The records of Cores 175-1077B-12H through 16H were correlated with the records of Cores 175-1077A-12H through 16H with the use of the time-series analysis program AnalySeries (Paillard, 1996). During the correlation, the distances between the data points within the cores from Hole 1077A were kept constant but the distances between the cores were allowed to vary. This operation resulted in a provisional depth scale (Fig. F1). The data of the cores from Hole 1077B were fit to the data obtained from cores from Hole 1077A, allowing downcore stretching and squeezing. The correlation was significantly improved by the use of the CORTEX scans. The Ca records provide extra tie points (Fig. F2A), and the Fe records occasionally proved to be more distinctive and comparable than the magnetic susceptibility records (Fig. F2B). The resulting correlation confirms the suspicion that there are more and larger gaps between the cores than originally recognized (Fig. F1; Table T1).

For the construction of the revised splice record, the tie points between Hole 1077A and Hole 1077B were left at the original positions if possible. Extra tie points had to be added near the transitions between Cores 175-1077A-12H, 13H, and 14H (Table T2). We applied only depth translations and abstained from magnification and reduction. Unfortunately, no junction could be detected between the records from Core 175-1077B-15H and Core 175-1077A-16H, which may indicate a (probably small) hiatus or gap between 150.60 and 150.82 meters revised composite depth (rmcd) (Fig. F3). This interval, however, may be represented by the core catcher sample of Core 175-1077B-15H. As a result of the additional adjustments, the revised composite depth record is 4.92 m longer than the original spliced record between 110 and 150 mbsf (Fig. F4). The revised offsets, rmcd scale, and new tie points are presented in Tables T1 and T2.