ASTEROIDAL OCCULTATION - REPORT FORM +------------------------------+ +------------------------------+ | EAON | | IOTA/ES | | | | INTERNATIONAL OCCULTATION | | EUROPEAN ASTEROIDAL | | TIMING ASSOCIATION | | OCCULTATION NETWORK | | EUROPEAN SECTION | +------------------------------+ +------------------------------+ 1 DATE (YYYY/MM/DD): 2022/05/12 STAR: HIP 93319 ASTEROID: 2010 BV71 N°: 343317 2 OBSERVERS: Name: Leszek Benedyktowicz PTMA SOPiZ E-mail: lechben@go2.pl Address: Krakow, Poland 3 OBSERVING STATION: Nearest city: Balice Station: mobile station Longitude (DD MM SS.s): E 019 47 05.39 (WGS84) Latitude (DD MM SS.s): N 50 04 07.89 (WGS84) Altitude (m): 238 m (WGS84) Single|Multiple station: Single +----------------------------+ 4 TIMING OF EVENTS: | | | EVENT REPORTED: POSITIVE | | | +----------------------------+ Event code S: observation Start I: Interruption start D: Disappearance J: Interruption end R: Reappearance B: Blink F: Flash E: observation End O: Other (specify) Comments Event Time (UT) P.E. Acc. Code HH:MM:SS.ss S.ss S.ss S - 01:21:37.50 D - 01:22:08.41 +/- 0.01 sec R - 01:22:08.86 +/- 0.01 sec E - 01:22:29.00 Duration : 0.45 +/- 0.01 sec Mid-event : 01:22:08.64 +/- 0.01 sec 5 TELESCOPE: Type: Schmidt-Cassegrain Aperture: 203 mm Focal length: 1000 mm (reducer 0.5x) Mount: Azimuth Motor drive: Yes Filter: 6 TIMING & RECORDING: Time source: SNTP , NetTime 3.20 Alpha3 Sensor: ZWO ASI 120MM Recording: 30 ms integration , (Exposure= 0,03 s) Recording device: laptop ASUS, SharpCap 3.2 (Windows10) Time insertion: time laptop corrected flashing LED GPS-inserter 7 OBSERVING CONDITIONS: Atmospheric transparency: good Wind: NO Temperature: 10 °C Star image stability: good Minor planet visible: NO 8 ADDITIONAL COMMENTS: gradual effect ----------------------------------------- Eric Frappa's comments: The reason of the gradual transitions for this event is Fresnel diffraction. The main point in this case is that the occultation times have to be extracted at 75% drop of the target star (and not 50% as usual). To do this, I used the corresponding function in PyOTE allowing to take diffraction into account. After correcting the occultation times by -1/2 exposure time (Tangra exports mid-exposure times in the .csv file where PyOTE expects to receive start-exposure times) I get the following result: D - 01:22:08.41 +/- 0.01 sec R - 01:22:08.86 +/- 0.01 sec Duration: 0.45 +/- 0.01 sec (PyOTE times below are uncorrected) =============== Summary report for Excel file ===================== This light curve has not been block integrated. The following lightcurve parameters were utilized: ==== use diff: is checked ==== exp: 0.030006 ==== dist(AU): 2.1480 ==== speed(km/sec): 4.1085 ==== Star diam(mas): 0.1000 ==== D limb angle: 90.0 ==== R limb angle: 90.0 This 'drop' has a 0.0000 probability of being an artifact of noise. magDrop: 1.827 +/- 0.269 (0.95 ci) snr: 5.74 D time: [01:22:08.4287] D: 0.6800 containment intervals: {+/- 0.0045} seconds D: 0.9500 containment intervals: {+/- 0.0105} seconds D: 0.9973 containment intervals: {+/- 0.0208} seconds R time: [01:22:08.8770] R: 0.6800 containment intervals: {+/- 0.0045} seconds R: 0.9500 containment intervals: {+/- 0.0105} seconds R: 0.9973 containment intervals: {+/- 0.0208} seconds Duration (R - D): 0.4483 seconds Duration: 0.6800 containment intervals: {+/- 0.0066} seconds Duration: 0.9500 containment intervals: {+/- 0.0145} seconds Duration: 0.9973 containment intervals: {+/- 0.0264} seconds =========== end Summary report for Excel file =====================