Activity Report: Slovakia

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Presentation transcript:

Activity Report: Slovakia Institute and researchers Researchers on JEM EUSO - K. Kudela - P. Bobik - S. Pastircak - J. Urbar (cooperating) Tatiana measurements analysis Huge background trigger simulations on KE PC cluster

Tatiana measurements archive http://space.saske.sk/JEM/tatiana.html To visualize Tatiana UV measurements and create reference frame for future use. Ak http://space.saske.sk - in internal JEM-EUSO part http://space.saske.sk/JEM. User: jemeuso Password: same as for RIKEN JEM- EUSO site ~7000 measurements of Universitetsky Tatiana satellite at ~25 000 figures (two types of figures) Selection parameters - Sun zenith angle - Moon zenith angle - length of one continuous measurement

Tatiana measurements archive ID:10, Sza > 108o, Date: 5 2 8 8 50 44 [y/m/d/h/min/sec]

Tatiana measurements archive ID:10, Sza > 135o, Mza > 90o, Date: 5 2 8 8 50 44

Tatiana measurements archive ID:108, Sza > 108o, Date: 5 3 8 15 31 26

Tatiana measurements archive ID:108, Sza > 135o, Mza > 90o, Date: 5 3 8 15 31 26

Tatiana measurements archive ID:142, Sza > 135o, Mza > 90o, Date: 5 3 14 17 2 34

Stability coefficient Stability of UV background clearly depend on Sun relative position to place of measurements i.e. on Sun zenith angle. It make sense then evaluate BG stability as function of Sun zenith angle threshold. To avoid moon light influence we select measurements where moon zenith angle Mza is higher than 90o. - four different stability coefficients was tested - as upper estimation coefficient based on ratio between maximum and minimum UV intensity values of measured periods - stability coefficient based on standard deviation of UV signal during measured periods - stability coefficient based on on curve length of UV signal graph during measured periods - stability coefficient based on average absolute deviation of measurements

Stability coefficient Different stability coefficient evaluate how UV light change during measurements on Earth orbit. From all coefficients we can see that stability of signal depend on Sun zenith angle, and change relatively fast till Sza reach 132o. This lead us to change (redefinition) of night definition for Tatiana orbit. Now we redefine night for orbit ~940 km as time when satellite local Sza>132o. Stability coefficient based on average absolute deviation show that stability of signal on the night side, when moon is under horizon is in order of 10ths percents from average value of UV intensity during measurement in previous/surrounding moments/orbit (flashes and TLE events are exception from this conclusion). Let us note that this results are evaluated from signal with flashes (TLE) events. Flashes was not cleaned from signal. If measurements with flashes will be cleaned out, stability increase.

JEM-EUSO duty cycle 2005 - 2007 from real ISS trajectory

JEM-EUSO duty cycle 2005 - 2007 from real ISS trajectory

Cloudiness influence on UV signal atmosph. propagation Study of influence of actual cloud situation (cloud fraction and pool of 202 parameters) on the UV light Universitetsky Tatiana-1 orbital nightside measurements using International Satel. Cloud Climatology Project (ISCCP) datahttp://isccp.giss.nasa.gov Gridded Cloud Product - Revised algorithm (D1) Resolution: 280km equal- area grid, 3hour, global, Spatial averages of DX quantities and statistical summaries, including properties of cloud types. Satellites are merged into a global grid. Atmosphere and surface properties from TOVS are appended.

Visualization of generated 3hour-global 280km grid cloud map (ISCCP) with UV measurements (Universitetsky Tatiana)