Doublestar analysis of lunar occultation of XZ14295 on May.2 2009

Observed by Hideyoshi Karasaki

and Masayuki Ishida

Analized by Kazuhisa Miyashita

Hideyoshi Karasaki (Tokyo) and Masayuki Ishida (Shiga) observed same star XZ14295 and they sent video file to the author of this article.
As a result of Limovie analysis, separation and position angle of double star have been obtained. These value almost agree the catalogue value.


Fig.1    Karasaki's observation.
Light curve of this dim star is scattered by air scintillation.

Catalogue details

Catalogue details
 XZ 14295
 RA =   9 26  8.5402   PM = 0.00078s
Dec =  12 58 20.717    PM = -0.0287"
 Mv = 9.93, Mb = 10.53, Mr = 9.62    Spectrum G0    Approx dia. .0001"

Star is the primary of the following pair
Name    Cmpt   Yr1  Yr2: PA1   PA2  :   Sep1   Sep2  :  Mag1  Mag2:     #1      #2  mean
HEI 353       1985 1995: 142.0 142.0:   0.500   0.500: 10.10 10.10: X 14295  ------
WDS Discoverer codes
HEI  Heintz, W.D.                        

Diffraction fitting and photometry


Fig.2A    Fitting Karasaki's observation to diffraction simulation.


Fig.2B    Fitting Ishida's observation to diffraction simulation.

Elements of separation to the radial direction of lunar are 0.556(Karasaki) and 0.539(Ishida) arcsec. These are larger than expected value 0.498(Karasaki) and 0.485(Ishida)

Result

Nerima
Object Phenomenon Timemagnitude
Component A  Disappearance 10h59m59.241s +/- 0.067sec 10.53
Component B Disappearance   11h00m00.656s +/- 0.067sec10.86
Time difference 1.415 sec

Moriyama
Object Phenomenon Timemagnitude
Component A  Disappearance 10h59m29.72s +/- 0.07sec 10.45
Component B Disappearance   10h59m31.20s +/- 0.07sec10.98
Time difference 1.487 sec
From two observation, the west star is slightly brighter than east star.

Astrometry


   Calclation of astrometry
Component's separation is slightly larger than the value of catalogue. Position angle is 5 degrees smaller than catalogue.