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27 results on '"Thizy, O."'

1. Evolution of the disk of pi Aqr: from near-disappearance to a strong maximum

Author

Naze, Y., Rauw, G., Flo, J . Guarro, De Bruin, A., Garde, O., Thizy, O., Houpert, F., Pollmann, E., Sawicki, C. J., Leonardi, M., Moll, M., Quandt, C. T., Berardi, P., Lester, T., Fosanelli, P., Favaro, A., Terry, J. N., Graham, K., Mauclaire, B., Bohlsen, T., Pujol, M., Bertrand, E., Bryssinck, E., Desnoux, V., Lailly, P., Montier, J., Mannucci, M., Montigiani, N., Stiewing, A., Daglen, J., Kreider, C., Lemoult, T., and Rodda, T.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Some Be stars display important variability of the strength of the emission lines formed in their disk. This is notably the case of pi Aqr. We present here the recent evolution of the Be disk in this system thanks to spectra collected by amateur spectroscopists since the end of 2013. A large transition occurred: the emission linked to the Be disk nearly disappeared in January 2014, but the disk has recovered, with a line strength now reaching levels only seen during the active phase of 1950--1990. In parallel to this change in strength occurs a change of disk structure, notably involving the disappearance of the strong asymmetry responsible for the V/R modulation., Comment: accepted by New Astronomy

Published
2019
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2. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author

Marciniak, A., Alí-Lagoa, V., Müller, T. G., Szakáts, R., Molnár, L., Pál, A., Gaca, E. Podlewska, Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Bąk, M. Butkiewicz, Crippa, R., Duffard, R., Ditteon, R., Feuerbach, M., Fauvaud, S., Garlitz, J., Geier, S., Goncalves, R., Grice, J., Grześkowiak, I., Hirsch, R., Horbowicz, J., Kamiński, K., Kamińska, M. K., Kim, D. -H., Kim, M. -J., Konstanciak, I., Kudak, V., Kulczak, P., Maestre, J. L., Manzini, F., Marks, S., Monteiro, F., Ogłoza, W., Oszkiewicz, D., Pilcher, F., Perig, V., Polakis, T., Polińska, M., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Thizy, O., Trela, P., Urakawa, S., Żejmo, M., and Żukowski, K.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the sub-surface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 hours, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3$^{+33}_{-3}$ and 45$^{+60}_{-30}$ Jm$^{-2}$s$^{-1/2}$K$^{-1}$. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2019
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3. The 2011 Periastron Passage of the Be Binary delta Scorpii

Author

Miroshnichenko, A. S., Pasechnik, A. V., Manset, N., Carciofi, A. C., Rivinius, Th., Stefl, S., Gvaramadze, V. V., Ribeiro, J., Fernando, A., Garrel, T., Knapen, J. H., Buil, C., Heathcote, B., Pollmann, E., Mauclaire, B., Thizy, O., Martin, J., Zharikov, S. V., Okazaki, A. T., Gandet, T. L., Eversberg, T., and Reinecke, N.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We describe the results of the world-wide observing campaign of the highly eccentric Be binary system delta Scorpii 2011 periastron passage which involved professional and amateur astronomers. Our spectroscopic observations provided a precise measurement of the system orbital period at 10.8092+/- 0.0005 years. Fitting of the He II 4686A line radial velocity curve determined the periastron passage time on 2011 July 3, UT 9:20 with a 0.9--day uncertainty. Both these results are in a very good agreement with recent findings from interferometry. We also derived new evolutionary masses of the binary components (13 and 8.2 Msun) and a new distance of 136 pc from the Sun, consistent with the HIPPARCOS parallax. The radial velocity and profile variations observed in the H_alpha line near the 2011 periastron reflected the interaction of the secondary component and the circumstellar disk around the primary component. Using these data, we estimated a disk radius of 150 Rsun. Our analysis of the radial velocity variations measured during the periastron passage time in 2000 and 2011 along with those measured during the 20th century, the high eccentricity of the system, and the presence of a bow shock-like structure around it suggest that delta Sco might be a runaway triple system. The third component should be external to the known binary and move on an elliptical orbit that is tilted by at least 40 degree with respect to the binary orbital plane for such a system to be stable and responsible for the observed long-term radial velocity variations., Comment: 35 pages, 6 figures, 3 tables, accepted to ApJ

Published
2013
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4. Multisite spectroscopic seismic study of the beta Cep star V2052 Oph: inhibition of mixing by its magnetic field

Author

Briquet, M., Neiner, C., Aerts, C., Morel, T., Mathis, S., Reese, D. R., Lehmann, H., Costero, R., Echevarria, J., Handler, G., Kambe, E., Hirata, R., Masuda, S., Wright, D., Yang, S., Pintado, O., Mkrtichian, D., Lee, B. -C., Han, I., Bruch, A., De Cat, P., Uytterhoeven, K., Lefever, K., Vanautgaerden, J., de Batz, B., Frémat, Y., Henrichs, H., Geers, V. C., Martayan, C., Hubert, A. M., Thizy, O., and Tijani, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We used extensive ground-based multisite and archival spectroscopy to derive observational constraints for a seismic modelling of the magnetic beta Cep star V2052 Ophiuchi. The line-profile variability is dominated by a radial mode (f_1=7.14846 d^{-1}) and by rotational modulation (P_rot=3.638833 d). Two non-radial low-amplitude modes (f_2=7.75603 d^{-1} and f_3=6.82308 d^{-1}) are also detected. The four periodicities that we found are the same as the ones discovered from a companion multisite photometric campaign (Handler et al. 2012) and known in the literature. Using the photometric constraints on the degrees l of the pulsation modes, we show that both f_2 and f_3 are prograde modes with (l,m)=(4,2) or (4,3). These results allowed us to deduce ranges for the mass (M \in [8.2,9.6] M_o) and central hydrogen abundance (X_c \in [0.25,0.32]) of V2052 Oph, to identify the radial orders n_1=1, n_2=-3 and n_3=-2, and to derive an equatorial rotation velocity v_eq \in [71,75] km s^{-1}. The model parameters are in full agreement with the effective temperature and surface gravity deduced from spectroscopy. Only models with no or mild core overshooting (alpha_ov \in [0,0.15] local pressure scale heights) can account for the observed properties. Such a low overshooting is opposite to our previous modelling results for the non-magnetic beta Cep star theta Oph having very similar parameters, except for a slower surface rotation rate. We discuss whether this result can be explained by the presence of a magnetic field in V2052 Oph that inhibits mixing in its interior., Comment: 12 pages, 6 figures and 5 tables; accepted for publication in MNRAS on 2012 August 15

Published
2012
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5. High cadence measurement of neutral sodium and potassium absorption during the 2009-2011 eclipse of epsilon Aurigae

Author

Leadbeater, R., Buil, C., Garrel, T., Gorodenski, S., Hansen, T., Schanne, L., Stencel, R., Stober, B., and Thizy, O.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The results of a spectroscopic survey of epsilon Aurigae during eclipse using a network of small telescopes are presented. The spectra have a resolution of 0.35 to 0.65{\AA} and cover the period 2008 to 2012 with a typical interval of 4 days during eclipse. This paper specifically covers variations in the K I 7699{\AA}, Na D and Mg II 4481{\AA} lines. Absorption started increasing in the KI 7699{\AA} line 3 months before the eclipse began photometrically and had not returned to pre eclipse levels by the end of the survey March 2012, 7 months after the brightness had returned to normal outside eclipse levels. The contribution of the eclipsing object to the KI 7699{\AA} line has been isolated and the data show the excess absorption increasing and decreasing in a series of steps during ingress and egress. This is interpreted as an indication of structure within the eclipsing object. The F star is totally obscured by the eclipsing object at the Na D wavelength during eclipse. The radial velocity of the F star and the mean and maximum radial velocity of the eclipsing material in front of the F star at any given time have been isolated and tracked throughout the eclipse. The quasi-periodic variations seen in the F star RV outside eclipse continued during the eclipse. It is hoped that these results can be used to constrain proposed models of the system and its components., Comment: 20 pages including 2 tables and 11 figures. Submitted to The Journal of the American Association of Variable Star Observers 14th May 2012

Published
2012

6. On the incidence of magnetic fields in slowly-pulsating B, Beta Cephei and B-type emission line stars

Author

Silvester, J., Neiner, C., Henrichs, H. F., Wade, G. A., Petit, V., Alecian, E., Huat, A. -L., Martayan, C., Power, J., and Thizy, O.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We have obtained 40 high-resolution circular spectropolarimetric measurements of 12 slowly-pulsating B (SPB) stars, 8 Beta Cephei stars and two Be stars with the ESPaDOnS and NARVAL spectropolarimeters. The aim of these observations is to evaluate recent claims of a high incidence of magnetic field detections in stars of these types obtained using low-resolution spectropolarimetry by Hubrig (2006), Hubrig (2007) and Hubrig (2009). The precision achieved is generally comparable to or superior to that obtained by Hubrig et al., although our new observations are distinguished by their resolution of metallic and He line profiles, and their consequent sensitivity to magnetic fields of zero net longitudinal component. In the SPB stars we confirm the detection of magnetic field in one star (16 Peg), but find no evidence of the presence of fields in the remaining 11. In the Beta Cep stars, we detect a field in xi^1 CMa, but not in any of the remaining 7 stars. Finally, neither of the two B-type emission line stars shows any evidence of magnetic field. Based on our results, we conclude that fields are not common in SPB, Beta Cep and B-type emission line stars, consistent with the general rarity of fields in the broader population of main sequence B-type stars., Comment: Accepted - MNRAS

Published
2009
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7. The magnetic field of the B3V star 16 Pegasi

Author

Henrichs, H. F., Neiner, C., Schnerr, R. S., Verdugo, E., Alecian, A., Catala, C., Cochard, F., Gutiérrez, J., Huat, A. -L., Silvester, J., and Thizy, O.

Subjects
Astrophysics
Abstract

The Slowly Pulsating B3V star 16 Pegasi was discovered by Hubrig (2006) to be magnetic, based on low-resolution spectropolarimetric observations with FORS1 at the VLT. We have confirmed the presence of a magnetic field with new measurements with the spectropolarimeters Narval at TBL, France and Espadons at CFHT, Hawaii during 2007. The most likely period is about 1.44 d for the modulation of the field, but this could not be firmly established with the available data set. No variability has been found in the UV stellar wind lines. Although the star was reported once to show H alpha in emission, there exists at present no confirmation that the star is a Be star., Comment: 2 pages, 4 figures, contrubuted poster at IAU Symposium 259 "Cosmic Magnetic Fields: from Planets, to Stars and Galaxies", Tenerife, Spain, November 3-7, 2008

Published
2008
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8. FRIPON: a worldwide network to track incoming meteoroids

Author

Marsset, Michaël, Brož, Miroslav, Castillo-Rogez, Julie, Hanuš, Josef, Viikinkoski, Matti, Ševeček, Pavel, Marchis, Franck, Podlewska-Gaca, Edyta, Asphaug, Erik, Bartczak, Przemyslaw, Berthier, Jérôme, Cipriani, Fabrice, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Ferrais, Marin, Fétick, Romain, Fusco, Thierry, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Richardson, Derek, Santana-Ros, Toni, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, Yang, Bin, Colas, François, Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, Mirel, Blanpain, C., Gattacceca, J., Jorda, Laurent, Lecubin, J., Marmo, C., Rault, J., Vaubaillon, J., Vernazza, Pierre, Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Trigo-Rodriguez, J., Lamy, H., Behrend, R., Ferrière, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G., Valsecchi, G., Volpicelli, C., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, Emmanuel, Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appéré, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Bǎdescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boacă, I., Boatǎ, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, Ph., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J., Corp, L., Costa, M., Costard, F., COTTIER, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J., D’Agostino, G., Daiffallah, K., Dǎnescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F., Drouard, Alexis, Dumont, J., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J., Joy, K., Julien, J., Kacerek, R., Kaire, M., Kempf, M., Koschny, D., Krier, C., Kwon, M., Lacassagne, L., Lachat, D., Lagain, A., Laisné, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J., Lecomte, J., Le Dû, P., LELONG, F., Lera, S., Leoni, J., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., LOCATELLI, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J., Martin-Brisset, J., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J., Meza, E., Moggi Cecchi, V., Moiroud, J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacşu, L., Notez, P., Ory, M., Pace, E., Paganelli, M., Pagola, A., Pajuelo, M., Palacián, J., Pallier, G., Paraschiv, P., Pardini, R., Pavone, M., Pavy, G., Payen, G., Pegoraro, A., Peña-Asensio, E., Perez, L., Pérez-Hoyos, S., Perlerin, V., Peyrot, A., Peth, F., Pic, V., Pietronave, S., Pilger, C., Piquel, M., Pisanu, T., Poppe, M., Portois, L., Prezeau, J., Pugno, N., Quantin, C., Quitté, G., Rambaux, Nicolas, Ravier, E., Repetti, U., Ribas, S., Richard, C., Richard, D., RIGONI, M., Rivet, J., Rizzi, N., Rochain, S., Rojas, J.F., Romeo, M., Rotaru, M., Rotger, M., Rougier, P., Rousselot, P., Rousset, J., Rousseu, D., Rubiera, O., Rudawska, R., Rudelle, J., Ruguet, J.P., Russo, P., Sales, S., Sauzereau, O., Salvati, F., Schieffer, M., Schreiner, D., Scribano, Y., Selvestrel, D., Serra, R., Shengold, L., Shuttleworth, A., Smareglia, R., Sohy, S., Soldi, M., Stanga, R., Steinhausser, A., Strafella, F., Sylla Mbaye, S., Smedley, A., Tagger, M., Tanga, Paolo, Taricco, C., Teng, J., Tercu, J., Thizy, O., Thomas, J., Tombelli, M., Trangosi, R., Tregon, B., Trivero, P., Tukkers, A., Turcu, V., Umbriaco, G., Unda-Sanzana, E., Vairetti, R., Valenzuela, M., Valente, G., Varennes, G., Vauclair, S., Vergne, J., Verlinden, M., Vidal-Alaiz, M., Vieira-Martins, R., Viel, A., Vîntdevarǎ, D., Vinogradoff, V., Volpini, P., Wendling, M., Wilhelm, P., Wohlgemuth, K., Yanguas, P., Zagarella, R., Zollo, A., l'Observatoire de Paris, Muséum national d'Histoire naturelle (France), Université Paris-Saclay, OSU Institut Pythéas, Istituto Nazionale di Astrofisica, Fondazione Cassa di Risparmio di Torino, Fondazione De Mari Savona, Diputación Foral de Bizkaia, Ministry of Research and Innovation (Romania), Museu de Astronomia e Ciências Afins (Brazil), Labex ESEP, Sorbonne Université, Universidad Pública de Navarra / Nafarroako Unibertsitate Publikoa. InaMat - Institute for Advanced Materials, Universidad Pública de Navarra. Departamento de Estadística, Informática y Matemáticas, Nafarroako Unibertsitate Publikoa. Estatistika, Informatika eta Matematika Saila, 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), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire de paléontologie, évolution, paléoécosystèmes, paléoprimatologie (PALEVOPRIM ), Université de Poitiers-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL), Diagnostic des Plasmas Hors Equilibres (DPHE), Institut national universitaire Champollion [Albi] (INUC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Architecture et Logiciels pour Systèmes Embarqués sur Puce (ALSOC), LIP6, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences - Le Mans (LPG - Le Mans), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Université de Technologie de Belfort-Montbeliard (UTBM)-Université de Bourgogne (UB)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT), Lumière, nanomatériaux et nanotechnologies (L2n), Institut Charles Delaunay (ICD), Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Morphodynamique Continentale et Côtière (M2C), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Jorda, L., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Koschny, D., Trigo-Rodriguez, J. M., Lamy, H., Behrend, R., Ferriere, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, E., Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appere, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Badescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L. D., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M. E., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boaca, I., Boata, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, P., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A. P. C., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J. Y., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J. P., Corp, L., Costa, M., Costard, F., Cottier, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J. C., D'Agostino, G., Daiffallah, K., Danescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J. P., Deleflie, F., D'Elia, M., De Luca, P., De Maria, P., Deverchere, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frincu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaume, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. K., Lacassagne, L., Lachat, D., Lagain, A., Laisne, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J. P., Lecomte, J., Le Du, P., Lelong, F., Lera, S., Leoni, J. F., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., Locatelli, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J. L., Martin-Brisset, J. C., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J. Y., Meza, E., Moggi Cecchi, V., Moiroud, J. J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacsu, L., Notez, P., Ory, M., Pace, E., Paganelli, M. A., Pagola, A., Pajuelo, M., Palacian, J. F., Pallier, G., Paraschiv, P., Pardini, R., Pavone, M., Pavy, G., Payen, G., Pegoraro, A., Pena-Asensio, E., Perez, L., Perez-Hoyos, S., Perlerin, V., Peyrot, A., Peth, F., Pic, V., Pietronave, S., Pilger, C., Piquel, M., Pisanu, T., Poppe, M., Portois, L., Prezeau, J. F., Pugno, N., Quantin, C., Quitte, G., Rambaux, N., Ravier, E., Repetti, U., Ribas, S., Richard, C., Richard, D., Rigoni, M., Rivet, J. P., Rizzi, N., Rochain, S., Rojas, J. F., Romeo, M., Rotaru, M., Rotger, M., Rougier, P., Rousselot, P., Rousset, J., Rousseu, D., Rubiera, O., Rudawska, R., Rudelle, J., Ruguet, J. P., Russo, P., Sales, S., Sauzereau, O., Salvati, F., Schieffer, M., Schreiner, D., Scribano, Y., Selvestrel, D., Serra, R., Shengold, L., Shuttleworth, A., Smareglia, R., Sohy, S., Soldi, M., Stanga, R., Steinhausser, A., Strafella, F., Sylla Mbaye, S., Smedley, A. R. D., Tagger, M., Tanga, P., Taricco, C., Teng, J. P., Tercu, J. O., Thizy, O., Thomas, J. P., Tombelli, M., Trangosi, R., Tregon, B., Trivero, P., Tukkers, A., Turcu, V., Umbriaco, G., Unda-Sanzana, E., Vairetti, R., Valenzuela, M., Valente, G., Varennes, G., Vauclair, S., Vergne, J., Verlinden, M., Vidal-Alaiz, M., Vieira-Martins, R., Viel, A., Vintdevara, D. C., Vinogradoff, V., Volpini, P., Wendling, M., Wilhelm, P., Wohlgemuth, K., Yanguas, P., Zagarella, R., Zollo, A., Universidad Pública de Navarra / Nafarroako Unibertsitate Publikoa. INAMAT2 - Institute for Advanced Materials and Mathematics, Ferrière, L., Appéré, T., Bǎdescu, O., Boacă, I., Boatǎ, R., Bramond, Ph., D’Agostino, G., Dǎnescu, C., D’Elia, M., Deverchère, P., Frîncu, M., Hyaumé, F., Laisné, E., Le Dû, P., Niacşu, L., Palacián, J. F., Peña-Asensio, E., Pérez-Hoyos, S., Quitté, G., Rojas, J.F., Ruguet, J.P., Vîntdevarǎ, D. C., Research unit Medical Physics, and Damage and Repair in Cancer Development and Cancer Treatment (DARE)

Subjects
DYNAMICS, [INFO.INFO-AR]Computer Science [cs]/Hardware Architecture [cs.AR], Meteors, Computer science, Radio receiver, [INFO.INFO-DM]Computer Science [cs]/Discrete Mathematics [cs.DM], Surveys, 010502 geochemistry & geophysics, Track (rail transport), 01 natural sciences, Meteorites, meteors, meteoroids, law.invention, Planets and planetary system, [INFO.INFO-TS]Computer Science [cs]/Signal and Image Processing, Methods: observational, law, [INFO.INFO-RB]Computer Science [cs]/Robotics [cs.RO], meteoroids, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Observational methods, Earth and Planetary Astrophysics (astro-ph.EP), meteoroids -surveys -methods: observational -interplanetary medium, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ORIGIN, [INFO.INFO-AO]Computer Science [cs]/Computer Arithmetic, meteorites, meteors, meteoroids – surveys – methods: observational – interplanetary medium, Meteoroids, RECOVERY, ORBIT, Meteorite, Fully automated, Interplanetary medium, [INFO.INFO-TI]Computer Science [cs]/Image Processing [eess.IV], [INFO.INFO-DC]Computer Science [cs]/Distributed, Parallel, and Cluster Computing [cs.DC], Astrophysics - Instrumentation and Methods for Astrophysics, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, FLUX, Real-time computing, fripon, [INFO.INFO-DS]Computer Science [cs]/Data Structures and Algorithms [cs.DS], FOS: Physical sciences, Context (language use), CAMERA, [INFO.INFO-SE]Computer Science [cs]/Software Engineering [cs.SE], [SPI.AUTO]Engineering Sciences [physics]/Automatic, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, FIREBALL NETWORK, observational [Methods], meteors, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Meteoroid, INNISFREE METEORITE, [INFO.INFO-CV]Computer Science [cs]/Computer Vision and Pattern Recognition [cs.CV], Astronomy and Astrophysics, METEORITE FALL, Meteorites, meteors, meteoroid, Camera network, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Interplanetary spaceflight, meteroids tracking, meteoroids - surveys - methods: observational, SYSTEM, Astrophysics - Earth and Planetary Astrophysics, Meteorites
Abstract

Context. Until recently, camera networks designed for monitoring fireballs worldwide were not fully automated, implying that in case of a meteorite fall, the recovery campaign was rarely immediate. This was an important limiting factor as the most fragile - hence precious - meteorites must be recovered rapidly to avoid their alteration. Aims. The Fireball Recovery and InterPlanetary Observation Network (FRIPON) scientific project was designed to overcome this limitation. This network comprises a fully automated camera and radio network deployed over a significant fraction of western Europe and a small fraction of Canada. As of today, it consists of 150 cameras and 25 European radio receivers and covers an area of about 1.5 × 10km. Methods. The FRIPON network, fully operational since 2018, has been monitoring meteoroid entries since 2016, thereby allowing the characterization of their dynamical and physical properties. In addition, the level of automation of the network makes it possible to trigger a meteorite recovery campaign only a few hours after it reaches the surface of the Earth. Recovery campaigns are only organized for meteorites with final masses estimated of at least 500 g, which is about one event per year in France. No recovery campaign is organized in the case of smaller final masses on the order of 50 to 100 g, which happens about three times a year; instead, the information is delivered to the local media so that it can reach the inhabitants living in the vicinity of the fall. Results. Nearly 4000 meteoroids have been detected so far and characterized by FRIPON. The distribution of their orbits appears to be bimodal, with a cometary population and a main belt population. Sporadic meteors amount to about 55% of all meteors. A first estimate of the absolute meteoroid flux (mag < -5; meteoroid size ≥∼1 cm) amounts to 1250/yr/10km. This value is compatible with previous estimates. Finally, the first meteorite was recovered in Italy (Cavezzo, January 2020) thanks to the PRISMA network, a component of the FRIPON science project., FRIPON was initiated by funding from ANR (grant N.13- BS05-0009-03), carried by the Paris Observatory, Muséum National d’Histoire Naturelle, Paris-Saclay University and Institut Pythéas (LAM-CEREGE). VigieCiel was part of the 65 Millions d’Observateurs project, carried by the Muséum National d’Histoire Naturelle and funded by the French Investissements d’Avenir program. FRIPON data are hosted and processed at Institut Pythéas SIP (Service Informatique Pythéas), and a mirror is hosted at IMCCE (Institut de Mécanique Céleste et de Calcul des Éphémérides / Paris Observatory) with the help of IDOC (https://idoc.ias.u-psud.fr) (Integrated Data and Operation Center), supported by CNRS and CNES. PRISMA is the Italian Network for Systematic surveillance of Meteors and Atmosphere. It is a collaboration initiated and coordinated by the Italian National Institute for Astrophysics (INAF) that counts members among research institutes, associations and schools (http://www.prisma.inaf.it). PRISMA was partially funded by 2016 and 2020 Research and Education grants from Fondazione Cassa di Risparmio di Torino and by a 2016 grant from Fondazione Agostino De Mari (Savona). FRIPON-Bilbao is supported by a grant from Diputacion Foral Bizkaia (DFB/BFA). FRIPONMOROI was supported by a grant of the Romanian Ministery of Research and Innovation, CCCDI - UEFISCDI, project number PN-III-P1-1.2-PCCDI2017-0226/16PCCDI/2018 , within PNCDI III. Rio de Janeiro camera is hosted and partially maintained by MAST (Museum of Astronomy and Related Sciences)/MCTIC. The Meteorix project acknowledges supports from labex ESEP (Exploration Spatiale des Environnements Planétaires), DIM-ACAV+ Région Île-de-France, Janus CNES, IDEX Sorbonne Universités and Sorbonne Université.

Published
2020

9. FRIPON: a worldwide network to track incoming meteoroids

Author

Colas, F., primary, Zanda, B., additional, Bouley, S., additional, Jeanne, S., additional, Malgoyre, A., additional, Birlan, M., additional, Blanpain, C., additional, Gattacceca, J., additional, Jorda, L., additional, Lecubin, J., additional, Marmo, C., additional, Rault, J. L., additional, Vaubaillon, J., additional, Vernazza, P., additional, Yohia, C., additional, Gardiol, D., additional, Nedelcu, A., additional, Poppe, B., additional, Rowe, J., additional, Forcier, M., additional, Koschny, D., additional, Trigo-Rodriguez, J. M., additional, Lamy, H., additional, Behrend, R., additional, Ferrière, L., additional, Barghini, D., additional, Buzzoni, A., additional, Carbognani, A., additional, Di Carlo, M., additional, Di Martino, M., additional, Knapic, C., additional, Londero, E., additional, Pratesi, G., additional, Rasetti, S., additional, Riva, W., additional, Stirpe, G. M., additional, Valsecchi, G. B., additional, Volpicelli, C. A., additional, Zorba, S., additional, Coward, D., additional, Drolshagen, E., additional, Drolshagen, G., additional, Hernandez, O., additional, Jehin, E., additional, Jobin, M., additional, King, A., additional, Nitschelm, C., additional, Ott, T., additional, Sanchez-Lavega, A., additional, Toni, A., additional, Abraham, P., additional, Affaticati, F., additional, Albani, M., additional, Andreis, A., additional, Andrieu, T., additional, Anghel, S., additional, Antaluca, E., additional, Antier, K., additional, Appéré, T., additional, Armand, A., additional, Ascione, G., additional, Audureau, Y., additional, Auxepaules, G., additional, Avoscan, T., additional, Baba Aissa, D., additional, Bacci, P., additional, Bǎdescu, O., additional, Baldini, R., additional, Baldo, R., additional, Balestrero, A., additional, Baratoux, D., additional, Barbotin, E., additional, Bardy, M., additional, Basso, S., additional, Bautista, O., additional, Bayle, L. D., additional, Beck, P., additional, Bellitto, R., additional, Belluso, R., additional, Benna, C., additional, Benammi, M., additional, Beneteau, E., additional, Benkhaldoun, Z., additional, Bergamini, P., additional, Bernardi, F., additional, Bertaina, M. E., additional, Bessin, P., additional, Betti, L., additional, Bettonvil, F., additional, Bihel, D., additional, Birnbaum, C., additional, Blagoi, O., additional, Blouri, E., additional, Boacă, I., additional, Boatǎ, R., additional, Bobiet, B., additional, Bonino, R., additional, Boros, K., additional, Bouchet, E., additional, Borgeot, V., additional, Bouchez, E., additional, Boust, D., additional, Boudon, V., additional, Bouman, T., additional, Bourget, P., additional, Brandenburg, S., additional, Bramond, Ph., additional, Braun, E., additional, Bussi, A., additional, Cacault, P., additional, Caillier, B., additional, Calegaro, A., additional, Camargo, J., additional, Caminade, S., additional, Campana, A. P. C., additional, Campbell-Burns, P., additional, Canal-Domingo, R., additional, Carell, O., additional, Carreau, S., additional, Cascone, E., additional, Cattaneo, C., additional, Cauhape, P., additional, Cavier, P., additional, Celestin, S., additional, Cellino, A., additional, Champenois, M., additional, Chennaoui Aoudjehane, H., additional, Chevrier, S., additional, Cholvy, P., additional, Chomier, L., additional, Christou, A., additional, Cricchio, D., additional, Coadou, P., additional, Cocaign, J. Y., additional, Cochard, F., additional, Cointin, S., additional, Colombi, E., additional, Colque Saavedra, J. P., additional, Corp, L., additional, Costa, M., additional, Costard, F., additional, Cottier, M., additional, Cournoyer, P., additional, Coustal, E., additional, Cremonese, G., additional, Cristea, O., additional, Cuzon, J. C., additional, D’Agostino, G., additional, Daiffallah, K., additional, Dǎnescu, C., additional, Dardon, A., additional, Dasse, T., additional, Davadan, C., additional, Debs, V., additional, Defaix, J. P., additional, Deleflie, F., additional, D’Elia, M., additional, De Luca, P., additional, De Maria, P., additional, Deverchère, P., additional, Devillepoix, H., additional, Dias, A., additional, Di Dato, A., additional, Di Luca, R., additional, Dominici, F. M., additional, Drouard, A., additional, Dumont, J. L., additional, Dupouy, P., additional, Duvignac, L., additional, Egal, A., additional, Erasmus, N., additional, Esseiva, N., additional, Ebel, A., additional, Eisengarten, B., additional, Federici, F., additional, Feral, S., additional, Ferrant, G., additional, Ferreol, E., additional, Finitzer, P., additional, Foucault, A., additional, Francois, P., additional, Frîncu, M., additional, Froger, J. L., additional, Gaborit, F., additional, Gagliarducci, V., additional, Galard, J., additional, Gardavot, A., additional, Garmier, M., additional, Garnung, M., additional, Gautier, B., additional, Gendre, B., additional, Gerard, D., additional, Gerardi, A., additional, Godet, J. P., additional, Grandchamps, A., additional, Grouiez, B., additional, Groult, S., additional, Guidetti, D., additional, Giuli, G., additional, Hello, Y., additional, Henry, X., additional, Herbreteau, G., additional, Herpin, M., additional, Hewins, P., additional, Hillairet, J. J., additional, Horak, J., additional, Hueso, R., additional, Huet, E., additional, Huet, S., additional, Hyaumé, F., additional, Interrante, G., additional, Isselin, Y., additional, Jeangeorges, Y., additional, Janeux, P., additional, Jeanneret, P., additional, Jobse, K., additional, Jouin, S., additional, Jouvard, J. M., additional, Joy, K., additional, Julien, J. F., additional, Kacerek, R., additional, Kaire, M., additional, Kempf, M., additional, Krier, C., additional, Kwon, M. K., additional, Lacassagne, L., additional, Lachat, D., additional, Lagain, A., additional, Laisné, E., additional, Lanchares, V., additional, Laskar, J., additional, Lazzarin, M., additional, Leblanc, M., additional, Lebreton, J. P., additional, Lecomte, J., additional, Le Dû, P., additional, Lelong, F., additional, Lera, S., additional, Leoni, J. F., additional, Le-Pichon, A., additional, Le-Poupon, P., additional, Leroy, A., additional, Leto, G., additional, Levansuu, A., additional, Lewin, E., additional, Lienard, A., additional, Licchelli, D., additional, Locatelli, H., additional, Loehle, S., additional, Loizeau, D., additional, Luciani, L., additional, Maignan, M., additional, Manca, F., additional, Mancuso, S., additional, Mandon, E., additional, Mangold, N., additional, Mannucci, F., additional, Maquet, L., additional, Marant, D., additional, Marchal, Y., additional, Marin, J. L., additional, Martin-Brisset, J. C., additional, Martin, D., additional, Mathieu, D., additional, Maury, A., additional, Mespoulet, N., additional, Meyer, F., additional, Meyer, J. Y., additional, Meza, E., additional, Moggi Cecchi, V., additional, Moiroud, J. J., additional, Millan, M., additional, Montesarchio, M., additional, Misiano, A., additional, Molinari, E., additional, Molau, S., additional, Monari, J., additional, Monflier, B., additional, Monkos, A., additional, Montemaggi, M., additional, Monti, G., additional, Moreau, R., additional, Morin, J., additional, Mourgues, R., additional, Mousis, O., additional, Nablanc, C., additional, Nastasi, A., additional, Niacşu, L., additional, Notez, P., additional, Ory, M., additional, Pace, E., additional, Paganelli, M. A., additional, Pagola, A., additional, Pajuelo, M., additional, Palacián, J. F., additional, Pallier, G., additional, Paraschiv, P., additional, Pardini, R., additional, Pavone, M., additional, Pavy, G., additional, Payen, G., additional, Pegoraro, A., additional, Peña-Asensio, E., additional, Perez, L., additional, Pérez-Hoyos, S., additional, Perlerin, V., additional, Peyrot, A., additional, Peth, F., additional, Pic, V., additional, Pietronave, S., additional, Pilger, C., additional, Piquel, M., additional, Pisanu, T., additional, Poppe, M., additional, Portois, L., additional, Prezeau, J. F., additional, Pugno, N., additional, Quantin, C., additional, Quitté, G., additional, Rambaux, N., additional, Ravier, E., additional, Repetti, U., additional, Ribas, S., additional, Richard, C., additional, Richard, D., additional, Rigoni, M., additional, Rivet, J. P., additional, Rizzi, N., additional, Rochain, S., additional, Rojas, J.F., additional, Romeo, M., additional, Rotaru, M., additional, Rotger, M., additional, Rougier, P., additional, Rousselot, P., additional, Rousset, J., additional, Rousseu, D., additional, Rubiera, O., additional, Rudawska, R., additional, Rudelle, J., additional, Ruguet, J.P., additional, Russo, P., additional, Sales, S., additional, Sauzereau, O., additional, Salvati, F., additional, Schieffer, M., additional, Schreiner, D., additional, Scribano, Y., additional, Selvestrel, D., additional, Serra, R., additional, Shengold, L., additional, Shuttleworth, A., additional, Smareglia, R., additional, Sohy, S., additional, Soldi, M., additional, Stanga, R., additional, Steinhausser, A., additional, Strafella, F., additional, Sylla Mbaye, S., additional, Smedley, A. R. D., additional, Tagger, M., additional, Tanga, P., additional, Taricco, C., additional, Teng, J. P., additional, Tercu, J. O., additional, Thizy, O., additional, Thomas, J. P., additional, Tombelli, M., additional, Trangosi, R., additional, Tregon, B., additional, Trivero, P., additional, Tukkers, A., additional, Turcu, V., additional, Umbriaco, G., additional, Unda-Sanzana, E., additional, Vairetti, R., additional, Valenzuela, M., additional, Valente, G., additional, Varennes, G., additional, Vauclair, S., additional, Vergne, J., additional, Verlinden, M., additional, Vidal-Alaiz, M., additional, Vieira-Martins, R., additional, Viel, A., additional, Vîntdevarǎ, D. C., additional, Vinogradoff, V., additional, Volpini, P., additional, Wendling, M., additional, Wilhelm, P., additional, Wohlgemuth, K., additional, Yanguas, P., additional, Zagarella, R., additional, and Zollo, A., additional

Published
2020
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10. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author

National Science Centre (Poland), European Commission, Ministry of Education (Slovak Republic), Ministerio de Ciencia, Innovación y Universidades (España), Hungarian Academy of Sciences, Marciniak, A., Ali-Lagoa, Victor, Mueller, T.G., Szakáts, R., Molnár, L., Pal, A., Podlewska-Gaca, E., Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Butkiewicz-Bąk, M., Crippa, R., Duffard, René D., Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S., Goncalves, R, Grice, J., Grzeskowiak, I, Hirsch, R., Horbowicz, J, Kaminski, K., Kamińska, M. K., Kim, D. H., Kim, M. J., Konstanciak, I., Kudak, V., Kulczak, P, Maestre, J.L., Manzini, F., Marks, S, Monteiro, F, Ogloza, W, Oszkiewicz, D., Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R., Sanabria, JJ, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, Zukowski, K, National Science Centre (Poland), European Commission, Ministry of Education (Slovak Republic), Ministerio de Ciencia, Innovación y Universidades (España), Hungarian Academy of Sciences, Marciniak, A., Ali-Lagoa, Victor, Mueller, T.G., Szakáts, R., Molnár, L., Pal, A., Podlewska-Gaca, E., Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Butkiewicz-Bąk, M., Crippa, R., Duffard, René D., Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S., Goncalves, R, Grice, J., Grzeskowiak, I, Hirsch, R., Horbowicz, J, Kaminski, K., Kamińska, M. K., Kim, D. H., Kim, M. J., Konstanciak, I., Kudak, V., Kulczak, P, Maestre, J.L., Manzini, F., Marks, S, Monteiro, F, Ogloza, W, Oszkiewicz, D., Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R., Sanabria, JJ, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, and Zukowski, K

Abstract

Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3(-3)(+33) and 45(-30)(+60) Jm(-2) s(-1/2) K-1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.© ESO 2019

Published
2019

11. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author

Marciniak, A., primary, Alí-Lagoa, V., additional, Müller, T. G., additional, Szakáts, R., additional, Molnár, L., additional, Pál, A., additional, Podlewska-Gaca, E., additional, Parley, N., additional, Antonini, P., additional, Barbotin, E., additional, Behrend, R., additional, Bernasconi, L., additional, Butkiewicz-Bąk, M., additional, Crippa, R., additional, Duffard, R., additional, Ditteon, R., additional, Feuerbach, M., additional, Fauvaud, S., additional, Garlitz, J., additional, Geier, S., additional, Goncalves, R., additional, Grice, J., additional, Grześkowiak, I., additional, Hirsch, R., additional, Horbowicz, J., additional, Kamiński, K., additional, Kamińska, M. K., additional, Kim, D.-H., additional, Kim, M.-J., additional, Konstanciak, I., additional, Kudak, V., additional, Kulczak, P., additional, Maestre, J. L., additional, Manzini, F., additional, Marks, S., additional, Monteiro, F., additional, Ogłoza, W., additional, Oszkiewicz, D., additional, Pilcher, F., additional, Perig, V., additional, Polakis, T., additional, Polińska, M., additional, Roy, R., additional, Sanabria, J. J., additional, Santana-Ros, T., additional, Skiff, B., additional, Skrzypek, J., additional, Sobkowiak, K., additional, Sonbas, E., additional, Thizy, O., additional, Trela, P., additional, Urakawa, S., additional, Żejmo, M., additional, and Żukowski, K., additional

Published
2019
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12. FRIPON, the French fireball network

Author

Colas, F., Zanda, B., Bouley, S., Vaubaillon, J., Chiara Marmo, Audureau, Y., Kwon, M. K., Rault, J. L., Caminade, S., Vernazza, P., Gattacceca, J., Birlan, M., Maquet, L., Egal, A., Rotaru, M., Gruson-Daniel, Y., Birnbaum, C., Cochard, F., Thizy, O., Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-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-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-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

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

International audience; FRIPON (Fireball Recovery and InterPlanetary Observation Network) [4](Colas et al, 2014) was recently founded by ANR (Agence Nationale de la Recherche). Its aim is to connect meteoritical science with asteroidal and cometary science in order to better understand solar system formation and evolution. The main idea is to set up an observation network covering all the French territory to collect a large number of meteorites (one or two per year) with accurate orbits, allowing us to pinpoint possible parent bodies. 100 all-sky cameras will be installed at the end of 2015 forming a dense network with an average distance of 100km between stations. To maximize the accuracy of orbit determination, we will mix our optical data with radar data from the GRAVES beacon received by 25 stations [5](Rault et al, 2015). As both the setting up of the network and the creation of search teams for meteorites will need manpower beyond our small team of professionals, we are developing a citizen science network called Vigie-Ciel [6](Zanda et al, 2015). The public at large will thus be able to simply use our data, participate in search campaigns or even setup their own cameras.

Published
2015

13. French Pro/Am collaborations in exoplanet

Author

Alexandre Santerne, Moutou, C., Vanhuysse, M., Bouchy, F., Buil, C., Cochard, F., Thizy, O., Martinez, P., Desnoux, V., Pujol, M., Colas, F., 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), OverSky, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Astronomical Ring for Access to Spectroscopy (ARAS), Shelyak Instruments, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

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

International audience; Amateur astronomers have access to huge telescope time and can reach photometric precision up to a few mmag as well as radial velocity precision up to ˜ 50m.s-1 on brightest stars. We will first present some results of french amateur astronomers in transit photometry and radial velocity and then, we will present an over-view of all the collaborations which can be done between professional and amateur astronomers in the competitive exoplanet domain, and especially the current collaboration between french Pro & Am astronomers which was used in publication in A&A. Finally, we will present a new internet wiki page which goal is to develop such collaboration in different countries.

Published
2011

14. The pulsations of the B5IVe star HD 181 231 observed with CoRoT and ground-based spectroscopy

Author

Neiner, C., Gutiérrez Soto, Juan, Baudin, F., De Batz, B., Frémat, Y., Huat, A.L., Floquet, M., Hubert, A.M., Leroy, B., Diago Nebot, Pascual David, Poretti, E., Carrier, F., Rainer, M., Catala, C., Thizy, O., Buil, C., Ribeiro, J., Andrade, L., Emilio, M., Espinosa-Lara, F., Fabregat Llueca, Juan, Janot-Pacheco, E., Martayan, C., Semaan, T., Suso, J., Baglin, A., Michel, E., and Samadi, R.

Subjects
Astronomia, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Ciència Ensenyament
Abstract

Context. HD 181231 is a B5IVe star, which has been observed with the CoRoT satellite during ∼5 consecutive months and simultaneously from the ground in spectroscopy and spectropolarimetry. Aims. By analysing these data, we aim to detect and characterize as many pulsation frequencies as possible, to search for the presence of beating effects possibly at the origin of the Be phenomenon. Our results will also pr ovide a basis for seismic modelling. Methods. The fundamental parameters of the star are determined from spectral fitting and from the study of the circumstellar emission. The CoRoT photometric data and ground-based spectroscopy are analysed using several Fourier Techniques: CLEAN-NG,PASPER,and TISAFT, as well as a time-frequency technique. A search for a magnetic field is performed by applying the LSD technique to the spectropolarimetric data. Results. We find that HD 181231 is a B5IVe star seen with an inclination of ∼45 degrees. No magnetic field is detected in its photo-sphere. We detect at least 10 independent significant frequencies of variations among the 54 detected frequencies, interpreted in termsof non-radial pulsation modes and rotation. Two longer-term variations are also detected: one at ∼14 days resulting from a beating effect between the two main frequencies of short-term variations, the other at ∼116 days due either to a beating of frequencies or to a zonal pulsation mode. Conclusions. Our analysis of the CoRoT light curve and ground-based spectroscopic data of HD 181231 has led to the determination of the fundamental and pulsational parameters of the star, including beating effects. This will allow a precise seismic modelling of this star.

Published
2009

15. Low-amplitude variations detected by CoRoT in the B8IIIe star HD 175 869

Author

Gutiérrez Soto, Juan, Floquet, M., Samadi, R., Neiner, C., Garrido, R., Fabregat Llueca, Juan, Frémat, Y., Diago Nebot, Pascual David, Huat, A. L., Leroy, B., Emilio, M., Hubert, A.M., Thizy, O., Andrade, L., De Batz, B., Janot-Pacheco, E., Espinosa-Lara, F., Martayan, C., Suso, J., Auvergne, M., Chaintreuil, S., Michel, E., and Catala, C.

Subjects
Esteroides, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

Context.The origin of the short-term variability in Be stars remains a matter of controversy. Pulsations and rotational modulation are the components of the favored hypothesis.Aims.We present our analysis of CoRoT data of the B8IIIe star HD 175869 observed during the first short run in the center direction (SRC1).Methods.We review both the instrumental effects visible in the CoRoT light curve and the analysis methods used by the CoRoT Be team. We applied these methods to the CoRoT light curve of the star HD 175869. A search for line-profile variations in the spectroscopic data was also performed. We also searched for a magnetic field, by applying the LSD technique to spectropolarimetric data.Results.The light curve exhibits low-amplitude variations of the order of 300 μ mag with a double wave shape. A frequency within the range determined for the rotational frequency and 6 of its harmonics are detected. The main frequency and its first harmonic exhibit amplitude variations of a few days. Other significant frequencies of low-amplitude from 25 to a few μmag are also found. The analysis of line profiles from ground-based spectrosc opic data does not detect an y variation. In addition, no Zeeman signature was found.Conclusions.Inhomogeneities caused by stellar activity in or just above the photosphere are proposed to produce the photometric variability detected by CoRoT in the Be star HD 175869. The hypothesis that non-radial pulsations are the origin of these variations cannot be excluded.

Published
2009

16. THE 2011 PERIASTRON PASSAGE OF THE Be BINARY δ Scorpii

Author

Miroshnichenko, A. S., primary, Pasechnik, A. V., additional, Manset, N., additional, Carciofi, A. C., additional, Rivinius, Th., additional, Štefl, S., additional, Gvaramadze, V. V., additional, Ribeiro, J., additional, Fernando, A., additional, Garrel, T., additional, Knapen, J. H., additional, Buil, C., additional, Heathcote, B., additional, Pollmann, E., additional, Mauclaire, B., additional, Thizy, O., additional, Martin, J., additional, Zharikov, S. V., additional, Okazaki, A. T., additional, Gandet, T. L., additional, Eversberg, T., additional, and Reinecke, N., additional

Published
2013
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17. Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field

Author

Briquet, M., primary, Neiner, C., additional, Aerts, C., additional, Morel, T., additional, Mathis, S., additional, Reese, D. R., additional, Lehmann, H., additional, Costero, R., additional, Echevarria, J., additional, Handler, G., additional, Kambe, E., additional, Hirata, R., additional, Masuda, S., additional, Wright, D., additional, Yang, S., additional, Pintado, O., additional, Mkrtichian, D., additional, Lee, B.-C., additional, Han, I., additional, Bruch, A., additional, De Cat, P., additional, Uytterhoeven, K., additional, Lefever, K., additional, Vanautgaerden, J., additional, de Batz, B., additional, Frémat, Y., additional, Henrichs, H., additional, Geers, V. C., additional, Martayan, C., additional, Hubert, A. M., additional, Thizy, O., additional, and Tijani, A., additional

Published
2012
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20. The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

Author

Neiner, C., primary, Gutiérrez-Soto, J., additional, Baudin, F., additional, de Batz, B., additional, Frémat, Y., additional, Huat, A. L., additional, Floquet, M., additional, Hubert, A.-M., additional, Leroy, B., additional, Diago, P. D., additional, Poretti, E., additional, Carrier, F., additional, Rainer, M., additional, Catala, C., additional, Thizy, O., additional, Buil, C., additional, Ribeiro, J., additional, Andrade, L., additional, Emilio, M., additional, Espinosa Lara, F., additional, Fabregat, J., additional, Janot-Pacheco, E., additional, Martayan, C., additional, Semaan, T., additional, Suso, J., additional, Baglin, A., additional, Michel, E., additional, and Samadi, R., additional

Published
2009
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21. The magnetic field of the B3V star 16 Pegasi

Author

Henrichs, Huib F., primary, Neiner, C., additional, Schnerr, R. S., additional, Verdugo, E., additional, Alecian, A., additional, Catala, C., additional, Cochard, F., additional, Gutiérrez, J., additional, Huat, A.-L., additional, Silvester, J., additional, and Thizy, O., additional

Published
2008
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22. The pulsations of the B5IVe star HD 181231observed with CoRoT and ground-based spectroscopy ***

Author

Neiner, C., Gutiérrez-Soto, J., Baudin, F., de Batz, B., Frémat, Y., Huat, A. L., Floquet, M., Hubert, A.-M., Leroy, B., Diago, P. D., Poretti, E., Carrier, F., Rainer, M., Catala, C., Thizy, O., Buil, C., Ribeiro, J., Andrade, L., Emilio, M., Espinosa Lara, F., Fabregat, J., Janot-Pacheco, E., Martayan, C., Semaan, T., Suso, J., Baglin, A., Michel, E., Samadi, R., Neiner, C., Gutiérrez-Soto, J., Baudin, F., de Batz, B., Frémat, Y., Huat, A. L., Floquet, M., Hubert, A.-M., Leroy, B., Diago, P. D., Poretti, E., Carrier, F., Rainer, M., Catala, C., Thizy, O., Buil, C., Ribeiro, J., Andrade, L., Emilio, M., Espinosa Lara, F., Fabregat, J., Janot-Pacheco, E., Martayan, C., Semaan, T., Suso, J., Baglin, A., Michel, E., and Samadi, R.

Abstract

Context. HD 181231is a B5IVe star, which has been observed with the CoRoT satellite during ~5 consecutive months and simultaneously from the ground in spectroscopy and spectropolarimetry.

Published
2009
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23. Detecting and modelling the magnetic field of the β Cephei star V2052 Ophiuchi.

Author

Neiner, C., Alecian, E., Briquet, M., Floquet, M., Frémat, Y., Martayan, C., and Thizy, O.

Subjects
MAGNETIC fields, VV Cephei stars, ASTROPHYSICAL spectropolarimetry, LEAST squares, POLARIZATION (Nuclear physics)
Abstract

Aims. Following the indirect detection of a magnetic field in the β Cephei star V2052Oph by Neiner and collaborators in 2003 with theMusicos spectropolarimeter, we remeasured the magnetic field of this star to attempt to directly confirm the detection of a magnetic field and study its configuration in greater detail. Methods. We used the Narval spectropolarimeter installed at TBL (Pic du Midi, France), which is about 20 times more efficient than the Musicos spectropolarimeter. We applied the least-squares deconvolution (LSD) technique to various groups of lines to measure the circular polarisation of the light coming from V2052 Oph. We synthesized the measured Stokes V profiles with a centred and off-centred dipole model. Results. For the first time, we clearly detect the Zeeman signature in the Stokes V profiles of V2052 Oph and thus directly prove the presence of a magnetic field in this star. The modulation with the rotation period is also confirmed and reflects an oblique dipole field. Thanks to the small error bars on the measurements, we are able to study the behaviour of different groups of lines and the centring of the dipole in the star. We find that the dipole is most likely off-centred along the magnetic axis and that He spots are present at the surface next to the magnetic axis. Conclusions. We conclude that V2052 Oph is a magnetic He-strong β Cep star, with a dipole field, probably off-centred, with Bpol ∼ 400 G and He patches close to the magnetic poles [ABSTRACT FROM AUTHOR]

Published
2012
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24. French fireball network FRIPON

Author

Colas, F., Zanda, B., Vaubaillon, J., Bouley, S., Chiara Marmo, Audureau, Y., Kwon, M. K., Rault, J. -L, Caminade, S., Vernazza, P., Gattacceca, J., Birlan, M., Maquet, L., Egal, A., Rotaru, M., Birnbaum, C., Cochard, F., Thizy, O., Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-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-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-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Rault, J.-L., Roggemans, and P.

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

International audience; FRIPON (Fireball Recovery and Interplanetary Observation Network) was recently founded by ANR (Agence Nationale de la Recherche), its aim being to connect meteoritical science with asteroidal and cometary sciences, in order to better understand our solar system formation and evolution. The main idea is to cover all the French territory to collect a large number of meteorites (one or two per year) with an accurate orbit determination, allowing to pinpoint possible parent bodies. 100 all-sky cameras will be installed at the end of 2015, creating a dense network with an average distance of 100 km between the stations. To maximize the accuracy of the orbit determination, we will mix our optical data with radar data from the GRAVES transmitter received by 25 stations (Rault et al., 2015). As the network installation and the creation of research teams for meteorites involves many persons, at least many more than our small team of professionals, we will develop a participative science network for amateurs called Vigie-Ciel (Zanda et al., 2015). It will be possible to simply use our data, participate in research campaigns or even add cameras to the FRIPON network.

25. FRIPON: a worldwide network to track incoming meteoroids

Author

Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Jorda, L., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Koschny, D., Trigo-Rodriguez, J. M., Lamy, H., Behrend, R., Ferrière, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, E., Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appéré, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Bǎdescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L. D., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M. E., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boacă, I., Boatǎ, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, Ph., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A. P. C., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J. Y., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J. P., Corp, L., Costa, M., Costard, F., Cottier, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J. C., D’Agostino, G., Daiffallah, K., Dǎnescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J. P., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. K., Lacassagne, L., Lachat, D., Lagain, A., Laisné, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J. P., Lecomte, J., Le Dû, P., Lelong, F., Lera, S., Leoni, J. F., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., Locatelli, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J. L., Martin-Brisset, J. C., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J. Y., Meza, E., Moggi Cecchi, V., Moiroud, J. J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacşu, L., Notez, P., Ory, M., Pace, E., Paganelli, M. A., Pagola, A., Pajuelo, M., Palacián, J. F., Pallier, G., Paraschiv, P., Pardini, R., Pavone, M., Pavy, G., Payen, G., Pegoraro, A., Peña-Asensio, E., Perez, L., Pérez-Hoyos, S., Perlerin, V., Peyrot, A., Peth, F., Pic, V., Pietronave, S., Pilger, C., Piquel, M., Pisanu, T., Poppe, M., Portois, L., Prezeau, J. F., Pugno, N., Quantin, C., Quitté, G., Rambaux, N., Ravier, E., Repetti, U., Ribas, S., Richard, C., Richard, D., Rigoni, M., Rivet, J. P., Rizzi, N., Rochain, S., Rojas, J.F., Romeo, M., Rotaru, M., Rotger, M., Rougier, P., Rousselot, P., Rousset, J., Rousseu, D., Rubiera, O., Rudawska, R., Rudelle, J., Ruguet, J.P., Russo, P., Sales, S., Sauzereau, O., Salvati, F., Schieffer, M., Schreiner, D., Scribano, Y., Selvestrel, D., Serra, R., Shengold, L., Shuttleworth, A., Smareglia, R., Sohy, S., Soldi, M., Stanga, R., Steinhausser, A., Strafella, F., Sylla Mbaye, S., Smedley, A. R. D., Tagger, M., Tanga, P., Taricco, C., Teng, J. P., Tercu, J. O., Thizy, O., Thomas, J. P., Tombelli, M., Trangosi, R., Tregon, B., Trivero, P., Tukkers, A., Turcu, V., Umbriaco, G., Unda-Sanzana, E., Vairetti, R., Valenzuela, M., Valente, G., Varennes, G., Vauclair, S., Vergne, J., Verlinden, M., Vidal-Alaiz, M., Vieira-Martins, R., Viel, A., Vîntdevarǎ, D. C., Vinogradoff, V., Volpini, P., Wendling, M., Wilhelm, P., Wohlgemuth, K., Yanguas, P., Zagarella, R., Zollo, A., Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Jorda, L., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Koschny, D., Trigo-Rodriguez, J. M., Lamy, H., Behrend, R., Ferrière, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, E., Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appéré, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Bǎdescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L. D., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M. E., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boacă, I., Boatǎ, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, Ph., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A. P. C., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J. Y., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J. P., Corp, L., Costa, M., Costard, F., Cottier, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J. C., D’Agostino, G., Daiffallah, K., Dǎnescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J. P., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. K., Lacassagne, L., Lachat, D., Lagain, A., Laisné, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J. P., Lecomte, J., Le Dû, P., Lelong, F., Lera, S., Leoni, J. F., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., Locatelli, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J. L., Martin-Brisset, J. C., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J. Y., Meza, E., Moggi Cecchi, V., Moiroud, J. J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacşu, L., Notez, P., Ory, M., Pace, E., Paganelli, M. A., Pagola, A., Pajuelo, M., Palacián, J. F., Pallier, G., Paraschiv, P., Pardini, R., Pavone, M., Pavy, G., Payen, G., Pegoraro, A., Peña-Asensio, E., Perez, L., Pérez-Hoyos, S., Perlerin, V., Peyrot, A., Peth, F., Pic, V., Pietronave, S., Pilger, C., Piquel, M., Pisanu, T., Poppe, M., Portois, L., Prezeau, J. F., Pugno, N., Quantin, C., Quitté, G., Rambaux, N., Ravier, E., Repetti, U., Ribas, S., Richard, C., Richard, D., Rigoni, M., Rivet, J. P., Rizzi, N., Rochain, S., Rojas, J.F., Romeo, M., Rotaru, M., Rotger, M., Rougier, P., Rousselot, P., Rousset, J., Rousseu, D., Rubiera, O., Rudawska, R., Rudelle, J., Ruguet, J.P., Russo, P., Sales, S., Sauzereau, O., Salvati, F., Schieffer, M., Schreiner, D., Scribano, Y., Selvestrel, D., Serra, R., Shengold, L., Shuttleworth, A., Smareglia, R., Sohy, S., Soldi, M., Stanga, R., Steinhausser, A., Strafella, F., Sylla Mbaye, S., Smedley, A. R. D., Tagger, M., Tanga, P., Taricco, C., Teng, J. P., Tercu, J. O., Thizy, O., Thomas, J. P., Tombelli, M., Trangosi, R., Tregon, B., Trivero, P., Tukkers, A., Turcu, V., Umbriaco, G., Unda-Sanzana, E., Vairetti, R., Valenzuela, M., Valente, G., Varennes, G., Vauclair, S., Vergne, J., Verlinden, M., Vidal-Alaiz, M., Vieira-Martins, R., Viel, A., Vîntdevarǎ, D. C., Vinogradoff, V., Volpini, P., Wendling, M., Wilhelm, P., Wohlgemuth, K., Yanguas, P., Zagarella, R., and Zollo, A.

Abstract

Context. Until recently, camera networks designed for monitoring fireballs worldwide were not fully automated, implying that in case of a meteorite fall, the recovery campaign was rarely immediate. This was an important limiting factor as the most fragile – hence precious – meteorites must be recovered rapidly to avoid their alteration. Aims. The Fireball Recovery and InterPlanetary Observation Network (FRIPON) scientific project was designed to overcome this limitation. This network comprises a fully automated camera and radio network deployed over a significant fraction of western Europe and a small fraction of Canada. As of today, it consists of 150 cameras and 25 European radio receivers and covers an area of about 1.5 × 106 km2. Methods. The FRIPON network, fully operational since 2018, has been monitoring meteoroid entries since 2016, thereby allowing the characterization of their dynamical and physical properties. In addition, the level of automation of the network makes it possible to trigger a meteorite recovery campaign only a few hours after it reaches the surface of the Earth. Recovery campaigns are only organized for meteorites with final masses estimated of at least 500 g, which is about one event per year in France. No recovery campaign is organized in the case of smaller final masses on the order of 50 to 100 g, which happens about three times a year; instead, the information is delivered to the local media so that it can reach the inhabitants living in the vicinity of the fall. Results. Nearly 4000 meteoroids have been detected so far and characterized by FRIPON. The distribution of their orbits appears to be bimodal, with a cometary population and a main belt population. Sporadic meteors amount to about 55% of all meteors. A first estimate of the absolute meteoroid flux (mag < –5; meteoroid size ≥~1 cm) amounts to 1250/yr/106 km

26. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author

Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S, Goncalves, R, Grice, J, Grzeskowiak, I, Hirsch, R, Horbowicz, J, Kaminski, K, Kaminska, M.K, Kim, D.H, Kim, M.J, Konstanciak, I, Kudak, V, Kulczak, P, Maestre, J.L, Manzini, F, Marks, S, Monteiro, F, Ogłoza, W, Oszkiewicz, D, Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R, Sanabria, J.J, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, Zukowski, K, Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S, Goncalves, R, Grice, J, Grzeskowiak, I, Hirsch, R, Horbowicz, J, Kaminski, K, Kaminska, M.K, Kim, D.H, Kim, M.J, Konstanciak, I, Kudak, V, Kulczak, P, Maestre, J.L, Manzini, F, Marks, S, Monteiro, F, Ogłoza, W, Oszkiewicz, D, Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R, Sanabria, J.J, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, and Zukowski, K

Abstract

Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3−3 and 3+−333 and 45+−6030 J m−2 s−1/2 K−1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.

27. FRIPON: a worldwide network to track incoming meteoroids

Author

Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Jorda, L., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Koschny, D., Trigo-Rodriguez, J. M., Lamy, H., Behrend, R., Ferrière, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, E., Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appéré, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Bǎdescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L. D., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M. E., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boacă, I., Boatǎ, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, Ph., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A. P. C., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J. Y., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J. P., Corp, L., Costa, M., Costard, F., Cottier, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J. C., D’Agostino, G., Daiffallah, K., Dǎnescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J. P., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. K., Lacassagne, L., Lachat, D., Lagain, A., Laisné, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J. P., Lecomte, J., Le Dû, P., Lelong, F., Lera, S., Leoni, J. F., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., Locatelli, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J. L., Martin-Brisset, J. C., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J. Y., Meza, E., Moggi Cecchi, V., Moiroud, J. J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacşu, L., Notez, P., Ory, M., Pace, E., Paganelli, M. A., Pagola, A., Pajuelo, M., Palacián, J. 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P., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. 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Abstract

Context. Until recently, camera networks designed for monitoring fireballs worldwide were not fully automated, implying that in case of a meteorite fall, the recovery campaign was rarely immediate. This was an important limiting factor as the most fragile – hence precious – meteorites must be recovered rapidly to avoid their alteration. Aims. The Fireball Recovery and InterPlanetary Observation Network (FRIPON) scientific project was designed to overcome this limitation. This network comprises a fully automated camera and radio network deployed over a significant fraction of western Europe and a small fraction of Canada. As of today, it consists of 150 cameras and 25 European radio receivers and covers an area of about 1.5 × 106 km2. Methods. The FRIPON network, fully operational since 2018, has been monitoring meteoroid entries since 2016, thereby allowing the characterization of their dynamical and physical properties. In addition, the level of automation of the network makes it possible to trigger a meteorite recovery campaign only a few hours after it reaches the surface of the Earth. Recovery campaigns are only organized for meteorites with final masses estimated of at least 500 g, which is about one event per year in France. No recovery campaign is organized in the case of smaller final masses on the order of 50 to 100 g, which happens about three times a year; instead, the information is delivered to the local media so that it can reach the inhabitants living in the vicinity of the fall. Results. Nearly 4000 meteoroids have been detected so far and characterized by FRIPON. The distribution of their orbits appears to be bimodal, with a cometary population and a main belt population. Sporadic meteors amount to about 55% of all meteors. A first estimate of the absolute meteoroid flux (mag < –5; meteoroid size ≥~1 cm) amounts to 1250/yr/106 km

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