Core-collapse SN neutrinos and GW bursts

1.  Core-collapse SN neutrinos and GW bursts • We are developing a proposal to the LSC-Virgo to search for associated bursts of low-energy neutrinos and GW bursts • Goal: to present proposal for March L-V meeting Neutrino community: W Fulgione (LNGS, LVD), K Scholberg (Duke U, Super-K) LIGO-Virgo community: L Cadonati (UMass), E Coccia (LNGS, Rome U), R Frey (U Oregon), E Katsavounidis (MIT), I Leonor (U Oregon), G Pagliaroli (LNGS) Theory/Phenom community: F Vissani (LNGS), G Pagliaroli (LNGS) R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

2.  Core-collapse supernovae • Classic multi-messenger astronomical events: • Gravitational Waves (GWs) • Low energy neutrinos • Electromagnetic • Optical (EM) signature: • may be obscured • unable to determine time of bounce to better than ~ day • Neutrinos and GWs directly probe the physics of core collapse • Signatures separated by few seconds • A tight coincidence window can be used to establish a correlation • Sensitivity range of current GW and neutrino detectors very similar • Super-K: ~104 detected neutrinos for galactic SN • ~1 for M31 R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

3.  SN neutrino signal R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

4.  Neutrino pointing to source R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

5. Summary of supernova neutrino detectors Galactic sensitivity Extragalactic R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

6.  GW emission from core-collapse • Several mechanisms may give rise to gravitational wave (GW) emission from core-collapse supernovae (see review by Ott astro-ph/0809.0695) • Rotating collapse and bounce. • Post-bounce convection and Stationary Accretion Shock Instability (SASI) • Anisotropic neutrino emission • PNS core oscillations and dynamical rotational instabilities • Significant uncertainties exist in energy going into GWs and open questions are being addressed by the numerical relativity community • Most optimistic simulation from PNS g-mode pulsations (acoustic mechanism) by Burrows et al yielding up to 8x10-5 Msolarc2 for a 25Msolar progenitor at 600-900Hz (-> reaching MC’s) Early and late g-modes Convection and SASI Core bounce R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

7.  Case for joint -GW analysis • A time-coincident GW-n search should provide a factor  2 improvement in the GW sensitivity relative to an all-sky search. • Improve chance of detection via lowering individual detector thresholds and increasing the time coverage of a global GW-n detector network. • Ability to explore “distant” SN searches (M31) unable to be seen reliably by neutrino detectors alone. (Assumes there is a detectable GW signal.) R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

8.  Modes of investigation • Galactic SN with loud  burst → SNEWS Gold alert • Already public and available to LIGO in real time • Analyze GW as for GRB bursts, for example • Intermediate  burst • As above but need access to neutrino information • Few- bursts • Joint analysis as described here • ~ Super-K “distant SN search” [astro-ph/0706.2283; ApJ] • Correlate with low-threshold GW bursts R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z

9.  Potential time-line and steps forward • Today: invitation to collaboration members to join • Help define proposal and analysis details • February 2009: circulate documents • Guiding principles: minimize FTE and computational resources, use existing data products from all parties (neutrino/GWs) • March 2009: present proposal at LSC-Virgo collab meeting and seek approval to proceed with (multi-party) MOU • April 2009: proof-of-principle analysis on S5/VSR1 data • May-June 2009: extension on S6/VSR2 early data and report to collaborations at June collab meeting • July++ 2009: analysis in auto-pilot (not necessarily online) R Frey U Maryland LSC-V 18 Dec 2008 G080654-00-Z