Binary Star Synthetic Photometry and Distance Determination Using Binsyn

Linnell, Albert P.; DeStefano, Paul; Hubený, I.

doi:10.1088/0004-6256/146/3/68

Cited by 6 publications

(4 citation statements)

References 45 publications

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“…The data point is the interferometric measurement of 6.048 mas (Davis et al 2011) with its 0.04 mas error bar. (Also compare with the discussion in Linnell et al (2013).) While the Davis et al (2011) measure agrees with the two results from both models within the 1σ uncertainty, increasing the model surface flux or decreasing the measured absolute CALSPEC flux by ∼1% would reduce the difference.…”

Section: The Grid Archivesupporting

confidence: 62%

A New Stellar Atmosphere Grid and Comparisons with HST/STIS CALSPEC Flux Distributions

et al. 2017

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The Space Telescope Imaging Spectrograph (STIS) has measured the spectral energy distributions (SEDs) for several stars of types O, B, A, F, and G. These absolute fluxes from the CALSPEC database are fit with a new spectral grid computed from the ATLAS-APOGEE ATLAS9 model atmosphere database using a chi-square minimization technique in four parameters. The quality of the fits are compared for complete LTE grids by Castelli & Kurucz (CK04) and our new comprehensive LTE grid (BOSZ). For the cooler stars, the fits with the MARCS LTE grid are also evaluated, while the hottest stars are also fit with the NLTE Lanz & Hubeny OB star grids. Unfortunately, these NLTE models do not transition smoothly in the infrared to agree with our new BOSZ LTE grid at the NLTE lower limit of T eff =15,000K.The new BOSZ grid is available via the Space Telescope Institute MAST archive and has a much finer sampled IR wavelength scale than CK04, which will facilitate the modeling of stars observed by the James Webb Space Telescope (JWST). Our result for the angular diameter of Sirius agrees with the groundbased interferometric value.

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Section: The Grid Archivesupporting

confidence: 62%

A New Stellar Atmosphere Grid and Comparisons with HST/STIS CALSPEC Flux Distributions

et al. 2017

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“…But in these codes each pixel radiates like a blackbody (using the appropriate local temperature after gravity darkening is included) and limb darkening laws are used to mimic the angular dependency. There are a few codes that can use tabulated specific intensities from model atmosphere computations, for example BINSYN (Linnell & Hubeny 1994;Linnell & DeStefano 2012, Linnell et al 2013, ELC (Orosz & Hauschildt 2000;Wittenmyer et al 2005), PHOEBE2 (Prša & Zwitter 2005;Prsa et al 2016), and most recently and noteably for exoplanets, ExoTETHyS by Morello et al (2020). However, the technique of integrating the intensities is computationally expensive, especially for cases where there is a large radius ratio that requires fine tiling of the star(s).…”

Section: Introductionmentioning

confidence: 99%

Fast Transit Computation Using Tabulated Stellar Intensities

Short,

Orosz,

Windmiller

et al. 2020

Preprint

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Limb darkening laws are convenient parameterizations of the stellar intensity center-to-limb variation, and their use is ubiquitous in eclipse and transit modeling. But they are not "laws" in any sensethey are simple approximations of the real intensity variations, and their limitations are becoming more and more apparent as stellar atmosphere models improve and higher precision data become available. When fitting eclipses and transit light curves, one would ideally like to use model intensities that are based on fundamental stellar parameters such as the mass, radius, and effective temperature of the star, rather than a limb darkening law representation and its coefficients. This is especially true when attempting to detect higher-order effects such as planetary oblateness, rings, satellites, or atmospheres. However, using model intensities requires numerically integrating many small-area "tiles" on the model stellar surface(s) and this has traditionally been too computationally expensive for general use. Here we present a fast technique to compute light curves and the Rossiter-McLaughlin effect that uses tabulated stellar models intensities. This is a step in the development of tools that obviate the need for limb darkening laws.

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“…In addition, synthetic photometry is used to estimate the physical parameters more accurately through the colour indices without needing the observed spectra of the binary systems (Straizys 1996;Castelli 1999;Bessell & Murphy 2012;Linnell et al 2013). It is a quantitatively analysis for the synthetic SED of a binary system which is about modifying stellar parameters such that the synthetic magnitudes fit the observed ones (Al-Wardat et al 2014b,a;Masda et al 2016;Al-Wardat et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Orbital and physical parameters of the close binary system GJ 9830 (HIP 116259)

Masda

Al-Wardat

Pathan

2019

Res. Astron. Astrophys.

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We present the complete set of physical and geometrical parameters of the visual close binary system GJ 9830 for the first time by using Al-Wardat's complex method. This method combines magnitude difference from speckle interferometry, synthetic spectral energy distributions of the binary components which are constructed depending on grids of Kurucz blanketed models (Atlas9), along with the orbital solution by using Tokovinin's dynamical method to estimate the parameters of the individual components. The analysis of the system by using synthetic photometry resulted in the following set of parameters: T eff. = 6220 ± 100 K, log g = 4.30 ± 0.12, R = 1.10 ± 0.08 R for the primary component and T eff. = 4870±100 K, log g = 4.60±0.11, R = 0.709±0.07 R for the secondary component. The recently published dynamical parallax from Gaia space mission was used to calculate the total mass of the binary system as 1.75±0.06 M which coincides with those estimated by using Al-Wardat's method as M A = 1.18 ± 0.10 M , M B = 0.75 ± 0.08 M . The analysis of the system reveals that both components belong to main sequence stars with an age around 1.4 ± 0.50 Gyr. The evolutionary tracks and isochrones of the system's components are discussed, and the fragmentation process is suggested as the most likely process for the formation of the system.

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Binary Star Synthetic Photometry and Distance Determination Using Binsyn

Cited by 6 publications

References 45 publications

A New Stellar Atmosphere Grid and Comparisons with HST/STIS CALSPEC Flux Distributions

A New Stellar Atmosphere Grid and Comparisons with HST/STIS CALSPEC Flux Distributions

Fast Transit Computation Using Tabulated Stellar Intensities

Orbital and physical parameters of the close binary system GJ 9830 (HIP 116259)

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