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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

Fouqué, P.; Heyrovský, D.; Dong, S.; Gould, A.; Udalski, A.; Albrow, M. D.; Batista, V.; Beaulieu, J.-P.; Bennett, D. P.; Bond, I. A.; Bramich, D. M.; Calchi Novati, S.; Cassan, A.; Coutures, C.; Dieters, S.; Dominik, M.; Dominis Prester, D.; Greenhill, J.; Horne, K.; Jørgensen, U. G.; Kozłowski, S.; Kubas, D.; Lee, C.-H.; Marquette, J.-B.; Mathiasen, M.; Menzies, J.; Monard, L. A. G.; Nishiyama, S.; Papadakis, I.; Street, R.; Sumi, T.; Williams, A.; Yee, J. C.; Brillant, S.; Caldwell, J. A. R.; Cole, A.; Cook, K. H.; Donatowicz, J.; Kains, N.; Kane, S. R.; Martin, R.; Pollard, K. R.; Sahu, K. C.; Tsapras, Y.; Wambsganss, J.; DePoy, D. L.; Gaudi, B. S.; Han, C.; Lee, C.-U.; Park, B.-G.; Kubiak, M.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Ulaczyk, K.; Abe, F.; Fukui, A.; Furusawa, K.; Gilmore, A. C.; Hearnshaw, J. B.; Itow, Y.; Kamiya, K.; Kilmartin, P. M.; Korpela, A. V.; Lin, W.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Ohnishi, K.; Okumura, T.; Perrott, Y.; Rattenbury, N. J.; Saito, To.; Sako, T.; Sato, S.; Skuljan, L.; Sullivan, D.; Sweatman, W.; Tristram, P. J.; Allan, A.; Bode, M. F.; Burgdorf, M. J.; Clay, N.; Fraser, S. N.; Hawkins, E.; Kerins, E.; Lister, T. A.; Mottram, C. J.; Saunders, E. S.; Snodgrass, C.; Steele, I. A.; Anguita, T.; Bozza, V.; Harpsøe, K.; Hinse, T. C.; Hundertmark, M.; Kjærgaard, P.; Liebig, C.; Mancini, L.; Masi, G.; Rahvar, S.; Ricci, D.; Scarpetta, G.; Southworth, J.; Surdej, J.; Thöne, C. C.; Riffeser, A. and Seitz, S. (2010). OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing. Astronomy & Astrophysics, 518, article no. A51.

DOI (Digital Object Identifier) Link: https://doi.org/10.1051/0004-6361/201014053
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Abstract

Context. Not only is gravitational microlensing a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event.

Aims. In high-magnification events, the lens caustic may cross over the source disk, which allows determination of the angular size of the source and measurement of its limb darkening.

Methods. When such extended-source effects appear close to maximum magnification, the resulting light curve differs from the characteristic Paczyński point-source curve. The exact shape of the light curve close to the peak depends on the limb darkening of the source. Dense photometric coverage permits measurement of the respective limb-darkening coefficients.

Results. In the case of the microlensing event OGLE 2008-BLG-290, the K giant source star reached a peak magnification at about 100. Thirteen different telescopes have covered this event in eight different photometric bands. Subsequent light-curve analysis yielded measurements of linear limb-darkening coefficients of the source in six photometric bands. The best-measured coefficients lead to an estimate of the source effective temperature of about 4700+100-200 K. However, the photometric estimate from colour-magnitude diagrams favours a cooler temperature of 4200 ± 100 K.

Conclusions. Because the limb-darkening measurements, at least in the CTIO/SMARTS2 Vs- and Is-bands, are among the most accurate obtained, the above disagreement needs to be understood. A solution is proposed, which may apply to previous events where such a discrepancy also appeared.

Item Type: Journal Item
Copyright Holders: 2010 ESO
ISSN: 1432-0746
Extra Information: Herschel: the first science highlights

12 pp.
Keywords: gravitational lensing; stars; atmospheres
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
Research Group: Space
Item ID: 43091
Depositing User: Colin Snodgrass
Date Deposited: 15 Jun 2015 09:49
Last Modified: 07 Dec 2018 10:31
URI: http://oro.open.ac.uk/id/eprint/43091
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