YKIS2018a Symposium General Relativity - The Next Generation - KAGRA and B-DECIGO Masaki Ando (Univ. of Tokyo / NAOJ) YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
First Detection of GW ・ On Feb. 11 th , 2016, LIGO announced first detection of gravitational wave. The signal was from inspiral and merger of binary black hole at 410Mpc distance. Opens a new field of ‘ GW astronomy ’. Courtesy Caltech/MIT/LIGO Laboratory YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Mergers of Binary Black Hole ・ 2nd: GW151226 (2016.6 announce) ・ 3rd: GW170104 (2017.6.2 announce) ・ 4th: GW170814 (2017.9.27 announce) ・ 5th: GW170608 (2017.11.15 announce) Mergers of binary black holes would be common events in the universe. http://ligo.org/detections/GW170608 YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Merger of Binary Neutron Stars ・ On Oct.16 th , 2017, LIGO-VIRGO collaboration announced the first detection of gravitational-wave signal from merger of binary neutron stars ・ The signal was detected on August 17 th , 2017. Named GW170817. ・ Source Localization ~30deg 2 Courtesy Caltech/MIT/LIGO Laboratory YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
・ EM counterpart was observed for the first time in GW170817. ・ New knowledge * Origin of SGRB. * Origin of heavy elements in the universe. * EoS of neutron star * Fundamental physics and cosmology: speed of GW, Hubble’s constant, …. ApJL 848 L12 (2017) YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
After the First Detections ... ・ The first GW (and EM counter part) detections demonstrated new possibilities by GW astronomy, and also showed new mysteries, such as the origin of heavier mass ( 30𝑁 ⨀ ) BBH. ・ Network of 2 nd -gen. GW antennae (aLIGO, AdVIRGO, KAGRA, LIGO-India) will be formed in several years. ・ Two ways after that for Astronomy and Cosmology: - 3 rd – gen. ground-based GW antennae (ET , CE). - Space GW antennae (LISA, DECIGO , ASTROD,…). YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA and DECIGO B-DECIGO (~2020s) KAGRA (~2019/20) Space observatory Terrestrial Detector Low frequency sources High frequency events Target: GW detection Target: GW astronomy YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA ( かぐら ) - Ground-based GW antenna in Japan- YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA KAGRA ( かぐら ) Large-scale Cryogenic Gravitational-wave Telescope 2 nd generation GW detector in Japan Large-scale Detector Baseline length: 3km High-power Interferometer Cryogenic interferometer Mirror temperature: 20K Underground site Kamioka mine, 1000m underground YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Collaboration KAGRA collaboration: ~300 members from ~60 Universities or Institutes Designed by S. Miyoki YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
International GW Network International network by 2 nd – gen GW antennae. GW astronomy (Detection, Parameter estimation, …) aLIGO (USA) 4km x 2 140 100 KAGRA (JPN) baseline 3km 20 20 LIGO-India GEO-HF (GER-UK) Adv.VIRGO (ITA-FRA) project approved baseline 600m baseline 3km YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Importance of Sky Localization ・ For GW astronomy, parameter estimation of the source is important. In particular, sky localization is critical for identification of EM counterapart. ・ In GW170817, the sky position was localized with ~30deg 2 error by 2 LIGO + 1 VIRGO detectors. ~20 galaxies in this region. Credit: LIGO/Virgo/NASA/Leo Singer Credit: Sarah Wilkinson / LCO (Milky Way Image: Alex Mellinger) (Taken from https://youtu.be/wnwMhvdDcfI) YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Source Localization LIGO: 1200deg 2 LIGO: 850deg 2 LIGO-VIRGO: 30deg 2 LIGO: 600deg 2 LIGO-VIRGO: 60deg 2 YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Antenna Pattern of GW Detector Antenna Pattern An Interferometric GW antenna has … * Good sky coverage * Poor angular resolution Difficult to determine the source sky position with single antenna. YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
International Network for Astronomy Animation : S. Kawamura (ICRR) Multiple Detector Identify the source by the arrival-time difference (and also signal strength) YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Sky Localization H: LIGO- ‐Hanford L: LIGO- ‐Livingston V: Virgo, K: KAGRA I: LIGO-Indea From presentation by H. Tagoshi J.Veitch+, PRD85, 104045 (2012) Tagoshi+ (2014) S.Fairhaurst CQG 28(2011) 105021 Adding KAGRA to the network (aLIGO + adv. VIRGO) Improvement of angular resolution by 3-4 times. YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Features ・ Large laser interferometer : Baseline 3km ・ Underground site : stable environment. ・ Cryogenic mirrors : thermal noise reduction Original advanced technologies in KAGRA, which also gives prospects for 3G detectors YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Site Underground site at Kamioka, Gifu prefecture Facility of the Institute of Cosmic-Ray Research (ICRR), Univ. of Tokyo. Underground Research Facility Neutrino : SK, Kamland <1hour by car from Toyama Dark matter : XMASS city or Toyama airport Gravitational Wave : CLIO, KAGRA Geophysics : Strain meter Kamioka Tokyo Osaka Map by Google YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Photos Office XMASS(dark matter) CLIO KamLAND(neutrino) (GW) Super Kamiokande (neutrino) KAGRA YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
iKAGRA Installation and Test Run ・ Tunnel and Facility are almost ready. iKAGRA (simple Michelson configuration) test run for 3weeks in spring 2016. ・ Currently, upgrading for full configuration. Type- Bp’ suspension for PR3 (Feb. 25 th , 2016) 3-km Tunnel and Beam Duct (Photo by S. Miyoki) YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Optical Design Input/Output Optics Main Interferometer - Beam Cleaning and stab. ETM - 3 km arm cavities - Modulator, Isolator - RSE with power recycling - Fixed pre-mode cleaner DC readout scheme Y-arm cavity - Suspended mode cleaner - Cryogenic test masses Length 26 m, Finesse 500 Sapphire, 20K - Output MC ‘Type - A’ vibration isolator - Photo detector Cryostat + Cryo-cooler - Room-temp. Core optics ITM (BS, PRM, SEM, …) Power Input 78 W 800 W BS ETM ITM PRM ~180 W Bench Power ~380 kW Laser 26-m MC X-arm cavity Power-recycling Length 3,000 m Gain ~11 Finesse 1,530 Laser Source RSE: (Resonant sideband Extraction) - Wavelength 1064 nm Signal-band Gain ~15 SEM - Output power 180 W Detuned RSE (Variable tuning) High-power MOPA YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Photos Vibration Isolation YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Photos Cryogenic Suspension YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
KAGRA Photos Sapphire Mirror: Diameter 22cm, Thickness 15cm YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Sensitivity Comparison KAGRA YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
Observation Scenario KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration: arXiv:1304.0670, Submitted to LLR (2017) ~3-months (2020.1 - 3) ~6-months (2021.1 - 6) Design : From 2022.1- Phase-3 Phase-1 Phase-2 Cryogenic RSE, 1-yr Cryogenic (PR)MI Cryogenic RSE commissioning after No sensitivity goal No sensitivity goal the first full operation YKIS2018a Symposium (Feb. 19th, 2018, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto)
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