Earth-based observations of the Galileo probe entry site

Science

Volumn 272, Issue 5263, 1996, Pages 839-840

  Orton, G ^a   Ortiz, J L ^b,c   Baines, K ^b   Bjoraker, G ^d   Carsenty, U ^e   Colas, F ^f   Dayal, A ^g   Deming, D ^d   Drossart, P ^h   Frappa, E ⁱ   Friedson, J ^a   Goguen, J ^b   Golisch, W ^j   Griep, D ^j   Hernandez, C ^b   Hoffmann, W ^g   Jennings, D ^d   Kaminski, C ^j   Kuhn, J ^k   Laques, P ⁱ   Limaye, S ^l   Lin, H ^k   Lecacheux, J ^h   Martin, T ^a   McCabe, G ^d   Momary, T ^m   Parker, D ^b   Puetter, R ⁿ   Ressler, M ^b   Reyes, G ^b   Sada, P ^d   Spencer, J ^o   Spitale, J ^p   Stewart, S ^p   Varsik, J ^k   Warell, J ^q   Wild, W ^r   Yanamandra Fisher, P ^a   Fazio, G ^s   Hora, J ^j   Deutsch, L ^t   more..

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b JPL ^*

^c INSTITUTO DE ASTROFÍSICA DE ANDALUCÍA CSIC   (Spain)

^d NASA GODDARD SPACE FLIGHT CENTER   (United States)

^e GERMAN AEROSPACE CENTER DLR   (Germany)

^f Bureau des Longitudes   (France)

^g UNIVERSITY OF ARIZONA   (United States)

^h OBSERVATOIRE DE PARIS   (France)

ⁱ OBSERVATOIRE MIDI PYRÉNÉES   (France)

^j UNIVERSITY OF HAWAII   (United States)

^k NATIONAL SOLAR OBSERVATORY   (United States)

^l UNIVERSITY OF WISCONSIN MADISON   (United States)

^m UNIVERSITY OF CALIFORNIA   (United States)

ⁿ UNIVERSITY OF CALIFORNIA   (United States)

^o LOWELL OBSERVATORY   (United States)

^p CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^q BOX 515   (Sweden)

^r UNIVERSITY OF CHICAGO   (United States)

^s SMITHSONIAN ASTROPHYSICAL OBSERVATORY   (United States)

^t UNIVERSITY OF MASSACHUSETTS   (United States)

more..

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0001149547     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.272.5263.839     Document Type: Article

References (22)

1. Observations from Earth close to the arrival date were challenging because Jupiter was only 9° from the center of the sun. Extensive baffling of the optical beam was used at several telescopes to reject sunlight and stabilize the image. At IRTF, a thin sheet of polypropylene was laid over the primary mirror, allowing transmission of only infrared radiation.
2. These regions were first detected by J. Westphal [Astrophys. J. 157,63 (1969)] and described in detail by J. Westphal, K. Matthews, and R. Terrile [ibid. 188, 111 (1974)].
3. These regions were first detected by J. Westphal [Astrophys. J. 157,63 (1969)] and described in detail by J. Westphal, K. Matthews, and R. Terrile [ibid. 188, 111 (1974)].
4. G. S. Orton et al., Science252, 537 (1991).
5. G. S. Orton et al., ibid. 265, 625 (1994).
6. Our 7.8-μm IRTF images in December were strongly degraded by the attenuation of the polypropylene safety screen (1), and our derived stratospheric temperatures are noisy, with little recognizable zonal structure. Our initial conclusions about stratospheric temperatures at the PES are based on a longitudinal average (zonal mean), and tentative conclusions about motions of waves are based on correlation with the brightest zonal feature at the PES latitude.
7. P. J. Gierasch, B. J. Conrath, J. A. Magalhaes, Icarus 67.456 (1986). We note, however, that the zonal mean stratospheric temperature variations displayed an unusually high correlation with those in the troposphere.
8. A. Seiff et al., Science 272, 846 (1996).
9. As summarized by R. West, D. Strobel, and M. Tomasko [Icarus 65, 161 (1986)].
10. B. E. Carlson, A. A. Lacis, W. B. Rossow, J. Geophys. Res. 98, 5251 (1993); G. L. Bjoraker, H. P. Larson, V. G. Kunde, Astrophys, J. 311, 1058 (1986).
11. B. E. Carlson, A. A. Lacis, W. B. Rossow, J. Geophys. Res. 98, 5251 (1993); G. L. Bjoraker, H. P. Larson, V. G. Kunde, Astrophys, J. 311, 1058 (1986).
12. B. Ragent, D. S. Colburn, P. Avrin, K. A. Rages, Science 272, 856 (1996).
13. L. Sromovsky et al., ibid., p. 853.
14. H. Niemann et al., ibid., p. 848.
15. The waves were not apparent during, for example, the intensive observing by IRTF associated with the collision of Shoemaker-Levy 9 [G. Orton et al., Science 267, 1277 (1995)].
16. One such phenomenon is the quasi-quadrennial oscillation [C. B. Leovy, A. J. Friedson, G. S. Orton, Nature 354, 380 (1991)].
17. S. Limaye, Icarus 65, 335 (1986); and references therein.
18. R. F. Beebe, A. A. Simon, L, F. Huber, Science 272, 842 (1996).
19. D.H. Atkinson, J. B. Pollack, A. Seiff, ibid., p. 843.
20. Pic-du-Midi images were processed to remove lowfrequency signal variations; the other images underwent goodness-of-fit and PIXON restoration techniques [R. C. Puetter Int. J. Imaging Syst. Technol. 6, 314 (1995); and references therein].
21. -1 relative to the rotation of the interior (System III). This value is consistent with Voyager (15) and HST (16) results, although the PES itself was characterized by a much stronger prograde jet over a narrower region (16, 17). Image restoration processing (18) was applied before mapping, and corrections were made for illumination and emission angle variations across the map. The uncertainty of the PES position in these maps [Fig. 1: ∼ ±2° in latitude and longitude for (A), ±1°for (B) and (C), and ≲0.5° for (D); Fig. 2: ≪for1° for (A), ≤∼0.5° for (B) and (C), and ∼1° to 2° for (D)] arises from uncertainty in fitting the limb.
22. We thank the staff of several observatories for their support in making a number of unusual but important changes to observing techniques and schedules. The mapping in Fig. 2A was kindly provided by A. Simon and R. Beebe. Our research was sponsored by various grants from NASA and NSF for work performed at each of the institutions with which we are associated. K.B., A.D., J.F., J.G., W.H., T.M., J.L.O., G.O., M.R., G.R., J. Spencer, J. Spitale, S.S., and P.Y.-F. were visiting astronomers at IRTF, which is operated by the University of Hawaii under contract to NASA. We also thank the French Programme National de Planetologie for support of the Pic-du-Midi observations. P.S. was supported by a NASA-National Research Council Resident Research Associateship.