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

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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)

Core-collapse supernovae

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• 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

SN neutrino signal

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Neutrino pointing to source

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Summary of supernova neutrino detectorsG

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ensi

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Ext

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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)

Core bounce

Convection and SASI Early and late g-modes

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Case for joint -GW analysis

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• A time-coincident GW- 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- 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.)

Modes of investigation

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• 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

Potential time-line and steps forward

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• 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)