A Photoelectric Polarimeter for Measurement of Transient Rotations*

Camp, Paul R.; Raymond, Richard C.

doi:10.1364/josa.42.000237

Cited by 7 publications

(3 citation statements)

References 5 publications

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“…The sensitivity of the Advanced Telescope for High ENergy Astrophysics (Athena) X-ray observatory 192 , which is expected to be launched around 2030, and the ambitious Lynx project 193 , proposed in the USA, will be of great value to detect fainter X-ray sources, such as the X-ray afterglow emission from relativistic jets observed off-axis. Mission concepts, such as the Transient High Energy Sky and Early Universe Surveyor (THESEUS 194 ) and the Transient Astrophysics Probe (TAP 195 ), are designed to have a unique combination of instruments for gamma-ray, X-ray and infrared transient detections to catch non-thermal and thermal emissions from GW sources.…”

Section: Multi-messenger Facilitiesmentioning

confidence: 99%

Gravitational-wave physics and astronomy in the 2020s and 2030s

et al. 2021

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The past five years have witnessed a revolution in astronomy. The direct detection of gravitational waves (GW) emitted from the binary black hole (BBH) merger GW150914 (Fig. 1) by the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) detector 1 on September 14, 2015 (reF. 2 ) was a watershed event, not only in demonstrating that GWs could be directly detected but more fundamentally in revealing new insights into these exotic objects and the Universe itself. On August 17, 2017, the Advanced LIGO and Advanced Virgo 3 detectors jointly detected GW170817, the merger of a binary neutron star (BNS) system 4 , an equally momentous event leading to the observation of electromagnetic (EM) radiation emitted across the entire spectrum through one of the most intense astronomical observing campaigns ever undertaken 5 .Coming nearly 100 years after Albert Einstein first predicted their existence 6 , but doubted that they could ever be measured, the first direct GW detections have undoubtedly opened a new window on the Universe. The scientific insights emerging from these detections have already revolutionized multiple domains of physics and astrophysics, yet, they are 'the tip of the iceberg' , representing only a small fraction of the future potential of GW astronomy. As is the case for the Universe seen through EM waves, different classes of astrophysical sources emit GWs across a broad spectrum ranging over more than 20 orders of magnitude, and require different detectors for the range of frequencies of interest (Fig. 2).In this Roadmap, we present the perspectives of the Gravitational Wave International Committee (GWIC, https://gwic.ligo.org) on the emerging field of GW astronomy and physics in the coming decades. The GWIC was formed in 1997 to facilitate international collaboration and cooperation in the construction, operation and use of the major GW detection facilities worldwide. Its primary goals are: to promote international cooperation in all phases of construction and scientific exploitation of GW detectors, to coordinate and support long-range planning for new instruments or existing instrument upgrades, and to promote the development of GW detection as an astronomical tool, exploiting especially the potential for multi-messenger astrophysics. Our intention in this Roadmap is to present a survey of the science opportunities and to highlight the future detectors that will be needed to realize those opportunities. The recent remarkable discoveries in GW astronomy have spurred the GWIC to re-examine and update the GWIC roadmap originally published a decade ago 7 .We first present an overview of GWs, the methods used to detect them and some scientific highlights from the past five years. Next, we provide a detailed survey

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Section: Multi-messenger Facilitiesmentioning

confidence: 99%

Gravitational-wave physics and astronomy in the 2020s and 2030s

et al. 2021

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“…Unfortunately, while the co-extrusion process that we use has been shown to be compatible with many different polymer constituents, most polymers show only a very small bulk Faraday effect [15][16][17]. Still, the simplicity of preparation and handling of our system, the high transparency of the materials outside the reflection band, and the new ease of constructing 1D-PCs with large numbers of layers afford us a useful medium for experimentally and theoretically separating the intrinsic and lattice structural effects contributing to Faraday rotation in a 1D-PC.…”

Section: Experiments a Materials And Processesmentioning

confidence: 99%

“…The intensity stability of the system ultimately limits the sensitivity of the Faraday rotation measurement. If θ pol 45°(commonly used in other Faraday rotation measurement, e.g., see [15,41]), then 2 tanθ pol 2 and a 1% variation in the light intensity correspond to a maximum rotation angle resolution sensitivity of 0.3°. If, however, a larger angle is used (for example, θ pol 85°as in most of our experiments), then 2 tanθ pol 22.8 and the resolution is increased by a factor of 11.4.…”

Section: B Faraday Rotation Measurementmentioning

confidence: 99%

Role of group velocity delay in Faraday rotation in a multilayer polymer lattice

et al. 2012

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We measure and model the spectral dependence of Faraday rotation in one-dimensional lattice structures composed of co-extruded alternating polymer layers of polymethylmethacrylate and polystyrene. We develop a theory that shows that the net Faraday rotation in a symmetric multilayer system is determined not by the total thickness of the constituent materials but by the time spent in each constituent material as measured by the overall group velocity delay of the structure and the relative energy distribution per material. We compare measured and computed Faraday rotation spectra for these films to theoretical predictions, taking into account ellipticity as well as layer thickness variations and finite spectral width detection. To measure rotations of these thin, nonmagnetic, weak Faraday rotators, we constructed and optimized an apparatus capable of measuring broadband Faraday rotation spectra at 0.001°resolution for rotation angles as small as 0.002°.

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