Randolph L Kirk, Ph.D.
Randolph Kirk’s research interests span both geoscience and mapping of planetary bodies. He has participated in many missions to the Moon, Venus, Mars, asteroids, comets, and icy satellites. He helped direct planetary mapping at the USGS since the early 1990s, and has developed practical methods for topomapping by shape from shading and by adapting commercial stereo workstations to planetary use.
Recent Accomplishments
- In 2020, NASA's Mars 2020 rover Perseverance landed in Jezero crater at a site mapped by the Astrogeology Science Center. Perseverence was the ninth Mars lander or rover to go to a site we mapped, all of which landed successfully. (Starting in 1962, 10 Mars landings attempted without USGS mapping failed for a variety of reasons. Just days before Perseverence the Chinese landerTianwen-1 became the first such mission to succeed.) Perseverance also carried our maps onboard and used them to guide its final descent, a technological first.
- We are helping to design and caibrate the Europa Imaging System (EIS) cameras for NASA's Europa Clipper mission and to develop software and procedures for making controlled image and topographic maps. As part of this task, we invented and demonstrated a new technique for correcting distortions in frame images that are read out line-by-line so that they can be used for precision mapping.
- We have used stereo images of Mars obtained by different cameras with pixel scales differing up to 50x to assess the resolution and precision of digital topographic models obtained under real-world (Mars) conditions. We are currently using similar techniques with images of Earth’s Moon to quantify how topographic models can be improved by photoclinometry (shape from shading) techniques using one or multiple images.
Education
- Ph.D., Planetary Science, Minor in Physics, California Institute of Technology, January 1987
- M.S., Planetary Science, California Institute of Technology, June 1984
- B.S., Physics, Stanford University, June 1981
Space Mission Participation
- Member, Europa Imaging System Science Team, May 2015–Present
- Member, ExoMars Trace Gas Orbiter CaSSIS Science Team, August 2010–Present
- Member, LRO and Chandrayaan-1 Mini-RF Science Teams, July 2006–Present
- Member, Mars Reconnaissance Orbiter HiRISE Science Team, December 2001–Present
- Member, Mars Exploration Rovers Science Team, August 2000–June 2018
- Associate, Deep Space 1 MICAS Science Team, March 2000–December 2002
- Participating Scientist, NEAR MSI/NIS Team, August 1999–July 2001
- Associate, Imager for Mars Pathfinder Science Team, July 1996–August 1998
- Member, Mars Express HRSC Science Team, January 2000–March 2020
- Associate, Mars 96 HRSC/WAOSS Science Team, March 1993–December 1996
- Member, Cassini RADAR Instrument Team, December 1990–September 2018
- Magellan Guest Investigator, October 1990–September 1994
- Associate, Voyager Imaging Science Team, 1989
Working Groups
- Member, IAU Working Group on Cartographic Coords & Rotational Elements, August 2012–present
- Member, NASA Lunar Geodesy/Cartography Working Group, December 2007–present
- Member, NASA Mars Geodesy/Cartography Working Group, June 1998–present
- Member, ISPRS Working Group “Planetary Mapping & Remote Sensing”, November 1996–present
- Chair, November 2000-October 2004, Co-Chair, Nove
Science and Products
Filter Total Items: 165
Titan's surface at 2.2-cm wavelength imaged by the Cassini RADAR radiometer: Calibration and first results
The first comprehensive calibration and mapping of the thermal microwave emission from Titan's surface is reported based on radiometric data obtained at 2.2-cm wavelength by the passive radiometer included in the Cassini Radar instrument. The data reported were accumulated from 69 separate observational segments in Titan passes from Ta (October 2004) through T30 (May 2007) and include...
Authors
M.A. Janssen, R. D. Lorenz, R. West, F. Paganelli, R.M. Lopes, Randolph L. Kirk, Charles Elachi, S. D. Wall, W.T.K. Johnson, Y. Anderson, R.A. Boehmer, P. Callahan, Yonggyu Gim, G.A. Hamilton, K.D. Kelleher, L. Roth, B. Stiles, Alice Le Gall
Extraterrestrial GIS
No abstract available.
Authors
Trent M. Hare, Randolph L. Kirk, James A. Skinner, Kenneth L. Tanaka
Determining Titan surface topography from Cassini SAR data
A technique, referred to as SARTopo, has been developed for obtaining surface height estimates with 10 km horizontal resolution and 75 m vertical resolution of the surface of Titan along each Cassini Synthetic Aperture Radar (SAR) swath. We describe the technique and present maps of the co-located data sets. A global map and regional maps of Xanadu and the northern hemisphere hydrocarbon...
Authors
Bryan W. Stiles, Scott Hensley, Yonggyu Gim, David M. Bates, Randolph L. Kirk, Alex G. Hayes, Jani Radebaugh, Ralph D. Lorenz, Karl L. Mitchell, Philip S. Callahan, Howard Zebker, William T.K. Johnson, Stephen D. Wall, Jonathan I. Lunine, Charles R. Wood, Michael A. Janssen, Frederic Pelletier, Richard D. West, Chandini Veeramacheneni
Observations of periglacial landforms in Utopia Planitia with the High Resolution Imaging Science Experiment (HiRISE)
The region of western Utopia Planitia (80-105 degreesE, 40-55 degrees N) displays several types of landforms similar to Earth periglacial features, including scallop-shaped depressions and networks of polygonal terrains. The scalloped depressions have been proposed to originate from thermokarstic processes such as sublimation and/or melting of near-surface ground ice. Using HiRISE...
Authors
Alexandra Lefort, P.S. Russell, N. Thomas, A. S. McEwen, C. M. Dundas, Randolph L. Kirk
Size and shape of Saturn's moon Titan
Cassini observations show that Saturn’s moon Titan is slightly oblate. A fourth-order spherical harmonic expansion yields north polar, south polar, and mean equatorial radii of 2574.32 ± 0.05 kilometers (km), 2574.36 ± 0.03 km, and 2574.91 ± 0.11 km, respectively; its mean radius is 2574.73 ± 0.09 km. Titan’s shape approximates a hydrostatic, synchronously rotating triaxial ellipsoid but...
Authors
Howard Zebker, Bryan W. Stiles, Scott Hensley, Ralph D. Lorenz, Randolph L. Kirk, Jonathan I. Lunine
Mars Exploration Program 2007 Phoenix landing site selection and characteristics
To ensure a successful touchdown and subsequent surface operations, the Mars Exploration Program 2007 Phoenix Lander must land within 65° to 72° north latitude, at an elevation less than −3.5 km. The landing site must have relatively low wind velocities and rock and slope distributions similar to or more benign than those found at the Viking Lander 2 site. Also, the site must have a soil...
Authors
Raymond E. Arvidson, D. M. Adams, G. Bonfiglio, P. R. Christensen, S. Cull, Matthew P. Golombek, J. Guinn, E. Guinness, T. Heet, Randolph L. Kirk, A. Knudson, M. C. Malin, M. T. Mellon, Alfred S. McEwen, A. Mushkin, T. J. Parker, F. Seelos, K. Seelos, P.S. Smith, D. Spencer, T. Stein, Leslie K Tamppari
Ultrahigh resolution topographic mapping of Mars with MRO HiRISE stereo images: Meter-scale slopes of candidate Phoenix landing sites
The objectives of this paper are twofold: first, to report our estimates of the meter‐to‐decameter‐scale topography and slopes of candidate landing sites for the Phoenix mission, based on analysis of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images with a typical pixel scale of 3 m and Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) images...
Authors
Randolph L. Kirk, Elpitha Howington-Kraus, Mark R. Rosiek, Jeffery A. Anderson, Brent A. Archinal, Kris J. Becker, D.A. Cook, Donna M. Galuszka, Paul E. Geissler, Trent M. Hare, I.M. Holmberg, Laszlo Kestay, Bonnie L. Redding, W.A. Delamere, D. Gallagher, J.D. Chapel, Eric M. Eliason, R. Andrew King, Alfred S. McEwen
Photometric changes on Saturn's Titan: Evidence for active cryovolcanism
We report infrared spectrophotometric variability on the surface of Saturn's moon Titan detected in images returned by the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini Saturn Orbiter. The changes were observed at 7°S, 138°W and occurred between October 27, 2005 and January 15, 2006. After that date the surface was unchanged until the most recent observation, March...
Authors
Robert M. Nelson, Lucas W. Kamp, Rosaly M.C. Lopes, Dennis L. Matson, Randolph L. Kirk, Bruce W. Hapke, Stephen D. Wall, Mark D. Boryta, Frank E. Leader, William D. Smythe, Karl L. Mitchell, Kevin H. Baines, Ralf Jaumann, Christophe Sotin, Roger N. Clark, Dale P. Cruikshank, Pierre Drossart, Jonathan I. Lunine, Michel Combes, Giancarlo Bellucci, Jean-Pierre Bibring, Fabrizio Capaccioni, Pricilla Cerroni, Angioletta Coradini, Vittorio Formisano, Gianrico Filacchione, Yves Langevin, Thomas B. McCord, Vito Mennella, Philip D. Nicholson, Bruno Sicardy, Patrick G.J. Irwin, John C. Pearl
Relative age of interior layered deposits in southwest Candor Chasma based on high-resolution structural mapping
High‐resolution topography generated from stereo HiRISE (High‐Resolution Imaging Science Experiment) imagery reveals the meter‐scale structure of interior layered deposits (ILD) in southwest Candor Chasma. This study seeks to determine the age of the local ILD relative to any normal faults that can be attributed to chasma formation. The study area is located near the contact of these ILD...
Authors
Chris Okubo, Kevin W. Lewis, Alfred S. McEwen, Randolph L. Kirk
Surface processes recorded by rocks and soils on Meridiani Planum, Mars: Microscopic Imager observations during Opportunity's first three extended missions
The Microscopic Imager (MI) on the Mars Exploration Rover Opportunity has returned images of Mars with higher resolution than any previous camera system, allowing detailed petrographic and sedimentological studies of the rocks and soils at the Meridiani Planum landing site. Designed to simulate a geologist's hand lens, the MI is mounted on Opportunity's instrument arm and can resolve...
Authors
Kenneth E. Herkenhoff, John P. Grotzinger, Andrew H. Knoll, Scott M. McLennan, Catherine M. Weitz, Aileen Yingst, Robert van Vleck Anderson, Brent A. Archinal, Raymond E. Arvidson, Janet M. Barrett, Kris J. Becker, James F. Bell, Charles Budney, Mary G. Chapman, Debbie Cook, Bethany L. Ehlmann, Brenda Franklin, Lisa Gaddis, Donna M. Galuszka, Patricia A. Garcia, Paul E. Geissler, Trent M. Hare, Elpitha Howington-Kraus, Jeffrey R. Johnson, Laszlo Kestay, Randolph L. Kirk, Peter Lanagan, Ella (Contractor) Lee, Craig Leff, Justin N. Maki, Kevin F. Mullins, Timothy J. Parker, Bonnie L. Redding, Mark R. Rosiek, Michael H. Sims, Laurence A. Soderblom, Nicole Spanovich, Richard Springer, Steven W. Squyres, Daniel A. Stolper, Robert M. Sucharski, Tracie L. Sucharski, Robert M. Sullivan, James M. Torson
Titan's rotation reveals an internal ocean and changing zonal winds
Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present-day rotation period difference from synchronous spin leads to a shift of ∼0.36° per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating...
Authors
Ralph D. Lorenz, Bryan W. Stiles, Randolph L. Kirk, Michael J. Allison, Paolo Persi del Marmo, Luciano Iess, Jonathan I. Lunine, Steven J. Ostro, Scott Hensley
Geology and Surface Processes on Titan
The surface of Titan has been revealed globally, if incompletely, by Cassini observations at infrared and radar wavelengths as well as locally by the instruments on the Huygens probe. Extended dune fields, lakes, mountainous terrain, dendritic erosion patterns and erosional remnants indicate dynamic surface processes. Valleys, small-scale gullies and rounded cobbles such as those...
Authors
Ralf Jaumann, Randolph L. Kirk, Ralph D. Lorenz, Rosaly M.C. Lopes, Ellen R. Stofan, Elizabeth P. Turtle, Horst Uwe Keller, Charles R. Wood, Christophe Sotin, Laurence A. Soderblom, Martin G. Tomasko
Science and Products
Filter Total Items: 165
Titan's surface at 2.2-cm wavelength imaged by the Cassini RADAR radiometer: Calibration and first results
The first comprehensive calibration and mapping of the thermal microwave emission from Titan's surface is reported based on radiometric data obtained at 2.2-cm wavelength by the passive radiometer included in the Cassini Radar instrument. The data reported were accumulated from 69 separate observational segments in Titan passes from Ta (October 2004) through T30 (May 2007) and include...
Authors
M.A. Janssen, R. D. Lorenz, R. West, F. Paganelli, R.M. Lopes, Randolph L. Kirk, Charles Elachi, S. D. Wall, W.T.K. Johnson, Y. Anderson, R.A. Boehmer, P. Callahan, Yonggyu Gim, G.A. Hamilton, K.D. Kelleher, L. Roth, B. Stiles, Alice Le Gall
Extraterrestrial GIS
No abstract available.
Authors
Trent M. Hare, Randolph L. Kirk, James A. Skinner, Kenneth L. Tanaka
Determining Titan surface topography from Cassini SAR data
A technique, referred to as SARTopo, has been developed for obtaining surface height estimates with 10 km horizontal resolution and 75 m vertical resolution of the surface of Titan along each Cassini Synthetic Aperture Radar (SAR) swath. We describe the technique and present maps of the co-located data sets. A global map and regional maps of Xanadu and the northern hemisphere hydrocarbon...
Authors
Bryan W. Stiles, Scott Hensley, Yonggyu Gim, David M. Bates, Randolph L. Kirk, Alex G. Hayes, Jani Radebaugh, Ralph D. Lorenz, Karl L. Mitchell, Philip S. Callahan, Howard Zebker, William T.K. Johnson, Stephen D. Wall, Jonathan I. Lunine, Charles R. Wood, Michael A. Janssen, Frederic Pelletier, Richard D. West, Chandini Veeramacheneni
Observations of periglacial landforms in Utopia Planitia with the High Resolution Imaging Science Experiment (HiRISE)
The region of western Utopia Planitia (80-105 degreesE, 40-55 degrees N) displays several types of landforms similar to Earth periglacial features, including scallop-shaped depressions and networks of polygonal terrains. The scalloped depressions have been proposed to originate from thermokarstic processes such as sublimation and/or melting of near-surface ground ice. Using HiRISE...
Authors
Alexandra Lefort, P.S. Russell, N. Thomas, A. S. McEwen, C. M. Dundas, Randolph L. Kirk
Size and shape of Saturn's moon Titan
Cassini observations show that Saturn’s moon Titan is slightly oblate. A fourth-order spherical harmonic expansion yields north polar, south polar, and mean equatorial radii of 2574.32 ± 0.05 kilometers (km), 2574.36 ± 0.03 km, and 2574.91 ± 0.11 km, respectively; its mean radius is 2574.73 ± 0.09 km. Titan’s shape approximates a hydrostatic, synchronously rotating triaxial ellipsoid but...
Authors
Howard Zebker, Bryan W. Stiles, Scott Hensley, Ralph D. Lorenz, Randolph L. Kirk, Jonathan I. Lunine
Mars Exploration Program 2007 Phoenix landing site selection and characteristics
To ensure a successful touchdown and subsequent surface operations, the Mars Exploration Program 2007 Phoenix Lander must land within 65° to 72° north latitude, at an elevation less than −3.5 km. The landing site must have relatively low wind velocities and rock and slope distributions similar to or more benign than those found at the Viking Lander 2 site. Also, the site must have a soil...
Authors
Raymond E. Arvidson, D. M. Adams, G. Bonfiglio, P. R. Christensen, S. Cull, Matthew P. Golombek, J. Guinn, E. Guinness, T. Heet, Randolph L. Kirk, A. Knudson, M. C. Malin, M. T. Mellon, Alfred S. McEwen, A. Mushkin, T. J. Parker, F. Seelos, K. Seelos, P.S. Smith, D. Spencer, T. Stein, Leslie K Tamppari
Ultrahigh resolution topographic mapping of Mars with MRO HiRISE stereo images: Meter-scale slopes of candidate Phoenix landing sites
The objectives of this paper are twofold: first, to report our estimates of the meter‐to‐decameter‐scale topography and slopes of candidate landing sites for the Phoenix mission, based on analysis of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images with a typical pixel scale of 3 m and Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) images...
Authors
Randolph L. Kirk, Elpitha Howington-Kraus, Mark R. Rosiek, Jeffery A. Anderson, Brent A. Archinal, Kris J. Becker, D.A. Cook, Donna M. Galuszka, Paul E. Geissler, Trent M. Hare, I.M. Holmberg, Laszlo Kestay, Bonnie L. Redding, W.A. Delamere, D. Gallagher, J.D. Chapel, Eric M. Eliason, R. Andrew King, Alfred S. McEwen
Photometric changes on Saturn's Titan: Evidence for active cryovolcanism
We report infrared spectrophotometric variability on the surface of Saturn's moon Titan detected in images returned by the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini Saturn Orbiter. The changes were observed at 7°S, 138°W and occurred between October 27, 2005 and January 15, 2006. After that date the surface was unchanged until the most recent observation, March...
Authors
Robert M. Nelson, Lucas W. Kamp, Rosaly M.C. Lopes, Dennis L. Matson, Randolph L. Kirk, Bruce W. Hapke, Stephen D. Wall, Mark D. Boryta, Frank E. Leader, William D. Smythe, Karl L. Mitchell, Kevin H. Baines, Ralf Jaumann, Christophe Sotin, Roger N. Clark, Dale P. Cruikshank, Pierre Drossart, Jonathan I. Lunine, Michel Combes, Giancarlo Bellucci, Jean-Pierre Bibring, Fabrizio Capaccioni, Pricilla Cerroni, Angioletta Coradini, Vittorio Formisano, Gianrico Filacchione, Yves Langevin, Thomas B. McCord, Vito Mennella, Philip D. Nicholson, Bruno Sicardy, Patrick G.J. Irwin, John C. Pearl
Relative age of interior layered deposits in southwest Candor Chasma based on high-resolution structural mapping
High‐resolution topography generated from stereo HiRISE (High‐Resolution Imaging Science Experiment) imagery reveals the meter‐scale structure of interior layered deposits (ILD) in southwest Candor Chasma. This study seeks to determine the age of the local ILD relative to any normal faults that can be attributed to chasma formation. The study area is located near the contact of these ILD...
Authors
Chris Okubo, Kevin W. Lewis, Alfred S. McEwen, Randolph L. Kirk
Surface processes recorded by rocks and soils on Meridiani Planum, Mars: Microscopic Imager observations during Opportunity's first three extended missions
The Microscopic Imager (MI) on the Mars Exploration Rover Opportunity has returned images of Mars with higher resolution than any previous camera system, allowing detailed petrographic and sedimentological studies of the rocks and soils at the Meridiani Planum landing site. Designed to simulate a geologist's hand lens, the MI is mounted on Opportunity's instrument arm and can resolve...
Authors
Kenneth E. Herkenhoff, John P. Grotzinger, Andrew H. Knoll, Scott M. McLennan, Catherine M. Weitz, Aileen Yingst, Robert van Vleck Anderson, Brent A. Archinal, Raymond E. Arvidson, Janet M. Barrett, Kris J. Becker, James F. Bell, Charles Budney, Mary G. Chapman, Debbie Cook, Bethany L. Ehlmann, Brenda Franklin, Lisa Gaddis, Donna M. Galuszka, Patricia A. Garcia, Paul E. Geissler, Trent M. Hare, Elpitha Howington-Kraus, Jeffrey R. Johnson, Laszlo Kestay, Randolph L. Kirk, Peter Lanagan, Ella (Contractor) Lee, Craig Leff, Justin N. Maki, Kevin F. Mullins, Timothy J. Parker, Bonnie L. Redding, Mark R. Rosiek, Michael H. Sims, Laurence A. Soderblom, Nicole Spanovich, Richard Springer, Steven W. Squyres, Daniel A. Stolper, Robert M. Sucharski, Tracie L. Sucharski, Robert M. Sullivan, James M. Torson
Titan's rotation reveals an internal ocean and changing zonal winds
Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present-day rotation period difference from synchronous spin leads to a shift of ∼0.36° per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating...
Authors
Ralph D. Lorenz, Bryan W. Stiles, Randolph L. Kirk, Michael J. Allison, Paolo Persi del Marmo, Luciano Iess, Jonathan I. Lunine, Steven J. Ostro, Scott Hensley
Geology and Surface Processes on Titan
The surface of Titan has been revealed globally, if incompletely, by Cassini observations at infrared and radar wavelengths as well as locally by the instruments on the Huygens probe. Extended dune fields, lakes, mountainous terrain, dendritic erosion patterns and erosional remnants indicate dynamic surface processes. Valleys, small-scale gullies and rounded cobbles such as those...
Authors
Ralf Jaumann, Randolph L. Kirk, Ralph D. Lorenz, Rosaly M.C. Lopes, Ellen R. Stofan, Elizabeth P. Turtle, Horst Uwe Keller, Charles R. Wood, Christophe Sotin, Laurence A. Soderblom, Martin G. Tomasko