LIGOBCBAct/talks02/Ph... · LHC ENERGY FRONTIER LHC Upgrades VLHC Linear Collider CLIC Muon Collider NuMI/MINOS LEPTON FLAVOR PHYSICS Neutrino Superbeam Neutrino Factory BaBar & BELLE

LIGOas a

Large Science Project

Barry Barish

Ph237b

April 23, 2002

24-Apr-02 Physics 237b 2

Experimental Research

! Traditional Mode – Single Investigator» Program built around a laboratory with some equipment» Experiment built to attack particular problem» Support from private funds and/or grants» Typical support ~$150K/year» NSF, DoE, NASA

! Larger Projects : Which ones, how implemented, etc» Astronomy (private, NSF, …)» Space science (NASA)» Particle physics (DoE, NSF)» LIGO (NSF, but …)


Experimental Research! Small Science

» Grants or private funding for the research (& infrastructure)» No direct accountability» Peer review for renewal or new grants» This system is flexible and creates experiment driven by science

and ideas

! Large Science» Large special funding required for equipment» Large National Labs (Fermilab, JPL, etc)» Direct accountability» Peer review for science + management, resources, etc» Strategic planning, high level direction, etc determine science

program


Experimental Research! Research vs Project for Large Science

» How to create an effective research environment for large science» The system should be flexible and create experiment driven by

science and ideas» Different models

– NASA – science teams separate from project team, open data– DoE – umbrella grants, internal guidelines and reviews, collaborations, ..– Private – Keck– LIGO – NSF funded - designed to evolve into standard peer review system

! Strategic Planning» NSF top down from high level planning committees» Astronomy from Decadal Review by NAS panel» Particle Physics from National Laboratories + Road Map» LIGO – New endeavor in a new experimental field (Thorne, Drever,

Weiss, Vogt, …)

HEP Long Range Planning

A Long Range Plan for

U.S. High Energy Physics

Jon Bagger & Barry BarishBriefing for Ray Orbach, Office of Science

12-March-02

HEPAP Subpanelon

Long Range Planning

12-March-02 Summary -- Long Range Plan for HEP 2

The Goal of our SubpanelTo create a vision for the field for the next 20 years

The questions we posed for ourselves• What is our role in society and education?• What is high energy physics?• What are our goals and the paths to accomplish them?• How have we been doing?• What do we expect in the near term?• What opportunities do we identify for the longer term?• How do the U.S. and global programs interact?• What are the essential elements of a realistic program aimed

at our goals?• How can we set priorities and make the best choices?• How do we prepare for the far future?


Developing a Long Range Strategy for HEPFrontier Pathway

Scenic and Historic BywayA “roadmap” is an extended look at the future of a chosen field of inquiry composed from the collective knowledge and imagination of the brightest drivers ofchange in that field.

R. GalvinMotorola


SLAC

Anti-Matter Asymmetry

High Energy PhysicsRecent Accomplishments

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Top Quark EventFermilab

Neutrino Mass

Non-accelerator


The Particle Physics RoadmapNear-Term Program

SLAC BaBar Fermilab Run 2

Precision Measurements

Next 5 Years ~ 500 fb-1 Pursuit of the Higgs

FermilabMINOS

Neutrino OscillationParameters

CDF

MINOS


Matter, Energy, Space and Time

From each of these goals flows a diverse research program that will be carried out in partnership with colleagues across the globe.

Paths to the Goals of Particle Physics


The Particle Physics Roadmap• We have many tools at our disposal from forefront

accelerators to satellites in space to experiments deep underground.

AcceleratorLHC Magnet

Space

Our science requires forefront accelerators at the energy and luminosity frontiers. It also requires innovative experiments in space, underground, and away from accelerators.

The Soudan MineMINOS


CERN LHC

The Particle Physics Roadmap

The Energy Frontier

• Higgs• Supersymmetry• Extra Dimensions• New Phenomena

CERN LHC: The Next Big Step for HEP

Accelerator, Atlas, CMS


CDF & DØH1 & Zeus

LHCENERGY FRONTIER LHC Upgrades

VLHCLinear Collider

CLICMuon Collider

NuMI/MINOSLEPTON FLAVOR PHYSICS Neutrino Superbeam

Neutrino Factory

BaBar & BELLEBTeV

QUARK FLAVOR PHYSICS CESR-cRSVPCKM

Super B Factory

UNIFICATION SCALE PHYSICS Proton DecayNUSL

COSMOLOGY SNAP

PARTICLE ASTROPHYSICS IceCubeGLAST

2000 20202005 20152010

Not all projects illustrated on the roadmap can be pursued.

The Particle Physics RoadmapLong Range Opportunities


ROADMAP

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NEW INITIATIVESLC OPERATIONLC OFFLHC LUM UPGRDLATTICE COMP.HI INT NEUTRINOSNAPCESR CRSVPICE CUBENUMI/MINOSCDMSSDSSVERITASPie rre Auge rGLAST LHC BASE-LABFNAL+SLAC

Scenario with off-shore linear collider


ROADMAP

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NEW INITIATIVESLC OPERATIONLC ONLHC LUM UPGRDLATTICE COMP.HI INT NEUTRINOSNAPCESR CRSVPICE CUBENUMI/MINOSCDMSSDSSVERITASPie rre Auge rGLAST LHC BASE-LABFNAL+SLAC

Scenario with on-shore linear collider


LIGO Project! Organized like typical construction project (1994-2000)

» Vertical organization – every task has task manager, budget, deliverables, direct line of reporting

» Integration is the hard part» Project guided by scientists

! Evolution to Operating Research Environment (2000 - )» Flat organization – separate groups by task operating like

small laboratories (40m, TNI, Advanced R&D, data analysis, commissioning)

» New projects (Adv LIGO) done as project task within this structure

» Broader community – LSC and open data access


Summary integrated schedule


LIGOfacilities milestones

Milestone Description PMPProjection/

Actual PMPProjection/

Actual

Initiate Site Development Mar-94 Mar-94 Aug-95 Jun-95Beam Tube Final Design Review Apr-94 Apr-94 Apr-94 Apr-94Select A&E Contractor Nov-94 Nov-94 Nov-94 Nov-94Complete Beam Tube Qualification Test Feb-95 Apr-95 Feb-95 Apr-95Select Vacuum Equipment Contractor Mar-95 Jul-95 Mar-95 Jul-95Complete Performance Measurement Baseline Apr-95 Apr-95 Apr-95 Apr-95Initiate Beam Tube Fabrication Oct-95 Dec-95 Oct-95 Dec-95Initiate Slab Construction Oct-95 Feb-96 Jan-97 Jan-97Initiate Building Construction Jun-96 Jul-96 Jan-97 Jan-97Joint Occupancy Sep-97 Oct-97 Mar-98 Feb-98Accept Tubes and Covers Mar-98 Mar-98 Mar-99 Oct-98Beneficial Occupancy Mar-98 Mar-98 Sep-98 Dec-98Accept Vacuum Equipment Mar-98 Nov-98 Sep-98 Jan-99Initiate Facility Shakedown Mar-98 Nov-98 Mar-99 Jan-99

Hanford Livingston


LIGOcosts & commitments


LIGOcontingency vs percent complete


Staffinghistory


Staffinglabor distribution projections

LIGOStatus


LIGO Hanford Observatory


Signals in CoincidenceHanford Observatory

LivingstonObservatory


Detection Strategycoincidences

! Two Sites - Three Interferometers» Single Interferometer non-gaussian level ~50/hr» Hanford (Doubles) correlated rate (x1000) ~1/day» Hanford + Livingston uncorrelated (x5000) <0.1/yr

! Data Recording (time series)» gravitational wave signal (0.2 MB/sec)» total data (16 MB/s)» on-line filters, diagnostics, data compression» off line data analysis, archive etc

! Signal Extraction» signal from noise (vetoes, noise analysis)» templates, wavelets, etc


LIGO Plansschedule

1996 Construction Underway (mostly civil)1997 Facility Construction (vacuum system)1998 Interferometer Construction (complete facilities)1999 Construction Complete (interferometers in vacuum)2000 Detector Installation (commissioning subsystems)2001 Commission Interferometers (first coincidences)2002 Sensitivity studies (initiate short data taking runs)2003+ LIGO I data run (one year integrated data at h ~ 10-21)

2006 Begin LIGO II installation


LIGO Facilitiesbeam tube enclosure

• minimal enclosure

• reinforced concrete

• no services


LIGObeam tube

! LIGO beam tube under construction in January 1998

! 65 ft spiral welded sections

! girth welded in portable clean room in the field

1.2 m diameter - 3mm stainless50 km of weld

NO LEAKS !!


LIGO I the noise floor

! Interferometry is limited by three fundamental noise sources

" seismic noise at the lowest frequencies" thermal noise at intermediate frequencies" shot noise at high frequencies

!Many other noise sources lurk underneath and must be controlled as the instrument is improved


Beam Tube bakeout

• I = 2000 amps for ~ 1 week

• no leaks !!

• final vacuum at level where not limiting noise, even for future detectors


LIGOvacuum equipment


Vacuum Chambersvibration isolation systems

» Reduce in-band seismic motion by 4 - 6 orders of magnitude» Compensate for microseism at 0.15 Hz by a factor of ten» Compensate (partially) for Earth tides


Seismic Isolationsprings and masses

damped springcross section


Seismic Isolationsuspension system

• support structure is welded tubular stainless steel

• suspension wire is 0.31 mm diameter steel music wire

• fundamental violin mode frequency of 340 Hz

suspension assembly for a core optic


LIGO Noise Curvesmodeled sensitivity

wire resonances


Core Opticsfused silica

Caltech data CSIRO data

! Surface uniformity < 1 nm rms! Scatter < 50 ppm! Absorption < 2 ppm! ROC matched < 3%! Internal mode Q’s > 2 x 106


Core Optics installation and alignment


ITMx Internal Mode Ringdowns

14.3737 kHz; Q = 1.2e+79.675 kHz; Q ~ 6e+5


LIGO laser

! Nd:YAG

! 1.064 µµµµm

! Output power > 8W in TEM00 mode


Commissioning configurations

! Mode cleaner and Pre-Stabilized Laser! 2km one-arm cavity ! short Michelson interferometer studies

! Lock entire Michelson Fabry-Perot interferometer

“First Lock”


Why is Locking Difficult?

One meter, about 40 inches

Human hair, about 100 microns000,10÷

Wavelength of light, about 1 micron100÷

LIGO sensitivity, 10-18 meter000,1÷

Nuclear diameter, 10-15 meter000,100÷

Atomic diameter, 10-10 meter000,10÷

Earthtides, about 100 microns

Microseismic motion, about 1 micron

Precision required to lock, about 10-10 meter


Laserstabilization

IO

10-WattLaser

PSL Interferometer

15m4 km

Tidal Wideband

! Deliver pre-stabilized laser light to the 15-m mode cleaner• Frequency fluctuations• In-band power fluctuations• Power fluctuations at 25 MHz

! Provide actuator inputs for further stabilization• Wideband• Tidal

10-1 Hz/Hz1/2 10-4 Hz/ Hz1/2 10-7 Hz/ Hz1/2


Prestabalized Laserperformance

! > 18,000 hours continuous operation

! Frequency and lock very robust

! TEM00 power > 8 watts

! Non-TEM00 power < 10%


LIGO“first lock”

signal

LaserX Arm

Y Arm

Composite Video


Watching the Interferometer Lock

signalX Arm

Y Arm

Laser

X arm

Anti-symmetricport

Y arm

Reflected light

2 min


Lock Acquisition


Engineering Test Run2 weeks – Jan 02

PRELIMINARY

2 Km Hanford

4 Km Livingston

4 Km Hanford


Strain Spectra for E7comparison with design sensitivity

LIGO I Design


Detecting the Earth Tides Sun and Moon


Run Plancommissioning & data taking

! • Science 1 run: 13 TB data “Upper Limits”» 29 June - 15 July» 2.5 weeks - comparable to E7» Target sensitivity: 200x design

! • Science 2 run: 44 TB data “Upper Limits”» 22 November - 6 January 2003» 8 weeks -- 15% of 1 yr» Target sensitivity: 20x design

! • Science 3 run: 142 TB data “Search Run”» 1 July 2003 -- 1January 2004» 26 weeks -- 50% of 1 yr» Target sensitivity: 5x design


LIGOconclusions

! LIGO construction complete

! LIGO commissioning and testing ‘on track’

! Engineering test runs underway, during period when emphasis is on commissioning, detector sensitivity and reliability. (Short upper limit data runs interleaved)

! First Science Search Run : first search run will begin during 2003

! Significant improvements in sensitivity anticipated to begin about 2007

Documents

LIGOBCBAct/talks02/Ph... · LHC ENERGY FRONTIER LHC Upgrades VLHC Linear Collider CLIC Muon Collider NuMI/MINOS LEPTON FLAVOR PHYSICS Neutrino Superbeam Neutrino Factory BaBar & BELLE