| Texto completo | |
| Autor(es): Mostrar menos - |
Ortiz, J. L.
[1]
;
Santos-Sanz, P.
[1]
;
Sicardy, B.
[2]
;
Benedetti-Rossi, G.
[3, 2]
;
Duffard, R.
[1]
;
Morales, N.
[1]
;
Braga-Ribas, F.
[3, 4, 5]
;
Fernandez-Valenzuela, E.
[6]
;
Nascimbeni, V
[7, 8]
;
Nardiello, D.
[7, 9, 8]
;
Carbognani, A.
[10]
;
Buzzi, L.
[11]
;
Aletti, A.
[11]
;
Bacci, P.
[12]
;
Maestripieri, M.
[12]
;
Mazzei, L.
[12]
;
Mikuz, H.
[13, 14]
;
Skvarc, J.
[13]
;
Ciabattari, F.
[15]
;
Lavalade, F.
[16]
;
Scarfi, G.
[17]
;
Mari, J. M.
[18]
;
Conjat, M.
[19]
;
Sposetti, S.
[20]
;
Bachini, M.
[21]
;
Succi, G.
[21]
;
Mancini, F.
[21]
;
Alighieri, M.
[21]
;
Dal Canto, E.
[21]
;
Masucci, M.
[21]
;
Vara-Lubiano, M.
[1]
;
Gutierrez, P. J.
[1]
;
Desmars, J.
[22, 23]
;
Lecacheux, J.
[2]
;
Vieira-Martins, R.
[3, 5]
;
Camargo, J. I. B.
[3, 5]
;
Assafin, M.
[3, 24]
;
Colas, F.
[23]
;
Beisker, W.
[25]
;
Behrend, R.
[26]
;
Mueller, T. G.
[27]
;
Meza, E.
[2]
;
Gomes-Junior, A. R.
[3, 28]
;
Roques, F.
[2]
;
Vachier, F.
[23]
;
Mottola, S.
[29]
;
Hellmich, S.
[29]
;
Campo Bagatin, A.
[30, 31]
;
Alvarez-Candal, A.
[5, 31]
;
Cikota, S.
[32]
;
Cikota, A.
[33]
;
Christille, J. M.
[34]
;
Pal, A.
[35]
;
Kiss, C.
[35, 36]
;
Pribulla, T.
[37, 38, 39]
;
Komzik, R.
[37]
;
Madiedo, J. M.
[1]
;
Charmandaris, V
[40, 41]
;
Alikakos, J.
[40]
;
Szakats, R.
[35]
;
Farkas-Takacs, A.
[35, 42]
;
Varga-Verebelyi, E.
[35]
;
Marton, G.
[35]
;
Marciniak, A.
[43]
;
Bartczak, P.
[43]
;
Butkiewicz-Bak, M.
[43]
;
Dudzinski, G.
[43]
;
Ali-Lagoa, V
[27]
;
Gazeas, K.
[43]
;
Paschalis, N.
[44]
;
Tsamis, V
[45]
;
Guirado, J. C.
[46]
;
Peris, V
[46]
;
Iglesias-Marzoa, R.
[47, 48]
;
Schnabel, C.
[25, 49]
;
Manzano, F.
[49]
;
Navarro, A.
[49]
;
Perello, C.
[25, 49]
;
Vecchione, A.
[50]
;
Noschese, A.
[50]
;
Morrone, L.
[51]
Número total de Autores: 81
|
| Afiliação do(s) autor(es): Mostrar menos - | [1] Inst Astrofis Andalucia, IAA CSIC, Glorieta Astron S-N, Granada 18008 - Spain
[2] Univ Paris, Sorbonne Univ, CNRS, LESIA, Observ Paris, Univ PSL, 5 Pl Jules Janssen, F-92195 Meudon - France
[3] Lab Interinst E Astron LineA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro - Brazil
[4] Fed Univ Technol Parana UTFPR DAFIS, Curitiba, Parana - Brazil
[5] Observ Nacl MCTIC, Rio De Janeiro - Brazil
[6] Univ Cent Florida, Florida Space Inst, 12354 Res Pkwy, Partnership 1, Orlando, FL 32816 - USA
[7] Univ Padua, Dipartimento Fis & Astron G Galilei, Padua - Italy
[8] INAF, Osservatorio Astron Padova, Padua - Italy
[9] Aix Marseille Univ, LAM, CNES, CNRS, Marseille - France
[10] INAF, Osservatorio Astrofis & Sci Spazio, Bologna - Italy
[11] Schiaparelli Astron Observ, Varese - Italy
[12] Astron Observ San Marcello Pistoiese CARA Project, Pistoia - Italy
[13] Crni Vrh Observ, Crni Vrh Nad Idrijo - Slovenia
[14] Univ Ljubljana, Fac Math & Phys, Ljubljana - Slovenia
[15] Osservatorio Astron Monte Agliale, Lucca - Italy
[16] 55 Impasse Marjolaine, F-83560 Vinon Sur Verdon - France
[17] Observatorio Astron Iota Scorpii, La Spezia - Italy
[18] 1075 Ave St Philippe, F-06410 Biot - France
[19] Observ Cote dAzur, Nice - France
[20] Gnosca Observ, Fun & Vign 7, CH-6525 Gnosca - Switzerland
[21] Osservatorio Astron Tavolaia, Pisa - Italy
[22] Inst Polytech Sci Avancees IPSA, 63 Blvd Brandebourg, F-94200 Ivry - France
[23] Univ Lille, Inst Mecan Celeste & Calcul Ephemerides, PSL Res Univ, IMCCE, Observ Paris, CNRS, Sorbonne Univ, UPMC, Univ P, 77 Av Denfert Rochereau, F-75014 Paris - France
[24] Univ Fed Rio de Janeiro, Observatorio Valongo, Rio de Janeiro - Brazil
[25] Int Occultat Timing Assoc European Sect IOTA ES, Hannover - Germany
[26] Observ Geneva, Sauverny - Switzerland
[27] Max Planck Inst Extraterr Phys MPE, Garching - Germany
[28] UNESP Sao Paulo State Univ, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta - Brazil
[29] German Aerosp Ctr DLR, Inst Planetary Res, Berlin - Germany
[30] Univ Alicante, DFISTS, Alicante - Spain
[31] Univ Alicante, IUFACyT, Alicante - Spain
[32] Univ Zagreb, Fac Elect Engn & Comp, Unska 3, Zagreb 10000 - Croatia
[33] EO Lawrence Berkeley Natl Lab, Div Phys, 1 Cyclotron Rd, Berkeley, CA 94720 - USA
[34] Astron Observ Autonomous Reg Aosta Valley OAVdA, Lignan 39, I-11020 Nus - Italy
[35] Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest - Hungary
[36] Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest - Hungary
[37] Slovak Acad Sci, Astron Inst, Tatranska Lomnica - Slovakia
[38] MTA ELTE Exoplanet Res Grp, Szent Imre H U 112, H-9700 Szombathely - Hungary
[39] ELTE Gothard Astrophys Observ, Szent Imre H U 112, H-9700 Szombathely - Hungary
[40] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Athens - Greece
[41] Univ Crete, Dept Phys, Iraklion - Greece
[42] Eotvos Lorand Univ, Fac Sci, Pazmany Peter Setany 1-A, H-1117 Budapest - Hungary
[43] Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, Poznan - Poland
[44] Nunki Observ, Xanemos - Greece
[45] Ellinogermaniki Agogi Observ, Pallini - Greece
[46] Univ Valencia, Observ Astron, Valencia - Spain
[47] Univ La Laguna, Dept Astrofis, Tenerife - Spain
[48] Ctr Estudios Fis Cosmos Aragon, Teruel - Spain
[49] Agrupacio Astron Sabadell, Barcelona - Spain
[50] Osservatorio Salvatore Giacomo, Astrocampania, Agerola, NA - Italy
[51] Via Radicosa 44, I-80051 Agerola - Italy
Número total de Afiliações: 51
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Astronomy & Astrophysics; v. 639, JUL 22 2020. |
| Citações Web of Science: | 1 |
| Resumo | |
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 m(v) similar to 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 similar 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 appears to be consistent with other ground-based data presented here. From the effective occultation diameter combined with absolute magnitude measurements we derive a geometric albedo of 0.147 +/- 0.005, which would be somewhat smaller if 2002 TC302 has a satellite. The best occultation light curves do not show any signs of ring features or any signatures of a global atmosphere. (AU) | |
| Processo FAPESP: | 18/11239-8 - Determinação de órbitas de satélites e anéis a partir da análise de imagens por sondas espaciais |
| Beneficiário: | Altair Ramos Gomes Junior |
| Modalidade de apoio: | Bolsas no Brasil - Pós-Doutorado |