Status of Virgo Gabriele Vajente INFN Pisa and Scuola Normale Superiore di Pisa On behalf of the Virgo Collaboration 11 th Gravitational Wave Data Analysis

Status of Virgo

Gabriele VajenteINFN Pisa and Scuola Normale Superiore di Pisa

On behalf of the Virgo Collaboration

11th Gravitational Wave Data Analysis Workshop Potsdam, December 18th 2006

GWDAW 11 December 18th , 2006 – Gabriele Vajente 2

Virgo collaboration

New groups joined the collaboration

ESPCI ParisLAPP LAL OrsayLMA LyonOCA

INFN Perugia INFN Firenze INFN NapoliINFN PisaINFN Roma 1

NIKHEF

INFN Roma 2


Restart after shutdown

Last winter shutdown for hardware upgrades

Injection bench replacement to run with higher input power (10 W enter the ITF)

Power Recycling mirror replacement with new monolithic mirror, higher reflectivity (95 %)

PR mirror mechanical transfer function OLD NEW


Thermal issues

Higher power produces thermal effects

Lock acquisition long (~20 min)Thermal transient is a critical periodWait for 10 min after reaching dark fringe conditionNeeded a reduction of input power to 5.5 W (entering the ITF)Need for a thermal compensation system, work starting

BS Pick-off power Lower sideband Higher sideband


WSR3 and WSR4 were canceled for bad conditions

Week-end Science Run

Periodic short data taking started in September 2006start moving towards a science run operationtake snapshots of the commissioning progresstake clean data in controlled conditionslight organizationpriority always on commissioning

WSR1 September 08th - 11th

WSR2 September 22th - 25th

WSR3 October 06th - 09th

WSR4 October 13th - 16th

WSR5 November 10th - 13th

WSR6 December 01th - 04th

WSR7 January 12th - 15th


Sensitivity in WSRs


Comparison of sensitivity


Duty cycle and horizon in WSRsH

oriz

on fo

r N

S N

S (

aver

aged

) [M

Pc]

WSR1

Duty cycle 87.7%

Longest lock 15 h

WSR2

Duty cycle 68.7%

Longest lock 27 h

WSR5

Duty cycle 64.2%

Longest lock 10 h

WSR6

Duty cycle 80.5%

Longest lock 18 h


Dependence on weather conditions

The horizon is affected by microseismic conditions

Sea activity

Wind

Suspension control improvements on-going

Ho

rizo

n N

S-N

S o

pti

mal

[M

Pc]

Sei

smic

act

ivit

y [a

.u.]

Sei

smic

act

ivit

y [a

.u.]

RMS 220 mHz – 1 Hz

RMS 30 mHz – 100 mHz


Noise budget

Below 50 Hz control noise (longitudinal and angular)

Above 1kHz frequency noise

and shot noise

Intermediate region

WSR5


Acoustic noise / diffused light

The main suspect is acoustic and seismic noise from benches in air

Through diffused and scattered light effects

Investigations on-going

Projection of acoustic noise introduced by the detection bench, measured with acoustic noise injections


Brief overview of Data Analysis at Virgo

Virgo search groups

Bursts

Binary inspirals

Periodic signals

Stochastic background

Noise studies

Virgo-Bars network

Virgo-LIGO collaboration



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Analysis of data quality (talk by E.Cuoco)

Studies on veto procedures and efficiency (poster by M. Del Prete)

Search fro bursts from GRB 050915a (poster by A. Corsi)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


On-line analysis perfomed using Merlino and MBTA algorithms(talk by L. B. Bosi)

Study on coherent analysis with a network of ITF(poster by S. Birindelli)

Improvements in the timing accuracy(poster by D. Grosjean)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Coincidence analysis between C6 and C7 run (talk by C.Palomba)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Analysis of prospect of detection in a network search Virgo/LSC(talk by G.Cella)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Search and removal of lines(poster by I. Fiori et al.)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Analyzed 24 hours of data in coincidence during Virgo C7 run

ILIAS-WG2 methodological paper under preparation(Talk by L. Baggio)



Virgo search groups

Bursts

Binary inspirals

Periodic signals


Noise studies

Virgo-Bars network


Comparison of calibration and pipelinesMethodological work on simulated dataExchanges of short data segments for developing and testing networkanalysis methods.


Prospects for the future20

0720

0820

09

Virgo WSRsVirgo commissioning

Virgo+ upgrade

Virgo+ commissioning

Virgo+ Scientific Run

Virgo commissioning

TIM

E

Virgo Scientific Run (in coincidence with S5)


Virgo+

50 W laser, F=150 cavitiesLow loss suprasil end mirrorsMonolitic suspensions

1 10 100 1000 1000010-23

10-22

10-21

10-20

10-19

10-18

h(f) [1

/sqrt(H

z)]

Frequency [Hz]

50W/2 + new losses model 50W/2 + new losses model + F=150 50W/2 + current mirrors Nominal Virgo 50W/2 + new losses mod+FS suspensions+F=150 Virgo+ with Newtonian Noise

NN

Shot noise decreasedThermal noise decreased


SummaryWSR program started and continuing

with good duty cycleimproving sensitivity (high frequency almost at measured shot noise, comparable with LIGO)

Commissioning continuesbig efforts in the 50 - 500 Hz region

Goal to have a Science Run in coincidence with LSC S5Plans for Virgo+ upgrade

Documents

Status of Virgo Gabriele Vajente INFN Pisa and Scuola Normale Superiore di Pisa On behalf of the Virgo Collaboration 11 th Gravitational Wave Data Analysis