Podcasts about interferometry

SpaceTime Series 27 Episode 140*Revisiting the Milky Way's Black Hole ImageA new study questions the accuracy of the first-ever image of Sagittarius A, the supermassive black hole at the centre of the Milky Way. Researchers suggest the image may not accurately represent its appearance, proposing a more elongated accretion disc instead of the ring-like structure previously released by the Event Horizon Telescope.*Methane in Titan's CrustData from NASA's Cassini spacecraft indicates that Saturn's moon Titan may have a methane-rich crust up to 10 kilometres thick. This insulating layer could explain Titan's shallow impact craters and its methane-rich atmosphere, providing insights into its unique geological and atmospheric dynamics.*Updates on Earth's Ozone HoleNASA reports that the annual ozone hole over Antarctica was smaller this year, ranking as the seventh smallest since recovery efforts began. The ozone layer is on track to fully recover by 2066, thanks to international agreements curbing ozone-depleting chemicals.The Science ReportAntarctic ice core samples suggest Earth has already surpassed a 1.5°C global temperature rise due to human-induced climate change. A study links outdoor lighting at night to increased Alzheimer's risk for those under 65. LED lights on surfboards could reduce shark attacks by mimicking natural camouflage. Nord's latest survey reveals continued use of weak passwords, with "123456" and "password" among the most common.www.spacetimewithstuartgary.comwww.bitesz.com

This episode is brought to you with the support of NordVPN. For our special Black Friday deal complete with 30 day money back guarantee, visit www.nordvpn.com/spacenuts. Space Nuts #462 Q&A EditionJoin Andrew Dunkley and Professor Fred Watson in another enlightening Q&A episode of Space Nuts, where they tackle intriguing questions from listeners around the globe. From the perplexing nature of dark matter and dark energy to the possibility of interferometry using Space and ground-based telescopes, this episode is packed with cosmic curiosities and insightful discussions.Episode Highlights:- Dark Matter and Dark Energy in the Solar System: Trent from St. John's, Newfoundland, Canada, questions why dark matter and dark energy, which comprise 96% of the universe, are not factored into the movements of our solar system. Fred Watson Watson explains the scale and influence of these mysterious forces.- Interferometry with Space Telescopes: Bo from Victoria wonders if it's theoretically possible to perform interferometry using Space telescopes like Hubble and James Webb, combined with ground-based telescopes. Explore the current limitations and future possibilities of this technology.- The Mystery of Gravitons: Vincent questions the existence of gravitons and their potential to form self-propagating waves. Delve into the intersection of quantum theory and relativity as Fred Watson Watson discusses this theoretical particle.- Biblical Floods and Astronomical Events: Christopher from Bayville, North Carolina, inquires about the possibility of biblical floods being linked to astronomical events. Discover the fascinating connections between historical events and cosmic phenomena.For more Space Nuts, including our continually updating newsfeed and to listen to all our episodes, visit our website at www.spacenutspodcast.com. Follow us on social media at SpaceNutsPod on facebook, X, YouTube, Instagram, and TikTok. We love engaging with our community, so be sure to drop us a message or comment on your favourite platform.For more Space and Astronomy News Podcasts, visit our HQ at www.bitesz.com.Become a supporter of this podcast: https://www.spreaker.com/podcast/space-nuts/support.Stay curious, keep looking up, and join us next time for more stellar insights and cosmic wonders. Until then, clear skies and happy stargazing.

We have already referred to the 66 antennas that make up ALMA, but how do they operate as one telescope? In this episode, Giorgio Siringo, Senior Radio-Frequency Engineer, will explain how interferometry works. Furthermore, let's discover how one supercomputer synchronizes and synthesizes the light received through the antennas to constitute only one giant telescope.

In this podcast episode, MRS Bulletin's Sophia Chen interviews Alice Soragni of the University of California, Los Angeles about her work in precision oncology. Rather than sequence the DNA of a patient's tumor, Soragni uses bioprinting to create organoids from the patient's cells. She then adds various drugs to the cells to directly test their response to each drug. To check the effectiveness of the drugs, Soragni's group measures the organoid's mass with a technique called interferometry. Interferometry is a non-invasive technique that involves shining light on the cells to monitor their response to the drug. This process allows Soragni to characterize the organoid's response to the drug in fine detail. This work was published in a recent issue of Nature Communications. 

Do you enjoy the shamelessly fringe? How about this podcast? We want to hear your voice in all it's weirdo glory! Go to ratethispodcast.com/openloopsThis week on Open Loops, we return with an episode exploring your sacral chakra.Just kidding. You can shove that episode premise up your sacral... because we're bringing in a bigwig investigative researcher who's been experiencing telepathic communication with ETs since the mid-90s. Peak Simpsons era, right before they started objectifying talented female singers in the Mickey Mouse Club. You know, the good times?Ever since George LuoBono has communicated with ETs, he's gained a multidimensional understanding of our mind, consciousness, the Universe, secret government alien programs, and even worked out an update to Einstein's Theory of Relativity that accounts for non-human intelligence all the way to the far edges of the cosmos.He joins Greg to discuss why the aliens who crashed at Roswell, and in any flying saucer for that matter, are NOT our friends (more like frenemies). He talks about Dark Matter and its relationship to consciousness. He discusses the exotic beauty of Red Dwarf Extraterrestrials unlike anything you've ever experienced.And they talk about Love a Dub Dub. Because love is all you need. But George's perspective on hyperdimensional energy will let that sink in even more naturally than you've experienced before...It's not the alien whistleblower response episode you wanted... it's even fringier. Shamelessly fringe, perhaps. And perhaps... it's an all-new OPEN LOOPS.George's Links: Follow George on Facebook at https://www.facebook.com/george.lobuono/Buy George's first book "Alien Mind; the Thought and Behavior of Extraterrestrials" on Amazon here. 

NICMOS Kernel-Phase Interferometry II: Demographics of Nearby Brown Dwarfs by Samuel M. Factor et al. on Wednesday 30 November Star formation theories have struggled to reproduce binary brown dwarf population demographics (frequency, separation, mass-ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of formation at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F=0.11^{+0.04}_{-0.03}$ and a separation distribution centered at $rho=2.2^{+1.2}_{-1.0}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index which strongly favors equal-mass systems: $gamma=4.0^{+1.7}_{-1.5}-11^{+4}_{-3}$ depending on the assumed age of the field population ($0.9-3.1$ Gyr). We attribute the change in values to our use of kernel-phase interferometry which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously-seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age sub-stellar regime; only $0.9^{+1.1}_{-0.6}$ % of systems are wider than 20 au and $

NICMOS Kernel-Phase Interferometry II: Demographics of Nearby Brown Dwarfs by Samuel M. Factor et al. on Wednesday 30 November Star formation theories have struggled to reproduce binary brown dwarf population demographics (frequency, separation, mass-ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of formation at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F=0.11^{+0.04}_{-0.03}$ and a separation distribution centered at $rho=2.2^{+1.2}_{-1.0}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index which strongly favors equal-mass systems: $gamma=4.0^{+1.7}_{-1.5}-11^{+4}_{-3}$ depending on the assumed age of the field population ($0.9-3.1$ Gyr). We attribute the change in values to our use of kernel-phase interferometry which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously-seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age sub-stellar regime; only $0.9^{+1.1}_{-0.6}$ % of systems are wider than 20 au and $

NICMOS Kernel-Phase Interferometry II: Demographics of Nearby Brown Dwarfs by Samuel M. Factor et al. on Wednesday 30 November Star formation theories have struggled to reproduce binary brown dwarf population demographics (frequency, separation, mass-ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of formation at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F=0.11^{+0.04}_{-0.03}$ and a separation distribution centered at $rho=2.2^{+1.2}_{-1.0}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index which strongly favors equal-mass systems: $gamma=4.0^{+1.7}_{-1.5}-11^{+4}_{-3}$ depending on the assumed age of the field population ($0.9-3.1$ Gyr). We attribute the change in values to our use of kernel-phase interferometry which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously-seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age sub-stellar regime; only $0.9^{+1.1}_{-0.6}$ % of systems are wider than 20 au and $

Asgard NOTT: L-band nulling interferometry at the VLTI I Simulating the expected high-contrast performance by Romain Laugier et al. on Monday 21 November Context: NOTT (formerly Hi-5) is a new high-contrast L' band (3.5-4.0 textmu m) beam combiner for the VLTI with the ambitious goal to be sensitive to young giant exoplanets down to 5 mas separation around nearby stars. The performance of nulling interferometers in these wavelengths is affected both by fundamental noise from the background and by the contributions of instrumental noises. This motivates the development of end-to-end simulations to optimize these instruments. Aims: To enable the performance evaluation and inform the design of such instruments on the current and future infrastructures, taking into account the different sources of noise, and their correlation. Methods: SCIFYsim is an end-to-end simulator for single mode filtered beam combiners, with an emphasis on nulling interferometers. It is used to compute a covariance matrix of the errors. Statistical detection tests based on likelihood ratios are then used to compute compound detection limits for the instrument. Results: With the current assumptions on the performance of the wavefront correction systems, the errors are dominated by correlated instrumental errors down to stars of magnitude 6-7 in the L band, beyond which thermal background from the telescopes and relay system becomes dominant. Conclusions: SCIFYsim is suited to anticipate some of the challenges of design, tuning, operation and signal processing for integrated optics beam combiners. The detection limits found for this early version of NOTT simulation with the unit telescopes are compatible with detections at contrasts up to $10^5$ in the L band at separations of 5 to 80 mas around bright stars. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.09548v1

Detecting planetary mass companions near the water frost-line using JWST interferometry by Shrishmoy Ray et al. on Monday 21 November JWST promises to be the most versatile infrared observatory for the next two decades. The Near Infrared and Slitless Spectrograph (NIRISS) instrument, when used in the Aperture Masking Interferometry (AMI) mode, will provide an unparalleled combination of angular resolution and sensitivity compared to any existing observatory at mid-infrared wavelengths. Using simulated observations in conjunction with evolutionary models, we present the capability of this mode to image planetary mass companions around nearby stars at small orbital separations near the circumstellar water frost-line for members of the young, kinematic moving groups Beta Pictoris, TW Hydrae, as well as the Taurus-Auriga association. We show that for appropriately chosen stars, JWST/NIRISS operating in the AMI mode can image sub-Jupiter companions near the water frost-lines with ~68% confidence. Among these, M-type stars are the most promising. We also show that this JWST mode will improve the minimum inner working angle by as much as ~50% in most cases when compared to the survey results from the best ground-based exoplanet direct imaging facilities (e.g. VLT/SPHERE). We also discuss how the NIRISS/AMI mode will be especially powerful for the mid-infrared characterization of the numerous exoplanets expected to be revealed by Gaia. When combined with dynamical masses from Gaia, such measurements will provide a much more robust characterization of the initial entropies of these young planets, thereby placing powerful constraints on their early thermal histories. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.09830v1

Detecting planetary mass companions near the water frost-line using JWST interferometry by Shrishmoy Ray et al. on Monday 21 November JWST promises to be the most versatile infrared observatory for the next two decades. The Near Infrared and Slitless Spectrograph (NIRISS) instrument, when used in the Aperture Masking Interferometry (AMI) mode, will provide an unparalleled combination of angular resolution and sensitivity compared to any existing observatory at mid-infrared wavelengths. Using simulated observations in conjunction with evolutionary models, we present the capability of this mode to image planetary mass companions around nearby stars at small orbital separations near the circumstellar water frost-line for members of the young, kinematic moving groups Beta Pictoris, TW Hydrae, as well as the Taurus-Auriga association. We show that for appropriately chosen stars, JWST/NIRISS operating in the AMI mode can image sub-Jupiter companions near the water frost-lines with ~68% confidence. Among these, M-type stars are the most promising. We also show that this JWST mode will improve the minimum inner working angle by as much as ~50% in most cases when compared to the survey results from the best ground-based exoplanet direct imaging facilities (e.g. VLT/SPHERE). We also discuss how the NIRISS/AMI mode will be especially powerful for the mid-infrared characterization of the numerous exoplanets expected to be revealed by Gaia. When combined with dynamical masses from Gaia, such measurements will provide a much more robust characterization of the initial entropies of these young planets, thereby placing powerful constraints on their early thermal histories. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.09830v1

Observing inside the coronagraphic regime with optimized single-mode nulling interferometry by E. Serabyn et al. on Tuesday 18 October The number of terrestrial exoplanets accessible to high-contrast coronagraphic imaging with large telescopes is limited by the smallest angular offset from bright stars at which coronagraphs can observe. However, it is possible to reach inside a telescopes coronagraphic regime by employing nulling interferometry across a telescopes pupil. Indeed, cross-aperture nulling interferometry can observe significantly closer to stars than typical coronagraphs, enabling observations even within the stellar diffraction core. Identifying an optimal nulling coronagraph, i.e., one with both a very small IWA and a high throughput for exoplanet light, would thus be of great interest. A systematic examination of available nulling options has therefore been carried out, which has led to three things. The first is a topological overview that unites both multi-aperture nulling interferometers and single-aperture phase coronagraphs into a common geometrical framework. The second is a new type of phase-mask coronagraph that has emerged from a gap in this framework, called here the split-ring coronagraph. The third is a clear identification of the optimal configuration for a nulling coronagraph, which turned out to be an aperture-plane phase knife, i.e., an achromatic pi-radian phase shift applied to half the telescope pupil prior to focusing the telescopes point spread function into a single-mode fiber. The theoretical peak efficiency of the phase-knife fiber coronagraph, 35.2 percent for a circular telescope aperture, is found to be almost twice that of the next most efficient case, the vortex fiber nuller, at 19.0 percent. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.09412v1

Solar System-scale interferometry on fast radio bursts could measure cosmic distances with sub-percent precision by Kyle Boone et al. on Sunday 16 October The light from a source at a distance d will arrive at detectors separated by 100 AU at times that differ by as much as 120 (d/100 Mpc)^{-1} nanoseconds because of the curvature of the wavefront. At gigahertz frequencies, the arrival time difference can be determined to better than a nanosecond with interferometry. If the space-time positions of the detectors are known to a few centimeters, comparable to the accuracy to which very long baseline interferometry baselines and global navigation satellite systems (GNSS) geolocations are constrained, nanosecond timing would allow competitive cosmological constraints. We show that a four-detector constellation at Solar radii of >10 AU could measure distances to individual sources with sub-percent precision and, hence, cosmological parameters such as the Hubble constant to this precision. FRBs are the only known bright extragalactic radio source that are sufficiently point-like. Galactic scattering limits the timing precision at

Solar System-scale interferometry on fast radio bursts could measure cosmic distances with sub-percent precision by Kyle Boone et al. on Sunday 16 October The light from a source at a distance d will arrive at detectors separated by 100 AU at times that differ by as much as 120 (d/100 Mpc)^{-1} nanoseconds because of the curvature of the wavefront. At gigahertz frequencies, the arrival time difference can be determined to better than a nanosecond with interferometry. If the space-time positions of the detectors are known to a few centimeters, comparable to the accuracy to which very long baseline interferometry baselines and global navigation satellite systems (GNSS) geolocations are constrained, nanosecond timing would allow competitive cosmological constraints. We show that a four-detector constellation at Solar radii of >10 AU could measure distances to individual sources with sub-percent precision and, hence, cosmological parameters such as the Hubble constant to this precision. FRBs are the only known bright extragalactic radio source that are sufficiently point-like. Galactic scattering limits the timing precision at

The effect of winds in red supergiants: modeling for interferometry by Gemma González-Torà et al. on Monday 10 October Red supergiants (RSGs) are evolved massive stars in a stage preceding core-collapse supernova. Understanding evolved-phases of these cool stars is key to understanding the cosmic matter cycle of our Universe, since they enrich the cosmos with newly formed elements. However, the physical processes that trigger mass loss in their atmospheres are still not fully understood, and remain one of the key questions in stellar astrophysics. We use a new method to study the extended atmospheres of these cold stars, exploring the effect of a stellar wind for both a simple radiative equilibrium model and a semi-empirical model that accounts for a chromospheric temperature structure. We then can compute the intensities, fluxes and visibilities matching the observations for the different instruments at the Very Large Telescope Interferometer (VLTI). Specifically, when comparing with the atmospheric structure of HD 95687 based on published VLTI/AMBER data, we find that our model can accurately match these observations in the Kband, showing the enormous potential of this methodology to reproduce extended atmospheres of RSGs. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.04495v1

Characterization of Mid-Infrared Intersubband Detectors for Astronomical Heterodyne Interferometry by Tituan Allain et al. on Sunday 18 September One of the major challenges of mid-infrared astronomical heterodyne interferometry is its sensitivity limitations. Detectors capable of handling several 10 GHz bandwidths have been identified as key building blocks of future instruments. Intersubband detectors based on heterostructures have recently demonstrated their ability to provide such performances. In this work we characterize a Quantum Well Infrared Photodetector in terms of noise, dynamic range and bandwidth in a non-interferometric heterodyne set-up. We discuss the possibility to use them on astronomical systems to measure the beating between the local oscillator and the astronomical signal. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07789v1

Parallel faceted imaging in radio interferometry via proximal splitting Faceted HyperSARA : II Code and real data proof of concept by Pierre-Antoine Thouvenin et al. on Sunday 18 September In a companion paper, a faceted wideband imaging technique for radio interferometry, dubbed Faceted HyperSARA, has been introduced and validated on synthetic data. Building on the recent HyperSARA approach, Faceted HyperSARA leverages the splitting functionality inherent to the underlying primal-dual forward-backward algorithm to decompose the image reconstruction over multiple spatio-spectral facets. The approach allows complex regularization to be injected into the imaging process while providing additional parallelization flexibility compared to HyperSARA. The present paper introduces new algorithm functionalities to address real datasets, implemented as part of a fully fledged MATLAB imaging library made available on Github. A large scale proof-of-concept is proposed to validate Faceted HyperSARA in a new data and parameter scale regime, compared to the state-of-the-art. The reconstruction of a 15 GB wideband image of Cyg A from 7.4 GB of VLA data is considered, utilizing 1440 CPU cores on a HPC system for about 9 hours. The conducted experiments illustrate the reconstruction performance of the proposed approach on real data, exploiting new functionalities to set, both an accurate model of the measurement operator accounting for known direction-dependent effects (DDEs), and an effective noise level accounting for imperfect calibration. They also demonstrate that, when combined with a further dimensionality reduction functionality, Faceted HyperSARA enables the recovery of a 3.6 GB image of Cyg A from the same data using only 91 CPU cores for 39 hours. In this setting, the proposed approach is shown to provide a superior reconstruction quality compared to the state-of-the-art wideband CLEAN-based algorithm of the WSClean software. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07604v1

Parallel faceted imaging in radio interferometry via proximal splitting Faceted HyperSARA : I Algorithm and simulations by Pierre-Antoine Thouvenin et al. on Sunday 18 September Upcoming radio interferometers are aiming to image the sky at new levels of resolution and sensitivity, with wide-band image cubes reaching close to the Petabyte scale for SKA. Modern proximal optimization algorithms have shown a potential to significantly outperform CLEAN thanks to their ability to inject complex image models to regularize the inverse problem for image formation from visibility data. They were also shown to be parallelizable over large data volumes thanks to a splitting functionality enabling the decomposition of the data into blocks, for parallel processing of block-specific data-fidelity terms involved in the objective function. Focusing on intensity imaging, the splitting functionality is further exploited in this work to decompose the image cube into spatio-spectral facets, and enable parallel processing of facet-specific regularization terms in the objective function, leading to the "Faceted HyperSARA" algorithm. Reliable heuristics enabling an automatic setting of the regularization parameters involved in the objective are also introduced, based on estimates of the noise level, transferred from the visibility domain to the domains where the regularization is applied. Simulation results based on a MATLAB implementation and involving synthetic image cubes and data close to Gigabyte size confirm that faceting can provide a major increase in parallelization capability when compared to the non-faceted approach (HyperSARA). arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2003.07358v2

Simulations of astrometric planet detection in Alpha Centauri by intensity interferometry by Km Nitu Rai et al. on Wednesday 14 September Recent dynamical studies indicate that the possibility of an Earth-like planet around $alpha;$Cen A or B should be taken seriously. Such a planet, if it exists, would perturb the orbital astrometry by $

Investigating the accuracy achievable in reconstructing the angular sizes of stars through stellar intensity interferometry observations by Michele Fiori et al. on Tuesday 13 September Context: In recent years, stellar intensity interferometry has seen renewed interest from the astronomical community because it can be efficiently applied to Cherenkov telescope arrays. Aims: We have investigated the accuracy that can be achieved in reconstructing stellar sizes by fitting the visibility curve measured on the ground. The large number of expected available astronomical targets, the limited number of nights in a year, and the likely presence of multiple baselines will require careful planning of the observational strategy to maximise the scientific output. Methods: We studied the trend of the error on the estimated angular size, considering the uniform disk model, by varying several parameters related to the observations, such as the total number of measurements, the integration time, the signal-to-noise ratio, and different positions along the baseline. Results: We found that measuring the value of the zero-baseline correlation is essential to obtain the best possible results. Systems that can measure this value directly or for which it is known in advance will have better sensitivity. We also found that to minimise the integration time, it is sufficient to obtain a second measurement at a baseline half-way between 0 and that corresponding to the first zero of the visibility function. This function does not have to be measured at multiple positions. Finally, we obtained some analytical expressions that can be used under specific conditions to determine the accuracy that can be achieved in reconstructing the angular size of a star in advance. This is useful to optimise the observation schedule. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.12277v2

Controlling petals using fringes: discontinuous wavefront sensing through sparse aperture interferometry at Subaru SCExAO by Vincent Deo et al. on Wednesday 07 September Low wind and petaling effects, caused by the discontinuous apertures of telescopes, are poorly corrected -- if at all -- by commonly used workhorse wavefront sensors (WFSs). Wavefront petaling breaks the coherence of the point spread function core, splitting it into several side lobes, dramatically shutting off scientific throughput. We demonstrate the re-purposing of non-redundant sparse aperture masking (SAM) interferometers into low-order WFSs complementing the high-order pyramid WFS, on the SCExAO experimental platform at Subaru Telescope. The SAM far-field interferograms formed from a 7-hole mask are used for direct retrieval of petaling aberrations, which are almost invisible to the main AO loop. We implement a visible light dual-band SAM mode, using two disjoint 25 nm wide channels, that we recombine to overcome the one-lambda ambiguity of fringe-tracking techniques. This enables a control over petaling with sufficient capture range yet without conflicting with coronagraphic modes in the near-infrared. We present on-sky engineering results demonstrating that the design is able to measure petaling well beyond the range of a single-wavelength equivalent design. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02898v1

Intensity Interferometry at Calern and beyond: progress report by Nolan Matthews et al. on Tuesday 06 September We present the current status of the I2C stellar intensity interferometer used towards high angular resolution observations of stars in visible wavelengths. In these proceedings, we present recent technical improvements to the instrument, and share results from ongoing campaigns using arrays of small diameter optical telescopes. A tip-tilt adaptive optics unit was integrated into the optical system to stabilize light injection into an optical fiber. The setup was successfully tested with several facilities on the Calern Plateau site of the Observatoire de la C^ote d'Azur. These include one of the 1 m diameter telescopes of the C2PU observatory, a portable 1 m diameter telescope, and also the 1.5 m M'eO telescope. To better constrain on-sky measurements, the spectral transmission of instrument was characterized in the laboratory using a high resolution spectrograph. The system was also tested with two of the auxiliary telescopes of the VLTI resulting in successful temporal and spatial correlation measurements of three stars. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02477v1

There's so much we don't know, or take for granted, about the way life really works on this planet. There's the biosphere, which includes the soft electricity of the Terran Field. I coined the words “Terran Field” to describe the background organic electrical nature of the interplay between life on the planet's surface and its oceans, and the upper atmospheric structures that feed subtle electrical energies between the ionosphere and ground. Lightning for example - without it we wouldn't have life, or the components that create and sustain life. Over the past half century some members of the military-scientific community have discovered some of what Tesla understood, and weaponized it for their own purposes. As a result, much of what we witness or experience daily now is degrading our life experience, or the ability of the planet to sustain itself. Geoengineering, smartphones, smart meters, 5G, nano particulates, graphene oxide, mind control…nefarious activity that victimizes the unawares. We must become aware to change course…we need to understand to respond. Are you ready to jump down the rabbit hole with me?Presented by Isaac George: https://IsaacGeorge.comAll Contact Info and Social Media: https://www.isaacgeorge.com/stay-in-touch-with-isaac.htmlFacebook: https://www.facebook.com/isaacgeorge999LinkedIn: https://www.linkedin.com/in/isaac-george-2736495a/MeWe: https://mewe.com/i/isaacgeorgeSoul Matrix: https://oursocialmatrix.com/profile/?arion/Tune into the show live on KindaSound Radio every Sunday: https://KindaSound.orgConnect with the KindaSound team on Telegram: https://t.me/ksradioNew podcast episodes every Thursday

Laura Pinzon-Rincon, Université Grenoble Alpes Seismologists eagerly seek new and preferably low-cost ways to map and monitor the complex structure of the top few kilometers of the crust. Passive seismic imaging appears as a novel, low-cost, and environmentally-friendly approach for exploring the sub-surface. Usually, passive seismic interferometry relies on blind correlations within long time series of seismic noise or coda waves. Here, we propose a complementary approach: seismic interferometry using opportune sources, specifically moving sources that are not stationary in time. This new approach relies on an accurate understanding of the seismic source's mechanism, a careful signal time-window and station pairs selection, and seismic phase identification. For example, massive freight trains were only recently recognized as a persistent, powerful cultural (human activity-caused) seismic source. Thus, these train signals can be considered an opportune seismic source for passive seismic interferometry because they are readily available, detectable, repeatable, and generate high-frequency broadband energy. To illustrate this novel method's potential, we show a case study in a mineral exploration context at the Marathon site, Ontario, Canada, where we deployed a dense nodal array of 1020 sensors. We retrieve high-frequency energy using train signals only, and we use these arrivals to generate a 3D shear-wave velocity model. We discuss the pros and cons of the method compared to more standard approaches with the help of numerical modeling. We showed that by correlating train tremors, we retrieved high-frequency arrivals with higher quality than using the standard method while using fewer data. Far from being restrained to near-surface imaging, this new way of analyzing opportune seismic sources can be applied in various contexts and scales using natural or man-generated signals.

Radio frequency inteferometric lightning maps are important tools for researchers exploring the electrical processes that unfold within storm clouds. Dr Xuan-Min Shao and colleagues at Los Alamos National Laboratory in New Mexico, who first introduced broadband interferometry to lightning research over two decades ago, have now developed an advanced ‘beam steering' interferometry technique to significantly improve the accuracy of lightning mapping. This approach, together with their recently developed polarisation detection technique, has begun to reveal new physics involved in lightning discharges. Their recent work shows how lightning initiation, which has been poorly understood until now, may be linked to high-energy cosmic particles entering Earth's atmosphere.

Measuring optics is a precision practice, and it's made possible with laser interferometry. In this episode of Metrology Matters, host Tyler Kern kicks off a series on laser interferometry with an introductory episode discussing the practice with Kate Medicus, CEO of Ruda Cardinal, and Bruce Truax, Director of Engineering at ZYGO, to delve into this core technology and to better understand its many use cases in numerous industries.

A. Shaw - Exploring foot-and-mouth disease virus antibody affinity using bio-layer interferometry​ by European Commission for the Control of FMD

Searching... Clean and resolve! Check out the paper: https://arxiv.org/abs/2008.11435

Link to bioRxiv paper: http://biorxiv.org/cgi/content/short/2020.10.20.348060v1?rss=1 Authors: KHODR, V., MACHILLOT, P., MIGLIORINI, E., REISER, J.-b., PICART, C. Abstract: Bone morphogenetic proteins (BMP) are an important family of growth factors playing a role in a large number of physiological and pathological processes, including bone homeostasis, tissue regeneration and cancers. In vivo, BMPs bind successively to both BMP receptors (BMPR) of type I and type II, and a promiscuity has been reported. In this study, we used bio-layer interferometry to perform parallel real-time biosensing and to deduce the kinetic parameters (ka, kd) and the equilibrium constant (KD) for a large range of BMPs/BMPR combinations in similar experimental conditions. We selected four members of the BMP family (BMP-2, 4, 7, 9) known for their physiological relevance and studied their interactions with five type-I BMP receptors (ALK1, 2, 3, 5, 6) and three type-II BMP receptors (BMPR-II, ACTR-IIA, ACTR-IIB). We reveal that BMP-2 and BMP-4 behave differently, especially regarding their kinetic interactions and affinities with the type-II BMPR. We found that BMP-7 has a higher affinity for ACTR-IIA and a tenfold lower affinity with the type-I receptors. While BMP-9 has a high and similar affinity for all type-II receptors, it can interact with ALK5 and ALK2, in addition to ALK1. Interestingly, we also found that all BMPs can interact with ALK5. The interaction between BMPs and both type-I and type II receptors immobilized on the same surface did not reveal further cooperativity. Our work provides a synthetic view of the interactions of these BMPs with their receptors and paves the way for future studies on their cell-type and receptor specific signaling pathways. Copy rights belong to original authors. Visit the link for more info

Sound waves have air, water waves have...well...water, but what about light waves? In Part 1 of this two-part episode, Beth explains the concept behind interferometry, and how we discovered what light does (or doesn't) travel through! https://linktr.ee/notyetadr Edited by: Alastair Questions or Suggestions? Email us at phd32b@gmail.com

http://www.astronomycast.com/archive/ From March 9, 2009. When it comes to telescopes, bigger is better. But bigger is more expensive. Way more expensive. To keep the costs reasonable while improving the sensitivity of their instruments, astronomers use an amazing technique called interferometry. Instead of building a single huge telescope, you can merge the light from several telescopes to act like a much larger telescope. It’s a technique that has already revolutionized Earth-based observing – but just wait until it gets into space…   We've added a new way to donate to 365 Days of Astronomy to support editing, hosting, and production costs. Just visit: https://www.patreon.com/365DaysOfAstronomy and donate as much as you can! Share the podcast with your friends and send the Patreon link to them too! Every bit helps! Thank you! ------------------------------------ Do go visit http://astrogear.spreadshirt.com/ for cool Astronomy Cast and CosmoQuest t-shirts, coffee mugs and other awesomeness! http://cosmoquest.org/Donate This show is made possible through your donations. Thank you! (Haven't donated? It's not too late! Just click!) The 365 Days of Astronomy Podcast is produced by Astrosphere New Media. http://www.astrosphere.org/ Visit us on the web at 365DaysOfAstronomy.org or email us at info@365DaysOfAstronomy.org.

You might not know it, but Melbourne has little earthquakes, even in the city centre and quite frequently.So says Michael Webster, engineering geologist at consulting, design and construction company, Golder Associates, and guest lecturer for the Master of Engineering at the University of Melbourne.“A lot of people know about the earthquakes down in Gippsland or the Otways, but actually in Melbourne itself, there have been earthquakes. You’d have to be a seismic instrument to actually feel these ones but they are there at all depths – some of them quite deep, some of them shallow,” he says.From the geology beneath Melbourne, Michael has created an intricate, three dimensional picture.“There are two lava flows under Melbourne, so you effectively get these beautiful layers cutting across each other, building up over about three to four million years to the present day,” he says.“So, in collaboration with the Arts Centre Melbourne and Development Victoria, we 3D printed a ground model and put on an exhibition at the Testing Grounds in Southbank.“It ran for a few weeks and it was lovely to see people’s interest and connection with the ground.“I’ve always found that geology is one of the more approachable sciences. If people talk about gravity waves it’s absolutely fascinating, but with geology it’s there – it is rivers, volcanos, lava.”Episode recorded: September 17, 2019.Interviewer: Dr Andi Horvath.Producer, editor and audio engineer: Chris Hatzis.Co-production: Silvi Vann-Wall and Dr Andi Horvath.Banner image: Golder Associates.

Wenn man das Universum richtig gut sehen will, dann braucht man Teleskope mit Löchern. Die Technik nennt sich "Interferometrie". Und sie hat die Aufnahme des ersten Bilds eines schwarzen Lochs möglich gemacht. Wie das geht erfahrt ihr in der neuen Folge des Sternengeschichten-Podcast.

After many bouts of lightning round, we finally got our lightning questions answered by Eric Brunning (@deeplycloudy). Eric is a Professor of Atmospheric Sciences at Texas Tech University specializing in storm electrification and lightning . You can hear some of Eric’s field adventures by listening to his episode of the Don’t Panic Geocast show. The Wikipedia page for lightning will lead you down many strange pathways. Though the Wikipedia Lightning Energy Harvesting page may convince you that it isn’t feasible (though some math might as well, as discussed on this show). For more about lightning interferometry, check out Michael Stock’s in-depth site. You can hear lightning on Jupiter if you listen to the right bands. Neat video of the Milky Way in radio waves reflecting off the moon Elecia really enjoyed The Cloudspotter’s Guide by Gavin Pretor-Pinney.

Harold McAlister from Georgia State University delivers a talk titled “Optical Interferometry: Ensuring Mount Wilson’s Second Century of Science.” This talk was included in the session titled “Taking the Measurement of the Stars. Part of “First Light: The Astronomy Century in California, 1917–2017,” a conference held at The Huntington Nov. 17–18, 2017.

Join Emma Barnett and Science & Discovery category judge Professor Lord Robert Winston as we continue our journey through the history of science and discovery in England. Visit Jodrell Bank Observatory, home to two Grade I listed radio telescopes and a centre for groundbreaking research in the fields of astronomy and interferometry, as we explore why ten places have been chosen from hundreds of your nominations. Nominate a place at HistoricEngland.org.uk/100Places A History of England in 100 Places is a Historic England podcast, sponsored by specialist insurer Ecclesiastical ecclesiastical.com

Given by Professor Charles Clark, Fellow of the Physical Measurement Laboratory at the National Institute of Standards and Technology, and Fellow and Adjunct Professor at the Joint Quantum Institute, University of Maryland, USA. Wave motions in nature were known to the ancients, and their mathematical expression in physics today is essentially the same as that first provided by d'Alembert and Euler in the mid-18th century. Yet it was only in the early 1990s that physicists managed to control a basic property of light waves: their capability of swirling around their own axis of propagation. During the past decade such techniques of control have also been developed for quantum particles: atoms, electrons and neutrons. I will present a simple description of these phenomena, emphasising the most basic aspects of wave and quantum particle motion. Neutron interferometry offers a poignant perspective on wave-particle duality: at the time one neutron is detected, the next neutron has not yet even been born. Here, indeed, each neutron "then only interferes with itself." Yet, using macroscopically-machined objects, we are able to twist neutron deBroglie waves with sub-nanometer wavelengths.

Physics Colloquium 10th June 2016 delivered by Professor Swapan Chattopadhyay Tremendous advances have been made in the last two decades in precision ‘Quantum' technologies and techniques in multiple disciplines e.g. cavity electrodynamics, atomic beam interferometry, SQUIDS, quantum optical “squeezed state” techniques for noise-free single photon detection, qubit-based quantum entanglement techniques, high-Q superconducting cavities, precision NMR detection via designer materials, etc. These advances promise to enable transformational research using ultra-sensitive probes to explore very “weak effects” on a laboratory scale. These weak effects are manifest everywhere in nature in material and living systems from the laboratory to outer space. Potential “mezzo-scale” experiments and facilities can be envisaged using “quantum sensors” to search for ultra-weak physical, chemical or biological signals of fundamental significance to the material and living world around us as well as explore the “inner” and “outer” dimension of “vacuum” believed to be manifest in the so-called “dark” universe. This talk will illustrate this potential via a few exciting examples discussed at the recent US DOE Round Table on Quantum Sensors in February 2016.

In this episode we host Omair Taibah to talk about the latest breakthrough in astrophysics and the detection of gravitational waves resulting from two black holes colliding billions of light years away. Show Links Loot Crate Interferometry  Eliminating terrestrial noise sources to improve the LIGO gravity wave detectors  LIGO Gravitational Wave Chirp The Perfect Theory A Short History of Nearly Everything Dark Matter and the Dinosaurs Musicophilia The Information: A History, A Theory, A Flood “Tsundoku,” the Japanese Word for the New Books That Pile Up on Our Shelves 20% Arabic – 80% English

Radio telescopes have really crummy resolution.but if we line them up and hook them together,  using a technique called "radio interferometry"  we can see the head of a screw 300 km away.   This episode, our guest is Ben Acker, one of the authors of "the thrilling adventure hour". amazing! Our Physicists are Rupinder Brar and Sabrina Stierwalt! exciting!

Tue, 9 Oct 2012 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/14934/ https://edoc.ub.uni-muenchen.de/14934/1/Grellmann_Rebekka.pdf Grellmann, Rebekka ddc:530, ddc:500, Fakultät für Physik

Caltech's Yanbei Chen discusses fundamentals of optical interferometry for gravitational wave detection (June 25, 2012).

Caltech's Yanbei Chen discusses fundamentals of optical interferometry for gravitational wave detection (June 25, 2012).

Thu, 29 Sep 2011 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/13526/ https://edoc.ub.uni-muenchen.de/13526/1/Ricci_Luca.pdf Ricci, Luca

Transcript -- How do radio astronomers see jets far outside our galaxy? Introducing the MERLIN array in the UK and the VLA in New Mexico.

How do radio astronomers see jets far outside our galaxy? Introducing the MERLIN array in the UK and the VLA in New Mexico.

Transcript -- How do radio astronomers see jets far outside our galaxy? Introducing the MERLIN array in the UK and the VLA in New Mexico.

How do radio astronomers see jets far outside our galaxy? Introducing the MERLIN array in the UK and the VLA in New Mexico.

Radio telescopes must be very large in size to achieve the same resolution as optical telescopes. The only way to do this is by coupling two or more of them, the further apart the better, and to analyse their combined signals. An interferometer is a system which can avoid increased expenses due to the large size of the receiver. It consists of two or more elements of large antennae. By connecting them in a special fashion, it is possible to artificially create a larger telescope. The European hub for what is called Very Long Baseline Interferometry (VLBI) is situated in Dwingeloo in the Netherlands, at the Joint Institute for VLBI in Europe, JIVE.ESApod video programme

If technology, cost, and terrain permitted, scientists seeking key data on stars in our galaxy would have loved to construct a behemoth 330 m wide telescope atop Mount Wilson, just northeast of Los Angeles. Instead, they arranged six smaller telescopes over an identical area, synchronizing the light to achieve an equally superlative resolution. Called the Center for High Angular Resolution Astronomy (CHARA), the array uses the technique of interferometry to spot details the size of a nickel seen from 16,000 km away. Hear from project astronomers why the labyrinthine engineering required for CHARA’s renowned precision is a small sacrifice for the valuable data it gleans on the properties and life cycles of stars.