U.S. DEPARTMENT OF THE INTERIOR Prepared for the GEOLOGIC INVESTIGATION SERIES I–2757 U.S. GEOLOGICAL SURVEY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION ATLAS OF JOVIAN SATELLITES: EUROPA 180° 0° 55° –55° NOTES ON BASE R.L., and Weller, L., 2001, Final digital global maps of Ganymede, This sheet is one in a series of maps of the Galilean satellites of Jupiter at a Europa, and Callisto, in Lunar and Planetary Science Conference nominal scale of 1:15,000,000. This series is based on data from the Galileo XXXII: Houston, Lunar and Planetary Institute, abs. no. 2009 [CD- 0° 21 0° 33 15 0° Orbiter Solid-State Imaging (SSI) camera and the Voyager 1 and 2 space- ROM]. 3 0° 60° craft. Becker, T.L, Rosanova, T., Cook, D., Davies, M.E., Colvin, T.R., Acton, C., –60° Bachman, N., Kirk, R.L., and Gaddis, L.R., 1999, Progress in PROJECTION improvement of geodetic control and production of final image mosa- Mercator and Polar Stereographic projections used for this map of Europa ics for Callisto and Ganymede, in Lunar and Planetary Science Con- are based on a sphere having a radius of 1,562.09 km. The scale is ference XXX: Houston, Lunar and Planetary Institute, abs. no. 1692 1:8,388,000 at ±56° latitude for both projections. Longitude increases to the [CD-ROM]. west in accordance with the International Astronomical Union (1971; Becker, T.L., Rosanova, T., Gaddis, L.R., McEwen, A.S., Phillips, C.B., Davies and others, 1996). Latitude is planetographic. Davies, M.E., and Colvin, T.R., 1998, Cartographic processing of the 70° Galileo SSI data—An update on the production of global mosaics of –70° ° 2 CONTROL 3 0 4 ° 0 0 0 2 the Galilean satellites, in Lunar and Planetary Science Conference 6 0 1 ° The process of creating a geometric control network began with selecting ° control points on the individual images, making pixel measurements of XXIX: Houston, Lunar and Planetary Institute, abs. no. 1892 [CD- their locations, using reseau locations to correct for geometric distortions, ROM]. and converting the measurements to millimeters in the focal plane. These Davies, M.E., Abalakin, V.K., Bursa, M., Lieske, J.H., Morando, B., Morri- data are combined with the camera focal lengths and navigation solutions son, D., Seidelmann, P.K., Sinclair, A.T., Yallop, B., and Tjuflin, Y.S., as input to a photogrammetric triangulation solution (Davies and others, 1996, Report of the IAU/IAG/COSPAR Working Group on Carto- 1998; Davies and Katayama, 1981). The solution used here was computed graphic Coordinates and Rotational Elements of the Planets and Satel- 80° –80° at the RAND Corporation in June 2000. Solved parameters include the lites, 1994: Celestial Mechanics and Dynamical Astronomy, v. 63, p. radius (given above) of the best-fitting sphere, the coordinates of the con- 127–148. trol points, the three orientation angles of the camera at each exposure Davies, M.E., Colvin, T.R., Oberst, J., Zeitler, W., Schuster, P., Neukum, G., McEwen, A.S., Phillips, C.B., Thomas, P.C., Veverka, J., Belton, (right ascension, declination, and twist), and an angle (W0) that defines the M.J.S., and Schubert, G., 1998, The control networks of the Galilean orientation of Europa in space. W0—in this solution 36.022°—is the angle a ine satellites and implications for global shape: Icarus, v. 135, p. 372–376. L along the equator to the east, between the 0° meridian and the equator’s on ed Davies, M.E., and Katayama, F.Y., 1981, Coordinates of features on the arp intersection with the celestial equator at the standard epoch J2000.0. This S 90° 270° solution places the crater Cilix at its defined longitude of 182° west (Davies Galilean satellites: Journal of Geophysical Research, v. 86, no. A10, p. 90° 270° and others, 1996). 8635–8657. Eliason, E.M., 1997, Production of Digital Image Models using the ISIS MAPPING TECHNIQUE system, in Lunar and Planetary Science Conference XXVIII: Houston, This global map base uses the best image quality and moderate resolution Lunar and Planetary Institute, p. 331. Gráinne . coverage supplied by Galileo SSI and Voyager 1 and 2 (Batson, 1987; . Maeve Gaddis, L.R., Anderson, J., Becker, K., Becker, T.L., Cook, D., Edwards, Diarmuid a e Becker and others, 1998; 1999; 2001). The digital map was produced using n K., Eliason, E.M., Hare, T., Kieffer, H.H., Lee, E.M., Mathews, J., i L Integrated Software for Imagers and Spectrometers (ISIS) (Eliason, 1997; . Soderblom, L.A., Sucharski, T., Torson, J., McEwen, A.S., Robinson, Rhiannon –80 80° Gaddis and others, 1997; Torson and Becker, 1997). The individual images ° M., 1997, An overview of the Integrated Software for Imaging Spec- were radiometrically calibrated and photometrically normalized using a trometers (ISIS), in Lunar and Planetary Science Conference XXVIII: Lunar-Lambert function with empirically derived values (McEwen, 1991; Houston, Lunar and Planetary Institute, p. 387. Kirk and others, 2000). A linear correction based on the statistics of all a Greeley, R., and Batson, R.M., 1990, Planetary Mapping, Cambridge Uni- e n overlapping areas was then applied to minimize image brightness varia- versity Press, Cambridge, p. 274–275. Li a tions. The image data were selected on the basis of overall image quality, International Astronomical Union, 1971, Commission 16—Physical study is e n a o l ° 1 d 6 reasonable original input resolution (from 20 km/pixel for gap fill to as A ° 0 a 0 of planets and satellites, in Proceedings of the 14th General Assembly, 2 0 0 0 4 ° p 3 much as 40 m/pixel), and availability of moderate emission/incidence ° 2 Brighton, 1970: Transactions of the International Astronomical Union, a y –70 e t 70 ° s ° angles for topography and albedo. Although consistency was achieved n v. 14B, p. 128–137. s i u A Flex L where possible, different filters were included for global image coverage as ———1980, Working Group for Planetary System Nomenclature, in Pro- Delphi necessary: clear/blue for Voyager 1 and 2; clear, near-IR (757 nm), and ceedings of the 17th General Assembly, Montreal, 1979: Transactions green (559 nm) for Galileo SSI. Individual images were projected to a of the International Astronomical Union, v.17B, p. 300. s a s u Sinusoidal Equal-Area projection at an image resolution of 500 m/pixel. u s ———1986, Working Group for Planetary System Nomenclature, in Pro- e ex in Fl a Cyclades The final constructed Sinusoidal projection mosaic was then reprojected to L h ceedings of the 19th General Assembly, New Delhi, 1985: Transac- . T Macula the Mercator and Polar Stereographic projections included on this sheet. tions of the International Astronomical Union, v.19B, p. 351. hynia T on NOMENCLATURE ———1999, Working Group for Planetary System Nomenclature, in Pro- Sid 60° ceedings of the 23rd General Assembly, Kyoto, 1997: Transactions of –60° ° Names on this sheet are approved by the International Astronomical Union 1 us ° 30 30 50 Flex a 10 ° 3 e 2 (IAU, 1980, 1986, 1999, and 2001). Names have been applied for features the International Astronomical Union, v.23B, p. 234–235. ° ia c n ili i clearly visible at the scale of this map; for a complete list of nomenclature ———2001, Working Group for Planetary System Nomenclature, in Pro- C L a ceedings of the 24th General Assembly, Manchester, 2000: Transac- by of Europa, please see http://planetarynames.wr.usgs.gov. Font color was Li 55° tions of the International Astronomical Union, v.24B [in press]. –55° 0° chosen only for readability. 180° Je 15M CMN: Abbreviation for Jupiter, Europa (satellite): 1:15,000,000 Kirk, R.L., Thompson, K.T., Becker, T.L., and Lee, E.M., 2000, Photomet- SCALE 1:8 388 000 (1 mm = 8.39 km) AT 56° LATITUDE series, controlled mosaic (CM), nomenclature (N) (Gree- ric modeling for planetary cartography, in Lunar and Planetary Sci- SCALE 1:8 388 000 (1 mm = 8.39 km) AT –56° LATITUDE POLAR STEREOGRAPHIC PROJECTION POLAR STEREOGRAPHIC PROJECTION ley and Batson, 1990). ence Conference XXXI: Houston, Lunar and Planetary Institute, abs. 500 400 300 200 100 50 0 50 100 200 300 400 500 no. 2025 [CD-ROM]. 500 400 300 200 100 50 0 50 100 200 300 400 500 90° 90° REFERENCES McEwen, A.S., 1991, Photometric functions for photoclinometry and other –90° –90° 70° 70° Batson, R.M., 1987, Digital cartography of the planets—New methods, its applications: Icarus, v. 92, p. 298–311. –70° –70° 55 55 –55 –55 ° ° status, and its future: Photogrammetric Engineering and Remote Sens- Torson, J.M., and Becker, K.J., 1997, ISIS—A software architecture for ° ° KILOMETERS ing, v. 53, no. 9, p. 1211–1218. processing planetary images, in Lunar and Planetary Science Confer- KILOMETERS NORTH POLAR REGION Becker, T.L., Archinal, B., Colvin, T.R., Davies, M.E., Gitlin, A., Kirk, ence XXVIII: Houston, Lunar and Planetary Institute, p. 1443. SOUTH POLAR REGION North 360° 350° 340° 330° 320° 310° 300° 290° 280° 270° 260° 250° 240° 230° 220° 210° 200° 190° 180° 170° 160° 150° 140° 130° 120° 110° 100° 90° 80° 70° 60° 50° 40° 30° 20° 10° 0° 57° 57° 50° 50° M ino s a ine L L os ea in in Lin e M a s adm 40° mu C u 40° ad s C Pela go n Li L nea in Tyre e a a nea Li e 30 a in 30 ° L ° e a A ni n R o m i g r a ha a e L a H in a d Te L v a c t e e m am a n u i n s t s h L u y ri s ë 20° o 20° te n P hoen o s ix t A a u e a e in A o in L L L inea n I s L o C onamara i L e .