Fig. 1. Schematic of space-based gravitational wave detector constellations
[13] Fig. 2. Schematic of low-noise MOPA laser
Fig. 3. Schematic of NPRO
Fig. 4. HSL prototype for NGGM at NPL laboratories
Fig. 5. Delivered m-NPRO packages and photo of the baseline fiber amplifier
Fig. 6. RIN and frequency noise of fiber laser and NPRO
Fig. 7. RIN and frequency noise of PW-ECL and NPRO
Fig. 8. Schematic layout and photograph of the micro-integrated PW-ECL
Fig. 9. The first prototype of a laser for LISA
Fig. 10. Schematic diagram of I2-stabilized laser for DECIGO
Fig. 11. Schematic diagram of fiber amplifier for DECIGO
Fig. 12. DBR laser head and schematic of the internal structure for Tianqin-1 mission
Fig. 13. Principle diagram of laser source for Taiji-1 satellite
Fig. 14. Schematic of suppressing the intensity noise based on optoelectronic feedback control
Fig. 15. Schematic of the experimental setup and measurement of the RPN
Fig. 16. Low-noise laser developed by Tsinghua University
Fig. 17. Schematic of the PDH laser frequency stabilization
Fig. 18. Frequency noise spectral density between the PDH and the molecular iodine
Mission | Armlength | Frequency range | Strain sensitivity | Operation orbit | Lunch time |
---|
DECIGO | 1.0×103 km | 0.1 Hz~10 Hz | 10-23/Hz1/2 | Heliocentric | 2030 | LISA | 2.5×106 km | 1 mHz~1 Hz | 10-20/Hz1/2 | Heliocentric | 2034 | Taiji | 3.0×106 km | 0.1 mHz~1 Hz | 10-20/Hz1/2 | Heliocentric | 2033 | TianQin | 1.7×105 km | 0.1 mHz~1 Hz | 10-20/Hz1/2 | Geocentric | 2035 |
|
Table 1. Design parameters for space-based gravitational wave detectors
Missions | Laser type | Wavelength/nm | Power/W | Power stability/Hz-1/2 | Frequency stability/(Hz·Hz-1/2) |
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DECIGO | MOPA | 515 | 10 | 1×10-8@1 Hz | 1 @1 Hz | LISA | MOPA | 1 064 | 2 | 2×10-4@0.1 mHz~1 Hz | 30 @10 mHz | Taiji | MOPA | 1 064 | 2 | 10-4@0.1 mHz~1 Hz | 30 @0.1 mHz~1 Hz | TianQin | MOPA | 1 064 | 4 | 2×10-4@1 mHz~1 Hz | 10 @10 mHz |
|
Table 2. Key parameters of low-noise lasers for space-based gravitational wave detector