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アウリガ. The AURIGA experiment: updates and prospects. バッジョ ルーチョ. BAGGIO Lucio ICRR on behalf of AURIGA collaboration. The AURIGA detector re-started data taking in Dec 2003, after 4 years of research and developement, in order to improve the sensitivity.

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The auriga experiment updates and prospects

アウリガ

The AURIGA experiment: updates and prospects

バッジョ ルーチョ

BAGGIOLucio

ICRR

on behalf of AURIGA collaboration

The AURIGA detector re-started data taking in Dec 2003, after 4 years of research and developement, in order to improve the sensitivity.

A brief overview of the results during last year will be given.

Present international collaborations and future prospects will be reviewed.

[email protected]


Topics of this presentation
Topics of this presentation

The AURIGA experiment: run 2

Characteristics and setup of the second run (after Dec 2003)

Burst analysis

Main issues with burst search: duty cycle, detection efficiency, background events

Collaborations

Memorandum of Understanding with LIGO, IGEC-2 agreement, contacts with VIRGO

Other activities

New cryogenic detector with optical transducer; the DUAL project

Next steps and Summary

New low-frequency suspensions, ultra-cryogenic cooling,



Old new auriga detector
Old & New AURIGA detector

1997/06

Cryogenic failure

1999/12

R&D

2003/12


Main upgrades for the 2 nd run
Main upgrades for the 2nd run

  • New mechanical suspensions:

  • attenuation > 360 dB at 1 kHz

  • FEM modelled

  • 3 resonant modes operation:

  • two mechanical modes

  • one electrical mode

  • New data analysis and data acquisition:

  • C++ object oriented code

  • frame data format

  • Monte Carlo software injections (internal or MDC)

  • improved noise matching algorithm

  • selectable templates

“New suspension system for the gravitational wave bar detector AURIGA” (in preparation, to be submitted toRev. Sc. Inst.)

3-mode detection for widening the bandwidth of resonant gravitational wave detectors

L. Baggio,M. Bignotto, M. Bonaldi,M. Cerdonio,L. Conti,P. Falferi,N. Liguori,A. Marin,R. Mezzena,A. Ortolan,S. Poggi,G. A. Prodi,F. Salemi,G. Soranzo,L. Taffarello,G. Vedovato,A. Vinante,S. Vitale,and J. P. Zendri

(submitted toPhys. Rev D.)


The new suspension system 1
The new suspension system (1)

Attenuation & Internal modes frequency (-240DB wide band  FEM)

(a,b,c,d,e,f) are resonances of the suspension predicted by FEM

Quality factor

Yield strength (no more than 25% to avoid creeps)

Ultracryogenic (0.1 K) compatibility (no thermal short-circuit with 4K container, good thermal link to diluition refrigerator)

Vacuum compatibility (10-6mb  no rubber)



New transducer amplifier
New transducer & amplifier

■ Two-stage SQUID: Tn(h) = 97 + 78T(K)

● Single stage SQUID: Tn(h) = 1280 +300T(K)

Noise Temperature (h)

Temperature (K)

  • three resonant modes operation:

    • two mechanical modes

    • one electrical mode

  • transducer bias field 8 MV/m

  • new SQUID amplifier :

    • double stage SQUID

    • 650  energy resolution at 4.5 K in the detector


Raw data calibration
Raw data& calibration

Mechanical transfer function (response to force applied by a electromechanical actuator attached to the bar)

Fully-automatic adaptive noise matching algorithm enbedded in AURIGA data analysis

1

2

3

Frequency [Hz]

Fit of the psd with ARMA noise model


Temperature of normal modes
Temperature of normal modes

Monday morning

mode 1

mode 2

mode 3

T [ K ]

date 13-15 Nov. 2004


Noise budget expected at 4 5k
Noise budget expected at 4.5K

Shh1/2 < 5·10-21Hz-1/2 over 90 Hz

single-sided Shh

Very good agreement with noise predictions

All these noise sources will scale with temperature


Burst analysis matched filter

Burst analysis(matched filter)


Typical sensitivity to bursts
Typical sensitivity to bursts

H

[Hz-1]

10-21 –

 [Hz-1]

Template:

2004, Nov 13-15 (weekend)



Unexpected non linear non stationary noise
Unexpected non-linear, non stationary noise

unmodeled spurious noise peaks within the sensitivity bandwidth

  • not related to the dynamical linear response ofthe detector

  • non gaussian statistics

  • related to mechanical external disturbances

  • up-conversion of low frequency noise


Epoch vetoes and goodness of fit tests
Epoch vetoes and goodness-of-fit tests

with template information, further improvement comes from check of compliance

Epoch vetoes from out-of-band information

SNR

Time [day]


Background events approaching the gaussian tail

cumulative event rate above threshold

false alarm rate [hour-1]

after vetoing

epoch vetoes (50% of time)

vetoed glitches

Remaining events after vetoing

Background events: approaching the gaussian tail

Amplitude distribution of events

AURIGA Nov. 13-14, 2004


Duty cycle
Duty cycle

low-frequency mechanical attenuators



Performances after the upgrade of suspensions
Performances after the upgrade of suspensions

10 days of stationary gaussian operation:

< 2 outliers/day

~60% duty cycle for gaussian data

Experimental data

Simulated data (gaussian noise)

2004 Dec 03-13

(after vetoes)

counts

SNR



International gravitational event collaboration
International Gravitational Event Collaboration

AURIGA is member of the IGEC since its foundation in 1997. IGEC HP: http://igec.lnl.infn.it

Main results in:

P. Astoneet al., “Methods and results of the IGEC search for burst gravitational waves in the years1997-2000”, Phys. Rev. D68 (2003) 022001

(also on astro-ph/0302482)

IGEC-2 Agreement, Jan 17th 2005

The groups running the four bar detectors ALLEGRO, AURIGA, EXPLORER, NAUTILUS have signed a Letter of Intent to perform a new joint observation starting from 2004 available data. The approach of this new joint observation, will be based on the previous IGEC experience. The observation times of the participating detectors will be coordinated. IGEC-2 is open to agreements with other projects sharing the same scientific objectives.


Ligo auriga mou
LIGO-AURIGA MoU

A Memorandum of understanding between the experiment AURIGA and the LIGO project has been recently signed, for the purposes of joint data analysis and dissemination of results

2004/07/12 LIGO-M040010-00-M (MoU)

2004/07/12 LIGO-M040191-00-M (Attachment 1)

2004/07/12 LIGO-M040198-00-M (Membership list)


Joint ligo auriga working group activity
Joint LIGO-AURIGA working group activity

STEP-ZERO

Outline of the most interesting analysis to be performed based on preliminary study of sensitivity and efficiency of the detectors

Document Type LIGO-T040202-00 2004/10/13

Proposal for the First AURIGA-LIGO Joint Analysis

L. Baggio, L Cadonati, S. Heng, W. Johnson, A. Mion, S. Poggi, G.A. Prodi, A. Ortolan, F. Salemi, P. Sutton, G.Vedovato, M. Zanolin

1st STEP

Cross-correlation between LIGOs (L1, H1 & H2) around the times of AURIGA triggers  Analysis of S3 data in progress

2nd STEP

Implementation of IGEC-like analysis (self adapting directional coincidence search between candidate event lists from each detector) <in preparation >


Ligo auriga mou1
LIGO-AURIGA MoU

A working group for the joint burst search in LIGO and AURIGA has been formed, with the purpose to:

  • develop methodologies for bar/interferometer searches, to be tested on real data

  • time coincidence, triggered based search on a 2-week coincidence period (Dec 24, 2003 – Jan 9, 2004)

  • explore coherent methods

‘best’ single-sided PSD

Simulations and methodological studies are in progress.


White paper on joint analysis
White paper on joint analysis

Two methods will be explored in parallel:

  • Method 1:

  • IGEC style, but with a new definition of consistent amplitude estimator in order to face the radically different spectral densities of the two kind of detectors (interferometers and bars).

  • To fully exploit IGEC philosophy, as the detectors are not parallel, polarization effects should be taken into account (multiple trials on polarization grid).

  • Method 2:

  • No assumptions are made on direction or waveform.

  • A CorrPower search (see poster) is applied to the LIGO interferometers around the time of the AURIGA triggers.

  • Efficiency for classes of waveforms and source population is performed through Monte Carlo simulation, LIGO-style (see talks by Zweizig, Yakushin, Klimenko).

  • The accidental rate (background) is obtained with unphysical time-shifts between data streams.



Optical readout for a bar detector
Optical readout for a bar detector

bar

Transducer cavity: a Fabry-Perot cavity between the bar and the resonant

Reference cavity: a stable Fabry-Perot cavity acting as length reference

Laser frequency locked to the reference cavity

Working principle:

Variations of the transducer cavity length are measured by the stabilized laser

bar


Room temperature prototype 2001
Room temperature prototype (2001)

The readout mechanics

The reference cavity

L = 110 mm, FSR = 1.36 GHz, F = 44000



New detector with cryogenic optical transducer 1
New detector with cryogenic optical transducer (1)

Sensitivity predicted at T=4K with already developed technology

Goal: acquire data from a cryogenic bar equipped with the optical readout

  • New transducer mechanics

  • New bench on top of the bar with cryogenic-compliant motorized mounts for optics

  • New cryogenic-compliant bar suspension

  • New clean vacuum system

  • New anechoic housing for the laser optical bench

  • Higher finesse cavity

The new reference cavity

TO DO:

New cryogenic bar housing (in progress)

Transducer with optimized mass (after first tests)


New detector with cryogenic optical transducer 2
New detector with cryogenic optical transducer (2)

cables and optical phiber thermalization

Lhe vessel

adaptater & pre-attenuation

single-column cryogenic suspension

Direct thermal links from the Lhe vessel

Roadmap:

April: delivery of the cryogenic container

Summer: assembling and testing

Autumn: commissioning of the complete detector

2006: first measures


Dual concept

Two possible configurations:

DUAL: concept

Measurement of differential deformations of two nested bodies, resonating at different frequencies and both sensitive to the gw signal

Dual sphere

PRL 87 (2001) 031101

antenna pattern:

isotropic

Dual cylinder

PRD 68 (2003) 102004

antenna pattern:

identical to that of 2 interferometers at 45 degrees with respect to each other

  • In the intermediate frequency range:

  • the outer resonator is driven above resonance,

  • the inner resonator is driven below resonance

  • → phase difference of 

In the differential measurement:

→ the signals sum up

→ the readout back action noise subtracts


Dual predicted sensitivity
DUAL: predicted sensitivity

Q/T > 2 108 K-1 , Standard Quantum Limit

  • Current activity:

  • Detector design

  • seismic noise control (pre-filtering)

  • high frequency (in band) mechanical

  • vibration filtering

  • underground operation

  • Readout system

  • Requirement: ~ 5x10-23 m/√Hz

  • Two concurrent studies: capacitive (+SQUID) and optical (folded Fabry-Perot, Phys. Lett. A 309, 15 (2003) ) readout

Mo Dual16.4 ton height 2.3 m Ø 0.94m

SiC Dual 62.2 ton height 3 m Ø 2.9m



New low frequency vibrational damping
New low frequency vibrational damping

New external suspensions: “fast” assembling in April-June

Air springs: effective above1-2 Hz



Further steps to increase the bandwidth
Further steps to increase the bandwidth

T = 0.1K

T = 0.1K and bias field x2.5



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