paris, 75014, France; Jahnke K., Max-Planck-Institut f Astronomie, Konigstuhl 17, Heidelberg, 69117, Germany; Jhabvala M., NASA, Goddard Space Flight Center, Greenbelt, 20771, MD, United States; Keihen E., Department of Physics, Helsinki Institute of Physics, University of Helsinki, Gustaf Hlstrin katu 2, 00014, Finland; Kermiche S., Aix-Marseille Universite, CNRS, IN2P3, CPPM, Marseille, France; Kiessling A., Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109, CA, United States; Kubik B., UniversitClaude Bernard Lyon 1, CNRS, IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, F-69100, France; Kunz M., Universitde Gene, Dartement de Physique Theorique, Centre for Astroparticle Physics, 24 quai Ernest-Ansermet, Geneve 4, CH-1211, Switzerland; Kurki-Suonio H., Department of Physics, University of Helsinki, P.O. Box 64, 00014, Finland, Helsinki Institute of Physics, University of Helsinki, Gustaf Hallstrin katu 2, Helsinki, Finland; Le Brun A.M.C., Laboratoire da Etude de la Univers et des Phenomenes EXtremes, Observatoire de Paris, UniversitPSL, Sorbonne Universite, CNRS, Meudon, 92190, France; Le Mignant D., Aix-Marseille Universite, CNRS, CNES, LAM, Marseille, France; Ligori S., INAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20 (TO), Pino Torinese, 10025, Italy; Lilje P.B., Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, Oslo, 0315, Norway; Lindholm V., Department of Physics, University of Helsinki, P.O. Box 64, 00014, Finland, Helsinki Institute of Physics, University of Helsinki, Gustaf Hallstrin katu 2, Helsinki, Finland; Lloro I., SKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, Cheshire, SK11 9FT, United Kingdom; Mainetti G., Centre de Calcul de La, IN2P3, CNRS, 21 avenue Pierre de Coubertin, Cedex, Villeurbanne, 69627, France; Maino D., INAF-IASF Milano, Via Alfonso Corti 12, Milano, 20133, Italy, Dipartimento di Fisica Aldo Pontremoli, UniversitDegli Studi di Milano, Via Celoria 16, Milano, 20133, Italy, Via Celoria 16, Milano, 20133, Italy; Maiorano E., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Mansutti O., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Marggraf O., Universit Bonn, Argelander-Institut fur Astronomie, Auf dem Hel 71, Bonn, 53121, Germany; Markovic K., Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109, CA, United States; Martinelli M., INAF-Osservatorio Astronomico di Roma, Via Frascati 33, Monteporzio Catone, 00078, Italy, INFN, Sezione di Roma, C/o Dipartimento di Fisica, Piazzale Aldo Moro, 2 , Edificio G. Marconi, Roma, 00185, Italy; Martinet N., Aix-Marseille Universite, CNRS, CNES, LAM, Marseille, France; Marulli F., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy, Dipartimento di Fisica e Astronomia Augusto Righi, Alma Mater Studiorum, Universita di Bologna, Via Piero Gobetti 93/2, Bologna, 40129, Italy; Massey R., Department of Physics, Institute for Computational Cosmology, Durham University, South Road, Durham, DH1 3LE, United Kingdom; Maurogordato S., UniversitCote da Azur, Observatoire de la Cote da Azur, CNRS, Laboratoire Lagrange, Bd de la Observatoire, CS 34229, cedex 4, Nice, 06304, France; Medinaceli E., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Mei S., UniversitParis Cite, CNRS, Astroparticule et Cosmologie, Paris, 75013, France, CNRS-UCB, International Research Laboratory, Centre Pierre Binetruy, IRL2007, CPB-IN2P3, Berkeley, United States; Mellier Y., Institut da Astrophysique de Paris, UMR 7095, CNRS, Sorbonne Universite, 98 bis boulevard Arago, Paris, 75014, France, Institut da Astrophysique de Paris, 98bis Boulevard Arago, Paris, 75014, France; Meneghetti M., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy; Merlin E., INAF-Osservatorio Astronomico di Roma, Via Frascati 33, Monteporzio Catone, 00078, Italy; Meylan G., Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fale de Lausanne (EPFL), Observatoire de Sauverny, Versoix, 1290, Switzerland; Mohr J.J., University Observatory, LMU, Faculty of Physics, Scheinerstrasse 1, Munich, 81679, Germany; Mora A., Aurora Technology for European Space Agency (ESA), Camino Bajo Del Castillo, s/n, Urbanizacion Villafranca del Castillo, Villanueva de la Canada, Madrid, 28692, Spain; Moresco M., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, Dipartimento di Fisica e Astronomia Augusto Righi, Alma Mater Studiorum, Universita di Bologna, Via Piero Gobetti 93/2, Bologna, 40129, Italy; Moscardini L., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy, Dipartimento di Fisica e Astronomia Augusto Righi, Alma Mater Studiorum, Universita di Bologna, Via Piero Gobetti 93/2, Bologna, 40129, Italy; Nakajima R., Universit Bonn, Argelander-Institut fur Astronomie, Auf dem Hel 71, Bonn, 53121, Germany; Neissner C., Port da InformaciCientica, Campus UAB, C. Albareda s/n, Bellaterra, Barcelona, 08193, Spain, Institut de Fica da Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, Bellaterra, Barcelona, 08193, Spain; Nichol R.C., School of Mathematics and Physics, University of Surrey, Guildford, Surrey, GU2 7XH, United Kingdom; Niemi S.-M., European Space Agency, ESTEC, Keplerlaan 1, Noordwijk, 2201 AZ, Netherlands; Nightingale J.W., School of Mathematics Statistics and Physics, Newcastle University, Herschel Building, Newcastle-upon-Tyne, NE1 7RU, United Kingdom; Padilla C., Institut de Fica da Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, Bellaterra, Barcelona, 08193, Spain; Paltani S., Department of Astronomy, University of Geneva, ch. da Ecogia 16, Versoix, 1290, Switzerland; Pasian F., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Pedersen K., DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 155, Copenhagen, 2200, Denmark; Percival W.J., Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, N2L 3G1, ON, Canada, Department of Physics and Astronomy, University of Waterloo, Waterloo, N2L 3G1, ON, Canada, Perimeter Institute for Theoretical Physics, Waterloo, N2L 2Y5, ON, Canada; Pettorino V., European Space Agency, ESTEC, Keplerlaan 1, Noordwijk, 2201 AZ, Netherlands; Pires S., UniversitParis-Saclay, UniversitParis Cite, CEA, CNRS, AIM, Gif-sur-Yvette, 91191, France; Polenta G., Space Science Data Center, Italian Space Agency, Via del Politecnico snc, Roma, 00133, Italy; Poncet M., Centre National da Etudes Spatiales, Centre Spatial de Toulouse, 18 avenue Edouard Belin Cedex 9, Toulouse, 31401, France; Popa L.A., Institute of Space Science, Str. Atomistilor, nr. 409 MA gurele, Ilfov, 077125, Romania; Pozzetti L., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Raison F., Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Rebolo R., Instituto de Astrofica de Canarias, Via Ltea, La Laguna, Tenerife, 38205, Spain, Consejo Superior de Investigaciones Cientificas, Calle Serrano 117, Madrid, 28006, Spain, Universidad de la Laguna, Departamento de Astrofica, La Laguna, Tenerife, 38206, Spain; Renzi A., INFN-Padova, Via Marzolo 8, Padova, 35131, Italy, Dipartimento di Fisica e Astronomia G. Galilei, Universitdi Padova, Via Marzolo 8, Padova, 35131, Italy; Rhodes J., Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109, CA, United States; Riccio G., INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, Napoli, 80131, Italy; Romelli E., INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Roncarelli M., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Rossetti E., Dipartimento di Fisica e Astronomia, Universitdi Bologna, Via Gobetti 93/2, Bologna, 40129, Italy; Saglia R., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Sakr Z., Institut f Theoretische Physik, University of Heidelberg, Philosophenweg 16, Heidelberg, 69120, Germany, Institut de Recherche en Astrophysique et Planologie (IRAP), Universitde Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, Toulouse, 31400, France, UniversitSt Joseph, Faculty of Sciences, Beirut, Lebanon; Sapone D., Departamento de Fica, FCFM, Universidad de Chile, Blanco Encalada, Santiago, 2008, Chile; Sartoris B., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany, INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Schewtschenko J.A., Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom; Schirmer M., Max-Planck-Institut f Astronomie, Konigstuhl 17, Heidelberg, 69117, Germany; Schneider P., Universit Bonn, Argelander-Institut fur Astronomie, Auf dem Hel 71, Bonn, 53121, Germany; Secroun A., Aix-Marseille Universite, CNRS, IN2P3, CPPM, Marseille, France; Seidel G., Max-Planck-Institut f Astronomie, Konigstuhl 17, Heidelberg, 69117, Germany; Seiffert M., Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109, CA, United States; Serrano S., Institut da Estudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC, Castelldefels, Barcelona, 08860, Spain, Satlantis, University Science Park, Sede Bld, Leioa, Bilbao, 48940, Spain, Institute of Space Sciences, ICE, CSIC, Campus UAB, Carrer de Can Magrans, s/n, Barcelona, 08193, Spain; Sirignano C., INFN-Padova, Via Marzolo 8, Padova, 35131, Italy, Dipartimento di Fisica e Astronomia G. Galilei, Universitdi Padova, Via Marzolo 8, Padova, 35131, Italy; Sirri G., INFN-Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, 40127, Italy; Stanco L., INFN-Padova, Via Marzolo 8, Padova, 35131, Italy; Steinwagner J., Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Tallada-CrespP., Centro de Investigaciones Energicas, Medioambientales y Tecnolicas (CIEMAT), Avenida Complutense 40, Madrid, 28040, Spain, Port da InformaciCientica, Campus UAB, C. Albareda s/n, Bellaterra, Barcelona, 08193, Spain; Taylor A.N., Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom; Tereno I., Departamento de Fica, Faculdade de Ciencias, Universidade de Lisboa, Edifio C8, Campo Grande, Lisboa, PT1749-016, Portugal, Instituto de Astrofica e Ciencias Do Espa, Faculdade de Ciencias, Universidade de Lisboa, Tapada da Ajuda, Lisboa, 1349-018, Portugal; Toft S., Cosmic Dawn Center (DAWN), Denmark, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, Copenhagen, 2200, Denmark; Toledo-Moreo R., Universidad Politnica de Cartagena, Departamento de Electrica y Tecnologia de Computadoras, Plaza del Hospital 1, Cartagena, 30202, Spain; Torradeflot F., Centro de Investigaciones Energicas, Medioambientales y Tecnolicas (CIEMAT), Avenida Complutense 40, Madrid, 28040, Spain, Port da InformaciCientica, Campus UAB, C. Albareda s/n, Bellaterra, Barcelona, 08193, Spain; Tutusaus I., Institut de Recherche en Astrophysique et Planologie (IRAP), Universitde Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, Toulouse, 31400, France; Valentijn E.A., Kapteyn Astronomical Institute, University of Groningen, PO Box 800, Groningen, 9700 AV, Netherlands; Valenziano L., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy, INFN-Bologna, Via Irnerio 46, Bologna, 40126, Italy; Valiviita J., Department of Physics, University of Helsinki, P.O. Box 64, 00014, Finland, Helsinki Institute of Physics, University of Helsinki, Gustaf Hallstrin katu 2, Helsinki, Finland; Vassallo T., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany, INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste, 34143, Italy; Verdoes Kleijn G., Kapteyn Astronomical Institute, University of Groningen, PO Box 800, Groningen, 9700 AV, Netherlands; Veropalumbo A., INAF, Osservatorio Astronomico di Brera, Via Brera 28, Milano, 20122, Italy, Dipartimento di Fisica, Universitdi Genova, Via Dodecaneso 33, Genova, 16146, Italy, INFN-Sezione di Genova, Via Dodecaneso 33, Genova, 16146, Italy; Wang Y., Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, 91125, CA, United States; Weller J., Universits-Sternwarte Mchen, Fakult f Physik, Ludwig-Maximilians-Universit Mchen, Scheinerstrasse 1, Mchen, 81679, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, Garching, 85748, Germany; Zamorani G., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Zerbi F.M., INAF, Osservatorio Astronomico di Brera, Via Brera 28, Milano, 20122, Italy; Zucca E., INAF, Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, Via Piero Gobetti 93/3, Bologna, 40129, Italy; Burigana C., INFN-Bologna, Via Irnerio 46, Bologna, 40126, Italy, INAF, Istituto di Radioastronomia, Via Piero Gobetti 101, Bologna, 40129, Italy; Gabarra L., Department of Physics, Oxford University, Keble Road, Oxford, OX1 3RH, United Kingdom; Mart-Fleitas J., Aurora Technology for European Space Agency (ESA), Camino Bajo Del Castillo, s/n, Urbanizacion Villafranca del Castillo, Villanueva de la Canada, Madrid, 28692, Spain; Scottez V., Institut da Astrophysique de Paris, 98bis Boulevard Arago, Paris, 75014, France, ICL, Junia, UniversitCatholique de Lille, LITL, Lille, 59000, France
The birth of Be star disks: I. from localized ejection to circularization
Circumstellar matter; Stars: emission-line, Be; Stars: oscillations; Stars: winds, outflows; Techniques: photometric; Techniques: spectroscopic
Context. Classical Be stars are well known to eject mass to build up a disk, but the details governing the initial distribution and subsequent evolution of this matter into a disk are in general poorly constrained through observations. Aims. By combining high-cadence time-series spectroscopy with contemporaneous space photometry from the Transiting Exoplanet Survey Satellite (TESS), we have sampled about 30 mass ejection events in 13 Be stars. Our goal is to constrain the geometrical and kinematic properties of the ejecta as early as possible, facilitating the investigation into the material's initial conditions and evolution, and understanding its interactions with preexisting material. Methods. The photometric variability is analyzed together with measurements of the at-times rapidly changing emission features in order to identify the onset of outburst events and obtain information about the geometry of the ejecta and how it changes over time. Short-lived line asymmetries display oscillation cycles (tefl frequencies), which are compared to photometric and stable spectroscopic frequencies. Results. All Be stars observed with sufficiently high cadence during an outburst are found to exhibit rapid oscillations of line asymmetry with a single frequency in the days following the start of the event. For a given star this circumstellar frequency may differ only slightly from event to event even when the outbursts they are associated with have different properties. These circumstellar frequencies are typically between 0.5 to 2 d- 1, and are generally near photometric frequencies. They are slightly below prominent (generally stable) spectroscopic frequencies seen in photospheric absorption lines. The emission asymmetry cycles break down after roughly 5- 10 cycles, with the emission line profile converging toward approximate symmetry shortly thereafter. In photometry, several frequencies typically emerge at relatively high amplitude at some point during the mass ejection process. Conclusions. In all observed cases, freshly ejected material was initially constrained within a narrow azimuthal range, indicating it was launched from a localized region on the stellar surface. The material orbits the star with a frequency consistent with the near-surface Keplerian orbital frequency. This material circularizes into a disk configuration after several orbital timescales. This is true whether or not there was a preexisting disk at the time of the observed outburst. We find no evidence for precursor phases prior to the ejection of mass in our sample. The several photometric frequencies that emerge during outburst are at least partially stellar in origin. The Authors 2025.
Labadie-Bartz, J.; Carciofi, A.C.; Rubio, A.C.; Baade, D.; Siverd, R.; Arcos, C.; Figueiredo, A.L.; Naz Y.; Neiner, C.; Rivinius, T.; Richardson, N.D.; Nova, S.; Pinho, M.L.; Bhattacharyya, S.; Leadbeater, R.; Guarro Fl J.; Lecocq, V.; Piehler, G.; Kozok, J.; Sollecchia, U.; Bryssinck, E.; Buil, C.; Martin, J.; Desnoux, V.; Heathcote, B.; Cacella, P.; Bertrand, G.; Broussat, J.J.; Ventura, A.; Diz, R.; Blais, A.; Somogyi, P.; Thizy, O.; Garde, O.; Charbonnel, S.; Le D P.; Mulato, L.; Petit, T.
Astronomy and Astrophysics;Volume;699;Issue;;Article No.;A82;
https://doi.org/10.1051/0004-6361/202453321 https://www.scopus.com/pages/publications/105009902359?origin=resultslist
Labadie-Bartz J., LIRA, Observatoire de Paris, UniversitPSL, CNRS, Sorbonne Universit UniversitParis Cit CY Cergy Paris Universit Meudon, 92190, France; Carciofi A.C., Instituto de Astronomia, Geofica e Cicias Atmosficas, Universidade de S Paulo, Rua do Mat 1226, Cidade Universitia, SP, S Paulo, B-05508-900, Brazil; Rubio A.C., Instituto de Astronomia, Geofica e Cicias Atmosficas, Universidade de S Paulo, Rua do Mat 1226, Cidade Universitia, SP, S Paulo, B-05508-900, Brazil, Max-Planck-Institut f Astrophysik, Karl-Schwarzschild-Str. 1, Garching b. Mchen, 85748, Germany; Baade D., European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Karl-Schwarzschild-Str. 2, Garching b. Mchen, 85748, Germany; Siverd R., Institute for Astronomy, University of Hawaii, 2680 Woodlawn, Honolulu, 96822, HI, United States; Arcos C., Instituto de Fica y Astronom, Facultad de Ciencias, Universidad de Valparao, Av. Gran Bretana 1111, Valparao, Chile; Figueiredo A.L., Instituto de Astronomia, Geofica e Cicias Atmosficas, Universidade de S Paulo, Rua do Mat 1226, Cidade Universitia, SP, S Paulo, B-05508-900, Brazil; NazY., Groupe d'Astrophysique des Hautes Energies, STAR, Universite de Liege, Quartier Agora (B5c, Institut d'Astrophysique et de Geophysique), All du 6 Ao 19c, Sart Tilman, Lie, 4000, Belgium; Neiner C., LIRA, Observatoire de Paris, UniversitPSL, CNRS, Sorbonne Universit UniversitParis Cit CY Cergy Paris Universit Meudon, 92190, France; Rivinius T., European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Casilla 19001, Santiago, 19, Chile; Richardson N.D., Department of Physics and Astronomy, Embry-Riddle Aeronautical University, 3700 Willow Creek Rd, Prescott, 86301, AZ, United States; Nova S., Department of Physics and Astronomy, Embry-Riddle Aeronautical University, 3700 Willow Creek Rd, Prescott, 86301, AZ, United States; Pinho M.L., Instituto de Astronomia, Geofica e Cicias Atmosficas, Universidade de S Paulo, Rua do Mat 1226, Cidade Universitia, SP, S Paulo, B-05508-900, Brazil; Bhattacharyya S., European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Casilla 19001, Santiago, 19, Chile, CHRIST (Deemed to Be University), Bangalore, India; Leadbeater R., Three Hills Observatory, The Birches, Torpenhow, CA7 1JF, United Kingdom, The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Guarro FlJ., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France, Piera Remote Observatory, C. de Jaume Balmes 2, Catalonia Piera, Barcelona, 08784, Spain, SMM Remote Observatory, Av. de Catalunya 38, Catalonia, Santa Maria de Montmagastrell (Trega), 25345, Spain; Lecocq V., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Piehler G., Selztal Observatory, Bechtolsheimer Weg 26, Friesenheim, 55278, Germany; Kozok J., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Sollecchia U., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Bryssinck E., BRIXIIS Observatory (MPC:B96), Kruibeke, Belgium; Buil C., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Martin J., Huggins Spectroscopic Observatory, Rayleigh, Essex, SS6 8AW, United Kingdom; Desnoux V., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Heathcote B., Glenpiper Observatory, 165 Sievers LaneGlenhope, 3444, VIC, Australia; Cacella P., DogsHeaven Observatory X87, Brasilia, Brazil; Bertrand G., La Montagne Observatory, 1 B Rue Jacques Prevert, La Montagne, 44620, France; Broussat J.J., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Ventura A., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Diz R., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Blais A., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Somogyi P., The Be Star Spectra (BeSS) Database Operated at LIRA, Observatoire de Paris, Meudon, France; Thizy O., Observatoire Belle Etoile, Revel, 38420, France; Garde O., 2SPOT, 45, Chemin du Lac, Chons, 38690, France; Charbonnel S., 2SPOT, 45, Chemin du Lac, Chons, 38690, France; Le DP., 2SPOT, 45, Chemin du Lac, Chons, 38690, France; Mulato L., 2SPOT, 45, Chemin du Lac, Chons, 38690, France; Petit T., 2SPOT, 45, Chemin du Lac, Chons, 38690, France
Probing the formation of megaparsec-scale giant radio galaxies: I. Dynamical insights from magnetohydrodynamic simulations
Galaxies: active; Galaxies: groups: general; Galaxies: jets; Magnetohydrodynamics (MHD); Methods: numerical
Context. Constituting a relatively small fraction of the extended-jetted population, giant radio galaxies (GRGs) form in a wide range of jet and environment configurations. This observed diversity complicates the identification of the growth factors that facilitate their attainment of megaparsec scales. Aims. This study aims to numerically investigate the hypothesized formation mechanisms of GRGs extending ?1 Mpc in order to assess their general applicability. Methods. We employed tri-axial ambient medium settings to generate varying levels of jet frustration and simulated jets with a low and a high power from different locations in the environment. This approach formulated five representations evolving under a relativistic magnetohydrodynamic framework. Results. The emergence of distinct giant phases in all five simulated scenarios suggests that GRGs may be more common than previously believed. This prediction can be verified with contemporary and forthcoming radio telescopes. We find that different combinations of jet morphology, power, and evolutionary age of the formed structure hold the potential to elucidate different formation scenarios. In all of these cases, the lobes are overpressured, prompting further investigation into pressure profiles when jet activity ceases, potentially distinguishing between relic and active GRGs. We observed a potential phase transition in GRGs marked by differences in lobe expansion speed and pressure variations compared to their smaller evolutionary phases. This suggests the need for further investigation across a broader parameter space to determine if lobe evolution in GRGs fundamentally differs from smaller radio galaxies. The axial ratio analysis reveals self-similar expansion in rapidly propagating jets, while there is a notable deviation when the jet forms wider lobes. Overall, this study emphasizes that multiple growth factors simultaneously at work can better elucidate the current-day population of GRGs, including scenarios such as the growth of GRGs in dense environments, GRGs extending several megaparsecs, development of GRGs in low-powered jets, and the formation of morphologies such as GRG-XRGs. The Authors 2025.
Giri, Gourab; Bagchi, Joydeep; Thorat, Kshitij; Deane, Roger P.; Delhaize, Jacinta; Saikia, Dhruba J.
Astronomy and Astrophysics;Volume;693;Issue;;Article No.;A77;
https://doi.org/10.1051/0004-6361/202451812 https://www.scopus.com/pages/publications/85215374760?origin=resultslist
Giri G., Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa, South African Radio Astronomy Observatory, 2 Fir St, Black River Park, Observatory, 7925, South Africa; Bagchi J., Department of Physics and Electronics, Christ University, Hosur Road, Bangalore, 560029, India; Thorat K., Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa; Deane R.P., Department of Physics, University of Pretoria, Private Bag X20, Hatfield, 0028, South Africa, Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Johannesburg, 2000, South Africa; Delhaize J., Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch, 7701, South Africa; Saikia D.J., Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Pune, 411007, India
Fe doped ZnO nanomaterials for energy storage applications as high-capacitance supercapacitor electrodes
Enhancing the performance of electrode materials is essential for developing high-capacitance supercapacitors, and transition-metal-doped metal oxides have shown particular promise in this regard. In this work, Fe-doped ZnO nanostructures were synthesized using a sonochemical method and systematically examined through XRD, SEM, TEM, XPS and UVvis analyses to verify Fe incorporation and the resulting changes in crystallinity, morphology and optical behaviour. The structural modifications induced by Fe were evident in the electrochemical response, with the optimized ZnOFe sample delivering a specific capacitance of 11.4 F g?1 at 0.1 A g?1 in the two-electrode system and 462 F g?1 in the three-electrode system, both measured in 3 M KOH electrolyte. A CR2032 coin cell assembled with this material achieved an energy density of 1.6 Wh kg?1 and a power density of 2890.93 W kg?1, demonstrating an effective balance between energy storage and power output. These findings highlight the suitability of Fe-doped ZnO as a tunable electrode material and support its further exploration in advanced supercapacitor systems. This journal is The Royal Society of Chemistry, 2026.
Veerabhadraiah, Srikanth R.; Soman, Gowri; Bhat, Sachin A.; Sharma, Rohit K.; Thimmappa, Ravikumar; Mirle, Chinmaya; Hegde, Gurumurthy; Yelamaggad, C.V.; Naik, Nagaraja
RSC Advances;Volume;16;Issue;27;pp.24997-25010
https://doi.org/10.1039/d6ra02336c https://www.scopus.com/pages/publications/105038651416?origin=resultslist
Veerabhadraiah S.R., Department of Studies in Chemistry, Manasagangotri, University of Mysore, Mysuru, 570006, India; Soman G., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India; Bhat S.A., Centre for Nano and Soft Matter Sciences, Bengaluru, 562162, India; Sharma R.K., Centre for Nano and Soft Matter Sciences, Bengaluru, 562162, India; Thimmappa R., Department of Energy Science and E-Mobility, Atria University, Bengaluru, 560024, India; Mirle C., Institute of Organic and Macromolecular Chemistry, Ulm University, Albert-Einstein-Allee11, Ulm, 89081, Germany; Hegde G., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Department of Chemistry, B. N. M. Institute of Technology, Banashankari, Karnataka, Bengaluru, 560070, India; Yelamaggad C.V., Centre for Nano and Soft Matter Sciences, Bengaluru, 562162, India; Naik N., Department of Studies in Chemistry, Manasagangotri, University of Mysore, Mysuru, 570006, India
Carbon dots derived from Averrhoa bilimbi fruit for the detection of cholesterol and chromium(vi)
Carbon dots (CDs) are a class of carbon-based nanomaterials, typically less than 10 nm in size, known for their unique optical and electronic properties. Their discovery led to the opening of new avenues in nanotechnology, particularly in the field of fluorescence-based sensing. Owing to their strong photoluminescence, excellent aqueous solubility, low cytotoxicity, and potential surface functionalization, CDs have been considered as effective fluorescent probes for the detection of a wide range of analytes. Herein, we report the hydrothermal synthesis of CDs from a natural source, Averrhoa bilimbi fruit, leading to the formation of CDs exhibiting useful photoluminescent properties and potential for selective detection of cholesterol and Cr(vi) ions. The average particle size of Averrhoa bilimbi fruit-derived CDs (AB-CDs) was found to be 6.022 nm. The properties of AB-CDs were unravelled from structural and optical characterization and the applicability of AB-CDs as sensors for heavy metals and biomarkers was studied. The selective fluorescence response towards cholesterol and Cr(vi) makes it an efficient fluoroprobe for practical applications. The limits of detection for the sensing of cholesterol and Cr(vi) were estimated to be 0.31 M and 1.71 M respectively. The sensor system using AB-CDs is economical, sustainable, and eco-friendly. This journal is The Royal Society of Chemistry, 2026
Joji Mathew, Aishwarya; Lisa John, Varsha; Aiswarya, P.S.; Vinod, T.P.
RSC Advances;Volume;16;Issue;13;pp.12132-12140
https://doi.org/10.1039/d6ra00222f https://www.scopus.com/pages/publications/105031638144?origin=resultslist
Joji Mathew A., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India; Lisa John V., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India; Aiswarya P.S., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India; Vinod T.P., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bengaluru, 560029, India
Defect engineered unzipped multiwalled carbon nanotube/vanadium pentoxide composite for high-performance supercapacitor application
In the pursuit of next-generation energy storage systems, the advancement of high-performance electrode materials with enhanced capacitance and durability remains critical. This study presents a binary composite of unzipped multi-walled carbon nanotubes (UzMWCNTs) integrated with vanadium pentoxide (V2O5). The unzipping process introduces surface defects and oxygen functional groups, which enhance dispersion and provide numerous active sites. V2O5 nanoparticles uniformly anchor onto the UzMWCNT surface, offering pseudocapacitive behavior and boosting redox activity. The synergistic interaction between electric double-layer capacitance and faradaic charge storage delivers superior electrochemical performance. Structural and morphological characterization confirms successful composite formation, while electrochemical evaluations reveal a specific capacitance of 1135 F g?1 and cycling stability with 88% retention over 2000 cycles. This work highlights the potential of UzMWCNT/V2O5 hybrids as promising candidates for high-efficiency, next-generation supercapacitor electrodes. This journal is The Royal Society of Chemistry, 2026
Aswathi, V.P.; Raman, Vidya; Sreeja, P.B.
RSC Advances;Volume;16;Issue;13;pp.11404-11414
https://doi.org/10.1039/d6ra00149a https://www.scopus.com/pages/publications/105031596571?origin=resultslist
Aswathi V.P., Centre for Renewable Energy and Environmental Sustainability, Department of Chemistry, CHRIST University, Karnataka, Bengaluru, 560029, India; Raman V., Department of Chemistry, T. M Jacob Memorial Government College, Manimalakkunu, Kerala, Koothattukulam, 686662, India; Sreeja P.B., Centre for Renewable Energy and Environmental Sustainability, Department of Chemistry, CHRIST University, Karnataka, Bengaluru, 560029, India
Hormonal-mediated Cicer arietinum L. leaf extract-assisted synthesis of a ternary g-C3N4/ZrTiO4/V2O5 nanocomposite for photocatalytic remediation of organic pollutants
A novel green synthesis approach was developed for the fabrication of a g-C3N4/ZrTiO4/V2O5 nanocomposite (NC) using a hormone-treated plant extract as a biogenic reducing and stabilizing agent. The hormone-assisted synthesis had a significant influence on the physical, chemical, and morphological properties of the nanocomposite compared to the control route. The obtained NCs, confirmed by XRD, FTIR, UV-vis, SEM, and EDX analyses, exhibited enhanced crystallinity, a reduced band gap, and a distinct morphological transformation from nanorods to nanocubic structures. Elemental composition analysis confirmed the successful integration of Zr, Ti, and V components, improving the photocatalytic performance of the material. The hormone-mediated g-C3N4/ZrTiO4/V2O5 NC achieved an 89.14% degradation efficiency of Rose Bengal dye, maintaining its activity over three successive cycles without notable loss of performance. Furthermore, the photocatalyst efficiently converted degradation intermediates, such as benzyl alcohols, into valuable substituted benzaldehyde derivatives with yields ranging from 75% to 92%, demonstrating sustained catalytic stability over four consecutive cycles. These findings highlight the potential of hormone-assisted green synthesis as a promising and sustainable approach for designing advanced photocatalytic nanomaterials. This journal is The Royal Society of Chemistry and the Centre National de la Recherche Scientifique, 2026
Venkatesan, Aakash; Nizam, Aatika; Theresa, Letcy V.; Xavier, Jobi; Ganganagappa, Nagaraju
New Journal of Chemistry;Volume;50;Issue;14;pp.6169-6181
https://doi.org/10.1039/d6nj00565a https://www.scopus.com/pages/publications/105034417818?origin=resultslist
Venkatesan A., Department of Chemistry, Christ University, Hosur Road, Bangalore, India; Nizam A., Department of Chemistry, Christ University, Hosur Road, Bangalore, India; Theresa L.V., Department of Chemistry, Christ University, Hosur Road, Bangalore, India; Xavier J., Department of Life Sciences, Christ University, Hosur Road, Bangalore, India; Ganganagappa N., Energy Materials Research Laboratory, Department of Chemistry, Siddaganga Institute of Technology, Tumakuru, 572103, India
Engineering Ru(ii) Schiff base complexes as biofunctional materials: cytotoxic and cell imaging perspectives
Four bromine-substituted Ru(ii)-arene Schiff base complexes derived from bromo-picolinaldehyde and 3-(1H-pyrazol-1-yl)propan-1-amine were examined for their cytotoxic behaviour toward cervical cancer (SiHa) and normal fibroblast (3T3-L1) cells using MTT-based in vitro assays. The ligands and complexes were comprehensively characterized by FTIR; 1H, 13C, and 19F NMR; and ESI-LCMS analyses. Single-crystal X-ray diffraction (SCXRD) confirmed the molecular structure of complex 3, while PXRD validated the crystalline nature of complexes 2 and 4. Density functional theory (DFT) calculations further supported the experimental data by revealing optimized geometries and key electronic descriptors. All complexes exhibited time- and dose-dependent anticancer effects, with complexes 24 showing the greatest cytotoxicity toward the SiHa cells (viability at 72 h: 20% 3%, 31% 3%, and 29% 3%, respectively) while maintaining high viability in normal fibroblasts (>90%). The IC50 values for complexes 14 were 19.54 2, 14.21 4, 12.43 4, and 12.43 4 M, respectively. Acridine orange (AO) and ethidium bromide (EtBr) staining and morphological analyses confirmed apoptosis as the primary mechanism of cell death, as evidenced by reduced adhesion, membrane blebbing, and cell rounding. The pronounced and selective cytotoxicity of these bromine-substituted Ru(ii) complexes highlights their potential as promising biomaterial candidates for targeted anticancer therapy. This journal is The Royal Society of Chemistry and the Centre National de la Recherche Scientifique, 2026
Bhunya, Debasis; Datta, Riya; Maity, Swapan; Sahoo, Subhasish; Samanta, Bidhan Chandra
New Journal of Chemistry;Volume;50;Issue;12;pp.5266-5276
https://doi.org/10.1039/d6nj00553e https://www.scopus.com/pages/publications/105032238479?origin=resultslist
Bhunya D., Department of Chemistry, Christ University, Hosur Road, Karnataka, Bengaluru, 560029, India; Datta R., Department of Chemistry, Christ University, Hosur Road, Karnataka, Bengaluru, 560029, India; Maity S., School of Materials Science and Technology, Indian Institute of Technology (IIT), BHU, Varanasi, India; Sahoo S., Department of Chemistry, National Institute of Technology, Rourkela, 769008, India; Samanta B.C., Department of Chemistry, Mugberia Gangadhar Mahavidyalaya, Bhupatinagar, Purba Medinipur, West Bengal, India
A turn-on bis-hydrazone fluorescent chemosensor for selective Cd2+ detection: synthesis, structural insights, and theoretical validation
Heavy metal pollution, particularly from cadmium(ii) ions (Cd2+), causes severe environmental and health risks due to its acute toxicity, carcinogenicity, and bioaccumulation, leading to kidney damage, neurological disorders, and other physiological issues. Herein, we report the one-pot synthesis of a bis-hydrazone-based fluorescent probe L2H2O (1) for selective detection of Cd2+. Probe 1 was derived from isophthalaldehyde and 3-pyridylcarbonyl hydrazine and single-crystal X-ray diffraction discloses a well-defined binding pocket with pyridyl, imine, and carbonyl donor sites suitable for Cd2+ coordination. Probe 1 exhibits weak emission in CH3CN/HEPES buffer (9?:?1, v/v, pH 7.4) due to photoinduced electron transfer (PET) and unrestricted intramolecular rotations. Upon selective binding to Cd2+, 1 displays a pronounced turn-on fluorescence response with intensity enhancements of at ?324 nm and at 420 nm, accompanied by bathochromic shifts to 327 nm (?? = 3 nm) and 445 nm (?? = 25 nm) (?ex = 295 nm). The limit of detection (LOD) for probe 1 with metal Cd2+ is 3.39 M, with a binding constant of 5 103 M?1. 1H NMR titration, DFT-optimized geometries (B3LYP/6-31+G(d)/LANL2DZ), and simulated UV-Vis spectra further confirm binding of Cd2+, blocking PET and rigidifying the structure via chelation-enhanced fluorescence (CHEF). This work presents a modular hydrazone scaffold for developing selective Cd2+ sensors with potential application in environmental and biological monitoring. The Royal Society of Chemistry and the Centre National de la Recherche Scientifique, 2026.
Adhikari, Suman; Nath, Sourav; Saha, Koushik; Baildya, Nabajyoti; Kaminsky, Werner; Kumar, Malavika S; Roy, Subhadip; Das, Avijit Kumar
https://doi.org/10.1039/d6nj00362a https://www.scopus.com/pages/publications/105037888529?origin=resultslist
Adhikari S., Department of Chemistry, Govt. Degree College, Tripura, Dharmanagar, (N)-799253, India; Nath S., Department of Chemistry, Govt. Degree College, Tripura, Dharmanagar, (N)-799253, India, Department of Chemistry and Vivekananda Centre for Research, Ramakrishna Mission Residential College, Narendrapur, Kolkata, 700103, India; Saha K., Department of Chemistry, Jadavpur University, West Bengal, Kolkata, 700032, India; Baildya N., Department of Chemistry, Milki High School, Milki, Malda, 732209, India; Kaminsky W., Department of Chemistry, University of Washington, Seattle, 98195, Washington, United States; Kumar M.S., Department of Chemistry, Christ University, Hosur Road, Karnataka, Bangalore, 560029, India; Roy S., Department of Chemistry, The ICFAI University Tripura, Kamalghat, Mohanpur, Tripura, Agartala, 799210, India; Das A.K., Department of Chemistry, Christ University, Hosur Road, Karnataka, Bangalore, 560029, India
Copper immobilized on a layered magnetite-based nanocatalyst for sustainable Ullmann cross-coupling reaction
This study demonstrates the efficient synthesis of diarylthioethers via CS cross-coupling between diverse aryl halides and arylthiols utilizing a magnetically retractable Fe3O4@SiO2PrNH2SACu(ii) nanocatalyst using K2CO3 as a base in DMF. The heterogeneous nanocatalyst was fabricated through a multistep process. The designed catalyst was characterized using various techniques, such as XRD, HRTEM, FESEM, STEM, EDAX, elemental mapping, TGA, VSM, XPS, ICP-OES and FT-IR. The catalyst design provides a dual role of the Schiff base-anchoring copper ions, to accelerate the oxidative addition and reductive elimination steps. This method makes use of ligand-free synthesis of diarylsulfides, enabling magnetic recovery and reuse of the catalyst for up to 6 cycles. The nanocatalyst exhibited high catalytic activity and a broad substrate scope. The magnetic nature of the nanocatalyst enabled easy separation from the reaction mixture using an external magnet, thus simplifying the workup. The synthesized nanocatalyst was then utilized for the synthesis of diarylthioethers and heterodiarylthioethers. The pure compounds were characterized using 1H and 13C NMR. This catalytic system offers a cost-effective, efficient, and simple protocol for the formation of the CS bond. This journal is The Royal Society of Chemistry, 2026.
Materials Advances;Volume;7;Issue;9;pp.4744-4753
https://doi.org/10.1039/d6ma00112b https://www.scopus.com/pages/publications/105036241855?origin=resultslist
D Souza E.S., Department of Chemistry, Christ University, Bengaluru, 560029, India; Nizam A., Department of Chemistry, Christ University, Bengaluru, 560029, India
Cr2MoAlC2 MAX phase and its derivative Cr2MoC2Tx MXene for supercapacitors and electrocatalytic water splitting
The expanding research on 2D MXenes has enabled new strategies to engineer material properties via structural design. While bimetallic or double transition metal (DTM) MXenes have continued to gain attention since their emergence in 2015, their versatile structure and exceptional physicochemical properties have inspired wide exploration. This study reports the synthesis of the Cr2MoAlC2 MAX phase and its derivative Cr2MoC2Tx MXene (Tx = F/OH/O), leveraging the synergistic incorporation of Cr and Mo as dual transition metals. The structural, thermal, chemical, and surface morphology characteristics were analyzed using various techniques. Cr2MoC2Tx MXene exhibits superior pseudocapacitance performance as an electrode material, achieving a specific capacitance of 1350 F g?1 at 1 A g?1 with 84% retention over 5000 cycles. In a two-electrode asymmetric device, Cr2MoC2Tx MXene delivers a specific capacitance of 438.3 F g?1 at 1 A g?1, an energy density of ?87.66 Wh kg?1, and a power density of 1200 W kg?1. Additionally, Cr2MoC2Tx MXene demonstrates excellent electrocatalytic activity for water splitting applications, with overpotentials of 186 mV for the hydrogen evolution reaction (HER) and 280 mV for the oxygen evolution reaction (OER), at 10 mA cm?2. This dual functionality, driven by the synergistic interaction between Cr and Mo, establishes Cr2MoC2Tx MXene as a promising material for both energy storage and hydrogen production, positioning it as a competitive candidate among state-of-the-art materials. Furthermore, this research aligns with the United Nations Sustainable Development Goal (SDG) 7, contributing to the advancement of high-performance electrode materials for next-generation electrochemical applications. This journal is The Royal Society of Chemistry, 2026.
Madhushree, R.; Sunajadevi, Kalathiparambil Rajendra Pai
https://doi.org/10.1039/d6dt00446f https://www.scopus.com/pages/publications/105040559558?origin=resultslist
Madhushree R., Department of Chemistry, Christ University, Bangalore, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bangalore, 560029, India; Sunajadevi K.R.P., Department of Chemistry, Christ University, Bangalore, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bangalore, 560029, India
A new benzothiazoloacetonitrile-derived fluorescent probe for selective hydrazine detection and its applications in bioimaging and cotton swab analysis
Hydrazine (N2H4) is extensively utilized in various chemical industries. However, it is a highly toxic and explosive chemical posing a serious risk to human health and the environment, which warrants its quick and selective detection. To address this issue, we introduce a benzothiazoloacetonitrile-based fluorescent probe containing a recognition site for hydrazine detection. Adding the benzothiazoloacetonitrile group to the phenanthroline-based imidazole fluorophore increased BTN's electrophilicity, aiding the nucleophilic attack by hydrazine. This led to a rapid fluorescence change from orange to green within one minute, with a limit of detection (LOD) of 0.21 M, resulting from the cleavage of the olefinic bond between the donor and acceptor units. The probe's selective response to hydrazine was supported by a specific reaction mechanism, confirmed by LC-MS and DFT studies. Additionally, the probe can detect hydrazine using cotton swabs for quick, on-site testing. It also allows for clear visualisation in living cells through different fluorescence channels. Overall, these results demonstrate that the probe exhibits significant potential for the detection of hydrazine in environmental and biological samples. This journal is The Royal Society of Chemistry, 2026.
Durgi, Nikita Kush; D. K., Ramesh; Manjappa, Kiran B.; Pujar, Prasad Pralhad
https://doi.org/10.1039/d6an00062b https://www.scopus.com/pages/publications/105038011958?origin=resultslist
Durgi N.K., Department of Chemistry, Christ University, Karnataka, Bangalore, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bangalore, 560029, India; D. K. R., Department of Chemistry, Christ University, Karnataka, Bangalore, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bangalore, 560029, India; Manjappa K.B., College of Science, Tunghai University, Bangalore, 560029, India; Pujar P.P., Department of Chemistry, Christ University, Karnataka, Bangalore, 560029, India, Centre for Renewable Energy and Environmental Sustainability, Christ University, Bangalore, 560029, India
Photoaligned nematic liquid crystals doped with palladium-immobilised carbon nanospheres for advanced low-voltage display and energy storage devices
This study presents a nematic liquid crystal (NLC), D30-17, doped with palladium-immobilised carbon nanospheres (CNS) Pd/ON10 at two different concentrations. The composites were prepared with 0.1 and 0.4 wt/wt% dopant concentrations and are referred to as Mix 1 and Mix 2, respectively. The palladium-immobilized carbon nanospheres were employed because they function as advanced materials for catalysis and energy applications owing to the catalytic properties of palladium. The sample holder used in this experiment consisted of photo-aligned cells coated with a photosensitive alignment layer, Cibacron brilliant yellow (CBY). The textural studies revealed improved alignment in the doped mixtures. The frequency- and temperature-dependent dielectric behaviour was analysed for the pure and doped systems in both the planar (at 0 V) and homeotropic (at 12 V) states. Dielectric studies showed that the relative permittivity, dielectric loss, and conductivity of the doped material increased with increasing dopant concentration compared with that of pure NLC. Compared with the pure NLC and Mix 2, Mix 1 exhibited greater dielectric anisotropy, leading to a lower threshold voltage. A reversal in the dielectric anisotropy was also observed, which was attributed to the bistable inversion in the CBY alignment layer of the photo-aligned cells. Optical studies indicated that there was no significant shift in wavelength with respect to the dopant concentration. These composites are expected to find applications in liquid-crystal-based electronic and photonic devices. This journal is The Royal Society of Chemistry, 2026
Shukla, Garima; Rastogi, Ayushi; S, Supriya; Hegde, Gurumurthy; Manohar, Rajiv
Journal of Materials Chemistry C;Volume;14;Issue;16;pp.6743-6755
https://doi.org/10.1039/d5tc04092b https://www.scopus.com/pages/publications/105031524121?origin=resultslist
Shukla G., Liquid Crystal Research Laboratory, Department of Physics, University of Lucknow, Uttar Pradesh, Lucknow, 226007, India; Rastogi A., Liquid Crystal Research Laboratory, Department of Physics, University of Lucknow, Uttar Pradesh, Lucknow, 226007, India, Amity School of Applied Sciences, Amity University, Karnataka, Bengaluru, 562110, India; S S., Department of Chemistry, B. M. S. College of Engineering, Bull Temple Road, Karnataka, Bengaluru, 560019, India, Centre for Nanomaterials & Displays, B. M. S. College of Engineering, Bull temple Road, Karnataka, Bengaluru, 560019, India; Hegde G., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Adindistech Private Limited, Manpho Pavillion Building, Bilekahalli, Bengaluru, 560076, India; Manohar R., Liquid Crystal Research Laboratory, Department of Physics, University of Lucknow, Uttar Pradesh, Lucknow, 226007, India
A self-powered and stretchable magnetic film for humanmachine interface applications
Developing stretchable, self-powered electronic interfaces for ambient energy harvesting is crucial for next-generation wearable electronics and humanmachine interface applications. We present a stretchable magnetoelectric composite film comprising Ni0.5Co0.5Fe2O4magnetic nanoparticles embedded in an Ecoflex matrix. The nanoparticles, synthesized via co-precipitation, exhibit a strong magnetic response, while Ecoflex ensures high stretchability and skin-mountable adaptability. The comprehensive structural, morphological, and magnetic analyses confirm the formation of a uniform and multifunctional film. The optimized device delivers a peak output voltage of ?8.3 V and a power density of 3.16 mW cm?3under ambient magnetic fields, outperforming conventional soft nanogenerators. The films demonstrate excellent durability under repeated deformation and maintain stable performance at tensile strains up to ?315%. Integration into a soft wearable platform enables real-time gesture recognition, with distinct voltage signals for finger bends and gestures under low-intensity magnetic fields. This work highlights the potential of magnetic/Ecoflex-based nanogenerators in self-powered, wearable, stretchable electronics, smart prosthetics, and intelligent humanmachine interfaces. This journal is The Royal Society of Chemistry, 2025
Yadav, Sandeep Kumar; Salian, Raksha D.; Mathias, Royston; Kumbhakar, Partha
Journal of Materials Chemistry C;Volume;13;Issue;46;pp.23259-23268
All Open Access; Hybrid Gold Open Access
https://doi.org/10.1039/d5tc03220b https://www.scopus.com/pages/publications/105023138553?origin=resultslist
Yadav S.K., Department of Physics and Electronics, Christ University Bangalore, 560029, India; Salian R.D., Department of Physics and Electronics, Christ University Bangalore, 560029, India; Mathias R., Department of Physics and Electronics, Christ University Bangalore, 560029, India; Kumbhakar P., Department of Physics and Electronics, Christ University Bangalore, 560029, India
Systematic investigation on unsymmetrical mesogenic cyanobiphenyl dimers towards optical storage devices: synthesis, mesomorphic, photo switching and DFT studies
This research presents the synthesis and analysis of a novel series of mesogenic dimers comprising cyanobiphenyl and azonaphthyl units. Structural validation was performed using FT-IR, 1H-NMR, 13C-NMR, elemental analysis, mass spectrometry, etc. The dimers thermotropic behaviours were studied through POM and DSC, revealing enantiotropic nematic phases in all cases, with some also showing monotropic smectic C phases. The study explores the relationship between the chemical structure of the dimers and the length of the flexible spacer, the odd-even effect, and their phase transition temperatures. Longer chains tended to form smectic phases, while shorter chains primarily exhibited nematic phases. Computational analysis using B3LYP/6-31g(d,p) and evaluations of electrostatic potential (ESP) and optical properties provided further insight into the electronic structures. Photoisomerization studies demonstrated consistent photochromic responses, with all dimers showing high conversion efficiency (88-95%) under UV light along with similar back relaxation times (?10-12 hours). Optical storage devices prepared by these materials showed excellent contrast between dark and bright states elucidating the importance of such materials for the future. 2025 The Royal Society of Chemistry.
Rabari, Mahima; Hegde, Vasundhara; Hegde, Gurumurthy; Prajapati, A.K.
Journal of Materials Chemistry C;Volume;13;Issue;21;pp.10700-10713
https://doi.org/10.1039/d5tc00421g https://www.scopus.com/pages/publications/105003871846?origin=resultslist
Rabari M., Department of Chemistry, Faculty of Science, The Maharaja Sayajirao University of Baroda, Vadodara, 390002, India; Hegde V., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India; Hegde G., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Centre for Advanced Research and Development, Christ University, Hosur Road, Bengaluru, 560029, India; Prajapati A.K., Department of Chemistry, Faculty of Science, The Maharaja Sayajirao University of Baroda, Vadodara, 390002, India