Extremely Large Telescope: publications

Ground-breaking Exoplanet Science with the ANDES spectrograph at the ELT

(2023)

Authors:

Enric Palle, Katia Biazzo, Emeline Bolmont, Paul Molliere, Katja Poppenhaeger, Jayne Birkby, Matteo Brogi, Gael Chauvin, Andrea Chiavassa, Jens Hoeijmakers, Emmanuel Lellouch, Christophe Lovis, Roberto Maiolino, Lisa Nortmann, Hannu Parviainen, Lorenzo Pino, Martin Turbet, Jesse Wender, Simon Albrecht, Simone Antoniucci, Susana C Barros, Andre Beaudoin, Bjorn Benneke, Isabelle Boisse, Aldo S Bonomo, Francesco Borsa, Alexis Brandeker, Wolfgang Brandner, Lars A Buchhave, Anne-Laure Cheffot, Robin Deborde, Florian Debras, Rene Doyon, Paolo Di Marcantonio, Paolo Giacobbe, Jonay I Gonzalez Hernandez, Ravit Helled, Laura Kreidberg, Pedro Machado, Jesus Maldonado, Alessandro Marconi, BL Canto Martins, Adriano Miceli, Christoph Mordasini, Mamadou N'Diaye, Andrezj Niedzielski, Brunella Nisini, Livia Origlia, Celine Peroux, Alex GM Pietrow, Enrico Pinna, Emily Rauscher, Sabine Reffert, Philippe Rousselot, Nicoletta Sanna, Adrien Simonnin, Alejandro Suarez Mascareno, Alessio Zanutta, Mathias Zechmeister

INSPIRE: INvestigating Stellar Population In RElics – V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness

Monthly Notices of the Royal Astronomical Society 91̽�� University Press (OUP) 527:3 (2023) 8793-8811

Authors:

C Spiniello, G D’Ago, L Coccato, J Hartke, C Tortora, A Ferré-Mateu, C Pulsoni, M Cappellari, M Maksymowicz-Maciata, M Arnaboldi, D Bevacqua, A Gallazzi, LK Hunt, F La Barbera, I Martín-Navarro, NR Napolitano, M Radovich, P Saracco, D Scognamiglio, M Spavone, S Zibetti

WISDOM project -- XVIII. Molecular gas distributions and kinematics of three megamaser galaxies

(2023)

Authors:

Fu-Heng Liang, Mark D Smith, Martin Bureau, Feng Gao, Timothy A Davis, Michele Cappellari, Jacob S Elford, Jenny E Greene, Satoru Iguchi, Federico Lelli, Anan Lu, Ilaria Ruffa, Thomas G Williams, Hengyue Zhang

Supermassive black hole mass in the massive elliptical galaxy M87 from integral-field stellar dynamics using OASIS and MUSE with adaptive optics: assessing systematic uncertainties

Monthly Notices of the Royal Astronomical Society 91̽�� University Press (OUP) 527:2 (2023) 2341-2361

Authors:

David A Simon, Michele Cappellari, Johanna Hartke

Bright-Moon sky as a wide-field linear Polarimetric flat source for calibration

Astronomy & Astrophysics EDP Sciences 679 (2023) A68-A68

Authors:

S Maharana, S Kiehlmann, D Blinov, V Pelgrims, V Pavlidou, K Tassis, JA Kypriotakis, AN Ramaprakash, RM Anche, A Basyrov, K Deka, HK Eriksen, T Ghosh, E Gjerløw, N Mandarakas, E Ntormousi, GV Panopoulou, A Papadaki, T Pearson, SB Potter, ACS Readhead, R Skalidis, IK Wehus

Abstract:

Context. Next-generation wide-field optical polarimeters such as Wide-Area Linear Optical Polarimeters (WALOPs) have a field of view (FoV) of tens of arcminutes. Wide-field polarimetric flat sources are essential to the efficient and accurate calibration of these instruments. However, no established wide-field polarimetric standard or flat sources exist at present. Aims. This study tests the feasibility of using the polarized sky patches of the size of around 10 × 10 arcminutes2, at a distance of up to 20° from the Moon, on bright-Moon nights as a wide-field linear polarimetric flat source. Methods. We observed 19 patches of the sky adjacent to the bright-Moon with the RoboPol instrument in the SDSS-r broadband filter. These patches were observed on five nights within two days of the full-Moon across two RoboPol observing seasons. Results. We find that for 18 of the 19 patches, the uniformity in the measured normalized Stokes parameters q and u is within 0.2%, with 12 patches exhibiting uniformity within 0.07% or better for both q and u simultaneously, making them reliable and stable wide-field linear polarization flats. Conclusions. We demonstrate that the sky on bright-Moon nights is an excellent wide-field linear polarization flat source. Various combinations of the normalized Stokes parameters q and u can be obtained by choosing suitable locations of the sky patch with respect to the Moon.

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