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14 results on '"Fetick, Romain"'

1. The ESO's Extremely Large Telescope Working Groups

Author

Padovani, Paolo, Cirasuolo, Michele, van der Burg, Remco, Cantalloube, Faustine, George, Elizabeth, Kasper, Markus, Leschinski, Kieran, Martins, Carlos, Milli, Julien, Möhler, Sabine, Neeser, Mark, Neichel, Benoit, Otarola, Angel, Sánchez-Janssen, Rubén, Serra, Benoit, Smette, Alain, Valenti, Elena, Verinaud, Christophe, Vernet, Joël, Absil, Olivier, Agapito, Guido, Andersen, Morten, Arcidiacono, Carmelo, Arko, Matej, Baudoz, Pierre, Beltramo-Martin, Olivier, Biancalani, Enrico, Bierwirth, Thomas, Burtscher, Leonard, Carlà, Giulia, Castro-Almazán, Julio A., Cheffot, Anne-Laure, Coccato, Lodovico, Correia, Carlos, Fetick, Romain, Fiorentino, Giuliana, Fusco, Thierry, García-Lorenzo, Begoña, Fusillo, Nicola Gentile, Gonzalez, Oscar, Grazian, Andrea, Gullieuszik, Marco, Hainaut, Olivier, Ivanov, Valentin, Kaasinen, Melanie, Kaddad, Darshan, Kamiński, Tomasz, Kausch, Wolfgang, Kerber, Florian, Kimeswenger, Stefan, Kokotanekova, Rosita, Kuznetsov, Arseniy, Lau, Alexis, Louarn, Miska Le, Lemmel, Frédéric, Liske, Jochen, Curto, Gaspare Lo, Lucsanyi, David, Lundin, Lars, Noll, Stefan, Oberti, Sylvain, Osborn, James, Masciadri, Elena, Milaković, Dinko, Murphy, Michael T., Pedichini, Fernando, Santaella, Miguel Pereira, Piazzesi, Roberto, López, Javier Piqueras, Plantet, Cédric, Prod'homme, Thibaut, Przybilla, Norbert, Puech, Mathieu, Reid, Derryck T., Reiners, Ansgar, Rijnenberg, Rutger, Rodrigues, Myriam, Rossi, Fabio, Routledge, Laurence, Smit, Hans, Tecza, Mathias, Thatte, Niranjan, van Boekel, Roy, Verma, Aprajita, and Vigan, Arthur

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Since 2005 ESO has been working with its community and industry to develop an extremely large optical/infrared telescope. ESO's Extremely Large Telescope, or ELT for short, is a revolutionary ground-based telescope that will have a 39-metre main mirror and will be the largest visible and infrared light telescope in the world. To address specific topics that are needed for the science operations and calibrations of the telescope, thirteen specific working groups were created to coordinate the effort between ESO, the instrument consortia, and the wider community. We describe here the goals of these working groups as well as their achievements so far., Comment: 8 pages, 4 figures

Published
2023
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2. Central kinematics of the Galactic globular cluster M80

Author

Göttgens, Fabian, Kamann, Sebastian, Baumgardt, Holger, Dreizler, Stefan, Giesers, Benjamin, Husser, Tim-Oliver, Brok, Mark den, Fétick, Romain, Krajnović, Davor, and Weilbacher, Peter M.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We use spectra observed with the integral-field spectrograph MUSE to reveal the central kinematics of the Galactic globular cluster Messier 80 (M80, NGC 6093). Using observations obtained with the recently commissioned narrow-field mode of MUSE, we are able to analyse 932 stars in the central 7.5 arcsec by 7.5 arcsec of the cluster for which no useful spectra previously existed. Mean radial velocities of individual stars derived from the spectra are compared to predictions from axisymmetric Jeans models, resulting in radial profiles of the velocity dispersion, the rotation amplitude, and the mass-to-light ratio. The new data allow us to search for an intermediate-mass black hole (IMBH) in the centre of the cluster. Our Jeans model finds two similarly probable solutions around different dynamical cluster centres. The first solution has a centre close to the photometric estimates available in the literature and does not need an IMBH to fit the observed kinematics. The second solution contains a location of the cluster centre that is offset by about 2.4 arcsec from the first one and it needs an IMBH mass of $4600^{+1700}_{-1400}$ solar masses. N-body models support the existence of an IMBH in this cluster with a mass of up to 6000 solar masses in this cluster, although models without an IMBH provide a better fit to the observed surface brightness profile. They further indicate that the cluster has lost nearly all stellar-mass black holes. We further discuss the detection of two potential high-velocity stars with radial velocities of 80 to 90 km/s relative to the cluster mean., Comment: accepted for publication in MNRAS; data can be found here: https://doi.org/10.25625/VCNHOR

Published
2021
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3. Joint estimation of atmospheric and instrumental defects using a parsimonious point spread function model.On-sky validation using state of the art worldwide adaptive-optics assisted instruments

Author

Beltramo-Martin, Olivier, Fétick, Romain, Neichel, Benoit, and Fusco, Thierry

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Modeling the optical point spread function (PSF) is particularly challenging for adaptive optics (AO)-assisted observations owing to the its complex shape and spatial variations. We aim to (i) exhaustively demonstrate the accuracy of a recent analytical model from comparison with a large sample of imaged PSFs, (ii) assess the conditions for which the model is optimal, and (iii) unleash the strength of this framework to enable the joint estimation of atmospheric parameters, AO performance and static aberrations. We gathered 4812 on-sky PSFs obtained from seven AO systems and used the same fitting algorithm to test the model on various AO PSFs and diagnose AO performance from the model outputs. Finally, we highlight how this framework enables the characterization of the so-called low wind effect on the SPHERE instrument and piston cophasing errors on the Keck II telescope. Over 4812 PSFs, the model reaches down to 4% of error on both the Strehl-ratio (SR) and full width at half maximum (FWHM). We particularly illustrate that the estimation of the Fried parameter, which is one of the model parameters, is consistent with known seeing statistics and follows expected trends in wavelength using the MUSE instrument ($\lambda^{6/5}$) and field (no variations) from GSAOI images with a standard deviation of 0.4cm. Finally, we show that we can retrieve a combination of differential piston, tip, and tilt modes introduced by the LWE that compares to ZELDA measurements, as well as segment piston errors from the Keck II telescope and particularly the stair mode that has already been revealed from previous studies. This model matches all types of AO PSFs at the level of 4% error and can be used for AO diagnosis, post-processing, and wavefront sensing purposes.

Published
2020
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4. Blind deconvolution in astronomy with adaptive optics: the parametric marginal approach

Author

Fétick, Romain, Mugnier, Laurent, Fusco, Thierry, and Neichel, Benoit

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

One of the major limitations of adaptive optics (AO) corrected image post-processing is the lack of knowledge on the system point spread function (PSF). The PSF is not always available as a direct imaging on isolated point like objects such as stars. Its prediction using AO telemetry also suffers from serious limitations and requires complex and yet not fully operational algorithms. A very attractive solution consists in a direct PSF estimation using the scientific images themselves thanks to blind or myopic post-processing approaches. We demonstrate that such approaches suffer from severe limitations when a joint restitution of object and PSF parameters is performed. As an alternative we propose here a marginalized PSF identification that overcomes this limitation. Then the PSF is used for image post-processing. Here we focus on deconvolution, a post-processing technique to restore the object, given the image and the PSF. We show that the PSF estimated by marginalisation provides good quality deconvolution. The full process of marginalized PSF estimation and deconvolution constitutes a successful blind deconvolution technique. It is tested on simulated data to measure its performance. It is also tested on experimental adaptive optics images of the asteroid 4-Vesta by VLT/SPHERE/Zimpol to demonstrate application to on-sky data.

Published
2020
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5. Physics-based model of the adaptive-optics corrected point-spread-function

Author

Fétick, Romain, Fusco, Thierry, Neichel, Benoit, Mugnier, Laurent, Beltramo-Martin, Olivier, Bonnefois, Aurélie, Petit, Cyril, Milli, Julien, Vernet, Joel, Oberti, Sylvain, and Bacon, Roland

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Context. Adaptive optics (AO) systems greatly increase the resolution of large telescopes, but produce complex point spread function (PSF) shapes, varying in time and across the field of view. This PSF must be accurately known since it provides crucial information about optical systems for design, characterisation, diagnostics and image post processing. Aims. We develop here a model of the AO long exposure PSF, adapted to various seeing conditions and any AO system. This model is made to match accurately both the core of the PSF and its turbulent halo. Methods. The PSF model we develop is based on a parsimonious parameterization of the phase power spectral density with only five parameters to describe circularly symmetric PSFs and seven parameters for asymmetrical ones. Moreover, one of the parameters is directly the Fried parameter r0 of the turbulence s strength. This physical parameter is an asset in the PSF model since it can be correlated with external measurements of the r0, such as phase slopes from the AO real time computer (RTC) or site seeing monitoring. Results. We fit our model against endtoend simulated PSFs using OOMAO tool, and against on sky PSFs from the SPHERE ZIMPOL imager and the MUSE integral field spectrometer working in AO narrowfield mode. Our model matches the shape of the AO PSF both in the core and the halo, with a sub 1 percent relative error for simulated and experimental data. We also show that we retrieve the r0 parameter with subcentimeter precision on simulated data. For ZIMPOL data, we show a correlation of 97 percent between our r0 estimation and the RTC estimation. Finally, MUSE allows us to test the spectral dependency of the fitted r0 parameter. It follows the theoretical $\lambda^{6/5}$ evolution with a standard deviation of 0.3 cm. Evolution of other PSF parameters, such as residual phase variance or aliasing, is also discussed.

Published
2019
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6. Performance characterization and near-real-time monitoring of MUSE adaptive optics modes at Paranal

Author

Wevers, Thomas, primary, Selman, Fernando J., additional, Reyes, Axel, additional, Vega Pallauta, Macarena, additional, Hartke, Johanna, additional, Bian, Fuyan, additional, Beltramo-Martin, Olivier A., additional, Fetick, Romain, additional, Kamann, Sebastian, additional, Kolb, Johann, additional, Kravtsov, Timo, additional, Moya, Cristobal, additional, Neichel, Benoit, additional, Oberti, Sylvain, additional, Reyes, Claudia, additional, and Valenti, Elena, additional

Published
2022
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7. The ESO’s Extremely Large Telescope Working Groups

Author

Padovani, Paolo, Cirasuolo, Michele, van der Burg, Remco, Cantalloube, Faustine, George, Elizabeth, Kasper, Markus, Leschinski, Kieran, Martins, Carlos, Milli, Julien, Möhler, Sabine, Neeser, Mark, Neichel, Benoit, Otarola, Angel, Sánchez-Janssen, Rubén, Serra, Benoit, Smette, Alain, Valenti, Elena, Verinaud, Christophe, Vernet, Joël, Absil, Olivier, Agapito, Guido, Andersen, Morten, Arcidiacono, Carmelo, Arko, Matej, Baudoz, Pierre, Beltramo-Martin, Olivier, Biancalani, Enrico, Bierwirth, Thomas, Burtscher, Leonard, Carlà, Giulia, Castro-Almazán, Julio A., Cheffot, Anne-Laure, Coccato, Lodovico, Correia, Carlos, Fetick, Romain, Fiorentino, Giuliana, Fusco, Thierry, García-Lorenzo, Begoña, Fusillo, Nicola Gentile, Gonzalez, Oscar, Grazian, Andrea, Gullieuszik, Marco, Hainaut, Olivier, Ivanov, Valentin, Kaasinen, Melanie, Kaddad, Darshan, Kamiński, Tomasz, Kausch, Wolfgang, Kerber, Florian, Kimeswenger, Stefan, Kokotanekova, Rosita, Kuznetsov, Arseniy, Lau, Alexis, Louarn, Miska Le, Lemmel, Frédéric, Liske, Jochen, Curto, Gaspare Lo, Lucsanyi, David, Lundin, Lars, Noll, Stefan, Oberti, Sylvain, Osborn, James, Masciadri, Elena, Milaković, Dinko, Murphy, Michael T., Pedichini, Fernando, Santaella, Miguel Pereira, Piazzesi, Roberto, López, Javier Piqueras, Plantet, Cédric, Prod'homme, Thibaut, Przybilla, Norbert, Puech, Mathieu, Reid, Derryck T., Reiners, Ansgar, Rijnenberg, Rutger, Rodrigues, Myriam, Rossi, Fabio, Routledge, Laurence, Smit, Hans, Tecza, Mathias, Thatte, Niranjan, van Boekel, Roy, Verma, Aprajita, Vigan, Arthur, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, [SDU]Sciences of the Universe [physics], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Since 2005 ESO has been working with its community and industry to develop an extremely large optical/infrared telescope. ESO's Extremely Large Telescope, or ELT for short, is a revolutionary ground-based telescope that will have a 39-metre main mirror and will be the largest visible and infrared light telescope in the world. To address specific topics that are needed for the science operations and calibrations of the telescope, thirteen specific working groups were created to coordinate the effort between ESO, the instrument consortia, and the wider community. We describe here the goals of these working groups as well as their achievements so far., Comment: 8 pages, 4 figures

Published
2022
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8. Current status of PAPYRUS : the pyramid based adaptive optics system at LAM/OHP

Author

Muslimov, Eduard, primary, Chambouleyron, Vincent, additional, Levraud, Nicolas, additional, Lau, Alexis, additional, Caillat, Amandine, additional, Pedreros, Felipe, additional, Otten, Gilles, additional, El Hadi, Kacem, additional, Joaquina, Kelly, additional, Lopez, Maxime, additional, El Morsy, Mona, additional, Beltramo-Martin, Olivier, additional, Fetick, Romain, additional, Ke, Zibo, additional, Laginja, Iva, additional, Fusco, Thierry, additional, Neichel, Benoit, additional, Sauvage, Jean François, additional, Schmitt, Jérome, additional, Le Van Suu, Auguste, additional, and Charton, Julien, additional

Published
2021
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9. HARMONI: first light spectroscopy for the ELT: instrument final design and quantitative performance predictions

Author

Thatte, Niranjan, primary, Bryson, Ian, additional, Clarke, Fraser, additional, Ferraro-Wood, Vanessa, additional, Fusco, Thierry, additional, Le Mignant, David, additional, Melotte, Dave J., additional, Neichel, Benoit, additional, Schnetler, Hermine, additional, Tecza, Matthias, additional, Arribas, Santiago, additional, Crespo, Alejandro, additional, Estrada Piqueras, Alberto, additional, García García, Miriam, additional, Pereira Santaella, Miguel, additional, Piqueras López, Javier, additional, Blaizot, Jeremy, additional, Bouché, Nicholas, additional, Boudon, Didier, additional, Chapuis, Diane, additional, Daguise, Eric, additional, Disseau, Karen, additional, Guibert, Mtthieu, additional, Jarno, Aurelien, additional, Jeanneau, Alexandre, additional, Laurent, Florence, additional, Loupias, Magali, additional, Migniau, Jean-Emmanuel, additional, Piqueras, Laure, additional, Remillieux, Alban, additional, Richard, Johan, additional, Pécontal-Rousset, Arlette, additional, Bardou, Lisa, additional, Close, Madeline M., additional, Deshmukh, Rishi, additional, Dimoudi, Sofia, additional, Dubbledam, Marc, additional, King, David, additional, Morris, Simon, additional, Morris, Timothy J., additional, O'Brien, Kieran S., additional, Staykov, Lazar, additional, Swinbank, Mark, additional, Townson, Matthew, additional, Younger, Eddy, additional, Accardo, Matteo, additional, Avarez Mendez, Domingo, additional, Conzelmann, Ralf, additional, Egner, Sebastian, additional, George, Elizabeth M., additional, Gonté, Frederic, additional, Hopgood, Joshua, additional, Ives, Derek, additional, Mehrgan, Leander, additional, Mueller, Eric, additional, Peroux, Celine, additional, Vernet, Joel, additional, Alonso-Sánchez, Ángel, additional, Giuseppina, Battaglia, additional, Cagigas, Miguel, additional, Delgado, Jose Miguel, additional, Fernandez Izquierdo, Patricia, additional, Fragoso López, Ana Belén, additional, García-Lorenzo, Maria Begoña, additional, Hernandez Suarez, Elvio, additional, Herreros Linares, José Miguel, additional, Joven, Enrique, additional, López, Roberto, additional, Martín Hernando, Yolanda, additional, Mediavilla, Evencio, additional, Monreal, Ana, additional, Peñate Castro, José, additional, Rasilla, Jose Luis, additional, Rebolo, Rafael, additional, Rodríguez-Ramos, Luis Fernando, additional, Vega Moreno, Afrodisio, additional, Viera, Teodora, additional, Carlotti, Alexis, additional, Correia, Jean-Jacques, additional, Delboulbe, Alain, additional, Guieu, Sylvain, additional, Hours, Adrien, additional, Hubert, Zoltan, additional, Jocou, Laurent, additional, Magnard, Yves, additional, Moulin, Thibaut, additional, Pancher, Fabrice, additional, Rabou, Patrick, additional, Stadler, Eric, additional, Contini, Thierry, additional, Larrieu, Marie, additional, Fantei-Caujolle, Yan, additional, Lecron, Daniel, additional, Rousseau, Sylvain, additional, Beltramo-Martin, Olivier, additional, Bon, William, additional, Bonnefoi, Anne, additional, Ceria, William, additional, Choquet, Elodie, additional, Correia, Carlos, additional, Costille, Anne, additional, Dohlen, Kjetil, additional, Ducret, Franck, additional, El Hadi, Kacem, additional, Epinat, Benoit, additional, Fetick, Romain, additional, Gach, Jean-Luc, additional, Groussin, Oliver, additional, Jaafar, Issa, additional, Le Merrer, Joel, additional, Llored, Marc, additional, Pedreros, Felipe, additional, Renault, Edgard, additional, Sanchez, Patrice, additional, Vigan, Arthur, additional, Vola, Pascal, additional, Lim, Caroline, additional, Vedrenne, Nicola, additional, Petit, Cyril, additional, Sauvage, Jean-Francois, additional, Bagci, Taha, additional, Cann, Nick, additional, Chao Ortiz, Jorge, additional, Elliott, Ellis, additional, Seitis, Tea, additional, Tosh, Ian, additional, Anderson, Josh, additional, Black, Martin, additional, Bond, Charlotte, additional, Born, Andy J., additional, Campbell, Kenny, additional, Campbell, Neil, additional, Carruthers, James, additional, Cochrane, William, additional, Dobson, Naomi, additional, Evans, Chris J., additional, Gallie, Angus, additional, Gonzalez, Oscar, additional, Harman, Joel, additional, Henry, David M., additional, Humphreys, William, additional, Louth, Tom, additional, Miller, Chris, additional, Montgomery, David M., additional, Murray, John, additional, O'Malley, Norman, additional, Ritchie, Lynn, additional, Sanchez-Janssen, Ruben, additional, Schwartz, Noah, additional, Smith, Patrick, additional, Watt, Stuart, additional, Wells, Martyn, additional, Wilson, Sandi, additional, Gultekin, Kayhan K., additional, Mateo, Mario L., additional, Meyer, Michael, additional, Valluri, Monica, additional, Ahmad, Munadi, additional, Booth, Michael, additional, Capone, John I., additional, Cappellari, Michele, additional, Gooding, David, additional, Grisdale, Kearn, additional, Hidalgo, Andrea, additional, Kariuki, James, additional, Lewis, Ian, additional, Lowe, Adam, additional, Lynn, Jim, additional, Menduina, Alvaro, additional, Ozer, Zeynep, additional, Preece, Roy, additional, Rigopoulou, Dimitra, additional, Rodrigues, Myriam, additional, and Routledge, Laurence, additional

Published
2020
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11. Pallas's formation and internal structure: New insights from VLT/SPHERE

Author

Marsset, Michael, Vernazza, Pierre, Castillo-Rogez, Julie C., Rambaux, Nicolas, Carry, Benoît, Hanus, Josef, Viikinkoski, Matti, Marchis, Franck, Drouard, Alexis, Fetick, Romain, Harissa, Team, Queen's University [Belfast] (QUB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astéroïdes, comètes, météores et éphémérides (ACME), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Astronomie et systèmes dynamiques (ASD), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), and Henry, Florence

Subjects
[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Large (D>100km) asteroids are the most direct remnants of the building blocks of planets. (2) Pallas is the third largest asteroid and the parent body of a small collisional family. Its spectral properties indicate a B-type surface, meaning Pallas is most likely linked to carbonaceous chondrite meteorites. Disc-resolved images have revealed a nearly hydrostatic shape overprinted by long-wavelength concavities (Schmidt et al. 2009, Carry et al. 2010). This was interpreted as evidence for an early phase of internal heating subsequent to Pallas's formation, followed by several large impact craters (Schmidt & Castillo-Rogez 2012). Recent estimates of Pallas's density, 2.40±0.25 g/cm3 (Schmidt et al. 2009), 3.40±0.90 g/cm3 (Carry et al. 2010) and 2.72±0.17 g/cm3 (Hanus et al. 2017), are rather inconsistent and prevent from differentiating among the various models proposed for its internal structure (Schmidt & Castillo-Rogez 2012). This currently limits our understanding of the formation and thermal evolution of Pallas. We report new high-angular resolution observations of Pallas collected in the frame of the SPHERE large survey of the asteroid belt (see Talk by P. Vernazza) with the adaptive-optics-fed SPHERE ZIMPOL camera on the VLT. 40 images acquired at 8 epochs provide a full longitudinal coverage of Pallas's southern hemisphere, with Pallas being resolved with ˜120 pixels along its longest axis. The optimal angular resolution of each image was restored with Mistral (Fusco et al. 2002), a myopic deconvolution algorithm optimised for images with sharp boundaries, which allows the identification of many craters and geological features on Pallas. A precise 3D-shape reconstruction was achieved with the ADAM software (Viikinkoski et al. 2015), providing a high precision estimate of Pallas's 3D shape, volume and hence density. Those are used to explore Pallas's early thermal evolution, its subsequent collisional evolution, and its current internal structure and composition. [1] Carry et al. 2010, Icarus, 205, 460 [2] Fusco et al. 2002, SPIE, 4839, 1065 [3] Hanus et al. 2017, A&A, 601, A114 [4] Schmidt et al. 2009, Science, 326, 275 [5] Schmidt & Castillo-Rogez, Icarus, 218, 478 [6] Viikinkoski et al. 2015, A&A, 576, A8

Published
2018

12. (16) Psyche: A Mesosiderite-like Asteroid With No Moons?

Author

Marchis, Franck, Viikinkoski, Matti, Vernazza, Pierre, Hanus, Josef, Marsset, Michael, Drouard, Alexis, Le Coroller, Hervé, Tazhenova, K., Carry, Benoît, Fetick, Romain, Fusco, Thierry, Durech, Josef, Harissa, Team, Henry, Florence, SETI Institute, Mountain View, California, UNITED STATES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astéroïdes, comètes, météores et éphémérides (ACME), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Asteroid (16) Psyche is the target of the NASA Psyche mission. It is considered as one of the few main-belt bodies that could be an exposed proto-planetary metallic core and that would thus be related to iron meteorites. Such association is however challenged by both its near- and mid-infrared spectral properties (e.g. Hardersen et al. Icarus 175, 2005; Takir et al. AJ, 153, 2017; Landsman et al. Icarus, 304, 2018). We observed (16) Psyche with ESO VLT SPHERE/ZIMPOL as part of our large program (ID 199.C-0074, PI Vernazza) between April 24 and June 6 2018. We use the high-angular resolution of these observations to reconstruct the 3D shape model of Psyche. When combined with the most recent estimates of its mass, the volume that we derive led to a bulk density of 3.99 ± 0.26 g.cm-3 for Psyche. While such density is incompatible at the 3-sigma level with any iron meteorites (˜7.8 g.cm-3), it appears fully consistent with that of stony-iron meteorites such as mesosiderites (density ˜4.25 g.cm-3). Although our observations only covered the northern hemisphere of Psyche, they reveal the presence of two peculiar units in the front views, namely one low and one high brightness regions nicknamed Panthia and Meroe. Meroe unit is about 7% brighter than the surrounding region, whereas the Panthia unit is 8% fainter. Panthia is a depression with a width of 90 km and a depth of 10 km. We did not detect any moons around Psyche and estimate the minimum radius of a moon to be detected around Psyche to 730 ± 100 m at 150 km (so 0.2% x RHill) of the primary and 400 ± 100 m at 2000 km from the primary corresponding to 3% x RHill) where most of the satellites of >100-km asteroids have been seen so far (Yang et al. AJL 820:L35, 2016). Considering that the visible and near-infrared spectral properties of mesosiderites are similar to those of Psyche, there is merit to the initial hypothesis by Davis et al. (1999) that Psyche could be a plausible candidate parent body for mesosiderites (Viikinkoski et al. submitted to A&A, 2018). This material is based upon work partially supported by the National Science Foundation under Grant No 1743015.

Published
2018

14. HARMONI at ELT: overview of the capabilities and expected performance of the ELT's first light, adaptive optics assisted integral field spectrograph.

Author

Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Thatte, Niranjan A., Melotte, Dave, Neichel, Benoit, Le Mignant, David, Bryson, Ian, Clarke, Fraser, Ferraro-Wood, Vanessa, Fusco, Thierry, Gonzalez, Oscar, Schnetler, Hermine, Tecza, Matthias, Wilson, Sandi, Álvarez Urueña, Alonso, Vilaseca, Heribert A., Arribas, Santiago, Carracedo Carballale, Gonzalo José, Crespo, Alejandro, Estrada Piqueras, Alberto, García García, Miriam, Martínez Martín, Cecilai, Pereira Santaella, Miguel, Perna, Michele, Piqueras Lopez, Javier, Bouché, Niolas, Boudon, Didier, Daguise, Eric, Disseau, Karen, Fensch, Jérémy J., Girardot, Adrien, Guibert, Matthieu, Jarno, Aurélien, Jeanneau, Alexandre, Krogager, Jens-Kristian, Laurent, Florence, Loupias, Magali, Migniau, Jean-Emmanuel, Piqueras, Laure, Remillieux, Alban, Richard, Johan, Pecontal, Arlette, Bardou, Lisa F., Barr, David, Cetre, Sylvain, Deshmukh, Rishi, Dimoudi, Sofia, Dubbledam, Marc, Dunn, Andrew, Gadotti, Dimitri, Guy, Joss J., King, David, Little, David J., McLeod, Anna, Morris, Simon, Morris, Tim, O'Brien, Kieran S., Ronson, Emily, Smith, Russell, Staykov, Lazar, Swinbank, Mark, Townson, Matthew, Accardo, Matteo, Alvarez Mendez, Domingo, George, Elizabeth, Hopgood, Joshua, Ives, Derek, Mehrgan, Leander, Mueller, Eric, Reyes, Javier, Conzelmann, Ralf, Gutierrez Cheetham, Pablo, Alonso-Sánchez, Ángel, Battaglia, Giuseppina, Cagigas, Miguel, Chulani, Haresh, Delgado García, Graciela, Fernandez Izquierdo, Patricia, Fragoso López, Ana Belén, García-Lorenzo, Begoña, Hernández González, Alberto, Hernandez Suarez, Elvio, Herreros Linares, Jose Miguel, Joven, Enrique, López López, Roberto, Lujan Gonzalez, Alejandro Antonio, Martín Hernando, Yolanda, Mediavilla, Evencio, Menéndez Mendoza, Saúl, Montoya Martínez, Luz Maria, Peñate Castro, José, Pérez, Álvaro, Rasilla, Jose Luis, Rebolo, Rafael, Rodríguez Ramos, Luis Fernando, Vega-Moreno, Afrodisio, Viera, Teodora, Zanon Dametto, Natacha, Carlotti, Alexis, Correia, Jean-Jacques, Curaba, Stéphane, Delboulbe, Alain, Guieu, Sylvain, Hours, Adrien, Hubert, Zoltan, Jocou, Laurent, Magnard, Yves, Moulin, Thibaut, Pancher, Fabrice, Rabou, Patrick, Stadler, Eric, Vérove, Maxime, Contini, Thierry, Larrieu, Marie, Boebion, Olivier, Fantei-Caujolle, Yan, Lecron, Daniel, Rousseau, Sylvain, Amram, Philippe, Beltramo-Martin, Olivier, Bon, William, Bonnefoi, Anne, Ceria, William, Challita, Zalpha, Charles, Yannick, Choquet, Elodie, Correia, Carlos, Costille, Anne, Dohlen, Kjetil, Ducret, Franck, El Hadi, Kacem, Gach, Jean-Luc, Gimenez, Jean-Luc, Groussin, Olivier, Jaquet, Marc, Jouve, Pierre, Madec, Fabrice, Pedreros, Felipe, Renault, Edgard, Sanchez, Patrice, Vigan, Arthur, Vola, Pascal, Zavago, Annie, Fetick, Romain, Lim, Caroline, Petit, Cyril, Sauvage, Jean-Francois, Védrenne, Nicolas, Bagci, Fehim Taha, Caldwell, Martin E., Elliott, Ellis, Hiscock, Peter, Johnson, Emma, Nalagatla, Murali, Seitis, Aristea, Wells, Mark, Black, Martin, Bond, Charlotte, Brierley, Saskia, Campbell, Kenny, Campbell, Neil, Carruthers, James, Cochrane, William, Evans, Chris, Harman, Joel, Humphreys, William, Louth, Thomas, Miller, Chris, Montgomery, David, Murali, Meenu, Murray, John, O'Malley, Norman, Sanchez-Janssen, Ruben, Schwartz, Noah, Smith, Patrick, Strachan, Jonathan, Todd, Stephen, Watt, Stuart, Wells, Martyn, Yaqoob, Asim, Bell, Eric, Gnedin, Oleg O., Gultekin, Kayhan, Mateo, Mario, Meyer, Michael, Ahmad, Munadi, Birkby, Jayne, Booth, Michael, Cappellari, Michele, Castillo Dominguez, Edgar, Chao Ortiz, Jorge, Gooding, David, Grisdale, Kearn, Hidalgo, Andrea, Hogan, Laurence, Kariuki, James, Lewis, Ian, Lowe, Adam, Ozer, Zeynep, Routledge, Laurence, Rigopoulou, Dimitra, and York, Alec

Published
2022
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