Hexbyte Glen Cove Extending our reach into the cosmos with new mirror coatings thumbnail

Hexbyte Glen Cove Extending our reach into the cosmos with new mirror coatings

Hexbyte Glen Cove

The LIGO coating materials to be tested are deposited on thin glass disks, much smaller than the LIGO mirrors. The pinkish color in the photo is due to the thin layer of metal oxide deposited on the surface. Credit: Caltech

Since the Laser Interferometer Gravitational-wave Observatory (LIGO)’s groundbreaking detection, in 2015, of gravitational waves produced by a pair of colliding black holes, the observatory, together with its European partner facility Virgo, has detected dozens of similar cosmic rumblings that send ripples through space and time.

In the future, as more and more upgrades are made to the National Science Foundation-funded LIGO observatories—one in Hanford, Washington, and the other in Livingston, Louisiana—the facilities are expected to detect increasingly large numbers of these extreme cosmic events. These observations will help solve fundamental mysteries about our universe, such as how form and how the ingredients of our universe are manufactured.

One important factor in increasing the sensitivity of the observatories involves the coatings on the glass mirrors that lie at the heart of the instruments. Each 40-kilogram (88-pound) mirror (there are four in each detector at the two LIGO observatories) is coated with that essentially turn the glass into mirrors. The mirrors reflect laser beams that are sensitive to passing gravitational waves.

Generally, the more reflective the mirrors, the more sensitive the instrument, but there is a catch: The coatings that make the mirrors reflective also can lead to background noise in the instrument—noise that masks gravitational-wave signals of interest.

Now, a new study by the LIGO team describes a new type of mirror coating made of titanium oxide and germanium oxide, and outlines how it can reduce in LIGO’s mirrors by a factor of two, thereby increasing the volume of space that LIGO can probe by a factor of eight.

“We wanted to find a material at the edge of what is possible today,” says Gabriele Vajente, a LIGO senior research scientist at Caltech and lead author of a paper about the work that appears in the journal Physical Review Letters. “Our ability to study the astronomically large scale of the universe is limited by what happens in this very tiny microscopic space.”

“With these new coatings, we expect to be able to increase the detection rate of gravitational waves from once a week to once a day or more,” says David Reitze, executive director of LIGO Laboratory at Caltech.

The research, which may have future applications in the fields of telecommunications and semiconductors, was a collaboration among Caltech; Colorado State University; the University of Montreal; and Stanford University, whose synchrotron at the SLAC National Accelerator Laboratory was used in the characterization of the coatings.

LIGO detects ripples in space-time using detectors called interferometers. In this setup, a powerful laser beam is split into two: Each beam travels down one arm of a large L-shaped vacuum enclosure toward mirrors 4 kilometers away. The mirrors reflect the laser beams back to the source from which they originated. When pass by, they will stretch and squeeze space by nearly imperceptible and yet detectable amounts (much less than the width of a proton). The perturbations change the timing of the arrival of the two laser beams back at the source.

Any jiggling in the mirrors themselves—even the microscopic thermal vibrations of the atoms in the mirrors’ coatings—can affect the timing of the ‘ arrival and make it hard to isolate the gravitational-wave signals.

“Every time light passes between two different materials, a fraction of that light is reflected,” says Vajente. “This is the same thing that happens in your windows: You can see your faint reflection in the glass. By adding multiple layers of different materials, we can reinforce each reflection and make our mirrors up to 99.999 percent reflective.”

“What’s important about this work is that we developed a new way to better test the materials,” says Vajente. “We can now test the properties of a new material in about eight hours, completely automated, when before it took almost a week. This allowed us to explore the periodic table by trying a lot of different materials and a lot of combinations. Some of the materials we tried didn’t work, but this gave us insights into what properties might be important.”

In the end, the scientists discovered that a coating material made from a combination of titanium oxide and germanium oxide dissipated the least energy (the equivalent of reducing thermal vibrations).

“We tailored the fabrication process to meet the stringent demands in optical quality and reduced thermal noise of the mirror coatings,” says Carmen Menoni, professor at Colorado State University and member of the LIGO Scientific Collaboration. Menoni and her colleagues at Colorado State used a method called ion beam sputtering to coat the mirrors. In this process, atoms of titanium and germanium are peeled away from a source, combined with oxygen, and then deposited onto the glass to create thin layers of atoms.

The new coating may be used for LIGO’s fifth observing run, which will begin in the middle of the decade as part of the Advanced LIGO Plus program. Meanwhile, LIGO’s fourth observing run, the last in the Advanced LIGO campaign, is expected to commence in the summer of 2022.

“This is a game changer for Advanced LIGO Plus,” says Reitze. “And this is a great example of how LIGO relies heavily on cutting-edge optics and materials science research and development. This is the biggest advance in precision optical development for LIGO in the past 20 years.”

More information:
Gabriele Vajente et al, Low Mechanical Loss TiO2:GeO2 Coatings for Reduced Thermal Noise in Gravitational Wave Interferometers, Physical Review Letters (2021). DOI: 10.1103/PhysRevLett.127.071101


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Hexbyte Glen Cove Candid cosmos: eROSITA cameras set benchmark for astronomical imaging thumbnail

Hexbyte Glen Cove Candid cosmos: eROSITA cameras set benchmark for astronomical imaging

Hexbyte Glen Cove

A team of scientists from the Max-Planck-Institut für extraterrestrische Physik, Germany, built an x-ray telescope called eROSITA consisting of an array of co-aligned focal plane cameras with one in the center and six surrounding it. Credit: P. Friedrich, doi 10.1117/1.JATIS.7.2.025004

Recently, the eROSITA (extended Roentgen Survey with an Imaging Telescope Array) X-ray telescope, an instrument developed by a team of scientists at Max-Planck-Institut für Extraterrestrische Physik (MPE), has gained attention among astronomers. The instrument performs an all-sky survey in the X-ray energy band of 0.2-8 kilo electron volts aboard the Spectrum-Roentgen-Gamma (SRG) satellite that was launched in 2019 from the Baikonur cosmodrome in Kazakhstan.

“The eROSITA has been designed to study the large-scale structure of the universe and test , including , by detecting with redshifts greater than 1, corresponding to a cosmological expansion faster than the ,” said Dr. Norbert Meidinger from MPE, a part of the team that developed the instrument. “We expect eROSITA to revolutionize our understanding of the evolution of supermassive black holes.” The details of the developmental work have been published in SPIE’s Journal of Astronomical Telescopes, Instruments, and Systems (JATIS).

eROSITA is not one telescope, but an array of seven identical, co-aligned telescopes, with each one composed of a mirror system and a focal-plane camera. The camera assembly, in turn, consists of the camera head, camera electronics, and filter wheel. The camera head is made up of the detector and its housing, a proton shield, and a heat pipe for detector cooling. The camera electronics include supply, control, and data acquisition electronics for detector operation. The filter wheel is mounted above the head and has four positions including an optical and UV blocking filter to reduce signal noise, a radioactive X-ray source for calibration, and a closed position that allows instrumental background measurements.

First light of the eROSITA X-ray telescope in space. Credit: Norbert Meidinger et al. doi: 10.1117/1.JATIS.7.2.025004

“It’s exciting to read about these X-ray cameras that are in orbit and enabling a broad set of scientific investigations on a major astrophysics mission,” says Megan Eckart of Lawrence Livermore National Laboratory, USA, who is the deputy editor of JATIS. “Dr. Meidinger and his team provide a clear description of the hardware development and ground testing, and wrap up the paper with a treat: first-light images from eROSITA and an assessment of onboard performance. Astrophysicists around the world will analyze data from these cameras for years to come.”

The eROSITA telescope is well on its way to becoming a game changer for X-ray astronomy.

More information:
Norbert Meidinger et al, eROSITA camera array on the SRG satellite, Journal of Astronomical Telescopes, Instruments, and Systems (2021). DOI: 10.1117/1.JATIS.7.2.025004

Candid cosmos: eROSITA cameras set benchmark for astronomical imaging (2021, May 25)
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