| Texto completo | |
| Autor(es): Mostrar menos - |
Rommel, F. L.
[1, 2, 3]
;
Braga-Ribas, F.
[1, 2, 3]
;
Desmars, J.
[4, 5, 6]
;
Camargo, J. I. B.
[1, 3]
;
Ortiz, J. L.
[7]
;
Sicardy, B.
[8]
;
Vieira-Martins, R.
[1, 3]
;
Assafin, M.
[9, 3]
;
Santos-Sanz, P.
[7]
;
Duffard, R.
[7]
;
Fernandez-Valenzuela, E.
[10]
;
Lecacheux, J.
[8]
;
Morgado, B. E.
[1, 3, 8]
;
Benedetti-Rossi, G.
[3, 8]
;
Gomes-Junior, A. R.
[11]
;
Pereira, C. L.
[2, 3]
;
Herald, D.
[12, 13, 14]
;
Hanna, W.
[12, 13]
;
Bradshaw, J.
[15]
;
Morales, N.
[7]
;
Brimacombe, J.
[16]
;
Burtovoi, A.
[17, 18]
;
Carruthers, T.
[19]
;
de Barros, J. R.
[20]
;
Fiori, M.
[17, 21]
;
Gilmore, A.
[22]
;
Hooper, D.
[12, 13]
;
Hornoch, K.
[23]
;
Jacques, C.
[20]
;
Janik, T.
[12]
;
Kerr, S.
[24, 13]
;
Kilmartin, P.
[22]
;
Winkel, Jan Maarten
[12]
;
Naletto, G.
[17, 21]
;
Nardiello, D.
[17, 25]
;
Nascimbeni, V
[17, 21]
;
Newman, J.
[12, 14]
;
Ossola, A.
[26]
;
Pal, A.
[27, 28, 29]
;
Pimentel, E.
[20]
;
Pravec, P.
[23]
;
Sposetti, S.
[26]
;
Stechina, A.
[30]
;
Szakats, R.
[27]
;
Ueno, Y.
[31]
;
Zampieri, L.
[17]
;
Broughton, J.
[13, 32]
;
Dunham, J. B.
[12]
;
Dunham, D. W.
[12]
;
Gault, D.
[13]
;
Hayamizu, T.
[31]
;
Hosoi, K.
[31]
;
Jehin, E.
[33]
;
Jones, R.
[12]
;
Kitazaki, K.
[31]
;
Komzik, R.
[34]
;
Marciniak, A.
[35]
;
Maury, A.
[36]
;
Mikuz, H.
[37]
;
Nosworthy, P.
[13]
;
Polleri, J. Fabrega
[38]
;
Rahvar, S.
[39]
;
Sfair, R.
[11]
;
Siqueira, P. B.
[11]
;
Snodgrass, C.
[40]
;
Sogorb, P.
[41]
;
Tomioka, H.
[31]
;
Tregloan-Reed, J.
[42]
;
Winter, O. C.
[11]
Número total de Autores: 69
|
| Afiliação do(s) autor(es): Mostrar menos - | [1] Observ Nacl, MCTIC, R Gen Jose Cristino 77, Rio De Janeiro, RJ - Brazil
[2] Fed Univ Technol Parana UTFPR, DAFIS, Rua Sete Setembro 3165, Curitiba, Parana - Brazil
[3] Lab Interinst Astron LIneA, Rua Gal Jose Cristino 77, Rio De Janeiro, RJ - Brazil
[4] Inst Polytech Sci Avancees IPSA, 63 Blvd Brandebourg, F-94200 Ivry - France
[5] INCT E Universo, Rua Gal Jose Cristino 77, Rio De Janeiro, RJ - Brazil
[6] Sorbonne Univ, PSL Res Univ, IMCCE, Observ Paris, CNRS, Univ Lille, UPMC Univ Paris 06, Inst Mecan Celeste & Calcul Ephemerides, 77 Av Denfert Rochereau, F-75014 Paris 06 - France
[7] Inst Astrofis Andalucia, IAA CSIC, Glorieta Astron S-N, Granada 18008 - Spain
[8] Sorbonne Univ, Univ PSL, Univ Paris Diderot, LESIA, Observ Paris, CNRS, Sorbonne Paris Cite, 5 Pl Jules Janssen, F-92195 Meudon - France
[9] Univ Fed Rio de Janeiro, Observ Valongo, Rio de Janeiro, RJ - Brazil
[10] Univ Cent Florida, Florida Space Inst, 12354 Res Pkwy, Partnership 1, Orlando, FL - USA
[11] UNESP Sao Paulo State Univ, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[12] Int Occultat Timing Assoc IOTA, POB 423, Greenbelt, MD 20768 - USA
[13] Trans Tasman Occultat Alliance TTOA, POB 3181, Wellington - New Zealand
[14] Canberra Astron Soc, Canberra, ACT - Australia
[15] Samford Valley Observ Q79, Brisbane, Qld - Australia
[16] Coral Towers Observ, Cairns, Qld 4870 - Australia
[17] INAF Astron Observ Padova, Vicolo Osservatorio 5, I-35122 Padua - Italy
[18] Univ Padua, Ctr Studies & Act Space CISAS G Colombo, Via Venezia 15, I-35131 Padua - Italy
[19] Jewel Box Observ, 69 Falcon St, Bayview Hts, Qld 4868 - Australia
[20] SONEAR Observ, Oliveira, MG - Brazil
[21] Univ Padua, Dept Phys & Astron G Galilei, Via Marzolo 8, I-35131 Padua - Italy
[22] Univ Canterbury, Mt John Univ Observ, POB 56, Lake Tekapo 7945 - New Zealand
[23] Acad Sci Czech Republ, Astron Inst, Fricova 298, Ondrejov 25165 - Czech Republic
[24] Astron Assoc Queensland, 5 Curtis St, Pimpama, Qld 4209 - Australia
[25] Aix Marseille Univ, LAM, CNES, CNRS, Marseille - France
[26] SOTAS Stellar Occultat Timing Assoc Switzerland, Swiss Astron Soc, Zurich - Switzerland
[27] Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest - Hungary
[28] Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest - Hungary
[29] Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setany 1-A, H-1117 Budapest - Hungary
[30] Ctr Amigos Astron Reconquista CAAR, Reconquista - Argentina
[31] Japan Occultat Informat Network Join, Nagatoshi - Japan
[32] Reedy Creek Observ, Gold Coast, Qld - Australia
[33] Univ Liege, Star Inst, Allee 6 Aout 19C, B-4000 Liege - Belgium
[34] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960 - Slovakia
[35] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Poznan - Poland
[36] San Pedro Atacama Celestial Explorat Space, Antofagasta - Chile
[37] Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000 - Slovenia
[38] Panamanian Observ San Pedro Atacama OPSPA, San Pedro De Atacama - Chile
[39] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran - Iran
[40] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh, Midlothian - Scotland
[41] Club Dastron Luberon Sud Astro, La Bastide Des Jourdans - France
[42] Univ Antofagasta, Ctr Astron CITEVA, Ave U Antofagasta, Antofagasta 02800 - Chile
Número total de Afiliações: 42
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Astronomy & Astrophysics; v. 644, NOV 27 2020. |
| Citações Web of Science: | 0 |
| Resumo | |
Context. Trans-Neptunian objects (TNOs) and Centaurs are remnants of our planetary system formation, and their physical properties have invaluable information for evolutionary theories. Stellar occultation is a ground-based method for studying these distant small bodies and has presented exciting results. These observations can provide precise profiles of the involved body, allowing an accurate determination of its size and shape.Aims. The goal is to show that even single-chord detections of TNOs allow us to measure their milliarcsecond astrometric positions in the reference frame of the Gaia second data release (DR2). Accurate ephemerides can then be generated, allowing predictions of stellar occultations with much higher reliability.Methods. We analyzed data from various stellar occultation detections to obtain astrometric positions of the involved bodies. The events published before the Gaia era were updated so that the Gaia DR2 stellar catalog is the reference, thus providing accurate positions. Events with detection from one or two different sites (single or double chord) were analyzed to determine the event duration. Previously determined sizes were used to calculate the position of the object center and its corresponding error with respectto the detected chord and the International Celestial Reference System propagated Gaia DR2 star position.Results. We derive 37 precise astrometric positions for 19 TNOs and four Centaurs. Twenty-one of these events are presented here for the first time. Although about 68% of our results are based on single-chord detection, most have intrinsic precision at the submilliarcsecond level. Lower limits on the diameter of bodies such as Sedna, 2002 KX14, and Echeclus, and also shape constraints on 2002 VE95, 2003 FF128, and 2005 TV189 are presented as valuable byproducts.Conclusions. Using the Gaia DR2 catalog, we show that even a single detection of a stellar occultation allows improving the object ephemeris significantly, which in turn enables predicting a future stellar occultation with high accuracy. Observational campaigns can be efficiently organized with this help, and may provide a full physical characterization of the involved object, or even the study of topographic features such as satellites or rings. (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 |
| Processo FAPESP: | 16/24561-0 - A relevância dos pequenos corpos em dinâmica orbital |
| Beneficiário: | Othon Cabo Winter |
| Modalidade de apoio: | Auxílio à Pesquisa - Temático |