arXiv subjects

Gáspár Bakos

Publications and source records attributed to Gáspár Bakos.

5 recordsLinked to original sources

arXiv2026

Atmospheric Light Pollution by Proposed Reflect Orbital Space Mirrors

ReflectOrbital is planning to launch a $18\times18$\,m mirror in space at a $\sim$600\,km altitude to illuminate a $2.5$\,km radius circular patch on Earth. The pilot satellite, called EARENDIL-1, is a pathfinder for a constellation of $\sim$50,000 larger mirrors, each with $54\times54$\,m in diameter, with the explicit goal to provide space-borne illumination on Earth. We calculate the sky brightness caused by the Rayleigh scattering and aerosol scattering of the incoming beam from one such satellite and by the light reflected back by the illuminated patch, for various atmospheric properties and ground albedos under cloud-free conditions. We demonstrate that the light pollution caused by one of these satellites is very significant, altering the nighttime environment up to distances of $\sim$30\,kms. The results show that for an observer within the beam of a single 54\,m satellite, the mirror will appear as a $-16.7$\,mag point-like source, i.e.~about 4 magnitudes brighter than the full moon. The diffuse sky background will be similar to the dusk sky shortly after sunset; too bright to see even the brightest stars. From a distance of 14\,km, the glow from a single mirror will exceed the luminance of the full moon sky for majority of the sky. From a distance of 34\,km the sky will still appear brighter than the moon-lit sky in the direction of the beam. If 400 such mirrors illuminate the same patch simultaneously, the glow will be obvious from 80\,kms.

astro-ph.IM↗

arXiv2025

The T16 Project: Image Subtraction Light Curves from TESS Cycle 1 Full-Frame Images for Stars with T < 16

We present 83,717,159 light curves for 56,401,549 stars with T < 16 mag observed in the Full-Frame Images (FFIs) of Cycle 1 of the NASA TESS mission. These light curves were extracted from subtracted images produced by the Cluster Difference Imaging Survey (CDIPS; Bouma et al. 2019). We make public the raw image subtraction light curves, together with light curves detrended against instrumental systematics. We compare the light curves to other publicly available light curves from the TESS FFIs, finding that for a substantial fraction of stars with T < 16, the T16 project provides the highest precision FFI light curves available. We demonstrate that the detrended T16 light curves are generally as good as, or better than, the light curves from other projects for the known TOIs. We also show that the un-detrended light curves can be used to study high amplitude variable stars. The light curves are being made available through the NASA Mikulski Archive for Space Telescopes (MAST). Light curve production is underway for additional TESS Cycles.

astro-ph.SR↗

arXiv2023

BU Canis Minoris -- the Most Compact Known Flat Doubly Eclipsing Quadruple System

We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 days. The previous record holder was TIC 219006972 (Kostov et al. 2023), with a period of 168 days. The quadruple nature of BU CMi was established by Volkov et al. (2021), but they misidentified the outer period as 6.6 years. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 days, and a substantial eccentricity of about 0.22. All four stars are within about 0.1 solar mass of 2.4 solar masses. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of about 30 years, thanks to the short outer orbital period. The outer period of 121 days is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations (ETV) curve of each EB by the other binary, and by modeling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 degree, but the overall system has an inclination angle near 83.5 degrees. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a timescale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. (2021) and led them to conclude that the outer period was 6.6 years rather than the 121 days that we establish here.

astro-ph.SR↗

arXiv2014

Astrometric exoplanet detection with Gaia

We provide a revised assessment of the number of exoplanets that should be discovered by Gaia astrometry, extending previous studies to a broader range of spectral types, distances, and magnitudes. Our assessment is based on a large representative sample of host stars from the TRILEGAL Galaxy population synthesis model, recent estimates of the exoplanet frequency distributions as a function of stellar type, and detailed simulation of the Gaia observations using the updated instrument performance and scanning law. We use two approaches to estimate detectable planetary systems: one based on the S/N of the astrometric signature per field crossing, easily reproducible and allowing comparisons with previous estimates, and a new and more robust metric based on orbit fitting to the simulated satellite data. With some plausible assumptions on planet occurrences, we find that some 21,000 (+/-6000) high-mass (1-15M_J) long-period planets should be discovered out to distances of ~500pc for the nominal 5-yr mission (including at least 1000-1500 around M dwarfs out to 100pc), rising to some 70,000 (+/-20,000) for a 10-yr mission. We indicate some of the expected features of this exoplanet population, amongst them ~25-50 intermediate-period (P~2-3yr) transiting systems.

astro-ph.EP↗

arXiv2005

Testing the Rate of False Planetary Transits due to Binary Star Blending

We investigate the rate of false planetary transit detection due to blending with eclipsing binaries. Our approach is purely empirical and is based on the analysis of the artificially blended light curves of the eclipsing binary stars in the Large Magellanic Cloud from the archive of the Optical Gravitational Lensing Experiment (OGLE). Employing parameters that characterize the significance of the transit and the amplitude of the variation out of the transit, we can substantially limit the number of potential false positives. Further constraint comes from the expected length of the transit by a possible planetary companion. By the application of these criteria we are left only with 18 candidates from the full sample of 2495 stars. Visual inspection of these remaining variables eliminates all of them for obvious reasons (e.g., for visible fingerprints of orbital eccentricity). We draw the attention to the short-period stars, where the false alarm rate is especially low.

astro-ph↗