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1. Scaling slowly rotating asteroids by stellar occultations

Author

Marciniak, A., Ďurech, J., Choukroun, A., Hanuš, J., Ogłoza, W., Szakáts, R., Molnár, L., Pál, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomavičienė, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K. L., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Błażewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Bąk, M. Butkiewicz, Caron, J., Casalnuovo, G., Castellani, J. J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Dróżdż, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gährken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halíř, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignácz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D. -H., Kim, M. -J., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Tóth, R. Könyves, Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczyńska, A., Kubánek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Mánek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motyliński, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakštienė, E., Pawłowski, M., Pereira, W., Perig, V., Perła, J., Pilcher, F., Podlewska-Gaca, E., Polák, J., Polakis, T., Polińska, M., Popowicz, A., Richard, F., Rives, J. J., Rodrigues, T., Rogiński, Ł., Rondón, E., Rottenborn, M., Schäfer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, Ha., Watanabe, Hi., Winiarski, M., Wróblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zelený, P., Żejmo, M., Żukowski, K., and Żywica, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

As evidenced by recent survey results, majority of asteroids are slow rotators (P>12 h), but lack spin and shape models due to selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 hours. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent. We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared data: large bodies are too bright for WISE mission. Therefore, we recently launched a campaign among stellar occultation observers, to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to stellar occultations resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, e.g. constitute a solid basis for density determinations when coupled with mass information. Spin and shape models continue to fill the gaps caused by various biases., Comment: Accepted to Astronomy & Astrophysics. 12 pages + appendices

Published
2023
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2. Asteroid spin-states of a 4 Gyr collisional family

Author

Athanasopoulos, D., Hanus, J., Avdellidou, C., Bonamico, R., Delbo, M., Conjat, M., Ferrero, A., Gazeas, K., Rivet, J. P., Sioulas, N., van Belle, G., Antonini, P., Audejean, M., Behrend, R., Bernasconi, L., Brinsfield, J. W., Brouillard, S., Brunetto, L., Fauvaud, M., Fauvaud, S., González, R., Higgins, D., Holoien, T. W. -S., Kobber, G., Koff, R. A., Kryszczynska, A., Livet, F., Marciniak, A., Oey, J., Pejcha, O., Rives, J. J., and Roy, R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Families of asteroids generated by the collisional fragmentation of a common parent body have been identified using clustering methods of asteroids in their proper orbital element space. An alternative method has been developed in order to identify collisional families from the correlation between the asteroid fragment sizes and their proper semi-major axis distance from the family centre (V-shape). This method has been shown to be effective in the cases of the very diffuse families that formed billions of years ago. We obtained photometric observations of asteroids in order to construct their rotational light curves; we combine them with the literature light curves and sparse-in-time photometry; we input these data in the light curve inversion methods to determine the shape and the spin pole of the asteroids in order to assess whether an object is prograde or retrograde. The ultimate goal is to assess whether we find an excess of retrograde asteroids on the inward side of the V-shape of a 4 Gyr asteroid family identified via the V-shape method. This excess of retrograde rotators is predicted by the theory of asteroid family evolution. We obtained the spin poles for 55 asteroids claimed to belong to a 4 Gyr collisional family of the inner main belt that consists of low-albedo asteroids. After re-evaluating the albedo and spectroscopic information, we found that nine of these asteroids are interlopers in the 4 Gyr family. Of the 46 remaining asteroids, 31 are found to be retrograde and 15 prograde. We also found that these retrograde rotators have a very low probability (1.29%) of being due to random sampling from an underlying uniform distribution of spin poles. Our results constitute corroborating evidence that the asteroids identified as members of a 4 Gyr collisional family have a common origin, thus strengthening their family membership., Comment: 20 pages, 7 figures. A&A (2022)

Published
2022
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3. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author

Marciniak, A., Ďurech, J., Alí-Lagoa, V., Ogłoza, W., Szakáts, R., Müller, T. G., Molnár, L., Pál, A., Monteiro, F., Arcoverde, P., Behrend, R., Benkhaldoun, Z., Bernasconi, L., Bosch, J., Brincat, S., Brunetto, L., Bąk, M. Butkiewicz, Del Freo, F., Duffard, R., Evangelista-Santana, M., Farroni, G., Fauvaud, S., Fauvaud, M., Ferrais, M., Geier, S., Golonka, J., Grice, J., Hirsch, R., Horbowicz, J., Jehin, E., Julien, P., Kalup, Cs., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kecskeméthy, V., Kim, D. -H., Kim, M. -J., Konstanciak, I., Krajewski, J., Kudak, V., Kulczak, P., Kundera, T., Lazzaro, D., Manzini, F., Medeiros, H., Michimani-Garcia, J., Morales, N., Nadolny, J., Oszkiewicz, D., Pakštienė, E., Pawłowski, M., Perig, V., Pilcher, F., Pinel, P., Podlewska-Gaca, E., Polakis, T., Richard, F., Rodrigues, T., Rondon, E., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Stachowski, G., Strajnic, J., Trela, P., Tychoniec, Ł., Urakawa, S., Verebelyi, E., Wagrez, K., Żejmo, M., and Żukowski, K.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Results from the TESS mission showed that previous studies strngly underestimated the number of slow rotators, revealing the importance of studying those asteroids. For most slowly rotating asteroids (P > 12), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. The goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS. In addition to data in the visible range, we also use thermal data from infrared space observatories (IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model (CITPM). This novel method has so far been applied to only a few targets, and in this work we further validate the method. We present the models of 16 slow rotators. All provide good fits to both thermal and visible data. The obtained sizes are on average accurate at the 5% precision, with diameters in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 hours, and the thermal inertia covers a wide range of values, from 2 to <400 SI units, not showing any correlation with the period. 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 do not display a previously suggested increasing trend with rotation period, which might be due to their small skin depth., Comment: Accepted to Astronomy & Astrophysics. 10 pages + appendices

Published
2021
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4. (216) Kleopatra, a low density critically rotating M-type asteroid

Author

Marchis, F., Jorda, L., Vernazza, P., Brož, M., Hanuš, J., Ferrais, M., Vachier, F., Rambaux, N., Marsset, M., Viikinkoski, M., Jehin, E., Benseguane, S., Podlewska-Gaca, E., Carry, B., Drouard, A., Fauvaud, S., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudzinski, G., Durech, J., Castillo-Rogez, J., Cipriani, F., Colas, F., Fetick, R., Fusco, T., Grice, J., Kryszczynska, A., Lamy, P., Marciniak, A., Michalowski, T., Michel, P., Pajuelo, M., Santana-Ros, T., Tanga, P., Vigan, A., Witasse, O., and Yang, B.

Subjects
Astrophysics - Earth and Planetary Astrophysics
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$^{-3}$. Such a high density implies a high metal content and 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, we aim to constrain the mass and the shape of Kleopatra with high accuracy, hence its density. Methods. We combined our new VLT/SPHERE observations of Kleopatra recorded in 2017 and 2018 with archival data, as well as lightcurve, occultation, and delay-Doppler images, to derive its 3D shape model 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 Kleopatra is very close to an equilibrium dumbbell figure with two lobes and a thick neck. Its volume equivalent diameter (118.75$\pm$1.40) km and mass (2.97$\pm$0.32) 10$^{18}$ kg imply a bulk density of (3.38$\pm$0.50) g cm$^{-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. 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. Kleopatra is a puzzling multiple system due to the unique characteristics of the primary. It deserves particular attention in the future, with the Extremely Large Telescopes and possibly a dedicated space mission., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2021
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5. An advanced multipole model for (216) Kleopatra triple system

Author

Brož, M., Marchis, F., Jorda, L., Hanuš, J., Vernazza, P., Ferrais, M., Vachier, F., Rambaux, N., Marsset, M., Viikinkoski, M., Jehin, E., Benseguane, S., Podlewska-Gaca, E., Carry, B., Drouard, A., Fauvaud, S., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudziński, G., Ďurech, J., Castillo-Rogez, J., Cipriani, F., Colas, F., Fetick, R., Fusco, T., Grice, J., Kryszczynska, A., Lamy, P., Marciniak, A., Michalowski, T., Michel, P., Pajuelo, M., Santana-Ros, T., Tanga, P., Vigan, A., Vokrouhlický, D., Witasse, O., and Yang, B.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons, orbiting an extremely irregular body and including their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. Consequently, we use a modified $N$-body integrator, which was significantly extended to include the multipole expansion of the gravitational field up to the order $\ell = 10$. Its convergence was verified against the `brute-force' algorithm. We computed the coefficients $C_{\ell m},S_{\!\ell m}$ for Kleopatra's shape, assuming a~constant bulk density. For solar-system applications, it was also necessary to implement a variable distance and geometry of observations. Our $\chi^2$ metric then accounts for the absolute astrometry, the relative astrometry (2nd moon with respect to 1st), angular velocities, and also silhouettes, constraining the pole orientation. This allowed us to derive the orbital elements of Kleopatra's two moons. Using both archival astrometric data and new VLT/SPHERE observations (ESO LP 199.C-0074), we were able to identify the true periods of the moons, $P_1 = (1.822359\pm0.004156)\,{\rm d}$, $P_2 = (2.745820\pm0.004820)\,{\rm d}$. They orbit very close to the 3:2 mean-motion resonance, but their osculating eccentricities are too small compared to other perturbations (multipole, mutual), so that regular librations of the critical argument are not present. The resulting mass of Kleopatra, $m_1 = (1.49\pm0.16)\cdot10^{-12}\,M_\odot$ or $2.97\cdot10^{18}\,{\rm kg}$, is significantly lower than previously thought. An implication explained in the accompanying paper (Marchis et al.) is that (216) Kleopatra is a critically rotating body., Comment: accepted in A&A

Published
2021
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6. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author

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

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

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

Published
2019
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7. The homogeneous internal structure of CM-like asteroid (41) Daphne

Author

Carry, B., Vachier, F., Berthier, J., Marsset, M., Vernazza, P., Grice, J., Merline, W. J., Lagadec, E., Fienga, A., Conrad, A., Podlewska-Gaca, E., Santana-Ros, T., Viikinkoski, M., Hanuš, J., Dumas, C., Drummond, J. D., Tamblyn, P. M., Chapman, C. R., Behrend, R., Bernasconi, L., Bartczak, P., Benkhaldoun, Z., Birlan, M., Castillo-Rogez, J., Cipriani, F., Colas, F., Drouard, A., Ďurech, J., Enke, B. L., Fauvaud, S., Ferrais, M., Fetick, R., Fusco, T., Gillon, M., Jehin, E., Jorda, L., Kaasalainen, M., Keppler, M., Kryszczynska, A., Lamy, P., Marchis, F., Marciniak, A., Michalowski, T., Michel, P., Pajuelo, M., Tanga, P., Vigan, A., Warner, B., Witasse, O., Yang, B., and Zurlo, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. CM-like asteroids (Ch and Cgh classes) are a major population within the broader C-complex, encompassing about 10% of the mass of the main asteroid belt. Their internal structure has been predicted to be homogeneous, based on their compositional similarity as inferred from spectroscopy (Vernazza et al., 2016, AJ 152, 154) and numerical modeling of their early thermal evolution (Bland & Travis, 2017, Sci. Adv. 3, e1602514). Aims. Here we aim to test this hypothesis by deriving the density of the CM-like asteroid (41) Daphne from detailed modeling of its shape and the orbit of its small satellite. Methods. We observed Daphne and its satellite within our imaging survey with the Very Large Telescope extreme adaptive-optics SPHERE/ZIMPOL camera (ID 199.C-0074, PI P. Vernazza) and complemented this data set with earlier Keck/NIRC2 and VLT/NACO observations. We analyzed the dynamics of the satellite with our Genoid meta-heuristic algorithm. Combining our high-angular resolution images with optical lightcurves and stellar occultations, we determine the spin period, orientation, and 3-D shape, using our ADAM shape modeling algorithm. Results. The satellite orbits Daphne on an equatorial, quasi-circular, prograde orbit, like the satellites of many other large main-belt asteroids. The shape model of Daphne reveals several large flat areas that could be large impact craters. The mass determined from this orbit combined with the volume computed from the shape model implies a density for Daphne of 1.77+/-0.26 g/cm3 (3 {\sigma}). This density is consistent with a primordial CM-like homogeneous internal structure with some level of macroporosity (~17%). Conclusions. Based on our analysis of the density of Daphne and 75 other Ch/Cgh-type asteroids gathered from the literature, we conclude that the primordial internal structure of the CM parent bodies was homogeneous.

Published
2019
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8. Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites

Author

Pajuelo, M., Carry, B., Vachier, F., Marsset, M., Berthier, J., Descamps, P., Merline, W. J., Tamblyn, P. M., Grice, J., Conrad, A., Storrs, A., Timerson, B., Dunham, D., Preston, S., Vigan, A., Yang, B., Vernazza, P., Fauvaud, S., Bernasconi, L., Romeuf, D., Behrend, R., Dumas, C., Drummond, J. D., Margot, J. -L., Kervella, P., Marchis, F., and Girard, J. H.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The population of large asteroids is thought to be primordial and they are the most direct witnesses of the early history of our Solar System. Those satellites allow study of the mass, and hence density and internal structure. We study here the properties of the triple asteroid (107) Camilla from lightcurves, stellar occultations, optical spectroscopy, and high-contrast and high-angular-resolution images and spectro-images. Using 80 positions over 15 years, we determine the orbit of its larger satellite to be circular, equatorial, and prograde, with RMS residuals of 7.8 mas. From 11 positions in three epochs only, in 2015 and 2016, we determine a preliminary orbit for the second satellite. We find the orbit to be somewhat eccentric and slightly inclined to the primary's equatorial plane, reminiscent of the inner satellites of other asteroid triple systems. Comparison of the near-infrared spectrum of the larger satellite reveals no significant difference with Camilla. Hence, these properties argue for a formation of the satellites by excavation from impact and re-accumulation of ejecta. We determine the spin and 3-D shape of Camilla. The model fits well each data set. We determine Camilla to be larger than reported from modeling of mid-infrared photometry, with a spherical-volume-equivalent diameter of 254 $\pm$ 36 km (3 $\sigma$ uncertainty), in agreement with recent results from shape modeling (Hanus2017+). Combining the mass of (1.12 $\pm$ 0.01) $\times$ 10$^{19}$ kg determined from the dynamics of the satellites and the volume from the 3-D shape model, we determine a density of 1,280 $\pm$ 130 SI. From this density, and considering Camilla's spectral similarities with (24) Themis and (65) Cybele (for which water ice coating on surface grains was reported), we infer a silicate-to-ice mass ratio of 1-6, with a 10-30% macroporosity., Comment: 40 pages, 16 figures, accepted for publication

Published
2018
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9. Against the biases in spins and shapes of asteroids

Author

Marciniak, A., Pilcher, F., Oszkiewicz, D., Santana-Ros, T., Urakawa, S., Fauvaud, S., Kankiewicz, P., Tychoniec, Ł., Fauvaud, M., Hirsch, R., Horbowicz, J., Kamiński, K., Konstanciak, I., Kosturkiewicz, E., Murawiecka, M., Nadolny, J., Nishiyama, K., Okumura, S., Polińska, M., Richard, F., Sakamoto, T., Sobkowiak, K., Stachowski, G., and Trela, P.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Physical studies of asteroids depend on an availability of lightcurve data. Targets that are easy to observe and analyse naturally have more data available, so their synodic periods are confirmed from multiple sources. Also, thanks to availability of data from a number of apparitions, their spin and shape models can often be obtained. Almost half of bright (H<=11 mag) main-belt asteroid population with known lightcurve parameters have rotation periods considered long (P>12 hours) and are rarely chosen for photometric observations. There is a similar selection effect against asteroids with low lightcurve amplitudes (a_max<=0.25 mag). As a result such targets, though numerous in this brightness range, are underrepresented in the sample of spin and shape modelled asteroids. In the range of fainter targets such effects are stronger. These selection effects can influence what is now known about asteroid spin vs. size distribution, on asteroid internal structure and densities and on spatial orientation of asteroid spin axes. To reduce both biases at the same time, we started a photometric survey of a substantial sample of those bright main-belt asteroids that displayed both features: periods longer than 12 hours, and amplitudes that did not exceed 0.25 magnitude. First we aim at finding synodic periods of rotation, and after a few observed apparitions, obtaining spin and shape models. As an initial result of our survey we found that a quarter of the studied sample (8 out of 34 targets) have rotation periods different from those widely accepted. We publish here these newly found period values with the lightcurves. The size/frequency plot might in reality look different in the long-period range. Further studies of asteroid spins, shapes, and structure should take into account serious biases that are present in the parameters available today., Comment: Published in Planetary and Space Science. 13 pages, 20 figures

Published
2017
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10. Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Author

Marciniak, A., Bartczak, P., Müller, T., Sanabria, J. J., Alí-Lagoa, V., Antonini, P., Behrend, R., Bernasconi, L., Bronikowska, M., Bąk, M. Butkiewicz, Cikota, A., Crippa, R., Ditteon, R., Dudziński, G., Duffard, R., Dziadura, K., Fauvaud, S., Geier, S., Hirsch, R., Horbowicz, J., Hren, M., Jerosimic, L., Kamiński, K., Kankiewicz, P., Konstanciak, I., Korlevic, P., Kosturkiewicz, E., Kudak, V., Manzini, F., Morales, N., Murawiecka, M., Ogłoza, W., Oszkiewicz, D., Pilcher, F., Polakis, T., Poncy, R., Santana-Ros, T., Siwak, M., Skiff, B., Sobkowiak, K., Stoss, R., Żejmo, M., and Żukowski, K.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The available set of spin and shape modelled asteroids is strongly biased against slowly rotating targets and those with low lightcurve amplitudes. As a consequence of these selection effects, the current picture of asteroid spin axis distribution, rotation rates, or radiometric properties, might be affected too. To counteract these selection effects, we are running a photometric campaign of a large sample of main belt asteroids omitted in most previous studies. We determined synodic rotation periods and verified previous determinations. When a dataset for a given target was sufficiently large and varied, we performed spin and shape modelling with two different methods. We used the convex inversion method and the non-convex SAGE algorithm, applied on the same datasets of dense lightcurves. Unlike convex inversion, the SAGE method allows for the existence of valleys and indentations on the shapes based only on lightcurves. We obtained detailed spin and shape models for the first five targets of our sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487) Venetia. When compared to stellar occultation chords, our models obtained an absolute size scale and major topographic features of the shape models were also confirmed. When applied to thermophysical modelling, they provided a very good fit to the infrared data and allowed their size, albedo, and thermal inertia to be determined. Convex and non-convex shape models provide comparable fits to lightcurves. However, some non-convex models fit notably better to stellar occultation chords and to infrared data in sophisticated thermophysical modelling (TPM). In some cases TPM showed strong preference for one of the spin and shape solutions. Also, we confirmed that slowly rotating asteroids tend to have higher-than-average values of thermal inertia., Comment: Accepted in astronomy astrophys. 39 pages, 49 figures

Published
2017
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11. Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites

Author

Pajuelo, M, Carry, B, Vachier, F, Marsset, M, Berthier, J, Descamps, P, Merline, WJ, Tamblyn, PM, Grice, J, Conrad, A, Storrs, A, Timerson, B, Dunham, D, Preston, S, Vigan, A, Yang, B, Vernazza, P, Fauvaud, S, Bernasconi, L, Romeuf, D, Behrend, R, Dumas, C, Drummond, JD, Margot, J-L, Kervella, P, Marchis, F, and Girard, JH

Subjects
Space Sciences, Physical Sciences, Asteroids, Composition, Satellites of asteroids, Photometry, Spectroscopy, astro-ph.EP, Astronomical and Space Sciences, Geochemistry, Geophysics, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract

The population of large asteroids is thought to be primordial and they arethe most direct witnesses of the early history of our Solar System. Thosesatellites allow study of the mass, and hence density and internal structure.We study here the properties of the triple asteroid (107) Camilla fromlightcurves, stellar occultations, optical spectroscopy, and high-contrast andhigh-angular-resolution images and spectro-images. Using 80 positions over 15years, we determine the orbit of its larger satellite to be circular,equatorial, and prograde, with RMS residuals of 7.8 mas. From 11 positions inthree epochs only, in 2015 and 2016, we determine a preliminary orbit for thesecond satellite. We find the orbit to be somewhat eccentric and slightlyinclined to the primary's equatorial plane, reminiscent of the inner satellitesof other asteroid triple systems. Comparison of the near-infrared spectrum ofthe larger satellite reveals no significant difference with Camilla. Hence,these properties argue for a formation of the satellites by excavation fromimpact and re-accumulation of ejecta. We determine the spin and 3-D shape ofCamilla. The model fits well each data set. We determine Camilla to be largerthan reported from modeling of mid-infrared photometry, with aspherical-volume-equivalent diameter of 254 $\pm$ 36 km (3 $\sigma$uncertainty), in agreement with recent results from shape modeling(Hanus2017+). Combining the mass of (1.12 $\pm$ 0.01) $\times$ 10$^{19}$ kgdetermined from the dynamics of the satellites and the volume from the 3-Dshape model, we determine a density of 1,280 $\pm$ 130 SI. From this density,and considering Camilla's spectral similarities with (24) Themis and (65)Cybele (for which water ice coating on surface grains was reported), we infer asilicate-to-ice mass ratio of 1-6, with a 10-30% macroporosity.

Published
2018

12. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author

Hanuš, J., Ďurech, J., Oszkiewicz, D. A., Behrend, R., Carry, B., Delbo', M., Adam, O., Afonina, V., Anquetin, R., Antonini, P., Arnold, L., Audejean, M., Aurard, P., Bachschmidt, M., Badue, B., Barbotin, E., Barroy, P., Baudouin, P., Berard, L., Berger, N., Bernasconi, L., Bosch, J-G., Bouley, S., Bozhinova, I., Brinsfield, J., Brunetto, L., Canaud, G., Caron, J., Carrier, F., Casalnuovo, G., Casulli, S., Cerda, M., Chalamet, L., Charbonnel, S., Chinaglia, B., Cikota, A., Colas, F., Coliac, J-F., Collet, A., Coloma, J., Conjat, M., Conseil, E., Costa, R., Crippa, R., Cristofanelli, M., Damerdji, Y., Debackere, A., Decock, A., Déhais, Q., Déléage, T., Delmelle, S., Demeautis, C., Dróżdż, M., Dubos, G., Dulcamara, T., Dumont, M., Durkee, R., Dymock, R., del Valle, A. Escalante, Esseiva, N., Esseiva, R., Esteban, M., Fauchez, T., Fauerbach, M., Fauvaud, M., Fauvaud, S., Forné, E., Fournel, C., Fradet, D., Garlitz, J., Gerteis, O., Gillier, C., Gillon, M., Giraud, R., Godard, J-P., Goncalves, R., Hamanowa, H., Hay, K., Hellmich, S., Heterier, S., Higgins, D., Hirsch, R., Hodosan, G., Hren, M., Hygate, A., Innocent, N., Jacquinot, H., Jawahar, S., Jehin, E., Jerosimic, L., Klotz, A., Koff, W., Korlevic, P., Kosturkiewicz, E., Krafft, P., Krugly, Y., Kugel, F., Labrevoir, O., Lecacheux, J., Lehký, M., Leroy, A., Lesquerbault, B., Lopez-Gonzales, M. J., Lutz, M., Mallecot, B., Manfroid, J., Manzini, F., Marciniak, A., Martin, A., Modave, B., Montaigut, R., Montier, J., Morelle, E., Morton, B., Mottola, S., Naves, R., Nomen, J., Oey, J., Ogłoza, W., Paiella, M., Pallares, H., Peyrot, A., Pilcher, F., Pirenne, J-F., Piron, P., Polinska, M., Polotto, M., Poncy, R., Previt, J. P., Reignier, F., Renauld, D., Ricci, D., Richard, F., Rinner, C., Risoldi, V., Robilliard, D., Romeuf, D., Rousseau, G., Roy, R., Ruthroff, J., Salom, P. A., Salvador, L., Sanchez, S., Santana-Ros, T., Scholz, A., Séné, G., Skiff, B., Sobkowiak, K., Sogorb, P., Soldán, F., Spiridakis, A., Splanska, E., Sposetti, S., Starkey, D., Stephens, R., Stiepen, A., Stoss, R., Strajnic, J., Teng, J-P., Tumolo, G., Vagnozzi, A., Vanoutryve, B., Vugnon, J. M., Warner, B. D., Waucomont, M., Wertz, O., Winiarski, M., and Wolf, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. This amount already provided a deep insight into physical properties of main-belt asteroids or large collisional families. We aim to increase the number of asteroid shape models and rotation states. Such results are an important input for various further studies such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides, in combination with known masses, bulk density estimates, but constrains also theoretical collisional and evolutional models of the Solar System. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as an input for the convex inversion method, and derive 3D shape models of asteroids, together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that one hundred observers who submit their optical data to publicly available databases. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature or their masses will be most likely determined from their gravitational influence on smaller bodies, which orbital deflection will be observed by the ESA Gaia astrometric mission. This was achieved by using additional optical data from recent apparitions for the shape optimization. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and 3 near-Earth asteroids., Comment: Accepted for publication in A&A

Published
2015
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13. The small binary asteroid (939) Isberga

Author

Carry, B., Matter, A., Scheirich, P., Pravec, P., Molnar, L., Mottola, S., Carbognani, A., Jehin, E., Marciniak, A., Binzel, R. P., DeMeo, F. E., Birlan, M., Delbo, M., Barbotin, E., Behrend, R., Bonnardeau, M., Colas, F., Farissier, P., Fauvaud, M., Fauvaud, S., Gillier, C., Gillon, M., Hellmich, S., Hirsch, R., Leroy, A., Manfroid, J., Montier, J., Morelle, E., Richard, F., Sobkowiak, K., Strajnic, J., and Vachier, F.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In understanding the composition and internal structure of asteroids, their density is perhaps the most diagnostic quantity. We aim here to characterize the surface composition, mutual orbit, size, mass, and density of the small main-belt binary asteroid (939) Isberga. For that, we conduct a suite of multi-technique observations, including optical lightcurves over many epochs, near-infrared spectroscopy, and interferometry in the thermal infrared. We develop a simple geometric model of binary systems to analyze the interferometric data in combination with the results of the lightcurve modeling. From spectroscopy, we classify Ibserga as a Sq-type asteroid, consistent with the albedo of 0.14$^{+0.09}_{-0.06}$ (all uncertainties are reported as 3-$\sigma$ range) we determine (average albedo of S-types is 0.197 $\pm$ 0.153, Pravec et al., 2012, Icarus 221, 365-387). Lightcurve analysis reveals that the mutual orbit has a period of 26.6304 $\pm$ 0.0001 h, is close to circular, and has pole coordinates within 7 deg. of (225, +86) in ECJ2000, implying a low obliquity of 1.5 deg. The combined analysis of lightcurves and interferometric data allows us to determine the dimension of the system and we find volume-equivalent diameters of 12.4$^{+2.5}_{-1.2}$ km and 3.6$^{+0.7}_{-0.3}$ km for Isberga and its satellite, circling each other on a 33 km wide orbit. Their density is assumed equal and found to be $2.91^{+1.72}_{-2.01}$ g.cm$^{-3}$, lower than that of the associated ordinary chondrite meteorites, suggesting the presence of some macroporosity, but typical of S-types of the same size range (Carry, 2012, P\&SS 73, 98-118). The present study is the first direct measurement of the size of a small main-belt binary. Although the interferometric observations of Isberga are at the edge of MIDI capabilities, the method described here is applicable to others suites of instruments (e.g, LBT, ALMA)., Comment: 12 pages, 6 figures, 4 tables

Published
2014
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14. Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author

Hanuš, J., Ďurech, J., Brož, M., Marciniak, A., Warner, B. D., Pilcher, F., Stephens, R., Behrend, R., Carry, B., Čapek, D., Antonini, P., Audejean, M., Augustesen, K., Barbotin, E., Baudouin, P., Bayol, A., Bernasconi, L., Borczyk, W., Bosch, J. -G., Brochard, E., Brunetto, L., Casulli, S., Cazenave, A., Charbonnel, S., Christophe, B., Colas, F., Coloma, J., Conjat, M., Cooney, W., Correira, H., Cotrez, V., Coupier, A., Crippa, R., Cristofanelli, M., Dalmas, Ch., Danavaro, C., Demeautis, C., Droege, T., Durkee, R., Esseiva, N., Esteban, M., Fagas, M., Farroni, G., Fauvaud, M., Fauvaud, S., Del Freo, F., Garcia, L., Geier, S., Godon, C., Grangeon, K., Hamanowa, H., Heck, N., Hellmich, S., Higgins, D., Hirsch, R., Husarik, M., Itkonen, T., Jade, O., Kamiński, K., Kankiewicz, P., Klotz, A., Koff, R. A., Kryszczyńska, A., Kwiatkowski, T., Laffont, A., Leroy, A., Lecacheux, J., Leonie, Y., Leyrat, C., Manzini, F., Martin, A., Masi, G., Matter, D., Michałowski, J., Michałowski, M. J., Michałowski, T., Michelet, J., Michelsen, R., Morelle, E., Mottola, S., Naves, R., Nomen, J., Oey, J., Ogloza, W., Oksanen, A., Oszkiewicz, D., Pääkkönen, P., Paiella, M., Pallares, H., Paulo, J., Pavic, M., Payet, B., Polińska, M., Polishook, D., Poncy, R., Revaz, Y., Rinner, C., Rocca, M., Roche, A., Romeuf, D., Roy, R., Saguin, H., Salom, P. A., Sanchez, S., Santacana, G., Santana-Ros, T., Sareyan, J. -P., Sobkowiak, K., Sposetti, S., Starkey, D., Stoss, R., Strajnic, J., Teng, J. -P., Tregon, B., Vagnozzi, A., Velichko, F. P., Waelchli, N., Wagrez, K., and Wücher, H.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6., Comment: Accepted for publication in A&A, January 15, 2013

Published
2013
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15. Spectroscopy of BL Cam - Observations

Author

Alvarez, M., Michel, R., Fox-Machado, L., Sareyan, J. P., Fauvaud, S., and Tovmassian, G.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The star BL Camelopardalis (GD 428, GSC 04067-00471, V=12.92, B=13.1), is a SX Phoenicis pulsating variable showing a high amplitude variability (300-350 mmag), with a very clear period of 56.3 min, that has being recently studied by Fauvaud et al. (2010). They show that the observed variability is due to a clear and single pulsation, as expected for these type of pulsators. It was discovered as a variable star on 1976 by Berg and Duthie (1977)., Comment: 1 page, 1 figure, to appear in proceedings of XIII Latin American Regional IAU Meeting, Morelia-Michoacan, Mexico 2010, RevMexAA(SC)

Published
2011

16. The field high-amplitude SX Phe variable BL Cam: results from a multisite photometric campaign. II. Evidence of a binary - possibly triple - system

Author

Fauvaud, S., Sareyan, J. -P., Ribas, I., Rodríguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, J. H., Wolf, M., Santacana, G., Zhou, A. -Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., López-González, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. -J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Král, L., Kocián, R., Kučáková, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. -M., Kotková, L., Truparová, K., Ulusoy, C., Yasarsoy, B., Avdibegovic, A., Blauzek, M., Kliner, J., Zasche, P., Bartošíková, S., Vilášek, M., Trondal, O., Abbeel, F. Van Den, Behrend, R., and Wücher, H.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Short-period high-amplitude pulsating stars of Population I ($\delta$ Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational behaviours, only one or two radial modes being excited. Nevertheless, BL Cam is a unique object among them, being an extreme metal-deficient field high-amplitude SX Phe variable with a large number of frequencies. Based on a frequency analysis, a pulsational interpretation was previously given. aims heading (mandatory) We attempt to interpret the long-term behaviour of the residuals that were not taken into account in the previous Observed-Calculated (O-C) short-term analyses. methods heading (mandatory) An investigation of the O-C times has been carried out, using a data set based on the previous published times of light maxima, largely enriched by those obtained during an intensive multisite photometric campaign of BL Cam lasting several months. results heading (mandatory) In addition to a positive (161 $\pm$ 3) x 10$^{-9}$ yr$^{-1}$ secular relative increase in the main pulsation period of BL Cam, we detected in the O-C data short- (144.2 d) and long-term ($\sim$ 3400 d) variations, both incompatible with a scenario of stellar evolution. conclusions heading (mandatory) Interpreted as a light travel-time effect, the short-term O-C variation is indicative of a massive stellar component (0.46 to 1 M$_{\sun}$) with a short period orbit (144.2 d), within a distance of 0.7 AU from the primary. More observations are needed to confirm the long-term O-C variations: if they were also to be caused by a light travel-time effect, they could be interpreted in terms of a third component, in this case probably a brown dwarf star ($\geq$ 0.03 \ M$_{\sun}$), orbiting in $\sim$ 3400 d at a distance of 4.5 AU from the primary., Comment: 7 pages, 5 figures, accepted for publication in A&A

Published
2010
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17. A Giant Crater on 90 Antiope?

Author

Descamps, P., Marchis, F., Michalowski, T., Berthier, J., Pollock, J., Wiggins, P., Birlan, M., Colas, F., Vachier, F., Fauvaud, S., Fauvaud, M., Sareyan, J. -P., Pilcher, F., and Klinglesmith, D. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Mutual event observations between the two components of 90 Antiope were carried out in 2007-2008. The pole position was refined to lambda0 = 199.5+/-0.5 eg and beta0 = 39.8+/-5 deg in J2000 ecliptic coordinates, leaving intact the physical solution for the components, assimilated to two perfect Roche ellipsoids, and derived after the 2005 mutual event season (Descamps et al., 2007). Furthermore, a large-scale geological depression, located on one of the components, was introduced to better match the observed lightcurves. This vast geological feature of about 68 km in diameter, which could be postulated as a bowl-shaped impact crater, is indeed responsible of the photometric asymmetries seen on the "shoulders" of the lightcurves. The bulk density was then recomputed to 1.28+/-0.04 gcm-3 to take into account this large-scale non-convexity. This giant crater could be the aftermath of a tremendous collision of a 100-km sized proto-Antiope with another Themis family member. This statement is supported by the fact that Antiope is sufficiently porous (~50%) to survive such an impact without being wholly destroyed. This violent shock would have then imparted enough angular momentum for fissioning of proto-Antiope into two equisized bodies. We calculated that the impactor must have a diameter greater than ~17 km, for an impact velocity ranging between 1 and 4 km/s. With such a projectile, this event has a substantial 50% probability to have occurred over the age of the Themis family., Comment: 30 pages, 3 Tables, 8 Figures. Accepted for publication in Icarus

Published
2009
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18. Scaling slowly rotating asteroids with stellar occultations

Author

Marciniak, A., primary, Ďurech, J., additional, Choukroun, A., additional, Hanuš, J., additional, Ogłoza, W., additional, Szakáts, R., additional, Molnár, L., additional, Pál, A., additional, Monteiro, F., additional, Frappa, E., additional, Beisker, W., additional, Pavlov, H., additional, Moore, J., additional, Adomavičienė, R., additional, Aikawa, R., additional, Andersson, S., additional, Antonini, P., additional, Argentin, Y., additional, Asai, A., additional, Assoignon, P., additional, Barton, J., additional, Baruffetti, P., additional, Bath, K. L., additional, Behrend, R., additional, Benedyktowicz, L., additional, Bernasconi, L., additional, Biguet, G., additional, Billiani, M., additional, Błażewicz, D., additional, Boninsegna, R., additional, Borkowski, M., additional, Bosch, J., additional, Brazill, S., additional, Bronikowska, M., additional, Bruno, A., additional, Butkiewicz-Bąk, M., additional, Caron, J., additional, Casalnuovo, G., additional, Castellani, J. J., additional, Ceravolo, P., additional, Conjat, M., additional, Delincak, P., additional, Delpau, J., additional, Demeautis, C., additional, Demirkol, A., additional, Dróżdż, M., additional, Duffard, R., additional, Durandet, C., additional, Eisfeldt, D., additional, Evangelista, M., additional, Fauvaud, S., additional, Fauvaud, M., additional, Ferrais, M., additional, Filipek, M., additional, Fini, P., additional, Fukui, K., additional, Gährken, B., additional, Geier, S., additional, George, T., additional, Goffin, B., additional, Golonka, J., additional, Goto, T., additional, Grice, J., additional, Guhl, K., additional, Halíř, K., additional, Hanna, W., additional, Harman, M., additional, Hashimoto, A., additional, Hasubick, W., additional, Higgins, D., additional, Higuchi, M., additional, Hirose, T., additional, Hirsch, R., additional, Hofschulz, O., additional, Horaguchi, T., additional, Horbowicz, J., additional, Ida, M., additional, Ignácz, B., additional, Ishida, M., additional, Isobe, K., additional, Jehin, E., additional, Joachimczyk, B., additional, Jones, A., additional, Juan, J., additional, Kamiński, K., additional, Kamińska, M. K., additional, Kankiewicz, P., additional, Kasebe, H., additional, Kattentidt, B., additional, Kim, D.-H., additional, Kim, M.-J., additional, Kitazaki, K., additional, Klotz, A., additional, Komraus, M., additional, Konstanciak, I., additional, Könyves-Tóth, R., additional, Kouno, K., additional, Kowald, E., additional, Krajewski, J., additional, Krannich, G., additional, Kreutzer, A., additional, Kryszczyńska, A., additional, Kubánek, J., additional, Kudak, V., additional, Kugel, F., additional, Kukita, R., additional, Kulczak, P., additional, Lazzaro, D., additional, Licandro, J., additional, Livet, F., additional, Maley, P., additional, Manago, N., additional, Mánek, J., additional, Manna, A., additional, Matsushita, H., additional, Meister, S., additional, Mesquita, W., additional, Messner, S., additional, Michelet, J., additional, Michimani, J., additional, Mieczkowska, I., additional, Morales, N., additional, Motyliński, M., additional, Murawiecka, M., additional, Newman, J., additional, Nikitin, V., additional, Nishimura, M., additional, Oey, J., additional, Oszkiewicz, D., additional, Owada, M., additional, Pakštienė, E., additional, Pawłowski, M., additional, Pereira, W., additional, Perig, V., additional, Perła, J., additional, Pilcher, F., additional, Podlewska-Gaca, E., additional, Polák, J., additional, Polakis, T., additional, Polińska, M., additional, Popowicz, A., additional, Richard, F., additional, Rives, J. J, additional, Rodrigues, T., additional, Rogiński, Ł., additional, Rondón, E., additional, Rottenborn, M., additional, Schäfer, R., additional, Schnabel, C., additional, Schreurs, O., additional, Selva, A., additional, Simon, M., additional, Skiff, B., additional, Skrutskie, M., additional, Skrzypek, J., additional, Sobkowiak, K., additional, Sonbas, E., additional, Sposetti, S., additional, Stuart, P., additional, Szyszka, K., additional, Terakubo, K., additional, Thomas, W., additional, Trela, P., additional, Uchiyama, S., additional, Urbanik, M., additional, Vaudescal, G., additional, Venable, R., additional, Watanabe, Ha., additional, Watanabe, Hi., additional, Winiarski, M., additional, Wróblewski, R., additional, Yamamura, H., additional, Yamashita, M., additional, Yoshihara, H., additional, Zawilski, M., additional, Zelený, P., additional, Żejmo, M., additional, Żukowski, K., additional, and Żywica, S., additional

Published
2023
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19. Against the biases in spins and shapes of asteroids

Author

Marciniak, A., Pilcher, F., Oszkiewicz, D., Santana-Ros, T., Urakawa, S., Fauvaud, S., Kankiewicz, P., Tychoniec, Ł., Fauvaud, M., Hirsch, R., Horbowicz, J., Kamiński, K., Konstanciak, I., Kosturkiewicz, E., Murawiecka, M., Nadolny, J., Nishiyama, K., Okumura, S., Polińska, M., Richard, F., Sakamoto, T., Sobkowiak, K., Stachowski, G., and Trela, P.

Published
2015
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20. The small binary asteroid (939) Isberga

Author

Carry, B., Matter, A., Scheirich, P., Pravec, P., Molnar, L., Mottola, S., Carbognani, A., Jehin, E., Marciniak, A., Binzel, R.P., DeMeo, F.E., Birlan, M., Delbo, M., Barbotin, E., Behrend, R., Bonnardeau, M., Colas, F., Farissier, P., Fauvaud, M., Fauvaud, S., Gillier, C., Gillon, M., Hellmich, S., Hirsch, R., Leroy, A., Manfroid, J., Montier, J., Morelle, E., Richard, F., Sobkowiak, K., Strajnic, J., and Vachier, F.

Published
2015
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21. Asteroid spin-states of a 4 Gyr collisional family

Author

Athanasopoulos, D., primary, Hanuš, J., additional, Avdellidou, C., additional, Bonamico, R., additional, Delbo, M., additional, Conjat, M., additional, Ferrero, A., additional, Gazeas, K., additional, Rivet, J. P., additional, Sioulas, N., additional, van Belle, G., additional, Antonini, P., additional, Audejean, M., additional, Behrend, R., additional, Bernasconi, L., additional, Brinsfield, J. W., additional, Brouillard, S., additional, Brunetto, L., additional, Fauvaud, M., additional, Fauvaud, S., additional, Gonzalez, R., additional, Higgins, D., additional, Holoien, T. W.-S., additional, Kober, G., additional, Koff, R. A., additional, Kryszczynska, A., additional, Livet, F., additional, Marciniak, A., additional, Oey, J., additional, Pejcha, O., additional, Rives, J. J., additional, and Roy, R., additional

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

Author

Ferrais, M., primary, Jorda, L., additional, Vernazza, P., additional, Carry, B., additional, Brož, M., additional, Rambaux, N., additional, Hanuš, J., additional, Dudziński, G., additional, Bartczak, P., additional, Vachier, F., additional, Aristidi, E., additional, Beck, P., additional, Marchis, F., additional, Marsset, M., additional, Viikinkoski, M., additional, Fetick, R., additional, Drouard, A., additional, Fusco, T., additional, Birlan, M., additional, Podlewska-Gaca, E., additional, Burbine, T. H., additional, Dyar, M. D., additional, Bendjoya, P., additional, Benkhaldoun, Z., additional, Berthier, J., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Colas, F., additional, Dumas, C., additional, Ďurech, J., additional, Fauvaud, S., additional, Grice, J., additional, Jehin, E., additional, Kaasalainen, M., additional, Kryszczynska, A., additional, Lamy, P., additional, Le Coroller, H., additional, Marciniak, A., additional, Michalowski, T., additional, Michel, P., additional, Prieur, J.-L., additional, Reddy, V., additional, Rivet, J.-P., additional, Santana-Ros, T., additional, Scardia, M., additional, Tanga, P., additional, Vigan, A., additional, Witasse, O., additional, and Yang, B., additional

Published
2022
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23. VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis

Author

Brož, M., Marchis, F., Jorda, L., Hanuš, J., Vernazza, P., Ferrais, M., Vachier, F., Rambaux, N., Marsset, M., Viikinkoski, M., Jehin, E., Benseguane, S., Podlewska-Gaca, E., Carry, B., Drouard, A., Fauvaud, S., Birlan, M., Berthier, J., Bartczak, P., Dumas, C., Dudziński, G., Ďurech, J., Castillo-Rogez, J., Cipriani, F., Colas, F., Fetick, R., Fusco, T., Grice, J., Kryszczynska, A., Lamy, P., Marciniak, A., Michalowski, T., Michel, Patrick, Pajuelo, M., Santana-Ros, T., Tanga, P., Vigan, A., Vokrouhlický, D., Witasse, O., Yang, B., Neveu, M., Beck, P., Kaasalainen, M., Le Coroller, H., Antonini, P., Audejean, M., Aurard, P., Behrend, R., Benkhaldoun, Z., Bosch, J., Chapman, A., Dalmon, L., Hamanowa, Hiroko, Hamanowa, Hiromi, His, J., Jones, A., Kim, D.-H., Kim, M.-J., Krajewski, J., Labrevoir, O., Leroy, A., Livet, F., Molina, D., Montaigut, R., Oey, J., Payre, N., Reddy, V., Sabin, P., Sanchez, A., Socha, L., and Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; Context. Until recently, the 3D shape, and therefore density (when combining the volume estimate with available mass estimates), and surface topography of the vast majority of the largest ( D ≥ 100 km) main-belt asteroids have remained poorly constrained. The improved capabilities of the SPHERE/ZIMPOL instrument have opened new doors into ground-based asteroid exploration. Aims. To constrain the formation and evolution of a representative sample of large asteroids, we conducted a high-angular-resolution imaging survey of 42 large main-belt asteroids with VLT/SPHERE/ZIMPOL. Our asteroid sample comprises 39 bodies with D ≥ 100 km and in particular most D ≥ 200 km main-belt asteroids (20/23). Furthermore, it nicely reflects the compositional diversity present in the main belt as the sampled bodies belong to the following taxonomic classes: A, B, C, Ch/Cgh, E/M/X, K, P/T, S, and V. Methods. The SPHERE/ZIMPOL images were first used to reconstruct the 3D shape of all targets with both the ADAM and MPCD reconstruction methods. We subsequently performed a detailed shape analysis and constrained the density of each target using available mass estimates including our own mass estimates in the case of multiple systems. Results. The analysis of the reconstructed shapes allowed us to identify two families of objects as a function of their diameters, namely “spherical” and “elongated” bodies. A difference in rotation period appears to be the main origin of this bimodality. In addition, all but one object (216 Kleopatra) are located along the Maclaurin sequence with large volatile-rich bodies being the closest to the latter. Our results further reveal that the primaries of most multiple systems possess a rotation period of shorter than 6 h and an elongated shape ( c ∕ a ≤ 0.65). Densities in our sample range from ~1.3 g cm −3 (87 Sylvia) to ~4.3 g cm −3 (22 Kalliope). Furthermore, the density distribution appears to be strongly bimodal with volatile-poor ( ρ ≥ 2.7 g cm −3 ) and volatile-rich ( ρ ≤ 2.2 g cm −3 ) bodies. Finally, 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.

Published
2021
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24. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Author

Marciniak, A., primary, Ďurech, J., additional, Alí-Lagoa, V., additional, Ogłoza, W., additional, Szakáts, R., additional, Müller, T. G., additional, Molnár, L., additional, Pál, A., additional, Monteiro, F., additional, Arcoverde, P., additional, Behrend, R., additional, Benkhaldoun, Z., additional, Bernasconi, L., additional, Bosch, J., additional, Brincat, S., additional, Brunetto, L., additional, Butkiewicz - Bąk, M., additional, Del Freo, F., additional, Duffard, R., additional, Evangelista-Santana, M., additional, Farroni, G., additional, Fauvaud, S., additional, Fauvaud, M., additional, Ferrais, M., additional, Geier, S., additional, Golonka, J., additional, Grice, J., additional, Hirsch, R., additional, Horbowicz, J., additional, Jehin, E., additional, Julien, P., additional, Kalup, Cs., additional, Kamiński, K., additional, Kamińska, M. K., additional, Kankiewicz, P., additional, Kecskeméthy, V., additional, Kim, D.-H., additional, Kim, M.-J., additional, Konstanciak, I., additional, Krajewski, J., additional, Kudak, V., additional, Kulczak, P., additional, Kundera, T., additional, Lazzaro, D., additional, Manzini, F., additional, Medeiros, H., additional, Michimani-Garcia, J., additional, Morales, N., additional, Nadolny, J., additional, Oszkiewicz, D., additional, Pakštienė, E., additional, Pawłowski, M., additional, Perig, V., additional, Pilcher, F., additional, Pinel, P., additional, Podlewska-Gaca, E., additional, Polakis, T., additional, Richard, F., additional, Rodrigues, T., additional, Rondón, E., additional, Roy, R., additional, Sanabria, J. J., additional, Santana-Ros, T., additional, Skiff, B., additional, Skrzypek, J., additional, Sobkowiak, K., additional, Sonbas, E., additional, Stachowski, G., additional, Strajnic, J., additional, Trela, P., additional, Tychoniec, Ł., additional, Urakawa, S., additional, Verebelyi, E., additional, Wagrez, K., additional, Żejmo, M., additional, and Żukowski, K., additional

Published
2021
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25. VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis

Author

Vernazza, P., primary, Ferrais, M., additional, Jorda, L., additional, Hanuš, J., additional, Carry, B., additional, Marsset, M., additional, Brož, M., additional, Fetick, R., additional, Viikinkoski, M., additional, Marchis, F., additional, Vachier, F., additional, Drouard, A., additional, Fusco, T., additional, Birlan, M., additional, Podlewska-Gaca, E., additional, Rambaux, N., additional, Neveu, M., additional, Bartczak, P., additional, Dudziński, G., additional, Jehin, E., additional, Beck, P., additional, Berthier, J., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Colas, F., additional, Dumas, C., additional, Ďurech, J., additional, Grice, J., additional, Kaasalainen, M., additional, Kryszczynska, A., additional, Lamy, P., additional, Le Coroller, H., additional, Marciniak, A., additional, Michalowski, T., additional, Michel, P., additional, Santana-Ros, T., additional, Tanga, P., additional, Vigan, A., additional, Witasse, O., additional, Yang, B., additional, Antonini, P., additional, Audejean, M., additional, Aurard, P., additional, Behrend, R., additional, Benkhaldoun, Z., additional, Bosch, J. M., additional, Chapman, A., additional, Dalmon, L., additional, Fauvaud, S., additional, Hamanowa, Hiroko, additional, Hamanowa, Hiromi, additional, His, J., additional, Jones, A., additional, Kim, D.-H., additional, Kim, M.-J., additional, Krajewski, J., additional, Labrevoir, O., additional, Leroy, A., additional, Livet, F., additional, Molina, D., additional, Montaigut, R., additional, Oey, J., additional, Payre, N., additional, Reddy, V., additional, Sabin, P., additional, Sanchez, A. G., additional, and Socha, L., additional

Published
2021
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26. (216) Kleopatra, a low density critically rotating M-type asteroid

Author

Marchis, F., primary, Jorda, L., additional, Vernazza, P., additional, Brož, M., additional, Hanuš, J., additional, Ferrais, M., additional, Vachier, F., additional, Rambaux, N., additional, Marsset, M., additional, Viikinkoski, M., additional, Jehin, E., additional, Benseguane, S., additional, Podlewska-Gaca, E., additional, Carry, B., additional, Drouard, A., additional, Fauvaud, S., additional, Birlan, M., additional, Berthier, J., additional, Bartczak, P., additional, Dumas, C., additional, Dudziński, G., additional, Ďurech, J., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Colas, F., additional, Fetick, R., additional, Fusco, T., additional, Grice, J., additional, Kryszczynska, A., additional, Lamy, P., additional, Marciniak, A., additional, Michalowski, T., additional, Michel, P., additional, Pajuelo, M., additional, Santana-Ros, T., additional, Tanga, P., additional, Vigan, A., additional, Witasse, O., additional, and Yang, B., additional

Published
2021
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27. An advanced multipole model for (216) Kleopatra triple system

Author

Brož, M., primary, Marchis, F., additional, Jorda, L., additional, Hanuš, J., additional, Vernazza, P., additional, Ferrais, M., additional, Vachier, F., additional, Rambaux, N., additional, Marsset, M., additional, Viikinkoski, M., additional, Jehin, E., additional, Benseguane, S., additional, Podlewska-Gaca, E., additional, Carry, B., additional, Drouard, A., additional, Fauvaud, S., additional, Birlan, M., additional, Berthier, J., additional, Bartczak, P., additional, Dumas, C., additional, Dudziński, G., additional, Ďurech, J., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Colas, F., additional, Fetick, R., additional, Fusco, T., additional, Grice, J., additional, Kryszczynska, A., additional, Lamy, P., additional, Marciniak, A., additional, Michalowski, T., additional, Michel, P., additional, Pajuelo, M., additional, Santana-Ros, T., additional, Tanga, P., additional, Vigan, A., additional, Vokrouhlický, D., additional, Witasse, O., additional, and Yang, B., additional

Published
2021
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28. 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

29. (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

30. Lightcurves of asteroids: spin, 3-D shape, density

Author

Carry, Benoît, Fauvaud, S., Marciniak, A., Behrend, Raoul, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astéroïdes, comètes, météores et éphémérides (ACME), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

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

International audience; The study of the physical properties of asteroids, spin and 3-D shape, is the first step in understanding their formation and the mechanisms that dictate their evolution. The 3-D shape is indeed required to compute precisely the density, the only quantity that tells us about the internal structure from remote sensing, which is at the crux of the question of the location of formation. Bodies accreted far from the Sun contain volatiles elements (ices) and are less dense. Similarly, the spin orientation is key in triggering the orbital Yarkovsky drift effect, which ultimately delivers meteorites to the Earth. Observations by amateur astronomers and professional astronomers are complementary to study these properties. Lightcurves provided by amateurs combined with high-angular resolution images obtained by professionals with 8m class telescopes allow detailed modeling of asteroids. In this proceeding, we describe the motivations to study asteroid physical properties, describe several on-going professional-amateur observing campaigns, and illustrate then with a few results.

Published
2018

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

Author

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

Published
2019
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32. Homogeneous internal structure of CM-like asteroid (41) Daphne

Author

Carry, B., primary, Vachier, F., additional, Berthier, J., additional, Marsset, M., additional, Vernazza, P., additional, Grice, J., additional, Merline, W. J., additional, Lagadec, E., additional, Fienga, A., additional, Conrad, A., additional, Podlewska-Gaca, E., additional, Santana-Ros, T., additional, Viikinkoski, M., additional, Hanuš, J., additional, Dumas, C., additional, Drummond, J. D., additional, Tamblyn, P. M., additional, Chapman, C. R., additional, Behrend, R., additional, Bernasconi, L., additional, Bartczak, P., additional, Benkhaldoun, Z., additional, Birlan, M., additional, Castillo-Rogez, J., additional, Cipriani, F., additional, Colas, F., additional, Drouard, A., additional, Ďurech, J., additional, Enke, B. L., additional, Fauvaud, S., additional, Ferrais, M., additional, Fetick, R., additional, Fusco, T., additional, Gillon, M., additional, Jehin, E., additional, Jorda, L., additional, Kaasalainen, M., additional, Keppler, M., additional, Kryszczynska, A., additional, Lamy, P., additional, Marchis, F., additional, Marciniak, A., additional, Michalowski, T., additional, Michel, P., additional, Pajuelo, M., additional, Tanga, P., additional, Vigan, A., additional, Warner, B., additional, Witasse, O., additional, Yang, B., additional, and Zurlo, A., additional

Published
2019
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33. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author

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

Abstract

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

Published
2019

34. Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites

Author

Pajuelo, M., primary, Carry, B., additional, Vachier, F., additional, Marsset, M., additional, Berthier, J., additional, Descamps, P., additional, Merline, W.J., additional, Tamblyn, P.M., additional, Grice, J., additional, Conrad, A., additional, Storrs, A., additional, Timerson, B., additional, Dunham, D., additional, Preston, S., additional, Vigan, A., additional, Yang, B., additional, Vernazza, P., additional, Fauvaud, S., additional, Bernasconi, L., additional, Romeuf, D., additional, Behrend, R., additional, Dumas, C., additional, Drummond, J.D., additional, Margot, J.-L., additional, Kervella, P., additional, Marchis, F., additional, and Girard, J.H., additional

Published
2018
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35. Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Author

Marciniak, A., primary, Bartczak, P., additional, Müller, T., additional, Sanabria, J. J., additional, Alí-Lagoa, V., additional, Antonini, P., additional, Behrend, R., additional, Bernasconi, L., additional, Bronikowska, M., additional, Butkiewicz-Bąk, M., additional, Cikota, A., additional, Crippa, R., additional, Ditteon, R., additional, Dudziński, G., additional, Duffard, R., additional, Dziadura, K., additional, Fauvaud, S., additional, Geier, S., additional, Hirsch, R., additional, Horbowicz, J., additional, Hren, M., additional, Jerosimic, L., additional, Kamiński, K., additional, Kankiewicz, P., additional, Konstanciak, I., additional, Korlevic, P., additional, Kosturkiewicz, E., additional, Kudak, V., additional, Manzini, F., additional, Morales, N., additional, Murawiecka, M., additional, Ogłoza, W., additional, Oszkiewicz, D., additional, Pilcher, F., additional, Polakis, T., additional, Poncy, R., additional, Santana-Ros, T., additional, Siwak, M., additional, Skiff, B., additional, Sobkowiak, K., additional, Stoss, R., additional, Żejmo, M., additional, and Żukowski, K., additional

Published
2018
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36. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author

Hanuš, J., primary, Ďurech, J., additional, Oszkiewicz, D. A., additional, Behrend, R., additional, Carry, B., additional, Delbo, M., additional, Adam, O., additional, Afonina, V., additional, Anquetin, R., additional, Antonini, P., additional, Arnold, L., additional, Audejean, M., additional, Aurard, P., additional, Bachschmidt, M., additional, Baduel, B., additional, Barbotin, E., additional, Barroy, P., additional, Baudouin, P., additional, Berard, L., additional, Berger, N., additional, Bernasconi, L., additional, Bosch, J-G., additional, Bouley, S., additional, Bozhinova, I., additional, Brinsfield, J., additional, Brunetto, L., additional, Canaud, G., additional, Caron, J., additional, Carrier, F., additional, Casalnuovo, G., additional, Casulli, S., additional, Cerda, M., additional, Chalamet, L., additional, Charbonnel, S., additional, Chinaglia, B., additional, Cikota, A., additional, Colas, F., additional, Coliac, J.-F., additional, Collet, A., additional, Coloma, J., additional, Conjat, M., additional, Conseil, E., additional, Costa, R., additional, Crippa, R., additional, Cristofanelli, M., additional, Damerdji, Y., additional, Debackère, A., additional, Decock, A., additional, Déhais, Q., additional, Déléage, T., additional, Delmelle, S., additional, Demeautis, C., additional, Dróżdż, M., additional, Dubos, G., additional, Dulcamara, T., additional, Dumont, M., additional, Durkee, R., additional, Dymock, R., additional, Escalante del Valle, A., additional, Esseiva, N., additional, Esseiva, R., additional, Esteban, M., additional, Fauchez, T., additional, Fauerbach, M., additional, Fauvaud, M., additional, Fauvaud, S., additional, Forné, E., additional, Fournel, C., additional, Fradet, D., additional, Garlitz, J., additional, Gerteis, O., additional, Gillier, C., additional, Gillon, M., additional, Giraud, R., additional, Godard, J.-P., additional, Goncalves, R., additional, Hamanowa, Hiroko, additional, Hamanowa, Hiromi, additional, Hay, K., additional, Hellmich, S., additional, Heterier, S., additional, Higgins, D., additional, Hirsch, R., additional, Hodosan, G., additional, Hren, M., additional, Hygate, A., additional, Innocent, N., additional, Jacquinot, H., additional, Jawahar, S., additional, Jehin, E., additional, Jerosimic, L., additional, Klotz, A., additional, Koff, W., additional, Korlevic, P., additional, Kosturkiewicz, E., additional, Krafft, P., additional, Krugly, Y., additional, Kugel, F., additional, Labrevoir, O., additional, Lecacheux, J., additional, Lehký, M., additional, Leroy, A., additional, Lesquerbault, B., additional, Lopez-Gonzales, M. J., additional, Lutz, M., additional, Mallecot, B., additional, Manfroid, J., additional, Manzini, F., additional, Marciniak, A., additional, Martin, A., additional, Modave, B., additional, Montaigut, R., additional, Montier, J., additional, Morelle, E., additional, Morton, B., additional, Mottola, S., additional, Naves, R., additional, Nomen, J., additional, Oey, J., additional, Ogłoza, W., additional, Paiella, M., additional, Pallares, H., additional, Peyrot, A., additional, Pilcher, F., additional, Pirenne, J.-F., additional, Piron, P., additional, Polińska, M., additional, Polotto, M., additional, Poncy, R., additional, Previt, J. P., additional, Reignier, F., additional, Renauld, D., additional, Ricci, D., additional, Richard, F., additional, Rinner, C., additional, Risoldi, V., additional, Robilliard, D., additional, Romeuf, D., additional, Rousseau, G., additional, Roy, R., additional, Ruthroff, J., additional, Salom, P. A., additional, Salvador, L., additional, Sanchez, S., additional, Santana-Ros, T., additional, Scholz, A., additional, Séné, G., additional, Skiff, B., additional, Sobkowiak, K., additional, Sogorb, P., additional, Soldán, F., additional, Spiridakis, A., additional, Splanska, E., additional, Sposetti, S., additional, Starkey, D., additional, Stephens, R., additional, Stiepen, A., additional, Stoss, R., additional, Strajnic, J., additional, Teng, J.-P., additional, Tumolo, G., additional, Vagnozzi, A., additional, Vanoutryve, B., additional, Vugnon, J. M., additional, Warner, B. D., additional, Waucomont, M., additional, Wertz, O., additional, Winiarski, M., additional, and Wolf, M., additional

Published
2016
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37. The field high-amplitude SX Phe variable BL Cam: results from a multisite photometric campaign

Author

Fauvaud, S., Sareyan, J. -P., Ribas, I., Rodriguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, J. H., Wolf, M., Santacana, G., Zhou, A. -Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., Lopez-Gonzalez, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. -J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Kral, L., Kocian, R., Kucakova, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. -M., Kotkova, L., Truparova, K., Ulusoy, C., Yasarsoy, B., Avdibegovic, A., Blazek, M., Kliner, J., Zasche, P., Bartosikova, S., Vilasek, M., Trondal, O., Van Den Abbeel, F., Behrend, R., Wuecher, H., and Ege Üniversitesi

Subjects
techniques: photometric, binaries: general, stars: variables: delta Scuti, stars: oscillations, stars: individual: BL Camelopardalis
Abstract

WOS: 000280505000008, Context. Short-period high-amplitude pulsating stars of Population I (delta Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational behaviours, only one or two radial modes being excited. Nevertheless, BL Cam is a unique object among them, being an extreme metal-deficient field high-amplitude SX Phe variable with a large number of frequencies. Based on a frequency analysis, a pulsational interpretation was previously given. Aims. We attempt to interpret the long-term behaviour of the residuals that were not taken into account in the previous Observed-Calculated (O-C) short-term analyses. Methods. An investigation of the O-C times has been carried out, using a data set based on the previous published times of light maxima, largely enriched by those obtained during an intensive multisite photometric campaign of BL Cam lasting several months. Results. In addition to a positive (161 +/- 3) x 10(-9) yr(-1) secular relative increase in the main pulsation period of BL Cam, we detected in the O-C data short- (144.2 d) and long-term (similar to 3400 d) variations, both incompatible with a scenario of stellar evolution. Conclusions. Interpreted as a light travel-time effect, the short- term O-C variation is indicative of a massive stellar component (0.46 to 1 M(circle dot)) with a short period orbit (144.2 d), within a distance of 0.7 AU from the primary. More observations are needed to confirm the long-term O-C variations: if they were also to be caused by a light travel-time effect, they could be interpreted in terms of a third component, in this case probably a brown dwarf star (>= 0.03 M(circle dot)), orbiting in similar to 3400 d at a distance of 4.5 AU from the primary., UNAMUniversidad Nacional Autonoma de Mexico [PAPIIT IN114309]; Junta de AndaluciaJunta de Andalucia; Spanish Direccion General de Investigacion (DGI)Ministry of Education and Science, Spain [AYA2006-06375, AYA2009-10394]; Belgian National Lottery, E.G.H. acknowledges the use of the 1.8-m Plaskett Telescope at the Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada. J.H.S. is very grateful to his group of students at the Physics Department of the Virginia Polytechnic Institute and State University. L.F.M. and M.A. acknowledge financial support from the UNAM under grant PAPIIT IN114309. S.F. thanks Russ Robb (University of Victoria, Canada) who provided the unpublished times of light maxima, and Jerome Berthier and Francois Colas (institut de mecanique celeste et de calcul des ephemerides, France). This investigation was partially supported by the Junta de Andalucia and the Spanish Direccion General de Investigacion (DGI) under projects AYA2006-06375 and AYA2009-10394. The observations were partially collected with the 1.5m telescope at SNO which is operated by the Instituto de Astrofisica de Andalucia. Data from Pic du Midi Observatory have been obtained with the 0.6 m telescope, a facility operated by observatoire Midi-Pyrenees and Association T60, an amateur association. Part of the data used in this work was acquired with equipment purchased thanks to a research fund financed by the Belgian National Lottery (1999). We acknowledge with thanks the variable star observations from the American Association of Variable Star Observers international database contributed by observers worldwide and used in this study. This research has made use of both the Simbad database, operated at CDS, Strasbourg, France, and the Astrophysics Data System, provided by NASA

Published
2010

38. The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

Author

Rodriguez, E., Fauvaud, S., Farrell, J. A., Zhou, A.-Y., Sareyan, J.-P., Lopez-Gonzalez, M. J., Dupret, M.-A., Grigahcene, A., de Ridder, J., Klingenberg, G., Wolf, M., Van Cauteren, P., Lampens, P., Martinez, D., Casanova, V. M., Aceituno, F. J., Helvaci, M., Hintz, E. G., Kral, L., Fumagalli, F., Simonetti, J. H., Granslo, B. H., Kotkova, L., Santacana, G., Michelet, J., Fauvaud, M., Vugnon, J-M, Sadsaoud, H., Aliouane, A., Grigahcene, Z. C., Martin-Ruiz, S., Amado, P. J., Suarez, J. C., Moya, A., Kucakova, H., Kocian, R., Truparova, B., Avdibegtovic, A., Blazek, M., Kliner, J., Zasche, P., Vilasek, M., Bartosikova, S., Yasarsoy, B., Ulusoy, C., Graham, K. A., Nicholson, M. P., Trondal, O., Yesilyaprak, C., Coker, D., and Ege Üniversitesi

Subjects
stars : variables : delta Sct, techniques : photometric, stars : oscillations, stars : individual : BL Camelopardalis
Abstract

WOS: 000248394400032, Context. BL Cam is an extreme metal-deficient field high-amplitude SX Phe-type variable where a very complex frequency spectrum is detected, with a number of independent nonradial modes excited, unusual among the high-amplitude pulsators in the Lower Classical Instability Strip. Aims. An extensive and detailed study has been carried out to investigate the pulsational content and properties of this object. Methods. The analysis is based on 283 h of CCD observations obtained in the Johnson V filter, during a long multisite photometric campaign carried out along the Northern autumn-winter of 2005-2006. Additionally, multicolour BI photometry was also collected to study the phase shifts and amplitude ratios, between light curves obtained in different filters, for modal discrimination of the main excited modes. Results. The detailed frequency analysis revealed a very rich and dense pulsational content consisting of 25 significant peaks, 22 of them corresponding to independent modes: one is the already known main periodicity f(0) = 25.5765 cd(-1) (Delta V = 153 mmag) and the other 21 are excited modes showing very small amplitudes. Some additional periodicities are probably still remaining in the residuals. This represents the most complex spectrum ever detected in a high-amplitude pulsator of this type. The majority of the secondary modes suspected from earlier works are confirmed here and, additionally, a large number of new peaks are detected. The amplitude of the main periodicity f(0) seems to be stable during decades, but the majority of the secondary modes show strong amplitude changes from one epoch to another. The suspected fundamental radial nature of the main periodicity of BL Cam is confirmed, while the secondary peak f(1) = 25.2523 cd(-1) is identified as a nonradial mixed mode g(4) with l = 1. The radial double-mode nature, claimed by some authors for the main two frequencies of BL Cam, is not confirmed. Nevertheless, the frequency f(6) = 32.6464 cd(-1) could correspond to the first radial overtone.

Published
2007

39. Photometry and models of selected main belt asteroids - IX. Introducing interactive service for asteroid models (ISAM)

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Bartczak, Przemyslaw, Santana-Ros, Toni, Michalowski, Tadeusz, Antonini, Pierre, Behrend, Raoul, Bembrick, C., Bernasconi, Laurent, Borczyk, W., Colas, François, Coloma, J., Crippa, R., Esseiva, N., Fagas, M., Fauvaud, M., Fauvaud, S., Ferreira, D.D.M., Hein Bertelsen, R.P., Higgins, D., Hirsch, R., Kajava, J.J.E., Kamiński, Krzysztof, Kryszczynska, Agnieszka, Kwiatkowski, T., Manzini, F., Michałowski, J., Michałowski, Michał J., Paschke, A., Polińska, M., Poncy, R., Roy, René, Santacana, G., Sobkowiak, Krzysztof, Stasik, M., Starczewski, S., Velichko, F., Wucher, H., Zafar, T., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Marciniak, Anna, Bartczak, Przemyslaw, Santana-Ros, Toni, Michalowski, Tadeusz, Antonini, Pierre, Behrend, Raoul, Bembrick, C., Bernasconi, Laurent, Borczyk, W., Colas, François, Coloma, J., Crippa, R., Esseiva, N., Fagas, M., Fauvaud, M., Fauvaud, S., Ferreira, D.D.M., Hein Bertelsen, R.P., Higgins, D., Hirsch, R., Kajava, J.J.E., Kamiński, Krzysztof, Kryszczynska, Agnieszka, Kwiatkowski, T., Manzini, F., Michałowski, J., Michałowski, Michał J., Paschke, A., Polińska, M., Poncy, R., Roy, René, Santacana, G., Sobkowiak, Krzysztof, Stasik, M., Starczewski, S., Velichko, F., Wucher, H., and Zafar, T.

Abstract

Context. The shapes and spin states of asteroids observed with photometric techniques can be reconstructed using the lightcurve inversion method. The resultant models can then be confirmed or exploited further by other techniques, such as adaptive optics, radar, thermal infrared, stellar occultations, or space probe imaging. Aims. During our ongoing work to increase the set of asteroids with known spin and shape parameters, there appeared a need for displaying the model plane-of-sky orientations for specific epochs to compare models from different techniques. It would also be instructive to be able to track how the complex lightcurves are produced by various asteroid shapes. Methods. Basing our analysis on an extensive photometric observational dataset, we obtained eight asteroid models with the convex lightcurve inversion method. To enable comparison of the photometric models with those from other observing/modelling techniques, we created an on-line service where we allow the inversion models to be orientated interactively. Results. Our sample of objects is quite representative, containing both relatively fast and slow rotators with highly and lowly inclined spin axes. With this work, we increase the sample of asteroid spin and shape models based on disk-integrated photometry to over 200. Three of the shape models obtained here are confirmed by the stellar occultation data; this also allowed independent determinations of their sizes to be made. Conclusions. The ISAM service can be widely exploited for past and future asteroid observations with various, complementary techniques and for asteroid dimension determination.

Published
2012

40. Photometry and models of selected main belt asteroids: IX. Introducing interactive service for asteroid models (ISAM)

Author

Marciniak, A., Bartczak, P., Santana-Ros, T., Michałowski, T., Borczyk, W., Fagas, M., Hirsch, R., Kamiński, K., Kryszczyńska, A., Kwiatkowski, T., Polińska, M., Sobkowiak, K., Stasik, M., Antonini, P., Behrend, R., Bembrick, C., Bernasconi, L., Colas, F., Coloma, J., Crippa, R., Manzini, F., Esseiva, N., Santacana, G., Wucher, H., Fauvaud, M., Fauvaud, S., Ferreira, Desiree Della Monica, Hein Bertelsen, R.P., Higgins, D., Kajava, J.J.E., Michałowski, J., Michałowski, M.J., Paschke, A., Poncy, R., Roy, R., Starczewski, S., Velichko, F., Zafar, T., Marciniak, A., Bartczak, P., Santana-Ros, T., Michałowski, T., Borczyk, W., Fagas, M., Hirsch, R., Kamiński, K., Kryszczyńska, A., Kwiatkowski, T., Polińska, M., Sobkowiak, K., Stasik, M., Antonini, P., Behrend, R., Bembrick, C., Bernasconi, L., Colas, F., Coloma, J., Crippa, R., Manzini, F., Esseiva, N., Santacana, G., Wucher, H., Fauvaud, M., Fauvaud, S., Ferreira, Desiree Della Monica, Hein Bertelsen, R.P., Higgins, D., Kajava, J.J.E., Michałowski, J., Michałowski, M.J., Paschke, A., Poncy, R., Roy, R., Starczewski, S., Velichko, F., and Zafar, T.

Abstract

Context. The shapes and spin states of asteroids observed with photometric techniques can be reconstructed using the lightcurve inversion method. The resultant models can then be confirmed or exploited further by other techniques, such as adaptive optics, radar, thermal infrared, stellar occultations, or space probe imaging. Aims. During our ongoing work to increase the set of asteroids with known spin and shape parameters, there appeared a need for displaying the model plane-of-sky orientations for specific epochs to compare models from different techniques. It would also be instructive to be able to track how the complex lightcurves are produced by various asteroid shapes. Methods. Basing our analysis on an extensive photometric observational dataset, we obtained eight asteroid models with the convex lightcurve inversion method. To enable comparison of the photometric models with those from other observing/modelling techniques, we created an on-line service where we allow the inversion models to be orientated interactively. Results. Our sample of objects is quite representative, containing both relatively fast and slow rotators with highly and lowly inclined spin axes. With this work, we increase the sample of asteroid spin and shape models based on disk-integrated photometry to over 200. Three of the shape models obtained here are confirmed by the stellar occultation data; this also allowed independent determinations of their sizes to be made. Conclusions. The ISAM service can be widely exploited for past and future asteroid observations with various, complementary techniques and for asteroid dimension determination. © 2012 ESO.

Published
2012

41. The field high-amplitude SX Phe variable BL Cam: results from a multisite photometric campaign

Author

Physics, Fauvaud, S., Sareyan, J. P., Ribas, I., Rodriguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, John H., Wolf, M., Santacana, G., Zhou, A. Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., Lopez-Gonzalez, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Kral, L., Kocian, R., Kucakova, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. M., Kotkova, L., Truparova, K., Ulusoy, C., Yasarsoy, B., Avdibegtovic, A., Blazek, M., Kliner, J., Zasche, P., Bartosikova, S., Vilasek, M., Trondal, O., Van Den Abbeel, F., Behrend, R., Wucher, H., Physics, Fauvaud, S., Sareyan, J. P., Ribas, I., Rodriguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, John H., Wolf, M., Santacana, G., Zhou, A. Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., Lopez-Gonzalez, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Kral, L., Kocian, R., Kucakova, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. M., Kotkova, L., Truparova, K., Ulusoy, C., Yasarsoy, B., Avdibegtovic, A., Blazek, M., Kliner, J., Zasche, P., Bartosikova, S., Vilasek, M., Trondal, O., Van Den Abbeel, F., Behrend, R., and Wucher, H.

Abstract

Context. Short-period high-amplitude pulsating stars of Population I (delta Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational behaviours, only one or two radial modes being excited. Nevertheless, BL Cam is a unique object among them, being an extreme metal-deficient field high-amplitude SX Phe variable with a large number of frequencies. Based on a frequency analysis, a pulsational interpretation was previously given. Aims. We attempt to interpret the long-term behaviour of the residuals that were not taken into account in the previous Observed-Calculated (O-C) short-term analyses. Methods. An investigation of the O-C times has been carried out, using a data set based on the previous published times of light maxima, largely enriched by those obtained during an intensive multisite photometric campaign of BL Cam lasting several months. Results. In addition to a positive (161 +/- 3) x 10(-9) yr(-1) secular relative increase in the main pulsation period of BL Cam, we detected in the O-C data short- (144.2 d) and long-term (similar to 3400 d) variations, both incompatible with a scenario of stellar evolution. Conclusions. Interpreted as a light travel-time effect, the short- term O-C variation is indicative of a massive stellar component (0.46 to 1 M(circle dot)) with a short period orbit (144.2 d), within a distance of 0.7 AU from the primary. More observations are needed to confirm the long-term O-C variations: if they were also to be caused by a light travel-time effect, they could be interpreted in terms of a third component, in this case probably a brown dwarf star (>= 0.03 M(circle dot)), orbiting in similar to 3400 d at a distance of 4.5 AU from the primary.

Published
2010

42. Asteroids’ physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author

Hanuš, J., primary, Ďurech, J., additional, Brož, M., additional, Marciniak, A., additional, Warner, B. D., additional, Pilcher, F., additional, Stephens, R., additional, Behrend, R., additional, Carry, B., additional, Čapek, D., additional, Antonini, P., additional, Audejean, M., additional, Augustesen, K., additional, Barbotin, E., additional, Baudouin, P., additional, Bayol, A., additional, Bernasconi, L., additional, Borczyk, W., additional, Bosch, J.-G., additional, Brochard, E., additional, Brunetto, L., additional, Casulli, S., additional, Cazenave, A., additional, Charbonnel, S., additional, Christophe, B., additional, Colas, F., additional, Coloma, J., additional, Conjat, M., additional, Cooney, W., additional, Correira, H., additional, Cotrez, V., additional, Coupier, A., additional, Crippa, R., additional, Cristofanelli, M., additional, Dalmas, Ch., additional, Danavaro, C., additional, Demeautis, C., additional, Droege, T., additional, Durkee, R., additional, Esseiva, N., additional, Esteban, M., additional, Fagas, M., additional, Farroni, G., additional, Fauvaud, M., additional, Fauvaud, S., additional, Del Freo, F., additional, Garcia, L., additional, Geier, S., additional, Godon, C., additional, Grangeon, K., additional, Hamanowa, H., additional, Heck, N., additional, Hellmich, S., additional, Higgins, D., additional, Hirsch, R., additional, Husarik, M., additional, Itkonen, T., additional, Jade, O., additional, Kamiński, K., additional, Kankiewicz, P., additional, Klotz, A., additional, Koff, R. A., additional, Kryszczyńska, A., additional, Kwiatkowski, T., additional, Laffont, A., additional, Leroy, A., additional, Lecacheux, J., additional, Leonie, Y., additional, Leyrat, C., additional, Manzini, F., additional, Martin, A., additional, Masi, G., additional, Matter, D., additional, Michałowski, J., additional, Michałowski, M. J., additional, Michałowski, T., additional, Michelet, J., additional, Michelsen, R., additional, Morelle, E., additional, Mottola, S., additional, Naves, R., additional, Nomen, J., additional, Oey, J., additional, Ogłoza, W., additional, Oksanen, A., additional, Oszkiewicz, D., additional, Pääkkönen, P., additional, Paiella, M., additional, Pallares, H., additional, Paulo, J., additional, Pavic, M., additional, Payet, B., additional, Polińska, M., additional, Polishook, D., additional, Poncy, R., additional, Revaz, Y., additional, Rinner, C., additional, Rocca, M., additional, Roche, A., additional, Romeuf, D., additional, Roy, R., additional, Saguin, H., additional, Salom, P. A., additional, Sanchez, S., additional, Santacana, G., additional, Santana-Ros, T., additional, Sareyan, J.-P., additional, Sobkowiak, K., additional, Sposetti, S., additional, Starkey, D., additional, Stoss, R., additional, Strajnic, J., additional, Teng, J.-P., additional, Trégon, B., additional, Vagnozzi, A., additional, Velichko, F. P., additional, Waelchli, N., additional, Wagrez, K., additional, and Wücher, H., additional

Published
2013
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43. The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

Author

Physics, Rodriguez, E., Fauvaud, S., Farrell, J. A., Zhou, A. Y., Sareyan, J. P., Lopez-Gonzalez, M. J., Dupret, M. A., Grigahcene, A., de Ridder, J., Klingenberg, G., Wolf, M., Van Cauteren, P., Lampens, P., Martinez, D., Casanova, V. M., Aceituno, F. J., Helvaci, M., Hintz, E. G., Kral, L., Fumagalli, F., Simonetti, John H., Granslo, B. H., Kotkova, L., Santacana, G., Michelet, J., Fauvaud, M., Vugnon, J. M., Sadsaoud, H., Aliouane, A., Grigahcene, Z. C., Martin-Ruiz, S., Amado, P. J., Suarez, J. C., Moya, A., Kucakova, H., Kocian, R., Truparova, B., Avdibegtovic, A., Blazek, M., Kliner, J., Zasche, P., Vilasek, M., Bartosikova, S., Yasarsoy, B., Ulusoy, C., Graham, K. A., Nicholson, M. P., Trondal, O., Yesilyaprak, C., Coker, D., Physics, Rodriguez, E., Fauvaud, S., Farrell, J. A., Zhou, A. Y., Sareyan, J. P., Lopez-Gonzalez, M. J., Dupret, M. A., Grigahcene, A., de Ridder, J., Klingenberg, G., Wolf, M., Van Cauteren, P., Lampens, P., Martinez, D., Casanova, V. M., Aceituno, F. J., Helvaci, M., Hintz, E. G., Kral, L., Fumagalli, F., Simonetti, John H., Granslo, B. H., Kotkova, L., Santacana, G., Michelet, J., Fauvaud, M., Vugnon, J. M., Sadsaoud, H., Aliouane, A., Grigahcene, Z. C., Martin-Ruiz, S., Amado, P. J., Suarez, J. C., Moya, A., Kucakova, H., Kocian, R., Truparova, B., Avdibegtovic, A., Blazek, M., Kliner, J., Zasche, P., Vilasek, M., Bartosikova, S., Yasarsoy, B., Ulusoy, C., Graham, K. A., Nicholson, M. P., Trondal, O., Yesilyaprak, C., and Coker, D.

Abstract

Context. BL Cam is an extreme metal-deficient field high-amplitude SX Phe-type variable where a very complex frequency spectrum is detected, with a number of independent nonradial modes excited, unusual among the high-amplitude pulsators in the Lower Classical Instability Strip. Aims. An extensive and detailed study has been carried out to investigate the pulsational content and properties of this object. Methods. The analysis is based on 283 h of CCD observations obtained in the Johnson V filter, during a long multisite photometric campaign carried out along the Northern autumn-winter of 2005-2006. Additionally, multicolour BI photometry was also collected to study the phase shifts and amplitude ratios, between light curves obtained in different filters, for modal discrimination of the main excited modes. Results. The detailed frequency analysis revealed a very rich and dense pulsational content consisting of 25 significant peaks, 22 of them corresponding to independent modes: one is the already known main periodicity f(0) = 25.5765 cd(-1) (Delta V = 153 mmag) and the other 21 are excited modes showing very small amplitudes. Some additional periodicities are probably still remaining in the residuals. This represents the most complex spectrum ever detected in a high-amplitude pulsator of this type. The majority of the secondary modes suspected from earlier works are confirmed here and, additionally, a large number of new peaks are detected. The amplitude of the main periodicity f(0) seems to be stable during decades, but the majority of the secondary modes show strong amplitude changes from one epoch to another. The suspected fundamental radial nature of the main periodicity of BL Cam is confirmed, while the secondary peak f(1) = 25.2523 cd(-1) is identified as a nonradial mixed mode g(4) with l = 1. The radial double-mode nature, claimed by some authors for the main two frequencies of BL Cam, is not confirmed. Nevertheless, the frequency f(6) = 32.6464 cd(-1) could

Published
2007

44. Photometry and models of selected main belt asteroids

Author

Marciniak, A., primary, Bartczak, P., additional, Santana-Ros, T., additional, Michałowski, T., additional, Antonini, P., additional, Behrend, R., additional, Bembrick, C., additional, Bernasconi, L., additional, Borczyk, W., additional, Colas, F., additional, Coloma, J., additional, Crippa, R., additional, Esseiva, N., additional, Fagas, M., additional, Fauvaud, M., additional, Fauvaud, S., additional, Ferreira, D. D. M., additional, Hein Bertelsen, R. P., additional, Higgins, D., additional, Hirsch, R., additional, Kajava, J. J. E., additional, Kamiński, K., additional, Kryszczyńska, A., additional, Kwiatkowski, T., additional, Manzini, F., additional, Michałowski, J., additional, Michałowski, M. J., additional, Paschke, A., additional, Polińska, M., additional, Poncy, R., additional, Roy, R., additional, Santacana, G., additional, Sobkowiak, K., additional, Stasik, M., additional, Starczewski, S., additional, Velichko, F., additional, Wucher, H., additional, and Zafar, T., additional

Published
2012
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45. The field high-amplitude SX Phe variable BL Cam: results from a multisite photometric campaign

Author

Fauvaud, S., primary, Sareyan, J.-P., additional, Ribas, I., additional, Rodríguez, E., additional, Lampens, P., additional, Klingenberg, G., additional, Farrell, J. A., additional, Fumagalli, F., additional, Simonetti, J. H., additional, Wolf, M., additional, Santacana, G., additional, Zhou, A.-Y., additional, Michel, R., additional, Fox-Machado, L., additional, Alvarez, M., additional, Nava-Vega, A., additional, López-González, M. J., additional, Casanova, V. M., additional, Aceituno, F. J., additional, Scheggia, I., additional, Rives, J.-J., additional, Hintz, E. G., additional, Van Cauteren, P., additional, Helvaci, M., additional, Yesilyaprak, C., additional, Graham, K. A., additional, Král, L., additional, Kocián, R., additional, Kučáková, H., additional, Fauvaud, M., additional, Granslo, B. H., additional, Michelet, J., additional, Nicholson, M. P., additional, Vugnon, J.-M., additional, Kotková, L., additional, Truparová, K., additional, Ulusoy, C., additional, Yasarsoy, B., additional, Avdibegovic, A., additional, Blaĭek, M., additional, Kliner, J., additional, Zasche, P., additional, Bartošíková, S., additional, Vilášek, M., additional, Trondal, O., additional, Van Den Abbeel, F., additional, Behrend, R., additional, and Wücher, H., additional

Published
2010
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46. Photometry and models of selected main belt asteroids

Author

Marciniak, A., primary, Michałowski, T., additional, Hirsch, R., additional, Behrend, R., additional, Bernasconi, L., additional, Descamps, P., additional, Colas, F., additional, Sobkowiak, K., additional, Kamiński, K., additional, Kryszczyńska, A., additional, Kwiatkowski, T., additional, Polińska, M., additional, Rudawska, R., additional, Fauvaud, S., additional, Santacana, G., additional, Bruno, A., additional, Fauvaud, M., additional, Teng-Chuen-Yu, J.-P., additional, and Peyrot, A., additional

Published
2009
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47. A giant crater on 90 Antiope?

Author

Descamps, P., primary, Marchis, F., additional, Michalowski, T., additional, Berthier, J., additional, Pollock, J., additional, Wiggins, P., additional, Birlan, M., additional, Colas, F., additional, Vachier, F., additional, Fauvaud, S., additional, Fauvaud, M., additional, Sareyan, J.-P., additional, Pilcher, F., additional, and Klinglesmith, D.A., additional

Published
2009
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48. Asteroid models from combined sparse and dense photometric data

Author

Ďurech, J., primary, Kaasalainen, M., additional, Warner, B. D., additional, Fauerbach, M., additional, Marks, S. A., additional, Fauvaud, S., additional, Fauvaud, M., additional, Vugnon, J.-M., additional, Pilcher, F., additional, Bernasconi, L., additional, and Behrend, R., additional

Published
2008
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49. Photometry and models of selected main belt asteroids

Author

Marciniak, A., primary, Michałowski, T., additional, Kaasalainen, M., additional, Ďurech, J., additional, Polińska, M., additional, Kwiatkowski, T., additional, Kryszczyńska, A., additional, Hirsch, R., additional, Kamiński, K., additional, Fagas, M., additional, Colas, F., additional, Fauvaud, S., additional, Santacana, G., additional, Behrend, R., additional, and Roy, R., additional

Published
2007
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50. The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

Author

Rodríguez, E., primary, Fauvaud, S., additional, Farrell, J. A., additional, Zhou, A.-Y., additional, Sareyan, J.-P., additional, López-González, M. J., additional, Dupret, M.-A., additional, Grigahcéne, A., additional, de Ridder, J., additional, Klingenberg, G., additional, Wolf, M., additional, Van Cauteren, P., additional, Lampens, P., additional, Martínez, D., additional, Casanova, V. M., additional, Aceituno, F. J., additional, Helvaci, M., additional, Hintz, E. G., additional, Král, L., additional, Fumagalli, F., additional, Simonetti, J. H., additional, Granslo, B. H., additional, Kotková, L., additional, Santacana, G., additional, Michelet, J., additional, Fauvaud, M., additional, Vugnon, J.-M., additional, Sadsaoud, H., additional, Aliouane, S., additional, Grigahcéne, Z. C., additional, Martín-Ruíz, S., additional, Amado, P. J., additional, Suárez, J. C., additional, Moya, A., additional, Kučáková, H., additional, Kocián, R., additional, Truparová, K., additional, Avdibegović, A., additional, Blažek, M., additional, Kliner, J., additional, Zasche, P., additional, Vilásek, M., additional, Bartošíková, S., additional, Yasarsoy, B., additional, Ulusoy, C., additional, Graham, K. A., additional, Nicholson, M. P., additional, Trondal, O., additional, Yesilyaprak, C., additional, and Coker, D., additional

Published
2007
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