Stellar Diameters and Temperatures. Iv. Predicting Stellar Angular Diameters

Boyajian, Tabetha S.; Belle, Gerald van; Braun, Kaspar von

doi:10.1088/0004-6256/147/3/47

Cited by 159 publications

(203 citation statements)

References 58 publications

(83 reference statements)

Supporting

Mentioning

187

Contrasting

Order By: Relevance

“…T eff was determined in two ways: (1) using θ LD -photometric calibrations (van Belle 1999; Kervella et al 2004;Di Benedetto 2005;Boyajian et al 2014) with the Stefan-Boltzmann law; and (2) using the IRFM (e.g. Blackwell & Shallis 1977;Blackwell et al 1979Blackwell et al , 1980Casagrande et al 2006Casagrande et al , 2010.…”

Section: Determination Of Effective Temperaturementioning

confidence: 99%

“…The θ LD was determined indirectly through photometric relationships. We have made use of four separate θ LD -photometric relations in order to test the robustness of this procedure (van Belle 1999; Kervella et al 2004;Di Benedetto 2005;Boyajian et al 2014). The first set of calibrations used were taken from the work of van Belle (1999).…”

Section: Deriving Temperature Using Angular Diameter-photometric Relamentioning

confidence: 99%

“…(1) and (2)). The final set of calibrations used were from Boyajian et al (2014). We made use of their θ LD -(B − V) relation (their Eq.…”

Section: Deriving Temperature Using Angular Diameter-photometric Relamentioning

confidence: 99%

See 2 more Smart Citations

GaiaFGK benchmark stars: new candidates at low metallicities

Hawkins

Jofré

Heiter

et al. 2016

A&A

View full text Add to dashboard Cite

Context. We have entered an era of large spectroscopic surveys in which we can measure, through automated pipelines, the atmospheric parameters and chemical abundances for large numbers of stars. Calibrating these survey pipelines using a set of "benchmark stars" in order to evaluate the accuracy and precision of the provided parameters and abundances is of utmost importance. The recent proposed set of Gaia FGK benchmark stars has up to five metal-poor stars but no recommended stars within −2.0 < [Fe/H] < −1.0 dex. However, this metallicity regime is critical to calibrate properly. Aims. In this paper, we aim to add candidate Gaia benchmark stars inside of this metal-poor gap. We began with a sample of 21 metalpoor stars which was reduced to 10 stars by requiring accurate photometry and parallaxes, and high-resolution archival spectra. Methods. The procedure used to determine the stellar parameters was similar to the previous works in this series for consistency. The difference was to homogeneously determine the angular diameter and effective temperature (T eff ) of all of our stars using the Infrared Flux Method utilizing multi-band photometry. The surface gravity (log g) was determined through fitting stellar evolutionary tracks. The [Fe/H] was determined using four different spectroscopic methods fixing the T eff and log g from the values determined independent of spectroscopy. Results. We discuss, star-by-star, the quality of each parameter including how it compares to literature, how it compares to a spectroscopic run where all parameters are free, and whether Fe i ionisation-excitation balance is achieved.Conclusions. From the 10 stars, we recommend a sample of five new metal-poor benchmark candidate stars which have consistent T eff , log g, and [Fe/H] determined through several means. These stars, which are within −1.3 < [Fe/H] < −1.0, can be used for calibration and validation purpose of stellar parameter and abundance pipelines and should be of highest priority for future interferometric studies.

show abstract

Section: Determination Of Effective Temperaturementioning

confidence: 99%

Section: Deriving Temperature Using Angular Diameter-photometric Relamentioning

confidence: 99%

See 1 more Smart Citation

GaiaFGK benchmark stars: new candidates at low metallicities

Hawkins

Jofré

Heiter

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…van Belle: Using the crude {V, K} angular size predictor in van Belle (1999) (updated nicely in Boyajian et al 2014), we can examine the rough angular sizes we should expect for these stars, which reveals some of the answer: The key here is that these stars are small -angular sizes measures of less than 1.5mas are very hard to do and require facilities with the highest amounts of angular resolution; since these are all southern hemisphere objects I presume that the attempts have been made with VLTI, which would find these angular scales challenging. For the first three, a facility such as CHARA or NPOI should be able to resolve the northern hemisphere counterparts of these objects (and a corresponding set of sufficiently small calibration…”

Section: Discussionmentioning

confidence: 99%

Basics of Optical Interferometry: A Gentle Introduction

Belle¹

2014

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…The source radius is calculated from the dereddened source magnitude and color using the following formula, obtained using a similar technique to that described in Boyajian et al (2014):…”

Section: -E V I Amentioning

confidence: 99%

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

View full text Add to dashboard Cite

We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong lightcurve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with -=  V I 1.48 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at =  D 6.9 1.1 kpc , and a projected star-planet separation of = -+ a 1.75 0.33 0.34 au. The lens-source relative proper motion is m =  6.5 1.1 rel mas yr −1 . The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6-8 yr after the peak magnification. So, by 2020-2022, we can hope to detect the lens star with deep, high-resolution images.

show abstract

Stellar Diameters and Temperatures. Iv. Predicting Stellar Angular Diameters

Cited by 159 publications

References 58 publications

GaiaFGK benchmark stars: new candidates at low metallicities

GaiaFGK benchmark stars: new candidates at low metallicities

Basics of Optical Interferometry: A Gentle Introduction

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Contact Info

Product

Resources

About