Limb-darkening measurements for a cool red giant in microlensing event OGLE 2004-BLG-482

被引：30

作者：

Zub, M. ^{[1
,2
,3
]}

Cassan, A. ^{[1
,4
]}

Heyrovsky, D. ^{[5
]}

Fouque, P. ^{[6
]}

Stempels, H. C. ^{[7
]}

Albrow, M. D. ^{[8
]}

Beaulieu, J-P ^{[4
]}

Brillant, S. ^{[9
]}

Christie, G. W. ^{[10
]}

Kains, N. ^{[11
]}

Kozlowski, S. ^{[12
]}

Kubas, D. ^{[4
,9
]}

Wambsganss, J. ^{[1
]}

Batista, V. ^{[4
]}

Bennett, D. P. ^{[13
]}

Cook, K. ^{[14
]}

Coutures, C. ^{[4
]}

Dieters, S. ^{[4
]}

Dominik, M. ^{[11
]}

Prester, D. Dominis ^{[15
]}

Donatowicz, J. ^{[16
]}

Greenhill, J. ^{[17
]}

Horne, K. ^{[11
]}

Jorgensen, U. G. ^{[18
,19
]}

Kane, S. R. ^{[20
]}

Marquette, J-B ^{[4
]}

Martin, R. ^{[21
]}

Menzies, J. ^{[22
]}

Pollard, K. R.

Sahu, K. C. ^{[23
]}

Vinter, C. ^{[18
,19
]}

Williams, A. ^{[21
]}

Gould, A. ^{[12
]}

Depoy, D. L. ^{[12
]}

Gal-Yam, A. ^{[24
]}

Gaudi, B. S. ^{[12
]}

Han, C. ^{[25
]}

Lipkin, Y. ^{[26
,27
]}

Maoz, D.

Ofek, E. O. ^{[28
]}

Park, B-G ^{[29
]}

Pogge, R. W. ^{[12
]}

McCormick, J. ^{[30
]}

Udalski, A. ^{[31
]}

Szymanski, M. K. ^{[31
]}

Kubiak, M. ^{[31
]}

Pietrzynski, G. ^{[31
,32
]}

Soszynski, I. ^{[31
]}

Szewczyk, O. ^{[31
]}

Wyrzykowski, L. ^{[31
,33
]}

机构：

[1] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany

[2] Heidelberg Univ, Int Max Planck Res Sch Astron & Cosm Phys, D-6900 Heidelberg, Germany

[3] Univ Zielona Gora, Inst Astron, PL-65265 Zielona Gora, Poland

[4] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[5] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic

[6] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France

[7] Dept Phys & Astron, S-75120 Uppsala, Sweden

[8] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand

[9] European So Observ, Santiago 19, Chile

[10] Auckland Observ, Auckland, New Zealand

[11] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[12] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[13] Univ Notre Dame, Dept Phys, Notre Dame, IN 46530 USA

[14] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA

[15] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia

[16] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria

[17] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia

[18] Niels Bohr Inst, DK-2100 Copenhagen, Denmark

[19] Ctr Star & Planet Format, DK-2100 Copenhagen, Denmark

[20] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA

[21] Perth Observ, Perth, WA 6076, Australia

[22] S African Astron Observ, ZA-7935 Observatory, South Africa

[23] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[24] Weizmann Inst Sci, Fac Phys, Astrophys Grp, IL-76100 Rehovot, Israel

[25] Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea

[26] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[27] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel

[28] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[29] Korea Astron & Space Sci Inst, Taejon 305348, South Korea

[30] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand

[31] Univ Warsaw Observ, PL-00478 Warsaw, Poland

[32] Univ Concepcion, Dept Fis, Concepcion, Chile

[33] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 525卷

关键词：

gravitational lensing: micro; stars: atmospheres; techniques: high angular resolution; stars: individual: OGLE 2004-BLG-482; STELLAR ATMOSPHERE MODELS; CLUMP ABSOLUTE MAGNITUDE; H-ALPHA LINE; GALACTIC BULGE; PLANET OBSERVATIONS; MACHO; 98-SMC-1; STARS; PHOTOMETRY; LENS; RESOLUTION;

D O I：

10.1051/0004-6361/200912007

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We present a detailed analysis of OGLE 2004-BLG-482, a relatively high-magnification single-lens microlensing event that exhibits clear extended-source effects. These events are relatively rare, but they potentially contain unique information on the stellar atmosphere properties of their source star, as shown in this study. Methods. Our dense photometric coverage of the overall light curve and a proper microlensing modelling allow us to derive measurements of the OGLE 2004-BLG-482 source star's linear limb-darkening coefficients in three bands, including standard Johnson-Cousins I and R, as well as in a broad clear filter. In particular, we discuss in detail the problems of multi-band and multi-site modelling on the expected precision of our results. We also obtained high-resolution UVES spectra as part of a ToO programme at ESO VLT, from which we derive the source star's precise fundamental parameters. Results. From the high-resolution UVES spectra, we find that OGLE 2004-BLG-482's source star is a red giant of MK type a bit later than M3, with T-eff = 3667 +/- 150 K, log g = 2.1 +/- 1.0 and an assumed solar metallicity. This is confirmed by an OGLE calibrated colour-magnitude diagram. We then obtain from a detailed microlensing modelling of the light curve linear limb-darkening coefficients that we compare to model-atmosphere predictions available in the literature, and find a very good agreement for the I and R bands. In addition, we perform a similar analysis using an alternative description of limb darkening based on a principal component analysis of ATLAS limb-darkening profiles, and also find a very good agreement between measurements and model predictions.

引用

页数：12

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