1. Targeted Supernova Search with Coherent Wave Burst M. Zanolin (ERAU), L. Corpuz (ERAU), and the cWB Team LSC Burst Face to Face – Krakow, Poland 2010

2. Why can we benefit from a new approach to Supernova searches? Kaufman et al. 2010 As we can see from this table, the uncertainty in the explosion time ranges from ±6 sec to ± 4 days. For the list of optically detected SN within ~20Mpc during S6, the uncertainty may be even longer. The light curves below can be used to back track from the first recorded signal to the probable time of the explosion

3. Optically Discovered SN Within 20Mpc During S6 These were taken from a complete list compiled by CBAT http://www.cfa.harvard.edu/iau/lists/Supernovae.html SN NameSN TypeHost GalaxyDistance 2010u?NGC 4214~2.7-3.5 2010kIIp12 02 46.67 +02 24 05? 2010giIIbIC 4660~16.4 2010brIb/c IIbNGC 4051~10.9 2009mkIIESO 293-34~18.3 2009mdIINGC 3389~15.9 2009lsIINGC 3423~10.9 2009krIInNGC 1832~14.2 2009jsIINGC 0918~17 2009ipIINGC 7259~20 2009ibIIpNGC 1559~12.6 2009hqIIpNGC 4152~13.1

4. Search Configuration The standard configuration of cWB will be modified by introducing a sky mask, during production, to both the foreground and the background runs. The smallest sky mask we can implement is 0.5°x0.5° (one pixel). We are also exploring larger sky masks to keep into account the angular resolution. -The frequency band we will use will be from 100-2000Hz. -The characteristic GW frequency evolves from ~100 Hz just after bounce to ~300-400 Hz, with higher frequencies corresponding to higher mass progenitors… - http://stellarcollapse.org/gwcatalog/murphyetal2009http://stellarcollapse.org/gwcatalog/murphyetal2009 [PNS Core Pulsation] C. Ott - http://tapir.pbworks.com/f/Ott_CCSN_GW_predictions.pdfhttp://tapir.pbworks.com/f/Ott_CCSN_GW_predictions.pdf

5. Search Configuration Continued We will use larger windows, on the order of weeks, to include the error in extrapolating the exact time of the first EM SN emission https://svn.ligo.caltech.edu/svn/snsearch/papers/surf_report2010/ PNS Pulsation models suggest we search within ±1day of the first EM signature – Luc Dessart  http://tapir.pbworks.com/f/Dessart.pdf http://tapir.pbworks.com/f/Dessart.pdf In collaboration with the CalTech effort, we will perform simulation studies with the following waveforms: 1.Analytic Bar Modes 2.Convection/SASI 3.PNS g-modes 4.More? Data quality will be handled the same way as the all-sky cWB search on S6 We are working on procedures to combine double and triple coincidence data both for detection and upper limit purposes.

6. Expectations and Time Scales We expect to improve the sensitivity of the all-sky all-time search by a factor of 2 S. Klimenko http://tapir.pbworks.com/f/caltechSN.pdf http://tapir.pbworks.com/f/caltechSN.pdf We might not be able to conclusively determine the supernova mechanism from the waveform. See C. Ott’s discussion at: http://stellarcollapse.org/talks/Ott_APS_April_2008.pdf http://stellarcollapse.org/talks/Ott_APS_April_2008.pdf We aim to do the analysis and produce a paper in about a year