Cryogenically cooled ultra low vibration silicon mirrors for gravitational wave observatories

Shapiro, B.; Adhikari, R. X.; Aguiar, O. D.; Bonilla, E.; Fan, Danyang; Gan, Litawn; Gomez, Ian; Khandelwal, Sanditi; Lantz, B.; MacDonald, T.; Madden-Fong, D. x.

doi:10.1016/j.cryogenics.2016.12.004

Cited by 26 publications

(19 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The cryogenic design concept for LIGO Voyager is discussed in [131]. The test masses are maintained at 123 K through radiative cooling, as illustrated in Figure 16.…”

Section: A Cryogenicsmentioning

confidence: 99%

A cryogenic silicon interferometer for gravitational-wave detection

Adhikari¹,

Aguiar²,

Arai³

et al. 2020

Class. Quantum Grav.

Self Cite

168

110

View full text Add to dashboard Cite

The detection of gravitational waves from compact binary mergers by LIGO has opened the era of gravitational wave astronomy, revealing a previously hidden side of the cosmos. To maximize the reach of the existing LIGO observatory facilities, we have designed a new instrument able to detect gravitational waves at distances 5 times further away than possible with Advanced LIGO, or at greater than 100 times the event rate. Observations with this new instrument will make possible dramatic steps toward understanding the physics of the nearby universe, as well as observing the universe out to cosmological distances by the detection of binary black hole coalescences. This article presents the instrument design and a quantitative analysis of the anticipated noise floor. • Quantum noise will be reduced by increasing the optical power stored in the arms. In Advanced LIGO, the stored power is limited by thermally induced wavefront distortion effects in the fused silica test masses. These effects will be alleviated by choosing a test mass material with a high thermal conductivity, such as silicon. • The test mass temperature will be lowered to 123 K, to mitigate thermo-elastic noise. This species of thermal noise is especially problematic in test masses ‡ 1/e 2 intensity § Round-trip loss; see section 5.2 (DRFPMI) with frequency dependent squeezed light injection. The beam from a 2µm prestabilized laser (PSL), passes through an input mode cleaner (IMC) and is injected into the DRFPMI via the power-recycling mirror (PRM). Signal bandwidth is shaped via the signal recycling mirror (SRM). A squeezed vacuum source (SQZ) injects this vacuum into the DRFPMI via an output Faraday isolator (OFI) after it is reflected off a filter-cavity to provide frequency dependent squeezing. A Faraday isolator (FCFI) facilitates this coupling to the filter cavity. The output from the DRFPMI is incident on a balanced homodyne detector, which employs two output mode cleaner cavities (OMC1 and OMC2) and the local oscillator light picked off from the DRFPMI. Cold shields surround the input and end test masses in both the X and Y arms (ITMX, ITMY, ETMX and ETMY) to maintain a temperature of 123 K in these optics. The high-reflectivity coatings of the test masses are made from amorphous silicon. detected (with SNR = 8) as a function of the total mass of the binary (in the source frame). (B) Donut visualization of the horizon distance of LIGO Voyager, aLIGO, and A+, shown with a population of binary neutron star mergers (yellow) and 30-30 M binary black hole mergers (gray). This assumes a Madau-Dickinson star formation rate [7] and a typical merger time of 100 Myr.

show abstract

“…The cryogenic design concept for LIGO Voyager is discussed in [131]. The test masses are maintained at 123 K through radiative cooling, as illustrated in Figure 16.…”

Section: A Cryogenicsmentioning

confidence: 99%

A cryogenic silicon interferometer for gravitational-wave detection

Adhikari¹,

Aguiar²,

Arai³

et al. 2020

Class. Quantum Grav.

Self Cite

168

110

View full text Add to dashboard Cite

show abstract

“…The increased sensitivity is intended to be achieved by improvements in all the departments (seismic isolation system, coatings of mirrors, heavier and larger test masses, increased beam power, etc.) of the advanced LIGO infrastructure combined with frequency dependent squeezing and cryogenic cooling of mirrors [102][103][104].…”

Section: Future Detectors and Networkmentioning

confidence: 99%

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

View full text Add to dashboard Cite

The observation of gravitational wave signals from binary black hole and binary neutron star mergers has established the field of gravitational wave astronomy. It is expected that future networks of gravitational wave detectors will possess great potential in probing various aspects of astronomy. An important consideration for successive improvement of current detectors or establishment on new sites is knowledge of the minimum number of detectors required to perform precision astronomy. We attempt to answer this question by assessing the ability of future detector networks to detect and localize binary neutron stars mergers on the sky. Good localization ability is crucial for many of the scientific goals of gravitational wave astronomy, such as electromagnetic follow-up, measuring the properties of compact binaries throughout cosmic history, and cosmology. We find that although two detectors at improved sensitivity are sufficient to get a substantial increase in the number of observed signals, at least three detectors of comparable sensitivity are required to localize majority of the signals, typically to within around 10 deg 2 -adequate for follow-up with most wide field of view optical telescopes.

show abstract

“…Another key aspect for cryogenic operation is minimizing durations of cool-down and warm-up, to maximize the observatory's duty cycle. In this context, achieving faster cool-downs by using an exchange gas has been examined [10,11].…”

Section: Introductionmentioning

confidence: 99%

Gas cooling of test masses for future gravitational-wave observatories

Reinhardt

Franke

Schaffran

et al. 2021

Class. Quantum Grav.

View full text Add to dashboard Cite

Recent observations made with Advanced LIGO and Advanced Virgo have initiated the era of gravitational-wave astronomy. The number of events detected by these "2 nd Generation" (2G) ground-based observatories is partially limited by noise arising from temperature-induced position fluctuations of the test mass mirror surfaces used for probing space time dynamics. The design of next-generation gravitationalwave observatories addresses this limitation by using cryogenically cooled test masses; current approaches for continuously removing heat (resulting from absorbed laser light) rely on heat extraction via black-body radiation or conduction through suspension fibers. As a complementing approach, we investigate cooling via helium gas impinging on the test mass in free molecular flow. We present analytical models for cooling power and related displacement noise, validated by comparison to numerical simulations. Applying this theoretical framework with regard to the conceptual design of the Einstein Telescope (ET), we find a cooling power of 10 mW at 18 K for a gas pressure that increases the ET design strain noise goal by at most a factor of ∼ 3 in a 8 Hz wide frequency band centered at 7 Hz. A cooling power of 100 mW at 18 K corresponds to a gas pressure that increases the ET design strain noise goal by at most a factor of ∼ 11 in a 26 Hz wide frequency band centered at 7 Hz.

show abstract

Cryogenically cooled ultra low vibration silicon mirrors for gravitational wave observatories

Cited by 26 publications

References 11 publications

A cryogenic silicon interferometer for gravitational-wave detection

A cryogenic silicon interferometer for gravitational-wave detection

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Gas cooling of test masses for future gravitational-wave observatories

Contact Info

Product

Resources

About