Survey
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Virgo status Marie-Anne Bizouard (LAL-Orsay) on behalf of the Virgo Collaboration Outline • Ground based gravitational wave detectors • Virgo detector commissioning – 2006 • Virgo data analysis – searches and detector characterization • Preparation of Virgo future – Virgo+ – Advanced Virgo ( M. Barsuglia GW1) (E. Cuoco GW4 C. Palomba GW4) (N. Man GW2) • Short term planning MG 11 - Berlin 2 The Virgo Collaboration as in 2006 • • • • • • • • • CNRS - LAPP - Annecy INFN - Firenze/Urbino CNRS - LMA/ESPCI – Lyon/Paris INFN – Napoli CNRS - OCA – Nice + EGO (European Gravitational Observatory) CNRS - LAL - Orsay INFN - Perugia INFN - Pisa INFN – Roma 2006: NIKHEF – Amsterdam (joining) Tor Vergata – Roma (just joining) 175 physicists / engineers MG 11 - Berlin 3 Growing ground based interferometers network 4 & 2 km 600 m GEO 3 km 300 m 4 km TAMA MG 11 - Berlin 4 Interferometers at a glance How to detect the path of a GW? measure the displacement of the mirrors induced by the GW h light phase shift measurement But: • GW amplitude is small h~10-21 L=3km • The laser has fluctuations in phase and amplitude • External forces push the mirrors L=10-18 m L 2 L Seismic noise h L / L Shot noise: quantum fluctuation in the number of detected photons Thermal noise: vibration of bulk due to non null temperature MG 11 - Berlin 5 Virgo optical layout L=3km Input Mode Cleaner cavity Length = 144 m Laser Nd:YVO4 P=20 W Recycling L=3km P=1kW Output Mode Cleaner cavity Length = 4 cm A Michelson with 3 partly-transparent mirrors to form optical cavities to increase the power inside the arms MG 11 - Berlin Virgo seismic attenuator 6 Interferometer controls 1: longitudinal control ITF output port • Keep the Fabry Perot cavities in resonance • Keep the output on the “dark fringe” ITF “locked” Keep the arms’ length constant within 10-12 m 2: angular control Recycling cavity power • Avoid high order mode generation (reduction of coupling dark fringe with frequency noise, power noise, input beam jitter, beam miscentering, ..) Alignment ON Reduction of the power fluctuation! MG 11 - Berlin A L I G N M E N T7 Interferometer controls • Complicated scheme! • Controls introduce noise in the dark fringe at low frequency (<100Hz) MG 11 - Berlin 8 Foreseen sensitivity Thermal noise Seismic wall MG 11 - Berlin 9 Virgo sensitivity curve progresses (as end of 2005) C7 run (sep. 2005): Best strain h ~ 6 10-22 / Hz1/2 NS/NS maximum range ~ 1.5 Mpc MG 11 - Berlin (optimal orientation) 10 Noise budget MG 11 - Berlin 11 Shutdown at end of 2005 – Why? • Increase the power 2005: need to operate with reduced power: 0.7 W instead of 10W because of backscattering light in the Mode Cleaner cavity Increase a lot the frequency noise Backscattering Solution: Faraday isolator on the injection bench to attenuate the backscattering light a new injection bench MG 11 - Berlin 12 Shutdown at end of 2005 – Why? • Non-monolithic and curved Power Recycling mirror – Curved: because part of the output telescope to match the beam – Non-monolithic: lots of resonances control problems and alignment drifts 350 mm 350 mm 120 mm 120 mm R=4100 mm R=4100 mm • Solution: – Monolithic mirror – Flat mirror Incident Incident Beam Beam Translations induce misalignment and jitter noise need of a telescope on the injection bench a new injection bench … MG 11 - Berlin 13 New injection bench Faraday isolator MG 11 - Berlin New parabolic telescope 14 Virgo commissioning – new input bench Sep 2005 – April 2006 Lots of work: – – – – New scheme of the alignment wrt to the ITF Parabolic telescope alignment done Beam matching: 95% reached Faraday isolator tuned No more backscattering light problem! M. Barsuglia GW1 7 W entering in the ITF 280 W on the BS (sep. 2005: 25W! ) MG 11 - Berlin 15 Virgo commissioning – full power recycled ITF Feb 2006 – until now We had few problems/difficulties: • Beam matching See M. Barsuglia in GW1 • Beam astigmatism • Beam clipping on detection bench • Oscillations in signals used for control lock losses! •Work Thermal effect in substrate (25W 280W on Beam Splitter mirror) ? done on: - demodulation phase tuning - more angular degrees of freedom controlled Lock stability improved a lot ! 10 hours Where are we now? •f>200 Hz: better than one year ago •f<200 Hz: a lot of work to be done! (dominated by control noise) … but the noise hunting period just restarted! MG 11 - Berlin 16 The last data taking periods - 2005 C6 July 2005 Maximal distance (Mpc) Maximal distance for SNR=8, optimally oriented 1.4/1.4 M NS-NS binary 14 days C7 Sep. 2005 5 days duty cycle: 86% in Science Mode duty cycle: 65% in Science Mode Shorter but better sensitivity best NS-NS distance range: 1.5 Mpc ! Beyond Andromeda reached! MG 11 - Berlin 17 Data analysis in Virgo at a glance NS EOS, Strong field gravity, GRB models, ..) Binary population … lots of astronomy! • Virgo search groups – – – – Burst (SN, neutron star and black hole birth, Binary inspiral (neutron star + black hole) Continuous waves (spinning neutron stars) Stochastic background (big bang + background of “standard” GW) But we don’t have yet the sensitivity to set competitive upper limits … So C6 & C7 data taking analysis …. more dealing with – pipeline development / tuning – detector characterization More details in E. Cuoco and C. Palomba’s talks than with “physics” search or competitive upper limits MG 11 - Berlin 18 Burst events search – – Events distribution dramatically different from Gaussian Vetoes based on auxiliary channels understand the machine Events • Burst studies on a single detector: hard! Frequency (Hz) SNR Vetoes definition: Excess noise above 100 Hz due to GW channel coupling • excess frequency noise with the frequency noise when the North End mirror is tilted without veto • environmental glitches (air conditioning, air plane, …) problem of mirror angular control with veto Time (s) (too loose during C6 &C7) Nice reduction of the burst fake events … but huge dead time: >20% Events Dark fringe (whiten) • Identification of the main source of excess noise for the burst search: • Vetoes strategy: MG 11 - Berlin SNR 19 Inspiral search • C6/C7 analysis focus: NS-NS search – – • 2 pipelines developed in Virgo Veto studies – Virgo data understanding Fake events rejection: 1. Veto against “identified” noisy data periods 2. Use of “2” methods to reject fake events Hardware GW injections (the 2 checks the compatibility between the signal waveform and the recorded strain) Before 2 After 2 • Fake event rejection safety test? – Hardware GW injections Hardware event injection (force applied on the mirrors) ( + signal recovery accuracy estimation) vetoes are safe for the hardware injections, while strongly reducing the event distribution tails ! MG 11 - Berlin 20 Continuous sources search • All-sky search pipeline: hierarchical + coincidence • C6 & C7 work goal: C. Palomba GW4 – 1kHz band considered (50Hz 1050 Hz) – Production of bank of candidates for C6 and C7 and perform coincidence – Detection of detector related noise that could bias the analysis Example: 10 Hz disturbance : pulses caused by a video camera C6: number of candidates before coincidence Number of candidates : excess for some frequencies! Sensitivity obtained : h~10-23 (Virgo design: h~10-25 [200-1000 Hz] @ 200 Hz) MG 11 - Berlin Frequency (Hz) 21 Stochastic background GW search with Virgo • This search requires cross-correlation between 2 detectors’ output (GW background sensitivity depends on distance and orientation) • Auriga/Nautilus/Explorer/Virgo Scope limited by the bars sensitivity curve Virgo at design sensitivity : WGW < 2 x 10-2 • LHO, LLO, GEO, Virgo – Isotropic background search S. Ballmer gr-qc/0510096 – Directional search (sky map luminosity) (background could be dominated by individual sources!) • First detectors generation sensitivity: WGW ~ 4 x 10-6 MG 11 - Berlin f> 300 Hz: Virgo-GEO performs good! advanced detectors needed! 22 International collaborations • Auriga-RoG-Virgo – Burst search + Stochastic background search • LSC-Virgo: – Burst + Inspiral : working effort for 2 years (simulated data) + SB just joins “Physics gain” to add a (non aligned) ITF to LIGO network: - reconstruction of the source location (need of at least 3 ITF!) - signal parameters estimation - detection efficiency enhanced by 50% (burst) or 30% (inspiral) – Now: discussions about • data exchange agreement (MOU to be signed) • how to work as a joint data analysis group • Sketching a tentative joint run planning MG 11 - Berlin 23 Outline • Ground based gravitational wave detectors • Virgo detector commissioning – 2006 • Virgo data analysis – searches and detector characterization • Preparation of Virgo future – Virgo+ – Advanced Virgo (second generation ITF) • Short term planning MG 11 - Berlin 24 Virgo future preparation • Virgo+ • Advanced Virgo (second generation ITF) LIGO - Virgo LIGO+ - Virgo+ AdvLIGO - AdvVirgo A factor 10 in distance to hit sources in a volume 1000 times larger Credit: R.Powell MG 11 - Berlin 25 Virgo upgrades planning Now • Short term – – – – Acoustic isolation Pre-Mode Cleaner Upgrade of the quadrant diode front-end electronics New coil drivers (R&D) • Intermediate term – – – – Eddy current dissipation mitigation New MC mirror payload New DSP electronics (R&D) Thermal compensation • Virgo+ upgrades 2007 2008 2009 MG 11 - Berlin 26 What is Virgo+ project? -18 10 h(f) [1/sqrt(Hz)] Last stage of the suspension thermal noise (pendulum mode excited) friction metallic wires clamping wire dissipation Monolithic suspension! (a) Virgo Nominal sensitivity (b) Seismic noise (c) Pendulum thermal noise (d) Mirror thermal noise (e) Shot Noise -19 10 -20 10 (b) -21 10 (d) -22 10 (a) (e) (c) -23 10 1 10 100 1000 10000 Frequency [Hz] shot noise higher power laser! mirror thermal noise (bulk + coating) higher Q new material + coating R&D MG 11 - Berlin 27 Virgo+ • Virgo+ upgrades – High power laser amplifier 20W 50W N. Man (GW2) – Replace all Virgo mirrors with Suprasil 311 fused silica (low losses) – Improved coatings R&D – Fused silica monolithic payload – New DAQ electronics (R&D) • Compatible with current Virgo optical configuration • Require a relative short shutdown MG 11 - Berlin 28 Monolithic payload on going activities 2 machines for producing and welding fused silica fibers in Cascina: H2-O2 (Perugia) (different technology) Fused silica fiber CO2 (Glasgow) Fused silicate fiber H2-O2 pulling machine on site Dummy mirror to test the monolithic suspension MG 11 - Berlin 29 Virgo+ scientific outreach -18 10 -19 10 h(f) [1/sqrt(Hz)] Thermal noise decrease 50W/2 + new losses model 50W/2 + current mirrors Nominal Virgo 50W/2 + new losses model+FS suspensions Virgo+ with Newtonian Noise -20 10 Shot noise decrease -21 10 -22 10 -23 10 1 10 100 1000 10000 Frequency [Hz] Virgo+ (NN) Mpc Opt. orientation NS-NS signal detection benefits(average) of the sensitivity improvement at NSNS intermediate frequency114 (45.6) BHBH 584 (234) MG 11 - Berlin 30 Short term planning - Conclusions • Commissioning: – Noise hunting phase – Reduction of control noise sources In the next weeks: reach LIGO sensitivity at high frequency Start collecting “Science” data this fall Soft transition towards long data taking periods for GW searches • Huge campaign of upgrades : Virgo+ foreseen in 2008 inspiral event rate: gain more than a factor 10! • Advanced Virgo: design choice by end of 2007 MG 11 - Berlin 31