55565.20130305 Occultation March 05, 2013

(last updated 2013 01 10)



Across the globe pictured above, the three solid lines correspond to the northern limit, centerline, and southern limit of 55565's shadow. The northern and southern limits correspond to a radius of 369 km. The upper and lower dashed lines indicate 3-sigma errors. The shaded area represents where the sun is more than 12 degrees below the horizon.
Table 1: Prediction Details
55565 Geocentric Mid-time (yyyy month dd hh:mm:ss)

2013 March 05 09:05:49± 00:01:021 UT

55565 Minimum Geocentric Separation 0.2763± 0.0461 arcsec
Position Angle (55565 relative to the star; measured north through east) +19.96 degrees
Geocentric Velocity 24.15 km/sec
Occultation Star UCAC2 magnitude 16.122

1One standard deviation of random error.
2The UCAC bandpass (579-642nm) is between V and R.

Table 2: Reference Star Position
Reference star position:
(UCAC2, at epoch of event)
RA (h:m:s; J2000) Dec (d:m:s; J2000) Notes
55565.20130305 Catalog 09 29 44.2808± 0.1767 +02 17 40.117± 0.153
55565.20130305 Measured3 09 29 44.2628± 0.0157 +02 17 40.166± 0.015
From 5 Lowell 42-inch frames
Table 3: Projected KBO Offsets from Reference Ephemeris at the Time of the Event
Body RA (arcsec) Dec (arcsec)  

–0.0557± 0.0425

+0.144± 0.044 See Notes 5 and 6

3Measured position corresponds to RA offset of –0.2693 and Dec. offset of +0.049.

4All "offsets" are defined in the ("corrected" – "reference") or ("observed" – "calculated") sense. The offsets should be added to reference positions to get the measured positions, which we use to calculate the prediction.

4Data analyzed using UCAC2 reference network. A weighted average of the data from the two telescopes was used to calculate the RA and DEC. The errors given are 1 standard deviation.

5The reference positions for Haumea are those given by JPL Horizon's ephemeris (55565 source file: JPL10; Earth center source file: DE405).

6Data from the USNO 61-inch, SMARTS 0.9m, and Lowell 42-inch telescopes over the span of 3 years were reduced with respect to stars in the UCAC2 catalog. A model was developed to fit the residuals obtained from our measured positions compared to that of the object's JPL ephemeris. All residuals obtained from the different telescopes were consistent with the model. The model includes the first-order effects of errors in the orbital elements of 55565: (i) constant offsets in RA and Dec, (ii) linear (in time) offsets in RA and Dec, and (iii) sinusoidal terms with the Earth's orbital period. The model was propagated to obtain the predicted position and error of the KBO at the time of the occultation. The errors listed for the KBO are 1 standard deviation.


Table 4: Site Information

East Longitude

Site Altitude6






Lowell Obs
-111 39 54
35 12 12
4489 S.
Mauna Kea (IRTF)
-155 28 29
19 49 46
7187 S.
-71 29 06
42 36 36
3432 S.
center of Earth
9050 S.

6Altitude of each observatory is measured in kilometers above sea level.

7"Distance" refers to the closest approach distance of the "Site" to the center of 55565's shadow in the shadow plane. The errors on all closest approach distances are ±1528 km (one standard deviation). "S." means the site is south of the center of 55565's shadow. "N." means the site is north of the center of 55565's shadow.

Table 5: 55565.20130305 Occultation Predictions for Individual Sites

KBO Immersion (UT)9
UT Mid-Time
KBO Altitude
Solar Altitude9

KBO Emersion (UT)9

Lowell Obs
Mauna Kea (IRTF)

9The errors on all times are ±1:02 (1 minute and 2 seconds; one standard deviation). The solar altitude is given for locations where it is relevant (solar altitude greater than -18°). No entry in the immersion and emersion columns indicates that the occultation is not predicted to be visible at that site.


Last updated by Carlos Zuluaga (czuluaga@mit.edu) 2013-01-10 12:01

Please direct all inquiries to PAL (planetary-astronomy@mit.edu)