|
25332 1999 KK6 (2012)
|
|
MPC Designation: |
1999 KK6 |
| Lightcurves |
Period (h): |
4.8277 ± 0.0003 |
|
Amplitude (mag): |
0.12 ± 0.01 |
|
Equipment: |
Filter: C
MagBand: V
Telescope: 0.35m f/9.1 SCT
Camera: FLI 1001E
Exposure: 240 |
|
Obs. Details |
Date E Mag Phase PABL PABB
2012-07-18 07:00 16.26 26.0 311.0 35.8
2012-07-20 07:00 16.24 25.8 311.3 35.9
2012-07-21 07:00 16.24 25.8 311.4 36.0
2012-07-23 07:00 16.22 25.6 311.7 36.1
2012-07-24 07:00 16.21 25.5 311.8 36.1
2012-07-26 07:00 16.20 25.4 312.1 36.2
2012-08-13 07:00 16.06 25.3 314.3 36.2
2012-08-17 07:00 16.07 25.5 314.8 35.9
2012-08-19 07:00 16.08 25.6 315.1 35.8
2012-08-20 07:00 16.08 25.7 315.2 35.7
2012-08-21 07:00 16.09 25.8 315.3 35.6
2012-08-22 07:00 16.09 25.9 315.5 35.5
2012-08-25 07:00 16.11 26.2 315.9 35.2
|
|
Data Points: |
228 |
|
|
|
|
Discovered: |
1999-05-17 Socorro LINEAR |
|
Family/Group: |
Hungaria |
|
Taxonomic Class: |
ES (Assumed) |
|
Published: |
MPB Pending |
|
|
|
|
NOTES: |
Unless otherwise stated, the "Reduced Magnitudes" in the plots are
Cousins R, based on 2MASS to BVRI conversions (Warner, MPB 34, 113-119)Followup to 2007 observations, when a period of 2.453/4.906 h was reported. There are distinct signs of a second period of 16.17 h. Attempts to fit the "primary" curve to the period of 4.906 h did not work. Simply put, the two results cannot both be right, even if they are fairly close. The 2007 data showed no signs of a secondary period and so that result may be a little more reliable because it was not "contaminated" by the secondary period. |
|
Contents © 2012 Brian D. Warner / Palmer Divide Observatory |
