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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. Photomeric analysis of eclipsing binaries: VY UMI, RU UMI AND GSC 04364-00648

Author

Kudak, V., Parimucha, Š., Perig, V., and Gajdoš, P.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the photometric analysis of \textit{BVR} and \textit{TESS} light curves of three eclipsing binaries (RU~UMi and purely studied VY~UMi, GSC 04364-00648), together with their period changes considering archival data and new minima times from our and \textit{TESS} observations. For the first time we detected wave-like variations with low-amplitude in $O-C$ residua of RU UMi, which can be interpreted as a consequence of the light-time effect caused by the 3rd invisible component with period 7370 days. Period increase with rate 2.56(9)$\times10^{-7}$~d/yr$^{-1}$ detected in the VY UMi system corresponds to mass transfer from the secondary to the primary component. For GSC 04364-00648 binary system we find some quadratic changes on the $O-C$ diagram, which corresponds to a period decrease with a high rate of $-2.26(5)\times10^{-5}$~d/yr$^{-1}$. We cannot assumptions about their nature, mainly due to short time of observation and uneven coverage of $O-C$ diagram. We also determined the absolute parameter of their components using the photometric solution and \textit{GAIA} distances., Comment: accepted to REVISTA MEXICANA DE ASTRONOM\'IA Y ASTROF\'ISICA. arXiv admin note: text overlap with arXiv:2102.09839

Published
2023
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3. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author

Santos-Sanz, P., Ortiz, J. L., Sicardy, B., Popescu, M., Benedetti-Rossi, G., Morales, N., Vara-Lubiano, M., Camargo, J. I. B., Pereira, C. L., Rommel, F. L., Assafin, M., Desmars, J., Braga-Ribas, F., Duffard, R., Oliveira, J. Marques, Vieira-Martins, R., Fernández-Valenzuela, E., Morgado, B. E., Acar, M., Anghel, S., Atalay, E., Ateş, A., Bakış, H., Bakış, V., Eker, Z., Erece, O., Kaspi, S., Kayhan, C., Kilic, S. E., Kilic, Y., Manulis, I., Nedelcu, D. A., Niaei, M. S., Nir, G., Ofek, E., Ozisik, T., Petrescu, E., Satir, O., Solmaz, A., Sonka, A., Tekes, M., Unsalan, O., Yesilyaprak, C., Anghel, R., Berteşteanu, D., Curelaru, L., Danescu, C., Dumitrescu, V., Gherase, R., Hudin, L., Stoian, A-M., Tercu, J. O., Truta, R., Turcu, V., Vantdevara, C., Belskaya, I., Dementiev, T. O., Gazeas, K., Karampotsiou, S., Kashuba, V., Kiss, Cs., Koshkin, N., Kozhukhov, O. M., Krugly, Y., Lecacheux, J., Pal, A., Püsküllü, Ç., Szakats, R., Zhukov, V., Bamberger, D., Mondon, B., Perelló, C., Pratt, A., Schnabel, C., Selva, A., Teng, J. P., Tigani, K., Tsamis, V., Weber, C., Wells, G., Kalkan, S., Kudak, V., Marciniak, A., Ogloza, W., Ozdemir, T., Pakstiene, E., Perig, V., and Zejmo, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Within our international program to obtain accurate physical properties of trans-Neptunian objects (TNOs) we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 (mG = 11.5 mag.) for March 18, 2019. After an extensive observational campaign, we updated the prediction and it turned out to be favorable to central Europe. Therefore, we mobilized half a hundred professional and amateur astronomers, and the occultation was finally detected from 21 telescopes located at 18 sites. This makes the Huya event one of the best ever observed stellar occultation by a TNO in terms of the number of chords. We determine accurate size, shape, and geometric albedo, and we also provide constraints on the density and other internal properties of this TNO. The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are (a', b') = (217.6 $\pm$ 3.5 km, 194.1 $\pm$ 6.1 km) with a position angle of the minor axis P' = 55.2 $\pm$ 9.1 degrees. From this fit, the projected area-equivalent diameter is 411.0 $\pm$ 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques (D = 406 $\pm$ 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya (p$\rm_V$ = 0.079 $\pm$ 0.004) and we explored possible 3D shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya is constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about p$_{\rm surf}$ = 10 nbar., Comment: Accepted for publication in Astronomy & Astrophysics (30-April-2022). 19 pages, 7 figures

Published
2022
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4. Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves

Author

Wilawer, E., Oszkiewicz, D., Kryszczyńska, A., Marciniak, A., Shevchenko, V., Belskaya, I., Kwiatkowski, T., Kankiewicz, P., Horbowicz, J., Kudak, V., Kulczak, P., Perig, V., and Sobkowiak, K.

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

The amount of sparse asteroid photometry being gathered by both space- and ground-based surveys is growing exponentially. This large volume of data poses a computational challenge owing to both the large amount of information to be processed and the new methods needed to combine data from different sources (e.g. obtained by different techniques, in different bands, and having different random and systematic errors). The main goal of this work is to develop an algorithm capable of merging sparse and dense data sets, both relative and differential, in preparation for asteroid observations originating from, for example, Gaia, TESS, ATLAS, LSST, K2, VISTA, and many other sources. We present a novel method to obtain asteroid phase curves by combining sparse photometry and differential ground-based photometry. In the traditional approach, the latter cannot be used for phase curves. Merging those two data types allows for the extraction of phase-curve information for a growing number of objects. Our method is validated for 26 sample asteroids observed by the Gaia mission., Comment: 10 pages, 7 figures (supplementary material: 20 pages, 58 figures)

Published
2022
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5. 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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6. A photometric study of two neglected eclipsing binaries

Author

Kudak, V., Fedurco, M., Perig, V., and Parimucha, Š.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the first BVR photometry, period variation, and photometric light-curve analysis of two poorly studied eclipsing binaries V1321 Cyg and CR Tau. Observations were carried out from November 2017 to January 2020 at the observatory of Uzhhorod National University. Period variations were studied using all available early published as well as our minima times. We have used newly developed ELISa code for the light curve analysis and determination of photometric parameters of both systems. We found that V1321 Cyg is a close detached eclipsing system with a low photometric mass ratio of $q=0.28$ which suggests that the binary is a post mass transfer system. No significant period changes in this system are detected. CR Tau is, on the other hand, a semi-detached system where the secondary component almost fills its Roche lobe. We detected a long-term period increase at a rate of $1.49 \times 10^{-7} d/y$, which support mass transfer from lower mass secondary component to the more massive primary.

Published
2021
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7. 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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8. 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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12. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author

Santos-Sanz, P., primary, Ortiz, J. L., additional, Sicardy, B., additional, Popescu, M., additional, Benedetti-Rossi, G., additional, Morales, N., additional, Vara-Lubiano, M., additional, Camargo, J. I. B., additional, Pereira, C. L., additional, Rommel, F. L., additional, Assafin, M., additional, Desmars, J., additional, Braga-Ribas, F., additional, Duffard, R., additional, Marques Oliveira, J., additional, Vieira-Martins, R., additional, Fernández-Valenzuela, E., additional, Morgado, B. E., additional, Acar, M., additional, Anghel, S., additional, Atalay, E., additional, Ateş, A., additional, Bakiş, H., additional, Bakis, V., additional, Eker, Z., additional, Erece, O., additional, Kaspi, S., additional, Kayhan, C., additional, Kilic, S. E., additional, Kilic, Y., additional, Manulis, I., additional, Nedelcu, D. A., additional, Niaei, M. S., additional, Nir, G., additional, Ofek, E., additional, Ozisik, T., additional, Petrescu, E., additional, Satir, O., additional, Solmaz, A., additional, Sonka, A., additional, Tekes, M., additional, Unsalan, O., additional, Yesilyaprak, C., additional, Anghel, R., additional, Berteşteanu, D., additional, Curelaru, L., additional, Danescu, C., additional, Dumitrescu, V., additional, Gherase, R., additional, Hudin, L., additional, Stoian, A-M., additional, Tercu, J. O., additional, Truta, R., additional, Turcu, V., additional, Vantdevara, C., additional, Belskaya, I., additional, Dementiev, T. O., additional, Gazeas, K., additional, Karampotsiou, S., additional, Kashuba, V., additional, Kiss, Cs., additional, Koshkin, N., additional, Kozhukhov, O. M., additional, Krugly, Y., additional, Lecacheux, J., additional, Pal, A., additional, Püsküllü, Ç., additional, Szakats, R., additional, Zhukov, V., additional, Bamberger, D., additional, Mondon, B., additional, Perelló, C., additional, Pratt, A., additional, Schnabel, C., additional, Selva, A., additional, Teng, J. P., additional, Tigani, K., additional, Tsamis, V., additional, Weber, C., additional, Wells, G., additional, Kalkan, S., additional, Kudak, V., additional, Marciniak, A., additional, Ogloza, W., additional, Özdemir, T., additional, Pakštiene, E., additional, Perig, V., additional, and Żejmo, M., additional

Published
2022
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13. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author

Santos-Sanz, P. Ortiz, J.L. Sicardy, B. Popescu, M. Benedetti-Rossi, G. Morales, N. Vara-Lubiano, M. Camargo, J.I.B. Pereira, C.L. Rommel, F.L. Assafin, M. Desmars, J. Braga-Ribas, F. Duffard, R. Marques Oliveira, J. Vieira-Martins, R. Fernández-Valenzuela, E. Morgado, B.E. Acar, M. Anghel, S. Atalay, E. Ateş, A. Bakış, H. Bakıs, V. Eker, Z. Erece, O. Kaspi, S. Kayhan, C. Kilic, S.E. Kilic, Y. Manulis, I. Nedelcu, D.A. Niaei, M.S. Nir, G. Ofek, E. Ozisik, T. Petrescu, E. Satir, O. Solmaz, A. Sonka, A. Tekes, M. Unsalan, O. Yesilyaprak, C. Anghel, R. Berteşteanu, D. Curelaru, L. Danescu, C. Dumitrescu, V. Gherase, R. Hudin, L. Stoian, A.-M. Tercu, J.O. Truta, R. Turcu, V. Vantdevara, C. Belskaya, I. Dementiev, T.O. Gazeas, K. Karampotsiou, S. Kashuba, V. Kiss, Cs. Koshkin, N. Kozhukhov, O.M. Krugly, Y. Lecacheux, J. Pal, A. Püsküllü, Ç. Szakats, R. Zhukov, V. Bamberger, D. Mondon, B. Perelló, C. Pratt, A. Schnabel, C. Selva, A. Teng, J.P. Tigani, K. Tsamis, V. Weber, C. Wells, G. Kalkan, S. Kudak, V. Marciniak, A. Ogłoza, W. Özdemir, T. Pakštienė, E. Perig, V. Żejmo, M. and Santos-Sanz, P. Ortiz, J.L. Sicardy, B. Popescu, M. Benedetti-Rossi, G. Morales, N. Vara-Lubiano, M. Camargo, J.I.B. Pereira, C.L. Rommel, F.L. Assafin, M. Desmars, J. Braga-Ribas, F. Duffard, R. Marques Oliveira, J. Vieira-Martins, R. Fernández-Valenzuela, E. Morgado, B.E. Acar, M. Anghel, S. Atalay, E. Ateş, A. Bakış, H. Bakıs, V. Eker, Z. Erece, O. Kaspi, S. Kayhan, C. Kilic, S.E. Kilic, Y. Manulis, I. Nedelcu, D.A. Niaei, M.S. Nir, G. Ofek, E. Ozisik, T. Petrescu, E. Satir, O. Solmaz, A. Sonka, A. Tekes, M. Unsalan, O. Yesilyaprak, C. Anghel, R. Berteşteanu, D. Curelaru, L. Danescu, C. Dumitrescu, V. Gherase, R. Hudin, L. Stoian, A.-M. Tercu, J.O. Truta, R. Turcu, V. Vantdevara, C. Belskaya, I. Dementiev, T.O. Gazeas, K. Karampotsiou, S. Kashuba, V. Kiss, Cs. Koshkin, N. Kozhukhov, O.M. Krugly, Y. Lecacheux, J. Pal, A. Püsküllü, Ç. Szakats, R. Zhukov, V. Bamberger, D. Mondon, B. Perelló, C. Pratt, A. Schnabel, C. Selva, A. Teng, J.P. Tigani, K. Tsamis, V. Weber, C. Wells, G. Kalkan, S. Kudak, V. Marciniak, A. Ogłoza, W. Özdemir, T. Pakštienė, E. Perig, V. Żejmo, M.

Published
2022

14. OUP accepted manuscript

Author

Wilawer, E, primary, Oszkiewicz, D, additional, Kryszczyńska, A, additional, Marciniak, A, additional, Shevchenko, V, additional, Belskaya, I, additional, Kwiatkowski, T, additional, Kankiewicz, P, additional, Horbowicz, J, additional, Kudak, V, additional, Kulczak, P, additional, Perig, V, additional, and Sobkowiak, K, additional

Published
2022
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15. 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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17. 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

18. Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves.

Author

Wilawer, E, Oszkiewicz, D, Kryszczyńska, A, Marciniak, A, Shevchenko, V, Belskaya, I, Kwiatkowski, T, Kankiewicz, P, Horbowicz, J, Kudak, V, Kulczak, P, Perig, V, and Sobkowiak, K

Subjects
LIGHT curves, ASTEROID detection, ASTEROIDS, SMALL solar system bodies, DATA mining, PHOTOMETRY
Abstract

The amount of sparse asteroid photometry being gathered by both space- and ground-based surveys is growing exponentially. This large volume of data poses a computational challenge owing to both the large amount of information to be processed and the new methods needed to combine data from different sources (e.g. obtained by different techniques, in different bands, and having different random and systematic errors). The main goal of this work is to develop an algorithm capable of merging sparse and dense data sets, both relative and differential, in preparation for asteroid observations originating from, for example, Gaia ,  TESS , ATLAS, LSST, K2 , VISTA, and many other sources. We present a novel method to obtain asteroid phase curves by combining sparse photometry and differential ground-based photometry. In the traditional approach, the latter cannot be used for phase curves. Merging those two data types allows for the extraction of phase-curve information for a growing number of objects. Our method is validated for 26 sample asteroids observed by the Gaia mission. [ABSTRACT FROM AUTHOR]

Published
2022
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19. Фотометрия близкого к земле астероида Florence (3122)

Author

Kudak, V., Perig, V., and Verbitsky, S.

Subjects
Asteroid, Photometry, Light curve, Period, Астероїд, Фотометрія, Крива блиску, Період, 520:52.14, Астероид, Фотометрия, Кривая блеска, Период
Abstract

Фотометрія астероїда Florence (3122), що наближався до Землі, виконувалася протягом двох ночей у серпні та двох ночей у вересні 2017 р. з обсерваторій на заході України - Лабораторії космічних досліджень Ужгородського національного університету та аматорської обсерваторії поблизу міста Тернопіль. Представлено короткий огляд визначення періоду астероїда Florence (3122) іншими авторами. Наведена крива блиску, отримана з даних спостережень. Період обертання астероїдів визначався програмою MPO Canopus. Отриманий період обертання підтверджує раніше опубліковані значення. Описано причини що привели до визначення двох дещо відмінних періодів впродовж двох сеансів спостережень., Фотометрия астероида Florence (3122), приближающийся к Земле, выполнялась в течение двух ночей в августе и двух ночей в сентябре 2017 из обсерваторий на западе Украины - Лаборатории космических исследований Ужгородского национального университета и любительской обсерватории близ города Тернополь. Представлены краткий обзор определения периода астероида Florence (3122) другими авторами. Приведенная кривая блеска, полученная по данным наблюдений. Период вращения астероидов определялся программой MPO Canopus. Полученный период обращения подтверждает ранее опубликованные значения. Описаны причины, приводящие к определению двух несколько отличных периодов в течение двух сеансов наблюдений., Purpose. The purpose of this work is investigation of asteroid period of own rotation in moment of its close approach to Earth. Increased brightness of the object create an opportunity to find hidden new aspects of asteroid surface based on higher signal noise ratio and better precision of photometry. Methods. In this work we use methods of CCD photometry. Observations were made on two telescopes with diameter 40 and 35 cm at different observatories.Results. Photometry of near Earth asteroid Florence (3122) is performed during two nights in August and two nights in September 2017 from observatories in west of Ukraine — Laboratory of space research of Uzhhorod National University and amateur observatory in Ternopil. Brief overview of Florence period determination by other authors is given. Light curves obtained from observation data are presented. Periods of asteroid rotation were defined by MPO Canopus software.Conclusions. Determined periods of rotation confirm previously published values. Presented period precisions are better than published before. Two different periods obtained on two observation sessions. Reasons of these results are described. No hidden aspects of asteroid surface were identified because of too fast phase angle change, also two light curves is not enough for such task salvation.

Published
2018

20. 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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21. 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

23. Фотометрія близького до землі астероїда Florence (3122)

Author

Kudak, V.; Лабораторія космічних досліджень Ужгородського національного університету, Perig, V.; Лабораторія космічних досліджень Ужгородського національного університету, Verbitsky, S.; “White Swong” company, Kudak, V.; Лабораторія космічних досліджень Ужгородського національного університету, Perig, V.; Лабораторія космічних досліджень Ужгородського національного університету, and Verbitsky, S.; “White Swong” company

Abstract

Фотометрія астероїда Florence (3122), що наближався до Землі, виконувалася протягом двох ночей у серпні та двох ночей у вересні 2017 р. з обсерваторій на заході України - Лабораторії космічних досліджень Ужгородського національного університету та аматорської обсерваторії поблизу міста Тернопіль. Представлено короткий огляд визначення періоду астероїда Florence (3122) іншими авторами. Наведена крива блиску, отримана з даних спостережень. Період обертання астероїдів визначався програмою MPO Canopus. Отриманий період обертання підтверджує раніше опубліковані значення. Описано причини що привели до визначення двох дещо відмінних періодів впродовж двох сеансів спостережень., Фотометрия астероида Florence (3122), приближающийся к Земле, выполнялась в течение двух ночей в августе и двух ночей в сентябре 2017 из обсерваторий на западе Украины - Лаборатории космических исследований Ужгородского национального университета и любительской обсерватории близ города Тернополь. Представлены краткий обзор определения периода астероида Florence (3122) другими авторами. Приведенная кривая блеска, полученная по данным наблюдений. Период вращения астероидов определялся программой MPO Canopus. Полученный период обращения подтверждает ранее опубликованные значения. Описаны причины, приводящие к определению двух несколько отличных периодов в течение двух сеансов наблюдений., Purpose. The purpose of this work is investigation of asteroid period of own rotation in moment of its close approach to Earth. Increased brightness of the object create an opportunity to find hidden new aspects of asteroid surface based on higher signal noise ratio and better precision of photometry. Methods. In this work we use methods of CCD photometry. Observations were made on two telescopes with diameter 40 and 35 cm at different observatories.Results. Photometry of near Earth asteroid Florence (3122) is performed during two nights in August and two nights in September 2017 from observatories in west of Ukraine — Laboratory of space research of Uzhhorod National University and amateur observatory in Ternopil. Brief overview of Florence period determination by other authors is given. Light curves obtained from observation data are presented. Periods of asteroid rotation were defined by MPO Canopus software.Conclusions. Determined periods of rotation confirm previously published values. Presented period precisions are better than published before. Two different periods obtained on two observation sessions. Reasons of these results are described. No hidden aspects of asteroid surface were identified because of too fast phase angle change, also two light curves is not enough for such task salvation.

Published
2018

24. MINIMA TIMES OF SELECTED ECLIPSING BINARIES.

Author

PARIMUCHA, Š, DUBOVSKÝ, P., KUDAK, V., and PERIG, V.

Subjects
BINARY stars, ECLIPSING binaries, MAXIMA & minima, CHARTS, diagrams, etc.
Abstract

A chart is presented depicting the observations of the minima times of chosen eclipsing binaries including the LO and GZ Andromedae and the V728 Herculis wherein the photometry was conducted using the C-Munipack package.

Published
2016

26. Comet C/2014 W11 (panstarrs)

Author

Johnson, J. A., Christensen, E. J., Gibbs, A. R., Grauer, A. D., Hill, R. E., Kowalski, R. A., Larson, S. M., Matheny, R. G., Shelly, F. C., Durig, D. T., Ikari, Y., Dupouy, P., Vanssay, J. B., Diepvens, A., Linkov, V., Polyakov, K., Savanevych, V., Nevski, V., Gibson, B., Goggia, T., Primak, N., Schultz, A., Willman, M., Kenneth Chambers, Chastel, S., Denneau, L., Flewelling, H., Huber, M., Magnier, E., Schunova, E., Wainscoat, R., Waters, C., Weryk, R., Sato, H., Lau, P. S., Kudak, V. I., Perig, V. M., Hudin, L., Namkhai, T., Schmalz, S., Ligustri, R., Maury, A., Noel, T., Soulier, J. -F, Bosch, J. -G, and Williams, G. V.

27. 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., Butkiewicz - Bąk, M., 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., Rondón, 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., Żukowski, K., 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., Butkiewicz - Bąk, M., 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., Rondón, 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.

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 wor

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

Author

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

Abstract

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

29. Scaling slowly rotating asteroids with 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., Butkiewicz-Bąk, M., 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., Könyves-Tóth, R., 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., Żywica, S., 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., Butkiewicz-Bąk, M., 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., Könyves-Tóth, R., 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.

Abstract

Context. As evidenced by recent survey results, the majority of asteroids are slow rotators (spin periods longer than 12 h), but lack spin and shape models because of 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 (>60 km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons. Aims. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 h. 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. Methods. 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 datasets: large bodies tend to saturate in WISE mission detectors. Therefore, we recently also launched a special campaign among stellar occultation observers, both in order to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. Results. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to chords from stellar occultation timings resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution from the pair of two mirror pole solutions, 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. Conclusions. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, for example, constitute a solid basis fo

30. 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., Butkiewicz - Bąk, M., 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., Rondón, 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., Żukowski, K., 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., Butkiewicz - Bąk, M., 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., Rondón, 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.

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 wor

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