Figure F3. A. Average inclination values for three inclination group models from Detroit Seamount; error bars = 95% confidence intervals. The predicted inclination at 81 Ma based on prior Pacific apparent polar wander path (APWP) poles (Gordon, 1983) is also shown. B. Paleolatitude values with 95% confidence intervals for the inclination groups. The present-day latitude of the Hawaiian hotspot (solid line) is also shown. C. Estimated angular dispersion (S) of the inclination groups (solid line) vs. the predicted values for 45-80 Ma (dark field) and 80-110 Ma (light field) from McFadden et al. (1991). VGP = virtual geomagnetic pole. D. Orthographic projection of the colatitude (primary) for Detroit Seamount (star). The colatitude is distinct at the 99% confidence level (shaded) from previous 81-82 Ma poles (ellipses). Poles are derived from the following: 81 Ma (Gordon, 1983), 82 Ma (Sager and Pringle, 1988), and 33n (79.1-73.6 Ma) (Vasas et al., 1994). The sense of offset between the natural remanent magnetization data and the demagnetized (primary) data is the same as that between the new paleolatitude result and results based on prior Pacific pole positions. This is the expected effect if these previous pole positions are contaminated by secondary magnetizations. This figure is after Tarduno and Cottrell (1997).

Figure F3. A. Average inclination values for three inclination group models from Detroit Seamount; error bars = 95% confidence intervals. The predicted inclination at 81 Ma based on prior Pacific apparent polar wander path (APWP) poles (Gordon, 1983) is also shown. B. Paleolatitude values with 95% confidence intervals for the inclination groups. The present-day latitude of the Hawaiian hotspot (solid line) is also shown. C. Estimated angular dispersion (S) of the inclination groups (solid line) vs. the predicted values for 45-80 Ma (dark field) and 80-110 Ma (light field) from McFadden et al. (1991). VGP = virtual geomagnetic pole. D. Orthographic projection of the colatitude (primary) for Detroit Seamount (star). The colatitude is distinct at the 99% confidence level (shaded) from previous 81-82 Ma poles (ellipses). Poles are derived from the following: 81 Ma (Gordon, 1983), 82 Ma (Sager and Pringle, 1988), and 33n (79.1-73.6 Ma) (Vasas et al., 1994). The sense of offset between the natural remanent magnetization data and the demagnetized (primary) data is the same as that between the new paleolatitude result and results based on prior Pacific pole positions. This is the expected effect if these previous pole positions are contaminated by secondary magnetizations. This figure is after Tarduno and Cottrell (1997).