1. PI OF THE SKY AND GRAVITATIONAL WAVES SEARCHES Adam Zadrożny

2. Core Information  Gravitational waves are still undetected  Some of detectable gravitational wave sources have E-M counter part  If an event in gravitational wave detector has an E- M counterpart, than it might be a good clue sugesting that it might be gravitational wave event

3. Agenda  Gravitational waves and where do they come from  Looc-Up project  Optical Transient Ext-Trig Search  Future  Summary

4. Gravitational Waves and where do they come from …

5. Gravitational Waves

6. Binary Coalescence and Supernova Explosions  NS-NS / NS-BH binaries  Supernovae

7. Detection of gravitational waves

8. Looc-Up Project

9. Locating and Observing Optical Counterparts to Unmodeled Pulses  Search for an optical counterpart to a gravitational waves event  to confirm an event  to gather more information

10. Looc-Up Project Science Runs  Winter Science Run 2009-2010  TAROT, QUEST, Swift  Autumn Science Run 2010  TAROT, QUEST, Switf, Skymapper, Pi of the Sky, ROTSE, PTF, ZADKO, Liverpool, LOFAR

11. LUMIN  A system for locating a position of an event on the sky (accuracy of positioning ~5 o )  Figuring out scopes for observations  Helping human to make a decisions about observations  LUMIN sends up to one alert per day

12. LUMIN

13. Telescopes Involved in Looc-Up Project  Quest (Chile, FOV 4.6 o x 4.1 o )  Tarot  North (France, FOV 1.86 o x 1.86 o )  South (Chile, FOV 1.86 o x 1.86 o )  Pi of the Sky (Poland, FOV 20 o x 20 o )  Zadko (Australia, FOV 0.23 o x 0.23 o )  … and other

14. Telescopes Involved in Looc-Up Project

15. Models of possible sources  Long GRB  Long GRB off-axis  Short GRB  Short GRB off-axis  Supernovae  Kilonovae  Other … Pi of the Sky limitting magnitude

16. Sky maps and tilling

17. Overview of the System  Camera:  FOV: 20 deg x 20 deg  Exposition time: 10 s  Limiting briththess: 12 mag  CCD: 2 K x 2 K  Observation site:  Koczargi Stare near Warsaw, Poland

18. Pi of the Sky observations  Observation took place during Autumn Science Run  One alert observed – G23004  444 Images taken  More than 2000 deg2 observed on the first night  Limiting magnitude: 10.5 – 11 mag

19. G23004 – images taken NightImages 023 1- 296 381 449 878 27117 Sumary444

20. Pipeline  For analysis we used catalog based pipeline  As a seed for star catalog we used Guide Star Catalog with stars up to 11 mag  For each exposition we add all recognized stars to the databases with their brightness measurements  Normalization of brightness to V magnitudes from TYCHO catalog

21. Transient Search  Transient search:  Looking for new objects that fulfill quality constrains  Looking a objects that suddenly increases their brightness  All transients are going under human inspection  Objects that are suppected to be transients were cross-corelated with INTA images taken months after the science run

22. Transient Recognition Efficiency

23. Lesson Learned  With Pi of the Sky system it is possible to image huge part of the sky within less than an hour  On-line transient recognition might be essential in next run for effective transients onservation an recognition

24. Optical Transient Ext-Trig search

25. Optical Transients ExtTrig Search  The main aim of the project is to make externally triggered search connected with optical transients of unknown astronomical origin  Currently we have data only from Pi of the Sky telescope

26. The Data that We Have  S5  About 40 optical transients were observed from Las Campanas Observatory Chile  S6eVSR4  31 transients were observed from San Pedro di Atacama

27. Optical Transients  Most of those transients has a duration less than 10 s.  One transient that coincide with S5 has a duration 60 s.  All transients were registered on both cameras

28. Pi of the Sky - Scopes  4 cameras that might work in coincidence or not  Each camera  FOV: 20 [deg] x 20 [deg]  Limiting brightness: 12 mag  Exposition time: 10 s  2 cameras working in coincidence  Each camera  FOV: 20 [deg] x 20 [deg]  Limiting brightness: 12 mag  Exposition time: 10 s INTA (Spain)San Pedro de Atacama (Chile)

29. Possible Sources  Off-axis short GRBs Or orphaned after glows from such a grbs  Some unknown astronomical events  For example this event also do not fit to our knowledge http://iopscience.iop.org/0004-637X/690/2/1358  Rarely flashing satellites that are not included in databases

30. The Search  Software used:  X-pipeline  Bandwidth:  64 Hz – 2000 Hz  On-Source Window  Begin: -600 s  End: 496 s  Off-Source Window  10800 s

31. Waveforms Used  Inspiral – incljitter (90)  Chirplet – incljitter (0, 90)  White Noise Burst

32. Post-Processing  Due to unknown origin of the transients we do not know anything about polarisation  We need to do postprocessing twice  Focused on circulary polarised waves  No constrains on polarisation

33. Summary  To make externally triggered search X-pipeline is used  The source of the transients is unknown  Project is going to be finish this year

34. Future

35. Future system  FOV : 1,5 sr  Paralax : > 100 km  Limiting magnitude: 12 mag  Site: Spain  Operational time:

36. Summary

37.  Pi of the Sky took a part in two gravitational wave searches projects  Looc-Up  Optical Transient ExtTrig Search  Published results from both projects are expected in late 2012 or early 2013  Pi of the Sky is biggest FOV telescope that taking part in gravitational wave searches

38. Questions?