Predicting stellar angular diameters from V, IC, H and K photometry

Adams, Arthur D.; Boyajian, Tabetha S.; Braun, Kaspar von

doi:10.1093/mnras/stx2367

Cited by 54 publications

(56 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Groenewegen (2004) published a CSB relation for M giants (3.2 < (V − K) 0 < 6.1), which gives angular radii that are systematically 10% lower than those based on Kervella et al (2004): θ * = 10.9 ± 0.7 µas (OGLE-2012-BLG-1323) and θ * = 29.8 ± 1.9 µas (OGLE-2017-BLG-0560). Adams et al (2018) recently published a new CSB relation for giants (−0.01 < (V − I) 0 < 1.74), from which we find θ * = 11.5 ± 0.9 µas (OGLE-2012-BLG-1323) and θ * = 32.3 ± 2.3 µas (OGLE-2017-BLG-0560), in good agreement with our determination. 11.9 ± 0.5 34.9 ± 1.5 15.1 ± 0.8…”

Section: Source Starssupporting

confidence: 92%

Two new free-floating or wide-orbit planets from microlensing

Mróz

Udalski

Bennett

et al. 2019

A&A

View full text Add to dashboard Cite

Planet formation theories predict the existence of free-floating planets that have been ejected from their parent systems. Although they emit little or no light, they can be detected during gravitational microlensing events. Microlensing events caused by rogue planets are characterized by very short timescales tE (typically below two days) and small angular Einstein radii θE (up to several μas). Here we present the discovery and characterization of two ultra-short microlensing events identified in data from the Optical Gravitational Lensing Experiment (OGLE) survey, which may have been caused by free-floating or wide-orbit planets. OGLE-2012-BLG-1323 is one of the shortest events discovered thus far (tE = 0.155 ± 0.005 d, θE = 2.37 ± 0.10μas) and was caused by an Earth-mass object in the Galactic disk or a Neptune-mass planet in the Galactic bulge. OGLE-2017-BLG-0560 (tE = 0.905 ± 0.005 d, θE = 38.7 ± 1.6μas) was caused by a Jupiter-mass planet in the Galactic disk or a brown dwarf in the bulge. We rule out stellar companions up to a distance of 6.0 and 3.9 au, respectively. We suggest that the lensing objects, whether located on very wide orbits or free-floating, may originate from the same physical mechanism. Although the sample of ultrashort microlensing events is small, these detections are consistent with low-mass wide-orbit or unbound planets being more common than stars in the Milky Way.

show abstract

Section: Source Starssupporting

confidence: 92%

Two new free-floating or wide-orbit planets from microlensing

Mróz

Udalski

Bennett

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…We interpolate the color tables in Bessell & Brett (1988) to arrive at a (V − K, K) source = (1.78 ± 0.04, 14.00 ± 0.06). Using the relationship between stellar angular size, (V − K) color, and K-magnitude given by Adams et al (2018), the source angular radius θ = 3.4 ± 0.2 µas.…”

Section: Source Star Limb Darkening and Angular Radiusmentioning

confidence: 99%

OGLE-2014-BLG-0962 and a Comparison of Galactic Model Priors to Microlensing Data

Shan¹,

Yee²,

Udalski³

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…Fortunately, the sharp planetary light-curve features enable a precise measurement of the source radius crossing time, t * . This provides a determination of the angular Einstein radius, θ E =θ * t E /t * , if we know the angular radius of the source star, θ * , which can be determined from the dereddened source magnitude and color (Kervella et al 2004;Boyajian et al 2014;Adams et al 2016). We determine θ * in Section 4.1.…”

Section: Lens System Propertiesmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

106

View full text Add to dashboard Cite

We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of q≈3.4×10 −4 , but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be M L ≈0.7  M . Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass m c =80±13 Å M , orbiting a pair of M dwarfs with masses of M A =0.41±0.07 and M B =0.30±0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.

show abstract

Predicting stellar angular diameters from V, IC, H and K photometry

Cited by 54 publications

References 59 publications

Two new free-floating or wide-orbit planets from microlensing

Two new free-floating or wide-orbit planets from microlensing

OGLE-2014-BLG-0962 and a Comparison of Galactic Model Priors to Microlensing Data

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Contact Info

Product

Resources

About