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1. The Discovery and Evolution of a Possible New Epoch of Cometary Activity by the Centaur (2060) Chiron

Author

Dobson, Matthew M., Schwamb, Megan E., Fitzsimmons, Alan, Schambeau, Charles, Beck, Aren, Denneau, Larry, Erasmus, Nicolas, Heinze, A. N., Shingles, Luke J., Siverd, Robert J., Smith, Ken W., Tonry, John L., Weiland, Henry, Young, David. R., Kelley, Michael S. P., Lister, Tim, Bernardinelli, Pedro H., Ferrais, Marin, Jehin, Emmanuel, Fedorets, Grigori, Benecchi, Susan D., Verbiscer, Anne J., Murtagh, Joseph, Duffard, Rene, Gomez, Edward, Chatelain, Joey, and Greenstreet, Sarah

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Centaurs are small Solar System objects on chaotic orbits in the giant planet region, forming an evolutionary continuum with the Kuiper belt objects and Jupiter-family comets. Some Centaurs are known to exhibit cometary activity, though unlike comets this activity tends not to correlate with heliocentric distance and the mechanism behind it is currently poorly understood. We utilize serendipitous observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS), Zwicky Transient Facility (ZTF), Panoramic Survey Telescope and Rapid Response System (Pan-STARRS), Dark Energy Survey (DES), and Gaia in addition to targeted follow-up observations from the Las Cumbres Observatory, TRAnsiting Planets and PlanetesImals Small Telescope South (TRAPPIST-South), and Gemini North telescope to analyze an unexpected brightening exhibited by the known active Centaur (2060) Chiron in 2021. This is highly indicative of a cometary outburst. As of 2023 February, Chiron has still not returned to its pre-brightening magnitude. We find Chiron's rotational lightcurve, phase curve effects, and possible high-albedo surface features to be unlikely causes of this observed brightening. We consider the most likely cause to be an epoch of either new or increased cometary activity, though we cannot rule out a possible contribution from Chiron's reported ring system, such as a collision of as-yet unseen satellites shepherding the rings. We find no evidence for coma in our Gemini or TRAPPIST-South observations, though this does not preclude the possibility that Chiron is exhibiting a coma that is too faint for observation or constrained to the immediate vicinity of the nucleus., Comment: 39 pages, 14 figures, 14 tables. Has been accepted for publication in PSJ

Published
2024
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2. Aperture photometry on asteroid trails: detection of the fastest rotating near-Earth object

Author

Devogèle, Maxime, Buzzi, Luca, Micheli, Marco, Cano, Juan Luis, Conversi, Luca, Jehin, Emmanuel, Ferrais, Marin, Ocaña, Francisco, Föhring, Dora, Drury, Charlie, Benkhaldoun, Zouhair, and Jenniskens, Peter

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Near-Earth objects (NEOs) on an impact course with Earth can move at high angular speed. Understanding their properties, including rotation state, is crucial for assessing impact risks and mitigation strategies. Traditional photometric methods face challenges in collecting data on fast-moving NEOs accurately. Aims. This study introduces an innovative approach to aperture photometry tailored to analyzing trailed images of fast-moving NEOs. Our primary aim is to extract rotation state information from these observations, particularly focusing on the efficacy of this technique for fast rotators. Methods. We applied our approach to analyze the trailed images of three asteroids: 2023 CX1, 2024 BX1, and 2024 EF, which were either on a collision courses or performing a close fly-by with Earth. By adjusting aperture sizes, we controlled the effective exposure times to increase the sampling rates of the photometric variations. This enabled us to detect short rotation periods that would be challenging with conventional methods. Results. Our analysis revealed that trailed photometry significantly reduces overhead time associated with CCD read-out, enhancing the sampling rate of the photometric variations. We demonstrated that this technique is particularly effective for fast-moving objects, providing reliable photometric data when the object is at its brightest and closest to Earth. For asteroid 2024 BX1, we detected a rotation period as short as 2.5888 +- 0.0002 seconds, the fastest ever recorded. Our findings underscore the efficacy of trailed observations coupled with aperture photometry for studying the rotation characteristics of small NEOs, offering crucial insights for impact risk assessment and mitigation strategies., Comment: 8 pages, 9 figures

Published
2024
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3. Photometry of the Didymos system across the DART impact apparition

Author

Moskovitz, Nicholas, Thomas, Cristina, Pravec, Petr, Lister, Tim, Polakis, Tom, Osip, David, Kareta, Theodore, Rożek, Agata, Chesley, Steven R., Naidu, Shantanu P., Scheirich, Peter, Ryan, William, Ryan, Eileen, Skiff, Brian, Snodgrass, Colin, Knight, Matthew M., Rivkin, Andrew S., Chabot, Nancy L., Ayvazian, Vova, Belskaya, Irina, Benkhaldoun, Zouhair, Berteşteanu, Daniel N., Bonavita, Mariangela, Bressi, Terrence H., Brucker, Melissa J., Burgdorf, Martin J., Burkhonov, Otabek, Burt, Brian, Contreras, Carlos, Chatelain, Joseph, Choi, Young-Jun, Daily, Matthew, de León, Julia, Ergashev, Kamoliddin, Farnham, Tony, Fatka, Petr, Ferrais, Marin, Geier, Stefan, Gomez, Edward, Greenstreet, Sarah, Gröller, Hannes, Hergenrother, Carl, Holt, Carrie, Hornoch, Kamil, Husárik, Marek, Inasaridze, Raguli, Jehin, Emmanuel, Khalouei, Elahe, Eluo, Jean-Baptiste Kikwaya, Kim, Myung-Jin, Krugly, Yurij, Kučáková, Hana, Kušnirák, Peter, Larsen, Jeffrey A., Lee, Hee-Jae, Lejoly, Cassandra, Licandro, Javier, Longa-Peña, Penélope, Mastaler, Ronald A., McCully, Curtis, Moon, Hong-Kyu, Morrell, Nidia, Nath, Arushi, Oszkiewicz, Dagmara, Parrott, Daniel, Phillips, Liz, Popescu, Marcel M., Pray, Donald, Prodan, George Pantelimon, Rabus, Markus, Read, Michael T., Reva, Inna, Roark, Vernon, Santana-Ros, Toni, Scotti, James V., Tatara, Taiyo, Thirouin, Audrey, Tholen, David, Troianskyi, Volodymyr, Tubbiolo, Andrew F., and Villa, Katelyn

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

On 26 September 2022, the Double Asteroid Redirection Test (DART) spacecraft impacted Dimorphos, the satellite of binary near-Earth asteroid (65803) Didymos. This demonstrated the efficacy of a kinetic impactor for planetary defense by changing the orbital period of Dimorphos by 33 minutes (Thomas et al. 2023). Measuring the period change relied heavily on a coordinated campaign of lightcurve photometry designed to detect mutual events (occultations and eclipses) as a direct probe of the satellite's orbital period. A total of 28 telescopes contributed 224 individual lightcurves during the impact apparition from July 2022 to February 2023. We focus here on decomposable lightcurves, i.e. those from which mutual events could be extracted. We describe our process of lightcurve decomposition and use that to release the full data set for future analysis. We leverage these data to place constraints on the post-impact evolution of ejecta. The measured depths of mutual events relative to models showed that the ejecta became optically thin within the first ~1 day after impact, and then faded with a decay time of about 25 days. The bulk magnitude of the system showed that ejecta no longer contributed measurable brightness enhancement after about 20 days post-impact. This bulk photometric behavior was not well represented by an HG photometric model. An HG1G2 model did fit the data well across a wide range of phase angles. Lastly, we note the presence of an ejecta tail through at least March 2023. Its persistence implied ongoing escape of ejecta from the system many months after DART impact., Comment: 52 pages, 5 tables, 9 figures, accepted to PSJ

Published
2023

4. Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN$_{35}$ Across a Wide Range of Phase Angles: Possible Mission Accessible A-type Asteroid

Author

Beniyama, Jin, Ohsawa, Ryou, Avdellidou, Chrysa, Sako, Shigeyuki, Takita, Satoshi, Ishiguro, Masateru, Sekiguchi, Tomohiko, Usui, Fumihiko, Kinoshita, Shinichi W., Lee, Kianhong, Takumi, Asami, Ferrais, Marin, and Jehin, Emmanuël

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Studying small near-Earth asteroids is important to understand their dynamical histories and origins as well as to mitigate the damage of the asteroid impact to the Earth. We report the results of multicolor photometry of the tiny near-Earth asteroid 2015 RN$_{35}$ using the 3.8 m Seimei telescope in Japan and the TRAPPIST-South telescope in Chile over 17 nights in 2022 December and 2023 January. We observed 2015 RN$_{35}$ across a wide range of phase angles from 2$^{\circ}$ to 30$^{\circ}$ in the $g$, $r$, $i$, and $z$ bands in the Pan-STARRS system. These lightcurves show that 2015 RN$_{35}$ is in a non-principal axis spin state with two characteristic periods of $1149.7\pm0.3$ s and $896.01\pm0.01$ s. We found that a slope of a visible spectrum of 2015 RN$_{35}$ is as red as asteroid (269) Justitia, one of the very red objects in the main belt, which indicates that 2015 RN$_{35}$ can be classified as an A- or Z-type asteroid. In conjunction with the shallow slope of the phase curve, we suppose that 2015 RN$_{35}$ is a high-albedo A-type asteroid. We demonstrated that surface properties of tiny asteroids could be well constrained by intensive observations across a wide range of phase angles. 2015 RN$_{35}$ is a possible mission accessible A-type near-Earth asteroid with a small $\Delta v$ of 11.801 km s$^{-1}$ in the launch window between 2030 and 2035., Comment: Accepted for publication in the Astronomical Journal. Any comments are welcome

Published
2023

5. Implications for the Formation of 2005 UD from a New Convex Shape Model

Author

Kueny, Jay K., Chandler, Colin Orion, Devogèle, Maxime, Moskovitz, Nicholas, Pravec, Petr, Kučáková, Hana, Hornoch, Kamil, Kušnirák, Peter, Granvik, Mikael, Konstantopoulou, Christina, Jannsen, Nicholas E., Moran, Shane, Siltala, Lauri, Fedorets, Grigori, Ferrais, Marin, Jehin, Emmanuel, Kareta, Theodore, and Hanuš, Josef

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

(155140) 2005 UD has a similar orbit to (3200) Phaethon, an active asteroid in a highly eccentric orbit thought to be the source of the Geminid meteor shower. Evidence points to a genetic relationship between these two objects, but we have yet to fully understand how 2005 UD and Phaethon could have separated into this associated pair. Presented herein are new observations of 2005 UD from five observatories that were carried out during the 2018, 2019, and 2021 apparitions. We implemented light curve inversion using our new data, as well as dense and sparse archival data from epochs in 2005--2021 to better constrain the rotational period and derive a convex shape model of 2005 UD. We discuss two equally well-fitting pole solutions ($\lambda = 116.6^{\circ}$, $\beta = -53.6^{\circ}$) and ($\lambda = 300.3^{\circ}$, $\beta = -55.4^{\circ}$), the former largely in agreement with previous thermophysical analyses and the latter interesting due to its proximity to Phaethon's pole orientation. We also present a refined sidereal period of $P_{\text{sid}} = 5.234246 \pm 0.000097$ hr. A search for surface color heterogeneity showed no significant rotational variation. An activity search using the deepest stacked image available of 2005 UD near aphelion did not reveal a coma or tail but allowed modeling of an upper limit of 0.04 to 0.37~kg s$^{-1}$ for dust production. We then leveraged our spin solutions to help limit the range of formation scenarios and the link to Phaethon in the context of nongravitational forces and timescales associated with the physical evolution of the system., Comment: 22 pages, 7 figure, 7 tables

Published
2023

6. Spectral evolution of dark asteroid surfaces induced by space weathering over a decade

Author

Hasegawa, Sunao, DeMeo, Francesca E., Marsset, Michael, Hanus, Josef, Avdellidou, Chrysa, Delbo, Marco, Bus, Schelte J., Hanayama, Hidekazu, Horiuchi, Takashi, Takir, Driss, Jehin, Emmanuel, Ferrais, Marin, Geem, Jooyeon, Im, Myungshin, Seo, Jinguk, Bach, Yoonsoo P., Jin, Sunho, Ishiguro, Masateru, Kuroda, Daisuke, Binzel, Richard P., Nakamura, Akiko M., Yang, Bin, and Vernazza, Pierre

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The surface of airless bodies like asteroids in the Solar System are known to be affected by space weathering. Experiments simulating space weathering are essential for studying the effects of this process on meteorite samples, but the problem is that the time spent to reproduce space weathering in these experiments is billions of times shorter than the actual phenomenon. In December 2010, the T-type asteroid 596 Scheila underwent a collision with a few-tens-of-meters impactor. A decade later, there is an opportunity to study how the surface layer of this asteroid is being altered by space weathering after the impact. To do so, we performed visible spectrophotometric and near-infrared spectroscopic observations of 596 Scheila. The acquired spectrum is consistent with those observed shortly after the 2010 impact event within the observational uncertainty range. This indicates that the surface color of dark asteroids is not noticeably changed by space weathering over a 10-year period. This study is the first to investigate color changes due to space weathering on an actual asteroid surface in the Solar System. Considering that fresh layers are regularly created on asteroid surfaces by collisions, we suggest a genetic link between D/T-type and dark (low albedo) X-complex asteroids and very red objects such as 269 Justitia, 732 Tjilaki (and 203 Pompeja). New observations show that 203 Pompeja has a X-type-like surface, with some local surface areas exhibiting a very red spectrum., Comment: 16 pages, 9 figures, 2 tables, Accepted for publication in ApJ Letters

Published
2022

7. (6478) Gault: Physical characterization of an active main-belt asteroid

Author

Devogèle, Maxime, Ferrais, Marin, Jehin, Emmanuel, Moskovitz, Nicholas, Skiff, Brian A., Levine, Stephen E., Gustafsson, Annika, Farnocchia, Davide, Micheli, Marco, Snodgrass, Colin, Borisov, Galin, Manfroid, Jean, Moulane, Youssef, Benkhaldoun, Zouhair, Burdanov, Artem, Pozuelos, Francisco J., Gillon, Michael, de Wit, Julien, Green, Simon F., Bendjoya, Philippe, Rivet, Jean-Pierre, Abe, Luy, Vernet, David, Chandler, Colin Orion, and Trujillo, Chadwick A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In December 2018, the main-belt asteroid (6478)~Gault was reported to display activity. Gault is an asteroid belonging to the Phocaea dynamical family and was not previously known to be active, nor was any other member of the Phocaea family. In this work we present the results of photometric and spectroscopic observations that commenced soon after the discovery of activity. We obtained observations over two apparitions to monitor its activity, rotation period, composition, and possible non-gravitational orbital evolution. We find that Gault has a rotation period of $P = 2.4929 \pm 0.0003$ hours with a lightcurve amplitude of $0.06$ magnitude. This short rotation period close to the spin barrier limit is consistent with Gault having a density no smaller than $\rho = 1.85$~g/cm$^3$ and its activity being triggered by the YORP spin-up mechanism. Analysis of the Gault phase curve over phase angles ranging from $0.4^{\circ}$ to $23.6^{\circ}$ provides an absolute magnitude of $H = 14.81 \pm 0.04$, $G1=0.25 \pm 0.07$, and $G2= 0.38 \pm 0.04$. Model fits to the phase curve find the surface regolith grain size constrained between 100-500 $\rm{\mu}$m. Using relations between the phase curve and albedo we determine that the geometrical albedo of Gault is $p_{\rm v} = 0.26 \pm 0.05$ corresponding to an equivalent diameter of $D = 2.8^{+0.4}_{-0.2}$ km. Our spectroscopic observations are all consistent with an ordinary chondrite-like composition (S, or Q-type in the Bus-DeMeo taxonomic classification). A search through archival photographic plate surveys found previously unidentified detections of Gault dating back to 1957 and 1958. Only the latter had been digitized, which we measured to nearly double the observation arc of Gault. Finally, we did not find any signal of activity during the 2020 apparition or non-gravitational effects on its orbit., Comment: 15 pages, 11 figures; Accepted in MNRAS

Published
2021
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8. Photometry of the Didymos System across the DART Impact Apparition

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Moskovitz, Nicholas A., Thomas, Cristina, Pravec, Petr, Lister, Tim, Polakis, Tom, Osip, David, Kareta, Teddy, Rożek, Agata, Chesley, Steven, Naidu, Shantanu P., Scheirich, Peter, Ryan, William, Ryan, Eileen, Skiff, Brian, Snodgrass, Colin, Knight, Matthew M., Rivkin, Andy, Chabot, Nancy, Ayvazian, Vova, Belskaya, Irina, Benkhaldoun, Zouhair, Berteşteanu, Daniel N., Bonavita, Mariangela, Bressi, Terrence H., Brucker, Melissa J., Burgdorf, Martin J., Burkhonov, Otabek, Burt, Brian, Contreras, Carlos, Chatelain, Joseph, Choi, Young-Jun, Daily, Matthew, de León, Julia, Ergashev, Kamoliddin, Farnham, Tony, Fatka, Petr, Ferrais, Marin, Geier, Stefan, Gomez, Edward, Greenstreet, Sarah, Gröller, Hannes, Hergenrother, Carl, Holt, Carrie, Hornoch, Kamil, Husárik, Marek, Inasaridze, Raguli, Jehin, Emmanuel, Khalouei, Elahe, Kikwaya Eluo, Jean-Baptiste, Kim, Myung-Jin, Krugly, Yurij, Kučáková, Hana, Kušnirák, Peter, Larsen, Jeffrey A., Lee, Hee-Jae, Lejoly, Cassandra, Licandro, Javier, Longa-Peña, Penélope, Mastaler, Ronald A., McCully, Curtis, Moon, Hong-Kyu, Morrell, Nidia I., Nath, Arushi, Oszkiewicz, Dagmara, Parrott, Daniel, Phillips, Liz, Popescu, Marcel, Pray, Donald, Prodan, George Pantelimon, Rabus, Markus, Read, Michael T., Reva, Inna, Roark, Vernon, Santana-Ros, Toni, Scotti, James V., Tatara, Taiyo, Thirouin, Audrey, Tholen, David J., Troianskyi, Volodymyr, Tubbiolo, Andrew F., Villa, Katelyn, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Moskovitz, Nicholas A., Thomas, Cristina, Pravec, Petr, Lister, Tim, Polakis, Tom, Osip, David, Kareta, Teddy, Rożek, Agata, Chesley, Steven, Naidu, Shantanu P., Scheirich, Peter, Ryan, William, Ryan, Eileen, Skiff, Brian, Snodgrass, Colin, Knight, Matthew M., Rivkin, Andy, Chabot, Nancy, Ayvazian, Vova, Belskaya, Irina, Benkhaldoun, Zouhair, Berteşteanu, Daniel N., Bonavita, Mariangela, Bressi, Terrence H., Brucker, Melissa J., Burgdorf, Martin J., Burkhonov, Otabek, Burt, Brian, Contreras, Carlos, Chatelain, Joseph, Choi, Young-Jun, Daily, Matthew, de León, Julia, Ergashev, Kamoliddin, Farnham, Tony, Fatka, Petr, Ferrais, Marin, Geier, Stefan, Gomez, Edward, Greenstreet, Sarah, Gröller, Hannes, Hergenrother, Carl, Holt, Carrie, Hornoch, Kamil, Husárik, Marek, Inasaridze, Raguli, Jehin, Emmanuel, Khalouei, Elahe, Kikwaya Eluo, Jean-Baptiste, Kim, Myung-Jin, Krugly, Yurij, Kučáková, Hana, Kušnirák, Peter, Larsen, Jeffrey A., Lee, Hee-Jae, Lejoly, Cassandra, Licandro, Javier, Longa-Peña, Penélope, Mastaler, Ronald A., McCully, Curtis, Moon, Hong-Kyu, Morrell, Nidia I., Nath, Arushi, Oszkiewicz, Dagmara, Parrott, Daniel, Phillips, Liz, Popescu, Marcel, Pray, Donald, Prodan, George Pantelimon, Rabus, Markus, Read, Michael T., Reva, Inna, Roark, Vernon, Santana-Ros, Toni, Scotti, James V., Tatara, Taiyo, Thirouin, Audrey, Tholen, David J., Troianskyi, Volodymyr, Tubbiolo, Andrew F., and Villa, Katelyn

Abstract

On 2022 September 26, the Double Asteroid Redirection Test (DART) spacecraft impacted Dimorphos, the satellite of binary near-Earth asteroid (65803) Didymos. This demonstrated the efficacy of a kinetic impactor for planetary defense by changing the orbital period of Dimorphos by 33 minutes. Measuring the period change relied heavily on a coordinated campaign of lightcurve photometry designed to detect mutual events (occultations and eclipses) as a direct probe of the satellite's orbital period. A total of 28 telescopes contributed 224 individual lightcurves during the impact apparition from 2022 July to 2023 February. We focus here on decomposable lightcurves, i.e., those from which mutual events could be extracted. We describe our process of lightcurve decomposition and use that to release the full data set for future analysis. We leverage these data to place constraints on the postimpact evolution of ejecta. The measured depths of mutual events relative to models showed that the ejecta became optically thin within the first ∼1 day after impact and then faded with a decay time of about 25 days. The bulk magnitude of the system showed that ejecta no longer contributed measurable brightness enhancement after about 20 days postimpact. This bulk photometric behavior was not well represented by an HG photometric model. An HG1G2 model did fit the data well across a wide range of phase angles. Lastly, we note the presence of an ejecta tail through at least 2023 March. Its persistence implied ongoing escape of ejecta from the system many months after DART impact.

Published
2024

9. 2023 DZ2 Planetary Defense Campaign

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, Wiles, Mike, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, and Wiles, Mike

Abstract

We present the results of a fourth planetary defense exercise, focused this time on the small near-Earth asteroid (NEA) 2023 DZ2 and conducted during its close approach to the Earth in 2023 March. The International Asteroid Warning Network (IAWN), with support from NASA's Planetary Defense Coordination Office (PDCO), has been coordinating planetary defense observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. The last campaign focused on the NEA Apophis, and an outcome of that exercise was the need for a short burst campaign to replicate a real-life near-Earth object impact hazard scenario. The goal of the 2023 DZ2 campaign was to characterize the small NEA as a potential impactor and exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication with a short notice of just 24 hr. The entire campaign lasted about 10 days. The campaign team was divided into several working groups based on the characterization method: photometry, spectroscopy, thermal IR photometry and optical polarimetry, radar, and risk assessment. Science results from the campaign show that 2023 DZ2 has a rotation period of 6.2745 ± 0.0030 minutes; visible wavelength color photometry/spectroscopy/polarimetry and near-IR spectroscopy all point to an E-type taxonomic classification with surface composition analogous to aubrite meteorites; and radar observations show that the object has a diameter of 30 ± 10 m, consistent with the high albedo (0.49) derived from polarimetric and thermal IR observations.

Published
2024

10. Photometry of the Didymos System across the DART Impact Apparition

Author

Moskovitz, Nicholas, primary, Thomas, Cristina, additional, Pravec, Petr, additional, Lister, Tim, additional, Polakis, Tom, additional, Osip, David, additional, Kareta, Theodore, additional, Rożek, Agata, additional, Chesley, Steven R., additional, Naidu, Shantanu P., additional, Scheirich, Peter, additional, Ryan, William, additional, Ryan, Eileen, additional, Skiff, Brian, additional, Snodgrass, Colin, additional, Knight, Matthew M., additional, Rivkin, Andrew S., additional, Chabot, Nancy L., additional, Ayvazian, Vova, additional, Belskaya, Irina, additional, Benkhaldoun, Zouhair, additional, Berteşteanu, Daniel N., additional, Bonavita, Mariangela, additional, Bressi, Terrence H., additional, Brucker, Melissa J., additional, Burgdorf, Martin J., additional, Burkhonov, Otabek, additional, Burt, Brian, additional, Contreras, Carlos, additional, Chatelain, Joseph, additional, Choi, Young-Jun, additional, Daily, Matthew, additional, de León, Julia, additional, Ergashev, Kamoliddin, additional, Farnham, Tony, additional, Fatka, Petr, additional, Ferrais, Marin, additional, Geier, Stefan, additional, Gomez, Edward, additional, Greenstreet, Sarah, additional, Gröller, Hannes, additional, Hergenrother, Carl, additional, Holt, Carrie, additional, Hornoch, Kamil, additional, Husárik, Marek, additional, Inasaridze, Raguli, additional, Jehin, Emmanuel, additional, Khalouei, Elahe, additional, Eluo, Jean-Baptiste Kikwaya, additional, Kim, Myung-Jin, additional, Krugly, Yurij, additional, Kučáková, Hana, additional, Kušnirák, Peter, additional, Larsen, Jeffrey A., additional, Lee, Hee-Jae, additional, Lejoly, Cassandra, additional, Licandro, Javier, additional, Longa-Peña, Penélope, additional, Mastaler, Ronald A., additional, McCully, Curtis, additional, Moon, Hong-Kyu, additional, Morrell, Nidia, additional, Nath, Arushi, additional, Oszkiewicz, Dagmara, additional, Parrott, Daniel, additional, Phillips, Liz, additional, Popescu, Marcel M., additional, Pray, Donald, additional, Prodan, George Pantelimon, additional, Rabus, Markus, additional, Read, Michael T., additional, Reva, Inna, additional, Roark, Vernon, additional, Santana-Ros, Toni, additional, Scotti, James V., additional, Tatara, Taiyo, additional, Thirouin, Audrey, additional, Tholen, David, additional, Troianskyi, Volodymyr, additional, Tubbiolo, Andrew F., additional, and Villa, Katelyn, additional

Published
2024
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11. Surface Heterogeneity, Physical, and Shape Model of Near-Earth Asteroid (52768) 1998 OR2

Author

Devogèle, Maxime, primary, McGilvray, Anna, additional, MacLennan, Eric, additional, Monchinski, Courteney, additional, Marshall, Sean E., additional, Hickson, Dylan, additional, Virkki, Anne, additional, Giorgini, Jon D., additional, Abe, Lyu, additional, Augustin, David, additional, Aznar-Macías, Amadeo, additional, Baudouin, Philippe, additional, Behrend, Raoul, additional, Bendjoya, Philippe, additional, Benkhaldoun, Zouhair, additional, Bosch, Josep, additional, Cellino, Alberto, additional, Chatelain, Joseph, additional, Deldem, Marc, additional, Ferrais, Marin, additional, Goncalves, Rui, additional, Houdin, Gerard, additional, Husárik, Marek, additional, Jehin, Emmanuel, additional, Kareta, Teddy, additional, Kim, Myung-Jin, additional, Licandro, Javier, additional, Lister, Tim, additional, Medeiros, Hissa, additional, Pravec, Petr, additional, Rivet, Jean-Pierre, additional, Rousseau, Gerald, additional, Roh, Dong-Goo, additional, Skiff, Brian, additional, Taylor, Patrick A., additional, Venditti, Flaviane, additional, Vernet, David, additional, Vienney, Jean-Michel, additional, Yim, Hong-Suh, additional, and Zambrano-Marin, Luisa, additional

Published
2024
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12. Achievement of the Planetary Defense Investigations of the Double Asteroid Redirection Test (DART) Mission

Author

Chabot, Nancy L., primary, Rivkin, Andrew S., additional, Cheng, Andrew F., additional, Barnouin, Olivier S., additional, Fahnestock, Eugene G., additional, Richardson, Derek C., additional, Stickle, Angela M., additional, Thomas, Cristina A., additional, Ernst, Carolyn M., additional, Terik Daly, R., additional, Dotto, Elisabetta, additional, Zinzi, Angelo, additional, Chesley, Steven R., additional, Moskovitz, Nicholas A., additional, Barbee, Brent W., additional, Abell, Paul, additional, Agrusa, Harrison F., additional, Bannister, Michele T., additional, Beccarelli, Joel, additional, Bekker, Dmitriy L., additional, Bruck Syal, Megan, additional, Buratti, Bonnie J., additional, Busch, Michael W., additional, Campo Bagatin, Adriano, additional, Chatelain, Joseph P., additional, Chocron, Sidney, additional, Collins, Gareth S., additional, Conversi, Luca, additional, Davison, Thomas M., additional, DeCoster, Mallory E., additional, Prasanna Deshapriya, J. D., additional, Eggl, Siegfried, additional, Espiritu, Raymond C., additional, Farnham, Tony L., additional, Ferrais, Marin, additional, Ferrari, Fabio, additional, Föhring, Dora, additional, Fuentes-Muñoz, Oscar, additional, Gai, Igor, additional, Giordano, Carmine, additional, Glenar, David A., additional, Gomez, Edward, additional, Graninger, Dawn M., additional, Green, Simon F., additional, Greenstreet, Sarah, additional, Hasselmann, Pedro H., additional, Herreros, Isabel, additional, Hirabayashi, Masatoshi, additional, Husárik, Marek, additional, Ieva, Simone, additional, Ivanovski, Stavro L., additional, Jackson, Samuel L., additional, Jehin, Emmanuel, additional, Jutzi, Martin, additional, Karatekin, Ozgur, additional, Knight, Matthew M., additional, Kolokolova, Ludmilla, additional, Kumamoto, Kathryn M., additional, Küppers, Michael, additional, La Forgia, Fiorangela, additional, Lazzarin, Monica, additional, Li, Jian-Yang, additional, Lister, Tim A., additional, Lolachi, Ramin, additional, Lucas, Michael P., additional, Lucchetti, Alice, additional, Luther, Robert, additional, Makadia, Rahil, additional, Mazzotta Epifani, Elena, additional, McMahon, Jay, additional, Merisio, Gianmario, additional, Merrill, Colby C., additional, Meyer, Alex J., additional, Michel, Patrick, additional, Micheli, Marco, additional, Migliorini, Alessandra, additional, Minker, Kate, additional, Modenini, Dario, additional, Moreno, Fernando, additional, Murdoch, Naomi, additional, Murphy, Brian, additional, Naidu, Shantanu P., additional, Nair, Hari, additional, Nakano, Ryota, additional, Opitom, Cyrielle, additional, Ormö, Jens, additional, Michael Owen, J., additional, Pajola, Maurizio, additional, Palmer, Eric E., additional, Palumbo, Pasquale, additional, Panicucci, Paolo, additional, Parro, Laura M., additional, Pearl, Jason M., additional, Penttilä, Antti, additional, Perna, Davide, additional, Petrescu, Elisabeta, additional, Pravec, Petr, additional, Raducan, Sabina D., additional, Ramesh, K. T., additional, Ridden-Harper, Ryan, additional, Rizos, Juan L., additional, Rossi, Alessandro, additional, Roth, Nathan X., additional, Rożek, Agata, additional, Rozitis, Benjamin, additional, Ryan, Eileen V., additional, Ryan, William H., additional, Sánchez, Paul, additional, Santana-Ros, Toni, additional, Scheeres, Daniel J., additional, Scheirich, Peter, additional, Berk Senel, Cem, additional, Snodgrass, Colin, additional, Soldini, Stefania, additional, Souami, Damya, additional, Statler, Thomas S., additional, Street, Rachel, additional, Stubbs, Timothy J., additional, Sunshine, Jessica M., additional, Tan, Nicole J., additional, Tancredi, Gonzalo, additional, Tinsman, Calley L., additional, Tortora, Paolo, additional, Tusberti, Filippo, additional, Walker, James D., additional, Waller, C. Dany, additional, Wünnemann, Kai, additional, Zannoni, Marco, additional, and Zhang, Yun, additional

Published
2024
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13. The violent collisional history of aqueously evolved (2) Pallas

Author

Marsset, Michaël, Brož, Miroslav, Vernazza, Pierre, Drouard, Alexis, Castillo-Rogez, Julie, Hanuš, Josef, Viikinkoski, Matti, Rambaux, Nicolas, Carry, Benoît, Jorda, Laurent, Ševeček, Pavel, Birlan, Mirel, Marchis, Franck, Podlewska-Gaca, Edyta, Asphaug, Erik, Bartczak, Przemyslaw, Berthier, Jérôme, Cipriani, Fabrice, Colas, François, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Ferrais, Marin, Fétick, Romain, Fusco, Thierry, Jehin, Emmanuel, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Richardson, Derek C., Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, and Yang, Bin

Published
2020
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14. Multicolor Photometry of Tiny Near-Earth Asteroid 2015 RN35 across a Wide Range of Phase Angles: Possible Mission-accessible A-type Asteroid

Author

Beniyama, Jin, primary, Ohsawa, Ryou, additional, Avdellidou, Chrysa, additional, Sako, Shigeyuki, additional, Takita, Satoshi, additional, Ishiguro, Masateru, additional, Sekiguchi, Tomohiko, additional, Usui, Fumihiko, additional, Kinoshita, Shinichi W., additional, Lee, Kianhong, additional, Takumi, Asami, additional, Ferrais, Marin, additional, and Jehin, Emmanuël, additional

Published
2023
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15. Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model

Author

Kueny, Jay K., primary, Chandler, Colin Orion, additional, Devogéle, Maxime, additional, Moskovitz, Nicholas, additional, Pravec, Petr, additional, Kučáková, Hana, additional, Hornoch, Kamil, additional, Kušnirák, Peter, additional, Granvik, Mikael, additional, Konstantopoulou, Christina, additional, Jannsen, Nicholas E., additional, Moran, Shane, additional, Siltala, Lauri, additional, Fedorets, Grigori, additional, Ferrais, Marin, additional, Jehin, Emmanuel, additional, Kareta, Theodore, additional, and Hanuš, Josef, additional

Published
2023
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16. The equilibrium shape of (65) Cybele: primordial or relic of a large impact?

Author

Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Marsset, Michaël, Brož, Miroslav, Vermersch, Julie, Rambaux, Nicolas, Ferrais, Marin, Viikinkoski, Matti, Hanuš, Josef, Jehin, Emmanuel, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Dudziński, Grzegorz, Carry, Benoît, Vernazza, Pierre, Szakáts, Róbert, Duffard, René, Jones, A., Molina, David, Santana-Ros, Toni, Benkhaldoun, Zouhair, Birlan, Mirel, Dumas, Christophe, Fétick, Romain, Fusco, Thierry, Jorda, Laurent, Marchis, Franck, Vachier, Frédéric, Yang, Bin, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Marsset, Michaël, Brož, Miroslav, Vermersch, Julie, Rambaux, Nicolas, Ferrais, Marin, Viikinkoski, Matti, Hanuš, Josef, Jehin, Emmanuel, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Dudziński, Grzegorz, Carry, Benoît, Vernazza, Pierre, Szakáts, Róbert, Duffard, René, Jones, A., Molina, David, Santana-Ros, Toni, Benkhaldoun, Zouhair, Birlan, Mirel, Dumas, Christophe, Fétick, Romain, Fusco, Thierry, Jorda, Laurent, Marchis, Franck, Vachier, Frédéric, and Yang, Bin

Abstract

Context. Cybele asteroids constitute an appealing reservoir of primitive material genetically linked to the outer Solar System, and the physical properties (size and shape) of the largest members can be readily accessed by large (8m class) telescopes. Aims. We took advantage of the bright apparition of the most iconic member of the Cybele population, (65) Cybele, in July and August 2021 to acquire high-angular-resolution images and optical light curves of the asteroid with which we aim to analyse its shape and bulk properties. Methods. Eight series of images were acquired with VLT/SPHERE+ZIMPOL, seven of which were combined with optical light curves to reconstruct the shape of the asteroid using the ADAM, MPCD, and SAGE algorithms. The origin of the shape was investigated by means of N-body simulations. Results. Cybele has a volume-equivalent diameter of 263±3 km and a bulk density of 1.55 ± 0.19 g cm−3. Notably, its shape and rotation state are closely compatible with those of a Maclaurin equilibrium figure. The lack of a collisional family associated with Cybele and the higher bulk density of that body with respect to other large P-type asteroids suggest that it never experienced any large disruptive impact followed by rapid re-accumulation. This would imply that its present-day shape represents the original one. However, numerical integration of the long-term dynamical evolution of a hypothetical family of Cybele shows that it is dispersed by gravitational perturbations and chaotic diffusion over gigayears of evolution. Conclusions. The very close match between Cybele and an equilibrium figure opens up the possibility that D ≥ 260 km (M ≥ 1.5 × 1019 kg) small bodies from the outer Solar System all formed at equilibrium. However, we cannot currently rule out an old impact as the origin of the equilibrium shape of Cybele. Cybele itself is found to be dynamically unstable, implying that it was ‘recently’ (<1 Gyr ago) placed on its current orbit either through slow d

Published
2023

17. Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Hasegawa, Sunao, DeMeo, Francesca E, Marsset, Michaël, Hanuš, Josef, Avdellidou, Chrysa, Delbo, Marco, Bus, Schelte J, Hanayama, Hidekazu, Horiuchi, Takashi, Takir, Driss, Jehin, Emmanuël, Ferrais, Marin, Geem, Jooyeon, Im, Myungshin, Seo, Jinguk, Bach, Yoonsoo P, Jin, Sunho, Ishiguro, Masateru, Kuroda, Daisuke, Binzel, Richard P, Nakamura, Akiko M, Yang, Bin, Vernazza, Pierre, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Hasegawa, Sunao, DeMeo, Francesca E, Marsset, Michaël, Hanuš, Josef, Avdellidou, Chrysa, Delbo, Marco, Bus, Schelte J, Hanayama, Hidekazu, Horiuchi, Takashi, Takir, Driss, Jehin, Emmanuël, Ferrais, Marin, Geem, Jooyeon, Im, Myungshin, Seo, Jinguk, Bach, Yoonsoo P, Jin, Sunho, Ishiguro, Masateru, Kuroda, Daisuke, Binzel, Richard P, Nakamura, Akiko M, Yang, Bin, and Vernazza, Pierre

Abstract

Abstract The surfaces of airless bodies like asteroids in the solar system are known to be affected by space weathering. Experiments simulating space weathering are essential for studying the effects of this process on meteorite samples, but the problem is that the time spent to reproduce space weathering in these experiments is billions of times shorter than the actual phenomenon. In 2010 December, the T-type asteroid 596 Scheila underwent a collision with an impactor a few tens of meters in size. A decade later, there is an opportunity to study how the surface layer of this asteroid is being altered by space weathering after the impact. To do so, we performed visible spectrophotometric and near-infrared spectroscopic observations of 596 Scheila. The acquired spectrum is consistent with those observed shortly after the 2010 impact event within the observational uncertainty range. This indicates that the surface color of dark asteroids is not noticeably changed by space weathering over a 10 yr period. This study is the first to investigate color changes due to space weathering on an actual asteroid surface in the solar system. Considering that fresh layers are regularly created on asteroid surfaces by collisions, we suggest a genetic link between D/T-type and dark (low albedo) X-complex asteroids and very red objects such as 269 Justitia, 732 Tjilaki, and 203 Pompeja. New observations show that 203 Pompeja has an X-type-like surface, with some local surface areas exhibiting a very red spectrum.

Published
2023

18. VLT/SPHERE imaging survey of D>100 km asteroids: Final results and synthesis

Author

Vernazza, Pierre, Carry, Benoit, Ferrais, Marin, Jorda, Laurent, Hanus, Josef, Marsset, Michael, Brož, Miroslav, Fetick, Roman, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague] (CU), and European Southern Observatory (ESO)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

Until recently, only three large main belt asteroids, Ceres, Vesta and Lutetia, had been imaged with a high level of detail, as they were visited by the space missions Dawn and Rosetta of NASA and the European Space Agency, respectively. The previously small number of detailed observations of asteroids meant that, until now, key characteristics such as their 3D shape or density had remained largely unknown. Between 2017 and 2019, we have been filling this gap by conducting a high-angular-resolution imaging survey of 42 large main-belt asteroids with VLT/SPHERE (ESO large programme; PI: P. Vernazza; ID: 199.C-0074), sampling the main compositional classes. These observations have allowed to cast some light on the following fundamental questions: – What is the diversity in shape among large asteroids and are the shapes close to equilibrium?– How do large impacts affect asteroid shape?– What is the bulk density of large asteroids and is there a relationship with their surface composition? Is there any evidence of differentiation among those bodies?– Is the density of those bodies that are predicted to be implanted bodies from the outer Solar System (P/D-types) compatible with that of small (D ≤ 300 km) trans-Neptunian objects?– What physical properties drive the formation of companions around large asteroids? Importantly, our survey along with previous observations provides evidence in support of the possibility that some C-complex bodies could be intrinsically related to IDP-like P- and D-type asteroids, representing different layers of a same body (C: core; P/D: outer shell). We therefore propose that P/ D-types and some C-types may have the same origin in the primordial trans-Neptunian disk. The main belt would thus host a population of former TNOs much more important than the one previously considered, consisting solely of P and D-type bodies. Here, we will present an overview of the results obtained from this survey ([1]) with a specific focus on the origin of a large fraction of the asteroid belt (typically C, P and D-type bodies). References [1] Vernazza, P., Ferrais, M., Jorda, L., et al. VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. A&A 654, 2021.

Published
2023

19. The changing rotation period of 3200 Phaethon

Author

Marshall, Sean, Devogele, Maxime, Taylor, Patrick, Magri, Christopher, Beniyama, Jin, Sekiguchi, Tomohiko, Kuroda, Daisuke, Urakawa, Seitaro, Yoshida, Fumi, Arai, Tomoko, Warner, Brian, Pravec, Petr, Kučáková, Hana, Hornoch, Kamil, Kušnirák, Peter, Hanuš, Josef, Ferrais, Marin, Jehin, Emmanuel, Kuznetsov, Eduard, Glamazda, Dmitrij, Kaiser, Galina, Shagabutdinov, Andrej, Vibe, Yuliya, Serebryanskiy, Aleksander, Krugov, Maxim, Reva, Inna, Kim, Myung-Jin, Kim, Dong-Heun, 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), and Beaussier, Catherine

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Abstract

International audience; 3200 Phaethon is one of the largest potentially hazardous asteroids. It is also the first asteroid to be discovered in spacecraft images, the parent body of the Geminid meteor stream, and the target of JAXA's upcoming DESTINY+ mission. We have developed a physical model of Phaethon's shape and rotation state, using radar data from Arecibo and Goldstone in 2007 and 2017, stellar occultations from 2019 through 2021, and lightcurves from many apparitions (from 1989 through 2021). Phaethon has a volume-equivalent diameter of about 5.3 kilometers. It is approximately spheroidal with an equatorial ridge, resembling the shapes of 101955 Bennu and 162173 Ryugu. The earliest available lightcurve of Phaethon is from 1989 October 9 (published in Wisniewski et al. 1997). Hanuš et al. (2016) noticed that their shape model's rotation phase differed from that 1989 observation by about 20 minutes. They noted that this may be from Phaethon's rotation period changing due to activity, but they could not say whether this was real or just a timing error in that one lightcurve, since the next lightcurves are from 1994. A model with a constant rotation period provided a good fit to all of the data from 1994 through 2020. However, this model could not adequately fit the lightcurves that were acquired from four different observatories in 2021. There was a difference of about 15 minutes between the predicted and observed rotation phases — clearly greater than what the observations' uncertainties could permit. We initially considered that Phaethon's rotation period may have changed before the 2021 observations, perhaps due to activity when it was near perihelion in December 2020. However, we found that a constant rotational acceleration provides a good fit to all of the data from 1989 through 2021, clearly accounting for the discrepancies seen in 1989 and 2021 while also slightly improving the model's agreement with the data during other apparitions. We find that Phaethon's sidereal rotation period in December 2017 was 3.603944 hours. Its spin rate is increasing at a rate of 2.1×10-6 deg/day2, which corresponds to its rotation period decreasing by about 4 milliseconds per year.

Published
2023

20. Polarimetry as a tool for physical characterization of potentially hazardous NEOs

Author

Devogele, Maxime, Masiero, Joseph, Vega Santiago, Nathalia, Bendjoya, Philippe, Rivet, Jean-Pierre, Cellino, Alberto, Ferrais, Marin, Jehin, Emmanuel, Macias, Isabella, Castaneda Jaimes, Joahan, Moskovitz, Nicholas, Borisov, Galin, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-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
[SDU]Sciences of the Universe [physics]
Abstract

International audience; The degree of linear polarization of sunlight scattered by an asteroid contains valuable information for rapid characterization of the surface properties of Near-Earth objects (NEOs). In the case of atmosphereless bodies the state of linear polarization varies as a function of the phase angle (α) and is described using the so-called Pr parameter [1]. The properties of the phase-polarization curve of an asteroid are mostly defined by its albedo (pV). Numerous calibrations between polarization and pV have been proposed for main-belt asteroids [2, 3]. However, main-belt asteroids rarely exceed phase angle > 30° while near Earth objects can be observed at phase angle as large as 100°[4]. These observations at higher phase angles allow for deeper characterization of the observed object, but there is currently a lack of observations of NEOs in polarimetry to accurately calibrate the albedo-polarization relationship at high phase angles. We recently started a survey of Near-earth Objects in polarimetry to characterize their phase-polarization curve at high phase angle in order to calibrate the relation between polarization and albedo. These polarimetric observations are complemented with visible photometry, thermal infra-red, spectroscopy, and/or radar observations to obtain independent characterization of the size, shape, albedo, and other surface properties of the objects observed in polarimetry. In this presentation, we will present the polarimetric observations obtained so far. We describe the large variety variety of polarimetric response at high phase angle with polarization ranging from 1 to 50% when observed at the same phase angle. We also discuss the first results using physical characterization using radar, photometric, and thermal observations and how these can be used to calibrate the relation existing between polarimetry and albedo. [1] I. Belskaya, A. Cellino, R. Gil-Hutton, et al., Asteroid Polarimetry, Asteroid IV, (2015) 151-163 [2] A. Cellino, R. Gil-Hutton, A. Dell'Oro, et al. A new calibration of the albedo-polarization relation for the asteroids, JQSRT 113 (2012) 2552–2560. [3] A. Cellino, S. Bagnulo, R. Gil-Hutton, et al., On the calibration of the relation between geometric albedo and polarimetric properties for the asteroids, MNRAS 451 (2015) 3473–3488. [4] M. Devogele, A. Cellino, G. Borisov, et al. The phase-polarization curve of asteroid (3200) Phaethon, MNRAS, 479 (2018) 3498-3508

Published
2023

21. Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade

Author

Hasegawa, Sunao, primary, DeMeo, Francesca E., additional, Marsset, Michaël, additional, Hanuš, Josef, additional, Avdellidou, Chrysa, additional, Delbo, Marco, additional, Bus, Schelte J., additional, Hanayama, Hidekazu, additional, Horiuchi, Takashi, additional, Takir, Driss, additional, Jehin, Emmanuël, additional, Ferrais, Marin, additional, Geem, Jooyeon, additional, Im, Myungshin, additional, Seo, Jinguk, additional, Bach, Yoonsoo P., additional, Jin, Sunho, additional, Ishiguro, Masateru, additional, Kuroda, Daisuke, additional, Binzel, Richard P., additional, Nakamura, Akiko M., additional, Yang, Bin, additional, and Vernazza, Pierre, additional

Published
2022
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22. Constraining the shape and density of binary asteroid (121) Hermione

Author

Ferrais, Marin, primary, Vernazza, Pierre, additional, Marsset, Michaël, additional, Jorda, Laurent, additional, Carry, Benoit, additional, Hanus, Josef, additional, Brož, Miroslav, additional, Yang, Bin, additional, Fétick, Romain, additional, Marchis, Franck, additional, Vachier, Frederic, additional, Birlan, Mirel, additional, Jehin, Emmanuël, additional, Podlewska-Gaca, Edyta, additional, Bartczak, Przemyslaw, additional, Fusco, Thierry, additional, and Dudziński, Grzegorz, additional

Published
2022
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23. (65) Cybele is the smallest asteroid at hydrostatic equilibrium, why?

Author

Marsset, Michaël, primary, Brož, Miroslav, additional, Vermersch, Julie, additional, Rambaux, Nicolas, additional, Ferrais, Marin, additional, Viikinkoski, Matti, additional, Hanuš, Josef, additional, Jehin, Emmanuel, additional, Podlewska-Gaca, Edyta, additional, Bartczak, Przemyslaw, additional, Dudziński, Grzegorz, additional, Carry, Benoit, additional, and Vernazza, Pierre, additional

Published
2022
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24. Hi’iaka’s physical and dynamical properties using long-term photometric data

Author

Fernández-Valenzuela, Estela, primary, Ortiz, José Luis, additional, Morales, Nicolás, additional, Jehin, Emmanuel, additional, Burdanov, Artem, additional, de Wit, Julien, additional, Ferrais, Marin, additional, Vara-Lubiano, Mónica, additional, Morales, Rafael, additional, Kretlow, Mike, additional, Santos-Sanz, Pablo, additional, Alvarez-Candal, Alvaro, additional, Duffard, René, additional, Pál, András, additional, Kiss, Csaba, additional, and Szakáts, Róbert, additional

Published
2022
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25. M-type (22) Kalliope: A tiny Mercury

Author

Ferrais, Marin, Jorda, L., Vernazza, Pierre, Carry, Benoit, Broz, M., Rambaux, N., Hanus, J., Dudzinski, G., Bartczak, P., Vachier, F., Aristidi, Eric, Beck, P., Marchis, F., Marsset, M., Viikinkoski, M., Fetick, R., Drouard, A., Fusco, T., Birlan, M., Podlewska-Gaca, E., Burbine, T.H., Dyar, M.D., Bendjoya, Philippe, Benkhaldoun, Zouhair, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, F., Dumas, Christophe, Ďurech, J., Fauvaud, S., Grice, J., Jehin, Emmanuël, Kaasalainen, M., Kryszczynska, A., Lamy, Philippe, Coroller, H., Marciniak, Alexandre, Michalowski, T., Michel, Patrick, Prieur, Jean-Louis, Reddy, V., Rivet, Jean‐pierre, Santana-Ros, Toni, Scardia, Marco, Tanga, Paolo, Vigan, Arthur, Witasse, Olivier, Yang, B., 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of Charles University, Charles University [Prague] (CU), 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), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, SETI Institute, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), University of Tampere [Finland], ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Astronomical Institute of Romanian Academy, Romanian Academy, Institute of Physics [Szczecin], University of Szczecin, Department of Astronomy of the Mount Holyoke College, Mount Holyoke College, Oukaimeden Observatory, Université Cadi Ayyad [Marrakech] (UCA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), TMT International Observatory, Observatoire du Bois de Bardon, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Universidad Diego Portales [Santiago] (UDP), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], Agence Spatiale Européenne = European Space Agency (ESA), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-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), Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.C-0074 (PI: P. Vernazza). P. V., A. D., M. F. and B. C. were supported by CNRS/INSU/PNP. The research of J.H. has been supported by the Czech Science Foundation through grant 20-08218S and by Charles University Research program no. UNCE/SCI/023. M.B. was supported by the Czech Science Foundation, grant 21-11058S. F.M. is supported by the National Science Foundation under grant no. 1743015. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liège, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is F.R.S.-FNRS Senior Research Associate. The work of T.S.R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE)., Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Tampere University, Computing Sciences, Centre National de la Recherche Scientifique (France), Charles University (Czech Republic), Czech Science Foundation, Fonds de La Recherche Scientifique (Belgique), National Science Foundation (US), Université Cadi Ayyad, Generalitat Valenciana, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), and European Commission

Subjects
asteroids, Astronomy and Astrophysics, Observation, (22) Kalliope, Techniques: high angular resolution, high angular resolution [Techniques], individual: (22) Kalliope [Minor planets, asteroids], Methods: observational, Space and Planetary Science, Asteroids: individual: (22) Kalliope, 111 Mathematics, minor planets, observational [Methods], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high angular resolution, ComputingMilieux_MISCELLANEOUS, Astronomía y Astrofísica
Abstract

M.Ferrais et al., [Context] Asteroid (22) Kalliope is the second largest M-type asteroid in the main belt and is orbited by a satellite, Linus. Whereas the mass of Kalliope is already well constrained thanks to the presence of a moon, its volume is still poorly known, leading to uncertainties on its bulk density and internal structure., [Aims] We aim to refine the shape of (22) Kalliope and thus its diameter and bulk density, as well as the orbit of its moon to better constrain its mass, hence density and internal structure., [Methods] We acquired disk-resolved observations of (22) Kalliope using the VLT/SPHERE/ZIMPOL instrument to reconstruct its three-dimensional (3D) shape using three different modeling techniques. These images were also used together with new speckle observations at the C2PU/PISCO instrument as well as archival images from other large ground-based telescopes to refine the orbit of Linus., [Results] The volume of (22) Kalliope given by the shape models, corresponding to D = 150 ± 5 km, and the mass constrained by its satellite’s orbit yield a density of ρ = 4.40 ± 0.46 g cm−3. This high density potentially makes (22) Kalliope the densest known small body in the Solar System. A macroporosity in the 10–25% range (as expected for this mass and size), implies a grain density in the 4.8–5.9 g cm−3 range. Kalliope’s high bulk density, along with its silicate-rich surface implied by its low radar albedo, implies a differentiated interior with metal contributing to most of the mass of the body., [Conclusions] Kalliope’s high metal content (40–60%) along with its metal-poor mantle makes it the smallest known Mercury-like body. A large impact at the origin of the formation of the moon Linus is likely the cause of its high metal content and density., Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.C-0074 (PI: P. Vernazza). P. V., A. D., M. F. and B. C. were supported by CNRS/INSU/PNP. The research of J.H. has been supported by the Czech Science Foundation through grant 20-08218S and by Charles University Research program no. UNCE/SCI/023. M.B. was supported by the Czech Science Foundation, grant 21-11058S. F.M. is supported by the National Science Foundation under grant no. 1743015. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liège, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is F.R.S.-FNRS Senior Research Associate. The work of T.S.R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE).

Published
2022

26. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Ďurech, Josef, Alí-Lagoa, Víctor, Ogłoza, W., Szakáts, Róbert, Müller, Thomas G., Molnár, László, Pál, András, Monteiro, F., Arcoverde, P., Behrend, Raoul, Benkhaldoun, Zouhair, Bernasconi, Laurent, Bosch, J., Brincat, S., Brunetto, L., Butkiewicz-Bąk, Magdalena, Del Freo, F., Duffard, René, Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, Marin, Geier, Stefan, Golonka, J., Grice, Jonny, Hirsch, R., Horbowicz, J., Jehin, Emmanuel, Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M.K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, Myung-Jin, Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, Nicolás, Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, Edyta, Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, René, Sanabria, J.J., Santana-Ros, Toni, Skiff, B., Skrzypek, J., Sobkowiak, Krzysztof, Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., Żukowski, K., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Ďurech, Josef, Alí-Lagoa, Víctor, Ogłoza, W., Szakáts, Róbert, Müller, Thomas G., Molnár, László, Pál, András, Monteiro, F., Arcoverde, P., Behrend, Raoul, Benkhaldoun, Zouhair, Bernasconi, Laurent, Bosch, J., Brincat, S., Brunetto, L., Butkiewicz-Bąk, Magdalena, Del Freo, F., Duffard, René, Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, Marin, Geier, Stefan, Golonka, J., Grice, Jonny, Hirsch, R., Horbowicz, J., Jehin, Emmanuel, Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M.K., Kankiewicz, P., Kecskeméthy, V., Kim, D.-H., Kim, Myung-Jin, Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, Nicolás, Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, Edyta, Polakis, T., Richard, F., Rodrigues, T., Rondón, E., Roy, René, Sanabria, J.J., Santana-Ros, Toni, Skiff, B., Skrzypek, J., Sobkowiak, Krzysztof, Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.

Abstract

Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to <400 J m−2 s−1∕2 K−1, not showing any correlation with the period. Conclusions. With this work we increase the sample of slow rotators with reliable spin and shape models and known thermal inertia by 40%. The thermal inertia values of our sample d

Published
2021

27. Evidence for differentiation of the most primitive small bodies

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Carry, Benoît, Vernazza, Pierre, Vachier, Frédéric, Neveu, Marc, Berthier, Jérôme, Hanuš, Josef, Ferrais, Marin, Jorda, Laurent, Marsset, Michaël, Viikinkoski, Matti, Bartczak, Przemyslaw, Behrend, Raoul, Benkhaldoun, Zouhair, Birlan, Mirel, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Drouard, Alexis, Dudziński, Grzegorz, Desmars, Josselin, Dumas, Christophe, Ďurech, Josef, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Jehin, Emmanuel, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Marchis, Franck, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Podlewska-Gaca, Edyta, Rambaux, Nicolas, Santana-Ros, Toni, Storrs, Alexander, Tanga, Paolo, Vigan, Arthur, Warner, Brian, Wieczorek, Mark, Witasse, Olivier, Yang, Bin, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Carry, Benoît, Vernazza, Pierre, Vachier, Frédéric, Neveu, Marc, Berthier, Jérôme, Hanuš, Josef, Ferrais, Marin, Jorda, Laurent, Marsset, Michaël, Viikinkoski, Matti, Bartczak, Przemyslaw, Behrend, Raoul, Benkhaldoun, Zouhair, Birlan, Mirel, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Drouard, Alexis, Dudziński, Grzegorz, Desmars, Josselin, Dumas, Christophe, Ďurech, Josef, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Jehin, Emmanuel, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Marchis, Franck, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Podlewska-Gaca, Edyta, Rambaux, Nicolas, Santana-Ros, Toni, Storrs, Alexander, Tanga, Paolo, Vigan, Arthur, Warner, Brian, Wieczorek, Mark, Witasse, Olivier, and Yang, Bin

Abstract

Context. Dynamical models of Solar System evolution have suggested that the so-called P- and D-type volatile-rich asteroids formed in the outer Solar System beyond Neptune’s orbit and may be genetically related to the Jupiter Trojans, comets, and small Kuiper belt objects (KBOs). Indeed, the spectral properties of P- and D-type asteroids resemble that of anhydrous cometary dust. Aims. We aim to gain insights into the above classes of bodies by characterizing the internal structure of a large P- and D-type asteroid. Methods. We report high-angular-resolution imaging observations of the P-type asteroid (87) Sylvia with the Very Large Telescope Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument. These images were used to reconstruct the 3D shape of Sylvia. Our images together with those obtained in the past with large ground-based telescopes were used to study the dynamics of its two satellites. We also modeled Sylvia’s thermal evolution. Results. The shape of Sylvia appears flattened and elongated (a/b ~1.45; a/c ~1.84). We derive a volume-equivalent diameter of 271 ± 5 km and a low density of 1378 ± 45 kg m−3. The two satellites orbit Sylvia on circular, equatorial orbits. The oblateness of Sylvia should imply a detectable nodal precession which contrasts with the fully-Keplerian dynamics of its two satellites. This reveals an inhomogeneous internal structure, suggesting that Sylvia is differentiated. Conclusions. Sylvia’s low density and differentiated interior can be explained by partial melting and mass redistribution through water percolation. The outer shell should be composed of material similar to interplanetary dust particles (IDPs) and the core should be similar to aqueously altered IDPs or carbonaceous chondrite meteorites such as the Tagish Lake meteorite. Numerical simulations of the thermal evolution of Sylvia show that for a body of such a size, partial melting was unavoidable due to the decay of long-lived radionuclides. In addit

Published
2021

28. (216) Kleopatra, a low density critically rotating M-type asteroid

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marchis, Franck, Jorda, Laurent, Vernazza, Pierre, Brož, Miroslav, Hanuš, Josef, Ferrais, Marin, Vachier, Frédéric, Rambaux, Nicolas, Marsset, Michaël, Viikinkoski, Matti, Jehin, Emmanuel, Benseguane, Selma, Podlewska-Gaca, Edyta, Carry, Benoît, Drouard, Alexis, Fauvaud, S., Birlan, Mirel, Berthier, Jérôme, Bartczak, Przemyslaw, Dumas, Christophe, Dudziński, Grzegorz, Ďurech, Josef, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Kryszczynska, Agnieszka, Lamy, Philippe, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Santana-Ros, Toni, Tanga, Paolo, Vigan, Arthur, Witasse, Olivier, Yang, Bin, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marchis, Franck, Jorda, Laurent, Vernazza, Pierre, Brož, Miroslav, Hanuš, Josef, Ferrais, Marin, Vachier, Frédéric, Rambaux, Nicolas, Marsset, Michaël, Viikinkoski, Matti, Jehin, Emmanuel, Benseguane, Selma, Podlewska-Gaca, Edyta, Carry, Benoît, Drouard, Alexis, Fauvaud, S., Birlan, Mirel, Berthier, Jérôme, Bartczak, Przemyslaw, Dumas, Christophe, Dudziński, Grzegorz, Ďurech, Josef, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Kryszczynska, Agnieszka, Lamy, Philippe, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Santana-Ros, Toni, Tanga, Paolo, Vigan, Arthur, Witasse, Olivier, and Yang, Bin

Abstract

Context. The recent estimates of the 3D shape of the M/Xe-type triple asteroid system (216) Kleopatra indicated a density of ~5 g cm−3, which is by far the highest for a small Solar System body. Such a high density implies a high metal content as well as a low porosity which is not easy to reconcile with its peculiar “dumbbell” shape. Aims. Given the unprecedented angular resolution of the VLT/SPHERE/ZIMPOL camera, here, we aim to constrain the mass (via the characterization of the orbits of the moons) and the shape of (216) Kleopatra with high accuracy, hence its density. Methods. We combined our new VLT/SPHERE observations of (216) Kleopatra recorded during two apparitions in 2017 and 2018 with archival data from the W. M. Keck Observatory, as well as lightcurve, occultation, and delay-Doppler images, to derive a model of its 3D shape using two different algorithms (ADAM, MPCD). Furthermore, an N-body dynamical model allowed us to retrieve the orbital elements of the two moons as explained in the accompanying paper. Results. The shape of (216) Kleopatra is very close to an equilibrium dumbbell figure with two lobes and a thick neck. Its volume equivalent diameter (118.75 ± 1.40) km and mass (2.97 ± 0.32) × 1018 kg (i.e., 56% lower than previously reported) imply a bulk density of (3.38 ± 0.50) g cm−3. Such a low density for a supposedly metal-rich body indicates a substantial porosity within the primary. This porous structure along with its near equilibrium shape is compatible with a formation scenario including a giant impact followed by reaccumulation. (216) Kleopatra’s current rotation period and dumbbell shape imply that it is in a critically rotating state. The low effective gravity along the equator of the body, together with the equatorial orbits of the moons and possibly rubble-pile structure, opens the possibility that the moons formed via mass shedding. Conclusions. (216) Kleopatra is a puzzling multiple system due to the unique characteristics of the pr

Published
2021

29. FRIPON: a worldwide network to track incoming meteoroids

Author

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

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

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

Published
2020

30. (6478) Gault: physical characterization of an active main-belt asteroid

Author

Devogèle, Maxime, primary, Ferrais, Marin, additional, Jehin, Emmanuel, additional, Moskovitz, Nicholas, additional, Skiff, Brian A, additional, Levine, Stephen E, additional, Gustafsson, Annika, additional, Farnocchia, Davide, additional, Micheli, Marco, additional, Snodgrass, Colin, additional, Borisov, Galin, additional, Manfroid, Jean, additional, Moulane, Youssef, additional, Benkhaldoun, Zouhair, additional, Burdanov, Artem, additional, Pozuelos, Francisco J, additional, Gillon, Michael, additional, de Wit, Julien, additional, Green, Simon F, additional, Bendjoya, Philippe, additional, Rivet, Jean-Pierre, additional, Abe, Luy, additional, Vernet, David, additional, Chandler, Colin Orion, additional, and Trujillo, Chadwick A, additional

Published
2021
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31. New Evidence for a Physical Link between Asteroids (155140) 2005 UD and (3200) Phaethon

Author

Devogèle, Maxime, MacLennan, Eric, Gustafsson, Annika, Moskovitz, Nicholas, Chatelain, Joey, Borisov, Galin, Abe, Shinsuke, Arai, Tomoko, Fedorets, Grigori, Ferrais, Marin, Granvik, Mikael, Jehin, Emmanuel, Siltala, Lauri, Pöntinen, Mikko, Mommert, Michael, Polishook, David, Skiff, Brian, Tanga, Paolo, Yoshida, Fumi, Devogèle, Maxime, MacLennan, Eric, Gustafsson, Annika, Moskovitz, Nicholas, Chatelain, Joey, Borisov, Galin, Abe, Shinsuke, Arai, Tomoko, Fedorets, Grigori, Ferrais, Marin, Granvik, Mikael, Jehin, Emmanuel, Siltala, Lauri, Pöntinen, Mikko, Mommert, Michael, Polishook, David, Skiff, Brian, Tanga, Paolo, and Yoshida, Fumi

Abstract

In 2018, the near-Earth object (155140) 2005 UD (hereafter UD) experienced a close fly by of the Earth. We present results from an observational campaign involving photometric, spectroscopic, and polarimetric observations carried out across a wide range of phase angles (07–88°). We also analyze archival NEOWISE observations. We report an absolute magnitude of H V = 17.51 ± 0.02 mag and an albedo of p V = 0.10 ± 0.02. UD has been dynamically linked to Phaethon due their similar orbital configurations. Assuming similar surface properties, we derived new estimates for the diameters of Phaethon and UD of D = 5.4 ± 0.5 km and D = 1.3 ± 0.1 km, respectively. Thermophysical modeling of NEOWISE data suggests a surface thermal inertia of and regolith grain size in the range of 0.9–10 mm for UD and grain sizes of 3–30 mm for Phaethon. The light curve of UD displays a symmetric shape with a reduced amplitude of Am(0) = 0.29 mag and increasing at a linear rate of 0.017 mag/° between phase angles of 0° and ~25°. Little variation in light-curve morphology was observed throughout the apparition. Using light-curve inversion techniques, we obtained a sidereal rotation period P = 5.235 ± 0.005 hr. A search for rotational variation in spectroscopic and polarimetric properties yielded negative results within observational uncertainties of ~10% μm−1 and ~16%, respectively. In this work, we present new evidence that Phaethon and UD are similar in composition and surface properties, strengthening the arguments for a genetic relationship between these two objects., Godkänd;2020;Nivå 0;2020-12-02 (alebob)

Published
2020
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32. Volume uncertainty of (7) Iris shape models from disc-resolved images

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Dudziński, Grzegorz, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Benseguane, Selma, Ferrais, Marin, Jorda, Laurent, Hanuš, Josef, Vernazza, Pierre, Rambaux, Nicolas, Carry, Benoît, Marchis, Franck, Marsset, Michaël, Viikinkoski, Matti, Brož, Miroslav, Fetick, Romain, Drouard, Alexis, Fusco, Thierry, Birlan, Mirel, Jehin, Emmanuel, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Dumas, Christophe, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, Yang, Bin, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Dudziński, Grzegorz, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Benseguane, Selma, Ferrais, Marin, Jorda, Laurent, Hanuš, Josef, Vernazza, Pierre, Rambaux, Nicolas, Carry, Benoît, Marchis, Franck, Marsset, Michaël, Viikinkoski, Matti, Brož, Miroslav, Fetick, Romain, Drouard, Alexis, Fusco, Thierry, Birlan, Mirel, Jehin, Emmanuel, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Dumas, Christophe, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, and Yang, Bin

Abstract

High angular resolution disc-resolved images of (7) Iris collected by VLT/SPHERE instrument are allowed for the detailed shape modelling of this large asteroid revealing its surface features. If (7) Iris did not suffer any events catastrophic enough to disrupt the body (which is very likely) by studying its topography, we might get insights into the early Solar system’s collisional history. When it comes to internal structure and composition, thoroughly assessing the volume and density uncertainties is necessary. In this work, we propose a method of uncertainty calculation of asteroid shape models based on light curve and adaptive optics (AO) images. We apply this method on four models of (7) Iris produced from independent Shaping Asteroids using Genetic Evolution and All-Data Asteroid Modelling inversion techniques and multiresolution photoclinometry by deformation. Obtained diameter uncertainties stem from both the observations from which the models were scaled and the models themselves. We show that despite the availability of high-resolution AO images, the volume and density of (7) Iris have substantial error bars that were underestimated in the previous studies.

Published
2020

33. Physical parameters of selected Gaia mass asteroids

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Podlewska-Gaca, Edyta, Marciniak, Anna, Alí-Lagoa, Víctor, Bartczak, Przemyslaw, Müller, Thomas G., Szakáts, Róbert, Duffard, René, Molnár, László, Pál, András, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Dziadura, Karolina, Antonini, Pierre, Asenjo, Víctor, Audejean, Maurice, Benkhaldoun, Zouhair, Behrend, Raoul, Bernasconi, Laurent, Bosch, Josep M., Chapman, Andrés, Dintinjana, Bojan, Farkas, Anikó, Ferrais, Marin, Geier, Stefan, Grice, Jonny, Hirsh, Roman, Jacquinot, Herve, Jehin, Emmanuel, Jones, A., Molina, David, Morales, Nicolás, Parley, Neil, Poncy, R., Roy, René, Santana-Ros, Toni, Seli, Bálint, Sobkowiak, Krzysztof, Verebélyi, Erika, Żukowski, K., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Podlewska-Gaca, Edyta, Marciniak, Anna, Alí-Lagoa, Víctor, Bartczak, Przemyslaw, Müller, Thomas G., Szakáts, Róbert, Duffard, René, Molnár, László, Pál, András, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Dziadura, Karolina, Antonini, Pierre, Asenjo, Víctor, Audejean, Maurice, Benkhaldoun, Zouhair, Behrend, Raoul, Bernasconi, Laurent, Bosch, Josep M., Chapman, Andrés, Dintinjana, Bojan, Farkas, Anikó, Ferrais, Marin, Geier, Stefan, Grice, Jonny, Hirsh, Roman, Jacquinot, Herve, Jehin, Emmanuel, Jones, A., Molina, David, Morales, Nicolás, Parley, Neil, Poncy, R., Roy, René, Santana-Ros, Toni, Seli, Bálint, Sobkowiak, Krzysztof, Verebélyi, Erika, and Żukowski, K.

Abstract

Context. Thanks to the Gaia mission, it will be possible to determine the masses of approximately hundreds of large main belt asteroids with very good precision. We currently have diameter estimates for all of them that can be used to compute their volume and hence their density. However, some of those diameters are still based on simple thermal models, which can occasionally lead to volume uncertainties as high as 20–30%. Aims. The aim of this paper is to determine the 3D shape models and compute the volumes for 13 main belt asteroids that were selected from those targets for which Gaia will provide the mass with an accuracy of better than 10%. Methods. We used the genetic Shaping Asteroids with Genetic Evolution (SAGE) algorithm to fit disk-integrated, dense photometric lightcurves and obtain detailed asteroid shape models. These models were scaled by fitting them to available stellar occultation and/or thermal infrared observations. Results. We determine the spin and shape models for 13 main belt asteroids using the SAGE algorithm. Occultation fitting enables us to confirm main shape features and the spin state, while thermophysical modeling leads to more precise diameters as well as estimates of thermal inertia values. Conclusions. We calculated the volume of our sample of main-belt asteroids for which the Gaia satellite will provide precise mass determinations. From our volumes, it will then be possible to more accurately compute the bulk density, which is a fundamental physical property needed to understand the formation and evolution processes of small Solar System bodies.

Published
2020

34. Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Ferrais, Marin, Vernazza, Pierre, Jorda, Laurent, Rambaux, Nicolas, Hanuš, Josef, Carry, Benoît, Marchis, Franck, Marsset, Michaël, Viikinkoski, Matti, Brož, Miroslav, Fetick, Romain, Drouard, Alexis, Fusco, Thierry, Birlan, Mirel, Podlewska-Gaca, Edyta, Jehin, Emmanuel, Bartczak, Przemyslaw, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, Yang, Bin, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Ferrais, Marin, Vernazza, Pierre, Jorda, Laurent, Rambaux, Nicolas, Hanuš, Josef, Carry, Benoît, Marchis, Franck, Marsset, Michaël, Viikinkoski, Matti, Brož, Miroslav, Fetick, Romain, Drouard, Alexis, Fusco, Thierry, Birlan, Mirel, Podlewska-Gaca, Edyta, Jehin, Emmanuel, Bartczak, Przemyslaw, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, and Yang, Bin

Abstract

Context. Asteroid (16) Psyche is the largest M-type asteroid in the main belt and the target of the NASA Psyche mission. It is also the only asteroid of this size (D > 200 km) known to be metal rich. Although various hypotheses have been proposed to explain the rather unique physical properties of this asteroid, a perfect understanding of its formation and bulk composition is still missing. Aims. We aim to refine the shape and bulk density of (16) Psyche and to perform a thorough analysis of its shape to better constrain possible formation scenarios and the structure of its interior. Methods. We obtained disk-resolved VLT/SPHERE/ZIMPOL images acquired within our ESO large program (ID 199.C-0074), which complement similar data obtained in 2018. Both data sets offer a complete coverage of Psyche’s surface. These images were used to reconstruct the three-dimensional (3D) shape of Psyche with two independent shape modeling algorithms (MPCD and ADAM). A shape analysis was subsequently performed, including a comparison with equilibrium figures and the identification of mass deficit regions. Results. Our 3D shape along with existing mass estimates imply a density of 4.20 ± 0.60 g cm−3, which is so far the highest for a solar system object following the four telluric planets. Furthermore, the shape of Psyche presents small deviations from an ellipsoid, that is, prominently three large depressions along its equator. The flatness and density of Psyche are compatible with a formation at hydrostatic equilibrium as a Jacobi ellipsoid with a shorter rotation period of ∼3h. Later impacts may have slowed down Psyche’s rotation, which is currently ∼4.2 h, while also creating the imaged depressions. Conclusions. Our results open the possibility that Psyche acquired its primordial shape either after a giant impact while its interior was already frozen or while its interior was still molten owing to the decay of the short-lived radionuclide 26Al.

Published
2020

35. Binary asteroid (31) Euphrosyne: ice-rich and nearly spherical

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Yang, Bin, Hanuš, Josef, Carry, Benoît, Vernazza, Pierre, Brož, Miroslav, Vachier, Frédéric, Rambaux, Nicolas, Marsset, Michaël, Chrenko, Ondrej, Ševeček, Pavel, Viikinkoski, Matti, Jehin, Emmanuel, Ferrais, Marin, Podlewska-Gaca, Edyta, Drouard, Alexis, Marchis, Franck, Birlan, Mirel, Benkhaldoun, Zouhair, Berthier, Jérôme, Bartczak, Przemyslaw, Dumas, Christophe, Dudziński, Grzegorz, Ďurech, Josef, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Jorda, Laurent, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Santana-Ros, Toni, Tanga, Paolo, Vigan, Arthur, Witasse, Olivier, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Yang, Bin, Hanuš, Josef, Carry, Benoît, Vernazza, Pierre, Brož, Miroslav, Vachier, Frédéric, Rambaux, Nicolas, Marsset, Michaël, Chrenko, Ondrej, Ševeček, Pavel, Viikinkoski, Matti, Jehin, Emmanuel, Ferrais, Marin, Podlewska-Gaca, Edyta, Drouard, Alexis, Marchis, Franck, Birlan, Mirel, Benkhaldoun, Zouhair, Berthier, Jérôme, Bartczak, Przemyslaw, Dumas, Christophe, Dudziński, Grzegorz, Ďurech, Josef, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, François, Fétick, Romain, Fusco, Thierry, Grice, Jonny, Jorda, Laurent, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Pajuelo, Myriam, Santana-Ros, Toni, Tanga, Paolo, Vigan, Arthur, and Witasse, Olivier

Abstract

Aims. Asteroid (31) Euphrosyne is one of the biggest objects in the asteroid main belt and it is also the largest member of its namesake family. The Euphrosyne family occupies a highly inclined region in the outer main belt and contains a remarkably large number of members, which is interpreted as an outcome of a disruptive cratering event. Methods. The goals of this adaptive-optics imaging study are threefold: to characterize the shape of Euphrosyne, to constrain its density, and to search for the large craters that may be associated with the family formation event. Results. We obtained disk-resolved images of Euphrosyne using SPHERE/ZIMPOL at the ESO 8.2 m VLT as part of our large program (ID: 199.C-0074, PI: Vernazza). We reconstructed its 3D shape via the ADAM shape modeling algorithm based on the SPHERE images and the available light curves of this asteroid. We analyzed the dynamics of the satellite with the Genoid meta-heuristic algorithm. Finally, we studied the shape of Euphrosyne using hydrostatic equilibrium models. Conclusions. Our SPHERE observations show that Euphrosyne has a nearly spherical shape with the sphericity index of 0.9888 and its surface lacks large impact craters. Euphrosyne’s diameter is 268 ± 6 km, making it one of the top ten largest main belt asteroids. We detected a satellite of Euphrosyne – S/2019 (31) 1 – that is about 4 km across, on a circular orbit. The mass determined from the orbit of the satellite together with the volume computed from the shape model imply a density of 1665 ± 242 kg m−3, suggesting that Euphrosyne probably contains a large fraction of water ice in its interior. We find that the spherical shape of Euphrosyne is a result of the reaccumulation process following the impact, as in the case of (10) Hygiea. However, our shape analysis reveals that, contrary to Hygiea, the axis ratios of Euphrosyne significantly differ from those suggested by fluid hydrostatic equilibrium following reaccumulation.

Published
2020

36. New Evidence for a Physical Link between Asteroids (155140) 2005 UD and (3200) Phaethon*

Author

Devogèle, Maxime, primary, MacLennan, Eric, additional, Gustafsson, Annika, additional, Moskovitz, Nicholas, additional, Chatelain, Joey, additional, Borisov, Galin, additional, Abe, Shinsuke, additional, Arai, Tomoko, additional, Fedorets, Grigori, additional, Ferrais, Marin, additional, Granvik, Mikael, additional, Jehin, Emmanuel, additional, Siltala, Lauri, additional, Pöntinen, Mikko, additional, Mommert, Michael, additional, Polishook, David, additional, Skiff, Brian, additional, Tanga, Paolo, additional, and Yoshida, Fumi, additional

Published
2020
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37. (6478) Gault: Physical characterization of an active main-belt asteroid

Author

Devogèle, Maxime, Ferrais, Marin, Jehin, Emmanuel, Moskovitz, Nicholas, Skiff, Brian A., Levine, Stephen E., Gustafsson, Annika, Farnocchia, Davide, Micheli, Marco, Snodgrass, Colin, Borisov, Galin, Manfroid, Jean, Moulane, Youssef, Benkhaldoun, Zouhair, Burdanov, Artem, Pozuelos, Francisco J., Gillon, Michael, de Wit, Julien, Green, Simon F., Bendjoya, Philippe, Rivet, Jean-Pierre, Abe, Luy, Vernet, David, Chandler, Colin Orion, Trujillo, Chadwick A., Devogèle, Maxime, Ferrais, Marin, Jehin, Emmanuel, Moskovitz, Nicholas, Skiff, Brian A., Levine, Stephen E., Gustafsson, Annika, Farnocchia, Davide, Micheli, Marco, Snodgrass, Colin, Borisov, Galin, Manfroid, Jean, Moulane, Youssef, Benkhaldoun, Zouhair, Burdanov, Artem, Pozuelos, Francisco J., Gillon, Michael, de Wit, Julien, Green, Simon F., Bendjoya, Philippe, Rivet, Jean-Pierre, Abe, Luy, Vernet, David, Chandler, Colin Orion, and Trujillo, Chadwick A.

Abstract

In December 2018, the main-belt asteroid (6478) Gault was reported to display activity. Gault is an asteroid belonging to the Phocaea dynamical family and was not previously known to be active, nor was any other member of the Phocaea family. In this work we present the results of photometric and spectroscopic observations that commenced soon after the discovery of activity. We obtained observations over two apparitions to monitor its activity, rotation period, composition, and possible non-gravitational orbital evolution. We find that Gault has a rotation period of P = 2.4929 ± 0.0003 hours with a lightcurve amplitude of 0.06 magnitude. This short rotation period close to the spin barrier limit is consistent with Gault having a density no smaller than ρ = 1.85 g cm−3 and its activity being triggered by the YORP spin-up mechanism. Analysis of the Gault phase curve over phase angles ranging from 0.4○ to 23.6○ provides an absolute magnitude of H = 14.81 ± 0.04, G1 = 0.25 ± 0.07, and G2 = 0.38 ± 0.04. Model fits to the phase curve find the surface regolith grain size constrained between 100-500 μm. Using relations between the phase curve and albedo we determine that the geometrical albedo of Gault is pv = 0.26 ± 0.05 corresponding to an equivalent diameter of D=2.8+0.4−0.2 km. Our spectroscopic observations are all consistent with an ordinary chondrite-like composition (S, or Q-type in the Bus-DeMeo taxonomic classification). A search through archival photographic plate surveys found previously unidentified detections of Gault dating back to 1957 and 1958. Only the latter had been digitized, which we measured to nearly double the observation arc of Gault. Finally, we did not find any signal of activity during the 2020 apparition or non-gravitational effects on its orbit.

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