1.  of the Sky Innovative approach to GRB optical counterparts detection Study of astrophysical phenomena with time scale from seconds to months http://grb.fuw.edu.pl K. Malek 2), L.W. Piotrowski 3), M. Biskup 3), M. Cwiok 3), W. Dominik 3), G.Kasprowicz 4), M. Kwiatkowski 4), A. Majczyna 1), L. Mankiewicz 2), M. Molak 4), K. Nawrocki 1), K. Pozniak 4), R. Romaniuk 4), D. Rybka 1), P. Sitek 1), M. Sokolowski 1), J. Uzycki 4), G. Wrochna 1), M. Zaremba??, A.F. Zarnecki 3) 1) Soltan Institute for Nuclear Studies; 2) Center for Theoretical Physics, Polish Academy of Sciences; 3) Institute of Experimantal Physics, Warsaw University; 4) Warsaw University of Technology Special thanks to prof. B. Paczynski (Princeton University) and G. Pojmanski (Warsaw University) and all staff of the Las Campanas Observatory. PROTOTYPE 2 CCD, 2000x2000 pixels each, lenses: Zeiss, f=85mm, f/d=1.2, FoV: 21 o ×21 o, angular resolution: 36'' limiting mag.: 11-13m (1 frame 10s), 13-14m (20 frames) We present an innovative approach to the GRB optical counterparts observations, which ought to overcome one of the main obstacles towards deeper understanding of GRB phenomenon: no observations in the very early stage of the burst. The “  of the Sky” introduces the idea of constant, high time resolution, large sky area monitoring. Special data stream reduction algorithms were created, to allow optical transient detections not depending on GRB satellites. NEW APPROACH constant large sky area monitoring none or even negative time delay to satellite GRB triggers self-triggering capabilities high time resolution FULL SYSTEM CAPABILITIES first data: fall 2007 optical counterparts observations after, during and even prior to GRB flare star detection variable and novae star observations different short time-scale astrophysical phenomena detection possibilities FULL SYSTEM (under construction) 2 matrices of 16 CCD cameras, 2000x2000 pixels, lenses: Canon EF f=85mm, f/d=1.2, matrices outlied by ~50 km, working in coincidence FoV: 16 × 20 o ×20 o = 2 steradians: more than Swift BAT FoV equal to GLAST FoV limiting mag.: 13.5 m (1 frame 10s), 15 m (coadded frames) Modes of observation The system works autonomously, according to schedule, which could be changed via Internet: follows SWIFT or Integral FoV independently detects optical flashes in real time (self-triggering) performs dedicated observations of interesting objects (eg. blasars, quasars, novae) in spare-time twice a night makes a full sky survey (2x40 min) instantaneously follows satellite alerts distributed by GCN On-line data stream reduction 3000 frames/night, 1 frame = 8 MB -> 25 GB/night (full system: 32x25 GB = 800 GB/night) algorithms inspired by particle physics – multilevel trigger Level 1 – very fast and simple single pixel analysis Level 2 – sophisticated object analysis Search for optical flashes: ~132 flashes < 10s detected (may be flashing satellites) 8 flashes >10s detected (including flare of CN Leo) 0 Search for GRB optical counterparts: 165 GCN alerts received (>7.2004): - 5 apparatus off - 6 clouds - 25 below horizon - 81 daytime - 24 outside FoV - 2 inside FoV limits 9m – 14.3m published: GRB 0040916, 041217, 050123, 050326, 050607, 060607, 060719, 061202, limits during the burst: GRB 040825A, GRB 050412 Outburst of CN Leo flare star, automatically detected by “  of the sky” on-line flash detection algorithm. Star was not visible in our range before its outburst, thus it well simulates expected behavior of GRB optical counterpart. IS  RANGE ENOUGH? Our knowledge about early brightness is weak, for most optical counterparts were observed long after GRB. How to estimate how many of them will be in “  of the Sky” range? Results of extrapolation of 45 best early lightcurves (<5000s) to 30 s after GRB. The average brightness, not filter corrected, is. 15.7 m. (data from GRBlog). Maximal GRB optical counterpart brightness in the first 100 s after GRB, for 39 bursts. The average brightness is 15.9 m (data from GRBlog). Both the extrapolation and the real maximal magnitudo show, that we should be able to see close to one half of the GRB optical counterparts (in night, on our hemisphere). That is very optimistic! This figure show events reduction ratio for several nights. Level 1 consists of very fast and simple cuts mainly for eliminating constant stars and apparatus effects. Coincidence performed between Level 1 and Level 2 mainly eliminates cosmic radiation effects. Level 2 is designed to eliminate real objects, like satellites, planes, meteors and stars not reduced by Level 1, that are not in our field of interest. Prototype working at Las Campanas, Chile, since 07.2004 FIRST RESULTS (from prototype) Full system (rendering)