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Targeted Supernova Search with Coherent Wave Burst

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. Why can we benefit from a new approach to Supernova searches?.

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Targeted Supernova Search with Coherent Wave Burst

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  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? The light curves below can be used to back track from the first recorded signal to the probable time of the explosion 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.

  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

  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/murphyetal2009 [PNS Core Pulsation] C. Ott - http://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 • In collaboration with the CalTech effort, we will perform simulation studies with the following waveforms: • Analytic Bar Modes • Convection/SASI • PNS g-modes • More? • Data quality will be handled the same way as the all-sky cWB search on S6 • We are working on procedures to combinedouble and triple coincidence databoth 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. Klimenkohttp://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 • Weaimto do the analysis and produce a paper in about a year

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