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1 tosphere) in the vicinity of both Europa and Callisto.
2 nificantly younger than that of Ganymede and Callisto.
3 similar to that of the non-ice components of Callisto and can be attributed to hydrous minerals.
4 evidence for internal liquid water oceans in Callisto and Europa, detection of a strong intrinsic mag
5 surface materials of the Galilean satellites Callisto and Ganymede from analysis of reflectance spect
6                                   Spectra of Callisto and Ganymede reveal a feature at 4.25 micromete
7 e and a tenuous carbon dioxide atmosphere at Callisto, and detection of condensed oxygen on Ganymede.
8  rock are mixed all the way to the center of Callisto are also consistent with the data.
9         The icy lithospheres of Ganymede and Callisto are equally ice-rich, but Europa's icy shell ha
10 ect information on the interior structure of Callisto determined from previous spacecraft fly-bys was
11  moon surfaces like Europa, Titan, Ganymede, Callisto, Enceladus, or Ceres.
12 mes for two cataract planning systems (ZEISS CALLISTO eye and the Wavetec AnalyzOR) in predicting res
13 ithin 0.25D in the ORA group compared to the CALLISTO eye group (56.5%); at all other levels outcomes
14 est refractive spherical error (MRSE) in the CALLISTO eye group 0.022 +/- 0.388 diopters (D) compared
15                        Lens selection in the CALLISTO eye group was based on Zeiss VERACITY Surgery P
16 vels outcomes were numerically higher in the CALLISTO eye group.
17 Less surgical time was needed when using the CALLISTO eye than the ORA when performing cataract surge
18                    There were 23 eyes in the CALLISTO group and 28 eyes in the ORA group.
19        Toric lens placement mean time in the CALLISTO group was 2.47 +/- 0.34 min compared to 3.88 +/
20               The mean surgical time for the CALLISTO group was 28.09 +/- 1.72 min compared to 34.41
21 roral footprint of the fourth Galilean moon, Callisto, has always been challenging because of its exp
22 meter have indicated that neither Europa nor Callisto have an appreciable internal magnetic field, in
23  (C10) indicate that the rock and ice within Callisto have partially, but not completely, separated.
24                                              Callisto may be differentiated into a rock-metal core le
25 galilean satellites-Io, Europa, Ganymede and Callisto-on each orbit.
26 of Jupiter's moons Io, Europa, Ganymede, and Callisto over the past few years.
27 alilean satellites--Io, Europa, Ganymede and Callisto-ranged from uniform mixtures of rock and ice (t
28               Concurrent observations within Callisto's flux tube reveal field-aligned electrons with
29               Here we report measurements of Callisto's gravitational field which reveal that, in con
30 to a rock-metal core less than 25 percent of Callisto's radius, an outer layer of clean ice less than
31 5 0.5 times the thicknesses of Ganymede's or Callisto's shells, depending on epoch.
32                                              Callisto's undifferentiated state is consistent with the
33 hs of impact craters on Europa, Ganymede and Callisto that reveal two anomalous transitions in crater
34 ncounter (C3) of the Galileo spacecraft with Callisto, the outermost Galilean moon of Jupiter, indica
35                          An off-limb scan of Callisto was conducted by the Galileo near-infrared mapp
36 ost Galilean moon of Jupiter, indicated that Callisto was probably undifferentiated.
37 s to the galilean moons Europa, Ganymede and Callisto, which reside within Jupiter's radiation belts.