A Java orbital plotting program developed and tested by et al. (2015) was used to calculate the x- and coordinates in pixels of the secondary star on the existing orbital solution in ImageJ. The observed positions were then compared to predicted positions provided by Brian Mason at the U.S. Naval Observatory. Results The results of the team’s measurements are shown in Table 1 including the position angle, separation, and location on the orbital diagram. Figures 4 and 5 show the new orbital plots of WDS 04545-0314 and WDS 04478+5318, respectively. WDS Identifier Position (°) Separation x-coordinate y-coordinate (″) WDS 04545-0314 188.459 0.1434 21.5 pixels left 144.7 pixels from center down WDS 0.637 0.6897 3.34 pixels left 300.0 pixels from center down Table 1: Observational results for WDS 04545-0314 and WDS 04478+5318. Figure 4: New orbital solution of WDS 04545-0314. The observed location is shown with an x near the top of the orbit. The nearest dot is the location predicted by the orbital solution. Figure 5: New orbital solution of WDS The observed location is shown with an x near the bottom of the orbit. The nearest dot is the location predicted by the orbital solution. Discussion For WDS both the predicted data and the new data confirm that the star is maintaining the previously established orbital solution. Referring back to Figure 1, the 2011 observation depicted a possible upward trend skewing away from the calculated orbit. However, our data do not support this apparent change in direction and the star appears to remain on the previously calculated orbit. After plotting both observed and predicted data for WDS 04478+5318, the team concluded that the apparent trend noted in previous speckle observations continued. The star appears to be moving in the downward direction, hinting at a longer period than previously determined. A source of error in the analysis arises from the fact that the measurements obtained through the Java program were rounded to the nearest hundredths value. When calculating the coordinates for both stars, the final results were rounded to whole numbers to allow proper plotting on the orbital solution since fractional pixels could not be used.
A Java orbital plotting program developed and tested by et al. (2015) was used to calculate the x- and coordinates in pixels of the secondary star on the existing orbital solution in ImageJ. The observed positions were then compared to predicted positions provided by Brian Mason at the U.S. Naval Observatory. Results The results of the team’s measurements are shown in Table 1 including the position angle, separation, and location on the orbital diagram. Figures 4 and 5 show the new orbital plots of WDS 04545-0314 and WDS 04478+5318, respectively. WDS Identifier Position (°) Separation (″) x-coordinate y-coordinate WDS 04545-0314 188.459 0.1434 21.5 pixels left from center 144.7 pixels down WDS 0.637 0.6897 3.34 pixels left from center 300.0 pixels down Table 1: Observational results for WDS 04545-0314 and WDS 04478+5318. Figure 4: New orbital solution of WDS 04545-0314. The observed location is shown with an x near the top of the orbit. The nearest dot is the location predicted by the orbital solution. Figure 5: New orbital solution of WDS The observed location is shown with an x near the bottom of the orbit. The nearest dot is the location predicted by the orbital solution. Discussion For WDS both the predicted data and the new data confirm that the star is maintaining the previously established orbital solution. Referring back to Figure 1, the 2011 observation depicted a possible upward trend skewing away from the calculated orbit. However, our data do not support this apparent change in direction and the star appears to remain on the previously calculated orbit. After plotting both observed and predicted data for WDS 04478+5318, the team concluded that the apparent trend noted in previous speckle observations continued. The star appears to be moving in the downward direction, hinting at a longer period than previously determined. A source of error in the analysis arises from the fact that the measurements obtained through the Java program were rounded to the nearest hundredths value. When calculating the coordinates for both stars, the final results were rounded to whole numbers to allow proper plotting on the orbital solution since fractional pixels could not be used.
DSR%20JDSOv3-16%2001%2003F.docx