GEOCIENCIAS-VOL 13-2 2009.vp 97 EARTH SCIENCES RESEARCH JOURNAL Earth Sci. Res. J. Vol. 13, No. 2 (December 2009): 97-107 GEOPHYSICAL EVIDENCE FOR AN IMPACT CRATER IN VICHADA, NORTHWESTERN SOUTH AMERICA AND ITS ECONOMIC POTENTIAL Orlando Hernández1,2, Ralph R.B. von Frese2,3, Khurama, S.1,4 1 Dept. of Geosciences, Universidad Nacional de Colombia, Bogotá, D.C., Colombia ohernandezp@unal.edu.co 2 School of Earth Sciences & Byrd Polar Research Center, The Ohio State University, Columbus, OH 43210, USA 3 Laboratory for Space Geodesy & Remote Sensing Research, The Ohio State University, Columbus, OH 43210, USA 4 Ingeominas. Bogotá, D.C., Colombia ABSTRACT A prominent positive free-air gravity anomaly mapped over a roughly 50-km diameter basin is consistent with a mascon cen- tered on (4°30`N, -69°15`W) in the Vichada Department, Colombia, South America. The inferred impact crater is nearly one third the size of the Chicxulub Crater. It must have formed recently, in the last 30 m.a because it controls the path of the Vichada River. The impact crater structure has been partially eroded and is almost completely covered by vegetation. No an- tipodal relationship has been established. The proposed impact appears to have contributed to the development of mineral de- posits of economic interest. The impact shock waves extensively thinned and disrupted the Precambrian cratonic crust. A thick sedimentary cover, dense vegetation and erosional processes greatly limits direct geological testing of the inferred im- pact basin. Ground follow up gravity and magnetic surveys are recommended for confirming the regional free air gravity anomalies. Key words: Impact crater, Vichada, Gravity, Magnetic. RESUMEN Una anomalía gravimétrica positiva de aire libre ha sido mapeada sobre una Cuenca de aproximadamente 50 km de diámetro, la cual coincide con la ubicación de una concentración de masa o MASCON, centrada en las coordenadas 4o30`N, -69o15`, en el Departamento de Vichada, Colombia, Suramérica. La estructura de impacto de meteorito inferida corresponde a una tercera parte del tamaño de la estructura de impacto de Chicxulub. Esta estructura debe haberse formado en los últimos 30 m.a. debido a que controla la trayectoria del río. La estructura de impacto ha sido parcialmente erosionada y está casi completamente cubierta por una densa vegetación. No se han establecido relaciones anti polares. El impacto de meteorito propuesto pudo haber contribuido al desarrollo de depósitos minerales de interés económico. Las ondas de choque han adelgazado y distorsionado intensamente la corteza cratónica precámbrica. Una delgada secuencia sedimentaria, la vegetación densa y los procesos erosivos limitan considerablemente la verificación de la estructura mediante geología de superficie. Se recomienda realizar estudios de gravimetría y magnetometría terrestre para confirmar la ocurrencia de las anomalías gravimétricas regionales asociadas a la estructura. Manuscript received: 11/06/2009 Accepted for publication: 20/11/2009 ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:13 p p p Composite 133 lpi at 45 degrees Palabras clave: estructura de impacto, Vichada, Gravimetría, Magnetometría. Introduction The Vichada structure is located in the southern region of the Vichada Department, Colombia (4º30’N – 69º15’W), hav- ing a multiple ring structure with inner and outer ring diame- ters of 30 km and 50 km, respectively (figure 1).The Vichada structure was initially proposed by Rocca (2004) who recognized a possible large impact crater structure based on the remote sensing interpretation of color Landsat satellite images of the area, with a resolution of 200m, ob- tained from the NASA’s John C. Stennis Space Center, USA (figure 2, Rocca, 2004). This area is part of the Vichada Plain and it is partially covered by quaternary deposits and vegetation. The central core consists of a ring about 30 Km. in diameter which surrounds a central depression of circular shape and 20 Km. in diameter. In this innermost region, there is a basin, the relief is quite smooth and it is the deepest part of the structure. The central basin is covered by dense vegetation and it is surrounded by 2 concentric rings of low hills of few meters each that have been intensively eroded. The outermost ring has 50 Km in diameter and in the South, the Vichada River flows around it in a perfect semi-circle path following the external limits of this outer ring of hills. The outer ring also controls some local drainage systems in the North and northwest. The flow of the rivers around these features is anomalous. The geology of the area is limited ex- posed and is represented by tertiary sandstone and claystone formations, covered by quaternary deposits (De la Espriella et al., 1990). The crystalline basement is formed by the Pre- cambrian Parguazan granite, outcropping along the Vichada and Orinoco rivers far away to the east of the studied area. The hidden geology includes metasedimentary and granitic rocks with an extensive sedimentary cover. The sedimentary 98 ORLANDO HERNÁNDEZ, RALPH R.B. VON FRESE AND KHURAMA, S. Figure 1: Geographic location of the Vichada Structure in Eastern Colombia, northwestern South America. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:13 p p p Composite 133 lpi at 45 degrees units are composed by a heterogeneous sequence of con- glomerates, sandstones and clays. They are dated Oligocene to Pliocene and they cover the Precambrian crystalline base- ment rocks. The structure was forwarded modeled for grav- ity and magnetic signatures that were compared with observed gravity and magnetic profiles (Khurama, 2007). This forward modeling eliminates the possibility of the pres- ence of other geological causative bodies such as igneous in- trusions, Maars, Diatremes or sedimentary structures, leaving the model of an impact crater as the most probable phenomenon that could generate the circular structure. Rocca (2004) suggested that the Vichada structure is proba- bly older than 30 Ma. There is not additional available geo- chronological data to support the age of the structure. The Vichada flat plain is located east of the Andean mountains. This part of northwestern South America has poorly been studied for crustal properties. The lack of air- borne and terrestrial geophysical data and poorly known ge- ology has been recognized in global databases such as the CRUST 2.0 model (Bassin et al., 2000) that assignees crustal thickness to the Guiana Craton taken data from other cratonic areas of the world. Extending the hunt for impact basins into South America is problematic because the jungle and quaternary deposits cover more than 95% the crust and the remote environment greatly limits field studies. Thus, our understanding of the geological and geophysical proper- ties of the crust is very poor. However, EGM96 spherical harmonic Earth Gravity Model to degree and order 360, EGM96 data (Lemoine, et al., 1998) provides important de- tails of the gravity field that can further our understanding of the crustal features. Spectral correlation theory was used to analyze the co-registered FAGA and TGE for their anomaly correlations. Specifically, the Fourier transforms T and F of TGE and FAGA, respectively, were used to obtain their correlation spectrum (von Frese et al., 1997a, Kim, et al., 2000) given by CC k k F k T k T k F k ( ) cos( ) Re ( ) ( ) ( ) ( ) � � � � � � � � where CC(k) is the correlation coefficient between the kth wavenumber components F(k) and T(k), and denotes tak- ing the real parts of the wavenumber components. Usually, 99 GEOPHYSICAL EVIDENCE FOR AN IMPACT CRATER IN VICHADA, NORTHWESTERN SOUTH AMERICA AND ITS ECONOMIC POTENTIAL Figure 2: TM image of the Vichada structure showing the Vichada river, the inner and out ring structures of 30 km and 50 km diameter, re- spectively (modified from Rocca, 2004) ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:14 p p p Composite 133 lpi at 45 degrees CC(k) is evaluated from the cosine of the phase difference between the two kth wavenumber components. Using the correlation spectrum between FAGA and TGE, spectral cor- relation filters were designed to extract terrain-correlated free-air gravity signals. Those wavenumber components showing intermediate to high positive (CCp(k) > 0.3) and negative (CCn(k) < 0.3) correlations were identified. The cut off values for the correlation filter were determined to mini- mize correlative features between the terrain-decorrelated free air and compensating terrain gravity components. In- 100 ORLANDO HERNÁNDEZ, RALPH R.B. VON FRESE AND KHURAMA, S. Terrain - correlated free - air gravity anomalies TDFAGA mGals TCFAGA mGals Terrain - decorrelated free - air gravity anomalies Corrected terrain gravity anomalies MOHO km CTGE mGals Depth to MOHO (km) Figure 3. Gravity anomaly maps including: a) Terrain correlated free air gravity anomalies, TCFAGA b) terrain decorrelated free air gravity anomalies, TDFAGA c) Compensated terrain gravity effects CTGE and d) depth to Moho, calculated at 20 km altitude. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:15 p p p Composite 133 lpi at 45 degrees versely transforming positively and negatively correlated free-air wavenumber components according to the selected cut off values yielded the terrain-correlated free air gravity anomalies (TCFAGA) in Figure 3.a. The residual ter- rain-decorrelated free-air gravity anomalies (TDFAGA) in Figure 3.b were calculated by subtracting TCFAGA from FAGA, so that FAGA = TCFAGA + TDFAGA TCFAGA are explained by anomalies associated with the topography while TDFAGA include the gravity effects of sources within the crust (i.e., local bodies) and the subcrust. As a result, figure 3 Shows a) the terrain correlated Free Air Gravity Anomalies (TCFAGA), b) terrain de-correlated free air gravity anomalies (TDFAGA), c) the compensated terrain gravity effects (CTGE) and d) inversely modeled depth to MOHO, respectively, calculated at 20 km from the Earth Gravity Model 1996 (Hernández, et al., 2008) that is con- strained by 30-arc minute averages of available surface gravity values and gravity estimates from orbital variations of satellites operating at altitudes generally higher than 700 km (Lemoine et al., 1998). TCFAGA and TDFAGA have been obtained by spectrally correlated Terrain gravity ef- fects (TGE) and free air gravity anomalies (FAGA). Simi- larly, FCTGE and FDTGE were calculated. TCFAGA detail is particularly significant over the Vichada structure. The ter- restrial EGM96 anomaly estimates in Figure 3 essentially re- flect the lower order effects from gravity observations located some ± 20 km. The EGM-96 results include the prominent positive anomaly feature that overlies the Vichada Structure basin in Figures 1 and 2 centered on (4º30’N – 69º15’W) in the Vichada Plain. It consists of a cir- cular central positive anomaly flanked by a negative ring anomaly that in isometric view looks like a Mexican som- brero. The sombrero anomaly is commonly observed over gi- ant impact basins on the Moon and Mars, where it is attrib- uted to the effects of uncompensated concentrations of mass produced within the crust from the impact (figure 4; von Frese et al, 2009). The central positive free-air gravity anomaly results from the subjacent concentration of en- hanced mass or ‘mascon’ of uncompensated components of 101 GEOPHYSICAL EVIDENCE FOR AN IMPACT CRATER IN VICHADA, NORTHWESTERN SOUTH AMERICA AND ITS ECONOMIC POTENTIAL Orientale Basin, Moon Isidis Basin, Mars WLIC Orientale, Moon Isidis Basin, Mars WLIC, Antarctica Figure 4: Terrain gravity effects (left), Free air gravity anomalies (center) and Depth to Moho (right) of giant impact craters including the Orientale basin in the moon (up), the Isidis basin in Mars (middle) and the Wilkes Land impact crater in Antarctica (bottom; von Frese et. al., 2009). The Vichada structure has similar features in gravity anomaly maps. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:15 p p p Composite 133 lpi at 45 degrees any basaltic fill in the crater and the mantle plug intruded into the crust when it recoiled from meteorite impact. The strength of the lithosphere presumably supports the mascon against mass-equilibrating isostatic forces to produce the central gravity maximum. Lithospheric strength also main- tains the isostatically under-compensated thickened crust around the mantle plug to produce the flanking ringed free-air minimum. In the sections below, we quantitatively model the crustal properties of the inferred Vichada impact crater from the EGM-96 and terrain data. We also consider the implica- tions of the inferred impact for the development potential economic deposits. Gravity anomaly modeling Figure 3 provides more detailed views of the EGM-96 free-air gravity anomalies at 20-km altitude superposed on the terrain topography of the Vichada study area. Gravity anomaly estimates were derived from the EGM-96 gravity model evaluated to spherical harmonic degree and order 90 to emphasize the more robust qualities of the EGM-96 mea- surements. The higher frequency components, for example, are relatively poorly determined according to the model’s covariance properties. And at lower altitudes, the anomaly estimates have dramatically increasing noise levels, as well as decreasing reliability due to the lack of terrestrial gravity observations (von Frese et al., 1999) and the lack of unique- ness of the gravity modeling (von Frese et al., 2005). TCFAGA and TGE were normalized to facilitate recog- nizing the anomaly correlations between them (von Frese et al., 1997). To enhance the visual perception of the anomaly correlations, the following transformation was applied: Zi (X) = � � � �z xi x x z � � � � � � � where �z and represent the values of the mean and stan- dard deviation, respectively, of the signal X. The expression in parentheses standardizes the xi coefficients to zero mean and unit standard deviation and is dimensionless. However, the values for mean and standard deviation of of the normal- ized signal Z can be specified by the user to facilitate the vi- sual analysis. Local favorability indices (Merriam and Sneath, 1966) were used to highlight the various anomaly correlations in the normalized TCFAGA and FCTGE (figure 5). Positively correlated features were mapped out by summed local favorability indexes (SLFI) obtained by: SLFI zi X z z zi Y z z i � � ( ( ) ) ( ( ) )� � � � where Z(X) and Z(Y) were the normalized TCFAGA and TGE coefficients, respectively. The peak-to-peak correla- tions between the two data sets were mapped out by positive SLFIi (figure 5a), whereas trough-to-trough correlations were mapped out by the negative coefficients of SLFIi (fig- ure 5b). The SLFI coefficients brought out the positively or directly correlated features, while suppressing the nega- tively and null correlated features between TCFAGA and TGE. To enhance the perception of inversely correlated fea- tures obtained from wavenumbers with negative correlation coefficients, the normalized and scaled datasets were sub- tracted cell by cell for differenced local favorability indexes (DLFI) by: DLFI zi X z z zi Y z z i � � ( ( ) ) ( ( ) )� � � � Positive features in TCFAGA which were correlative with negative TGE features (peak-to-trough) were mapped out by positive DLFI in Figure 5c, whereas negative TCFAGA that were correlative with positive TGE were mapped out by negative DLFI in Figure 5d. The DLFI coeffi- cients emphasized the inversely correlated features, while suppressing the positively and null correlated features be- tween TCFAGA and TGE. With an exception of figure 5b, it is clear how the SLFI and DLFI products show local favorability indices that enhance the Vichada impact struc- ture. The mascon gravity anomaly in Figure 6 consists of the well-defined relatively positive 26 mGal anomaly overlying the inferred impact basin. To evaluate the inferred mascon’s first order crustal properties, Moho relief was determined with gravity effects that fully nullified the gravity effects of the terrain. Then, this Moho relief was adjusted to lower lev- els until it nullified the EGM-96 mascon free-air gravity anomaly. Thus, the mascon was interpreted underlying the basin as the uncompensated component of the mantle plug given by the difference between the two Moho levels. The modeling, although not unique, accounts for the independ- ently observed terrain and gravity data of the study region. The spherical coordinate gravity effects of the terrain were modeled at 20 km altitude using Gauss-Legendre quadrature integration (von Frese et al., 1981; Hernandez, 2006) and a density of 2.85 gm/cm3 for the components of the terrain. The altitude of 20 km was chosen for modeling these effects to limit local terrain density errors (Leftwich et al., 2005). Then, Moho variations were modeled from the in- 102 ORLANDO HERNÁNDEZ, RALPH R.B. VON FRESE AND KHURAMA, S. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:15 p p p Composite 133 lpi at 45 degrees 103 GEOPHYSICAL EVIDENCE FOR AN IMPACT CRATER IN VICHADA, NORTHWESTERN SOUTH AMERICA AND ITS ECONOMIC POTENTIAL TCFAGA (peak) - to - FCTGE (peak) SLFI peak - to - peak SLFI Trough- to - trough TCFAGA (trough) - to FCTGE (trough) TCFAGA (peak) - to - FCTGE (trough) DLFI T eakrough - to - p DLFI Peak - to - trough TCFAGA (trough) - to - FCTGE (peak) Figure 5: Local favorability indices including a) SLFI TCFAGA peak to FCTGE peak, b) SLFI TCFAGA trough to FCTGE trough c) DLFI TCFAGA peak to FCTGE trough and d) DLFI TCFAGA trough to FCTGE Peak. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:16 p p p Composite 133 lpi at 45 degrees version of complete Bouguer anomalies obtained by sub- tracting the terrain gravity effects from zero free-air anomalies. For this modeling, a horizontal density contrast of 0.4 g/cm3 was assumed between mantle and crust fully compensated the basin’s crust across the Moho. Figure 6 summarizes the modeling results on a profile along E-W for an inverse modeling using the utilities from GM-SYS. The geological model shows the inferred Moho esti- mates that characterize the mantle plug beneath the impact ba- sin as being some 30-km across and 5-km thick. These spatial dimensions are probably minimal because erosion, sedimen- tation, and viscous relaxation of the crust have muted the to- pography. However, the overlying positive EGM-96 free-air anomaly suggests that the crustal model may not be com- pletely compensated. Therefore, the inferred Moho was ad- justed to obtain the equilibrium Moho with gravity effects that effectively nullify the EGM-96 free-air anomaly. Discussion The crustal modeling suggests that the mantle component in Figures 3d and 6 can account for the mascon of the inferred Vichada impact crater. The diameter D1 � 50 km of its cen- tral basin ring estimated from the topography is nearly one third times the 180-km central basin diameter of Chicxulub impact crater. Large multi-ring basins of the Moon and other terrestrial planets appear to follow the Dn n� ( )2 1 D1 ring spacing rule for the diameter Dn of the nth-ring (e.g., Spudis, 2005). By this rule, the Vichada impact crater roughly inter- sects the Vichada River as shown in Figures 1 and 2. This result raises the interesting possibility that meteor- ite-impacted crust influenced the formation of mineral and hydrocarbon deposits of economic interest in the area, as proposed for the Sudbury impact crater and associated min- eral deposits in Ontario, Canada (Wilson, 1989). The most expedient and viable test of the inferred Vichada structure mascon is to explore for confirming anomalies with airborne gravity and magnetic surveys. Impacts such as Chicxulub are also known to modify crustal magnetization signifi- cantly. Satellite magnetic observations mostly characterize the thinned crust of the study region as positively magne- tized consistent with the effects of post-impact igneous mod- ifications of the crust. Clearly, modern aeromagnetic surveying can provide another important test of the crustal properties of Vichada impact crater. Economic implications Resource-forming processes can be linked to approximately 25% of all terrestrial impact structures world-wide, either as 104 ORLANDO HERNÁNDEZ, RALPH R.B. VON FRESE AND KHURAMA, S. C:\VICHADA\CRATER Gravity Observed CalculatedG ra vi ty (m G al s) D ep th (k m ) 40 -10 -60 2 22 42 Crust (2.2 gm/cc) Mantle (3.25 gm/cc) Distance (km) MASCON -10 165 340 C:\VICHADA\MASCONVW Gravity Observed Calculated G ra vi ty (m G al s) D ep th (k m ) 40 -10 -60 32 36 40 Crust (2.85 gm/cc) Mantle (3.25 gm/cc) Distance (km) MASCON -10 165 340 C:\VICHADA\CRATERVW Gravity Observed Calculated G ra vi ty (m G al s) D ep th (k m ) 40 -10 -60 -0.1 -0.05 0 Distance (km) Outer ring -10 165 340 Crust (2.85 gm/cc) Inner ring Figure 6: Inversely modeled TCFAGA at 20 km, oriented E-W along the Vichada structure, enhancing the topography (upper right) and the MASCON (lower right) or mass concentration of the Mantle plug into the lower crust. ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:16 p p p Composite 133 lpi at 45 degrees a direct result of the impact event or through subsequent modification of the target rocks. Meteoroid impacts are cata- strophic events that release enormous amounts of energy that can heat, displace and metamorphose the target rocks in- stantaneously. The extreme geologic environment and pro- cesses that result from an impact event can result in the creation, or preservation of, a range of economic resources. Grieve and Masiatis (1994) predict that resource-forming processes can be linked to approximately 25% of all terres- trial impact structures, either as a direct result of the impact event or through subsequent modification of the target rocks. The Sudbury impact event was one of the largest ever recorded on the Earth, with an estimated original crater di- ameter in excess of 200 km. The impact event is predicted to have excavated a hole in the crust 20 km deep and created a melt sheet 60 km wide and 2.5 km deep (Masaitis, 1989). During the early stages of cooling of this melt, the Sudbury Igneous Complex, sulphide-rich liquids exsolved and settled to the bottom of the sheet to produce the 50 or more known Ni, Cu and PGE deposits of the Sudbury Camp. Extreme shock pressures, in excess of 35 GPa, near the point of im- pact may create impact diamonds by the direct modification of the atomic structure of graphite or coal within the target rocks. While rich concentrations of diamond may be found in impact melt rocks produced from a graphite-bearing tar- get rock, eg 1.5 Mt at 9.13 carats/t at Zapadnaja, Ukraine (Grieve and Masaitis, 1994), these solely consist of fine-grained aggregates suitable only for industrial pur- poses. The most significant example of a progenetic rela- tionship of an economic resource with an impact crater is between the Witwatersrand goldfields and the Vredefort structure where many of the mining districts are likely to have been preserved from erosion by the downwards dis- placement by several kilometres of the target rocks within the structure surrounding the Vredefort Dome. Hydrocarbon accumulations are one of most common economic resources associated with impact craters, with almost half of the twenty-six craters formed in North American basins associ- ated with commercially exploited fields. A number of geo- logic effects resulting from a meteorite impact directly affect the ability of the target rocks to generate and accumulate hy- drocarbons. The most important effect is the creation of thick layers of brecciated and faulted rock, both within and outside the crater, that can form ideal reservoir rocks that can produce at high rates of flow. These can then be “capped” by a layer of fine grained fallout that can produce a natural seal for the reservoir. Structural traps may also be produced faulting in the collapsed terraces of a complex crater. Heat transferred into the ground by the impact and stored in the deformed rocks of the central uplift and the surrounding melt and breccia can interact with ground or meteoric waters to produce local hydrothermal systems. For example, fluid inclusion studies of the 24 km diameter Haughton crater in Canada suggest that a hydrothermal system with tempera- tures between 200ºC and 600ºC existed for several thousand years following the impact event. Except for the origin of the melt, these hydrothermal systems are analogous to the con- vection cells set up by igneous intrusions and have the po- tential to remobilize metal and form epithermal deposits. Several small vein-hosted deposits have been found within, or close to, the central uplift of several impact craters, in- cluding historically mined deposits totaling 300kt grading 3% Pb, 1.5% Zn near the 55 km diameter Siljan structure in Sweden (Grieve and Masiatis, 1994). Very large impact craters, which can maintain hydrothermal activity for around a million years, can produce their own exhalative systems in the overlying sedimentary rocks. Two such de- posits, with a combined resource of over 6Mt @ 4.4% Zn, 1.4% Cu and 1.2% Pb, are formed in the sedimentary rocks of Sudbury Basin that overlie the thick sequence of impact breccia and melt. Perhaps more important than the transient hydrothermal cells driven by heat generated by the impact event, deformation of the target rocks will have a long term effect on the local hydrogeology around the impact site. The same deformed rocks that form hydrocarbon reservoirs can also be excellent aquifers. Craters can also naturally fill with water to form large lakes in wet climates. When the mouth of the river draining from the 70 km diameter Manicouagan structure was dammed it produced a reservoir with a capacity of approximately 142 trillion litres of water. Outflow from this reservoir powers two hydroelectric power stations with a combined capacity of 2500 MW per annum. The impact crater itself can form a third order basin where the deposition of sediments may be greatly different from the surrounding area. If a crater-lake is formed in a dry climate, this can pro- vide an excellent location the formation of thick evaporite de- posits. Massive oil shale deposits are found within several craters in the former USSR, containing a potential resource of close to a billion barrels of oil. The Vichada structure can be one of the seven hidden impact crater structures that may be for each known outcropping impact craters that have gener- ated associated mineral deposits. Conclusions The occurrence of an impact in the Vichada Plain, in north- western South America is consistent with the regionally dis- rupted and thinned crust of the Vichada structure which includes a local 50km diameter depression beneath a 105 GEOPHYSICAL EVIDENCE FOR AN IMPACT CRATER IN VICHADA, NORTHWESTERN SOUTH AMERICA AND ITS ECONOMIC POTENTIAL ENERO 30-GEOCIENCIAS-VOL 13-2 2009.prn D:\GEOCIENCIAS 13-2 DIC 2009\GEOCIENCIAS-VOL 13-2 2009.vp sÆbado, 30 de enero de 2010 18:16:16 p p p Composite 133 lpi at 45 degrees well-defined EGM-96 free-air gravity maximum. The crater’s terrain gravity effects accommodate an underlying roughly 30-km wide, 5-km thick mantle plug produced by crustal rebound from meteorite impact. However, the in- ferred mascon signal in the EGM-96 gravity data suggests that no more than about 70% of the mantle plug’s mass may be isostatically compensated at the Moho. The crustal ring structure of the Vichada impact crater intersects the Vichada river thus the impact pre-dated and in- fluenced the development of the Vichada river and the mor- phological features around its inner and outer rings. The impact scenario also helps explain the crustal thinning on the studied area. Impact craters have generally been poorly re- garded as targets or economic resources despite many global examples confirming their prospectivity. The greatest chance of exploration success lies in targeting craters formed in sedimentary basins for hydrocarbons; almost 50% of such structures in North America are associated with oil or gas reserves. In the quest to meet the world’s growing energy needs, an understanding of the role of hydrocarbons in meteorite impact structures may become increasingly important. This can only happen with a clearer understanding of impact structures in general and the conditions necessary to form petroleum systems within them. Identifying impact struc- tures that meet these conditions is difficult, but the results of such efforts hold the possibility of significant economic re- turns. The Vichada impact crater is supported from Land- sat-TM images and interpreted EGM-96 data. This 50km- diameter impact crater is the biggest in South America. This structure is an interesting prospect for mineral and/or hydrocarbon exploration. It has a multiple ring structure covered by a sedimentary sequence of varying thickness from 200m to 1600m. The Vichada Impact crater affected rocks from the Precambrian Guiana granitic craton and tertiary sedimentary units. A combined EM and Magnetic airborne survey is recommended to resolve additional crustal and basin properties and evaluate its economic po- tential Acknowledgements Elements of this research were produced with support from the Geophysical Group at The Universidad Nacional de Co- lombia, Fulbright Commission, Anglogold Ashanti and Colfuturo. 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