CNRS. APC Paris LMA Lyon LAL Orsay LAPP Annecy LKB - Paris OCA Nice

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2 INFN CNRS Sez. Firenze/Un.Urbino Sez. Genoa Sez. Napoli/Un. Federico II & Salerno Sez.Perugia/Un. Perugia & Camerino Sez. Pisa/Un. Pisa Sez. Roma/Un. Sapienza Sez.Roma 2/Un. Tor Vergata Sez. Padova/ Un. Trento APC Paris LMA Lyon LAL Orsay LAPP Annecy LKB - Paris OCA Nice Nikhef Amsterdam POLGRAV Warsaw (Polish Ac. Sci.) EGO phys. group RMKI (Hungarian Ac. Sci. Budapest) 2

3 3 km long Fabry-Perot cavities: to lengthen the optical path to 100 km Power recycling mirror: to increase the light power to 1 kw 3

4 3 km long Fabry-Perot cavities: to lengthen the optical path to 100 km Power recycling mirror: to increase the light power to 1 kw 4

5 LIGO Hanford, WA GEO600, Hanover, Germany LIGO Livingston, LA Virgo, Pisa, Italy Virgo and the LIGO Scientific Collaboration have signed a MoU for full data exchange and joint data analysis and publication policy 5

6 Now LIGO GEO S4 S5 AstroWatch S6 Advanced LIGO GEO-HF?? S7 S8 Virgo VSR1 VSR2 VSR3 Advanced Virgo VSR4 VSR5 6

7 The last decade has seen the demonstration of GW interferometers technology. Design sensitivity reached, high duty cycle, O(90%) NO DETECTION, YET 7

8 Coalescing binaries: Phys. Rev. D 79, (2009), arxiv: Bursts: arxiv: , arxiv: (submitted. Phys. Rev.) 8

9 no statistically significant gravitational-wave candidates within a [ 5, + 1) s window around the trigger time of any GRB no evidence for an excess of weak gravitational-wave signals in our sample of GRBs neutron star-black hole progenitors excluded up to a median 90% confidence exclusion distance of 6.7 Mpc 9

10 Vela 10

11 Vela spin-down limit in ~80 day 11

12 Remnant from supernova in year 1054 Spin frequency ν EM = 29.8 Hz ν gw = 2 ν EM = 59.6 Hz observed luminosity of the Crab nebula spin down due to: accounts for < 1/2 spin down power electromagnetic braking particle acceleration GW emission? early S5 result: h < 3.9 x ~ 4X below the spin down limit ellipticity upper limit: ε < 2.1 x 10-4 GW energy upper limit < 6% of radiated energy is in GWs Abbott, et al., Beating the spin-down limit on gravitational wave emission from the Crab pulsar, Ap. J. Lett. 683, L45-L49, (2008). 12

13 Rome Matched filter in Fourier space New method- Extremely effective from computational point of view Warsaw Uses original F-statistic and new G-statistic for imposing constraint from known orientation of pulsar Glasgow Uses familiar coarse/fine heterodyne stages and Bayesian pdf determination. Standard approach of the LIGO community 13

14 Try to capture an EM transient that would otherwise have been missed! First attempts underway Swift TAROT QUEST 14

15 Models for emission from GRBs even failed GRBs Joint searches planned with neutrino telescopes ANTARES IceCube Arecibo Green Bank LOFAR 15

16 Increase input power Laser amplifier 50 W New input mode-cleaner mirror Thermal compensation system Cut down on environmental noises New control electronics Improve thermal noise Monolithic suspensions Dedicated shutdown(s) for installation during VSR2» Change mirrors for higher cavity finesse at the same time 16

17 Increase input power Laser amplifier 50 W New input mode-cleaner mirror Thermal compensation system Cut down on environmental noises New control electronics Improve thermal noise Monolithic suspensions Dedicated shutdown(s) for installation during VSR2» Change mirrors for higher cavity finesse at the same time 17

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20 The prism, the most brilliant object B1S dumper from west 20

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23 1) Suspended Detection bench/tower dominates Hz and contributes significantly up to 150 Hz 2) WE contributes 40 and 100 Hz region. Now almost canceled by last week intervention 23

24 Suprasill substrate, Ta 2 O 5 :Ti coating VIRGO * North arm VIRGO * West arm VIRGO + North arm VIRGO + West arm Curvature [m] Losses(TEM00) [ppm] (*VIRGO configuration before2008, i.e. before the change of the North end mirror because of the viewport accident) Higher losses, but limited loss asymmetry between the two cavities ( V 70 ppm, V+ 180 ppm) Higher geometrical asymmetry. Curvature Difference : from V* 40 m, V+ 130 m beam overlap less efficient (transverse beam dimension 17.5 and 19.5 mm) less power in the TEM 00 mode higher shot noise contribution more diffused light 24

25 Courtesy of GEO 25

26 Supporting plate (Aluminum) Ring Heater Body (Aluminum) PEEK Thermal Insulating Supports 26

27 A factor 10 on the sensitivity A factor 1000 on the rate of events 1 year of initial detectors < 1 day of advanced detectors! LIGO - Virgo eligo - Virgo+ AdvLIGO - AdvVirgo 27

28 A factor 10 on the sensitivity A factor 1000 on the rate of events 1 year of initial detectors < 1 day of advanced detectors! LIGO - Virgo Predictions for the Rates of Compact Binary Coalescences Observable by Ground-based Gravitational-wave Detectors C.Q.G.27:173001,2010 eligo - Virgo+ AdvLIGO - AdvVirgo 28

29 A factor 10 on the sensitivity A factor 1000 on the rate of events 1 year of initial detectors < 1 day of advanced detectors! LIGO - Virgo Predictions for the Rates of Compact Binary Coalescences Observable by Ground-based Gravitational-wave Detectors C.Q.G.27:173001,2010 eligo - Virgo+ AdvLIGO - AdvVirgo 29

30 heavier mirrors low dissipation coating larger spot high finesse cavity compensation of thermal lensing signal recycling fused silica suspension fibers high power laser (200 W) DC detection 30

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33 Test mass substrates received Corrective coating robot being assembled Order for the first cryotrap ready to go 33

34 Underground facility to minimize seismic noise Mirrors held at cryogenic temperature 10 km arms, new geometries E.T. - Einstein gravitational-wave Telescope Design Study Proposal funded by EU within FP7 Large part of the European GW community involved (EGO, INFN, MPI, CNRS, NIKHEF, Univ. Birmingham, Cardiff, Glasgow) Credit: H.Lück 34

35 Underground facility to minimize seismic noise Mirrors held at cryogenic temperature 10 km arms, new geometries E.T. - Einstein gravitational-wave Telescope Design Study Proposal funded by EU within FP7 Large part of the European GW community involved (EGO, INFN, MPI, CNRS, NIKHEF, Univ. Birmingham, Cardiff, Glasgow) Credit: H.Lück 35

36 First generation GW detectors demonstrated! LIGO and Virgo upgrading towards 2 generation!! Science results start to flow in, good hope that 2 generation will start GW ASTRONOMY! Closer cooperation with the astrophysical community is a must. Gamma, neutrino, radio, optical, GW information are complementary to understand emission mechanisms and ultimately the physics of the sources. 36