The japanese space gravitational wave antenna decigo
This presentation is the property of its rightful owner.
Sponsored Links
1 / 14

The Japanese Space Gravitational Wave Antenna DECIGO PowerPoint PPT Presentation


  • 67 Views
  • Uploaded on
  • Presentation posted in: General

The Japanese Space Gravitational Wave Antenna DECIGO. TAUP2007 @Sendai, Japan Aug 11, 2007

Download Presentation

The Japanese Space Gravitational Wave Antenna DECIGO

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


The japanese space gravitational wave antenna decigo

The Japanese Space Gravitational Wave Antenna DECIGO

TAUP2007 @Sendai, Japan

Aug 11, 2007

Seiji Kawamura, Masaki Ando, Takashi Nakamura, Kimio Tsubono, Takahiro Tanaka, Ikkoh Funaki, Naoki Seto, Kenji Numata, Shuichi Sato, Nobuyuki Kanda, Takeshi Takashima, Kunihito Ioka, Kazuhiro Agatsuma, Tomotada Akutsu, Tomomi Akutsu, Koh-suke Aoyanagi, Koji Arai, Yuta Arase, Akito Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Motohiro Enoki, Yoshiharu Eriguchi, Masa-Katsu Fujimoto, Ryuichi Fujita, Mitsuhiro Fukushima, Toshifumi Futamase, Katsuhiko Ganzu, Tomohiro Harada, Tatsuaki Hashimoto, Kazuhiro Hayama, Wataru Hikida, Yoshiaki Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Feng-Lei Hong, Hideyuki Horisawa, Mizuhiko Hosokawa, Kiyotomo Ichiki, Takeshi Ikegami, Kaiki T. Inoue, Koji Ishidoshiro, Hideki Ishihara, Takehiko Ishikawa, Hideharu Ishizaki, Hiroyuki Ito, Yousuke Itoh, Shogo Kamagasako, Nobuki Kawashima, Fumiko Kawazoe, Hiroyuki Kirihara, Naoko Kishimoto, Kenta Kiuchi, Shiho Kobayashi, Kazunori Kohri, Hiroyuki Koizumi, Yasufumi Kojima, Keiko Kokeyama, WataruKokuyama, Kei Kotake, Yoshihide Kozai, Hideaki Kudoh, Hiroo Kunimori, Hitoshi Kuninaka, Kazuaki Kuroda, Kei-ichi Maeda, Hideo Matsuhara, Yasushi Mino, Osamu Miyakawa, Shinji Miyoki, Mutsuko Y. Morimoto, Tomoko Morioka , Toshiyuki Morisawa, Shigenori Moriwaki, Shinji Mukohyama, Mitsuru Musha, Shigeo Nagano, Isao Naito, Noriyasu Nakagawa, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi Nakasuka, Yoshinori Nakayama, Erina Nishida, Kazutaka Nishiyama, Atsushi Nishizawa, Yoshito Niwa, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Akira Okutomi, Kouji Onozato, Kenichi Oohara, Norichika Sago, Motoyuki Saijo, Masaaki Sakagami, Shin-ichiro Sakai, Shihori Sakata, Misao Sasaki, Takashi Sato, Masaru Shibata, Hisaaki Shinkai, Kentaro Somiya, Hajime Sotani, Naoshi Sugiyama, Yudai Suwa, Hideyuki Tagoshi, Kakeru Takahashi, Keitaro Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Takamori Akiteru, Tadashi Takano, Keisuke Taniguchi, Atsushi Taruya, Hiroyuki Tashiro, Mitsuru Tokuda, Masao Tokunari, Morio Toyoshima, Shinji Tsujikawa, Yoshiki Tsunesada, Ken-ichi Ueda, Masayoshi Utashima, Hiroshi Yamakawa, Kazuhiro Yamamoto, Toshitaka Yamazaki, Jun'ichi Yokoyama, Chul-Moon Yoo, Shijun Yoshida, Taizoh Yoshino


What is decigo

10-18

have moved

Above LISA band

10-20

will move

into TD band

10-22

10-24

What is DECIGO?

Deci-hertz Interferometer Gravitational Wave Observatory

(Kawamura, et al., CQG 23 (2006) S125-S131)

  • Bridges the gap between LISA and terrestrial detectors

  • Low confusion noise  Extremely high sensitivity

Terrestrial detectors (e.g. LCGT)

LISA

Strain [Hz-1/2]

DECIGO

Confusion Noise

10-4

102

100

104

10-2

Frequency [Hz]


Pre conceptual design

Pre-conceptual design

Differential FP interferometer

Arm length: 1000 km

Mirror diameter: 1 m

Laser wavelength:0.532 m

Finesse: 10

Laser power: 10 W

Mirror mass: 100 kg

S/C: drag free

3 interferometers

Arm cavity

Arm cavity

Laser

Mirror

Photo-

detector

Drag-free S/C


Why fp cavity

Shorten

arm length

Implement FP cavity

Radiation pressure noise f-2

Shorten

arm length

Shot noise f1

Shot noise

Implement FP cavity

FP cavity type

Better best- sensitivity

Why FP cavity?

Transponder type

(e.g. LISA)

Radiation pressure noise f-2

Shot noise f1

Strain

Shot noise

Transponder type

(e.g. LISA)

Frequency


Drag free and fp cavity compatible

S/C I

S/C II

Drag free and FP cavity: compatible?

Mirror


Fp cavity and drag free compatible

S/C I

S/C II

FP cavity and drag free : compatible?

Relative position between mirror and S/C

Local sensor

Mirror

Thruster

Thruster


Drag free and fp cavity compatible1

No signal

mixture

S/C I

S/C II

Drag free and FP cavity: compatible?

Relative position between mirror and S/C

Local sensor

Mirror

Thruster

Thruster

Actuator

Interferometer output (GW signal)


Orbit and constellation preliminary

Orbit and constellation (preliminary)

Earth

Correlation for stochastic background

Record disk

Sun

Increase angular resolution


Goal sensitivity and science

BH binary

(1000 M◎ z=1)

Coalescence

5 years

3 months

NS binary (z=1)

Inflation

Coalescence

Goal Sensitivity and Science

10-19

10-20

10-21

10-22

10-23

10-24

10-25

10-26

Formation of Super-massive BH

1 unit

Radiation pressure noise

Strain [Hz-1/2]

Acceleration of Universe

Dark energy

Shot noise

Correlation

(3 years)

Verification of inflation

10-3 10-2 10-1 1 10 102 103

Frequency [Hz]


Requirements

Requirements

  • Acceleration noise should be suppressed below radiation pressure noise

    • Force noise: DECIGO = LISA/50

      (Acceleration noise in terms of h: 1, Distance: 1/5000, Mass: 100)

    • Fluctuation of magnetic field, electric field, gravitational field, temperature, pressure, etc.

  • Sensor noise should be suppressed below shot noise.

    • Phase noise: DECIGO = LCGT×10

      (Sensor noise in terms of h: 1, storage time: 10)

    • Frequency noise, intensity noise, beam jitter, etc.

  • Thruster system should satisfy range, noise, bandwidth, and durability.


Roadmap

Roadmap

R&D

Fabrication

R&D

Fabrication

R&D

Fabrication

DICIGO Pathfinder (DPF)

 Ando’ s talk

Pre-DECIGO

DECIGO


Interim organization

Interim organization

PI: Kawamura (NAOJ)

Deputy: Ando (Tokyo)

Executive Committee

Kawamura (NAOJ), Ando (Tokyo), Seto (NAOJ), Nakamura (Kyoto), Tsubono (Tokyo), Tanaka (Kyoto), Funaki (ISAS), Numata (Merryland), Sato (NAOJ), Kanda (Osaka city), Takashima (ISAS), Ioka (Kyoto)

Pre-DECIGO

Sato (NAOJ)

Detector

Numata (Merryland)

Ando (Tokyo)

Science, Data

Tanaka (Kyoto)

Seto (NAOJ)

Kanda (Osaka city)

Satellite

Funaki (ISAS)

Design phase

DECIGO pathfinder

Leader: Ando (Tokyo)

Deputy: Takashima (ISAS)

Mission phase

Detector

Ando (Tokyo)

Laser

Ueda (ILS)

Musya (ILS)

Housing

Sato (NAOJ)

Drag free

Moriwaki (Tokyo)

Sakai (ISAS)

Thruster

Funaki (ISAS)

Bus

Takashima (ISAS)

Data

Kanda (Osaka city)


Current status

Current status

  • There are now 140 members from 50 institutes in DECIGO working group

  • Budget request (DECIGO R&D and fabrication of DPF, $20M, 6 years) was rejected.

  • We will submit budget request (R&D for DECIGO and DP, $10M, 5-6 years) this year again.

  • DPF working group was formally approved by JAXA/ISAS.

  • Budget request (R&D for DPF, $65K, 1 year) to JAXA/ISAS was approved.


Summary

Summary

  • DECIGO can not only bridge the gap between terrestrial detectors and LISA, but also open a very deep window at 0.1 – 10 Hz.

  • DECIGO will use FP arm cavity to further improve the sensitivity.

  • We have obtained some budget to initiate R&D for DPF.

  • We hope that we will obtain a bigger budget for DECIGO R&D, and that DPF mission will be approved soon!


  • Login