Modelling the Galactic bar using OGLE-II Red Clump Giant Stars

Red clump giant stars can be used as distance indicators to trace the mass distribution of the Galactic bar. We use RCG stars from 44 bulge fields from the OGLE-II microlensing collaboration database to constrain analytic tri-axial models for the Galactic bar. We find the bar major axis is oriented at an angle of 24 - 27 degrees to the Sun-Galactic centre line-of-sight. The ratio of semi-major and semi-minor bar axis scale lengths in the Galactic plane x_0, y_0, and vertical bar scale length z_0, is x_0 : y_0 : z_0 = 10 : 3.5 : 2.6, suggesting a slightly more prolate bar structure than the working model of Gerhard (2002) which gives the scale length ratios as x_0 : y_0 : z_0 = 10 : 4 : 3 .Comment: 15 pages, 10 figures, accepted for publication in MNRAS. Supplementary material available online: 10 pages, 10 figure

Microlensing of close binary stars

The gravity due to a multiple-mass system has a remarkable gravitational effect: the extreme magnification of background light sources along extended so-called caustic lines. This property has been the channel for some remarkable astrophysical discoveries over the past decade, including the detection and characterisation of extra-solar planets, the routine analysis of limb-darkening, and, in one case, limits set on the apparent shape of a star several kiloparsec distant. In this paper we investigate the properties of the microlensing of close binary star systems. We show that in some cases it is possible to detect flux from the Roche lobes of close binary stars. Such observations could constrain models of close binary stellar systems.Comment: 10 pages, accepted to MNRA

Predictions for the Detection and Characterization of a Population ofFree-floating Planets with K2 Campaign 9

K2 Campaign 9 (K2C9) offers the first chance to measure parallaxes and masses of members of the large population of free-floating planets (FFPs) that has previously been inferred from measurements of the rate of short-timescale microlensing events. Using detailed simulations of the nominal campaign (ignoring the loss of events due to Kepler\u27s emergency mode) and ground-based microlensing surveys, we predict the number of events that can be detected if there is a population of 1 MjupiterFFPs matching current observational constraints. Using a Fisher matrix analysis, we also estimate the number of detections for which it will be possible to measure the microlensing parallax, angular Einstein radius, and FFP mass. We predict that between 1.4 and 7.9 events will be detected in the K2 data, depending on the noise floor that can be reached, but with the optimistic scenario being more likely. For nearly all of these, it will be possible to either measure the parallax or constrain it to be probabilistically consistent with only planetary-mass lenses. We expect that for between 0.42 and 0.98 events it will be possible to gain a complete solution and measure the FFP mass. For the emergency-mode truncated campaign, these numbers are reduced by 20 percent. We argue that when combined with prompt high-resolution imaging of a larger sample of short-timescale events, K2C9 will conclusively determine if the putative FFP population is indeed both planetary and free-floating

Taiaho Observatory: An Automated Future Optical Communications Ground Station

Free Space Optical Communications (FSOC) is the next revolution in high-bandwidth satellite-to-earth data transmission. The critical challenge facing the widespread, commercial adoption of FSOC is requirement of a cloud-free line of sight (CFLOS) between the spaceborne asset and the optical ground station (OGS). One solution to this problem is the use of multiple OGSs in a geographically distributed network. Such networks include the European Optical Nucleus Network (EONN) and the Australasian Optical Ground Station Network (AOGSN). To transition from research to commercialization will necessitate an increase in the number of OGSs and their continuous operation. Automation will play a critical role in enabling 24/7 link availability by reducing the number of required operators per OGS. OGS automation will consist of several discrete control loops including: network-wide astronomical seeing comparisons; assessment of local atmospheric conditions to permit operation; short term cloud cover prediction over the satellite pass; calibration of the pointing model; and tracking the asset pass. Fully automated ground stations would enable near-seamless switching between OGS nodes during a pass, further increasing the link time. The work begun at Taiaho is focused on a single-node automation; weather monitoring, cloud predictions, and pass tracking. These goals are achievable through a combination of modern hardware and software, including a state-of-the-art weather and atmospheric turbulence monitoring station (ISM, Miratlas SAS), a direct-drive telescope mount with integrated pointing model (L350, Planewave Instruments Inc.), and a custom software framework linking these with a command-and-control suite

Data Processing Techniques for Ion and Electron Energy Distribution Functions

Retarding field energy analyzers and Langmuir probes are routinely used to obtain ion and electron energy distribution functions (IEDF, EEDF). These typically require knowledge of the first and second derivatives of the I-V characteristics, both of which can be obtained in various ways. This poses challenges inherent to differentiating noisy signals, a frequent problem with electric-probe plasma diagnostics. A brief review of commonly used analog and numerical filtering and differentiation techniques is presented, together with their application on experimental data collected in a radio-frequency plasma. The application of each method is detailed with regards to the obtained IEDF and EEDF, the deduced plasma parameters, dynamic range, energy resolution and signal distortion.Comment: A.C. and F.F. are co-first authors. The following article has been submitted to Physics of Plasmas. After it is published, it will be found at https://aip.scitation.org/journal/ph

Helicon waves in a converging-diverging magnetoplasma

Waves propagating along a converging-diverging rf magnetoplasma having the characteristics of a bounded m=0 helicon mode are reported and characterised. The discharge features a 30 cm separation between the region of radiofrequency energy deposition by a single loop antenna and the region of maximum magnetic field applied by a pair of coils. With 200 W of rf input power, the resulting plasma exhibits a strong axial plasma density gradient peaking at the magnetic mirror throat where an Ar II blue-core is observed. Two dimensional B-dot probe measurements show that the rf magnetic fields are closely guided by the converging-diverging geometry. The wave is characterised as a m=0 mode satisfying the helicon dispersion relation on-axis with radial boundary conditions approximately matching the radii of the plasma column. Analysis of the wave phase velocity and wave axial damping failed to identify collisionless or collisional wave-plasma coupling mechanisms. Instead, the wave axial amplitude variations can be explained by local wave resonances and possible reflections from localised rapid changes of the refractive index. A Venturi-like effect owing to the funnel-shaped magnetoplasma and conservation of the wave energy may also explain some level of amplitude variations.Comment: The following article has been submitted to Plasma Sources Science and Technolog

Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey

The PRime-focus Infrared Microlensing Experiment (PRIME) will be the first to conduct a dedicated near infrared (NIR) microlensing survey by using a 1.8m telescope with a wide field of view of 1.45 ${\rm deg^{2}}$ at the South African Astronomical Observatory (SAAO). The major goals of the PRIME microlensing survey are to measure the microlensing event rate in the inner Galactic bulge to help design the observing strategy for the exoplanet microlensing survey by the {\it Nancy Grace Roman Space Telescope} and to make a first statistical measurement of exoplanet demographics in the central bulge fields where optical observations are very difficult owing to the high extinction in these fields. Here we conduct a simulation of the PRIME microlensing survey to estimate its planet yields and determine the optimal survey strategy, using a Galactic model optimized for the inner Galactic bulge. In order to maximize the number of planet detections and the range of planet mass, we compare the planet yields among four observation strategies. Assuming {the \citet{2012Natur.481..167C} mass function as modified by \citet{2019ApJS..241....3P}}, we predict that PRIME will detect planetary signals for $42-52$ planets ($1-2$ planets with $M_p \leq 1 M_\oplus$, $22-25$ planets with mass $1 M_\oplus < M_p \leq 100 M_\oplus$, $19-25$ planets $100 M_\oplus < M_p \leq 10000 M_\oplus$), per year depending on the chosen observation strategy.Comment: 25 pages, 17 figures, and 3 tables. Accept for publication in The Astronomical Journa

Mapping Guaranteed Positive Secret Key Rates for Continuous Variable Quantum Key Distribution

Continuous variable quantum key distribution (CVQKD) is the sharing of secret keys between different parties using the continuous amplitude and phase quadratures of light. There are many protocols in which different modulation schemes are used to implement CVQKD. However, there has been no tool for comparison between different CVQKD protocols to determine the optimal protocol for varying channels while simultaneously taking into account the effects of different parameters. Here, a comparison tool has been developed to map regions of positive secret key rate (SKR), given a channel's transmittance and excess noise, where a user's modulation can be adjusted to guarantee a positive SKR in an arbitrary environment. The method has been developed for discrete modulated CVQKD (DM-CVQKD) protocols but can be extended to other current and future protocols and security proofs.Comment: 15 pages, 9 figure

Proper Motion Dispersions of Red Clump Giants in the Galactic Bulge: Observations and Model Comparisons

Red clump giants in the Galactic bulge are approximate standard candles and hence they can be used as distance indicators. We compute the proper motion dispersions of RCG stars in the Galactic bulge using the proper motion catalogue from the second phase of the Optical Gravitational Microlensing Experiment (OGLE-II, Sumi et al. 2004) for 45 fields. The proper motion dispersions are measured to a few per cent accuracy due to the large number of stars in the fields. The observational sample is comprised of 577736 stars. These observed data are compared to a state-of-the-art particle simulation of the Galactic bulge region. The predictions are in rough agreement with observations, but appear to be too anisotropic in the velocity ellipsoid. We note that there is significant field-to-field variation in the observed proper motion dispersions. This could either be a real feature, or due to some unknown systematic effect.Comment: 12 pages, 13 figures, accepted for publication in MNRA