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1. The optical, seismic, and infrasound signature of the March 5 2022, bolide over Central Italy

Author: Marco Olivieri, Davide Piccinini, Gilberto Saccorotti, Dario Barghini, Daniele Gardiol, Nicola Alessandro Pino, Maurizio Ripepe, Giulio Betti, Giorgio Lacanna, and Lorenzo Arcidiaco
Subjects: Medicine, Science
Abstract: Abstract On March 5, 2022, a 12 kg meteoroid crossed the sky above Central Italy and was observed by three different observational systems: the PRISMA all-sky camera network (10 stations), the Italian national seismic network (61 stations), and a 4-element infrasound array. The corresponding datasets, each with its own resolution, provided three independent assessments of the trajectory, size and speed of the meteoroid. The bolide traveled across central Italy with an azimuth of 102 degrees, becoming visible at about 91 km above sea level with a velocity of about 15.4 km/s. Its visible trajectory lasted about 15 s. Reasonably, the residual portion of the ablated bolide terminated its path in the Adriatic Sea and could not be recovered. Seismic and infrasound data well match optical observations detecting the bolide Mach cone at 68 km above sea level with a back azimuth of 25 degrees with respect to the array. By comparing results from the three different systems, discrepancies are within the estimated uncertainties, thus confirming the mutual consistency of the adopted methodologies. Therefore, this study shows that different approaches can be integrated to improve the detection capability for bolide crossing the sky in monitored regions.
Published: 2023
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2. Cosmogenic radionuclides in the Cavezzo meteorite: Gamma-ray measurement and detection efficiency simulations

Author: Ilaria Bizzarri, Dario Barghini, Paolo Colombetti, Daniele Gardiol, Sara Rubinetti, Salvatore Mancuso, Mario Di Martino, Giovanni Pratesi, Vanni Moggi Cecchi, Nora Groschopf, Andrea Aquino, Matthias Laubenstein, Narendra Bhandari, and Carla Taricco
Subjects: Radiation, Cosmogenic radionuclides, Gamma-ray spectrometry, Meteorites
Published: 2023

3. Sorvegliati Spaziali:an innovative outreach project on Planetary Defense

Author: Daria Guidetti, Caterina Boccato, Davide Coero Borga, Marco Galliani, Daniele Gardiol, and Paolo Soletta
Abstract: The aim of this talk i s to present “Sorvegliati Spaziali – know the Space to protect the Planet”, a public dissemination project of the Italian National Institute for Astrophysics (INAF) dedicated to the Planetary Defense: from near Earth asteroids and comets to space weather, from meteors and meteorites to space debris, as well as prevention/mitigation strategies of their possible effects on the Earth environment.Sorvegliati Spaziali represents one of the first coordinated public outreach initiatives on such topics by a research body and its main objective is to provide scientific and cultural knowledge to convey how our Planet is exposed to various natural and man-made threats in Space, as well as our current plans for response to them, meanwhile rowing against the many fake news about Planetary Defense that has biased the collective imagination.The core of the project is the Italian entirely graphic and multimedia website sorvegliatispaziali.inaf.it available online since October 2021 (translation in English in progress), which intends to become a national point of reference for information and in-depth content on Planetary Defense, timely disseminating scientific and cultural knowledge through a variety of original state-of-the-art multimedia information products, meanwhile relaunching news from other national and international research bodies.INAF original products, including the project website, are characterized by a strong and consistent visual identity and are: educational video-clips, interviews to scientists, geolocalized map with live satellites tracking, augmented reality and 3D computer graphic content, video-recorded theatrical pills, solar and Near Earth objects bulletins, infographics, a glossary. It is moreover foreseen the organization of a multimedia public event on the occasion of the Asteroid Day 2022 including a round table, movie screenings and a meteorites exhibition.The project is developed in collaboration with external research institutions, web design and professional theatrical companies and is endorsed by the Outreach Office of the NASA Planetary Defense Coordination Office. The figure below illustrates part of the homepage of the website sorvegliatispaziali.inaf.it .
Published: 2022
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4. Cavezzo—The double face of a meteorite: Mineralogy, petrography, and geochemistry of a very unusual chondrite

Author: Carla Taricco, Albino Carbognani, Daniele Gardiol, Giovanni Pratesi, Richard C. Greenwood, Vanni Moggi Cecchi, Ian A. Franchi, Mario Di Martino, Dario Barghini, and Samantha J. Hammond
Subjects: Olivine, Geochemistry, Mineralogy, Pyroxene, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Parent body, Troilite, Geophysics, Meteorite, Space and Planetary Science, Chondrite, 0103 physical sciences, engineering, Plagioclase, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Ordinary chondrite
Abstract: The Cavezzo meteorite, which fell on January 1, 2020, is the first meteorite detected and recovered by the Italian PRISMA Fireball Network. Two specimens, weighing 3.12 g (specimen 1) and 52.19 g (specimen 2), were collected 3 days after the bolide was observed, thanks to an effective media campaign that encouraged the involvement of local people. The two specimens of this meteorite have not only completely different lithological characteristics but also a different geochemistry and oxygen isotopic composition as well. Specimen 1 is anomalous both for the textural–structural features, varying seamlessly from chondritic to “achondritic,” and a very unusual modal mineralogy—such as the relatively high amount of olivine (63.1 vol%), plagioclase (18.2 vol%), high-Ca pyroxene (10.3 vol%), and chlorapatite (2.1 vol%); and the unusually low content of low-Ca pyroxene (5.8 vol%), metal (0.1 vol%), and troilite (much lesser than 0.1 vol%)—although the compositional values for olivine (Fa 24.24 mol%) and low-Ca pyroxene (Fs 20.41 mol%) appear to be similar to those of the L chondrite group. Conversely, in specimen 2, not only the texture and the crystal chemistry but also the modal mineralogy (low-Ca pyroxene much more abundant than high-Ca pyroxene and occurrence of metal and sulfides) look like those of an ordinary L chondrite. The differences between the two specimens are also confirmed by geochemistry. The oxygen isotope composition of specimen 1 plots at the boundary between the H and L groups (δ17O‰ 3.250; δ18O‰ 4.736; Δ17O‰ 0.788) whereas specimen 2 plots at the boundary of the L and LL fields (δ17O‰ 3.737; δ18O‰ 4.957; Δ17O‰ 1.159). The bulk chemistry shows a different content of many minor and trace elements (including rare earth elements), such as a strong depletion of siderophile and chalcophile elements in specimen 1. The two specimens then do not contain fragments of each other, thus preventing us from classifying this “double face” meteorite as an ordinary chondrite breccia. In detail, specimen 1 can be considered a “xenolith” in which chondritic structure and igneous texture coexist without discontinuity, and therefore, it represents a previously unsampled portion of the L parent body. In summary, these findings support the classification of Cavezzo as an L5 anomalous chondrite.
Published: 2021
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5. Planetary sciences artfully told

Author: Daniele Gardiol
Abstract: In the context of a project of narration of astrophysical themes through Cinema and Theater, we will tell the story of the birth of a documentary film on the discovery of the Cavezzo Meteorite, made by the PRISMA fireball network in January 2020. The Italian National Institute for Astrophysics and the theater company Il Piccolo Teatro d'Arte have created a documentary that brings the voices of the protagonists of the discovery together with the mythical, historical and poetic narration of the meteoric phenomenon in a broad sense, with the aim of obtaining an involvement of the audience on both sound science and emotionality.
Published: 2021
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6. Experiential teaching of planetary sciences from kindergartens to secondary schools: the 'Astronomiadi' educational project

Author: Daniele Gardiol, Carlo Benna, Valentina Vignale, and Fabrizio Radicati di Primeglio
Abstract: The Piedmontese town of Pino Torinese is one of the twelve italian locations hosting a local department of the Italian National Institute for Astrophysics, the Astronomical Observatory of Turin. This peculiarity led to the development of a close collaboration between researchers, teachers and local community and administration, aiming at the promotion of astronomy, and in particular planetary sciences, among students from kindergartens to secondary schools. The chosen driving approach, experiential learning, is not very common in Italy.
Published: 2021
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7. Study of the calibration method using the stars measured by the EUSO-TA telescope

Author: F. Bisconti, Dario Barghini, R. Lipiec, Z. Plebaniak, Lech Wiktor Piotrowski, M. Przybylak, J. Szabelski, Marco Casolino, M. E. Bertaina, K. Shinozaki, and Daniele Gardiol
Subjects: Point spread function, Physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Field of view, Star position, law.invention, Telescope, Stars, Optics, law, Physics::Space Physics, Calibration, Ultra-high-energy cosmic ray, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: EUSO-TA is a ground-based experiment, placed at Black Rock Mesa of the Telescope Array site as a part of the JEM-EUSO (Joint Experiment Missions for the Extreme Universe Space Observatory) program. The UV fluorescence imaging telescope with a field of view of about 10.6 deg x 10.6 deg consisting of 2304 pixels (36 Multi-Anode Photomultipliers, 64 pixels each) works with 2.5-microsecond time resolution. An experimental setup with two Fresnel lenses allows for measurements of Ultra High Energy Cosmic Rays in parallel with the TA experiment as well as the other sources like flashes of lightning, artificial signals from UV calibration lasers, meteors and stars. Stars increase counts on pixels while crossing the field of view as the point-like sources. In this work, we discuss the method for calibration of EUSO fluorescence detectors based on signals from stars registered by the EUSO-TA experiment during several campaigns. As the star position is known, the analysis of signals gives an opportunity to determine the pointing accuracy of the detector. This can be applied to space-borne or balloon-borne EUSO missions. We describe in details the method of the analysis which provides information about detector parameters like the shape of the point spread function and is the way to perform absolute calibration of EUSO cameras.
Published: 2021
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8. Luminous efficiency based on FRIPON meteors and limitations of ablation models

Author: Björn Poppe, B. Zanda, C. A. Volpicelli, J. Vaubaillon, Jim Rowe, Detlef Koschny, Pierre Vernazza, O. Hernandez, François Colas, Dan Alin Nedelcu, M. Forcier, Sylvain Bouley, Theresa Ott, Agustín Sánchez-Lavega, Josep M. Trigo-Rodríguez, Cristina Knapic, S. Rasetti, Esther Drolshagen, Daniele Gardiol, A. Toni, M. Di Carlo, Giovanni Pratesi, H. Lamy, Giovanni B. Valsecchi, Ludovic Ferrière, Sonia Zorba, E. Peña-Asensio, Mirel Birlan, Albert Rimola, A. Malgoyre, M. Jobin, S. Jeanne, Ashley J. King, Albino Carbognani, Emmanuel Jehin, Dario Barghini, Gerhard Drolshagen, W. Riva, G. M. Stirpe, A. Grandchamps, M. Di Martino, 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), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Meteor (satellite), 010504 meteorology & atmospheric sciences, Meteors, Context (language use), Astrophysics, 01 natural sciences, meteorites, techniques: photometric, 0103 physical sciences, meteorites, meteors, meteoroids, minor planets, asteroids: general, comets: general, techniques: photometric, atmospheric effects, methods: data analysis, Emission spectrum, meteors, data analysis [Methods], meteoroids, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Meteoroid, comets: general, photometric [Techniques], Minor planets, general [Comets], Astronomy and Astrophysics, Meteoroids, Atmospheric effects, methods: data analysis, asteroids: general, Wavelength, Meteorite, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], minor planets, Luminous efficacy, Interplanetary spaceflight, general [Asteroids], Meteorites, atmospheric effects
Abstract: Drolshagen, E., et al., [Context] In meteor physics, the luminous efficiency τ is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. [Aims] In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. [Methods] Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. [Results] We find τ-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10-6-100 kg. The derived τ-values have a median of τmedian = 2.17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of τ on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of τ = 0.0023 ve2.3. Furthermore, a dependence of τ on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: τ = 0.48 Me-0.47. [Conclusions] The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of τ on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.
Published: 2021
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9. 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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10. Characterization of the DIMS system based on astronomical meteor techniques for macroscopic dark matter search

Author: Alberto Cellino, Hiroyuki Sagawa, Simone Valenti, Sachiko Tada, Daiki Shinto, F. Kajino, Mizuho Arahori, Soon-Wook Kim, Toshikazu Ebisuzaki, Glenn D. Starkman, Shinsuke Abe, Maria Hajdukova, Daniele Gardiol, Corbin Covault, Ryushin Ide, Dario Barghini, Marco Casolino, M. E. Bertaina, Yuichiro Tameda, John N. Matthews, Il Han Park, Kenji Shinozaki, Yoshiyuki Takizawa, Jagjit Singh Sidhu, Yugo Iwami, Lech Wiktor Piotrowski, Kaoru Nadamoto, and Yasunori Fujiwara
Subjects: Meteor (satellite), Physics, Dark matter, Astronomy, Characterization (materials science)
Published: 2021

11. PRISMA and the finding of the Cavezzo meteorite: the success of a close collaboration among professional astronomers, amateurs and citizens

Author: Daniele Gardiol
Subjects: Meteorite, Political science, Library science
Abstract: I will tell the story of the recent success of the italian fireball network PRISMA (Prima Rete Italiana per la Sorveglianza sistematica di Meteore e Atmosfera) in finding the first italian meteorite thanks to the computation of a precise strewn-field made possible by observations with eight all-sky camera of the network. And how this success is due to close cooperation among professional astronomers, amateur astronomers, astronomy enthusiasts and simple citizens.
Published: 2020
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12. A report on the New Year's meteorite found near Cavezzo, Italy

Author: Alberto Buzzoni, S. Rasetti, Cristina Knapic, Daniele Gardiol, Sonia Zorba, Team Prisma, Di Carlo Matteo, Giovanni B. Valsecchi, G. M. Stirpe, Elisa Londero, W. Riva, Dario Barghini, Giovanni Pratesi, Antonio Volpicelli, Albino Carbognani, and Di Martino Mario
Subjects: Planetary science, Meteorite, Geology, Astrobiology
Abstract: In this talk we report about the recent finding of two meteorite samples in Italy, near Cavezzo (Modena). The meteorite-dropping fireball was observed on the evening of New Year's Day 2020 by eight all-sky cameras of the PRISMA network, partner of FRIPON. The two fragments, weighing 4 g and 52 g respectively, were collected as a result of a dedicated field search and thanks to the involvement of the local population.
Published: 2020
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13. A case study of the May 30, 2017, Italian fireball

Author: Mirel Birlan, D. Barghini, Alberto Buzzoni, P. Demaria, L. Maquet, J. Vaubaillon, Brigitte Zanda, Daniele Gardiol, Giovanni B. Valsecchi, Chiara Marmo, M. Di Martino, Jerome Gattacceca, Sonia Zorba, M. Di Carlo, Pierre Vernazza, Cristina Knapic, Jean-Louis Rault, Elisa Londero, P. Trivero, François Colas, F. Zanotti, Sylvain Bouley, S. Rasetti, C. A. Volpicelli, Albino Carbognani, D. Valeri, M. Morini, D. Selvestrel, Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVDA), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), 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), Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Grupo de Acuicultura y Biodiversidad, Instituto de Ciencia y Tecnología Animal, Universitat Politècnica de València (UPV), 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), 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), 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), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universitat Politecnica de Valencia (UPV), UMS Nano-analyses (UNA), Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), 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), and Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Collège de France (CdF)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Meteoroid, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, 13. Climate action, Sky, 0103 physical sciences, Atmospheric dynamics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Astrophysics - Earth and Planetary Astrophysics
Abstract: On May 30th, 2017 at about 21h 09m 17s UTC a green bright fireball crossed the sky of north-eastern Italy. The fireball path was observed from some all-sky cameras starting from a mean altitude of $81.1 \pm 0.2$ km (Lat. $44.369^{\circ} \pm 0.002^{\circ}$ N; Long. $11.859^{\circ} \pm 0.002^{\circ}$ E) and extinct at $23.3 \pm 0.2$ km (Lat. $45.246^{\circ} \pm 0.002^{\circ}$ N; Long. $12.046^{\circ} \pm 0.002^{\circ}$ E), between the Italian cities of Venice and Padua. In this paper, on the basis of simple physical models, we will compute the atmospheric trajectory, analize the meteoroid atmospheric dynamics, the dark flight phase (with the strewn field) and compute the best heliocentric orbit of the progenitor body. Search for meteorites on the ground has not produced any results so far., 19 pages, 17 figures. Accepted for publication in The European Physical Journal PLUS
Published: 2020
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14. Luminous efficiency of meteors derived from ablation model after assessment of its range of validity

Author: M. Di Carlo, Ashley J. King, Esther Drolshagen, Mirel Birlan, Pierre Vernazza, M. Forcier, Ludovic Ferrière, E. Peña-Asensio, Theresa Ott, Dan Alin Nedelcu, C. A. Volpicelli, François Colas, O. Hernandez, Sylvain Bouley, Daniele Gardiol, Cristina Knapic, Giovanni Pratesi, Agustín Sánchez-Lavega, Josep M. Trigo-Rodríguez, H. Lamy, G. M. Stirpe, S. Rasetti, Giovanni B. Valsecchi, Jim Rowe, Sonia Zorba, Albert Rimola, J. Vaubaillon, Brigitte Zanda, S. Jeanne, A. Toni, M. Di Martino, M. Jobin, Albino Carbognani, Björn Poppe, Gerhard Drolshagen, A. Grandchamps, Emmanuel Jehin, W. Riva, Detlef Koschny, Dario Barghini, A. Malgoyre, 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), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Meteors, 010504 meteorology & atmospheric sciences, Context (language use), Astrophysics, 01 natural sciences, meteorites, techniques: photometric, 0103 physical sciences, Range (statistics), meteorites, meteors, meteoroids, minor planets, asteroids: general, comets: general, techniques: photometric, atmospheric effects, methods: data analysis, meteors, data analysis [Methods], meteoroids, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Meteoroid, comets: general, photometric [Techniques], Relative velocity, Minor planets, general [Comets], Astronomy and Astrophysics, Meteoroids, Function (mathematics), Atmospheric effects, methods: data analysis, asteroids: general, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Asteroid, minor planets, Meteorities, Luminous efficacy, Interplanetary spaceflight, general [Asteroids], atmospheric effects
Abstract: Drolshagen, E., et al., [Context] The luminous efficiency, τ, can be used to compute the pre-Atmospheric masses of meteoroids from corresponding recorded meteor brightnesses. The derivation of the luminous efficiency is non-Trivial and is subject to biases and model assumptions. This has led to greatly varying results in the last decades of studies. [Aims] The present paper aims to investigate how a reduction in various observational biases can be achieved to derive (more) reliable values for the luminous efficiency. [Methods] A total of 281 meteors observed by the Fireball Recovery and InterPlanetary Observation Network (FRIPON) are studied. The luminous efficiencies of the events are computed using an ablation-based model. The relations of τ as a function of the pre-Atmospheric meteoroid velocity, ve, and mass, Me, are studied. Various aspects that could render the method less valid, cause inaccuracies, or bias the results are investigated. On this basis, the best suitable meteors were selected for luminous efficiency computations. [Results] The presented analysis shows the limits of the used method. The most influential characteristics that are necessary for reliable results for the τ computation were identified. We study the dependence of τ on the assumed meteoroid's density, ρ, and include improved ρ-values for objects with identified meteoroid stream association. Based on the discovered individual biases and constraints we create a pre-debiased subset of 54 well-recorded events with a relative velocity change >80%, a final height
Published: 2021
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15. Il bolide d’autunno

Author: Daniele Gardiol
Abstract: Avvistata due sere fa da sette fotocamere della rete Prisma mentre solcava i cieli della Toscana, la meteora si è spenta a circa 80 km di quota. L’alta velocità di ingresso in atmosfera e la significativa eccentricità dell'orbita inducono a ritenere che abbia un’origine cometaria
Published: 2020
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16. Meteor detection from space with Mini-EUSO telescope

Author: Hiroko Miyamoto, Guillaume Prévôt, Matteo Battisti, Enzo Reali, A. Belov, M. E. Bertaina, Dario Barghini, L. Marcelli, Pavel Klimov, Daniele Gardiol, Francesca Capel, Naoto Sakaki, Piergiorgio Picozza, Toshikazu Ebisuzaki, Lech Wiktor Piotrowski, Yoshiyuki Takizawa, Francesca Bisconti, and Marco Casolino
Subjects: Telescope, Meteor (satellite), Physics, law, Astronomy, Space (mathematics), law.invention
Abstract: Mini-EUSO is a very wide (44°x44°) field of view telescope installed on August 2019 inside the Zvezda Module of the ISS, looking nadir through a UV transparent window and taking data since October 2019. Its optical system consists of two Fresnel lenses, focusing the light onto an array of 36 multi-anode photomultiplier tubes. The focal surface counts a total of 2304 pixels, each one having a footprint of about 6.5 km on ground. The instrument triggers on two different timescales, respectively 2.5 μs (D1) and 320 μs (D2), and perform a continuous monitoring of the UV emission at a 40.96 ms timescale (D3). At time of writing, about one thousand meteors on D3 data have been classified as meteors using our current detection algorithm. We describe here a concept of an alternative algorithm to recognize meteors in the D3 continuous data-stream, which can be also implemented in the future for online triggering, and show some examples of detected meteors by our instrument. We also performed a search of possible coincident detections of Mini-EUSO meteors by ground meteor and fireball networks, such as PRISMA in Italy, to gain a stereoscopic vision of the event itself. In light of these initial results, we present here the capabilities of Mini-EUSO instrument in meteor science.
Published: 2020

17. The EUSO@Turlab Project: Tests of Mini-EUSO Engineering Model

Author: A. Franceschi, L. Marcelli, G. Contino, Maria Teresa Ricci, A. Djakonow, Marco Mignone, Lech Wiktor Piotrowski, A. Murashov, J. Szabelski, M.E Bertaina, Naoto Sakaki, Pavel Klimov, W. Marszał, Matteo Battisti, F. Bisconti, Alexander S. Belov, A. Poroshin, K. Shinozaki, S. Blin-Bondil, Daniele Gardiol, Francesca Capel, Francesco Fenu, Enzo Reali, M. Przybylak, A. Cellino, E. Parizot, P. Picozza, M. I. Panasyuk, G. Suino, M. Bertaina, S. Turriziani, Toshikazu Ebisuzaki, Federico Fausti, Marco Casolino, Claudio Fornaro, Guillaume Prévôt, G. Cambiè, I. Churilo, P. Gorodetzky, F. Kajino, M. Traïche, F. Cafagna, Y. Takizawa, Z. Plebaniak, G. Osteria, Christer Fuglesang, R. Bonino, T. Napolitano, Rossella Caruso, G. Cotto, Organisation de Micro-Électronique Générale Avancée (OMEGA), École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), JEM-EUSO, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Brightness, business.industry, Detector, Cosmic ray, Field of view, Rotating tank, law.invention, Telescope, law, Environmental science, Focal surface, Aerospace engineering, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Space debris
Abstract: International audience; The TurLab facility is a laboratory, equipped with a 5 m diameter and 1 m depth rotating tank, located in the Physics Department of the University of Turin. Originally, it was mainly built to study systems of different scales where rotation plays a key role in the fluid behaviour such as in atmospheric and oceanic flows. In the past few years the TurLab facility has been used to perform experiments related to the observation of Extreme Energy Cosmic Rays (EECRs) from space using the fluorescence technique. For example, in the case of the JEM-EUSO mission, where the diffuse night brightness and artificial light sources can vary significantly in time and space inside the Field of View of the telescope. The Focal Surface of Mini-EUSO Engineering Model (Mini-EUSO EM) with the level 1 (L1) and 2 (L2) trigger logics implemented in the Photo-Detector Module (PDM) has been tested at TurLab. Tests related to the possibility of using an EUSO-like detector for other type of applications such as Space Debris (SD) monitoring and imaging detector have also been pursued. The tests and results obtained within the EUSO@TurLab Project on these different topics are presented.
Published: 2019
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18. Calibration of fish-eye lens and error estimation on fireball trajectories: application to the FRIPON network

Author: J. Rault, Laurent Jorda, Jeremie Vaubaillon, Daniele Gardiol, François Colas, S. Jeanne, Sylvain Bouley, H. Lamy, Julien Lecubin, Albino Carbognani, Cyrille Blanpain, A. Malgoyre, Mirel Birlan, David Baratoux, Pierre Vernazza, P. Hewins, J. Gattacceca, B. Zanda, Chiara Marmo, 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 de minéralogie et de physique des milieux condensés (IMPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), 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), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), 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), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Royal Belgian Inst Space Aeron, Ave Circulaire 3, B-1180 Brussels, Belgium, Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), ITA, FRA, Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-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 de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 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), IMCCE-CNRS, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Collège de France (CdF)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA), INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy, and Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Polynomial, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Context (language use), Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, meteorites, 0103 physical sciences, Calibration, meteors, meteoroids, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Pixel, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Distortion (optics), Astronomy and Astrophysics, Astrometry, meteorites, meteors, meteoroids, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Trajectory, Orbit (dynamics), astrometry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm
Abstract: Context. Fireball networks are developing over the whole planet, with the aim of recovering meteorites and at the same time determining their orbits. The ultimate goal of such networks is to identify the parent bodies of meteorite families to achieve this, orbit accuracy is critical. Yet, the determination of an orbit relies on a long and complex reduction process including: (1) astrometry, with heavy distortion for fish-eye lenses, (2) estimation of the external bias on the observation, (3) fit of the trajectory, (4) deceleration model, and (5) actual orbit computation. Aims. Our goal is to compute accurate trajectories with an estimate of internal and external errors as realistic as possible, taking advantage of the dense observation network FRIPON (Fireball Recovery and InterPlanetary Observation Network), which comprises more than 100 cameras in France and Europe. In particular, we pay special attention to the distortion of images due to fish-eye lenses. In the present paper, we describe the analytical protocol that allows us to compute trajectories and their uncertainties. Methods. We developed a general distortion model to be used on the FRIPON fish-eye cameras. Such a model needs to be accurate even at low elevation, as most fireball observations are performed low on the horizon. The radial distortion is modelled by a nine-degree odd polynomial, hence by five parameters. In addition, we used three parameters to describe the geometry of the camera and two for non-symmetrical distortion. Lastly, we used a new statistical method taking systematic errors into account, which allows us to compute realistic confidence intervals. We tested our method on a fireball that fell on 2017-08-94 UT 00:06. Results. The accuracy of our astrometrical model for each camera is 2 arcmin (1σ), but the internal error on the fireball of 2017-08-94 UT 00:06 measurement is 0.7 arcmin (better than 1/10 pixel). We developed a method to estimate the external error considering that each station is independent and found it equal to 0.8 arcmin. Real residuals are coherent with our estimation of internal and external error for each camera, which confirms the internal consistency of our method. We discuss the advantages and disadvantages of this protocol.
Published: 2019
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19. Anatomia del bolide del 27 marzo

Author: Daniele Gardiol
Abstract: Nella notte fra il 27 e il 28 marzo 2019 un brillante bolide ha fatto la sua comparsa nei cieli del nord Italia. Il bolide è stato ripreso da ben 13 camere della rete Prisma. Grazie ai numerosi dati raccolti, è stato possibile tracciare un identikit dettagliato del fenomeno
Published: 2019
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20. Mini-EUSO engineering model: tests in open-sky condition

Author: Christer Fuglesang, S. Turriziani, Toshikazu Ebisuzaki, Federico Fausti, Lech Wiktor Piotrowski, Z. Plebaniak, J. Szabelski, G. Osteria, A. Djakonow, Naoto Sakaki, P. Gorodetzky, W. Marszał, G. Cotto, A. Belov, A. Murashov, A. Cellino, G. Suino, Matteo Battisti, Marco Casolino, Claudio Fornaro, Daniele Gardiol, Dario Barghini, Y. Takizawa, P. Picozza, Francesca Capel, G. Cambiè, I. Churilo, S. Blin-Bondil, T. Napolitano, F. Bisconti, K. Shinozaki, Hiroko Miyamoto, A. Poroshin, Maria Teresa Ricci, Enzo Reali, A. Franceschi, L. Marcelli, Guillaume Prévôt, Francesco Fenu, F. Kajino, E. Parizot, M. Traïche, M. Przybylak, F. Cafagna, Marco Mignone, M. E. Bertaina, Pavel Klimov, M. I. Panasyuk, Organisation de Micro-Électronique Générale Avancée (OMEGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), JEM-EUSO, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Night sky, FOS: Physical sciences, Cosmic ray, law.invention, Atmosphere, Telescope, Planet, law, International Space Station, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Meteoroid, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 13. Climate action, Sky, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Mini-EUSO is a UV telescope that will look downwards to the Earth's atmosphere onboard the International Space Station. With the design of the ultra-high energy cosmic ray fluorescence detectors belonging to the JEM-EUSO program, it will make the first UV map of the Earth by observing atmospheric phenomena such as transient luminous events, sprites and lightning, as well as meteors and bioluminescence from earth. Diffused light from laser shots from the ground, which mimic the fluorescence light emitted by Nitrogen molecules when extensive air showers pass through the atmosphere, can be used to verify the capability of this kind of detector to observe ultra-high energy cosmic rays. To validate the electronics and the trigger algorithms developed for Mini-EUSO, a scaled down version of the telescope with 1:9 of the original focal surface and a lens of 2.5 cm diameter has been built. Tests of the Mini-EUSO engineering model have been made in laboratory and in open sky condition. In this paper, we report results of observations of the night sky, which include the detection of stars, meteors, a planet and a rocket body reflecting the sunlight. Interesting results of the observation of city lights are also reported., Comment: presented at the 36th ICRC (Madison, WI; 2019)
Published: 2019
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21. SOXS: a wide band spectrograph to follow up transients

Author: Johan P. U. Fynbo, H. U. Käufl, J. Lehti, A. Brucalassi, Massimo Turatto, T. Kumar, Matteo Accardo, H. Kuncarayacti, Matteo Genoni, Marco Riva, P. D'Avanzo, Daniela Fantinel, Matteo Aliverti, Jari Kotilainen, Federico Biondi, Davide Loreggia, Adam Rubin, Rosario Cosentino, Stephen J. Smartt, Sergio Campana, Fabrizio Vitali, Andrea Baruffolo, Seppo Mattila, R. Zanmar Sanchez, Salvo Scuderi, Matteo Munari, Giuliano Pignata, Francesco D'Alessio, Antonino Bianco, M. Hirvonen, Sergio D'Orsi, M. Della Valle, S. Ben Ami, Iair Arcavi, G. Capasso, Daniele Gardiol, D. Ricci, Luca Marafatto, G. Li Causi, Enrico Cappellaro, J. Achrén, Riccardo Claudi, Avishay Gal-Yam, J. Antonio Araiza-Duran, Giorgio Pariani, Bernardo Salasnich, Marco Landoni, O. Diner, O. Hershko, Pietro Schipani, M. Colapietro, and Michael Rappaport
Subjects: Physics, ta115, 010504 meteorology & atmospheric sciences, Gravitational wave, FOS: Physical sciences, Astronomy, 01 natural sciences, law.invention, SOXS, Telescope, Photometry (optics), Supernova, Limiting magnitude, law, Target of opportunity, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, astro-ph.IM, 0105 earth and related environmental sciences
Abstract: SOXS (Son Of X-Shooter) will be a spectrograph for the ESO NTT telescope capable to cover the optical and NIR bands, based on the heritage of the X-Shooter at the ESO-VLT. SOXS will be built and run by an international consortium, carrying out rapid and longer term Target of Opportunity requests on a variety of astronomical objects. SOXS will observe all kind of transient and variable sources from different surveys. These will be a mixture of fast alerts (e.g. gamma-ray bursts, gravitational waves, neutrino events), mid-term alerts (e.g. supernovae, X-ray transients), fixed time events (e.g. close-by passage of minor bodies). While the focus is on transients and variables, still there is a wide range of other astrophysical targets and science topics that will benefit from SOXS. The design foresees a spectrograph with a Resolution-Slit product ~ 4500, capable of simultaneously observing over the entire band the complete spectral range from the U- to the H-band. The limiting magnitude of R~20 (1 hr at S/N~10) is suited to study transients identified from on-going imaging surveys. Light imaging capabilities in the optical band (grizy) are also envisaged to allow for multi-band photometry of the faintest transients. This paper outlines the status of the project, now in Final Design Phase., Comment: 12 pages, 14 figures, to be published in SPIE Proceedings 10702
Published: 2018
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22. The acquisition camera system for SOXS at NTT

Author: Enrico Cappellaro, Marco Landoni, Federico Biondi, M. Hirvonen, Giorgio Pariani, A. Brucalassi, Salvatore Scuderi, Michael Rappaport, Bernardo Salasnich, Marco Riva, Daniela Fantinel, Pietro Schipani, M. Colapietro, O. Diner, J. Lehti, Sagi Ben-Ami, Matteo Genoni, Riccardo Claudi, Fabrizio Vitali, Jari Kotilainen, O. Hershko, Massimo Turatto, Luca Marafatto, Andrea Bianco, Avishay Gal-Yam, J. A. Araiza-Duran, Seppo Mattila, D. Ricci, Iair Arcavi, Sergio Campana, Johan P. U. Fynbo, Sergio D'Orsi, J. Achrén, G. Li Causi, Stephen J. Smartt, Hanindyo Kuncarayakti, R. Zanmar Sanchez, P. D'Avanzo, Matteo Aliverti, Davide Loreggia, Daniele Gardiol, Adam Rubin, Giuliano Pignata, Francesco D'Alessio, G. Capasso, Matteo Munari, Andrea Baruffolo, M. Della Valle, T. Kumar, and Rosario Cosentino
Subjects: ta115, ta114, Computer science, Real-time computing, Response time, 01 natural sciences, Target acquisition, Optical quality, law.invention, 010309 optics, SOXS, Telescope, Photometry (optics), Relay, law, 0103 physical sciences, 010303 astronomy & astrophysics, Spectrograph
Abstract: SOXS (Son of X-Shooter) will be the new medium resolution (R~4500 for a 1 arcsec slit), high-efficiency, wide band spectrograph for the ESO-NTT telescope on La Silla. It will be able to cover simultaneously optical and NIR bands (350-2000nm) using two different arms and a pre-slit Common Path feeding system. SOXS will provide an unique facility to follow up any kind of transient event with the best possible response time in addition to high efficiency and availability. Furthermore, a Calibration Unit and an Acquisition Camera System with all the necessary relay optics will be connected to the Common Path sub-system. The Acquisition Camera, working in optical regime, will be primarily focused on target acquisition and secondary guiding, but will also provide an imaging mode for scientific photometry. In this work we give an overview of the Acquisition Camera System for SOXS with all the different functionalities. The optical and mechanical design of the system are also presented together with the preliminary performances in terms of optical quality, throughput, magnitude limits and photometric properties.
Published: 2018

23. Improvement of the extraction method of faint signals in $ \gamma$ γ -activity measurements of meteorites⋆

Author: Sara Rubinetti, Salvatore Mancuso, Dario Barghini, Daniele Gardiol, M. Di Martino, P. Colombetti, and Carla Taricco
Subjects: Physics, 010504 meteorology & atmospheric sciences, Spectrometer, Detector, General Physics and Astronomy, 01 natural sciences, Coincidence, Computational physics, Astrobiology, Activity measurements, Meteorite, 0103 physical sciences, Underground laboratory, Extraction methods, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: At the underground laboratory of Monte dei Cappuccini (OATo-INAF) in Torino (Italy) we set up selective HPGe-NaI(Tl) spectrometers for measurements of cosmogenic radioisotopes in meteorites in order to study centennial-scale modulation of solar activity. 44 Ti is a suitable proxy for this timescale, but its detection is difficult due to the strong interference by naturally occurring 214 Bi. In order to optimize the extraction of the 44 Ti signal, we have developed software procedures specifically designed to improve selectivity of the Ge-NaI detectors coincidence.
Published: 2017
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24. Astrometric calibration for all-sky cameras revisited

Author: Salvatore Mancuso, Dario Barghini, Albino Carbognani, Daniele Gardiol, and ITA
Subjects: Point spread function, Physics, 010308 nuclear & particles physics, Random projection, techniques: image processing, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrometry, methods: data analysis, 01 natural sciences, meteorites, Cardinal point, Space and Planetary Science, Position (vector), Bolide, 0103 physical sciences, Parametric model, astrometry, meteors, meteoroids, 010303 astronomy & astrophysics, Algorithm, meteorites, meteors, meteoroids, astrometry, methods: data analysis, techniques: image processing
Abstract: Context. Several fireball networks deploy all-sky cameras for the observation of bright meteors and bolides. Because the field is heavily distorted, a dedicated astrometric reduction is needed. A precise computation of the astrometric solution is essential to determine reliable orbital elements of the parent body and to recover possible fragments on ground.Aims. The purpose of this article is to assess the astrometric performances of this type of instruments, which is characterized by a wide field of view and small apertures. The currently available parametric models show a high level of complexity and generally suffer from parameter crosstalk and local minimum confinement if the initial estimates are not precisely provided. We address these issues here and propose a solution by adopting a new explicit parametrisation.Methods. The mismatch between the optical axis and the local zenith direction requires a geometric description that includes two centres of symmetry that lie very close to each other on the focal plane, causing an unreliable estimate of the related parameters. The introduction of new physical coordinates overcomes these issues, allowing a direct and independent estimation. We assessed the performances of different centroiding algorithms in the experimental conditions of an undersampled point spread function of reference stars and saturated bolides on video records. We implemented the algorithm for an automatic identification of bright sources on calibration frames and subsequent correlation with catalogue positions using astrometric projections of increasing complexity.Results. The algorithm and the new parametrisation of the astrometric solution are tested against real data from the PRISMA Italian fireball network and ensure good convergence properties for all cameras we tested so far. By processing astrometric data with a few months’ statistics, we can achieve a random projection indeterminacy of the order of 10 arcsec, which is negligible with respect to single measurement errors on the bolide position.
Published: 2019
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25. The ASTRI SST-2M prototype for the Cherenkov Telescope Array: opto-mechanical performance

Author: Giovanni Pareschi, Federico Russo, Enrico Marcuzzi, Gianpietro Marchiori, D. Fugazza, Luca Stringhetti, Salvatore Scuderi, Daniele Gardiol, Giorgia Sironi, Enrico Giro, Rodolfo Canestrari, Elisa Antolini, Gino Tosti, Ivan Folla, Claudio Tanci, A. Busatta, Carlos Eduardo Fermino, ITA, and BRA
Subjects: Imaging atmospheric cherenkov telescope, Kinematics, Very high-energy gamma-rays, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, 01 natural sciences, Imaging atmospheric Cherenkov telescopes, law.invention, Telescope, Tellurium compounds, Observatory, law, 0103 physical sciences, ASTRI, Very high energies, Segmented optics, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Cherenkov radiation, Physics, Wide field, Airborne telescopes, Mirrors, Tellurium compounds, ASTRI, Wide field, Gamma rays, CTA, Wide-field aplanatic telescope, 010308 nuclear & particles physics, Gamma rays, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Cherenkov Telescope Array, Reflectivity
Abstract: ASTRI SST-2M is an end-to-end telescope prototype developed by the Italian National Institute of Astrophysics (INAF) in the framework of the Cherenkov Telescope Array (CTA). The CTA observatory, with a combination of large-, medium-, and small-sized telescopes (LST, MST and SST, respectively), will represent the next generation of imaging atmospheric Cherenkov telescopes. It will explore the very high-energy domain from a few tens of GeV up to few hundreds of TeV. The ASTRI SST-2M telescope structure and mirrors have been installed at the INAF observing station at Serra La Nave, on Mt. Etna (Sicily, Italy) in September 2014. Its performance verification phase began in autumn 2015. Part of the scheduled activities foresees the study and characterization of the optical and opto-mechanical performance of the telescope prototype. In this contribution we report the results achieved in terms of kinematic model analysis, mirrors reflectivity evolution, telescopes positioning, flexures and pointing model and the thermal behavior.
Published: 2016
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26. Instrument physical model for the SOXS (Son Of X-Shooter) spectrograph

Author: Daniele Gardiol, Davide Loreggia, and ITA
Subjects: SOXS, Engineering, Optics, Software, business.industry, Limiting magnitude, Electronic engineering, Ranging, Field of view, business, Spectrograph, Data reduction, Physical quantity
Abstract: We present the proposal for the physical instrument model of the SOXS (Son OF X-Shooter) spectroscopic facility mainly devoted to the follow-up observation of transient sources. A dedicated suitable instrument to exploit the science of these transients is lacking, resulting in severe science "dissipation". SOXS will cover the optical/NIR band (0.35-1.75 μm) with a medium resolution (R 4500), down to the limiting magnitude of R 20-20.5 (1 hr at S/N 10) that is perfectly suited to study transients from on-going imaging surveys. Imaging capabilities in the optical are also foreseen to allow for multi-band photometry of the faintest transients with a field of view of at least 2arcmin. We propose to implement a physical modelling approach in order to link the instrument parameters and behaviour to physical quantities, thus providing a description of the instrument that can be connected with measurements. The method has been already successfully applied to the X-shooter instrument. The X-shooter physical model is based on a kernel optical ray-tracing realised by means of matrix optics representation, which can handle a large number of wavelengths. This can be extended to the SOXS design. The foreseen applications of the SOXS physical model are broad, ranging from support to detailed instrument design and development of the data reduction software, wavelength calibration, evaluation of instrument performance as a function of the model parameters, instrument alignment, and support during the commissioning phase and as a tool for quality check during operations.
Published: 2016
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27. Long Term Analysis for the BAM device

Author: D. Bonino and Daniele Gardiol
Subjects: Physics, Space and Planetary Science, Calibration (statistics), Pipeline (computing), Work (physics), General Engineering, Astronomy and Astrophysics, Variation (game tree), Data mining, computer.software_genre, Focus (optics), computer, Term (time)
Abstract: Algorithms aimed at the evaluation of critical quantities are based on models with many parameters, which values are estimated from data. The knowledge, with high accuracy, of these values and the control of their temporal evolution are important features. In this work, we focus on the latter subject, and we show a proposed pipeline for the BAM (Basic Angle Monitoring) Long Term Analysis, aimed at the study of the calibration parameters of the BAM device and of the Basic Angle variation, searching for unwanted trends, cyclic features, or other potential unexpected behaviours.
Published: 2010
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28. The new SOXS instrument for the ESO NTT

Author: V. De Caprio, Sergio Campana, Francesco D'Alessio, Matteo Munari, Sergio D'Orsi, Avishay Gal-Yam, Brian P. Schmidt, Enrico Cappellaro, Rosario Cosentino, Fabrizio Vitali, R. Franzen, Stephen J. Smartt, Stefano Basso, Salvatore Scuderi, A. de Ugarte Postigo, J. P. U. Fynbo, Andrea Baruffolo, S. Basa, Mario Hamuy, Enrico Giro, M. Della Valle, S. Savarese, Marco Riva, Giuliano Pignata, M. Iuzzolino, Davide Loreggia, Enrico Cascone, Riccardo Claudi, P. Schipani, Seppo Mattila, and Daniele Gardiol
Subjects: Physics, business.industry, Near-infrared spectroscopy, FOS: Physical sciences, 01 natural sciences, law.invention, 010309 optics, Telescope, SOXS, Optics, law, 0103 physical sciences, Visible band, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: SOXS (Son Of X-Shooter) will be a unique spectroscopic facility for the ESO-NTT 3.5-m telescope in La Silla (Chile), able to cover the optical/NIR band (350-1750 nm). The design foresees a high-efficiency spectrograph with a resolution-slit product of ~4,500, capable of simultaneously observing the complete spectral range 350 - 1750 nm with a good sensitivity, with light imaging capabilities in the visible band. This paper outlines the status of the project., Comment: 10 pages, submitted to SPIE Astronomical Telescopes & Instrumentation 2016, paper 9908-152
Published: 2016

29. The ASTRI mini-array software system (MASS) implementation: a proposal for the Cherenkov Telescope Array

Author: Federico Russo, Elisa Antolini, Alessandro Grillo, Andrea Di Paola, Valentina Fioretti, Nicola La Palombara, Federico Di Pierro, Vincenzo Testa, Maria Concetta Maccarone, Ciro Bigongiari, M. Capalbi, M. Trifoglio, Andrea Zoli, Gino Tosti, Enrico Cascone, Rodolfo Canestrari, Salvo Scuderi, Luca Stringhetti, Pietro Bruno, S. Vercellone, Giovanni Pareschi, P. Sangiorgi, Enrico Giro, Vito Conforti, Claudio Tanci, Osvaldo Catalano, Daniele Gardiol, J. Schwarz, Fulvio Gianotti, L. A. Antonelli, Stefano Gallozzi, Giuseppe Leto, Andrea Bulgarelli, Saverio Lombardi, and ITA
Subjects: Physics, business.industry, Data management, 02 engineering and technology, 021001 nanoscience & nanotechnology, Cherenkov Telescope Array, 01 natural sciences, law.invention, 010309 optics, Telescope, Set (abstract data type), Software, Data acquisition, law, Observatory, 0103 physical sciences, Software system, 0210 nano-technology, business, Computer hardware, Remote sensing
Abstract: The ASTRI mini-array, composed of nine small-size dual mirror (SST-2M) telescopes, has been proposed to be installed at the southern site of the Cherenkov Telescope Array (CTA), as a set of preproduction units of the CTA observatory. The ASTRI mini-array is a collaborative and international effort carried out by Italy, Brazil and South Africa and led by the Italian National Institute of Astrophysics, INAF. We present the main features of the current implementation of the Mini-Array Software System (MASS) now in use for the activities of the ASTRI SST-2M telescope prototype located at the INAF observing station on Mt. Etna, Italy and the characteristics that make it a prototype for the CTA control software system. CTA Data Management (CTADATA) and CTA Array Control and Data Acquisition (CTA-ACTL) requirements and guidelines as well as the ASTRI use cases were considered in the MASS design, most of its features are derived from the Atacama Large Millimeter/sub-millimeter Array Control software. The MASS will provide a set of tools to manage all onsite operations of the ASTRI mini-array in order to perform the observations specified in the short term schedule (including monitoring and controlling all the hardware components of each telescope and calibration device), to analyze the acquired data online and to store/retrieve all the data products to/from the onsite repository.
Published: 2016

30. Models for the active optics system of the ASTRI SST-2M prototype proposed for the Cherenkov Telescope Array

Author: Davide Loreggia, Enrico Giro, Federico Russo, G. Rodeghiero, Luigi Lessio, Daniele Gardiol, and ITA
Subjects: Physics, Initial Seed, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Active optics, Cherenkov Telescope Array, Astronomical instrumentation, law.invention, Primary mirror, Telescope, Optics, law, Secondary mirror, business, Cherenkov radiation, Astrophysics::Galaxy Astrophysics
Abstract: ASTRI SST-2M is an end-to-end prototype of Small Size class of Telescope proposed for the Cherenkov Telescope Array (CTA). Currently under completion at the Serra La Nave observing station (Mt. Etna, Catania, Italy), the ASTRI SST- 2M telescope is the first imaging dual-mirror telescope ever realized for Cherenkov telescopes. A mini-array of nine such telescopes will form the ASTRI mini-array proposed as a precursor and initial seed of CTA to be installed at the final CTA southern site. ASTRI SST-2M is equipped with an active optics system, controlling both the segmented primary mirror and the monolithic secondary mirror, which allows optical re-alignment during telescope slew. We describe the hardware and software solution that have been implemented for optics control and the models we developed for the system.
Published: 2016

31. Active optics system of the ASTRI SST-2M prototype for the Cherenkov Telescope Array

Author: Daniela Fantinel, Luigi Lessio, Federico Russo, Gerardo Capobianco, G. Rodeghiero, Enrico Giro, Antonio Volpicelli, Davide Loreggia, and Daniele Gardiol
Subjects: Physics, Reflecting telescope, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Active optics, Cherenkov Telescope Array, law.invention, Telescope, Primary mirror, Tilt (optics), Optics, law, Astrophysics::Earth and Planetary Astrophysics, Secondary mirror, business, Cherenkov radiation
Abstract: ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) SST-2M is an end-to-end prototype of Small Size class of Telescope for the Cherenkov Telescope Array. It will apply a dual mirror configuration to Imaging Atmospheric Cherenkov Telescopes. The 18 segments composing the primary mirror (diameter 4.3 m) are equipped with an active optics system enabling optical re-alignment during telescope slew. The secondary mirror (diameter 1.8 m) can be moved along three degrees of freedom to perform focus and tilt correc tions. We describe the kinematic model used to predict the system performance as well as the hardware and software de sign solution that will be implemented for optics control. Keywords: Imaging Atmospheric Cherenkov Telescope, CTA, ASTRI, gamma-rays, active optics 1. INTRODUCTION The dual-mirror ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Small Size Telescope prototype, named ASTRI SST-2M, is a wide field of view Schwarzschild-Couder Cherenkov telescope developed within the Cherenkov Telescope Array (CTA) framework
Published: 2014
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32. Tests characterization and alignment for the optics of the ASTRI SST-2M telescope prototype for the Cherenkov Telescope Array

Author: G. Rodeghiero, Nicola La Palombara, Enrico Giro, Rodolfo Canestrari, L. M. Perri, Gerardo Capobianco, Giovanni Pareschi, Giacomo Bonnoli, Daniela Fantinel, M. Fiorini, Daniele Gardiol, Antonio Volpicelli, Luigi Lessio, Paolo Conconi, Danilo Selvestrel, Luca Stringhetti, Gino Tosti, Giorgio Toso, and Giorgia Sironi
Subjects: Optical alignment, Astrophysics::High Energy Astrophysical Phenomena, Context (language use), law.invention, Telescope, Optics, Lightweight mirrors, law, Electronic, Wide field aplanatic telescope, ASTRI, Dual mirror telescopes, Optical and Magnetic Materials, Electrical and Electronic Engineering, Cherenkov radiation, Physics, CTA, Gamma-rays, Imaging Atmospheric Cherenkov Telescope, Applied Mathematics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Cherenkov Telescope Array, Characterization (materials science), business
Abstract: ASTRI SST-2M is a prototype dual mirror Small Size class of Telescope for the Cherenkov Telescope Array (CTA). Its innovative design based on a Schwarzschild-Couder configuration will permit use Silicon Photo-multipliers as focalplane detectors. The dual mirror configuration is a challenge for the realization of both the primary and secondary. Accurate tests and characterization are mandatory to understand the behavior of the optical configuration, its limits and the possibility of improvements of the full CTA array. Moreover, optical alignment requires solutions and procedures that have not been used so far on Cherenkov telescopes. The aim of paper is to provide an analysis of these topics in the context of the ASTRI SST-2M telescope.
Published: 2014
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33. The Italian contribution to the Gaia data processing and archiving

Author: Vilma Icardi, R. Messineo, Maria Sarasso, Roberto Morbidelli, Marco M. Castronuovo, Deborah Busonero, Armando Ciampolini, Angelo Fabio Mulone, Ronald Drimmel, Alberto Vecchiato, Mariateresa Crosta, Mario G. Lattanzi, Enrico Pigozzi, Daniele Gardiol, Filomena Solitro, and Michele Martino
Subjects: Physics, Data processing, Space and Planetary Science, Astronomy and Astrophysics, Astrometry, Data science, Remote sensing
Abstract: Gaia is an ESA Cornerstone mission, scheduled to be launched in spring 2013, dedicated to precisely measure the positions and motions of over a billion stars in our galaxy: the Milky Way. Gaia Data Processing Center Turin (DPCT), the Italian DPC, is hosted and operated at ALTEC in Turin. The primary objective of DPCT is to provide the infrastructure and operations support to the Astrometric Verification Unit (AVU) activities for CU3 and the Italian participation to the Gaia data processing tasks. DPCT will archive all of the data, produced for and delivered to DPAC as part of the Italian contribution to the activities of CU4, CU5, CU7, and CU8.
Published: 2010
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34. An active telescope secondary mirror control system

Author: Daniela Fantinel, Favio Bortoletto, Daniele Gardiol, Claudio Pernechele, and Carlotta Bonoli
Subjects: Hexapod, Computer science, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Coma (optics), Stewart platform, law.invention, Telescope, Optics, law, Control system, Secondary mirror, business, Focus (optics), Actuator, Instrumentation
Abstract: One of the main constraints for a modern astronomical telescope is the active control of the secondary mirror, mainly for the correction of the decentering coma and defocus induced by thermomechanical distortions. The mirror movements should be smooth, as precise as the optical design requires, and restricted to within predefined limits. It should be possible to perform mirror alignment and focus corrections without pausing the exposure (online control). The Galileo telescope achieves all this by using a support structure driven via six actuator bars (a hexapod system or Stewart platform) and a real-time control system based on a transputer network that allows parallel control of each actuator. Both the hexapod secondary support and the control system have been built and tested at the telescope. The results show that the errors introduced during mirror positioning lead to optical aberrations well below the diffraction figure of the telescope, and the systems work smoothly enough to allow online control.
Published: 1999
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35. Active optics system of the ASTRI SST-2M prototype for the Cherenkov Telescope ArrayAdvances in Optical and Mechanical Technologies for Telescopes and Instrumentation

Author: Ramón, Navarro, Cunningham, Colin R., Barto, Allison A., Daniele, Gardiol, Gerardo, Capobianco, Daniela, Fantinel, Enrico, Giro, Luigi, Lessio, Davide, Loreggia, Rodeghiero, Gabriele, Federico, Russo, and Volpicelli, Antonio C.
Published: 2014

36. Tests characterization and alignment for the optics of the ASTRI SST-2M telescope prototype for the Cherenkov Telescope ArrayAdvances in Optical and Mechanical Technologies for Telescopes and Instrumentation

Author: Ramón, Navarro, Cunningham, Colin R., Barto, Allison A., Enrico, Giro, Rodeghiero, Gabriele, Giacomo, Bonnoli, Rodolfo, Canestrari, Paolo, Conconi, Mauro, Fiorini, Daniela, Fantinel, Daniele, Gardiol, Luigi, Lessio, Nicola La Palombara, Giovanni, Pareschi, Luca, Perri, Danilo, Selvestrel, Giorgia, Sironi, Luca, Stringhetti, Giorgio, Toso, Gino, Tosti, Antonio, Volpicelli, and Gerardo, Capobianco
Published: 2014

37. Introducing the CTA concept

Author: A. Mathieu, R. G. Wagner, K. Panagiotidis, S Rosier Lees, Julien Rousselle, M. Gómez Berisso, Michela Uslenghi, Stephen Maxfield, R. C. Shellard, Ivica Puljak, T. Le Flour, Thomas Schanz, Tobias C. Walther, Juanan Aguilar, Pierre Colin, M. Chikawa, N. Fouque, Mosè Mariotti, G. Fontaine, Merja Tornikoski, V. Diez-Blanco, Enrico Giro, A. Krepps, G. Koss, J. M. Martin, Sergio Billotta, E. de Oña Wilhelmi, Keitaro Takahashi, S. Buson, P. Brook, S. Steiner, M. Dyrda, Joseph Silk, Sera Markoff, P. Lubinski, U. Schwanke, Sauvik Bhattacharyya, J. Ripken, T. Haubold, C. Zurbach, H. Wetteskind, R. Hermel, J. Darling, J. Nicolau-Kukliński, Konstancja Satalecka, M. Videla, Stefan Funk, P. Conconi, S. Bajtlik, Lukasz Stawarz, J. M. Paredes, K. Reitberger, Stefan Wagner, Teresa Mineo, David Kieda, G. Pareschi, Shigeto Kabuki, Makoto Sawada, Antonio Stamerra, Rodolfo Canestrari, N. Baby, G. Crimi, P. Kostka, J. Grube, R. Zanin, I. K. Kominis, L. Mc Comb, R. Sternberger, M. Fesquet, M. Tokarz, David Fink, Daniela Dorner, N. Hamer Heras, A. Moralejo Olaizola, M. de Naurois, Diego F. Torres, Claes Fransson, K. Nishijima, Yutaka Fujita, L. Fresnillo, B. García, R. Kossakowski, A. Masserot, H. von Gunten, Alkiviadis F. Bais, Ciro Bigongiari, A. Saggion, G. Papyan, I. Mrusek, K. Farakos, J. Michałowski, A. Franckowiak, Fernando Martinez, M. Doert, R. Wawrzaszek, Michele Doro, L. Sapozhnikov, Claudia Lavalley, D. Thuermann, A.A. Zdziarski, Cristina Knapic, Karen Byrum, N. Neyroud, Petr Schovanek, W. Domainko, D. Kastana, E. Birsin, Adrian Biland, F. Sánchez, Alexandre Marcowith, M. Errando, R. L. C. Starling, J. Schultze, A. Weinstein, B. B. Singh, Yassir Moudden, Jelena Aleksić, C. L. Naumann, V. Waegebaert, M. Shayduk, U. F. Katz, Gianpiero Tagliaferri, M. Schroedter, A. Vollhardt, O. Reimann, Hideyuki Ohoka, Vincenzo Testa, C. Jablonski, Tsuguya Naito, J. Schäfer, Stavros Maltezos, A. Wierzcholska, P. Wawer, L. Nellen, F. Mirabel, Tatsuo Yoshida, P. H. Carton, Nina Nowak, L. Platos, Riccardo Rando, P. P. Krueger, R. Wischnewski, W. Romaszkan, E. Fede, Martino Marisaldi, Markus Gaug, Richard Willingale, J. H. Buckley, U. De AlmeidaBarres, J. Knapp, Saverio Lombardi, D. della Volpe, A. Herrero, A. Bottani, E. Delagnes, Martin J. Hardcastle, C. Morello, Anna Lipniacka, T. Greenshaw, M. Renaud, Giancarlo Cusumano, Jonathan Biteau, M. Sowiński, J. R. T. de Mello Neto, T. B. Humensky, Michael G. Richer, G. Parks, G. Grasseau, H. Baba, Gino Tosti, Damir Lelas, H. Krawzcynski, David Paneque, M. Barcelo, R. Dickherber, P. Ferrando, Shinji Hara, D. Florin, Hideaki Katagiri, T. Shibata, Fuyuki Tokanai, N. A. McCubbin, J. Gomez-Ortega, D. Nakajima, A. Liolios, P. Laporte, Orjan Dale, A. Sillanpää, Dainis Dravins, Timothée Grégoire, Nu. Komin, A. Mihailidis, L. Sidoli, Shiu-Hang Lee, A. W. Chen, J. M. Illa, A. Kuznetsov, P. Munar-Adrover, D. Dominis Prester, Marcos Daniel Actis, Abraham D. Falcone, L. Journet, D. Hadasch, N. Galante, A. 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F., M., L., Fresnillo, C., Fruck, Y., Fujita, Y., Fukazawa, Y., Fukui, S., Funk, W., Gaebele, S., Gabici, R., Gabriele, A., Gadola, N., Galante, D., Gall, Y., Gallant, J., Gamez Garcia, B., Garcia, R. G., Lopez, D., Gardiol, D., Garrido, L., Garrido, D., Gascon, M., Gaug, J., Gaweda, L., Gebremedhin, N., Geffroy, L., Gerard, A., Ghedina, M., Ghigo, E., Giannakaki, F., Gianotti, S., Giarrusso, G., Giavitto, B., Giebel, V., Gika, P., Giommi, N., Girard, E., Giro, A., Giuliani, T., Glanzman, J. . ., F., N., Godinovic, V., Golev, M. G., Berisso, J., Gomez Ortega, M. M., Gonzalez, A., Gonzalez, F., Gonzalez, A. G., Munoz, K. S., Gothe, M., Gougerot, R., Graciani, P., Grandi, F., Granena, J., Granot, G., Grasseau, R., Gredig, A., Green, T., Greenshaw, T., Gregoire, O., Grimm, J., Grube, M., Grudzinska, V., Gruev, S., Gruenewald, J., Grygorczuk, V., Guarino, S., Gunji, G., Gyuk, D., Hadasch, R., Hagiwara, J., Hahn, N., Hakansson, A., Hallgren, N. H., Hera, S., Hara, M. 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B., Kieda, T., Kifune, T., Kihm, T., Kishimoto, K., Kitamoto, W., Kluzniak, C., Knapic, J. w., Knapp, J., Knoedlseder, F., Koeck, J., Kocot, K., Kodani, J. . ., H., K., Kohri, K., Kokkota, D., Kolitzu, N., Komin, I., Komini, Y., Konno, H., Koeppel, P., Korohoda, K., Kosack, G., Ko, R., Kossakowski, P., Kostka, R., Koul, G., Kowal, S., Koyama, J., Koziol, T., Kraehenbuehl, J., Krause, H., Krawzcynski, F., Krennrich, A., Krepp, A., Kretzschmann, R., Krobot, P., Krueger, H., Kubo, V. A., Kudryavtsev, J., Kushida, A., Kuznetsov, A. L., Barbera, N. L., Palombara, V. L., Parola, G. L., Rosa, K., Lacombe, G., Lamanna, J., Lande, D., Languignon, J., Lapington, P., Laporte, C., Lavalley, T. L., Flour, A. L., Padellec, S. . ., H., W. H., Lee, M. A., Leigui, D., Lela, D. J., Leopold, T., Lerch, L., Lessio, B., Lieunard, E., Lindfor, A., Liolio, A., Lipniacka, H., Lockart, T., Lohse, S., Lombardi, A., Lopatin, M., Lopez, R., Lopez Coto, A., Lopez Orama, A., Lorca, E., Lorenz, P., Lubinski, F., Lucarelli, H., Luedecke, J., Ludwin, P. L., Luque Escamilla, W., Lustermann, O., Luz, E., Lyard, M. C., Maccarone, T. J., Maccarone, G. M., Madejski, A., Madhavan, M., Mahabir, G., Maier, P., Majumdar, G., Malaguti, S., Maltezo, A., Manalaysay, A., Mancilla, D., Mandat, G., Maneva, A., Mangano, P., Manigot, K., Mannheim, I., Mantho, N., Marago, A., Marcowith, M., Mariotti, M., Marisaldi, S., Markoff, A., Marszalek, C., Marten, J., Marti, P., Martin, G., Martinez, F., Martinez, M., Martinez, A., Masserot, A., Mastichiadi, A., Mathieu, H., Matsumoto, F., Mattana, S., Mattiazzo, G., Maurin, S., Maxfield, J., Maya, D., Mazin, L. M., Comb, N., Mccubbin, I., Mchardy, R., Mckay, C., Medina, C., Melioli, D., Melkumyan, S., Mereghetti, P., Mertsch, M., Meucci, J., Michalowski, P., Micolon, A., Mihailidi, T., Mineo, M., Minuti, N., Mirabal, F., Mirabel, J. M., Miranda, R., Mirzoyan, T., Mizuno, B., Moal, R., Moderski, I., Mognet, E., Molinari, M., Molinaro, T., Montaruli, I., Monteiro, P., Moore, A. M., Olaizola, M., Mordalska, C., Morello, K., Mori, F., Mottez, Y., Moudden, E., Moulin, I., Mrusek, R., Mukherjee, P., Munar Adrover, H., Muraishi, K., Murase, A., Murphy, S., Nagataki, T., Naito, D., Nakajima, T., Nakamori, K., Nakayama, C., Naumann, D., Naumann, M., Naumann Godo, P., Nayman, D., Nedbal, D., Neise, L., Nellen, V., Neustroev, N., Neyroud, L., Nicastro, J., Nicolau Kuklinski, A., Niedzwiecki, J., Niemiec, D., Nieto, A., Nikolaidi, K., Nishijima, S., Nolan, R., Northrop, D., Nosek, N., Nowak, A., Nozato, P., O'Brien, Y., Ohira, M., Ohishi, S., Ohm, H., Ohoka, T., Okuda, A., Okumura, R. A., Ong, R., Orito, M., Orr, J., Osborne, M., Ostrowski, L. A., Otero, N., Otte, E., Ovcharov, I., Oya, A., Ozieblo, L., Padilla, S., Paiano, D., Paillot, A., Paizi, S., Palanque, M., Palatka, J., Pallota, K., Panagiotidi, D., Paneque, M., Panter, R., Paoletti, A., Papayanni, G., Papyan, J. M., Parede, G., Pareschi, G., Park, D., Parson, M. P., Arriba, M., Pech, G., Pedaletti, V., Pelassa, D., Pelat, M. D., C., M., Persic, P. . ., O., B., Peyaud, A., Pichel, S., Pita, F., Pizzolato, L., Plato, R., Platzer, L., Pogosyan, M., Pohl, G., Pojmanski, J. D., Ponz, W., Potter, J., Poutanen, E., Prandini, J., Prast, R., Preece, F., Profeti, H., Prokoph, M., Prouza, M., Proyetti, I., Puerto Gimenez, G., Puehlhofer, I., Puljak, M., Punch, R., Pyziol, E. J., Quel, J., Quinn, A., Quirrenbach, E., Racero, P. J., Rajda, P., Ramon, R., Rando, R. C., Rannot, M., Rataj, M., Raue, P., Reardon, O., Reimann, A., Reimer, O., Reimer, K., Reitberger, M., Renaud, S., Renner, B., Reville, W., Rhode, M., Ribo, M., Ribordy, M. G., Richer, J., Rico, J., Ridky, F., Rieger, P., Ringegni, J., Ripken, P. R., Ristori, A., Riviere, S., Rivoire, L., Rob, U., Roeser, R., Rohlf, G., Roja, P., Romano, W., Romaszkan, G. E., Romero, S., Rosen, S. R., Lee, D., Ro, G., Rouaix, J., Rousselle, S., Rousselle, A. C., Rovero, F., Roy, S., Royer, B., Rudak, C., Rulten, M., Rupinski, F., Russo, F., Ryde, B., Sacco, E. O., Saemann, A., Saggion, V., Safiakian, K., Saito, T., Saito, Y., Saito, N., Sakaki, R., Sakonaka, A., Salini, F., Sanchez, M., Sanchez Conde, A., Sandoval, H., Sandaker, E., Sant'Ambrogio, A., Santangelo, E. M., Santo, A., Sanuy, L., Sapozhnikov, S., Sarkar, N., Sartore, H., Sasaki, K., Satalecka, M., Sawada, V., Scalzotto, V., Scapin, M., Scarcioffolo, J., Schafer, T., Schanz, S., Schlenstedt, R., Schlickeiser, T., Schmidt, J., Schmoll, P., Schovanek, M., Schroedter, C., Schultz, J., Schultze, A., Schulz, K., Schure, T., Schwab, U., Schwanke, J., Schwarz, S., Schwarzburg, T., Schweizer, S., Schwemmer, A., Segreto, G. H., Sembroski, K., Seweryn, M., Sharma, M., Shayduk, R. C., Shellard, J., Shi, T., Shibata, A., Shibuya, E., Shum, L., Sidoli, M., Sidz, J., Sieiro, M., Sikora, J., Silk, A., Sillanpaa, B. B., Singh, J., Sitarek, C., Skole, R., Smareglia, A., Smith, D., Smith, J., Smith, N., Smith, D., Sobczynska, H., Sol, G., Sottile, M., Sowinski, F., Spanier, D., Spiga, S., Spyrou, V., Stamatescu, A., Stamerra, R., Starling, L., Stawarz, R., Steenkamp, C., Stegmann, S., Steiner, N., Stergioula, R., Sternberger, M., Sterzel, F., Stinzing, M., Stodulski, U., Straumann, E., Strazzeri, L., Stringhetti, A., Suarez, M., Suchenek, R., Sugawara, K. . ., H., S., Sun, A. D., Supanitsky, T., Suric, P., Sutcliffe, J., Syke, M., Szanecki, T., Szepieniec, A., Szostek, G., Tagliaferri, H., Tajima, H., Takahashi, K., Takahashi, L., Takalo, H., Takami, C., Talbot, J., Tammi, M., Tanaka, S., Tanaka, J., Tasan, M., Tavani, L. A., Tejedor, I., Telezhinsky, P., Temnikov, C., Tenzer, Y., Terada, R., Terrier, M., Teshima, V., Testa, D., Tezier, D., Thuermann, L., Tibaldo, O., Tibolla, A., Tiengo, M., Tluczykont, C. J., Todero, F., Tokanai, M., Tokarz, K., Toma, K., Torii, M., Tornikoski, D. F., Torre, M., Torre, G., Tosti, T., Totani, C., Toussenel, G., Tovmassian, P., Travnicek, M., Trifoglio, I., Troyano, K., Tsingano, H., Ueno, K., Umehara, S. S., Upadhya, T., Usher, M., Uslenghi, J. F., Valdes Galicia, P., Vallania, G., Vallejo, W. v., Driel, C. v., Eldik, J., Vandenbrouke, J., Vanderwalt, H., Vankov, G., Vasileiadi, V., Vassiliev, D., Veberic, I., Vega, S., Vercellone, S., Vergani, C., Veyssiere, J. P., Vialle, A., Viana, M., Videla, P., Vincent, S., Vincent, J., Vink, N., Vlahaki, L., Vlaho, P., Vogler, A., Vollhardt, H. . ., P., S., Vorobiov, C., Vuerli, V., Waegebaert, R., Wagner, R. G., Wagner, S., Wagner, S. P., Wakely, R., Walter, T., Walther, K., Warda, R., Warwick, P., Wawer, R., Wawrzaszek, N., Webb, P., Wegner, A., Weinstein, Q., Weitzel, R., Welsing, M., Werner, H., Wetteskind, R., White, A., Wierzcholska, S., Wiesand, M., Wilkinson, D. A., William, R., Willingale, K., Winiarski, R., Wischnewski, L., Wisniewski, M., Wood, A., Woernlein, Q., Xiong, K. K., Yadav, H., Yamamoto, T., Yamamoto, R., Yamazaki, S., Yanagita, J. M., Yebra, D., Yelo, A., Yoshida, T., Yoshida, T., Yoshikoshi, V., Zabalza, M., Zacharia, A., Zajczyk, R., Zanin, A., Zdziarski, A., Zech, A., Zhao, X., Zhou, K., Zietara, J., Ziolkowski, P., Ziolkowski, V., Zitelli, C., Zurbach, P., Zychowski, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CTA, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'Annecy de Physique des Particules (LAPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Next generation Cherenkov telescopes, Ciencias Físicas, 01 natural sciences, 7. Clean energy, TeV GAMMA-RAY ASTRONOMY, Observatory, Air showers, HESS, Cherenkov Telescopes, 010303 astronomy & astrophysics, MISSION, SUPERNOVA REMNANT W44, TELESCOPE, ASTRONOMY, EMISSION, Physics, ta213, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, TeV gamma-ray astronomy, ddc:540, CIENCIAS NATURALES Y EXACTAS, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Air shower, AIR SHOWERS, Astrophysics::High Energy Astrophysical Phenomena, 0103 physical sciences, Preparatory phase, ta115, TeV gamma-ray astronomy Air showers Cherenkov Telescopes, 010308 nuclear & particles physics, business.industry, CHERENKOV TELESCOPES, Física, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, ASTROFÍSICA, Cherenkov Telescope Array, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomía, Design study, Telecommunications, business
Abstract: The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project., La lista completa de autores puede consultarse en el documento o en la página web de la revista., Facultad de Ingeniería
Published: 2013
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38. TESTING GENERAL RELATIVITY BY ASTROMETRIC MEASUREMENTS CLOSE TO JUPITER, THE REAL GAREX- PART II

Author: Mario G. Lattanzi, Daniele Gardiol, Maria Teresa Crosta, and Roberto Morbidelli
Subjects: Physics, Jupiter, General relativity, Astrophysics
Published: 2008
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39. Fizeau interferometry from space: a challenging frontier in global astrometry

Author: Deborah Busonero, Mario G. Lattanzi, Mario Gai, Daniele Gardiol, and Davide Loreggia
Subjects: Physics, Fizeau interferometer, Interferometry, Optics, business.industry, Astronomical interferometer, Focal length, Context (language use), Field of view, Astrometry, business, Space exploration
Abstract: The design and performance of a Fizeau interferometer with long focal length and large field of view are discussed. The optical scheme presented is well suited for very accurate astrometric measurements from space, being optimised, in terms of geometry and aberrations, to observe astronomical targets down to the visual magnitude mV=20, with a measurement accuracy of 10 microarcseconds at mV=15. This study is in the context of the next generation astrometric space missions, in particular for a mission profile similar to that of the Gaia mission of the European Space Agency. Beyond the accuracy goal, the great effort in optical aberrations reduction, particularly distortion, aims at the optimal exploitation of data acquisition done with CCD arrays working in Time Delay Integration mode. The design solution we present reaches the astrometric goals with a field of view of 0.5 square degrees.
Published: 2004
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40. End-to-end optomechanical simulation for high-precision global astrometry

Author: Mario Gai, Daniele Gardiol, Luca Perachino, Davide Loreggia, Sergio Mannu, S. Mottini, and Mario G. Lattanzi
Subjects: Physics, Telescope, Sight, Software, Optics, End-to-end principle, business.industry, law, Software tool, Astrometry, business, law.invention
Abstract: We describe a software tool developed to simulate the behaviour of the angle between two lines of sight in a dual view telescope assembly (usually referred to as basic angle) due to optical misalignments induced by thermo-mechanical fluctuations. The tool applies to a variety of reflective optical designs. In principle, not only the basic angle behaviour can be simulated, but also other optical parameters. As a practical example, we present and discuss results obtained from application of our software to the case of the Gaia baseline optical design. We show that the final error can be severely degraded by fluctuations of the basic angle due to thermo-mechanical effects.
Published: 2004
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41. Design, deposition, and characterization of multilayer coatings for the ultraviolet and visible-light coronagraphic imager

Author: Valentino Rigato, Maria Guglielmina Pelizzo, Piergiorgio Nicolosi, Alessandro Patelli, and Daniele Gardiol
Subjects: Fabrication, Sounding rocket, Materials science, business.industry, Payload, Materials Science (miscellaneous), Optical instrument, medicine.disease_cause, Industrial and Manufacturing Engineering, law.invention, Orbiter, Optics, Optical coating, law, medicine, Business and International Management, business, Coronagraph, Ultraviolet
Abstract: The Ultraviolet and Visible-Light Coronagraphic Imager is the baseline coronagraph for the European Space Agency's payload Solar Orbiter, a solar mission whose launch in 2011 is expected. To prove the feasibility of its innovative design, a sounding rocket version of the same instrument has been approved by NASA. One of the main technological challenges of the instrument is the achievement of multilayer optical coatings with suitable properties. We describe the design, fabrication, and characterization of such coatings.
Published: 2004

42. CCD camera for ground- and space-based solar corona observations

Author: Silvano Fineschi, Emanuele Pace, Marco Romoli, Luca Gori, Alessandro Gherardi, Ester Antonucci, Daniele Gardiol, Mauro Focardi, and L. Zangrilli
Subjects: Physics, business.product_category, business.industry, Controller (computing), Detector, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Polarimetry, law.invention, Optics, Rocket, law, Broadband, Charge-coupled device, Space Science, business, Coronagraph, Remote sensing
Abstract: A new concept CCD camera is currently under development at the XUVLab of the Department of Astronomy and Space Science of the University of Florence. This CCD camera is the proposed detector for the space- and ground-based solar corona observations. This camera will be the detector for the polarimetric channels of the UVC coronagraph of the HERSCHEL rocket mission to observe the solar corona in an optical broadband. The ground-based application consists in a UVC prototype for coronagraphic measurements from Earth in the visible range. Within this project, a CCD camera with innovative features has been produced: the camera controller allows the fine tuning of all the parameters related to charge transfer and CCD readout, i.e., the use of virtually any CCD sensor, and it implements the new concept of high level of versatility, easy management, TCP/IP remote control and display.
Published: 2004
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43. SPECTRE: a spectro-heliograph for the transition region

Author: Marco Malvezzi, D. Moses, Daniele Gardiol, Silvano Fineschi, P. Nicolosi, Ester Antonucci, Giampiero Naletto, Marco Romoli, Russell A. Howard, L. Zangrilli, V. Da Deppo, and Davide Loreggia
Subjects: Physics, Solar dynamics observatory, Solar transition region, Astronomy, Solar atmosphere, Heliograph
Abstract: The SPECtro-heliograph for the Transition REgion (SPECTRE) experiment is one of the instruments of the Solar Heliospheric Activity Research and Prediction Program (SHARPP) suite initially foreseen aboard the NASA mission Solar Dynamics Observatory (SDO) of the International Living With a Star (ILWS) program. The scientific objective of the SPECTRE experiment was to characterize the rapid evolution of plasma in the transition region of the solar atmosphere, producing full-disk 1.2 arcsec-resolution images of the solar atmosphere at the very critical 63 nm OV spectral line, characterizing a solar plasma temperature of about 250,000 K. Unfortunately, NASA very recently and unexpectedly, during the instrument Phase A study, decided not to proceed with the realization of SHARPP. The authors of this paper think that all the work done so far in the definition of SPECTRE should not be lost. So, they have decided to summarize in this paper the main characteristics of this instrument and the results of the analysis so far performed: the hope is that in a next future this work can be used again for realizing an instrument having similar characteristics.
Published: 2004

44. Ultraviolet and Visible-light Coronagraphic Imager (UVCI)

Author: Vania Da Deppo, Marco Romoli, Daniele Gardiol, Giancarlo Noci, Silvano Fineschi, Silvio Giordano, Giampiero Naletto, Marco Malvezzi, L. Zangrilli, and Ester Antonucci
Subjects: Physics, business.industry, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Coronal loop, Corona, law.invention, Solar wind, Optics, law, Extreme ultraviolet, Physics::Space Physics, Extreme ultraviolet Imaging Telescope, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph, Astrophysics::Galaxy Astrophysics, Heliosphere
Abstract: The HERSCHEL (HElium Resonance Scattering in the Corona and HELiosphere) Sun-Earth Sub-Orbital Program is a proposed sounding-rocket payload designed to investigate helium coronal abundance and solar wind acceleration from a range of solar source structures by obtaining simultaneous observations of the electron, proton and helium solar coronae. HERSCHEL will provide the first measurements of the coronal helium abundance in source regions of the solar wind, thus bringing key elements to our understanding of the Sun-Earth connections. The HERSCHEL instrument package consists of the Extreme Ultraviolet Imaging Telescope (EIT) for on-disk coronal observations and the Ultraviolet and Visible-light Coronagraphic Imager (UVCI) for off-limb observations of the corona. The UVCI is an externally occulted, reflecting coronagraph with an off-axis Gregorian telescope. UVCI will be able to take coronal images at heliocentric heights comprised between 1.2 to 3.5 solar radii of a) K-corona polarized brightness (pB); b) H I Lyman-α, 121.6 nm, line-emission; c) He II Lyman-α, 30.4 nm, line. The key element in the UVCI instrument concept is that the mirrors with multilayer coatings optimized for 30.4 nm still have good reflectivity at 121.6 nm and in the visible. The optical design concept for the UVCI instrument will be discussed, together with its expected optical and throughput performances.
Published: 2003
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45. The Ultraviolet and Visible-light Coronagraph of the HERSCHEL experiment

Author: L. Zangrilli, Giampiero Naletto, A. Gherardi, Jean-Pierre Delaboudiniere, Ester Antonucci, Jeffrey S. Newmark, Silvano Fineschi, Federico Landini, R. A. Howard, M. G. Pelizzo, Marco Romoli, F. Auchere, Piergiorgio Nicolosi, Daniele Gardiol, John D. Moses, V. Da Deppo, Luca Gori, Marco Malvezzi, and Emanuele Pace
Subjects: Physics, business.industry, Stray light, Astronomy, Coronal loop, solar system, Corona, Helium, straylight, law.invention, Solar cycle, Solar wind, Optics, law, Extreme ultraviolet Imaging Telescope, Coronal mass ejection, Solar radiation, business, Coronagraph
Abstract: The Herschel (HElium Resonant Scattering in the Corona and HELiosphere) experiment, to be flown on a sounding rocket, will investigate the helium coronal abundance and the solar wind acceleration from a range of solar source structures by obtaining the first simultaneous observations of the electron, proton and helium solar corona. The HERSCHEL payload consists of the EUV Imaging Telescope (EIT), that resembles the SOHO/EIT instrument, and the Ultraviolet and Visible Coronagraph (UVC).UVC is an imaging coronagraph that will image the solar corona from 1.4 to 4 solar radii in the EUV lines of HI 121.6 nm and the HeII 30.4 nm and in the visible broadband polarized brightness. The UVC coronagraph is externally occulted with a novel design as far as the stray light rejection is concerned. Therefore, HERSCHEL will also establish proof‐of‐principle for the Ultraviolet Coronagraph, which is in the ESA Solar Orbiter Mission baseline.The scientific objectives of the experiment will be discussed, togetherwith a description of the UVC coronagraph.
Published: 2003

46. Development of multilayer coatings for solar space experiments

Author: Elsa Bontempi, Daniele Gardiol, Piergiorgio Nicolosi, G. Salmaso, Alessandro Patelli, Valentino Rigato, and Maria Guglielmina Pelizzo
Subjects: Materials science, Sounding rocket, business.industry, Payload, multilayer, solar corona, Reflectivity, Characterization (materials science), On board, Optics, Optical coating, Deposition (phase transition), Development (differential geometry), business
Abstract: Deposition and characterization results of multilayer coatings optimized for HeII 30.4 nm high reflectivity will be presented. Additional characterization of reflectivity at HI Ly-α and in the visible spectral range has been also accomplished in order to investigate the performances of such coatings in view of their application to the UVCI instrument on board of ESA payload SOLO and to HERSCHEL, a sounding rocket experiment.
Published: 2003

47. FINITO: A Fringe Sensor for VLTI in Two and Three Beam Configuration

Author: Daniele Gardiol, Giuseppe Massone, Davide Loreggia, Leonardo Corcione, Mario G. Lattanzi, Alberto Gennai, Serge Menardi, D. Bonino, and Mario Gai
Subjects: Physics, Time delay and integration, Very Large Telescope, business.industry, law.invention, Telescope, Interferometry, Optics, Observatory, law, Closure phase, Astronomical interferometer, business, Optical path length, Remote sensing
Abstract: ESO and the Astronomical Observatory of Torino (OATo) are collaborating for development of a Fringe Sensor Unit (FSU) for the Very Large Telescope Interferometer (VLTI, see [1] and references therein): FINITO (Fringe-tracking Instrument of Nice and Torino), derived from the concept demonstrated by a prototype from the Observatoire de la Cote d’Azur. It will be used for stabilisation of the Optical Path Difference (OPD) between telescope beams for the first generation scientific interferometers (AMBER, MIDI, VINCI), providing an improvement of up to five magnitudes in limiting sensitivity, thanks to the integration time increased from a few ten milliseconds up to minutes. Accordingly to current planning, FINITO is the only FSU able to support three-beam observations, allowing closure phase measurements in the near and mid IR range.
Published: 2002
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48. Stray light evaluation of the Ultraviolet and Visible-light Coronagraph Imager (UVCI) rocket prototype

Author: Giampiero Naletto, Daniele Gardiol, Marco Malvezzi, Giuseppe Tondello, Ester Antonucci, Silvano Fineschi, Federico Landini, Marco Romoli, and Giancarlo Noci
Subjects: Physics, Brightness, business.industry, Aperture, Stray light, Optical engineering, Astrophysics::Instrumentation and Methods for Astrophysics, medicine.disease_cause, law.invention, Optics, law, Extreme ultraviolet, Physics::Space Physics, medicine, Astrophysics::Solar and Stellar Astrophysics, Optoelectronics, Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph, Ultraviolet, Visible spectrum
Abstract: The Ultraviolet and Visible-light Coronagraph Imager (UVCI) proposed for the European Space Agency (ESA) Solar Orbiter mission, is designed to image the visible and the ultraviolet coronal emissions, in order to diagnose the solar corona. The UVCI is an externally occulted reflection coronagraph that obtains monochromatic images in the neutral hydrogen HI 121.6 nm and in the single ionized helium HeII 30.4 nm lines, and measures the polarized brightness (pB) of the K-corona in broadband visible light. One of the most stringent requirements in the design of a coronagraph is the stray light rejection. The stray light is produced by solar disk radiation which is several order of magnitude brighter than the coronal radiation in both visible and UV. The solar disk radiation enters the instrument through the external aperture and stray light is produced by diffraction off the edges of the apertures and of the optical components, non-specular reflections off the mirror surfaces, and scattering off the mechanical structure. In this paper, the features in the optical design that contribute to the stray light reduction are described, and an analysis of all possible stray light contributions is performed on the optical configuration of the UVCI sounding rocket prototype (UVC-SR). From this analysis, a stray light model has been developed and its results are compared with the minimum measurable signal expected from the solar corona.© (2001) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Published: 2001
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49. Ultraviolet and visible-light coronagraph for the Solar Orbiter mission

Author: Giampiero Naletto, Giuseppe Tondello, Daniele Gardiol, Marco Zattarin, Stefano Cesare, Marco Romoli, Silvano Fineschi, Giancarlo Noci, Ester Antonucci, and A. M. Malvezzi
Subjects: Physics, Brightness, business.industry, Astronomical unit, medicine.disease_cause, law.invention, Orbiter, Optics, Optical coating, law, Extreme ultraviolet, Physics::Space Physics, medicine, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph, Ultraviolet, Visible spectrum
Abstract: The Ultraviolet and Visible-light Coronagraph (UVC) is one of the solar remote-sensing instruments proposed for the model payload of the Solar Orbiter mission. The Solar Orbiter is one of the two 'Flexible' missions selected in September 2000 by the European Space Agency (ESA) for the definition study phase. A novel orbital design takes the orbiter as close as 0.21 astronomical units (AU) to the Sun, with heliographic latitudes as high as 38 degrees for observations of the solar polar regions at very high spatial resolution. From this vantage point, the UVC can, at the same time, image the visible and ultraviolet coronal emissions and diagnose, with unprecedented temporal and spatial resolution (down to 1200 km) the full solar corona. The UVC's optical design, presented here, consists of an externally occulted, off-axis Gregorian with multilayer-coated optics. The UVC can obtain monochromatic images in the neutral hydrogen HI Lyman (alpha) , (lambda) 121.6 nm, and single-ionized helium HEII Lyman (alpha) , (lambda) 30.4 nm, lines and measure the polarized brightness (pB) of the visible K-corona. The ultraviolet Lyman (alpha) lines are separated with two multilayer coatings mirror and an extreme-ultraviolet transmission filter. The mirrors' coating optimized for 30.4 nm still has a good reflectivity at 121.6 nm and visible. The optical performances, resulting from ray-tracing calculations, are presented here, along with the expected system response to the coronal signal.© (2000) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Published: 2000
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50. Preliminary design of a NIR prime focus corrector for the Galileo Telescope

Author: Fabio Bortoletto, Paolo Conconi, Claudio Pernechele, Filippo Maria Zerbi, E. Molinari, and Daniele Gardiol
Subjects: Physics, Pixel, business.industry, Astrophysics (astro-ph), Detector, FOS: Physical sciences, Astrophysics, law.invention, Primary mirror, Telescope, Lens (optics), Cardinal point, Optics, law, Galileo (vibration training), business, Focus (optics)
Abstract: In this paper a preliminary design for a prime focus corrector to be mounted at the Telescopio Nazionale Galileo (TNG) is presented. The telescope is located on La Palma (Canary Islands) and has a primary mirror of 3.5 m with a hyperbolic sag. Two optical designs have been considered in order to exploit detectors with 1k x 1k and 2k x 2k pixels. Each design makes use of four lenses, two of which are aspherical. The first lens diameters are, respectively, of 140 mm and 320 mm for the two kind of detectors. For both designs the telescope pupil is deliberately not re-imaged, and therefore it will not be possible to insert a cold stop. For such a reason particular care has been dedicated to the telescope thermal background study, in order to optimise the baffling system. The optics is able to correct fields of 11' x 11' and of 60'x60', depending on the design. It should be considered that the particular geometry of the focal plane array mosaic does not permit a full exploitation of the entire field, being based on a combination of four detectors. The selected chips are HgCdTe manufactured by Rockwell, i.e. Hawaii I in the 1k x 1k case and Hawaii II in the 2k x 2k case., 7 pages, SPIE proceedings
Published: 2000
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