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📃Scientific paper: Evaluating residual acceleration noise for TianQin gravitational waves observatory with an empirical magnetic field model Abstract: TianQin \(TQ\) project plans to deploy three satellites in space around the Earth to measure the displacement change of test masses caused by gravitational waves via laser interferometry. The requirement of the acceleration noise of the test mass is on the order of $10^\{-15\}\~\,\{\rm m\}\,\{\rm s\}^\{-2\}\,\{\rm Hz\}^\{-1/2\}$ in the sensitive frequency range of TQ, %the extremely precise acceleration measurement requirements make it necessary to investigate acceleration noise due to space magnetic fields. which is so stringent that the acceleration noise caused by the interaction of the space magnetic field with the test mass needs to be investigated. In this work, by using the Tsyganenko model, a data-based empirical space magnetic field model, we obtain the magnetic field distribution around TQ's orbit spanning two solar cycles in 23 years from 1998 to 2020. With the obtained space magnetic field, we derive the distribution and amplitude spectral densities \(ASDs\) of the acceleration noise of TQ in 23 years. Our results reveal that the average values of the ratio of the acceleration noise cauesd by the space magnetic field to the requirements of TQ at 1 mHz \($R\_\{\rm 1mHz\}$\) and 6 mHz \($R\_\{\rm 6mHz\}$\) are 0.123$\pm$0.052 and 0.027$\pm$0.013, respectively. The occurence probabilities of $R\_\{\rm 1mHz\}\>0.2$ and $\>0.3$ are only 7.9% and 1.2%, respectively, and $R\_\{\rm 6mHz\}$ never exceeds 0.2. ;Comment: 13 pages, 10 figures, Published in PRD Continued on ES/IODE ➡️ https://etcse.fr/gpk ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

This week at the #PrecisionFair (www.precisionfair.com) in Den Bosch I will present where we need industry to contribute to the challenges for the construction of the #EinsteinTelescope. Einstein Telescope: construction of the instrument to measure gravitational waves. Gravitational waves are an exciting tool to observe the Universe. Measuring gravitational waves with much higher precision than currently possible requires an underground facility with many technological innovations, such as multi-stage seismic isolation systems to dampen the noise that propagates through the ground; ultra-high vacuum in what might well prove to be the largest vacuum vessel in the world; cryogenics cooling of the mirrors to around 10 K, without disturbing their isolation from the ground-noise. With a facility this large, design for assembly, installation, and maintenance will be paramount. Therefore early industry involvement is envisioned to ensure swift industrial producibility.

The Smallsat Technology Accelerated Maturation Platform-1 (STAMP-1): A Proposal to Advance Ultraviolet Science, Workforce, and Technology for the Habitable Worlds Observatory We present a concept for the Smallsat Technology Accelerated Maturation Platform (STAMP), an integrated facility, laboratory, and instrument prototype development program that could be supported through the GOMAP framework and applied to any of NASA’s Future Great Observatories (FGOs). This brief describes the recommendation for the first entrant into this program, “STAMP-1”, an ESPA Grande-class mission advancing key technologies to enable the ultraviolet capabilities of HWO. https://lnkd.in/gVmuqhU4

IMRA, a creative research and innovation organization that develops essential technologies for industrial use, tackled many of the issues associated with the THz regime recently when working at frequencies above 300 GHz. Researchers at the Colorado-based laboratory were looking to use molecules as stable frequency references that could potentially be used as clocks. “We actually had a WR 3.4 band isolator from Micro Harmonics on the shelf from past research projects,” explains Research Scientist James Greenberg, a program manager at IMRA. “We plugged it in and got fantastic results.” Under a NASA awarded contract, we designed an advanced line of MMW isolators capable of optimal operation between WR-28 and WR-2.8 (26.5 GHz to 400 GHz). The commercial off-the-shelf (COTS) components offered IMRA the high isolation, low insertion loss and small footprint it was looking for. In fact, IMRA reported getting 30 dB of isolation with the isolators. But it was the incredibly low insertion loss of less than 2 dB in the WR-3.4 band that made the difference. “We were starved for power because our transmitter was weak, and we were really pleased with the low insertion loss the isolator provided which allowed us to get the maximum signal to noise.” -James Greenberg, Ph.D. Research Scientist/Program Manager, IMRA #mmwave #MicroHarmonics #THztechnology #researchanddevelopment #rfengineering

Exploring the Cosmos: How Radio Interferometry and Aperture Synthesis Unveil the Secrets of the Universe Ever marvel at the stunning images of distant galaxies and cosmic phenomena? The secret is #RadioInterferometry, especially #ApertureSynthesis. This advanced technique acts like a superpower for astronomers, combining signals from multiple radio telescopes to create incredibly detailed images of the universe. It allows scientists to see cosmic structures with remarkable clarity, revealing the wonders of space like never before. https://lnkd.in/dh56JGNv #GMRT

Time on Earth is determined through a complex interplay of various scientific principles and technological advancements. At the core of timekeeping are atomic clocks, which rely on the precise and consistent energy transitions of atoms, such as cesium and strontium. The passage of time is fundamentally affected by the influence of gravity. As described by Einstein's theory of general relativity, the presence of massive objects like the Earth causes a distortion in the fabric of spacetime, leading to a slight slowing of the flow of time. This effect is known as gravitational time dilation and is a crucial consideration in the accurate measurement of time. To overcome the challenges posed by gravitational influences, modern atomic clocks employ advanced techniques to maintain exceptional precision. The energy transitions of atoms, such as the oscillation of a cesium atom, are used as the basis for these highly accurate timekeepers. The frequency of these transitions is then used to define the second, the fundamental unit of time. Furthermore, the development of technologies like the Global Positioning System (GPS) has revolutionized the way we measure and synchronize time across the globe. By utilizing the signals from a network of satellites, GPS receivers can determine their precise location and time, enabling a wide range of applications that rely on accurate timekeeping. Ongoing research in the field of timekeeping continues to push the boundaries of accuracy, with the development of even more precise clocks, such as those based on strontium or mercury atoms. These advancements pave the way for a deeper understanding of the fundamental nature of time and its measurement on Earth. #time #atomicclock #earth #scientificresearch

📃Scientific paper: Millimeter-wave CO and SiO Observations toward the Broad-velocity-width Molecular Feature CO 16.134-0.553: a Smith cloud scenario? Abstract: We report the results of the CO $\textit J$=1-0 and SiO $\textit J$=2-1 mapping observations towards the broad-velocity-width molecular feature CO 16.134-0.553 with the Nobeyama Radio Observatory 45 m telescope. The high quality CO map shows that the 5-pc size broad-velocity-width feature bridges two separate velocity components at $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ and 65 km s$^\{-1\}$ in the position-velocity space. The kinetic power of CO 16.134-0.553 amounts to $7.8\times10^2$ $\textit L$$\_\odot$ whereas no apparent driving sources were identified. Prominent SiO emission was detected from the broad-velocity-width feature and its root in the $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ component. In the CO Galactic plane survey data, CO 16.134-0.553 appears to correspond to the Galactic eastern rim of a 15-pc diameter expanding CO shell. An $1\deg$-diameter H I emission void and $4\deg$-long vertical H I filament were also found above and below the CO shell, respectively. We propose that the high-velocity plunge of a dark matter subhalo with a clump of baryonic matter was responsible for the formation of the H I void, CO 16.134-0.553/CO shell, and the H I filament. ;Comment: 7 pages, 6 figures, 2 table, accepted for publication in ApJ Continued on ES/IODE ➡️ https://etcse.fr/Bmuf ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: Millimeter-wave CO and SiO Observations toward the Broad-velocity-width Molecular Feature CO 16.134-0.553: a Smith cloud scenario? Abstract: We report the results of the CO $\textit J$=1-0 and SiO $\textit J$=2-1 mapping observations towards the broad-velocity-width molecular feature CO 16.134-0.553 with the Nobeyama Radio Observatory 45 m telescope. The high quality CO map shows that the 5-pc size broad-velocity-width feature bridges two separate velocity components at $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ and 65 km s$^\{-1\}$ in the position-velocity space. The kinetic power of CO 16.134-0.553 amounts to $7.8\times10^2$ $\textit L$$\_\odot$ whereas no apparent driving sources were identified. Prominent SiO emission was detected from the broad-velocity-width feature and its root in the $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ component. In the CO Galactic plane survey data, CO 16.134-0.553 appears to correspond to the Galactic eastern rim of a 15-pc diameter expanding CO shell. An $1\deg$-diameter H I emission void and $4\deg$-long vertical H I filament were also found above and below the CO shell, respectively. We propose that the high-velocity plunge of a dark matter subhalo with a clump of baryonic matter was responsible for the formation of the H I void, CO 16.134-0.553/CO shell, and the H I filament. ;Comment: 7 pages, 6 figures, 2 table, accepted for publication in ApJ Continued on ES/IODE ➡️ https://etcse.fr/Bmuf ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: A star-based method for precise flux calibration of the Chinese Space Station Telescope \(CSST\) slitless spectroscopic survey Abstract: The upcoming Chinese Space Station Telescope \(CSST\) slitless spectroscopic survey poses a challenge of flux calibration, which requires a large number of flux-standard stars. In this work, we design an uncertainty-aware residual attention network, the UaRA-net, to derive the CSST SEDs with a resolution of R = 200 over the wavelength range of 2500-10000 \AA using LAMOST normalized spectra with a resolution of R = 2000 over the wavelength range of 4000-7000 \AA. With the special structure and training strategy, the proposed model can not only provide accurate predictions of SEDs but also their corresponding errors. The precision of the predicted SEDs depends on effective temperature \(Teff\), wavelength, and the LAMOST spectral signal-to-noise ratios \(SNRs\), particularly in the GU band. For stars with Teff = 6000 K, the typical SED precisions in the GU band are 4.2%, 2.1%, and 1.5% at SNR values of 20, 40, and 80, respectively. As Teff increases to 8000 K, the precision increases to 1.2%, 0.6%, and 0.5%, respectively. The precision is higher at redder wavelengths. In the GI band, the typical SED precisions for stars with Teff = 6000 K increase to 0.3%, 0.1%, and 0.1% at SNR values of 20, 40, and 80, respectively. We further verify our model using the empirical spectra of the MILES and find good performance. The proposed method will open up new possibilities for optimal utilization of slitless spectra of the CSST and other surveys. ;Comment: 20 pages, 15 figures, accep... Continued on ES/IODE ➡️ https://etcse.fr/E71fV ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

Ultraviolet “winds” from nearby massive stars are stripping the gas from a young star’s protoplanetary disk, causing it to rapidly lose mass, according to a new study. It reports the first directly observed evidence of far-ultraviolet (FUV)-driven photoevaporation of a protoplanetary disk. The findings, which use observations from the James Web Space Telescope (JWST), provide new insights into the constraints of gas giant planet formation, including in our own Solar System. Young low-mass stars are often surrounded by relatively short-lived protoplanetary disks of dust and gas, which provide the raw materials from which planets form. As such, gas giant planet formation is limited by processes that remove mass from protoplanetary disks, such as photoevaporation. Photoevaporation occurs when the upper layers of protoplanetary disks are heated by x-ray or ultraviolet protons, which increases the gas temperature and causes it to escape from the system. Since most low-mass stars form in clusters also containing massive stars, protoplanetary disks are expected to be exposed to external radiation and experience ultraviolet-driven photoevaporation. Using near-infrared and submillimeter measurements from the JWST and the Atacama Large Millimeter Array (ALMA), respectively, Olivier Berné and colleagues report observations of a FUV-irradiated protoplanetary disk, d203-506, located inside the Orion Nebula. By modeling the kinematics and excitation of the emission lines detected within the PDR, the researchers found that d203-506 is losing mass at a high rate due to FUV-driven heating and ionization. #cosmos #photoevaporation #jwst #measurements https://lnkd.in/gbbuFyD8