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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. The stellar occultation by (319) Leona on 13 September 2023 in preparation for the occultation of Betelgeuse

Author

Ortiz, J. L., Kretlow, M., Schnabel, C., Morales, N., Flores-Martín, J., González, M. Sánchez, Casarramona, F., Selva, A., Perelló, C., Román-Reche, A., Alonso, S., Rizos, J. L., Gonçalves, R., Castillo, A., Madiedo, J. M., Sánchez, P. Martínez, andújar, J. M. Fernández, Maestre, J. L., Smith, E., Gil, M., Pelenjow, V., Soriano, S. Moral, Martí, J., Luque-Escamilla, P. L., Casas, R., Casal, J. Delgado, Rovira, J., Aceituno, F. J., Dekert, V., Guimerá, V. de Ory, Estepa, J. Serrano, Kilic, Y., Leiva, R., Santos-Sanz, P., Duffard, R., Fernández-Valenzuela, E., Vara-Lubiano, M., Alvarez-Candal, A., and Rommel, F. L.

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

On 12 December 2023, the star $\alpha$ Orionis (Betelgeuse) will be occulted by the asteroid (319) Leona. This represents an extraordinary and unique opportunity to analyze the diameter and brightness distribution of Betelgeuse's photosphere with extreme angular resolution by studying the light curve as the asteroid occults the star from different points on Earth and at different wavelengths. Here we present observations of another occultation by Leona on 13 September 2023 to determine its projected shape and size in preparation for the December 12th event. The occultation observation campaign was highly successful. The effective diameter in projected area derived from the positive detections at 17 sites turned out to be 66 km $\pm$ 2 km using an elliptical fit to the instantaneous limb. The body is highly elongated, with dimensions of 79.6 $\pm$ 2.2 km x 54.8 $\pm$ 1.3 km in its long and short axis, respectively, at the occultation time. Also, an accurate position coming from the occultation, to improve the orbit determination of Leona for December 12 is provided., Comment: Two figures. Letter submitted to A&A

Published
2023
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3. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS$_4$ measured from stellar occultations

Author

Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., and Wake, D. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

This work aims at constraining the size, shape, and geometric albedo of the dwarf planet candidate 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also studied the object's topography by analyzing the obtained limb and the residuals between observed chords and the best-fitted ellipse. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with three to up to sixty-one positive chords. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fitted ellipse, combined with the object's rotational information from the literature, constrains the object's size, shape, and albedo. Additionally, we developed a new method to characterize topography features on the object's limb. The global limb has a semi-major axis of 412 $\pm$ 10 km, a semi-minor axis of 385 $\pm$ 17 km, and the position angle of the minor axis is 121 $^\circ$ $\pm$ 16$^\circ$. From this instantaneous limb, we obtained 2002 MS4's geometric albedo and the projected area-equivalent diameter. Significant deviations from the fitted ellipse in the northernmost limb are detected from multiple sites highlighting three distinct topographic features: one 11 km depth depression followed by a 25$^{+4}_{-5}$ km height elevation next to a crater-like depression with an extension of 322 $\pm$ 39 km and 45.1 $\pm$ 1.5 km deep. Our results present an object that is $\approx$138 km smaller in diameter than derived from thermal data, possibly indicating the presence of a so-far unknown satellite. However, within the error bars, the geometric albedo in the V-band agrees with the results published in the literature, even with the radiometric-derived albedo.

Published
2023
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4. 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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5. The 2017 May 20$^{\rm th}$ stellar occultation by the elongated centaur (95626) 2002 GZ$_{32}$

Author

Santos-Sanz, P., Ortiz, J. L., Sicardy, B., Benedetti-Rossi, G., Morales, N., Fernández-Valenzuela, E., Duffard, R., Iglesias-Marzoa, R., Lamadrid, J. L., Maícas, N., Pérez, L., Gazeas, K., Guirado, J. C., Peris, V., Ballesteros, F. J., Organero, F., Ana-Hernández, L., Fonseca, F., Alvarez-Candal, A., Jiménez-Teja, Y., Vara-Lubiano, M., Braga-Ribas, F., Camargo, J. I. B., Desmars, J., Assafin, M., Vieira-Martins, R., Alikakos, J., Boutet, M., Bretton, M., Carbognani, A., Charmandaris, V., Ciabattari, F., Delincak, P., Leiva, A. Fuambuena, González, H., Haymes, T., Hellmich, S., Horbowicz, J., Jennings, M., Kattentidt, B., Kiss, Cs., Komžík, R., Lecacheux, J., Marciniak, A., Moindrot, S., Mottola, S., Pal, A., Paschalis, N., Pastor, S., Perello, C., Pribulla, T., Ratinaud, C., Reyes, J. A., Sanchez, J., Schnabel, C., Selva, A., Signoret, F., Sonbas, E., and Alí-Lagoa, V.

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

We predicted a stellar occultation of the bright star Gaia DR1 4332852996360346368 (UCAC4 385-75921) (m$_{\rm V}$= 14.0 mag) by the centaur 2002 GZ$_{32}$ for 2017 May 20$^{\rm th}$. Our latest shadow path prediction was favourable to a large region in Europe. Observations were arranged in a broad region inside the nominal shadow path. Series of images were obtained with 29 telescopes throughout Europe and from six of them (five in Spain and one in Greece) we detected the occultation. This is the fourth centaur, besides Chariklo, Chiron and Bienor, for which a multi-chord stellar occultation is reported. By means of an elliptical fit to the occultation chords we obtained the limb of 2002 GZ$_{32}$ during the occultation, resulting in an ellipse with axes of 305 $\pm$ 17 km $\times$ 146 $\pm$ 8 km. From this limb, thanks to a rotational light curve obtained shortly after the occultation, we derived the geometric albedo of 2002 GZ$_{32}$ ($p_{\rm V}$ = 0.043 $\pm$ 0.007) and a 3-D ellipsoidal shape with axes 366 km $\times$ 306 km $\times$ 120 km. This shape is not fully consistent with a homogeneous body in hydrostatic equilibrium for the known rotation period of 2002 GZ$_{32}$. The size (albedo) obtained from the occultation is respectively smaller (greater) than that derived from the radiometric technique but compatible within error bars. No rings or debris around 2002 GZ$_{32}$ were detected from the occultation, but narrow and thin rings cannot be discarded., Comment: Accepted for publication in MNRAS (8-Dec.-2020), 15 pages, 9 figures

Published
2020
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6. The large Trans-Neptunian Object 2002 TC$_{302}$ from combined stellar occultation, photometry and astrometry data

Author

Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Duffard, R., Morales, N., Braga-Ribas, F., Fernández-Valenzuela, E., Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, L., Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J. M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Canto, E. Dal, Masucci, M., Vara-Lubiano, M., Gutiérrez, P. J., Desmars, J., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Beisker, W., Behrend, R., Mueller, T. G., Meza, E., Gomes-Junior, A. R., Roques, F., Vachier, F., Mottola, S., Hellmich, S., Bagatin, A. Campo, Alvarez-Candal, A., Cikota, S., Cikota, A., Christille, J. M., Pál, A., Kiss, C., Pribulla, T., Komžík, R., Madiedo, J. M., Charmandaris, V., Alikakos, J., Szakáts, R., Farkas-Takács, A., Varga-Verebélyi, E., Marton, G., Marciniak, A., Bartczak, P., Butkiewicz-Bak, M., Dudziński, G., Alí-Lagoa, V., Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J. C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., and Morrone, L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

On 28th January 2018, the large Trans-Neptunian Object (TNO) 2002TC302 occulted a m$_v= $15.3 star with ID 130957813463146112 in the Gaia DR2 stellar catalog. 12 positive occultation chords were obtained from Italy, France, Slovenia and Switzerland. Also, 4 negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto, in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body, compatible with the near misses, can be obtained. The resulting ellipse has major and minor axes of 543 $\pm$ 18 km and 460 $\pm$ 11 km, respectively, with a position angle of 3 $\pm$ 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5m telescope at Sierra Nevada Observatory and the 1.23m telescope at Calar Alto observatory, allows us to derive possible 3D shapes and density estimations for the body, based on hydrostatic equilibrium assumptions. The effective area equivalent diameter is $\sim$ 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to $\sim$ 300 km in diameter, to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also appears to be consistent with other ground-based data presented here. From the effective occultation diameter combined with H$_V$ measurements we derive a geometric albedo of 0.147 $\pm$ 0.005, which would be somewhat smaller if 2002TC302 has a satellite. The best occultation light curves do not show any signs of ring features or any signatures of a global atmosphere., Comment: Accepted for publication in Astronomy & Astrophysics. 14 pages, 9 figures

Published
2020
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7. The stellar occultation by (319) Leona on 13 September 2023 in preparation for the occultation of Betelgeuse

Author

Ortiz, J L, primary, Kretlow, M, additional, Schnabel, C, additional, Morales, N, additional, Flores-Martín, J, additional, González, M Sánchez, additional, Casarramona, F, additional, Selva, A, additional, Perelló, C, additional, Román-Reche, A, additional, Alonso, S, additional, Rizos, J L, additional, Gonçalves, R, additional, Castillo, A, additional, Madiedo, J M, additional, Sánchez, P Martínez, additional, Andújar, J M Fernández, additional, Maestre, J L, additional, Smith, E, additional, Gil, M, additional, Pelenjow, V, additional, Soriano, S Moral, additional, Martí, J, additional, Luque-Escamilla, P L, additional, Casas, R, additional, Casal, J Delgado, additional, Rovira, J, additional, Aceituno, F J, additional, Dekert, V, additional, Farfan, R G, additional, de Ory Guimerá, V, additional, Estepa, J Serrano, additional, Jehin, E, additional, Ferrais, M, additional, Alarcon, M R, additional, Licandro, J, additional, Serra-Ricart, M, additional, Gutiérrez, P J, additional, Kilic, Y, additional, Leiva, R, additional, Santos-Sanz, P, additional, Duffard, R, additional, Fernández-Valenzuela, E, additional, Vara-Lubiano, M, additional, Alvarez-Candal, A, additional, and Rommel, F L, additional

Published
2023
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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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9. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author

Rommel, F. L., primary, Braga-Ribas, F., additional, Ortiz, J. L., additional, Sicardy, B., additional, Santos-Sanz, P., additional, Desmars, J., additional, Camargo, J. I. B., additional, Vieira-Martins, R., additional, Assafin, M., additional, Morgado, B. E., additional, Boufleur, R. C., additional, Benedetti-Rossi, G., additional, Gomes-Júnior, A. R., additional, Fernández-Valenzuela, E., additional, Holler, B. J., additional, Souami, D., additional, Duffard, R., additional, Margoti, G., additional, Vara-Lubiano, M., additional, Lecacheux, J., additional, Plouvier, J. L., additional, Morales, N., additional, Maury, A., additional, Fabrega, J., additional, Ceravolo, P., additional, Jehin, E., additional, Albanese, D., additional, Mariey, H., additional, Cikota, S., additional, Ruždjak, D., additional, Cikota, A., additional, Szakáts, R., additional, Baba Aissa, D., additional, Gringahcene, Z., additional, Kashuba, V., additional, Koshkin, N., additional, Zhukov, V., additional, Fişek, S., additional, Çakir, O., additional, Özer, S., additional, Schnabel, C., additional, Schnabel, M., additional, Signoret, F., additional, Morrone, L., additional, Santana-Ros, T., additional, Pereira, C. L., additional, Emilio, M., additional, Burdanov, A. Y., additional, de Wit, J., additional, Barkaoui, K., additional, Gillon, M., additional, Leto, G., additional, Frasca, A., additional, Catanzaro, G., additional, Sanchez, R. Zanmar, additional, Tagliaferri, U., additional, Di Sora, M., additional, Isopi, G., additional, Krugly, Y., additional, Slyusarev, I., additional, Chiorny, V., additional, Mikuž, H., additional, Bacci, P., additional, Maestripieri, M., additional, Grazia, M. D., additional, de la Cueva, I., additional, Yuste-Moreno, M., additional, Ciabattari, F., additional, Kozhukhov, O. M., additional, Serra-Ricart, M., additional, Alarcon, M. R., additional, Licandro, J., additional, Masi, G., additional, Bacci, R., additional, Bosch, J. M., additional, Behem, R., additional, Prost, J.-P., additional, Renner, S., additional, Conjat, M., additional, Bachini, M., additional, Succi, G., additional, Stoian, L., additional, Juravle, A., additional, Carosati, D., additional, Gowe, B., additional, Carrillo, J., additional, Zheleznyak, A. P., additional, Montigiani, N., additional, Foster, C. R., additional, Mannucci, M., additional, Ruocco, N., additional, Cuevas, F., additional, Di Marcantonio, P., additional, Coretti, I., additional, Iafrate, G., additional, Baldini, V., additional, Collins, M., additional, Pál, A., additional, Csák, B., additional, Fernández-Garcia, E., additional, Castro-Tirado, A. J., additional, Hudin, L., additional, Madiedo, J. M., additional, Anghel, R. M., additional, Calvo-Fernández, J. F., additional, Valvasori, A., additional, Guido, E., additional, Gherase, R. M., additional, Kamoun, S., additional, Fafet, R., additional, Sánchez-González, M., additional, Curelaru, L., additional, Vîntdevară, C. D., additional, Danescu, C. A., additional, Gout, J.-F., additional, Schmitz, C. J., additional, Sota, A., additional, Belskaya, I., additional, Rodríguez-Marco, M., additional, Kilic, Y., additional, Frappa, E., additional, Klotz, A., additional, Lavayssière, M., additional, Oliveira, J. Marques, additional, Popescu, M., additional, Mammana, L. A., additional, Fernández-Lajús, E., additional, Schmidt, M., additional, Hopp, U., additional, Komžík, R., additional, Pribulla, T., additional, Tomko, D., additional, Husárik, M., additional, Erece, O., additional, Eryilmaz, S., additional, Buzzi, L., additional, Gährken, B., additional, Nardiello, D., additional, Hornoch, K., additional, Sonbas, E., additional, Er, H., additional, Burwitz, V., additional, Sybilski, P. Waldemar, additional, Bykowski, W., additional, Müller, T. G., additional, Ogloza, W., additional, Gonçalves, R., additional, Ferreira, J. F., additional, Ferreira, M., additional, Bento, M., additional, Meister, S., additional, Bagiran, M. N., additional, Tekeş, M., additional, Marciniak, A., additional, Moravec, Z., additional, Delinčák, P., additional, Gianni, G., additional, Casalnuovo, G. B., additional, Boutet, M., additional, Sanchez, J., additional, Klemt, B., additional, Wuensche, N., additional, Burzynski, W., additional, Borkowski, M., additional, Serrau, M., additional, Dangl, G., additional, Klös, O., additional, Weber, C., additional, Urbaník, M., additional, Rousselot, L., additional, Kubánek, J., additional, André, P., additional, Colazo, C., additional, Spagnotto, J., additional, Sickafoose, A. A., additional, Hueso, R., additional, Sánchez-Lavega, A., additional, Fisher, R. S., additional, Rengstorf, A. W., additional, Perelló, C., additional, Dascalu, M., additional, Altan, M., additional, Gazeas, K., additional, de Santana, T., additional, Sfair, R., additional, Winter, O. C., additional, Kalkan, S., additional, Canales-Moreno, O., additional, Trigo-Rodríguez, J. M., additional, Tsamis, V., additional, Tigani, K., additional, Sioulas, N., additional, Lekkas, G., additional, Bertesteanu, D. N., additional, Dumitrescu, V., additional, Wilberger, A. J., additional, Barnes, J. W., additional, Fieber-Beyer, S. K., additional, Swaney, R. L., additional, Fuentes, C., additional, Mendez, R. A., additional, Dumitru, B. D., additional, Flynn, R. L., additional, and Wake, D. A., additional

Published
2023
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10. The stellar occultation by (319) Leona on 2023 September 13 in preparation for the occultation of Betelgeuse.

Author

Ortiz, J L, Kretlow, M, Schnabel, C, Morales, N, Flores-Martín, J, Sánchez González, M, Casarramona, F, Selva, A, Perelló, C, Román-Reche, A, Alonso, S, Rizos, J L, Gonçalves, R, Castillo, A, Madiedo, J M, Martínez Sánchez, P, Fernández Andújar, J M, Maestre, J L, Smith, E, and Gil, M

Subjects
OCCULTATIONS (Astronomy), LIGHT curves, SMALL solar system bodies, TIME series analysis, ASTEROIDS, ORBITS (Astronomy), PHOTOMETRY
Abstract

On 2023 December 12, the star α Orionis will be occulted by asteroid (319) Leona. This represents an extraordinary and unique opportunity to analyse the brightness distribution of Betelgeuse's photosphere with extreme angular resolution by studying light curves from different points on Earth and at different wavelengths. Here we present observations of another occultation by asteroid Leona, on 2023 September 13, whose goal was to determine Leona's projected shape and size in preparation for the December 12th event and its interpretation. The occultation campaign was highly successful with 25 positive detections from 17 different sites and a near miss. The effective diameter in projected area derived from the positive detections was 66 ± 2 km using an elliptical fit to the instantaneous limb. The body is highly elongated, with dimensions of 79.6 ± 2.2 km × 54.8 ± 1.3 km in its long and short axis, respectively, at occultation time. This result, in combination with dense time series photometry of Leona that we recently obtained, together with archival sparse photometry, allowed us to predict the angular size of the asteroid for the Betelgeuse event and to simulate the expected brightness change. Also, an accurate position coming from the occultation is provided, to improve the orbit of Leona. [ABSTRACT FROM AUTHOR]

Published
2024
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13. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, B., Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Burwitz, V., Waldemar Sybilski, P., Bykowski, W., Müller, Thomas G., Ogloza, W., Gonçalves, R., Ferreira, J.F., Ferreira, M., Bento, M., Urbaník, M., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Holler, B.J., Er, H., Weber, C., Kalkan, S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, B., Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Burwitz, V., Waldemar Sybilski, P., Bykowski, W., Müller, Thomas G., Ogloza, W., Gonçalves, R., Ferreira, J.F., Ferreira, M., Bento, M., Urbaník, M., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Holler, B.J., Er, H., Weber, C., and Kalkan, S.

Abstract

Context. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs’ fundamental physical properties with high precision, such as size and shape. Aims. This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also study the object’s topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fit ellipse, combined with the object’s rotational information from the literature, sets constraints on the object’s size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object’s limb. Results. The global limb has a semi-major axis of a′ = 412 ± 10 km, a semi-minor axis of b′= 385 ± 17 km, and the position angle of the minor axis is 121° ± 16°. From this instantaneous limb, we obtained 2002 MS4’s geometric albedo of pV = 0.1 ± 0.025, using HV = 3.63 ± 0.05 mag and a projected area-equivalent diameter of 796 ± 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25−5+4 k

Published
2023

16. 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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25. Evolution of the early to late Archean mantle from Hf-Nd-Ce isotope systematics in basalts and komatiites from the Pilbara Craton

Author

Hasenstab, E., Tusch, J., Schnabel, C., Marien, C. S., Van Kranendonk, M. J., Smithies, H., Howard, H., Maier, W. D., Muenker, C., Hasenstab, E., Tusch, J., Schnabel, C., Marien, C. S., Van Kranendonk, M. J., Smithies, H., Howard, H., Maier, W. D., and Muenker, C.

Abstract

Inferences on the early evolution of the Earth's mantle can be deduced from long-lived radiogenic isotope Lu-176-Hf-176 and systems such as Sm-147-Nd-143, for which both parent and daughter elements largely remain immobile at low metamorphic grades. However, it remains ambiguous when and to what extent mantle-crust differentiation processes had started in the Archean. For a better understanding of Archean mantle-crust evolution, we determined the initial Lu-176-Hf-176, Sm-147-Nd-143, and, in a new approach, the La-138-Ce-138 isotope compositions of a suite of Archean mafic-ultramafic rock samples from the 3.53-2.83 Ga old Pilbara Craton and 2.78-2.63 Ga old Fortescue Group in NW Australia. These rocks represent one of the best-preserved Archean successions worldwide and contain mafic-ultramafic rocks that were erupted during repeated and long-lived pulses of volcanism throughout much of the Archean. Mantlederived mafic-ultramafic rock samples were collected from six major stratigraphic groups of the Pilbara Craton and the overlying Fortescue Group in order to characterize the parental mantle source regions of the lavas and to reconstruct the temporal evolution of the ambient mantle beneath this piece of cratonic lithosphere. In addition, we analyzed contemporaneous TTG-like igneous suites and interbedded sediments in order to reconstruct the lithospheric evolution of the Pilbara Craton. The Hf-Nd-Ce isotope data imply the onset of mantle-crust differentiation in the Pilbara Craton as early as similar to 4.2 Ga, well prior to any of the preserved stratigraphy. Within error, coupled Ce-Nd-Hf isotope arrays all intersect chondritic values, implying that the Earth is of broadly chondritic composition, also for the La-138-Ce-138 isotope system. Mafic rocks usually yield strongly coupled epsilon Hf-(i), epsilon Nd-(i) and epsilon Ce-(i) values that form a mixing line between an evolving depleted upper mantle composition and the primitive mantle value (epsilon Hf-(i) ca. 0

Published
2021

28. Baily’s Beads Atlas in 2005 – 2008 Eclipses

Author

Sigismondi, C., Dunham, D. W., Guhl, K., Andersson, S., Bode, H., Canales, O., Colona, P., Farago, O., Fernández-Ocaña, M., Gabel, A., Haupt, M., Herold, C., Nugent, R., Oliva, P., Patel, M., Perello, C., Rothe, W., Rovira, J., Schaefer, T., Schnabel, C., Schwartz, D., Selva, A., Strickling, W., Tegtmeier, A., Tegtmeier, C., Thome, B., and Warren, W. H.

Published
2009
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29. SUERC AMS ion detection

Author

Maden, C., Anastasi, P.A.F., Dougans, A., Freeman, S.P.H.T., Kitchen, R., Klody, G., Schnabel, C., Sundquist, M., Vanner, K., and Xu, S.

Published
2007
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31. The large trans-Neptunian object 2002 TC302 from combined stellar occultation, photometry, and astrometry data

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Duffard, René, Morales Palomino, Nicolás, Braga-Ribas, F., Fernández-Valenzuela, Estela, Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, Luca, Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J.M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Dal Canto, E., Masucci, M., Vara-Lubiano, M., Gutiérrez, P.J., Desmars, Josselin, Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Beisker, W., Behrend, Raoul, Mueller, T.G., Meza, E., Gomes-Junior, A.R., Roques, F., Vachier, Frédéric, Mottola, S., Hellmich, S., Campo Bagatin, Adriano, Alvarez-Candal, Alvaro, Cikota, S., Cikota, A., Christille, J.M., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Madiedo, J.M., Charmandaris, V., Alikakos, J., Szakáts, Róbert, Farkas, Anikó, Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J.C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., Morrone, L., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Duffard, René, Morales Palomino, Nicolás, Braga-Ribas, F., Fernández-Valenzuela, Estela, Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, Luca, Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J.M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Dal Canto, E., Masucci, M., Vara-Lubiano, M., Gutiérrez, P.J., Desmars, Josselin, Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Beisker, W., Behrend, Raoul, Mueller, T.G., Meza, E., Gomes-Junior, A.R., Roques, F., Vachier, Frédéric, Mottola, S., Hellmich, S., Campo Bagatin, Adriano, Alvarez-Candal, Alvaro, Cikota, S., Cikota, A., Christille, J.M., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Madiedo, J.M., Charmandaris, V., Alikakos, J., Szakáts, Róbert, Farkas, Anikó, Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J.C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., and Morrone, L.

Abstract

Context. Deriving physical properties of trans-Neptunian objects is important for the understanding of our Solar System. This requires observational efforts and the development of techniques suitable for these studies. Aims. Our aim is to characterize the large trans-Neptunian object (TNO) 2002 TC302. Methods. Stellar occultations offer unique opportunities to determine key physical properties of TNOs. On 28 January 2018, 2002 TC302 occulted a mv ~ 15.3 star with designation 593-005847 in the UCAC4 stellar catalog, corresponding to Gaia source 130957813463146112. Twelve positive occultation chords were obtained from Italy, France, Slovenia, and Switzerland. Also, four negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body can be obtained that is compatible with the near misses. Results. The resulting ellipse has major and minor axes of 543 ± 18 km and 460 ± 11 km, respectively, with a position angle of 3 ± 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5 m telescope at Sierra Nevada Observatory and the 1.23 m telescope at Calar Alto observatory, allows us to derive possible three-dimensional shapes and density estimations for the body based on hydrostatic equilibrium assumptions. The effective diameter in equivalent area is around 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to ~300 km in diameter, which is required to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also a

Published
2020

37. The 2017 May 20 stellar occultation by the elongated centaur (95626) 2002 GZ32

Author

Santos-Sanz, P, primary, Ortiz, J L, additional, Sicardy, B, additional, Benedetti-Rossi, G, additional, Morales, N, additional, Fernández-Valenzuela, E, additional, Duffard, R, additional, Iglesias-Marzoa, R, additional, Lamadrid, J L, additional, Maícas, N, additional, Pérez, L, additional, Gazeas, K, additional, Guirado, J C, additional, Peris, V, additional, Ballesteros, F J, additional, Organero, F, additional, Ana-Hernández, L, additional, Fonseca, F, additional, Alvarez-Candal, A, additional, Jiménez-Teja, Y, additional, Vara-Lubiano, M, additional, Braga-Ribas, F, additional, Camargo, J I B, additional, Desmars, J, additional, Assafin, M, additional, Vieira-Martins, R, additional, Alikakos, J, additional, Boutet, M, additional, Bretton, M, additional, Carbognani, A, additional, Charmandaris, V, additional, Ciabattari, F, additional, Delincak, P, additional, Fuambuena Leiva, A, additional, González, H, additional, Haymes, T, additional, Hellmich, S, additional, Horbowicz, J, additional, Jennings, M, additional, Kattentidt, B, additional, Kiss, Cs, additional, Komžík, R, additional, Lecacheux, J, additional, Marciniak, A, additional, Moindrot, S, additional, Mottola, S, additional, Pal, A, additional, Paschalis, N, additional, Pastor, S, additional, Perello, C, additional, Pribulla, T, additional, Ratinaud, C, additional, Reyes, J A, additional, Sanchez, J, additional, Schnabel, C, additional, Selva, A, additional, Signoret, F, additional, Sonbas, E, additional, and Alí-Lagoa, V, additional

Published
2020
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38. The large trans-Neptunian object 2002 TC302from combined stellar occultation, photometry, and astrometry data

Author

Ortiz, J. L., primary, Santos-Sanz, P., additional, Sicardy, B., additional, Benedetti-Rossi, G., additional, Duffard, R., additional, Morales, N., additional, Braga-Ribas, F., additional, Fernández-Valenzuela, E., additional, Nascimbeni, V., additional, Nardiello, D., additional, Carbognani, A., additional, Buzzi, L., additional, Aletti, A., additional, Bacci, P., additional, Maestripieri, M., additional, Mazzei, L., additional, Mikuz, H., additional, Skvarc, J., additional, Ciabattari, F., additional, Lavalade, F., additional, Scarfi, G., additional, Mari, J. M., additional, Conjat, M., additional, Sposetti, S., additional, Bachini, M., additional, Succi, G., additional, Mancini, F., additional, Alighieri, M., additional, Dal Canto, E., additional, Masucci, M., additional, Vara-Lubiano, M., additional, Gutiérrez, P. J., additional, Desmars, J., additional, Lecacheux, J., additional, Vieira-Martins, R., additional, Camargo, J. I. B., additional, Assafin, M., additional, Colas, F., additional, Beisker, W., additional, Behrend, R., additional, Mueller, T. G., additional, Meza, E., additional, Gomes-Junior, A. R., additional, Roques, F., additional, Vachier, F., additional, Mottola, S., additional, Hellmich, S., additional, Campo Bagatin, A., additional, Alvarez-Candal, A., additional, Cikota, S., additional, Cikota, A., additional, Christille, J. M., additional, Pál, A., additional, Kiss, C., additional, Pribulla, T., additional, Komžík, R., additional, Madiedo, J. M., additional, Charmandaris, V., additional, Alikakos, J., additional, Szakáts, R., additional, Farkas-Takács, A., additional, Varga-Verebélyi, E., additional, Marton, G., additional, Marciniak, A., additional, Bartczak, P., additional, Butkiewicz-Ba̧k, M., additional, Dudziński, G., additional, Alí-Lagoa, V., additional, Gazeas, K., additional, Paschalis, N., additional, Tsamis, V., additional, Guirado, J. C., additional, Peris, V., additional, Iglesias-Marzoa, R., additional, Schnabel, C., additional, Manzano, F., additional, Navarro, A., additional, Perelló, C., additional, Vecchione, A., additional, Noschese, A., additional, and Morrone, L., additional

Published
2020
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45. Electrical Characterization of Defects in SiC Schottky Barriers

Author

Schnabel, C. M, Tabib-Azar, M, Raffaelle, R. P, Su, H. B, Dudley, M, Neudeck, P. G, and Bailey, S

Subjects
Solid-State Physics
Abstract

We have been investigating the effect of screw dislocation and other structural defects on the electrical properties of SiC. SiC is a wide-bandgap semiconductor that is currently received much attention due to its favorable high temperature behavior and high electric field breakdown strength. Unfortunately, the current state-of-the-art crystal growth and device processing methods produce material with high defect densities, resulting in a limited commercial viability

Published
2005

46. PEONS-CAAP48 – Evaluation von C-terminalem Alpha-1 Antitrypsin Peptid (CAAP48) als potentieller diagnostischer Biomarker der Early-Onset Neonatalen Sepsis (EONS) nach mütterlichem frühem vorzeitigen Blasensprung (Preterm Premature Rupture of membranes – PPROM)

Author

Zöllkau, J, additional, Dawczynski, K, additional, Pastuschek, J, additional, Heimann, Y, additional, Kiehntopf, M, additional, Schnabel, C, additional, Bergner, M, additional, Haase, R, additional, Stubert, J, additional, Olbertz, DM, additional, and Schleußner, E, additional

Published
2019
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47. Nickel-59 in Surface Layers of Lunar Basalt 74275: Implications for the Solar Alpha Particle Flux

Author

Schnabel, C, Xue, S, Ma, P, Herzog, G. F, Fifield, K, Cresswell, R. G, diTada, M. L, Hausladen, Paul, and Reedy, R. C

Subjects
Lunar And Planetary Science And Exploration
Abstract

By using AMS we have profiled 59 Ni/Ni ratios in lunar basalt 74275. Activities (dpm 59 Ni/[kg Fe]) range from 120 to 10 at depths (mg/cm 2) from about 30 to 650. Modeling results hint at higher solar alpha fluxes during the last about 0.5 My than during the last approximately 1 My.

Published
2000

48. In vivo imaging in the oral cavity by endoscopic optical coherence tomography

Author

Walther, J., Schnabel, C., Tetschke, F., Rosenauer, T., Golde, J., Ebert, N., Baumann, M., Hannig, C., Koch, E., Walther, J., Schnabel, C., Tetschke, F., Rosenauer, T., Golde, J., Ebert, N., Baumann, M., Hannig, C., and Koch, E.

Abstract

The common way to diagnose hard and soft tissue irregularities in the oral cavity is initially the visual inspection by an experienced dentist followed by further medical examinations, such as radiological imaging and/or histopathological investigation. For the diagnosis of oral hard and soft tissues, the detection of early transformations is mostly hampered by poor visual access, low specificity of the diagnosis techniques, and/or limited feasibility of frequent screenings. Therefore, optical noninvasive diagnosis of oral tissue is promising to improve the accuracy of oral screening. Considering this demand, a rigid handheld endoscopic scanner was developed for optical coherence tomography (OCT). The novelty is the usage of a commercially near-infrared endoscope with fitting optics in combination with an established spectral-domain OCT system of our workgroup. By reaching a high spatial resolution, in vivo images of anterior and especially posterior dental and mucosal tissues were obtained from the oral cavity of two volunteers. The convincing image quality of the endoscopic OCT device is particularly obvious for the imaging of different regions of the human soft palate with highly scattering fibrous layer and capillary network within the lamina propria

Published
2018

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