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: 163
Compositional stratigraphy of clay-bearing layered deposits at Mawrth Vallis, Mars
Phyllosilicates have previously been detected in layered outcrops in and around the Martian outflow channel Mawrth Vallis. CRISM spectra of these outcrops exhibit features diagnostic of kaolinite, montmorillonite, and Fe/Mg-rich smectites, along with crystalline ferric oxide minerals such as hematite. These minerals occur in distinct stratigraphic horizons, implying changing environmental conditio
Authors
J.J. Wray, B.L. Ehlmann, S. W. Squyres, J.F. Mustard, Randolph L. Kirk
Dunes on Titan observed by Cassini Radar
Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within ±30° of the equator in optically-, near-infrared-, and radar-dark regions, indicating a strong proportion of organics, and cover well over 5% of Titan's surface. Their longitudinal duneform, interactions with topography, and correlation with other aeolian f
Authors
J. Radebaugh, R. D. Lorenz, J. I. Lunine, S. D. Wall, G. Boubin, E. Reffet, Randolph L. Kirk, R.M. Lopes, E. R. Stofan, Laurence A. Soderblom, M. Allison, M. Janssen, P. Paillou, P. Callahan, C. Spencer
Recent bright gully deposits on Mars: Wet or dry flow?
Bright gully sediments attributed to liquid water flow have been deposited on Mars within the past several years. To test the liquid water flow hypothesis, we constructed a high-resolution (1 m/pixel) photogrammetric digital elevation model of a crater in the Centauri Montes region, where a bright gully deposit formed between 2001 and 2005. We conducted one-dimensional (1-D) and 2-D numerical flow
Authors
Jon D. Pelletier, Kelly J. Kolb, Alfred S. McEwen, Randolph L. Kirk
Titan's surface from the Cassini RADAR radiometry data during SAR mode
We present initial results on the calibration and interpretation of the high-resolution radiometry data acquired during the Synthetic Aperture Radar (SAR) mode (SAR-radiometry) of the Cassini Radar Mapper during its first five flybys of Saturn's moon Titan.We construct maps of the brightness temperature at the 2-cm wavelength coincident with SAR swath imaging. A preliminary radiometry calibration
Authors
F. Paganelli, M.A. Janssen, R.M. Lopes, E. Stofan, S. D. Wall, R. D. Lorenz, J. I. Lunine, Randolph L. Kirk, L. Roth, C. Elachi
Quasi-periodic bedding in the sedimentary rock record of mars
Widespread sedimentary rocks on Mars preserve evidence of surface conditions different from the modern cold and dry environment, although it is unknown how long conditions favorable to deposition persisted. We used 1-meter stereo topographic maps to demonstrate the presence of rhythmic bedding at several outcrops in the Arabia Terra region. Repeating beds are ∼10 meters thick, and one site contain
Authors
Kevin W. Lewis, Oded Aharonson, John P. Grotzinger, Randolph L. Kirk, Alfred S. McEwen, Terry-Ann Suer
Degradation of Victoria crater, Mars
The ∼750 m diameter and ∼75 m deep Victoria crater in Meridiani Planum, Mars, is a degraded primary impact structure retaining a ∼5 m raised rim consisting of 1–2 m of uplifted rocks overlain by ∼3 m of ejecta at the rim crest. The rim is 120–220 m wide and is surrounded by a dark annulus reaching an average of 590 m beyond the raised rim. Comparison between observed morphology and that expected f
Authors
John A. Grant, Sharon A. Wilson, Barbara A. Cohen, Matthew P. Golombek, Paul E. Geissler, Robert J. Sullivan, Randolph L. Kirk, Timothy J. Parker
Fluvial channels on Titan: Initial Cassini RADAR observations
Cassini radar images show a variety of fluvial channels on Titan's surface, often several hundreds of kilometers in length. Some (predominantly at low- and mid-latitude) are radar-bright and braided, resembling desert washes where fines have been removed by energetic surface liquid flow, presumably from methane rainstorms. Others (predominantly at high latitudes) are radar-dark and meandering and
Authors
R. D. Lorenz, R.M. Lopes, F. Paganelli, J. I. Lunine, Randolph L. Kirk, K. L. Mitchell, Laurence A. Soderblom, E. R. Stofan, G. Ori, M. Myers, H. Miyamoto, J. Radebaugh, B. Stiles, S. D. Wall, C. A. Wood
The imaging performance of the SRC on Mars Express
The Mars Express spacecraft carries the pushbroom scanner high-resolution stereo camera (HRSC) and its added imaging subsystem super resolution channel (SRC). The SRC is equipped with its own optical system and a 1024×1024 framing sensor. SRC produces snapshots with 2.3 m ground pixel size from the nominal spacecraft pericenter height of 250 km, which are typically embedded in the central part of
Authors
J. Oberst, G. Schwarz, T. Behnke, H. Hoffmann, K.-D. Matz, J. Flohrer, H. Hirsch, T. Roatsch, F. Scholten, E. Hauber, B. Brinkmann, R. Jaumann, D. Williams, Randolph L. Kirk, T. Duxbury, C. Leu, G. Neukum
Titan's diverse landscapes as evidenced by Cassini RADAR's third and fourth looks at Titan
Cassini's third and fourth radar flybys, T7 and T8, covered diverse terrains in the high southern and equatorial latitudes, respectively. The T7 synthetic aperture radar (SAR) swath is somewhat more straightforward to understand in terms of a progressive poleward descent from a high, dissected, and partly hilly terrain down to a low flat plain with embayments and deposits suggestive of the past or
Authors
J. I. Lunine, C. Elachi, S. D. Wall, M.A. Janssen, M.D. Allison, Y. Anderson, R. Boehmer, P. Callahan, P. Encrenaz, E. Flamini, G. Franceschetti, Y. Gim, G. Hamilton, S. Hensley, W.T.K. Johnson, K. Kelleher, Randolph L. Kirk, R.M. Lopes, R. Lorenz, D.O. Muhleman, R. Orosei, S.J. Ostro, F. Paganelli, P. Paillou, G. Picardi, F. Posa, J. Radebaugh, L.E. Roth, R. Seu, S. Shaffer, Laurence A. Soderblom, B. Stiles, E. R. Stofan, S. Vetrella, R. West, C. A. Wood, L. Wye, H. Zebker, G. Alberti, E. Karkoschka, B. Rizk, E. McFarlane, C. See, B. Kazeminejad
Cartography for lunar exploration: 2008 status and mission plans
The initial spacecraft exploration of the Moon in the 1960s-70s yielded extensive data, primarily in the form of film and television images, which were used to produce a large number of hardcopy maps by conventional techniques. A second era of exploration, beginning in the early 1990s, has produced digital data including global multispectral imagery and altimetry, from which a new generation of di
Authors
Randolph L. Kirk, Brent A. Archinal, Lisa R. Gaddis, Mark R. Rosiek
Radargrammetry on three planets
Synthetic Aperture Radar (SAR) can provide useful images in situations where passive optical imaging cannot, either because the microwaves used can penetrate atmospheric clouds, because active imaging can "see in the dark," or both. We have participated in the NASA Magellan mission to Venus in the 1990s and the current NASA-ESA Cassini-Huygens mission to Saturn and Titan, which have used SAR to se
Authors
Randolph L. Kirk, Elpitha Howington-Kraus
Determining Titan's spin state from Cassini RADAR images
For some 19 areas of Titan's surface, the Cassini RADAR instrument has obtained synthetic aperture radar (SAR) images during two different flybys. The time interval between flybys varies from several weeks to two years. We have used the apparent misregistration (by 10-30 km) of features between separate flybys to construct a refined model of Titan's spin state, estimating six parameters: north pol
Authors
B.W. Stiles, Randolph L. Kirk, R. D. Lorenz, S. Hensley, E. Lee, S.J. Ostro, M.D. Allison, P.S. Callahan, Y. Gim, L. Iess, P.P. Del Marmo, G. Hamilton, W.T.K. Johnson, R.D. West
Science and Products
Filter Total Items: 163
Compositional stratigraphy of clay-bearing layered deposits at Mawrth Vallis, Mars
Phyllosilicates have previously been detected in layered outcrops in and around the Martian outflow channel Mawrth Vallis. CRISM spectra of these outcrops exhibit features diagnostic of kaolinite, montmorillonite, and Fe/Mg-rich smectites, along with crystalline ferric oxide minerals such as hematite. These minerals occur in distinct stratigraphic horizons, implying changing environmental conditio
Authors
J.J. Wray, B.L. Ehlmann, S. W. Squyres, J.F. Mustard, Randolph L. Kirk
Dunes on Titan observed by Cassini Radar
Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within ±30° of the equator in optically-, near-infrared-, and radar-dark regions, indicating a strong proportion of organics, and cover well over 5% of Titan's surface. Their longitudinal duneform, interactions with topography, and correlation with other aeolian f
Authors
J. Radebaugh, R. D. Lorenz, J. I. Lunine, S. D. Wall, G. Boubin, E. Reffet, Randolph L. Kirk, R.M. Lopes, E. R. Stofan, Laurence A. Soderblom, M. Allison, M. Janssen, P. Paillou, P. Callahan, C. Spencer
Recent bright gully deposits on Mars: Wet or dry flow?
Bright gully sediments attributed to liquid water flow have been deposited on Mars within the past several years. To test the liquid water flow hypothesis, we constructed a high-resolution (1 m/pixel) photogrammetric digital elevation model of a crater in the Centauri Montes region, where a bright gully deposit formed between 2001 and 2005. We conducted one-dimensional (1-D) and 2-D numerical flow
Authors
Jon D. Pelletier, Kelly J. Kolb, Alfred S. McEwen, Randolph L. Kirk
Titan's surface from the Cassini RADAR radiometry data during SAR mode
We present initial results on the calibration and interpretation of the high-resolution radiometry data acquired during the Synthetic Aperture Radar (SAR) mode (SAR-radiometry) of the Cassini Radar Mapper during its first five flybys of Saturn's moon Titan.We construct maps of the brightness temperature at the 2-cm wavelength coincident with SAR swath imaging. A preliminary radiometry calibration
Authors
F. Paganelli, M.A. Janssen, R.M. Lopes, E. Stofan, S. D. Wall, R. D. Lorenz, J. I. Lunine, Randolph L. Kirk, L. Roth, C. Elachi
Quasi-periodic bedding in the sedimentary rock record of mars
Widespread sedimentary rocks on Mars preserve evidence of surface conditions different from the modern cold and dry environment, although it is unknown how long conditions favorable to deposition persisted. We used 1-meter stereo topographic maps to demonstrate the presence of rhythmic bedding at several outcrops in the Arabia Terra region. Repeating beds are ∼10 meters thick, and one site contain
Authors
Kevin W. Lewis, Oded Aharonson, John P. Grotzinger, Randolph L. Kirk, Alfred S. McEwen, Terry-Ann Suer
Degradation of Victoria crater, Mars
The ∼750 m diameter and ∼75 m deep Victoria crater in Meridiani Planum, Mars, is a degraded primary impact structure retaining a ∼5 m raised rim consisting of 1–2 m of uplifted rocks overlain by ∼3 m of ejecta at the rim crest. The rim is 120–220 m wide and is surrounded by a dark annulus reaching an average of 590 m beyond the raised rim. Comparison between observed morphology and that expected f
Authors
John A. Grant, Sharon A. Wilson, Barbara A. Cohen, Matthew P. Golombek, Paul E. Geissler, Robert J. Sullivan, Randolph L. Kirk, Timothy J. Parker
Fluvial channels on Titan: Initial Cassini RADAR observations
Cassini radar images show a variety of fluvial channels on Titan's surface, often several hundreds of kilometers in length. Some (predominantly at low- and mid-latitude) are radar-bright and braided, resembling desert washes where fines have been removed by energetic surface liquid flow, presumably from methane rainstorms. Others (predominantly at high latitudes) are radar-dark and meandering and
Authors
R. D. Lorenz, R.M. Lopes, F. Paganelli, J. I. Lunine, Randolph L. Kirk, K. L. Mitchell, Laurence A. Soderblom, E. R. Stofan, G. Ori, M. Myers, H. Miyamoto, J. Radebaugh, B. Stiles, S. D. Wall, C. A. Wood
The imaging performance of the SRC on Mars Express
The Mars Express spacecraft carries the pushbroom scanner high-resolution stereo camera (HRSC) and its added imaging subsystem super resolution channel (SRC). The SRC is equipped with its own optical system and a 1024×1024 framing sensor. SRC produces snapshots with 2.3 m ground pixel size from the nominal spacecraft pericenter height of 250 km, which are typically embedded in the central part of
Authors
J. Oberst, G. Schwarz, T. Behnke, H. Hoffmann, K.-D. Matz, J. Flohrer, H. Hirsch, T. Roatsch, F. Scholten, E. Hauber, B. Brinkmann, R. Jaumann, D. Williams, Randolph L. Kirk, T. Duxbury, C. Leu, G. Neukum
Titan's diverse landscapes as evidenced by Cassini RADAR's third and fourth looks at Titan
Cassini's third and fourth radar flybys, T7 and T8, covered diverse terrains in the high southern and equatorial latitudes, respectively. The T7 synthetic aperture radar (SAR) swath is somewhat more straightforward to understand in terms of a progressive poleward descent from a high, dissected, and partly hilly terrain down to a low flat plain with embayments and deposits suggestive of the past or
Authors
J. I. Lunine, C. Elachi, S. D. Wall, M.A. Janssen, M.D. Allison, Y. Anderson, R. Boehmer, P. Callahan, P. Encrenaz, E. Flamini, G. Franceschetti, Y. Gim, G. Hamilton, S. Hensley, W.T.K. Johnson, K. Kelleher, Randolph L. Kirk, R.M. Lopes, R. Lorenz, D.O. Muhleman, R. Orosei, S.J. Ostro, F. Paganelli, P. Paillou, G. Picardi, F. Posa, J. Radebaugh, L.E. Roth, R. Seu, S. Shaffer, Laurence A. Soderblom, B. Stiles, E. R. Stofan, S. Vetrella, R. West, C. A. Wood, L. Wye, H. Zebker, G. Alberti, E. Karkoschka, B. Rizk, E. McFarlane, C. See, B. Kazeminejad
Cartography for lunar exploration: 2008 status and mission plans
The initial spacecraft exploration of the Moon in the 1960s-70s yielded extensive data, primarily in the form of film and television images, which were used to produce a large number of hardcopy maps by conventional techniques. A second era of exploration, beginning in the early 1990s, has produced digital data including global multispectral imagery and altimetry, from which a new generation of di
Authors
Randolph L. Kirk, Brent A. Archinal, Lisa R. Gaddis, Mark R. Rosiek
Radargrammetry on three planets
Synthetic Aperture Radar (SAR) can provide useful images in situations where passive optical imaging cannot, either because the microwaves used can penetrate atmospheric clouds, because active imaging can "see in the dark," or both. We have participated in the NASA Magellan mission to Venus in the 1990s and the current NASA-ESA Cassini-Huygens mission to Saturn and Titan, which have used SAR to se
Authors
Randolph L. Kirk, Elpitha Howington-Kraus
Determining Titan's spin state from Cassini RADAR images
For some 19 areas of Titan's surface, the Cassini RADAR instrument has obtained synthetic aperture radar (SAR) images during two different flybys. The time interval between flybys varies from several weeks to two years. We have used the apparent misregistration (by 10-30 km) of features between separate flybys to construct a refined model of Titan's spin state, estimating six parameters: north pol
Authors
B.W. Stiles, Randolph L. Kirk, R. D. Lorenz, S. Hensley, E. Lee, S.J. Ostro, M.D. Allison, P.S. Callahan, Y. Gim, L. Iess, P.P. Del Marmo, G. Hamilton, W.T.K. Johnson, R.D. West