Status of LIGO Keita KAWABE, LIGO Hanford Observatory/Caltech for - PowerPoint PPT Presentation

LIGO Status of LIGO Keita KAWABE, LIGO Hanford Observatory/Caltech for the LIGO Scientific Collaboration LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO TOC ● Who we are – Introduction to LIGO and LSC ● Where we are at now – Status of Current Science Run (S5) – Detector Performance etc. ● Future LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Who We Are LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Who We Are ● Laser Interferometer Gravitational-Wave Observatory ● Funding: NSF ● Operation: Caltech-MIT ● 2 observatories, 3 detectors – Hanford (LHO), 4km & 2km, (30+ local staffs) – Livingston (LLO), 4km, (30+ local staffs) ● CIT/MIT staffs outside of site (more than 100) ● LIGO Scientific Collaboration (LSC), a body carrying out the scientific program of LIGO (about 570 as of now, all over the world) LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Hanford Observatory (LHO) LIGO H1 : 4 km arms H2 : 2 km arms Desert in north west, Washington 3000km, 10 ms LIGO Livingston Observatory (LLO) L1 : 4 km arms Swamp in gulf coast, Louisianna ● Adap dap ted ted from from “The “The Blu Blu e M e M arb rb le: L le: L and and Surfac urfac e, e, Ocean Col Col or or and and Sea I a I ce” at e” at visib isib lee lee ar ar th. th. nas nas a. a. gov ● NAS AS A A God od da da rd Sp d Sp ace Fl ce Fl igh igh t Center Ima Center Ima ge b e b y Reto Stö o Stö ckli ( ckli ( land nd sur sur face, ce, sh sh allo lo w w wa wa ter, ter, clou clou ds) s) . Enh Enh anc nc em em en en ts by ts by Rob Rob ert ert Simmon mmon (oc oc ean ean color color , co co mpos os itin tin g, 3D g 3D g lob lob es, es, anima anima tion tion ). Da . Da ta ta and nd technica technica l l sup up por or t: M t: M ODI DI S Lan S Lan d Grou ou p; p; MODIS MODIS Scie cie nce Da ce Da ta Su ta Su pp pp ort rt Team; m; MODIS At MODIS At mosp sp here G ere G ro ro up up ; MODIS Ocean MODIS Ocean Group up Ad Ad dition ition al d al d at at a: a: U U SGS E S E ROS Dat ROS Dat a C a C ent ent er ( ( to to po po grap ap hy) hy) ; USG USG S Ter S Ter restr restr ial Remote ial Remote LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting Sen Sen sin in g Flagsta Flagsta ff f Fiel Fiel d Ce Ce nter ( ter ( An An tar tar ct ct ica) a) ; Def Def ense Meteor ense Meteor olo olo gic ic al Sa al Sa tel tel lite P lite P ro ro gram ( am ( city city li li gh gh ts).

LIGO Detection concept ● Compare the travel time of photons in orthogonal directions using laser interferometer ● Power-recycled, ● Michelson IFO, ● Fabry-Perot arms – 4km (or 2km) LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Initial LIGO Core Optics ● Substrate: SiO2 – 25cm diam ö 10cm thick – Homogeneity < 5ö10 -7 – Internal mode Q factor > 2ö10 6 ● Polishing – Surface uniformity < 1nm rms – Radius of curvature matched < 3% ● Coating – Scatter < 50ppm – Absorption < 2ppm – Uniformity < 10 -3 LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

Core Optics Suspention LIGO and Vibration Isolation Vibration-isolated chambers using stack Core Optics Suspension LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Where We Are At Now LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Where We Are At Now ● 4 Science Runs (S1-S4) in the past ● S5, starting Nov/04/2005, is still ongoing – The last run with the current configuration – At design sensitivity (or better) for all 3 IFOs – Close to the end: 2007/Oct/01 00:00:00 UTC ● Will accumulate one year's worth of 3-IFO coincidence by then – Coincident run with GEO and VIRGO ● Sometimes 5-fold coincidence LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO LIGO History Now ow 1999 2000 2001 2002 2003 2004 2005 2006 2007 2 4 2 4 3 4 1 3 1 3 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 Ina na ug ug ur ur ati ti on on All ll IF IF O Firs rs t t Loc oc k 4K K st st rai ai n n noi oi se se at t 15 15 0 H H z z [Hz Hz -1/2 ] 10 -17 10 10 -18 10 -20 10 10 -21 10 -22 10 4k k Bes es t t NS- S- NS NS ra ra ng ng e i i n n Mpc pc 6.5 .5 7.7 .7 12 12 15. 5. 1 16. 6. 3 (1. 1. 4 M M su su n, , al al l-s -s ky ky av av er er age ge , , S/N /N =8 =8 ) S5 end S1 S2 S3 S4 S5 Science (3 IFOs) TAMA, GEO, GEO, GEO Joint TAMA, coincidence Allegro Allegro, GEO run Auriga TAMA VIRGO LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

A Little about LIGO Detector Noise Limit ● Shot noise (and radiation pressure noise) ● Thermal motion of mirror and suspension ● Seismic motion ● Gravity gradient ● Residual gas ● Many, many technical noise not shown here – Electronics etc. LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO Design target (10 -22 /sqrtHz, 100Hz BW) LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO S P C B B V C C V V V VV C P P P P LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

3 IFOs running well: LIGO Recent control room screen ● 12 hr trend of NS-NS inspiral range LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO NS-NS binary range from the start of S5 Duty factor from the start of S5 LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

Anticipated Sources in LIGO's Band LIGO (And corresponding LSC Search Groups) ● Periodic sources – Binary pulsars, spinning NS, low mass X-ray binaries “Mountain” on neutron star Wobbling neutron star – Eöample of upper limits (targeted) ● h 0 < 4.8ö10 -26 (PSR J1623-2631) ● ε < 1.1ö10 -7 (PSR J2124-3358) Accreting neutron star R-modes ● Crab pulsar: observational GW emission upper limit is smaller than the spin-down derived limit – Coalescing compact binaries NS-NS, NS-BH, BH-BH ● Physics regimes: Inspiral, merger, ● ringdown Numerical relativity is essential to ● interpret GW waveform ~16Mpc (1.4-1.4 M ☉ , all-sky, S/N=8) ● LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

Anticipated Sources in LIGO's Band LIGO (Continued) ● Burst gravitational waves – e.g. Supernovae with asymmetric collapse – Abrupt, uncharacterized impulse. Ex) Upper limit: – ● E GW ~ 0.1 M ☉ at 20 MpA (153 Hz case, untriggered) – to 10 8 – M ☉ (SGR1806- ● E GW ~ 10 7 20 at 5-10 kpA) – Stochastic background Primordial Big Bang (t = 10 -22 ● sec) Cross correlation of signals in ● pairs (LHO-LLO, LHO-LHO) Eö.) First upper limit all-sky ● map of stochastic point source for S4 LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

BTW, We Need Interaction With LIGO Non-GW Researchers ● Knowledge from any other Control room sAreen for GRB alert means/channels – better GW source model etc. – trigger with location information (e.g. GRB/SWIFT) etc. ● GW detection might also impact underlying physics of observed objects – e.g. non aöi-symmetry and NS equation of state ● NS specialists: please don't leave until the end of this talk (conference ad alert!) . www.astroscu.unam.mx/neutrones/NS-Picture/NStar/NStar_lS.gif LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

I'm afraid I don't have LIGO time to talk about these ● Many observational results for S4 and earlier were already published. – Please go to http://www.ligo.org ● Some analysis are going on for S4 and S5. – Some already appeared in conference talks. ● Again http://www.ligo.org LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO S5 summary ● Design sensitivity requirement met by all 3 IFOs. ● Good duty factors. ● As of Sep/10/2007, about 97.3 % of 1-year (~355 days) 3-coincidence data has been accumulated. – Already more than 1-year 2-site coincidence (accomplished July 2007) ● End of S5 date set: 2007/Oct/01 00:00:00 UTC – We'll very likely accumulate more than 1year worth of 3-coincidence data. ● We'll be ready for the neöt step very soon! LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting

LIGO LIGO Future LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai Insert Name of the Meeting