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Shreevathsa Chalathadka Subrahmanya

Publications and source records attributed to Shreevathsa Chalathadka Subrahmanya.

6 recordsLinked to original sources

Demonstration of a compact optical resonator-based displacement sensing technique with sub-femtometer precision

We demonstrate sub-femtometer displacement-sensing results achieved with a compact optical resonator-based laser interferometry technique called heterodyne cavity-tracking, intended for local displacement or inertial sensing with ultra-high sensitivity. Displacement sensing at this sensitivity is required for ambitious improvements to current gravitational-wave detectors and to enable future ground- and space-based observatories. The optical topology employs a centimeter-scale dynamic cavity incorporating a proof mass, and the relative length fluctuations of this cavity are measured using a heterodyne readout. The fundamental limits of the technique lie significantly below the femtometer level and are ultimately defined by the coating thermal noise of the cavity mirrors. In our experimental demonstration, we achieve a sub-femtometer per Hz$^{1/2}$ displacement sensitivity for Fourier frequencies above 8 Hz and a sub-picometer per Hz$^{1/2}$ sensitivity above 3 mHz, with the sensitivity at lower frequencies limited by mechanical and temperature-induced noise sources. When the length of the dynamic cavity was intentionally actuated, the technique could track a maximum motion of about 0.6 $μ$m, thereby achieving a dynamic range of roughly ten orders of magnitude in displacement sensing. We thus demonstrate the key features of this scheme - sub-femtometer performance and a dynamic range spanning ten orders of magnitude - in a laboratory setting, paving the way for development of an integrated system. Such a system is a currently unrealized technology that is necessary for precision physics experiments in the coming decades.

physics.ins-det↗

Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors

Space-based gravitational wave detectors, such as the Laser Interferometer Space Antenna (LISA), use picometer-precision laser interferometry to detect gravitational waves at frequencies from 1 Hz down to below 0.1 mHz. Laser interferometers used for on-ground prototyping and testing of such instruments are typically constructed by permanently bonding or gluing optics onto an ultra-stable bench made of low-expansion glass ceramic. This design minimizes temperature coupling to length and tilt, which dominates the noise at low frequencies due to finite temperature stability achievable in laboratories and vacuum environments. Here, we present the study of an alternative opto-mechanical concept where optical components are placed with adjustable and freely positionable mounts on an ultra-stable bench, while maintaining picometer length stability. With this concept, a given interferometer configuration can be realised very quickly due to a simplified and speed-up assembly process, reducing the realisation time from weeks or months to a matter of hours. We built a corresponding test facility and verified the length stability of our concept by measuring the length change in an optical cavity that was probed with two different locking schemes, heterodyne laser frequency stabilisation and Pound-Drever-Hall locking. We studied the limitations of both locking schemes and verified that the cavity length noise is below 1 pm/sqrt(Hz) for frequencies down to 3 mHz. We thereby demonstrate that our concept can simplify the testing of interferometer configurations and opto-mechanical components and is suitable to realise flexible optical ground support equipment for space missions that use laser interferometry, such as future space-based gravitational wave detectors and satellite geodesy missions.

physics.ins-det↗

Integrating high-precision and fringe-scale displacement sensing using heterodyne cavity-tracking

We present a heterodyne stabilized cavity-based interferometer scheme that can serve as a compact and high-sensitivity displacement sensor with a fringe-scale operating range. The technique, in principle, can reach a sub-femtometer noise floor and an operating range on the order of one laser wavelength at $λ\approx 1\,μm$. With our current experimental setup, we achieve a sensitivity of about $260 fm/\sqrt{\mathrm{Hz}}$ at $1\,Hz$ and $46 fm/\sqrt{\mathrm{Hz}}$ at around $130\,Hz$. By probing a length actuated cavity, we demonstrate six orders of magnitude of dynamic range for displacement measurement, reaching a maximum motion of $0.15\,μm$. The tracking bandwidth and displacement range are limited by analog effects in the signal digitization and are extendable in the future.

physics.optics↗

On the Development of an RFSoC-Based Ultra-Fast Phasemeter With GHz Bandwidth

Precise measurements of the frequency and phase of an electrical or optical signal play a key role in various branches of science and engineering. Tracking changing laser frequencies is especially demanding when the lasers themselves are noisy or if the frequencies rapidly change because they encode highly dynamic signals in, e.g., Doppler-ranging or dynamic cavity readout. Here, to address these and other possible applications, we report the development of a high signal bandwidth (> 2 GHz) and high tracking bandwidth (2 MHz) multi-channel Phasemeter. The implementation utilizes an all-digital phase-locked loop realized within the field programmable gate array (FPGA) part of a radio frequency system-on-chip (RFSoC), the programmable logic (PL). The new features of the phasemeter are obtained by operating the PL at its timing limits and introducing a multi-demodulation and phase accumulation scheme. We present performance measurements, discuss the role of the high tracking bandwidth for tracking highly dynamic signals, and demonstrate ultra-stable phase locking of a beat note between two widely tunable external cavity diode lasers. We achieve a phase-noise floor in the sub-milli radian regime when comparing two signals, even for GHz frequencies, and demonstrate stable tracking of signals with a frequency change rate of 240 GHz/s.

physics.ins-det↗

The Lunar Gravitational-wave Antenna: Mission Studies and Science Case

The Lunar Gravitational-wave Antenna (LGWA) is a proposed array of next-generation inertial sensors to monitor the response of the Moon to gravitational waves (GWs). Given the size of the Moon and the expected noise produced by the lunar seismic background, the LGWA would be able to observe GWs from about 1 mHz to 1 Hz. This would make the LGWA the missing link between space-borne detectors like LISA with peak sensitivities around a few millihertz and proposed future terrestrial detectors like Einstein Telescope or Cosmic Explorer. In this article, we provide a first comprehensive analysis of the LGWA science case including its multi-messenger aspects and lunar science with LGWA data. We also describe the scientific analyses of the Moon required to plan the LGWA mission.

gr-qc↗

The payload of the Lunar Gravitational-wave Antenna

The toolbox to study the Universe grew on 14 September 2015 when the LIGO-Virgo collaboration heard a signal from two colliding black holes between 30-250 Hz. Since then, many more gravitational waves have been detected as detectors increased sensitivity. However, the current detector design sensitivity curves still have a lower cut-off of 10 Hz. To detect even lower-frequency gravitational-wave signals, the Lunar Gravitational-wave Antenna will use an array of seismic stations in a permanently shadowed crater. It aims to detect the differential between the elastic response of the Moon and the suspended inertial sensor proof mass motion induced by gravitational waves. A cryogenic superconducting inertial sensor is under development that aims for fm/rtHz sensitivity or better down to 1 Hz and is planned to be deployed in seismic stations. Here, we describe the current state of research towards the inertial sensor, its applications and additional auxiliary technologies in the payload of the lunar gravitational-wave detection mission.

gr-qc↗