General Relativistic Gravity in Core Collapse SN: Meeting the Model Needs Lee Samuel Finn Center for Gravitational Wave Physics Meeting the model needs • Importance of GR for SN physics? • Most likely quantitative, not qualitative, except for questions of black hole formation (when, how, mass spectrum)? • Gravitational waves as a diagnostic of supernova physics • General relativistic collapse dynamics makes qualitative difference in wave character Outline

• Gravitational wave detection & detector status • Detector sensitivity • Gravitational waves as supernova physics diagnostic LIGO Status

• United States effort funded by the National Science Foundation • Two sites • Hanford, Washington & Livingston, Louisiana • Construction from 1994 – 2000 • Commissioning from 2000 – 2004 • Interleaved with science runs from Sep’02 • First science results gr-qc/0308050, 0308069, 0312056, 0312088 Detecting Gravitational Waves: Interferometry

t – Global Detector Network LIGO miniGRAIL GEO Auriga CEGO

TAMA/ LCGT ALLEGRO

Schenberg

Nautilus Virgo Explorer AIGO Astronomical Sources: NS/NS Binaries

Now: N ~1 MWEG • G,NS over 1 week

Target: N ~ 600 • G,NS MWEG over 1 year

Adv. LIGO: N ~ • G,NS 6x106 MWEG over 1 year Astronomical Sources: Rapidly Rotating NSs

range Pulsar

10-2-10-1 B1951+32, J1913+1011, B0531+21

10-3-10-2

-4 -3 B1821-24, B0021-72D, J1910-5959D, 10 -10 B1516+02A, J1748-2446C, J1910-5959B J1939+2134, B0021-72C, B0021-72F, B0021-72L, B0021-72G, B0021-72M, 10-5-10-4 B0021-72N, B1820-30A, J0711-6830, J1730-2304, J1721-2457, J1629-6902, J1910-5959E, J1910-5959C, J2322+2057

-6 -5 J1024-0719, J2124-3358, J0030+0451, 10 -10 J1744-1134

Preliminary S2 upper limits on ellipticity of Initial, advanced LIGO Limits on
for 1 yr 28 known pulsars observation of pulsar @ 10 Kpc Astronomical Sources: Stochastic Background

• Primordial or “confusion-limit” Now:
< 2x10-2 (preliminary S2 result) • GW Target:
< 10-6 in (40,150) Hz over 1 yr • GW Advanced LIGO:
< 10-9 in (10, 200) • GW Hz over 1 yr Detector Sensitivity

1 T

= lim dt h2(t) T →∞ 2T −T

∞   1 ˜ 2 = lim df hT (f) T →∞ 2T −∞  h(t) |t|

• LLO seismic noise exceeds dynamic range of isolation • Isolation retrofit using “advanced LIGO” technology • (Late) Fall ‘04: S4 “re- commission” • Spring ‘05: S5 • 6 months at ~ design sensitivity Detector Sensitivity

1 T

= lim dt h2(t) T →∞ 2T −T

∞   1 ˜ 2 = lim df hT (f) T →∞ 2T −∞  h(t) |t|

• Ott et al. model S15A1000
0.{1,4} • 15 M
, differential rotation with 1000 Km characteristic radius •
0.1: higher frequency, shorter duration; bounce is most energetic feature •
0.4: most energetic feature is post-bounce Detection issues

• Multiple detectors provide opportunity to identify signal through correlations • Blind deconvolution techniques look for common signal in multiple inputs; can recognize time-shift due to wave incident direction Ott et al. S15A1000
0.1 Time-frequency diagnostic Time-frequency diagnostic Conclusions

• General relativity ... • may be important for SN mechanism; • is important for using grav. waves as physics diagnostic • Don’t need waveform to connect observations to physical models • Look for robust, qualitative differences in signal character