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85°W 84°W 275°E 276°E 83°W SOUTH 277°E 82°W 278°E 81°W 279°E 80°W 280°E SCALE 1:502 000 (1 mm = 502 m) AT 270° E. (90° W.) LONGITUDE Prepared on behalf of the Planetary Geology and Geophysics Pro- TRANSVERSE MERCATOR PROJECTION gram, Solar System Exploration Division, Office of Space Science, 10 10 20 30 40 6070 80 90 100 National Aeronautics and Space Administration. Manuscript approved for publication August 14, 2003 KILOMETERS CONTOUR INTERVAL 250 METERS Planetocentric latitude and east longitude coordinate system shown in black. Planetographic latitude and west longitude coordinate system shown in red.

NOTES ON BASE vation measurements associated with them. This lack of elevation measurements Contour Guide, in meters 65° 65° This map, compiled photogrammetrically from Viking Orbiter stereo image pairs, may result in contour lines that do not adequately represent some features. The pur- 5250 MC–1 is part of a series of topographic maps of areas of special scientific interest on pose of this mapping project is to produce the digital orthophoto and DTM. This 648334 4113 Mars. map provides a graphical representation of the digital products that are available. 5000 5758 4750 ADOPTED FIGURE IMAGE BASE The image base for this map employs Viking Orbiter images from orbits 682, 608, 4500 The figure of Mars used for the computation of the map projection is an oblate MC–2 MC–4 spheroid (flattening of 1/176.875) with an equatorial radius of 3396.0 km and a 912, and 334. An orthophotomosaic was created on the digital photogrammetric 4250 MC–3 polar radius of 3376.8 km (Kirk and others, 2000). The datum (the 0-km contour workstation using the DTM compiled from stereo models. Integrated Software for 4000 Imagers and Spectrometers (ISIS; Torson and Becker, 1997) provided the software 30° 30° line) for elevations is defined as the equipotential surface (gravitational plus rota- 3750 tional) whose average value at the equator is equal to the mean radius as deter- to project the orthophotomosaic into the Transverse Mercator Projection. 6457 3500 mined by Mars Orbiter Laser Altimeter (MOLA; Smith and others, 2001). NOMENCLATURE 120° 60° 3250 PROJECTION Names on this sheet are approved by the International Astronomical Union (IAU). 5964 For a complete list of IAU approved names, see the Gazeteer of Planetary Nomen- 3000 The projection is part of a Mars Transverse Mercator (MTM) system with 20° wide MC–8 MC–9 MC–10 MC–11 zones. For the area covered by this map sheet the central meridian is at 270° E. (70° clature at http://planetarynames.wr.usgs.gov. 2750 W.). The scale factor at the central meridian of the zone containing this quadrangle MTM 500k –05/277E OMKT: Abbreviation for Mars Transverse Mercator; 2500 is 0.9960 relative to a nominal scale of 1:500,000. 1:500,000 series; center of sheet latitude 5° S., longitude 277.5° E. in 2250 180° 135° 90° 45° 0° planetocentric coordinate system (this corresponds to –05/082; latitude 5° COORDINATE SYSTEM 2000 S., longitude 82.5° W. in planetographic coordinate system); orthophoto- 6558 Longitude increases to the east and latitude is planetocentric as allowed by mosaic (OM) with color-coded (K) topographic contours and nomencla- 1750 6358 IAU/IAG standards (Seidelmann and others, 2002) and in accordance with current 4112 ture (T) [Greeley and Batson, 1990] 1500 MC–17 MC–18 NASA and USGS standards (Duxbury and others, 2002). A secondary grid (printed 6558 MC–16 MC–19 1250 in red) has been added to the map as a reference to the west longitude/planeto- REFERENCES graphic latitude system that is also allowed by IAU/IAG standards (Seidelmann and 1000 6559 Duxbury, T.C., Kirk, R.L., Archinal, B.A., and Neumann, G.A., 2002, Mars Geod- 120° 60° others, 2002) and has been used for previous Mars maps. 750 esy/Cartography Working Group Recommendations on Mars Cartographic 5759 6558 CONTROL Constants and Coordinate Systems, in Joint International Symposium on Geo- 500 spatial Theory, Processing and Applications, Ottawa, Canada, 2002, Commis- –30° –30° Horizontal and vertical control was established using the Mosaicked Digital Image 250 MC–25 Model 2.0 (MDIM 2.0; Kirk and others, 2000) and MOLA data. A portion of sion IV, Working Group 9—Extraterrestrial Mapping, Proceedings: Ottawa, MTM –05/277E QUADRANGLE VIKING STEREOMODEL COVERAGE 0 MC–24 MC–26 MDIM 2.0 covering the mapping area was extracted in simple cylindrical projec- Canada, International Society for Photogrammetry and Remote Sensing –250 The following is a list of image pairs used to produce the topographic information tion. This MDIM image was georeferenced to the MOLA data with an affine trans- [http://www.isprs.org/commission4/proceedings/ paper.html]. for this map. Numbers below correspond to the numbers on the diagram above. formation. The MDIM image and georeferencing information were imported into a Environmental Systems Research Institute, 1994, Arc commands: Redlands Calif., –500 Environmental Systems Research Institute, Inc. ID IMAGE PAIR ID IMAGE PAIR ID IMAGE PAIR digital photogrammetric workstation (Miller and Walker, 1993) and used as an –750 Greeley, Ronald, and Batson, R.M., 1990, Planetary mapping: New York, Cam- 6559 065A12–059A22 065A11–059A22 059A25–064A27 orthophoto to provide horizontal control to stereopairs of Viking imagery. The hor- MC–30 –1000 065A22–059A25 065A11–059A20 059A25–064A25 izontal information was used to extract vertical control from the MOLA data. Note bridge University Press, p. 261–276. –65° –65° 065A20–059A25 065A10–059A20 059A24–064A27 that the distribution of Viking Orbiter images suitable for mapping at a scale of Kirk, R.L., Lee, E.M., Sucharski, R.M., Richie, J., Grecu, A., and Castro, S.K., –1250 2000, MDIM 2.0: A revised global digital image mosaic of Mars in Lunar and 065A19–059A25 648334 648A10–334S44 059A24–064A26 1:500,000 is uneven. Areas mapped in this series are chosen, often in blocks of two –1500 QUADRANGLE LOCATION Planetary Science XXXI:Houston, Lunar and Planetary Institute, abstract 2011 065A19–059A23 6558 065A21–058A73 059A24–064A25 or more adjacent quadrangles, based on scientific interest as well as on the availa- –1750 Photomosaic showing location of map area. An outline of [CD–ROM]. 065A18–059A25 065A19–058A73 059A24–064A24 bility of suitable data for accurate mapping. 065A18–059A24 065A13–058A71 059A24–064A23 1:5,000,000-scale quadrangles is provided for reference. Miller, S.B., and Walker, A.S., 1993, Further developments of Leica Digital Photo- –2000 065A18–059A23 065A12–058A72 059A22–064A21 CONTOURS grammetric Systems by Helava, ACSM/ASPRS Annual Convention and –2250 065A17–059A23 065A11–058A74 5758 057A47–058A67 Contours were derived from a digital terrain model (DTM) compiled on a digital Exposition, Technical Papers, v. 3, p. 256–263. –2500 065A16–059A24 6457 064A26–057A47 057A45–058A70 photogrammetric workstation using Viking Orbiter stereo image pairs with orienta- Seidelmann, P.K. (chair), Abalakin, V.K., Bursa, M., Davies, M.E., De Bergh, C., –2750 065A16–059A23 064A24–057A45 057A43–058A70 tion parameters derived from an analytic aerotriangulation. Contours were drawn Lieske, J.H., Oberst, J., Simon, J.L., Standish, E.M., Stooke, P., and Thomas, 065A16–059A22 064A21–057A45 5759 057A43–059A22 –3000 automatically using a commercial geographic information system (GIS) software P.C., 2002, Report of the IAU/IAG Working Group on Cartographic Coordi- 065A15–059A23 6358 063A44–058A73 057A43–059A20 package (Environmental Systems Research Institute, 1994). For the stereomodels, nates and Rotational Elements of the Planets and Satellites: 2000: Celestial –3250 065A15–059A21 063A42–058A75 057A41–059A20 Mechanics and Dynamical Astronomy, v. 82, p. 83–110. the local expected vertical precision, based on image resolutions, parallax-to-height –3500 065A14–059A22 063A42–058A73 4112 041A30–012A13 ratio (that is, convergence angle), and a matching accuracy of 0.2 pixel ranges from Smith, D.E., Zuber, M.T., Frey, H.V., Garvin, J.B., Head, J.W., Muhleman, D.O., 065A13–059A21 063A40–058A76 4113 041A20–013A13 –3750 42 m to 403 m, with a mean of 83 m. Elevation (in meters) is given with respect to Pettengill, G.H., Phillips, R.J., Solomon, S.C., Zwally, H.J., Banerdt, W.B., 065A13–059A20 5964 059A26–064A27 the adopted Mars topographic datum (see "Adopted Figure" section). A comparison Duxbury, T.C., Golombek, M.P., Lemoine, F.G., Neumann, G.A., Rowlands, –4000 065A12–059A20 059A26–064A26 of the DTM values at the MOLA point locations shows that the DTM is on average D.D., Aharonson, O., Ford, P.G., Ivanov, A.B., McGovern, P.J., Abshire, J.B., –4250 7 meters higher than the MOLA points (n=248,951; µ=7 m; σ=152 m). Contour Afzal, R.S., and Sun, X., 2001, Mars Orbiter Laser Altimeter (MO- –4500 lines were generated automatically using GIS software and were not edited. LA)–Experiment summary after the first year of global mapping of Mars: Because the contour lines were not edited, small closed contour lines, contour lines Journal of Geophysical Research, v. 106, p. 23,689–23,722. –4750 that intersect, and contour lines that do not match features are present. The post Torson, J.M., and K.J., Becker, 1997, ISIS—A software architecture for processing –5000 spacing for the DTM is 600 m; features that are less than 600 m in size will not be planetary images (abs.), in Lunar and Planetary Science Conference XXVIII: –5250 resolved and features that are smaller than 1800 m in size may only have four ele- Houston, Lunar and Planetary Institute, p. 1443.

Topographic Map of the Tithonium Chasma Region of Mars MTM 500k –05/277E OMKT Any use of trade, product, or firm names in this publication is for descriptive pur- By poses only and does not imply endorsement by the U.S. Government. Dimensional calibration may vary between electronic plotters and between X and Y directions on the same plotter, and paper may change size due to atmospheric con- U.S. Geological Survey ditions; therefore, scale and proportions may not be true on plots of this map. 2004 Digital files available on World Wide Web at http://pubs.usgs.gov/imap/i2806