baalke@mars.jpl.nasa.gov (Ron Baalke) (12/15/90)
GALILEO STATUS REPORT EARTH FLYBY December 8, 1990 At 12:35PM (PST) the Galileo spacecraft made it closest approach to Earth. Galileo came within 597 miles of Earth and just 0.4 seconds off the predited time. The gravity assisted enabled to pick up an additional 11,000 mph to its velocity relative to the Sun up to a speed of about 78,000 mph. Highlights of the day are listed below. Prior the ECA (Earth Closest Approach) at 12:01 AM, the NIMS (Near Infrared Mapping Spectrometer) took a thermal map mosaic of crater Langrenus in Mare Fecunditatis on the Moon, at phase angles of 136.6 to 133.2 degrees. A long map mode was utilized to characterize instrument response. Subspacecraft latitude was at -6.2 degrees and longitude was t 294.4 degrees west. The NIMS resolution was approximately 276 km. At 2:04 AM, the SSI (Solid State Imaging) camera obtain low-light level images of the Moon in both earthlight and/or starlight for the purpose of assessing the imaging system sensitivity as well as to search for the possible presence of lunar volatiles. The SSI also did some lunar multispectral mapping to calibrate the SSI with "ground truth" from Apollo landing sites, to map red spots and other non-mare volcanism, and to explore unmapped areas. At 3:15 AM, the NIMS mapped Mare Fecunditatis in the proximity of the Messier crater at an approximate resolution of 206 km with phase angles of 122 to 126 degrees at one instrument mode. An SSI frame was also taken with a clear filter. At 4:21 AM, the UVS (Ultraviolet Spectrometer) instrument observed the Earth's geotail to study the distribution of hydrogen atoms in the antisunward direction. The UVS measurements at H Lyman-Alpha are 16 times the sensitivity of the EUV's (Extreme Ultraviolet Spectrometer). They will be cross-compared with simultaneous measurements with EUV. The first geotail observations were at 90 degrees cone and will slow slew from above to equidistantly below the ecliptic plane at a slew rate of about 1 degree/minute (290.82 microradians/second). The second observation is performed by a slow slew about the antisunward directions (180 degrees or as close as allowed to 180 degrees cone) to 160 degree cone angle in constant clock. At 5:37 AM, the PPR (Photopolarimeter Radiometer) instrument made another phase angle map of the lunar disk. At 5:55 AM, the NIMS made its fourth full map mosaic, this time on Mare Tranquillitatis with a range of phase angles of 118 to 111 degrees, utilizing full map modes (204 wavelenghts, Gain state=1). The NIMS resolution was at 194 km. The next NIM thermal map occurred at 8:22 AM with the mosaic centered on the southern portion of Mare Tranquillitatis in the proximity of Maskelyne crater north of the Apollo 11 landing site, with phase angles from 107.5 degrees to 96 degrees. Three SSI frames were taken using the clear filter. At about 9 AM, lunar periapsis occurred with the spacecraft 74,150 miles from the Moon. At 10:15 AM, the PPR made another lunar phase angle map. At 10:19 AM, the PWS made a high resolution observation near the Earth's plasmsphere using the 80 kHz wideband mode. At 10:30 AM, the UVS made its second measurment of the Earth's geotail. At 10:52 AM, NIMS made another thermal map mosaic, this time along the terminator and the highland south of Rima Ariadaeus in Mare Tranquillitatis. The SSI took two frames with the clear filter. At 11:15 AM, at about 1 hours 20 minutes before ECA, the star scanner shutter was closed and the spacecraft's attitude was based on the gyroscopes only. The Magnetometer (MAG) was configured for calibration at 11:33 AM. The MAG will be operated in 6 of its 8 different configurations during the Earth 1 encounter. The PLS (Plasma) instrument was safed at 11:54 AM. At 12:03 PM with the spacecraft now only 9,512 miles from Earth, the NIMS recorded some mesopheric water profiles derived from the night side limb scans. Water was observed in the tell-tale emissions in longspectrometer mdoe. One scan was acquired near the equater over the Indian Ocean, another near the 70 N latitude near USSR/Scandinavia. The SSI simultaneously acquired auroral imaging during the 70 N latitude scan with 5-10 km vertical resolution. At 12:14 PM, the SSI made lightning and aurora observations which was recorded on the tape recoder. Communications was switched from LGA-1 (Low Gain Antenna 1) to LGA-2. UVS observation was made at 12:23 AM of the night airglow morpology and altitude variations of NO gamma (236.3 nm) and NO delta (198.0 nm) emissions. Altitudes started at 1000 km and sampled down to the surface. The EUV made measurements to search for emissions of H, He and O+ in the 50.0 to 125.0 region of the spectrum starting in the exosphere on the nightside and ending in the exosphere on the dayside. At 12:30 PM, the DSN (Deep Space Network) lost contact with the spacecraft as expected, as Galileo passed out of view of the tracking stations. ECA occurred at 12:34:34 PM. At 12:38PM and 12:56PM, the NIMS made two more mesopheric water profiles over the equator of the Pacific Ocean. At 12:59 PM, the PWS made some more high resolution observations of the near Earth plasmasphere. The PLS made observations of the magnetosphere to determine the composition and source of the near Earth solar wind, and to search for ion beams, charged oxygen, helium and other heavy ions. At 13:17 PM, the SSI took it first multispectral images of Australia from the time it became visible near the terminator. The SSI will continue to take images of Australia until it rotated out of view over the limb. These images will be combine together to form an Earth feature track/zoom movie. At 13:20 PM, the PPR measured the polarization at three separate wavelengths on the day side of the Earth. The resulting mosaic will provide the best chance of observing both clouds and ocean surfaces. At 13:33 PM, the NIMS made its first Moon observation since ECA, centering across Sinus Medii east of the Murchison crater. The SSI camera took two frames with the green filter. The shutter of the star scanner was opened a 13:45 PM. At 14:04 PM the HIC (Heavy Ion Counter) instrument was enabled to measure solar flares and cosmic rays. The EUV was turned off. At 14:16 PM, the NIMS obtained a Nyquist-sampled map of Australia and its surrounding water to calibrate the NIMS longmap spectra as well as to obtain spacial distributions of various mineralogical and vegetation types. This map, the first of two Australia maps, concentrates on the western half of Australia within 30 degress of the morning terminator with spacial resolution of 35-50 km per nimsel. The SSI acquired 4-color maps "on the fly" during each observation. At 14:19 PM, the MAG starting taking measurements every 5 minutes for about an hour to study the high freqency structure of the Earth's bow shock, which the spacecraft crossed multiple times. At 14:34 PM, the PWS made observations using its 80 kHz wideband mode. At 15:05 PM, the NIMS made its second Nyquist-sampled map of Australia, this time concentrating on the eastern half some 60 degrees from the terminator. At 15:34 PM, the UVS starting making UNEWS (UVS North East West South) scans to provide a valuable set of control data for comparison with the data acquired during the UVS NIMS Antarctica Map, as well as provide several swaths of data regarding ozone abundance over the Antarctic. The North South swath will start near the South Pole of the Earth and will be compared with the Equatorial swath and the 55 degree latitude swath that may be be observed in the ozone emissions. At 16:09 PM, the NIMS made its second lunar observation since ECA, and eighth overall. The mosaic was centered on Sammering crater (lattide = 0.5 degrees, W longitude = 8 degrees) and east of the Apollo 14 and 12 landing sites. Two SSI frames were taken with the clear filter. At 16:59 PM, the NIMS now focused it attention on Antartica by taking a Nyquist-sampled map of Antartic ice and it surrounding water. The SSI acquired contigous 3-color maps with a spacial resolution of 85 km per pixel. The second map was made by NIMS at 17:56 PM. At 19:23 PM, the NIMS made its ninth lunar observation, this time on northwest poing of Montes Riphaeus in Mare Insularum south of the Apollo 12 landing site. Using the long map mode with a phase angle of 56.4 degrees, NIMS obtained it best lunar spectral map resolution (123 km). The SSI obtained 4 frames with the clear filter. At 19:44 PM, the NIMS obtained a lunar thermal map at 147 to 144 degrees phase, over the Kastner crater in mare Smyhil. The NIMS resolution is at about 274 km. At 19:56 PM, the NIMS obtained its first Nyquist-sampled map for a Earth global mosaic. Comprised of 12 OAPELS over some 25 hours, this map will cover 30N to 30S near Africa at a spacial resolution of 125 km per pixel. At 21:06 PM, the NIMS continued its Moon farside coverage by obtaining a spectral map of Oceanus Procellarum between Euclides and Letronne craters at a phase angle of 49 degree with 179 km resolution. The NIMS obtained the Earth global moscaic #2 at 21:28 PM. Mosaic #3 came at 22:11 PM and mosaic #4 at 23:48 PM. At 23:34 PM, the NIMS made its 11th lunar observation on the area of Hansteen and Billy craters in Oceanus Procellarum at a phase angle of 39.3 degrees with a resoltion of 188 km. ___ _____ ___ /_ /| /____/ \ /_ /| | | | | __ \ /| | | | Ron Baalke | baalke@mars.jpl.nasa.gov ___| | | | |__) |/ | | |___ Jet Propulsion Lab | baalke@jems.jpl.nasa.gov /___| | | | ___/ | |/__ /| M/S 301-355 | |_____|/ |_|/ |_____|/ Pasadena, CA 91109 |