大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象@宇宙線研究所共同利用研究会「ガンマ線天文学〜日本の戦略〜」2010/11/16神田展行（大阪市立大学） Nobuyuki Kanda (Osaka City Univ.) LCGT collaboration + GW&EM followup working group 11

Gravitational Waves
● What ? ● Why ? • Sources
LCGT
• Overview • Construction Schedule • Detection Range for GWs
Counterpart / Follow-up observations
• Possible Sources • Science (Physics) outcome
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

R p v 1 ーK T μν 5  9μv R  : Curved space-time Propagation of the distortion ● --> Waves !
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGT
Gravitational Waves Einstein Equation： R v | 1 I μν R  -K T μν In case of small perturbation ‘h’, a wave equation is derived as;
1 p2 c2 百t2 --> Wave of strain ‘h’ Gravitational Wave • light speed • transverse • quadrupole (tidal force)
0 0 0 0 (0 0 0 0 0 1 0
h+ =
h × h
11 0 0 0
0
0 0 0 0 0
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
4
Tidal force on masses h+ cos(k・x — 2πfgwt) 0 0 0 0 0 0 0
0 1 (0 0 ( ) 0 0 0ノリハリバハメタイタイタイタイタイ/    /    /    /    /アア メ  メ  メメメ メ メ メ  ↓  ↓  ↓ ,  , ・・・・・・・・・・・・・・・・・ /  /  /  /  /  /  /  /  /
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
Physics TEST of Einstein’s general relativity in strong field. Astronomy, Astrophysics • Radiation from compact / massive objects. Physics of black-hole, neuron star, supernovae, etc... --> Gravitational Wave Astronomy
Cosmology
• Cosmic background radiation of GW • POP-III stars, star formation, etc... Physics on early universe.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

Event like:
• Compact Binary Coalescence neutron star (NS) black-hole (BH) • Supernovae • BH ringdown
Continuous waves:
● Pulsar rotation • Binaries
Stochastic Background
• Early universe (i.e. Inflation) • Cosmic string (& Unknown sources...)
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
• small amplitude • Waveform can determine masses and absolute amplitude. --> ‘standard candle’ amplitude ~10-24 for NS-NS at 200Mpc away! (in frequency spectrum, ~10-22~-23 [/./Hz] @10~100Hz)
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
9 • small amplitude • Waveform can determine masses and absolute amplitude. --> ‘standard candle’ • small amplitude • Waveform can determine masses and absolute amplitude. -> ‘standard siren

日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

Interference cos( 2 pi  2dL /lambda) Michelson Interferometer
日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

Free mass --> suspended mirror To integrate strain ‘h’ --> long baseline arms.   h δl Limited size --> Folding arms / Storage cavity Against noises --> • high power laser • Cooling • etc..
Underground • in Kamioka, Japan Silent & Stable environment 3km baseline Cryogenic Mirror • 20K • saffhire substrate Plan 2010  : construction start now! 2014  : first run in normal temperture 2017- : observation with cryogenic mirror 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
K Kuroda¹, I Nakatani¹, M Ohashi¹, S Miyoki¹, T Uchiyama¹, O Miyakawa¹, H Ishiduka¹, K Agatsuma¹, T Saito¹, M-K Fujimoto², S Kawamura², R Takahashi², D Tatsumi², A Ueda², M Fukushima², H Ishizaki², Y Torii², S Sakata², A Nishizawa², K Kotake², Y Sekiguchi², A Yamamoto³, Y Saito³, T Haruyama 3 , T Suzuki 3 , N Kimura 3 , T Tomaru 3 , K Ioka 3 , K Tsubono , Y Aso , K Ishidoshiro , K Takahashi , W Kokuyama , K Okada , S Kawara , N Matsumoto , F Takahashi , A Taruie , J Yokoyama , K Ueda , H Yoneda , K Nakagawa ", M Musha ", N Mio ", S Moriwaki ", N Omae ", T Ogikubo , Y Tokuda , A Araya , A Takamori , K Izumi , N Kanda 9 , K Nakao 9 , S Sato 10 , S Telada 11 , T Takatsuji 11 , Y Bito¹¹, S Nagano¹², H Tagoshi¹³, T Nakamura¹¹, N Seto¹¹, M Ando 14 , M Sasaki 15 , M Shibata 15 , T Tanaka 15 , N Sago 15 , E Nishida 16 , Y Wakabayashi 16 , T Shintomi 7 , H Asada 18 , Y Itho 19 , T Futamase 19 , K Oohara 20 , M Saijo 21 , T Harada 21 , S Yamada 22 , N Himemoto²³, H Takahashi²¹, Y Kojima²³, K Uryu²³, K Yamamoto 27 , F Kawazoe 27 , A Pai 7 , K Hayama 27 , Y Chen 28 , K Kawabe 28 , K Arai 8 , K Somiya 8 , M.E.Tobar 29 , D Blair 29 , J Li 29 , C Zhao 29 , L Wen 29 , J Warren 30 , H Nakano 31 , R Stuart 32 , M Szabolcs 33 , K K Kokeyama 34 , Z-H Zhu 35 , SDhurandhar 36 , S Mitra 36 , H Mukhopadhyay 36 , V Milyukov 37 , L Baggio 38 , Y Zhang 39 , J Cao 40 , C-G Huang 41 , W-T Ni 22 , S-S Pan 43 , S-J Chen 43 , K Numata 44 o D 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
Re-design is under going ;for example ---removing the 180 m long mode cleaner cavity ---flexibility change of possible adoption of detuned RSE
** for reducing noise due to a residual gas effect ** for maintenance minimizing 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
A)SAS(GASF 3stage)+cryo-sus: FM1、FM2、EM1、EM2 B)SAS(GASF 2stage)+non-cryo: EM、FM、MC2F、MC2E C)STACK+2stages: MC1F、MC1E、MMT、PD A B
18
NS-NS Detection Range (sky average) (optimal direction) Expected # of events Probability of detection at least one event 90% for 1st event 123 Mpc 281 Mpc 6.9 +17.3-5.5 events/year 99.9 % for one year 4 months u 2010/11/16 「大型低温重力波
construction (on-site) observation The construction/observation plan is in 2 stages: In 2014, non-cryogenic observation. Full observation with the cryogenic system, at the beginning of 2017.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

https://gwic.ligo.org/ https://gwic.ligo.org/roadmap/Roadmap_100814.pdf
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
LIGO x2 + VIRGO 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンFig. 4.3 – Chandra image of the Galactic Center (left). Illustration of massive stars formed from a large disk of gas 'around Sagittarius A*, the Milky Way's central black hole (illustration on right). Credit:  X-ray: NASA/CXC/MIT/ ルギF.K.Baganoff et al.; Illustration; NASA/CXC/M.Weiss e the story of the story
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

「
• Before merger, 10% of final S/N before 1 min. 40% before 10 sec. for S/N>8, 1 min --> 25Mpc 10 sec --> 80Mpc (*optimal direction.) Forecast by GW is not easy, however it is not impossible in principle. Even it is not a forecast, faster alert is useful for observe the transient behavior.
Since GW observation’s error box is wide, it will require large F.O.V. for gamma/X telescopes.角度分解能(1.4,1.4)Msolar, @200Mpcの場合LIGO-L1, VIRGO, LCGT 3台の場合方向, inclination角,偏極角に依存する.これらを乱数で与える. ISCOまで積分:平均S/N (p)平均角度分解能8.2から8.9 （各検出器で）長軸7.6度,短軸0.99度(3台のとき)重力波周波数50Hzで打ち切り:平均S/N(p) 2.5から2.8 （各検出器で）平均角度分解能長軸123度,短軸13度(3台のとき)短軸by H.Tagoshi 「ガンマ線天文字〜日本の戦略〜」2010/11/16    '大型低温重力波望遠鏡LCGTで探る高エネルキー天体現象」
lf beaming of GRB is about 0.2 rad, a chance is once for 30 times. S/N for GW event VS. distance to the source GRB chance probability , when GW is detected.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギ

Fig. 1. — The IPN3 (IPN3 2007) (y-ray) error box overlaps with the spiral arms of the Andromeda galaxy (M31). The inset image shows the full error box superimposed on an SDSS ( Adelman-McCarthy et al. 2006 ; SDSS 2007 ) image of M31. The main figure shows the overlap of the error box and the spiral arms of M31 in UV light ( Thilker et al. 2005 ). GRB 070201, this distance was 35.7 Mpc and 15.3 Mpc for burst whose electromagnetically determined sky position is coincident with the spiral arms of the Andromeda galaxy (M31). Possible progenitors of such short hard GRBs include mergers of neutron stars or a neutron star and black hole, or soft γ-ray repeater (SGR) flares. These events can be accompanied by gravitational-wave emission. No plausible gravitational wave candidates were found within a 180 s long window around the time of GRB 070201. This result implies that a compact binary progenitor of GRB 070201, with masses in the range 1 Mo < m 1 < 3 Mo and 1 Mo < m 2 < 40 Mo , located in M31 is excluded at > 99% confidence. Indeed, if GRB 070201 were caused by a binary neutron star merger, we find that D < 3.5 Mpc is excluded, assuming random inclination, at 90% confidence. The result also implies that an unmodeled gravitational wave burst from GRB 070201 most probably emitted less than 4.4 × 10 * M c ² (7.9×10 50 ergs) in any 100 ms long period within the signal region if the source was in M31 and radiated isotropically at the same frequency as LIGO's peak sensitivity (f ≈ 150 Hz). This upper limit does not exclude current models of SGRs at the M31 distance. It was NOT CBC. (excluded 99%) Astrophys.J.681:1419-1428,2008   LIGO collab. 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
GW emissions from different phases carry out different informations. In case of CBC, methods of waveform prediction are also different.
Inspiral (Post-Newton)
•  frequency development  ---> mass of stars, and absolute amplitude •  measured amplitude ---> distance from the earth •  polarization ---> inclination angle of binary orbit
Merger (Numerical Relativity)
•  depends of many (initial/boundary) conditions ---> Complex information of stars , e.g. radius, viscosity, EOS ...
Ringdown (Perturbation)
BH quasi-normal mode •  frequency ---> mass •  decay time ---> spin (Kerr parameter) What a fruitful source is it !
Supernova will emit GW also in various phase of its development. core bounce convection formation of proto-neutron star • g-mode oscillation neutrino emission accretion • cf: SASI (standing-accretion-shock instability)
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

by K.Kotake SASI 1秒(？) ＞数時間数ミリ秒Oが陽菊ヨ力成食母ゆ無Subaru Tanaka+06(属光Maeda+06
GW • Typical Range < 1Mpc • Typical Angular Resolution ~ 3 degree Neutrino (Super-Kamiokande) • Typical Range ~ several 100 kpc • Typical Angular Resolution at 10kpc C.L.68% (=1 sigma) --> 4.7 degree C.L.95% (=2 sigma) --> 7.8 degree Angular distribution of vcp → ne+ events (green) and elastic scattering events ve → ve − (blue) of one simu- lated SN. Phys.Rev. D68 (2003) 093013 / arXiv:hep-ph/0307050v2   l /degree R. Tomas, D. Semikoz, G. G. Raffelt, M. Kachelriess, A. S. Dighe 「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」 Magnetor Magnetar Super strongly magnetized neutron star B² R³ Magnetic energy 210円GM² / R* Gravitational energy   B 1016G Deformation of neutron stars 1. Precession 2. GW source (e.g., GRB) 3. Influence on the oscillation Equilibrium of magnetized stars
We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR 1900+14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3 X 1045 and 9 X 1052 erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models. FIG. 1 (color online). its for the entire SGR burst sample for various circularly or linearly polarized RDs (RDC/RDL) and white noise burst (WNB) signals. The limits shown in Table I, for the giant flare and the 060806 event, are indicated in the figure by circles and diamonds, respectively. PRL 101, 2111102 (2008), LIGO collab.
Radiometry Filter λ H(f) :  GW PSD P i Simulation by Y.Okada Stochastic GW (convolution of point sources, random phases) will be able to detetect.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」
Other Possible Sources Cusp/Kink of Cosmic String LMXB (Wagoner star) SMBH, IMBH Pulser (Continuous,  Pulser glitch)
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

GW obs.
• fast processing event searches • reliable alert (low false alarm rate, high efficiency) ● trigger data-base
EM / high energy particle counterparts
• larger field of view / quick response ● sky coverage GW will be detect from whole sky.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」

LCGT
has been funded partially, and the construction start now! (First run will be 2014.) Full observation will start at late 2016 or early 2017 with world network of GW observatories.
Mutually Follow-up
observations between GW and electromagnetic or high energy particles or both is expected. Counterpart information will make appear the inside/structure/ development of high energy astrophysical objects.
「ガンマ線天文学〜日本の戦略〜」2010/11/16  「大型低温重力波望遠鏡LCGTで探る高エネルギー天体現象」