HAL, PRB, SMD : videorecording

BTG : no occ. > 0.5 s. HDG : videorecording, no occ. > 0.2 s. WSG : videorecording, no occ. > 0.15 s.

BUL : both disappearance and reappearance were gradual events, estimated duration 0.3 s and 0.15 s resp.;
JNK : disappearance seemed gradual

The two chords and the PRB’ negative observation lead to an elongated profile, with long axis running parallel to the asteroid motion. A significant part (at least a half) of the profile is lacking, as the (488) Kreusa mean diameter is about 150 km. The shadow path must have been shifted by at least half of its width, toward NE, relative to the prediction.

HCP and PAR were in the predicted track ; incertitude was large for this 26 km asteroid.

BLI, DNZ : videorecording;

BLI was in the predicted path and registered an event with duration in agreement with the expected one, so prediction must have been exact.

BAH, BDR, DGG, GKB, HAL, HDG, HCP, HRB, KND, OKE, PAR, RTH, SFH, SMD, WSG : videorecording ;

GAA: CCD drift scan; GKB : parallel visual observation with 13 inch Dobson; VIG : with P. De CAT, CCD imaging

HCP : with J. HUBER, D and R gradual; PAR : with Klaus NAGEL (NGK).

Thomas WINTERER observed a 2 s occultation from N 48 32 41.4 E 10 51 39.3 + 433 m, at nearly 22:46:37

Ronald STOYAN observed a 1.5 s occultation from N 49 37 31.7 E 11 01 06.7 +275 m, at nearly 22:46:30

Chords can be fitted with an elliptic profile, 76 × 63 km. This has to be compared to the mean circular value of 90 km, used for calculation. Fit can be improved, taking into account the binarity of the star (r = 4.7 ± 0.4", q = 113 ± 8°).

Observations (especially HCP positive and HRB and RTT negatives ones) show the path has been shifted by 0.2 times its width, toward SW.

DNZ, FAR, MHH, PAR : videorecording; PCI : CCD drift scan

BTG observation, performed in strong crepuscular light must be related to (519) Sylvania, since the appulse was predicted at 19:21:52 s for his location. BTG was just at the northern border of the predicted shadow path, so the real one must have been shifted slightly toward North (the max predicted duration is 1.6 s for a diameter of 48 km).

FST, RHE, RTH, SMD : videorecording; GJD : CCD drift-scan. FST : no occ. > 0.1 s; JNK : no occ. > 0.5 s.

RHE and RTH were effectively close to the predicted centreline. Note that max predicted duration was 1.2 s : the asteroid is elongated and/or larger than supposed (20 km)

FST : videorecording, no occ. > 0.1 s. Incertitude was very large for this small asteroid (22 km)

JDO : CCD drift-scan

Charon is the first discovered satellite of the transneptunian planet (134340) PLUTO

JLX : videorecording; path was expected close to Pic-du-Midi, but incertitude was large for this small asteroid (22 km)

JLX : videorecording; (S/2005 P1) Hydra is the outer satellite of the transneptunian planet (134340) PLUTO. Target star is the component B of a binary. Path was expected across north Morocco or the south tip of Spain.

DGG, ENK, GHD, HRB, HZL, MNK, OKE, PAR, PRB, RHE, SMD, SVA, WCH : videorecording;

GAA, HRH, KUS : CCD drift-scan;

HRH : with T. Henych; OTA : has started 3 minutes too late, was in double station with BAL; PLK : in double station with VCA

PLK : both D and R gradual, flat bottom about 1 magnitude below maximum; VCA : D instantaneous (star invisible), then gradual brightening lasting 5 s ; SMD : the star brightness dropped by approx. 2 mag only.

Taking into account the star binarity (see below), chords can be fitted with an elliptic profile, 95 × 71 km. This has to be compared to the mean circular value of 92 km, used for calculation.

Target star is known as a binary and reduction leads to the parameters r = 42", q = 77°. HRB (the first positive observation for this observer!) registered the occultation of successively the two components; SMD, BTA, PLK and VCA, observed the occultation of the same one component. MNK : a grazing occultation remains possible, but would imply that BAL missed a short occultation; the event may be spurious because of the bad signal to noise ratio of the videorecording.

Centreline was predicted over Berlin (ENK’ location). Nevertheless, according to the drawn profile, SMD observed a nearly central event : path has been shifted by one of its width, toward SW.

PAR : videorecording, no occultation > 1s despite an observing station within predicted path.

FOC : videorecording

RVA : videorecording

DGG, FAP, PAR : videorecording; IVY : double observation, visual + CCD drift scan; LDT : star track; KHL : possible short occultation missed due to thin clouds; PAR : no occ. > 0.1 s

Chords can be fitted by an elliptic profile (113 ± 3) km × (72 ± 5) km, to be compared with the 80 km mean diameter used for calculations.

From its 2006 lightcurve, R. BEHREND (Observatory of Geneva University) suggested that (676) Melitta could be a binary.
A. LOSYUK and V. MECHINSKY suggested that two of the chords (IVY and GKB ones) can be interpreted by the presence of a 20 km satellite.

BAL, DGG and OTA : videorecording; BAL and OTA in double station

ZNA : star track, was effectively close to the predicted centreline. The event occurred 20 s after the predicted appulse time (00:36:15) but incertitude was large for this small asteroid (23 km). Note that max predicted duration was 2.7 s.

DEN: videorecording ; RTH videorecording, interruption due to clouds.

Incertitude was great for this very small asteroid (16 km).