The Gamburtsev Subglacial Mountains (GSM), located near the center of East Antarctica, are the highest feature within the East Antarctic highlands and have been investigated seismically for the first time during the 2007/2008 International Polar Year by the Gamburtsev Mountains Seismic Experiment. Using data from a network of 26 broadband seismic stations and body wave tomography, the P and S wave velocity structure of the upper mantle beneath the GSM and adjacent regions has been examined. Tomographic images produced from teleseismic P and S phases reveal several large-scale, small amplitude anomalies (δVp = 1.0%, δVs = 2.0%) in the upper 250 km of the mantle. The lateral distributions of these large-scale anomalies are similar in both the P and S wave velocity models and resolution tests show that they are well resolved. Velocity anomalies indicate slower, thinner lithosphere beneath the likely Meso- or Neoproterozoic Polar Subglacial Basin and faster, thicker lithosphere beneath the likely Archean/Paleoproterozoic East Antarctic highlands. Within the region of faster, thicker lithosphere, a lower amplitude (δVp = 0.5%, δVs = 1.0%) slow to fast velocity pattern is observed beneath the western flank of the GSM, suggesting a suture between two lithospheric blocks possibly of similar age. These findings point to a Precambrian origin for the high topography of the GSM, corroborating other studies invoking a long-lived highland landscape in central East Antarctica, as opposed to uplift caused by Permian/Cretaceous rifting or Cenozoic magmatism. The longevity of the GSM makes them geologically unusual; however, plausible analogs exist, such as the 550 Ma Petermann Ranges in central Australia. Additional uplift may have occurred by the reactivation of pre-existing faults, for example, during the Carboniferous-Permian collision of Gondwana and Laurussia.
If you can't find a tool you're looking for, please click the link at the top of the page to "Go to old article view". Alternatively, view our Knowledge Base articles for additional help. Your feedback is important to us, so please let us know if you have comments or ideas for improvement.
 The Gamburtsev Subglacial Mountains (GSM) are located near the center of East Antarctica, reaching elevations of ~3 km with relief on the order of 1–2 km that is characterized by classic alpine geomorphology (Figures 1 and 2) [Bo et al., 2009; Ferraccioli et al., 2011]. The 2–3 km thick East Antarctic ice sheet obscures the geology and tectonic structure of the GSM and precludes the collection of geologic samples. Therefore, with only reconnaissance-scale geophysics, it has been difficult to determine the origin of the high and rugged topography.
 Tectonic reconstructions of East Antarctica and geochemical studies of the interior based on U-Pb ages from detrital zircons, as well as 40Ar/39Ar ages from detrital hornblends suggest that the last major tectonic event in the East Antarctic interior was prior to 480 Ma [van del Flierdt et al., 2008; Veevers and Saeed, 2011], leading some to suggest the GSM could be a remnant of the Australian Pinjarra Orogeny [Fitzsimons, 2003] or formed through a series of ancient collisional orogenies spanning from 1.0 to 0.5 Ga [Veevers and Saeed, 2008]. More recent uplift may have been accomplished by crustal shortening during the Variscan collision of Gondwana and Laurussia [Veevers, 1994], Permian convergence along the Paleo-Pacific margin of East Antarctica [Lisker et al., 2003], or by a combination of erosional unloading, Permian and Cretaceous rift flank uplift of a postulated East Antarctic rift system, and warming of the crustal root beneath the GSM [Phillips and Läufer, 2009; Ferraccioli et al., 2011]. Alternatively, Sleep  notes that thinner lithosphere (~150–220 km) in the vicinity of the GSM [Morelli and Danesi, 2004] is characteristic of Cenozoic magmatism and suggests that the GSM represents a young hotspot orogeny, similar to the Hoggar Massif in the central Sahara.
 In this study, we use P and S wave travel time residuals from teleseismic events recorded by the Gamburtsev Mountains Seismic Experiment (GAMSEIS) to produce tomographic images of the upper mantle velocity structure beneath the GSM and adjoining regions of East Antarctica. The results provide new constraints on both the origin of the GSM and the tectonic framework of central East Antarctica. Following a brief review of the tectonic history and past geophysical studies of the East Antarctic lithosphere, we present the data and methods used in the tomographic inversions along with the resulting P and S wave velocity models, and then in the final section we discuss the implications of the tomographic images for the tectonic framework of central East Antarctica and the origin of the GSM.
2.1 Tectonic History of East Antarctica
 Little is known of the geology and tectonic history of East Antarctica due to the 2–3 km thick East Antarctic ice sheet that obscures all but a handful of outcrops along the coast and in the Transantarctic Mountains (TAM; Figure 1). In situ geologic studies indicate that Archean to Proterozoic outcrops prevail along the East Antarctic coast [Tingey, 1991] and Proterozoic outcrops are seen throughout the Transantarctic Mountains [Goodge et al., 2001]. Most tectonic reconstructions have therefore assumed that East Antarctica is a Precambrian shield with an Archean nucleus that formed prior to or during the amalgamation of Rodinia [Dalziel, 1991; Hoffman, 1991; Moores, 1991; Tingey, 1991; Rogers et al., 1995], while others have suggested that the final assembly of East Antarctica was not achieved until the early Paleozoic through a series of Neoproterozoic/early Paleozoic orogenic events [Zhao et al., 1995; Fitzsimons, 2000a; Powell and Pisarevsky, 2002].
 Gondwana reconstructions show a strong correlation between the exposed coastal terranes of East Antarctica and those juxtaposed in Africa, India, and Australia (Figure 1). Regions of intense late Neoproterozoic-Early Cambrian tectonism separate three Grenville age provinces that dominate the exposed coastal terranes [Fitzsimons, 2000a, 2000b]. In particular, 600–500 Ma Pan-African age tectonism evident in the Raur group of Prydz Bay [Stüwe and Powell, 1989; Zhao et al., 1995] and Obruchev Hills in the Denman Glacier region [Fitzsimons, 2000a] may indicate the inland extension of the Australian Pinjarra Orogeny into East Antarctica between the Rayner and Wilkes provinces. Fitzsimons  suggests that ((1)) the Australian Pinjarra Orogeny cuts across East Antarctica through the GSM intersecting the Mozambique Belt in the Shackleton Range or ((2)) intersects the Ross-Delamerian Orogen in the TAM. Alternatively, Boger et al.  suggests that ((3)) this orogeny trends westward through the Lambert Terrane intersecting the Mozambique Belt somewhere in Dronning Maud Land, and a more recent reinterpretation by Boger  further suggests that Mesoproterozoic collisional belt may extend inland from the Denman Glacier region through the Vostok Subglacial Highlands (VSH) to the Shackleton Range.
2.2 Lithospheric Structure of East Antarctica
 Global and continental-scale surface wave studies of East Antarctica possessing lateral resolution no better than ~600 km indicate seismically fast upper mantle velocities resembling an old stable Precambrian shield with lithospheric thicknesses of 150 to >250 km [Roult et al., 1994; Danesi and Morelli, 2000, 2001; Ritzwoller et al., 2001; Morelli and Danesi, 2004; Kobayashi and Zhao, 2004]. While some of the lithosphere in East Antarctica may be ≥250 km thick, thinner lithosphere (150–220 km) is suggested beneath the Wilkes Subglacial Basin (WSB) and the Polar Subglacial Basin (PSB), as well as beneath the flanks of the GSM by some models [Morelli and Danesi, 2004]. Regional studies indicate that fast upper mantle seismic velocities [Watson et al., 2006; Lawrence et al., 2006a; Heeszel et al., Rayleigh wave constraints on the structure and tectonic history of the Gamburtsev Subglacial Mountains, East Antarctica, submitted to Journal of Geophysical Research, 2012, hereafter Heeszel et al., submitted manuscript, 2012] and a region of low attenuation [Lawrence et al., 2006b] extend across much of East Antarctica, consistent with a Precambrian shield.
 Surface wave and gravity studies indicate that East Antarctica has a mean crustal thickness of 37–45 km [e.g., Danesi and Morelli, 2000; Ritzwoller et al., 2001] and gravity studies further suggest a region of thickened crust (42–63 km) beneath the GSM [Groushinsky and Sazhina, 1982a, 1982b; von Frese et al. 1999; Block et al., 2009; Ferraccioli et al., 2011]. Recent S wave receiver functions (SRFs) [Hansen et al., 2009 and Hansen et al., 2010] and Monte Carlo modeling of shear wave velocities (Heeszel et al., submitted manuscript, 2012) indicate crustal thicknesses of 55–58 km beneath the GSM and 40–45 km beneath the surrounding regions. However, one notable exception is that significantly thinner crust (30–35 km) is observed beneath GM01 (Figure 2) [Hansen et al., 2010; Heeszel et al., submitted manuscript, 2012], AGO1 (Figure 2) (Heeszel et al., submitted manuscript, 2012), and South Pole Station (34 km) [Baranov, 2011], reflecting the transition from the East Antarctic Highlands to the PSB.
3 Data and Methodology
3.1 Seismic Data
 This study utilizes data collected during the GAMSEIS broadband deployment (Figure 2) in conjunction with the 2007–2008 International Polar Year, Antarctica's Gamburtsev Provence (AGAP) project, which also consisted of an aerial geophysical survey (GAMBIT) [Bell et al., 2011; Ferraccioli et al., 2011]. Deployment of the GAMSEIS stations occurred during the 2007–2008 and 2008–2009 Antarctic field season via Twin Otter flights out of South Pole Station and AGAP-S field camp. The bulk of the GAMSEIS array was demobilized during the 2009–2010 Antarctic field season; however, eight stations remain in operation until at least 2014. The complete GAMSEIS deployment consisted of 26 broadband seismic stations. Twelve stations were arranged in a 900 km long linear array as a continuation of the TAMSEIS N-S array and included the reoccupation of the TAMSEIS stations N124 and N132 [Watson et al., 2006; Lawrence et al., 2006a]. Six stations were arranged in a second 550 km long linear array (Polar array) intersecting the first array and eight stations were installed between the two linear arrays to improve 3-D resolution (Figure 2).
 Each station consisted of three main components: (1) either a Guralp 3T or a Nanometrics T240 broadband seismometer installed beneath the snow on a phenolic block and covered by a foam “hat” and plastic dome, (2) a buried insulated box containing a Quanterra Q330 digitizer, hard disk, power module, lithium battery packs, and rechargeable batteries, and (3) a metal pole supporting three 20 W solar panels and a GPS antenna. The GAMSEIS stations operated year-round running on solar power during the austral summer and on lithium battery packs during the austral winter. Stations equipped with a Xeos iridium modem transmitted a daily “state of health” report; however, bandwidth and power limitations prohibited the acquisition of real time data. Despite the extreme conditions, a data return of 87% and 91% was achieved during 2008 and 2009, respectively.
3.2 Relative Arrival Times
 Relative arrival times have been determined using the multichannel cross-correlation (MCCC) technique of VanDecar and Crosson  on teleseismic P and S phases from events with Mw ≥ 5.5 and at distances of 30°–90° and 30°–85°, respectively (Figure 3), in the Fast Archive Recovery Method (FARM) earthquake catalog. The majority of the events are located in the southwest Pacific following the Pacific-Indian plate boundary from Tonga/Fiji to Sumatra or clustered along the South American subduction zone. A small gap in the event distribution occurs toward the central Pacific.
 Coherent P energy observed throughout all seismograms for a single event was picked from the vertical component after applying a 0.4–2.0 Hz band-pass filter. Similarly, coherent S energy was picked from the transverse component after applying a 0.04–0.2 Hz band-pass filter. The resulting P and S data sets consisted of 3891 P arrivals from 288 events and 3299 S arrivals from 261 events. When absolute arrival times could be identified, the observed P or S phases arrived earlier than predicted by the IASP91 velocity model [Kennett and Engdahl, 1991], after correcting for the ice and crustal thickness.
 Multichannel cross-correlation was applied to a windowed portion of the waveforms relative to an initial pick. A window of [−1.0 s, 2.0 s] was applied to P phases and a window of [−5.0 s, 10.0 s] was applied to S phases. For n traces, the MCCC compares the ith trace to the jth trace and determines the needed time shift (τij) relative to the ith pick to achieve the cross-correlation maximum, resulting in a series of linear equations. To further constrain the system the sum of all relative arrival times for a given event was forced to equal 0.0 s:
where N is the number of observations for a given event, TRi and TRj are the relative arrival time of the ith and jth trace, respectively, Ψ is a [2 ∗ (N − 1)!] × N matrix with entries of ±1 and 0, TR is a vector of relative arrival times, and τ is a vector containing the time shifts (τij) and the sum of all the relative arrival times for a given event (0.0 s). A linear least squares method was used to solve for the relative arrival times and the event variance (, ) [VanDecar and Crosson, 1990].
3.3 Relative Travel Time Residuals
 Theoretical arrival times were calculated using a version of the IASP91 velocity model [Kennett and Engdahl, 1991] corrected for Moho depths determined by SRFs and ice thicknesses obtained from either high frequency P wave receiver functions or ice-penetrating radar [Hansen, 2009; Hansen et al., 2010]. The corrections were made on a station-by-station basis assuming a mean crustal P wave velocity of 6.2 km/s (Vp) and S wave velocity of 3.6 km/s (Vs), while the P and S wave velocities of ice are taken to be 3.8 and 1.9 km/s, respectively. These simplified geologic models of the crust and ice are directly dependent on the delay time of the receiver functions and therefore serve as a high-precision station term that not only accounts for the geometry of the ice and crust, but also heterogeneities existing within these layers.
 Theoretical arrival times and observed relative arrival times were used to calculate the relative travel time residuals, which preserve only heterogeneity information proximal to the array using
where Δti is the relative travel time residual for the ith station, TTi is the absolute theoretical travel time at the ith station, and N is the number of observations for a given event. Average P and S wave relative travel time residuals (Figure 4) indicate delayed arrivals beneath the PSB, while the average residuals at the remaining stations are not far removed from the mean (0.0 s).
 Relative travel time residuals were inverted using a modified version of the code developed by Zhao et al. . Prior to inverting for velocity, all station and earthquake locations were rotated such that the N-S array lies along the equator. The model space was then laterally partitioned with nodes laid out in a 0.75° by 0.75° grid and vertically partitioned with a node spacing of 25 km from 0 to 400 km depth and node spacing of 50 km from 400 to 1300 km depth. This maximum depth was chosen after investigating the trade-off between the model depth and total RMS travel time residual (Figure 5a). Likewise, optimal damping (Figure 5b) and smoothing coefficients were determined by investigating a wide range of combinations in search of a solution that minimizes damping, while a second derivative smoothing matrix was used to limit high wave number features in the model.
 The method developed by Zhao et al.  finds the pierce point at the model boundary for a given event-station pair using a dichromatic approach. The raypath from pierce point to station is iteratively determined following the method of Zhao et al. , which uses Snell's law to perturb the raypath at velocity discontinuities and the pseudobending algorithm of Um and Thurber  to perturb the raypath in regions of continuous velocity. The pseudobending algorithm iteratively perturbs an initial path estimate in a piecewise fashion in order to minimize the travel time; thereby, the ray equations do not have to be directly solved. Using the calculated ray path, the partial derivatives of the travel times with respect to our modified IASP91 velocity model are calculated and a system of equations relating the relative travel time residuals to the medium parameters is determined following Aki and Lee , Thurber , and Zhao . The resulting large sparse system of equations is then inverted for a relative node velocity using a LSQR conjugate gradient algorithm [Paige and Saunders, 1982] with appropriate damping and smoothing coefficients [Zhao, 2001, 2004; Lei and Zhao, 2007]. The resulting P and S wave velocity models reduce the variance of the relative travel time residuals by ~86% and ~90%, respectively.
4.1 P Wave Results
 Horizontal slices through the P wave velocity model at depths of 150, 200, 250, and 300 km (Figure 6), as well as vertical slices along profiles A-A′ and B-B′ (Figure 7), reveal a fairly uniform velocity structure beneath the study area consisting of broad, weak anomalies with amplitudes ranging from ±0.5%, relative to the mean of the model. At lithospheric depths, these anomalies correlate well with the major terranes dissecting the region. Faster velocity anomalies (≥0.25%) extend to depths of 350 km beneath the GSM and portions of the VSH, while velocities beneath the remainder of the VSH are near the mean of the model. Slower velocity anomalies (less than or equal to −0.25%) are observed beneath the PSB and regions west of the GSM. At a depth of 350 km, velocity anomalies across the study region decrease to ±0.25%. Although some smaller features (<150 km across) do exist, they are not well resolved and thus are not used in the interpretation.
4.2 P Wave Resolution Test
 The resolution of the model has been evaluated by performing several checkerboard tests, in which synthetic travel times are calculated for a given input model. Gaussian random noise with a mean of 0.0 s and a variance of 0.02 s2 was added to the synthetic residuals in order to account for the P phase event variance of the MCCC. The synthetic travel times were inverted to determine the level at which the input model can be resolved. Figure 8 shows checkerboard resolution tests consisting of ±0.5% anomalies, with lateral dimension of ~250 × ~250 km and a thickness of 200 km centered at 100 and 300 km depth.
 The horizontal checkered structure of the input anomalies is recovered beneath the GAMSEIS array at depths of ~150–350 km, beyond which the extent of the anomalies is increasingly influenced by the divergence of the raypaths relative to the array. Vertical resolution is more limited due to the near-vertical ray paths that cause 200 km thick input anomalies to smear to thicknesses of ~300 km (Figure 9), indicating vertical resolution is greater than 100 km. More complex vertical resolution tests, not shown, indicate there is a possibility that alternating slow/fast vertical velocity patterns could go unresolved. However surface wave studies (Heeszel et al., submitted manuscript, 2012) possessing superior vertical resolution indicate such structures do not exist within the study region. Finally, amplitude recovery is between 60% and 80% beneath the N-S and Polar array, while beneath the off-array stations, amplitude recovery is at most 50%.
4.3 S Wave Results
 Horizontal slices through the S wave velocity model at depths of 150, 200, 250, and 300 km (Figure 10), as well as vertical slices along profile A-A′ and B-B′ (Figure 11), reveal anomalies of up to ±1.0%. Within the upper 250 km, lateral variations in S wave velocity are generally consistent with anomalies observed in the P wave velocity model. For example, there are faster velocities (≥0.25%) beneath the GSM and VSH and slower velocities (less than or equal to −0.5%) beneath the PSB and west of the GSM, which are consistent with the P wave velocity model. At depths greater than 250 km, the P and S wave velocity models begin to show less correlation beneath the GSM, possibly due to a more limited raypath coverage in the S wave velocity model compared to the P wave velocity model. Finally, like the P wave velocity model, some smaller-scale features (<150 km across) exist but are not reliably resolved and thus cannot be interpreted.
4.4 S Wave Resolution Test
 Similar resolution tests to those performed for the P wave velocity model were carried out for the S wave velocity model (Figures 12 and 13). Gaussian random noise with a mean of 0.0 s and a variance of 0.12 s2 was added to the synthetic residuals in order to account for the S phase event variance of the MCCC. Results from checkerboard tests with velocity anomalies of ±1.0% are similar to those of the P wave velocity model, possessing good lateral resolution between ~150 and 350 km depth. Vertical resolution is again more limited with 200 km deep anomalies smearing to ~300–350 km depth. Amplitude recovery along the N-S and Polar array is likewise between 60% and 80% and at off-array stations, where the checkered structure is recovered, at most 50% of the amplitude is recovered.
 The P and S wave velocity models show strong lateral correlation of anomalies within the upper 250 km of the mantle, but P and S wave velocity variations are small (δVp = 1.0%, δVs = 2.0%) and thus at best only first-order structures can be interpreted. These include the faster anomalies beneath the GSM and much of the VSH, as well as the slower velocity anomalies beneath the PSB and west of the GSM.
 The S wave velocity model agrees reasonably well with a regional S model obtained from surface wave tomography that incorporates data from the TAMSEIS, GAMSEIS, and POLENET deployments [Heeszel, 2011], as well as the surface wave study of Heeszel et al. (submitted manuscript, 2012) that uses only the GAMSEIS data set. In particular, at depths of 150–200 km, all models indicate faster velocities beneath the GSM and slower velocities beneath the PSB. Both surface wave studies account for azimuthal anisotropy [Heeszel, 2011; Heeszel et al., submitted manuscript, 2012], while our models assume an isotropic medium. Given this, small variations in lateral velocity in our models may be, in part, due to changes in anisotropic lithospheric fabrics that often dominated Precambrian shields [Plomerová et al., 2011].
 Lateral velocity variations in our models are too small to be well resolved by continental-scale tomographic studies; however, after vertical smearing effects are considered, the depth extent of anomalies is consistent with many other models. Anomalies in both the P and S wave velocity models extend to depths of ≥350 km, and resolution tests suggest these anomalies have smeared vertically ~100–150 km, indicating that these anomalies extend to depths of around 200–250 km. Fast structure extending to such depths (Figures 7 and 11) suggests a lithospheric thickness of 200–250 km across much of the study region, consistent with other velocity models of East Antarctica [Roult et al., 1994; Danesi and Morelli, 2000, 2001; Ritzwoller et al., 2001; Morelli and Danesi, 2004; Kobayashi and Zhao, 2004; Heeszel et al., submitted manuscript, 2012].
5.1 Implications for the Structure of Central East Antarctica
 Tomographic studies of continental shields have demonstrated that Archean and Proterozoic terranes can often be delineated based on lithospheric velocity variations, which are typically attributed to a mixture of thermal and compositional effects. Global comparisons of shear wave velocity within cratonic shields determined by surface wave analyses indicate that Meso- or Neoproterozoic lithosphere is on average 3% slower than Archean lithosphere [Lebedev and van der Hilst, 2008; Lebedev et al., 2009]. Perhaps the best example of this dichotomy is observed in southern Africa, where the Archean Kaapvaal and Zimbabwe cratons show faster seismic velocities than the surrounding Proterozoic mobile belts. Body wave tomography models of this region indicate that Archean lithosphere is ~2% for δVp and ~2.5% for δVs faster than Proterozoic lithosphere [Fouch et al., 2004]. In the following, we discuss the extent to which the anomalies in Figures 6, 7, 10, and 11 can be used to delineate terrane boundaries within central East Antarctica.
 Thinner crust [Hansen et al., 2010; Baranov, 2011; Heeszel et al., submitted manuscript, 2012] and lithosphere [Morelli and Danesi, 2004], as well as a high magnetic anomaly interpreted as unmodified Precambrian basement of the Nimrod igneous province [Finn et al., 2006; Goodge and Finn, 2010] differentiate the PSB from the surrounding East Antarctic highlands. Beneath this region, the lithosphere in our model is 1.0% for δVp and 1.7% for δVs slower than beneath the GSM (Figure 14). Resolution tests indicate that this anomaly could be underestimated by as much as 50% and thus similar in magnitude to globally observed differences in lithospheric velocity beneath Archean and Proterozoic terranes [Fouch et al., 2004; Lebedev and van der Hilst, 2008; Lebedev et al., 2009]. Zircon U-Pb ages of glacial clasts recovered in the TAM indicate the presence of ~1.1 Ga igneous crust inboard of the central TAM [Goodge et al., 2010]. If this is so, then slower seismic velocities observed beneath the PSB may reflect, at least in part, thinner lithosphere and a warmer geotherm associated with a younger Proterozoic terrane.
 Variations in δVp (0.50%) and δVs (1.0%) across the GSM and surrounding regions are too small to be readily attributed to significant variations in lithospheric thickness, even after correcting for the 20% reduction in amplitude observed across the N-S array. The velocity variations are of similar magnitude to those observed within distinct Precambrian lithospheric blocks elsewhere, such as the Kaapvaal and Zimbabwe cratons in southern Africa (δVp = 0.6%, δVs = 0.8%) [Fouch et al., 2004], unmodified Grenvillian lithosphere in North America (δVp = 0.4%, δVs = 0.6%) [Aktas and Eaton, 2006], and the São Francisco craton in South America (δVp = 0.5%, δVs = 0.8%) [Rocha et al., 2011]. This suggests that the lithosphere beneath the GSM and surrounding regions is of comparable age, although not necessarily a single unit. The variations in velocity may be accommodated by small differences in temperature, or alternatively by a ~26% difference in olivine wt.% (Vp) and a change in Mg# of ~3 (Vs) [Lee, 2003; Schutt and Lesher, 2010]. Such compositional variability is observed in xenoliths from the Kaapvaal craton [Schutt and Lesher, 2010], indicating that variations in velocity across the GSM and surrounding regions could plausibly result from compositional heterogeneity in the lithosphere.
 For example, the velocity change of 0.5% in δVp and 1.0% in δVs observed on the western flank of the GSM along the N-S array between stations N198 and N206 at 150 km depth (Figures 6, 7a, 10, and 11a) could be indicative of a suture between two lithospheric blocks with somewhat different compositions, but of similar age (Figure 14). In the P wave velocity model, the slower velocity region continues to the southwest beneath stations GM05, GM06, and GM07. In the S wave velocity model, a similar slower velocity region is observed beneath stations GM06 and GM07. In both instances, this velocity pattern correlates well with a change in magnetic fabric [Ferraccioli et al., 2011], lending support to this interpretation (Figures 6, 7a, 10, and 11a).
5.2 Implications for the Uplift of the Gamburstev Subglacial Mountains
 Our tomographic images, in conjunction with regional and global surface wave studies of Antarctica [Roult et al., 1994; Danesi and Morelli, 2000, 2001; Ritzwoller et al., 2001; Morelli and Danesi, 2004; Kobayashi and Zhao, 2004; Heeszel et al., submitted manuscript, 2012;], indicate that a cold seismically fast upper mantle underlies the majority of East Antarctica. The average Rayleigh wave phase velocity dispersion curves for the study region are most consistent with Archean or Paleoproterozoic terrains globally (Heeszel et al., submitted manuscript, 2012). Therefore, no evidence is found for a significant thermal anomaly beneath the GSM, precluding the existence of a Cenozoic hotspot as suggested by Sleep .
 A recent model for the origin of the GSM proposed by Ferraccioli et al.  invokes a combination of erosional unloading, Permian and Cretaceous rift flank uplift associated with a postulated East Antarctic rift system, and warming of the crustal root beneath the GSM. In this model, it is assumed that Permian extension and Cretaceous transtension led to the formation of a rift system similar to that of the Cenozoic East African rift system, in which rifting occurred in thinner Proterozoic lithosphere that surrounds thicker Archean lithosphere [Ritsema et al., 1998; Adams et al., 2012]. However, the amplitudes of the P and S wave velocity variations in our models are not consistent with this supposition and instead indicate little change in lithospheric thickness beneath the GSM and surrounding regions.
 In addition, as discussed previously, this region has fast velocities extending to depths of >200 km, indicative of thick Archean/Paleoproterozoic lithosphere. Cold thick lithosphere is rheologically strong and thus significant Phanerozoic extension and concomitant thinning of the lithosphere seem unlikely. Nonetheless, if the thick cratonic lithosphere somehow were rifted in the Permian and/or Cretaceous, then the thermal anomaly caused by destroying the cratonic lithosphere and replacing it with warm asthenosphere would persist to the present. For conductive heat transfer, assuming instantaneous heating of a semi-infinite half-space, the time (τ′) required for a thermal anomaly to propagate a distance l is given by
where κ is the thermal diffusivity [Turcotte and Schubert, 2002]. Using a κ of 31.5 km2/Myr and a lithosphere thickness of 200 km, the minimum time required for a thermal anomaly to reach the surface is on the order of 500 Myr and to fully dissipate ~1 Ga. The fact that thick, cold cratonic lithosphere with high seismic velocities at 150–200 km depth is not observed beneath terrains younger than Paleoproterozoic also suggests that the development of cratonic lithosphere requires times greater than 1 Ga. Therefore, a thermal anomaly associated with lithospheric thinning during a Permian and/or Cretaceous rifting event would likely be present today and be resolved in our tomographic images as a pronounced low velocity anomaly. The absence of a significant low velocity anomaly beneath the location of the proposed East Antarctic rift system indicates that our tomographic images are not consistent with the uplift model proposed by Ferraccioli et al. .
 While we have shown that the analogy to the East African rift system and the uplift model of Ferraccioli et al.  is not consistent with our tomographic images, it is still possible that the observed basins are rift features. If this is so, then our results require extension to have been limited causing only minor modification of the upper mantle or to have been accommodated within the brittle lithosphere, and thus leading to negligible rift flank uplift. A possible analog is the Karoo basin system that formed in response to extensional or transtensional stresses associated with the breakup of Gondwana [Catuneanu et al., 2005]. Similar transtensional stresses have been invoked, in part, to explain the basins in central East Antarctica by Ferraccioli et al. . Many Karoo basins formed along the margin of Archean cratons and there are no pronounced velocity anomalies beneath them [Adams et al., 2012].
 In another model for the GSM, uplift is attributed to one or more Proterozoic compressional orogenic events that are likely associated with supercontinent assembly during the Pan-African or Grenville [Fitzsimons, 2003; Veevers and Saeed, 2008; Boger, 2011], and would not necessarily destroy or thermally reset the underlying lithosphere. It is at this time that the crustal root of the GSM likely formed. The preservation of crustal roots beneath ancient compressional orogenic belts is well documented beneath the Ural Mountains [Grad et al., 2009], as well as portions of the Trans-Hudson orogeny [Hammer et al., 2011]. The combination of a low geotherm and fluid-absent conditions may have hindered the eclogitization and delamination of the crustal root beneath these orogenic belts [Leech, 2001] and similar conditions may have led to the preservation of the crustal root beneath the GSM, thus prohibiting post-orogenic extensional collapse.
 If the GSM are solely a remnant of an ancient orogenic belt, then erosion within the interior of East Antarctica must have proceeded very slowly in order for significant topography to persist to the present day. This may be possible as analyses of detrital apatites from Eocene sands in the Prydz Bay region indicate average erosion rates of 10–20 m/Myr since 250–500 Ma [Cox et al., 2010], while another study has reported erosion rates to be an order of magnitude less for the last 118 Myr [Jamieson et al., 2005]. These low long-term erosion rates are one to two orders of magnitude less than what is typically expected in high relief terranes (i.e., European Alps) [Bernet et al., 2001], requiring either a dry and arid long-term climate or an unusual glacial regime within the interior of East Antarctica [Cox et al., 2010]. The juxtaposition of East Antarctica and Australia until the late Cretaceous opens the possibility that the dry and arid Australian climate, permitting similar low erosion rates (100–101 m/Myr) and allowing many geologic features to be preserved for tens to hundred million years [Gale, 1992], may have existed within the interior of East Antarctica. For example, the Petermann Ranges in central Australia represents the remnants of a ~550 Ma compressional intraplate orogeny associated with the formation of Gondwana [Aitken et al., 2009]. Although only the stumps of this ancient orogeny remain, reaching elevations of at most 1.2 km with relief on the order of 300 m, it is clear that the preservation of ancient highland landscapes is possible, if not unusual.
 In addition to the very slow erosion rates, it is also possible that Carboniferous-Permian events, such as the collision of Gondwana and Laurussia [Veevers, 1994] or convergence along the Palaeo-Pacific margin of East Antarctica [Lisker et al., 2003] may have led to crustal shortening and reactivation of preexisting faults, thus rejuvenating the ancestral GSM. Regardless of whether or not there was any reactivation of old faults, the P and S wave velocity models in this study are consistent with an ancient origin for the GSM in which the small amplitude velocity variations within and surrounding the GSM are caused primarily by compositional variations between lithospheric blocks that may be of similar age.
6 Summary and Conclusions
 This study utilizes broadband seismic data collected as part of the GAMSEIS deployment in order to develop both P and S body wave tomography models. Relative arrival times from teleseismic events were determined using the MCCC technique of Van Decar and Crosson , and relative travel time residuals were calculated using a modified version of the IASP91 velocity model that accounts for the geometry and heterogeneity of the ice and crust beneath each station. Relative travel time residuals were inverted using the method of Zhao et al.  to obtain both P and S wave velocity models. Classical checkerboard resolution tests were performed to determine the level of resolution achieved by the models. These tests indicate that anomalies similar in magnitude and scale to those observed in the tomographic images are well resolved.
P and S wave velocity models exhibit small variation in velocity with a nearly identical distribution of fast and slow anomalies within the upper 200–250 km. These anomalies indicate at least two distinct lithospheric blocks that differentiate the slower and likely Meso- or Neoproterozoic PSB from the faster and likely Archean/Paleoproterozoic East Antarctic highlands. Lithospheric velocity variations beneath the East Antarctic highlands are similar to those observed globally within discrete lithospheric blocks. A transition from faster velocities to slower velocities beneath the western flank of the GSM correlates well with a change in magnetic fabric [Ferraccioli et al., 2011] and can be interpreted as a suture between two lithospheric blocks that maybe of similar age. Although much of the tectonic framework in the interior of East Antarctica is still unknown, these results provide important pinning points within the center of East Antarctica (Figure 14) that future tectonic models must take into account.
 The small variations in seismic velocities within and surrounding the GSM are inconsistent with the Cenozoic hotspot model of Sleep , and also the presence of an analogous East African rift system within the interior of East Antarctica that was most recently active in the Permian and/or Cretaceous, as proposed in the uplift model of Ferraccioli et al. . Instead our models suggest an ancient origin for the GSM, such as an orogenic event associated with supercontinent assembly during the Neoproterozoic, followed by very slow erosion of the landscape through the Phanerozoic. Possible rejuvenation of the ancestral GSM may have occurred from the Carboniferous-Permian collision of Gondwana with Laurussia or from convergence along the Paleo-Pacific margin of East Antarctica. Regardless of whether or not additional uplift occurred during the Phanerozoic, the long-lived crustal root and high topography of the GSM are geologically unusual and undoubtedly important for the initiation of the East Antarctic ice sheet.
 We wish to thank IRIS-PASSCAL for providing both instrumentation and field support during the operation of the GAMSEIS array in Antarctica, as well as the pilots and staff of Kenn Borek Air and the New York Air National Guard for flight support. We thank Raytheon Polar Services and the staff at AGAP-S camp, South Pole Station, and McMurdo Station for logistical support. We also thank Anya Reading, Karin Sigloch, Thorsten Becker, and an anonymous reviewer for their critiques on this manuscript. This work was completed with supported from the United States National Science Foundation (grants ANT-0537597, ANT-0537371, ANT-0838934, and ANT-0838973) and the Japanese National Institute of Polar Research. Figures in this paper were created using GMT [Wessel and Smith, 1998].