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40 results on '"Licchelli, D."'

1. VZ Sex: X-ray confirmation of its intermediate polar nature

Author

Nucita, A. A., De Paolis, F., Licchelli, D., Strafella, F., Ingrosso, G., and Maiorano, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Intermediate polars are members of the cataclysmic variable binary stars. They are characterized by a moderately magnetized white dwarf accreting matter from a cool main-sequence companion star. In many cases, this accretion gives rise to a detectable $X$-ray emission. VZ Sex is an interesting $X$-ray source whose nature needs a robust confirmation. Here, we used archive $XMM$-Newton observation to assign the source to the intermediate polar class. We applied the Lomb-Scargle periodogram method to detect any relevant periodic feature in the $0.1$--$10$ keV light curve and performed a spectral fitting of the $X$-ray spectrum in order to get information on the on-going accretion mechanism. By inspecting the periodogram, we detected a clear periodic feature at $\simeq 20.3$ minutes that we interpret as the spin period of the white dwarf. We additionally found the typical side bands expected as the consequence of the beat between the spin and the orbital period of $\simeq 3.581$ hours. The source is characterized by a unabsorbed flux of $\simeq 2.98\times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$ corresponding to an intrinsic luminosity {of $\simeq 7 \times 10^{31}$ erg s$^{-1}$ } {for a distance of $\simeq 433$ pc}. The existence of such features allow us to classify VZ Sex as a clear member of the intermediate polar class. Furthermore, with the estimated WD spin, the ratio $P_{spin}/P_{orb}$ is $\simeq 0.09$, i.e. consistent with that expected for a typical IP system above the period gap. In addition, the estimated intrinsic luminosity opens the possibility that a bridge linking the normally bright IPs to the faint population of sources does exist., Comment: Accepted for publication on The Astrophysical Journal. 10 pages, 5 figures

Published
2020
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2. HP Cet and Swift J0820.6-2805: two candidate intermediate polars observed by XMM-Newton

Author

Nucita, A. A., De Paolis, F., Strafella, F., and Licchelli, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on the XMM-Newton observation of HP Cet and Swift J0820.6-2805, two X-ray photon sources that are candidates to be members of the intermediate polar class of cataclysmic variables. If the historical optical light curve of HP Cet shows a periodic feature at $\simeq 96$ minutes, a clear identification of such a signature in the high energy band (apart for a variability on a time scale of $\simeq 8$ minutes as detected by the ROSAT satellite) is lacking. By using XMM-Newton archive data, we clearly identify a feature (at $\simeq 88$ minutes) which is marginally consistent with one of the binary system orbital periods reported in the literature. We also found a signature of a periodic features on the time scale of $\simeq 5.6$ minutes. In the case of Swift J0820.6-2805, the intermediate polar nature was previously unclear and the orbital and the white dwarf spin periods were unknown. Here, the 0.3-10 keV data undoubtedly reveal an orbital period and a white dwarf spin of $\simeq 87.5$ minutes and $\simeq 27.9$ minutes, respectively. The spectral analysis showed that both HP Cet and Swift J0820.6-280 are members of the under-luminous IP subclass since their luminosity in the $0.3-10$ keV band is estimated to be $\simeq 5\times 10^{30}$ erg s$^{-1}$ and $\simeq 3.8\times 10^{29}$ erg s$^{-1}$, respectively., Comment: Accepted for publication on MNRAS, main journal, 2020. 9 Pages. 9 Figures

Published
2020
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3. A Quasar microlensing event towards J1249+3449?

Author

De Paolis, F., Nucita, A. A., Strafella, F., Licchelli, D., and Ingrosso, G.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We show that the optical flare event discovered by Graham et al. (2020) towards the active galactic nucleus J1249+3449 is fully consistent with being a quasar microlensing event due to a $\simeq 0.1 M_{\odot}$ star, although other explanations, such as that, mainly supported by Graham et al. (2020), of being the electromagnetic counterpart associated to a binary black hole merger, cannot be completely excluded at present., Comment: Accepted for publication on the Monthly Notices of the Royal Astronomical Society Letters - (MNRAS Letter) -, 2020, 5 pages, 2 figures

Published
2020
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4. DW Cancri in x-rays

Author

Nucita, A. A., Conversi, L., and Licchelli, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on the $XMM$-Newton observation of DW Cnc, a candidate intermediate polar candidate whose historical optical light curve shows the existence of periods at $\simeq 38$, $\simeq 86$ and $\simeq 69$ minutes which were interpreted as the white dwarf spin, the orbital and the spin-orbit beat periodicities. By studying the $0.3-10$ keV light curves, we confirm the existence of a period at $\simeq 38$ minutes and find in the OM light curve a signature for a period at $75\pm 21$ minutes which is consistent with both the orbital and spin-orbit beat. { These findings allow us to unveil without any doubt, the nature of DW Cnc as an accreting intermediate polar. The EPIC and RGS source spectra were analyzed and a best fit model, consisting of a multi-temperature plasma, was found. The maximum temperature found when fitting the data is $kT_{max}\simeq 31$ keV which can be interpreted as an upper limit to the temperature of the shock., Comment: 2019. Accepted for publication on MNRAS. 5 figures, 1 table. Updated as, by mistake, an author affiliation was missing from the list

Published
2019
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5. Discovery of a bright microlensing event with planetary features towards the Taurus region: a super Earth planet

Author

Nucita, A. A., Licchelli, D., De Paolis, F., Ingrosso, G., Strafella, F., Katysheva, N., and Shugarov, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The transient event labeled as TCP J05074264+2447555 recently discovered towards the Taurus region was quickly recognized to be an ongoing microlensing event on a source located at distance of only $700-800$ pc from Earth. Here, we show that observations with high sampling rate close to the time of maximum magnification revealed features that imply the presence of a binary lens system with very low mass ratio components. We present a complete description of the binary lens system which hosts an Earth-like planet with most likely mass of $9.2\pm 6.6$ M$_{\oplus}$. Furthermore, the source estimated location and detailed Monte Carlo simulations allowed us to classify the event as due to the closest lens system, being at a distance of $\simeq 380$ pc and mass $\simeq 0.25$ M$_{\odot}$., Comment: Accepted for publication on MNRAS, 2018. 6 Pages, 5 Figures. References updated

Published
2018
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6. Optical, near-IR and $X$-ray observations of SN 2015J and its host galaxy

Author

Nucita, A. A., De Paolis, F., Saxton, R., Testa, V., Strafella, F., Read, A., Licchelli, D., Ingrosso, G., Convenga, F., and Boutsia, K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

SN 2015J was discovered on April 27th 2015 and is classified as a type IIn supernova. At first, it appeared to be an orphan SN candidate, i.e. without any clear identification of its host galaxy. Here, we present the analysis of the observations carried out {by the VLT 8-m class telescope with the FORS2 camera in the R band and the Magellan telescope (6.5 m) equipped with the IMACS Short-Camera (V and I filters) and the FourStar camera (Ks filter)}. We show that SN 2015J resides in what appears to be a very compact galaxy establishing a relation between the SN event and its natural host. We also present and discuss archival and new $X$-ray data centred on SN 2015J. At the time of the supernova explosion, Swift/XRT observations were made and a weak X-ray source was detected at the location of SN 2015J. Almost one year later, the same source was unambiguously identified during serendipitous observations by Swift/XRT and $XMM$-Newton, clearly showing an enhancement of the 0.3-10 keV band flux by a factor $\simeq 30$ with respect to the initial state. Swift/XRT observations show that the source is still active in the $X$-rays at a level of $\simeq 0.05$ counts s$^{-1}$. The unabsorbed X-ray luminosity derived from the {\it XMM}-Newton slew and SWIFT observations, $L_{x}\simeq 5\times10^{41}$ erg s$^{-1}$, places SN 2015J among the brightest young supernovae in X-rays., Comment: The Astrophysical Journal, Volume 850, Number 2

Published
2017
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8. Analysis of lunar craters: A PLS path among impact physics, craterization simulations and image processing

Author

D'Elia M., Licchelli D., Orofino V., Strafella F., de Giorgi M. L., Ventura A., D'Elia, M., Licchelli, D., Orofino, V., Strafella, F., de Giorgi, M. L., and Ventura, A.

Subjects
craterization simulations, image processing, PLS project
Abstract

This contribution concerns the training course that the Astrophysics Group of the University of Salento proposed to the students of the Piano Lauree Scientifiche for the school year 2019–2020. Since the first edition of the Piano Lauree Scientifiche - Fisica of the University of Salento, the proposal of the Astrophysics Laboratory has been varied and every year different topics have been addressed, developing new methodologies for a more attractive teaching and a better education guidance. Arousing great interest from students, this year the proposal of the Astrophysics Group was dedicated to Planetology with a direct laboratory experience focused on the simulation and analysis of impact craters. After an introduction on the minor bodies of the Solar System and on the impact crater physics, the students digitally processed images of the Moon’s surface with a dedicated software, obtained the necessary information for the subsequent calculation of the involved physical parameters, and finally processed the results, comparing them with those reported in the literature.

Published
2021

9. 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
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12. 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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13. Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Author

Gardiol, D, primary, 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, Salerno, R, additional, Stirpe, G M, additional, Valsecchi, G B, additional, Volpicelli, C A, additional, Zorba, S, additional, Colas, F, additional, Zanda, B, additional, Bouley, S, additional, Jeanne, S, additional, Malgoyre, A, additional, Birlan, M, additional, Blanpain, C, additional, Gattacceca, J, additional, Lecubin, J, additional, Marmo, C, additional, Rault, J L, additional, Vaubaillon, J, additional, Vernazza, P, additional, Affaticati, F, additional, Albani, M, additional, Andreis, A, additional, Ascione, G, additional, Avoscan, T, additional, Bacci, P, additional, Baldini, R, additional, Balestrero, A, additional, Basso, S, additional, Bellitto, R, additional, Belluso, M, additional, Benna, C, additional, Bernardi, F, additional, Bertaina, M E, additional, Betti, L, additional, Bonino, R, additional, Boros, K, additional, Bussi, A, additional, Carli, C, additional, Carriero, T, additional, Cascone, E, additional, Cattaneo, C, additional, Cellino, A, additional, Colombetti, P, additional, Colombi, E, additional, Costa, M, additional, Cremonese, G, additional, Cricchio, D, additional, D’Agostino, G, additional, D’Elia, M, additional, De Maio, M, additional, Demaria, P, additional, Di Dato, A, additional, Di Luca, R, additional, Federici, F, additional, Gagliarducci, V, additional, Gerardi, A, additional, Giuli, G, additional, Guidetti, D, additional, Interrante, G, additional, Lazzarin, M, additional, Lera, S, additional, Leto, G, additional, Licchelli, D, additional, Lippolis, F, additional, Manca, F, additional, Mancuso, S, additional, Mannucci, F, additional, Masi, R, additional, Masiero, S, additional, Meucci, S, additional, Misiano, A, additional, Moggi Cecchi, V, additional, Molinari, E, additional, Monari, J, additional, Montemaggi, M, additional, Montesarchio, M, additional, Monti, G, additional, Morini, P, additional, Nastasi, A, additional, Pace, E, additional, Pardini, R, additional, Pavone, M, additional, Pegoraro, A, additional, Pietronave, S, additional, Pisanu, T, additional, Pugno, N, additional, Repetti, U, additional, Rigoni, M, additional, Rizzi, N, additional, Romeni, C, additional, Romeo, M, additional, Rubinetti, S, additional, Russo, P, additional, Salvati, F, additional, Selvestrel, D, additional, Serra, R, additional, Simoncelli, C, additional, Smareglia, R, additional, Soldi, M, additional, Stanga, R, additional, Strafella, F, additional, Suvieri, M, additional, Taricco, C, additional, Tigani Sava, G, additional, Tombelli, M, additional, Trivero, P, additional, Umbriaco, G, additional, Vairetti, R, additional, Valente, G, additional, Volpini, P, additional, Zagarella, R, additional, and Zollo, A, additional

Published
2020
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20. ASTRONET: planetariy observations in remote collaborative web environment

Author

LICCHELLI D, BERNARDO A, BLANCO, Armando, BOCHICCHIO, Mario Alessandro, FONTI, Sergio, D'ELIA, Marcella, Licchelli, D, Blanco, Armando, Bochicchio, Mario Alessandro, Bernardo, A, Fonti, Sergio, and D'Elia, Marcella

Subjects
Remote planetary observation, remote laboratory
Abstract

In this paper we discuss the objectives, the key technical aspects and the main results of AstroNet, a Web-controlled telescope that can be simultaneously operated by small groups of users (2-20 in turn), like in a real astronomical observatory. AstroNet is the outcome of a collaboration between the Astrophysics group and the DIDA-Lab of the University of Salento and has been developed to respond to the increasing number of re- quests coming from schools and families about astronomy lectures and sky observation tutorials. In the last year, AstroNet permitted to about 1000 young students to perform rich observation experiences from both school and home, with the same global effort previously needed to offer a similar experience to about 100 people. The recognition and the analysis of the main lunar geologic structures, the monitoring of the complex and diversified Jupiter atmosphere, the evolution of comets in proximity of perihelion are only some of the possible targets of observations and imaging sessions that are suitable to a great number of thorough analyses. Moreover, with the same instrumental equipment, even if with a more well-constructed approach, it is possible to start low cost scientific research projects in the field of asteroid photometry, variable stars or extrasolar planet transits.

Published
2008

23. Infrared spectroscopy of carbonate samples of biotic origin relevant to Mars exobiological studies

Author

OROFINO, Vincenzo, BLANCO, Armando, D'ELIA, Marcella, FONTI, Sergio, LICCHELLI D., Orofino, Vincenzo, Blanco, Armando, D'Elia, Marcella, Licchelli, D., and Fonti, Sergio

Abstract

Because it is possible that Mars experienced an ancient climate warmer and wetter than the present one, it is reasonable to suppose that simple forms of life developed there, in the underground or at the surface, as in the terrestrial primitive biosphere. In this work we have performed infrared (IR) transmission spectroscopic analyses directed to examine the reaction to heat treatments of biotic (fresh and fossil materials) and abiotic particulate samples composed of calcium carbonate (aragonite or calcite). The aim is to check if IR spectroscopy can be a useful tool for discriminating between abiotic and biotic (fossil) carbonate samples collected on the martian surface, during in situ or sample-return missions. An important result we found is that, after thermal processing, it is possible to distinguish, by means of IR spectroscopy, abiotic aragonite from aragonite of recent biological origin. In addition we have found that the spectral behaviour of all the analysed fossil samples after heat treatment is the same as that of fresh biotic material irrespective of the original structure (whether aragonite or calcite).

Published
2007

28. 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

29. 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

30. Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Author

C. A. Volpicelli, Enrico Cascone, M. Belluso, Stefano Basso, Riccardo Smareglia, Cyril Blanpain, A. Andreis, G. Monti, M. E. Bertaina, S. Masiero, Tonino Pisanu, G. Interrante, F. Lippolis, G. Tigani Sava, G. Valente, D. Barghini, Sonia Zorba, Alberto Buzzoni, V. Gagliarducci, M. Soldi, Fabio Manca, Cristina Knapic, Cristian Carli, M. Montesarchio, Giovanni Pratesi, S. Rubinetti, D. Licchelli, T. Avoscan, A. Misiano, D. Cricchio, F. Federici, P. Colombetti, M. Romeo, G. Ascione, Daniele Gardiol, Alberto Cellino, A. Gerardi, François Colas, M. Suvieri, F. Strafella, R. Di Luca, F. Bernardi, A. Nastasi, J. L. Rault, S. Jeanne, C. Simoncelli, R. Stanga, Monica Lazzarin, C. Romeni, C. Cattaneo, S. Rasetti, Albino Carbognani, A. Malgoyre, Jader Monari, P. Demaria, Carla Taricco, M. Tombelli, Gabriele Giuli, Giuseppe Leto, A. Di Dato, N. Rizzi, M. Di Carlo, R. Serra, A. Pegoraro, Sylvain Bouley, S. Pietronave, Matteo Albani, R. Baldini, D. Guidetti, F. Salvati, M. Montemaggi, G. D’Agostino, Elisa Londero, A. Zollo, Chiara Marmo, F. Mannucci, W. Riva, J. Vaubaillon, Brigitte Zanda, Mirel Birlan, M. Rigoni, P. Morini, Jérôme Gattacceca, U. Repetti, M. Pavone, R. Zagarella, G. Cremonese, S. Meucci, S. Lera, R. Bellitto, M. D’Elia, A. Balestrero, F. Affaticati, M. De Maio, T. Carriero, R. Masi, S. Mancuso, Giovanni B. Valsecchi, Emilio Molinari, N. Pugno, R. Salerno, R. Bonino, R. Pardini, Pierre Vernazza, P. Russo, A. Bussi, V. Moggi Cecchi, C. Benna, G. M. Stirpe, K. Boros, J. Lecubin, P. Bacci, Gabriele Umbriaco, M. Costa, D. Selvestrel, E. Pace, M. Di Martino, R. Vairetti, E. Colombi, L. Betti, P. Trivero, P. Volpini, 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), 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), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Gardiol, D., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Salerno, R., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Affaticati, F., Albani, M., Andreis, A., Ascione, G., Avoscan, T., Bacci, P., Baldini, R., Balestrero, A., Basso, S., Bellitto, R., Belluso, M., Benna, C., Bernardi, F., Bertaina, M. E., Betti, L., Bonino, R., Boros, K., Bussi, A., Carli, C., Carriero, T., Cascone, E., Cattaneo, C., Cellino, A., Colombetti, P., Colombi, E., Costa, M., Cremonese, G., Cricchio, D., D'Agostino, G., D'Elia, M., De Maio, M., Demaria, P., Di Dato, A., Di Luca, R., Federici, F., Gagliarducci, V., Gerardi, A., Giuli, G., Guidetti, D., Interrante, G., Lazzarin, M., Lera, S., Leto, G., Licchelli, D., Lippolis, F., Manca, F., Mancuso, S., Mannucci, F., Masi, R., Masiero, S., Meucci, S., Misiano, A., Moggi Cecchi, V., Molinari, E., Monari, J., Montemaggi, M., Montesarchio, M., Monti, G., Morini, P., Nastasi, A., Pace, E., Pardini, R., Pavone, M., Pegoraro, A., Pietronave, S., Pisanu, T., Pugno, N., Repetti, U., Rigoni, M., Rizzi, N., Romeni, C., Romeo, M., Rubinetti, S., Russo, P., Salvati, F., Selvestrel, D., Serra, R., Simoncelli, C., Smareglia, R., Soldi, M., Stanga, R., Strafella, F., Suvieri, M., Taricco, C., Tigani Sava, G., Tombelli, M., Trivero, P., Umbriaco, G., Vairetti, R., Valente, G., Volpini, P., Zagarella, R., Zollo, A., Gardiol D., Barghini D., Buzzoni A., Carbognani A., Di Carlo M., Di Martino M., Knapic C., Londero E., Pratesi G., Rasetti S., Riva W., Salerno R., Stirpe G.M., Valsecchi G.B., Volpicelli C.A., Zorba S., Colas F., Zanda B., Bouley S., Jeanne S., Malgoyre A., Birlan M., Blanpain C., Gattacceca J., Lecubin J., Marmo C., Rault J.L., Vaubaillon J., Vernazza P., Affaticati F., Albani M., Andreis A., Ascione G., Avoscan T., Bacci P., Baldini R., Balestrero A., Basso S., Bellitto R., Belluso M., Benna C., Bernardi F., Bertaina M.E., Betti L., Bonino R., Boros K., Bussi A., Carli C., Carriero T., Cascone E., Cattaneo C., Cellino A., Colombetti P., Colombi E., Costa M., Cremonese G., Cricchio D., D'Agostino G., D'Elia M., De Maio M., Demaria P., Di Dato A., Di Luca R., Federici F., Gagliarducci V., Gerardi A., Giuli G., Guidetti D., Interrante G., Lazzarin M., Lera S., Leto G., Licchelli D., Lippolis F., Manca F., Mancuso S., Mannucci F., Masi R., Masiero S., Meucci S., Misiano A., Moggi Cecchi V., Molinari E., Monari J., Montemaggi M., Montesarchio M., Monti G., Morini P., Nastasi A., Pace E., Pardini R., Pavone M., Pegoraro A., Pietronave S., Pisanu T., Pugno N., Repetti U., Rigoni M., Rizzi N., Romeni C., Romeo M., Rubinetti S., Russo P., Salvati F., Selvestrel D., Serra R., Simoncelli C., Smareglia R., Soldi M., Stanga R., Strafella F., Suvieri M., Taricco C., Tigani Sava G., Tombelli M., Trivero P., Umbriaco G., Vairetti R., Valente G., Volpini P., Zagarella R., Zollo A., and ITA

Subjects
meteoroids -methods: data analysis -techniques: image processing, 010502 geochemistry & geophysics, 01 natural sciences, Strewn field, meteorites, 0103 physical sciences, meteors, meteoroids, 010303 astronomy & astrophysics, meteoroid, 0105 earth and related environmental sciences, Physics, Meteoroid, image processing, methods: data analysis, techniques, meteor, Astronomy, Astronomy and Astrophysics, meteorite, Meteorite, Space and Planetary Science, [SDU]Sciences of the Universe [physics], data analysi [methods], Trajectory, Orbit (control theory)
Abstract

Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 2020 January 4th. The associated fireball was observed on the evening of New Year’s Day 2020 by eight all-sky cameras of the PRISMA fireball network, a partner of FRIPON. The computed trajectory had an inclination angle of approximately 68° and a velocity at infinity of 12.8 km s−1. Together with the relatively low terminal height, estimated as 21.5 km, those values were indicating the significant possibility of a meteorite dropping event, as additionally confirmed by the non-zero residual total mass. The strewn-field was computed taking into account the presence of two bright light flashes, revealing that the meteoroid had been very likely subject to fragmentation. Three days after the event, two samples, weighing 3.1 and 52.2 g, were collected as a result of a dedicated field search and thanks to the involvement of the local people. The two pieces were immediately recognized as freshly fallen fragments of meteorite. The computed orbital elements, compared with the ones of known Near-Earth Asteroids from the NEODyS database, are compatible with one asteroid only; 2013 VC10. The estimated original mass of the meteoroid, 3.5 kg, and size, approximately 13 cm, is so far the smallest among the current 35 cases in which meteorites were recovered from precise strewn-field computation thanks to observational data. This result demonstrates the effectiveness of accurate processing of fireball network data even on challenging events generated by small size meteoroids.

Published
2021
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31. Timing analysis of a sample of five cataclysmic variable candidates observed by the XMM–Newton satellite

Author

A A Nucita, S M Lezzi, F De Paolis, F Strafella, D Licchelli, A Franco, M Maiorano, Nucita, A A, Lezzi, S M, De Paolis, F, Strafella, F, Licchelli, D, Franco, A, and Maiorano, M

Subjects
binaries [novae, cataclysmic variables, white dwarfs, X-rays], Space and Planetary Science, Astronomy and Astrophysics
Abstract

Intermediate polars are a class of cataclysmic variables in which a white dwarf accretes material from a companion star. The intermediate polar nature confirmation usually derives from the detection of two periods in both X-ray and optical photometry. In this respect, the high-energy signal is often characterized by modulations on the white dwarf spin and the orbital period. However, noting that the periodograms may be characterized by strong features also at the synodic period and/or other sidebands, the timing analysis of the X-ray signal may offer the unique possibility to firmly discover an intermediate polar candidate. Here, we concentrate on a sample of five cataclysmic variable binary candidates: i.e. SAXJ1748.2-2808, 1RXS J211336.1 + 542226, CXOGC J174622.7-285218, CXOGC J174517.4-290650, and V381 Vel, listed in the IPHome catalogue. Our main aim is to confirm if they belong to the intermediate polar class or not. The results of our analysis show that we can safely assess the intermediate polar nature of all the considered sources, apart for the case of V381 Vel which instead behaves like a cataclysmic variable of the polar subclass. Moreover, the source SAXJ1748.2-2808, previously classified as an HMXB, appears to be, most likely, an intermediate polar variable.

Published
2022

32. DW Cancri in X-rays

Author

L. Conversi, D. Licchelli, A. A. Nucita, Nucita, A A, Conversi, L, and Licchelli, D

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Maximum temperature, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Beat (acoustics), White dwarf, Astronomy and Astrophysics, Plasma, Astrophysics, EPIC, Light curve, 01 natural sciences, Spectral line, Intermediate polar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, x-rays, wd
Abstract

We report on the $XMM$-Newton observation of DW Cnc, a candidate intermediate polar candidate whose historical optical light curve shows the existence of periods at $\simeq 38$, $\simeq 86$ and $\simeq 69$ minutes which were interpreted as the white dwarf spin, the orbital and the spin-orbit beat periodicities. By studying the $0.3-10$ keV light curves, we confirm the existence of a period at $\simeq 38$ minutes and find in the OM light curve a signature for a period at $75\pm 21$ minutes which is consistent with both the orbital and spin-orbit beat. { These findings allow us to unveil without any doubt, the nature of DW Cnc as an accreting intermediate polar. The EPIC and RGS source spectra were analyzed and a best fit model, consisting of a multi-temperature plasma, was found. The maximum temperature found when fitting the data is $kT_{max}\simeq 31$ keV which can be interpreted as an upper limit to the temperature of the shock., Comment: 2019. Accepted for publication on MNRAS. 5 figures, 1 table. Updated as, by mistake, an author affiliation was missing from the list

Published
2019
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33. VZ Sex: X-Ray Confirmation of Its Intermediate Polar Nature

Author

F. De Paolis, Francesco Strafella, G. Ingrosso, M. Maiorano, A. A. Nucita, D. Licchelli, Nucita, A. A., De Paolis, F., Licchelli, D., Strafella, F., Ingrosso, G., and Maiorano, M.

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, X-ray binary, Cataclysmic variable star, FOS: Physical sciences, X-rays. White dwarfs. cataclysmic variables- Period analysis, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Intermediate polar, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Order (ring theory), White dwarf, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Intermediate polars are members of the cataclysmic variable binary stars. They are characterized by a moderately magnetized white dwarf accreting matter from a cool main-sequence companion star. In many cases, this accretion gives rise to a detectable $X$-ray emission. VZ Sex is an interesting $X$-ray source whose nature needs a robust confirmation. Here, we used archive $XMM$-Newton observation to assign the source to the intermediate polar class. We applied the Lomb-Scargle periodogram method to detect any relevant periodic feature in the $0.1$--$10$ keV light curve and performed a spectral fitting of the $X$-ray spectrum in order to get information on the on-going accretion mechanism. By inspecting the periodogram, we detected a clear periodic feature at $\simeq 20.3$ minutes that we interpret as the spin period of the white dwarf. We additionally found the typical side bands expected as the consequence of the beat between the spin and the orbital period of $\simeq 3.581$ hours. The source is characterized by a unabsorbed flux of $\simeq 2.98\times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$ corresponding to an intrinsic luminosity {of $\simeq 7 \times 10^{31}$ erg s$^{-1}$ } {for a distance of $\simeq 433$ pc}. The existence of such features allow us to classify VZ Sex as a clear member of the intermediate polar class. Furthermore, with the estimated WD spin, the ratio $P_{spin}/P_{orb}$ is $\simeq 0.09$, i.e. consistent with that expected for a typical IP system above the period gap. In addition, the estimated intrinsic luminosity opens the possibility that a bridge linking the normally bright IPs to the faint population of sources does exist., Comment: Accepted for publication on The Astrophysical Journal. 10 pages, 5 figures

Published
2021

34. HP Cet and Swift J0820.6–2805: two candidate intermediate polars observed by XMM–Newton

Author

D. Licchelli, Francesco Strafella, A. A. Nucita, F. De Paolis, Nucita, A A, De paolis, F, Strafella, F, and Licchelli, D

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, Orbital period, Light curve, 01 natural sciences, Luminosity, CV, White dwarfs, Magnetic Field driven accretion, intermediate polars, High Energy emission, Intermediate polar, Space and Planetary Science, 0103 physical sciences, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Spin-½
Abstract

We report on the XMM-Newton observation of HP Cet and Swift J0820.6-2805, two X-ray photon sources that are candidates to be members of the intermediate polar class of cataclysmic variables. If the historical optical light curve of HP Cet shows a periodic feature at $\simeq 96$ minutes, a clear identification of such a signature in the high energy band (apart for a variability on a time scale of $\simeq 8$ minutes as detected by the ROSAT satellite) is lacking. By using XMM-Newton archive data, we clearly identify a feature (at $\simeq 88$ minutes) which is marginally consistent with one of the binary system orbital periods reported in the literature. We also found a signature of a periodic features on the time scale of $\simeq 5.6$ minutes. In the case of Swift J0820.6-2805, the intermediate polar nature was previously unclear and the orbital and the white dwarf spin periods were unknown. Here, the 0.3-10 keV data undoubtedly reveal an orbital period and a white dwarf spin of $\simeq 87.5$ minutes and $\simeq 27.9$ minutes, respectively. The spectral analysis showed that both HP Cet and Swift J0820.6-280 are members of the under-luminous IP subclass since their luminosity in the $0.3-10$ keV band is estimated to be $\simeq 5\times 10^{30}$ erg s$^{-1}$ and $\simeq 3.8\times 10^{29}$ erg s$^{-1}$, respectively., Accepted for publication on MNRAS, main journal, 2020. 9 Pages. 9 Figures

Published
2020

35. A quasar microlensing event towards J1249+3449?

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, A. A. Nucita, D. Licchelli, De Paolis, F., Nucita, A. A., Strafella, F., Licchelli, D., and Ingrosso, G.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Active galactic nucleus, Event (relativity), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Gravitational microlensing, Astrophysics - Astrophysics of Galaxies, law.invention, Binary black hole, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Microlensing. Dark Matter. Planetary events. Quasars, Astrophysics::Galaxy Astrophysics, Flare
Abstract

We show that the optical flare event discovered by Graham et al. (2020) towards the active galactic nucleus J1249+3449 is fully consistent with being a quasar microlensing event due to a $\simeq 0.1 M_{\odot}$ star, although other explanations, such as that, mainly supported by Graham et al. (2020), of being the electromagnetic counterpart associated to a binary black hole merger, cannot be completely excluded at present., Accepted for publication on the Monthly Notices of the Royal Astronomical Society Letters - (MNRAS Letter) -, 2020, 5 pages, 2 figures

Published
2020

36. Discovery of a bright microlensing event with planetary features towards the Taurus region: a super-Earth planet

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, S.Y. Shugarov, D. Licchelli, Natalia Katysheva, A. A. Nucita, Nucita, A A, Licchelli, D, De Paolis, F, Ingrosso, G, Strafella, F, Katysheva, N, and Shugarov, S

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, 010308 nuclear & particles physics, Monte Carlo method, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Planetary system, Gravitational microlensing, 01 natural sciences, Microlensing, Exo Planets, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Low Mass, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics - Earth and Planetary Astrophysics
Abstract

The transient event labeled as TCP J05074264+2447555 recently discovered towards the Taurus region was quickly recognized to be an ongoing microlensing event on a source located at distance of only $700-800$ pc from Earth. Here, we show that observations with high sampling rate close to the time of maximum magnification revealed features that imply the presence of a binary lens system with very low mass ratio components. We present a complete description of the binary lens system which hosts an Earth-like planet with most likely mass of $9.2\pm 6.6$ M$_{\oplus}$. Furthermore, the source estimated location and detailed Monte Carlo simulations allowed us to classify the event as due to the closest lens system, being at a distance of $\simeq 380$ pc and mass $\simeq 0.25$ M$_{\odot}$., Accepted for publication on MNRAS, 2018. 6 Pages, 5 Figures. References updated

Published
2018
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37. Optical, near-IR and $X$-ray observations of SN 2015J and its host galaxy

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, Konstantina Boutsia, A. A. Nucita, Vincenzo Testa, A. M. Read, R. Saxton, D. Licchelli, Fabio Convenga, ITA, USA, GBR, GRC, Nucita, A. A., Paolis, F. De, Saxton, R., Testa, V., Strafella, F., Read, A., Licchelli, D., Ingrosso, G., Convenga, F., and Boutsia, K.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, X-ray, individual (SN 2015J) [supernovae], FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy and Astrophysic, 01 natural sciences, Galaxy, Luminosity, law.invention, Telescope, Supernova, Space and Planetary Science, law, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

SN 2015J was discovered on April 27th 2015 and is classified as a type IIn supernova. At first, it appeared to be an orphan SN candidate, i.e. without any clear identification of its host galaxy. Here, we present the analysis of the observations carried out {by the VLT 8-m class telescope with the FORS2 camera in the R band and the Magellan telescope (6.5 m) equipped with the IMACS Short-Camera (V and I filters) and the FourStar camera (Ks filter)}. We show that SN 2015J resides in what appears to be a very compact galaxy establishing a relation between the SN event and its natural host. We also present and discuss archival and new $X$-ray data centred on SN 2015J. At the time of the supernova explosion, Swift/XRT observations were made and a weak X-ray source was detected at the location of SN 2015J. Almost one year later, the same source was unambiguously identified during serendipitous observations by Swift/XRT and $XMM$-Newton, clearly showing an enhancement of the 0.3-10 keV band flux by a factor $\simeq 30$ with respect to the initial state. Swift/XRT observations show that the source is still active in the $X$-rays at a level of $\simeq 0.05$ counts s$^{-1}$. The unabsorbed X-ray luminosity derived from the {\it XMM}-Newton slew and SWIFT observations, $L_{x}\simeq 5\times10^{41}$ erg s$^{-1}$, places SN 2015J among the brightest young supernovae in X-rays., The Astrophysical Journal, Volume 850, Number 2

Published
2017

38. Time-dependent degradation of biotic carbonates and the search for past life on Mars

Author

Vincenzo Orofino, Armando Blanco, Sergio Fonti, M. D'Elia, D. Licchelli, Orofino, Vincenzo, Blanco, Armando, D’Elia, M., Fonti, Sergio, and Licchelli, D.

Subjects
Abiotic component, Martian, life, Carbonate, Astronomy and Astrophysics, Mars Exploration Program, Life on Mars, Astrobiology, chemistry.chemical_compound, Mar, Calcium carbonate, chemistry, Space and Planetary Science, Planet, Martian surface, Geology
Abstract

Searching for traces of extinct and/or extant life on the surface of Mars is one of the major objectives for remote-sensing and in-situ exploration of the planet. In the present paper we study the infrared (IR) spectral modifications induced by thermal processing on differently preserved calcium carbonate fossils, in order to discriminate them from their abiotic counterparts. The main conclusion of this study is that the degree of alteration of the fossils, derived from IR spectral analysis, seems to be well correlated with the sample age, and that terrestrial fossils after a billion years are so altered that it becomes impossible to trace their biotic origin. Since it is reasonable to assume that the putative Martian fossils should be at least 3.5 billion years old, this would imply that our spectroscopic method could not be able to detect them, if their degradation rate were the same as that we have found in usual conditions for the terrestrial fossils. However, due to the different climate evolution of the two planets, there is the possibility of having two different degradation rates, much lower for Mars than for Earth, especially if the fossils are embedded in a protective layer, such as a clay deposit. In this case IR spectroscopy, coupled with thermal processing, can be a useful tool for discriminating between abiotic and biotic (fossil) carbonate samples collected on the Martian surface.

Published
2009

39. Studies of Biominerals Relevant to the Search for Life on Mars

Author

Vincenzo Orofino, Armando Blanco, Sergio Fonti, M. D'Elia, D. Licchelli, J. Brucato, Blanco, Armando, D'Elia, Marcella, Licchelli, D., Orofino, Vincenzo, and Fonti, Sergio

Subjects
Abiotic component, Calcite, Water erosion, Extraterrestrial Environment, Spectrophotometry, Infrared, Liquid water, Aragonite, Origin of Life, Mars, Mineralogy, General Medicine, Mars Exploration Program, engineering.material, Life on Mars, Calcium Carbonate, Astrobiology, chemistry.chemical_compound, Durapatite, chemistry, Space and Planetary Science, Planet, Exobiology, engineering, Ecology, Evolution, Behavior and Systematics, Geology
Abstract

The evidence of the water erosion on Mars is particularly interesting since present climatic conditions are such that liquid water cannot exist at the surface. But, if water was present on the planet in the past, there may have been life, too. Since the discovery of carbonates on Mars also may have very important implications on the possibility that life developed there, we are studying minerals that can have biotic or abiotic origin: calcite (CaCO(3)) and aragonite, a metastable state of calcite.We have analysed biomineral aragonite, in the form of recent sea shells, as well as crystals of mineral aragonite. Infrared spectroscopy in the 2-25 mum wavelength range reveals that, after thermal processing, the biotic samples have a different spectral behaviour from the abiotic ones. As a result, it is possible to distinguish abiotic mineral aragonite from aragonite of recent biological origin.Obviously, if life existed in the past on the Red Planet, we could expect to find "ancient" biotic carbonates, which should therefore be investigated, in order to search for a way of discriminating them from abiotic minerals. For this reason, at the beginning we have considered samples of crushed fossil shells of aragonite composition. Afterwards, in order to take into account that fossilization processes almost always produce a transformation of metastable form (aragonite) into more stable form (calcite), we also studied samples of mineral calcite and different types of fossils completely transformed into calcite. All these biotic fossil samples show the same spectral behaviour as the fresh biotic material after thermal annealing at 485 degrees C. Instead, the calcite behaves like abiotic aragonite.Furthermore, it is known that seashells and other biominerals are formed through an intimate association of inorganic materials with organic macromolecules. The macromolecules control the nucleation, structure, morphology, crystal orientation and spatial confinement of the inorganic phase: this differentiates biominerals from minerals. Analysing the aragonite or calcite fossils with a Scanning Electron Microscope, we found that the fossilization process did not modify the structure of the biominerals which maintain their microscopic characteristics. Looking at the morphology of fossil biominerals, it is evident that the crystals are arranged in complex architectures compared with the compact structure of the mineral crystals. In conclusion, the properties and structure of the biominerals are different from those of the minerals. The rapid increase of the crystalline structure developed under biotic conditions makes these minerals less resistant to thermal treatments, compared with samples of abiotic origin. This result holds both for recent shells as well as all fossil samples. The spectroscopic behaviour of all analysed calcium carbonates of biotic origin is different from that of the abiotic one. Therefore, the infrared spectroscopy is a valid technique to discern the origin of the samples and a powerful tool for analysing in-situ and "sample-return" Mars missions specimens. Also Optical and Scanning Electron Microscopy can be useful to support this type of studies.

Published
2006
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40. Studies of biominerals relevant to the search for life on Mars.

Author

Blanco A, D'Elia M, Licchelli D, Orofino V, and Fonti S

Subjects
Calcium Carbonate analysis, Calcium Carbonate chemistry, Durapatite analysis, Durapatite chemistry, Extraterrestrial Environment chemistry, Origin of Life, Spectrophotometry, Infrared, Exobiology methods, Mars
Abstract

The evidence of the water erosion on Mars is particularly interesting since present climatic conditions are such that liquid water cannot exist at the surface. But, if water was present on the planet in the past, there may have been life, too. Since the discovery of carbonates on Mars also may have very important implications on the possibility that life developed there, we are studying minerals that can have biotic or abiotic origin: calcite (CaCO(3)) and aragonite, a metastable state of calcite.We have analysed biomineral aragonite, in the form of recent sea shells, as well as crystals of mineral aragonite. Infrared spectroscopy in the 2-25 mum wavelength range reveals that, after thermal processing, the biotic samples have a different spectral behaviour from the abiotic ones. As a result, it is possible to distinguish abiotic mineral aragonite from aragonite of recent biological origin.Obviously, if life existed in the past on the Red Planet, we could expect to find "ancient" biotic carbonates, which should therefore be investigated, in order to search for a way of discriminating them from abiotic minerals. For this reason, at the beginning we have considered samples of crushed fossil shells of aragonite composition. Afterwards, in order to take into account that fossilization processes almost always produce a transformation of metastable form (aragonite) into more stable form (calcite), we also studied samples of mineral calcite and different types of fossils completely transformed into calcite. All these biotic fossil samples show the same spectral behaviour as the fresh biotic material after thermal annealing at 485 degrees C. Instead, the calcite behaves like abiotic aragonite.Furthermore, it is known that seashells and other biominerals are formed through an intimate association of inorganic materials with organic macromolecules. The macromolecules control the nucleation, structure, morphology, crystal orientation and spatial confinement of the inorganic phase: this differentiates biominerals from minerals. Analysing the aragonite or calcite fossils with a Scanning Electron Microscope, we found that the fossilization process did not modify the structure of the biominerals which maintain their microscopic characteristics. Looking at the morphology of fossil biominerals, it is evident that the crystals are arranged in complex architectures compared with the compact structure of the mineral crystals. In conclusion, the properties and structure of the biominerals are different from those of the minerals. The rapid increase of the crystalline structure developed under biotic conditions makes these minerals less resistant to thermal treatments, compared with samples of abiotic origin. This result holds both for recent shells as well as all fossil samples. The spectroscopic behaviour of all analysed calcium carbonates of biotic origin is different from that of the abiotic one. Therefore, the infrared spectroscopy is a valid technique to discern the origin of the samples and a powerful tool for analysing in-situ and "sample-return" Mars missions specimens. Also Optical and Scanning Electron Microscopy can be useful to support this type of studies.

Published
2006
Full Text
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