KAGRA Masatake OHASHI (ICRR) KAGRA 1 General outline of f KAGRA - - PowerPoint PPT Presentation

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KAGRA Masatake OHASHI (ICRR) KAGRA 1 General outline of f KAGRA - - PowerPoint PPT Presentation

Feb 28, 2024 274 likes •595 views

KAGRA Masatake OHASHI (ICRR) KAGRA 1 General outline of f KAGRA Pro roject KAGRA is 3km L-shaped underground laser interferometer with cryogenic mirrors Project framework ICRR hosts this project, and KEK and NAOJ cohost it to

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KAGRA

1 KAGRA

Masatake OHASHI (ICRR)

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General outline of f KAGRA Pro roject

Purpose of this project ・To understand astronomical phenomena like supernovae explosion and coalescence of binary compact stars with gravitational waves . Project framework ・ICRR hosts this project, and KEK and NAOJ co‐host it to construct KAGRA for gravitational wave astronomy

  • Univ. of Toyama also supports it.

2 KAGRA

KAGRA is 3km L-shaped underground laser interferometer with cryogenic mirrors

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KAGRA 3

Expected Scie ience wit ith Gravitational Waves

  • Binary black hole merger

Testing GR （QNM, No hair theorem, ．．．） Testing modified theory of gravity

  • BNS, BH-NS mergers

Relation to Gamma Ray burst Equation of state and internal structure Relation to r-process nucleosynthesis

  • Supernova explosions

Explosion mechanism

  • Test of polarization modes of GW
  • …

NS=Neutron star, BH=Black Hole

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Ultimate sensitivity of KAGRA

4 KAGRA

Duty factor: > 80% Inspiral range: 153 Mpc

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Two key features of f KAGRA

5 KAGRA

  • 1. KAGRA is constructed at underground site.
  • 2. KAGRA uses cryogenic mirrors.
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Seismic noise in in Kamioka Mine

6 KAGRA

Seismic noise is serious for GW detection. Underground site Is very quiet. So we selected underground site for KAGRA.

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Two key features of f KAGRA

7 KAGRA

  • 1. KAGRA is constructed at underground site.
  • 2. KAGRA uses cryogenic mirrors.
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Thermal noises

8 KAGRA

The sensitivity of interferometer around 100Hz is ordinarily limited by thermal noises.

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Mirror th thermal noise

9 KAGRA

Amplitude of thermal noise is proportional to

(T/Q)1/2

In general, Q (inverse number of magnitude of dissipation) depends on T (temperature). Sapphire Q becomes highest at low temperature. Therefore KAGRA mirrors use sapphire substrates and cooled to around 20K.

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SLIDE 10

Schedule of f KAGRA Pro roject

10 KAGRA

Calendar year 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 Project start Tunnel Excavation iKAGRA bKAGRA

First operation 3km Cryogenic Interferometer Final installation Commissioning and Observation

iKAGRA

3km Michelson Interferometer

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SLIDE 11
  • Construction budget

164MD

  • Operation budget

4.5MD/year

  • Upgrade budget in future over 10MD

(International budgets are necessary for it.)

KAGRA 11

KAGRA Budget

MD=108 Japanese Yen

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KAGRA Surface building (K (KAGRA started here)

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KAGRA office (since 2012, 140m2) KAGRA office building completed in March 2014 (340m2).

KAGRA office (since March, 2018, donated by Hida-city)

KAGRA office building Old Public Hall (Hida-city)

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Tunnel Excavation

13 KAGRA

3 corner stations are complicated because of tall towers for Vibration Isolation Systems.

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Dif ifficulty of f Underground sit ite

14 KAGRA

Springwater

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Spring water fr from wall surfaces

15 KAGRA

All surfaces were covered by waterproof sheets. It took 4 years to overcome spring water in the tunnel.

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Sil ilica Mir irrors for iK iKAGRA

16 大型低温重力波望遠鏡 KAGRA 16 KAGRA

iKAGRA TM (250mm dia) during figure measurement Beamsplitter(370mm dia) during coating characterization

Courtesy of LIGO We use a silica beam splitter for both iKAGRA and bKAGRA. We use sapphire substrates for bKAGRA and did not have silica substrates. By courtesy

  • f LIGO, we used iLIGO mirrors

for iKAGRA operation.

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iK iKAGRA Test Run

17 大型低温重力波望遠鏡 KAGRA 17 KAGRA

1st run： March 25 - 31, 2016 2nd run： April 12 - 25, 2016

Room temperature mirrors

Main purpose: Demonstration of 3km interferometer operation

  • 3km Michelson interferometer
  • Typical sensitivity
  • 1st run: 3 x 10-15 Hz-1/2 @ 100 Hz
  • 2nd run: 6 x 10-16 Hz-1/2 @ 100 Hz
  • Duty cycle ( = (lock time)/(total time) )
  • 1st run: 85.2 %
  • 2nd run: 90.4 %
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Completion of f four sapphire mir irrors

18 KAGRA

Advanced LIGO Hanford Advanced LIGO Livingston Advanced Virgo KAGRA

crystal polish coating Zygo Crystal systems & Shinkosha LMA

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Cry ryogenic mir irror suspension system

19 KAGRA

~ 14 m

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Cry ryogenic payload

20 KAGRA

type A

Cryogenic payload with mirror Mirror was cooled below 20K

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bKAGRA Phase-1 1

21 大型低温重力波望遠鏡 KAGRA 21 KAGRA

April 2016 – March 2018: Construction March – April 2018 : test run

Cryogenic mirrors Sensitivity ~ 3x10-17 Hz-1/2 at 100Hz We improved it by one order from iKAGRA Dark Noise

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X-arm (3 (3km Fabry-Perot Cavity) ) Test

22 KAGRA

  • X-arm test has completed
  • X-arm locked with the axillary (green) laser, then

successfully handed off to the IR laser

  • Noise budget

Enomoto, klog 7561

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In International Network for GW Observ rvation

23 KAGRA

GEO600 Advanced LIGO Hanford Advanced LIGO Livingston Advanced Virgo LIGO-India (anticipated) KAGRA

It is necessary to determine the direction of GW sources.

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Toward jo joining O3

24 KAGRA

acceleration

  • We have decided to accelerate KAGRA schedule to join O3.
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Jo Joint Run Planning wit ith LI LIGO and Vir irgo

25 大型低温重力波望遠鏡 KAGRA 25 KAGRA

KAGRA plans to join O3 in the fall of 2019.

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Current GW network + KAGRA

26 KAGRA

x denotes blind spots

  • S. Fairhurst, “Improved source localization with

LIGO India”, J. Phys.: Conf. Ser. 484 012007

LHO + LLO + Virgo LHO + LLO + Virgo + KAGRA

KAGRA improves the accuracy of the direction of the GW sources.

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KAGRA management stru ructure

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PI (T. Kajita) Vice-PI (M. Ohashi) Executive Office (EO) Chair: T. Kajita (PI) KAGRA Scientific Congress (KSC) Chair: H. Shinkai Systems Engineering Office (SEO) Chair: Y. Saito (PM) Data Analysis Committee (DAC) Chair: H. Tagoshi (Sub-groups) (Data Analysis WGs) Detector construction/commissioning Data analysis Collaboration with LIGO/Virgo

27 KAGRA

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KAGRA upgrade

O3 O4 O5?

Sensitivity upgrade with the existing instruments + Upgrade 1(?) Upgrade 2(?) Sensitivity upgrade with the existing instruments

  • It is almost the time to think about the future of KAGRA.
  • For discussing the KAGRA upgrade, KAGRA has formed the Future Planning

Committee (FPC) under KSC.

  • Following the recommendation of the FPC, SEO will decide the plan to install

the upgrade into the KAGRA interferometer.

  • As a guideline, the research group which plans the upgrade should have the

responsibility to install the upgrade into KAGRA including the responsibility

  • n the budget.

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(KAGRA needs the upgrade money from another countries.)

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KAGRA Observ rvatory ry as an In International re research center

29 KAGRA

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Summary

  • In the spring of 2019, we completed the

construction phase and move on to the commissioning phase. KAGRA plans to join O3 in the fall of 2019.

30 30 KAGRA