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Mass measurement of a single unseen star and planetary detection efficiency for OGLE 2007-BLG-050 (2009) |
- Batista, V.,
- Dong, Subo,
- Gould, A.,
- Beaulieu, J. P.,
- Cassan, A.,
- Christie, G. W.,
- Han, C.,
- Udalski, A.,
- Allen, W.,
- DePoy, D. L.,
- Gal-Yam, A.,
- Gaudi, B. S.,
- Johnson, B.,
- Kaspi, S.,
- Lee, C. U.,
- Maoz, D.,
- McCormick, J.,
- McGreer, I.,
- Monard, B.,
- Natusch, T.,
- Ofek, E.,
- Pogge, R. W.,
- Polishook, D.,
- Shporer, A.,
- Albrow, M. D.,
- Bennett, D. P.,
- Brillant, S.,
- Bode, M.,
- Bramich, D. M.,
- Burgdorf, M.,
- Caldwell, J. A. R.,
- Calitz, H.,
- Cole, A.,
- Cook, K. H.,
- Coutures, Ch.,
- Dieters, S.,
- Dominik, M.,
- Prester, D. Dominis,
- Donatowicz, J.,
- Fouqué, P.,
- Greenhill, J.,
- Hoffman, M.,
- Horne, K.,
- Jørgensen, U. G.,
- Kains, N.,
- Kane, S.,
- Kubas, D.,
- Marquette, J. B.,
- Martin, R.,
- Meintjes, P.,
- Menzies, J.,
- Pollard, K. R.,
- Sahu, K. C.,
- Snodgrass, C.,
- Steele, I.,
- Tsapras, Y.,
- Wambsganss, J.,
- Williams, A.,
- Zub, M.,
- Wyrzykowski, Ł.,
- Kubiak, M.,
- Szymański, M. K.,
- Pietrzyński, G.,
- Soszyński, I.,
- Szewczyk, O.,
- Ulaczyk, K.,
- Abe, F.,
- Bond, I. A.,
- Fukui, A.,
- Furusawa, K.,
- Hearnshaw, J. B.,
- Holderness, S.,
- Itow, Y.,
- Kamiya, K.,
- Kilmartin, P. M.,
- Korpela, A.,
- Lin, W.,
- Ling, C. H.,
- Masuda, K.,
- Matsubara, Y.,
- Miyake, N.,
- Muraki, Y.,
- Nagaya, M.,
- Ohnishi, K.,
- Okumura, T.,
- Perrott, Y. C.,
- Rattenbury, N.,
- Saito, To.,
- Sako, T.,
- Skuljan, L.,
- Sullivan, D.,
- Sumi, T.,
- Sweatman, W. L.,
- Tristram, P. J.,
- Yock, P. C. M.
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Abstract |
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We analyze OGLE-2007-BLG-050, a high magnification microlensing event (A ~ 432) whose peak occurred on 2 May, 2007, with pronounced finite-source and parallax effects. We compute planet detection efficiencies for this event in order to determine its sensitivity to the presence of planets around the lens star. Both finite-source and parallax effects permit a measurement of the angular Einstein radius \theta_E = 0.48 +/- 0.01 mas and the parallax \pi_E = 0.12 +/- 0.03, leading to an estimate of the lens mass M = 0.50 +/- 0.14 M_Sun and its distance to the observer D_L = 5.5 +/- 0.4 kpc. This is only the second determination of a reasonably precise (.
Comment: 20 pages, 23 figures |
Publication details |
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