OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

Fouqué, P.; Heyrovsky, David; Dong, Subo; Gould, Andrew; Udalski, A.; Albrow, M. D.; Batista, V.; Beaulieu, J. P.; Bennett, D. P.; Bond, I. A.; Bramich, D. M.; Novati, S. Calchi; Cassan, A.; Coutures, C.; Dieters, S.; Dominik, M.; Prester, D. Dominis; Greenhill, J.; Horne, K.; Jørgensen, U. G.; Kozłowski, S.; Kubas, D.; Lee, C.-H.; Marquette, J. B.; Mathiasen, M.; Menzies, John; Monard, L. A. G.; Nishiyama, Shogo; Papadakis, I. E.; Street, R. A.; Sumi, T.; Williams, A.; Yee, Jennifer C.; Brillant, S.; Caldwell, J. A. R.; Cole, A. A.; Cook, K. H.; Donatowicz, J.; Kains, N.; Kane, Stephen R.; Martín, Roland; Pollard, K. R.; Sahu, Kailash C.; Tsapras, Y.; Wambsganß, J.; Zub, M.; Depoy, D. L.; Gaudi, B. Scott; Han, Cheongho; Lee, C.-U.; Park, B.-G.; Pogge, Richard W.; Kubiak, M.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Ulaczyk, K.; Wyrzykowski, Ł.; Abe, F.; Fukui, A.; Furusawa, K.; Gilmore, A. C.; Hearnshaw, John; Itow, Y.; Kamiya, K.; Kilmartin, P. M.; Korpela, A.; Lin, Wei; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Ohnishi, Koji; Okumura, Teppei; Perrott, Y. C.; Rattenbury, N. J.; Saito, To.; Sako, T.; Sato, S.; Skuljan, L.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Yock, P. C. M.; Allan, A.; Bode, M. F.; Burgdorf, M.; Clay, N.; Fraser, S. N.; Hawkins, E.; Kerins, E.; Lister, Tim; Mottram, C. J.; Saunders, Eric S.; Snodgrass, C.; Steele, I. A.; Wheatley, P. J.; Anguita, T.; Bozza, V.; Harpsøe, K.; Hinse, T. C.; Hundertmark, M.; Kjærgaard, P.; Liebig, C.; Mancini, L.; Masi, G.; Rahvar, S.; Ricci, Davide; Scarpetta, G.; Southworth, J.; Surdej, Jean; Thöne, C. C.; Riffeser, A.; Seitz, S.; Bender, Ralf

doi:10.1051/0004-6361/201014053

Cited by 14 publications

(3 citation statements)

References 64 publications

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“…Barge et al 2008), or microlensing (e.g. Fouqué et al 2010). Besides, Sing (2010) has shown discrepancies between its modelled LD and the LD deduced from planetary transits observed by CoRoT.…”

Section: Discussionmentioning

confidence: 93%

Visibilities and bolometric corrections for stellar oscillation modes observed byKepler

Ballot

Barban

Veer-Menneret

2011

A&A

110

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Context. Kepler produces a large amount of data used for asteroseismological analyses, particularly of solar-like stars and red giants. The mode amplitudes observed in the Kepler spectral band have to be converted into bolometric amplitudes to be compared to models. Aims. We give a simple bolometric correction for the amplitudes of radial modes observed with Kepler, as well as the relative visibilities of non-radial modes. Methods. We numerically compute the bolometric correction c K−bol and mode visibilities for different effective temperatures T eff within the range 4000-7500 K, using a similar approach to a recent one from the literature. Results. We derive a law for the correction to bolometric values: . We show that using LD profiles already integrated over the spectral band provides quick and good approximations for visibilities. We point out the limits of these classical visibility estimations.

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Section: Discussionmentioning

confidence: 93%

Visibilities and bolometric corrections for stellar oscillation modes observed byKepler

Ballot

Barban

Veer-Menneret

2011

A&A

110

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“…See, for instance, the Cousins I band and SDSS i band, or the Wratten #12 filter (W12) used at some amateur telescopes to mimic an R band. More details about the derivation of these values for each telescope can be found in Heyrovský (2007), Fouqué et al (2010), and Muraki et al (2011).…”

Section: Appendix D Detailed Treatment Of Limb-darkening Correctionsmentioning

confidence: 99%

MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT

Bachelet¹,

Shin²,

Han³

et al. 2012

ApJ

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Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10 −3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θ E = 1.38 ± 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M * = 0.67 +0.33 −0.13 M and m p = 1.5 +0.8 −0.3 M JUP at a distance of D = 2.3 ± 0.6 kpc, and with a semi-major axis of a = 2 +3 −1 AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.

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“…In the cases where dense-coverage and good-quality data are available, the measured coefficients are generally in good agreement with theoretical values (Choi et al 2012;Shvartzvald et al 2019). In other cases, large differences (but with large uncertainties) between the measured results and the theoretical values are common (Fouqué et al 2010). For this event, fitting limb-darkening coefficients is even harder due to the modifications introduced by the variable source.…”

Section: Microlensing Modelmentioning

confidence: 64%

OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Li¹,

Zang²,

Udalski³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Abstract We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average time-scale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 $\mu$as) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M⊙ brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M⊙ ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a $\sim 35{{\ \rm per\ cent}}$ probability for the lens to be a bulge object and $\sim 65{{\ \rm per\ cent}}$ to be a background disc object.

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OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

Cited by 14 publications

References 64 publications

Visibilities and bolometric corrections for stellar oscillation modes observed byKepler

Visibilities and bolometric corrections for stellar oscillation modes observed byKepler

MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT

OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

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