lcgt project status n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
LCGT Project Status PowerPoint Presentation
Download Presentation
LCGT Project Status

Loading in 2 Seconds...

play fullscreen
1 / 26

LCGT Project Status - PowerPoint PPT Presentation


  • 105 Views
  • Uploaded on

LCGT Project Status. EGO-ICRR Meeting 4 October 2011 @ University of Tokyo Seiji Kawamura (ICRR). Objectives of LCGT. Detect gravitational waves together with Virgo and LIGO for the first time Establish Gravitational W ave Astronomy

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'LCGT Project Status' - tevy


Download Now An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
lcgt project status

LCGT Project Status

EGO-ICRR Meeting

4 October 2011

@ University of Tokyo

Seiji Kawamura (ICRR)

objectives of lcgt
Objectives of LCGT
  • Detect gravitational waves together with Virgo and LIGO for the first time
  • Establish Gravitational Wave Astronomy
  • Establish multi-messenger observations between GWs and Electromagnetic waves/Cosmic rays
expected gw sources
Expected GW sources
  • Neutron star binary coalescence
    • correlation with GRB
  • Black hole binary coalescence
  • Black hole ringdown
  • Supernovae
    • Correlation with Neutrino
  • Pulsar
  • Early universe
  • Unknown
key features of lcgt
Key Features of LCGT

Underground Cryogenic mirrors/

suspensions

These are essential features for the 3rd GW detectors such as ET.

slide5

Underground Site

We are here.

advantage of underground site
Advantage of Underground Site
  • Not only linear effect
  • But also nonlinear effect

Smaller low-frequency motion of mirror

 Lower gain of control system necessary

 Lower in-band noise imposed by control system

sensitivity comparison
Sensitivity Comparison

20m prototype was moved from Tokyo to Kamiokain 1998.

@ Tokyo

Displacement spectrum m/RHz

@ Kamioka

Hz

cryogenics system
Cryogenics System

Inner Wall (8K)

Platform (14 K)

Upper Mass (15 K)

Mirror (20 K)

Flexible Heat Link

Baffles Thermal Shield

Pulse Tube Cryocooler

sapphire mirror
Sapphire Mirror

Sapphire mirror at 20 K

  • Transparent at 1064 nm
  • Low thermal noise
    • High Quality factor at 20 K
  • Low thermoelastic noise
    • High thermal conductivity at 20 K
    • Low thermal expansion coefficient at 20 K
seismic attenuation system sas for lcgt
Seismic Attenuation System (SAS) for LCGT

Tunnel (2nd floor)

Chamber

Inverted Pendulum

GAS Filter

(invented by DeSalvo)

Tunnel (1st floor)

Chamber

Mirror

SAS was designed based on the Virgo SA.

external review
External Review
  • Feb. 28 – Mar. 4, 2011 @ICRR
  • Almost all the subsystems were reviewed
  • Review items:
    • Requirements
    • Design
    • Schedule
    • Prototype test plan
    • Etc.
report
Report
  • We obtained report on March 10, 2011
  • 12 pages
  • Consists of:
    • Executive summary
    • Recommendations to management
    • Recommendations to each subsystem
executive summary 1
Executive Summary 1

focusing interferometer noise optimization (and corresponding astrophysics goals) to capitalize on the unique advantages of the underground site and cryogenic operation

Bandwidth working group (led by K. Somiya) was convened to discuss this. It turned out that shifting the frequency band lower will not gain significant advantages.

executive summary 2
Executive Summary 2

establishing a strong Systems group to insure subsystem interfaces and design goals are properly distributed, and sufficient, but not excessive

Systems Engineering Office has been created.

executive summary 4 5
Executive Summary 4 & 5

wherever feasible, employing (or at least starting with) established, tested component designs requiring minimal modification;

proceeding rapidly toward integrated system testing (e.g., through enhanced scope for the iLCGT phase) to minimize the risk of late surprises

Roadmap working group (led by M. Ando) was convened to discuss this. We decided to employ a simple isolation system for iLCGTand meanwhile to develop SAS at the site.

program advisory board
Program Advisory Board
  • Jun. 21 – 22, 2011 @ICRR
  • Review items:
    • Management
    • Schedule
    • Design
    • Etc.
report1
Report
  • We obtained report on August 30, 2011
  • 6 pages
  • Consists of responses to the following points:
    • If the management and organization of the project are OK.
    • If the construction status & plan are OK.
    • If the scientific goals are reasonable.
    • What should be improved in the LCGT construction?
    • Whatever the advice for this project.
  • Actions:
    • We have started discussing possible actions to the report.
schedule of lcgt
Schedule of LCGT

2011

2012

2013

2014

2015

2016

2017

bLCGT

Observation

iLCGT

organization of lcgt
Organization of LCGT

LCGT Council

Director

(Kajita)

Program

Advisory Board

Systems Engineering Office

(Kawamura, Ando, Miyoki, Somiya)

Executive Committee

( Nakatani (PM), Kuroda, Ohashi, Kawamura, Mio, Ando)

Executive Support

DATA Analysis

Tunnel

Facility

Vacuum

Vibration isolation

Cryogenics

Mirror

Main interferometer

Digital system

Analog Electronics

Input/Output Optics

Laser

Auxiliary optics

Geophysics Interferometer

Subsystem

joining the worldwide gw network
Joining the worldwide GW network

GEO-HF

Advanced LIGO

LCGT

Advanced Virgo

LCGT will join the world network of gravitational wave detectors, with full reciprocal sharing of data with the Virgo collaboration, the LIGO Collaboration and the GEO600 Collaboration at a time determined by mutual agreement of all parties - LCGT, Virgo, LIGO, and GEO.

lcgt in network

L/H+L/L+V+LCGT

50%

L/H+L/L+V 50%

LCGT in network
  • LIGO(H)+LIGO(L)+Virgo+LCGT
  • Max sensitivity (M.S.): +13%
  • Coverage at 0.5 M.S.: 100%
  • 3 detector duty cycle: 82%
  • LIGO(H)+LIGO(L)+Virgo
  • Coverage at 0.5 M.S.: 72%
  • 3 detector duty cycle: 51%

B. F. Schutz