SIMBAD references

2009A&A...508..467B - Astronomy and Astrophysics, volume 508, 467-478 (2009/12-2)

Mass measurement of a single unseen star and planetary detection efficiency. for OGLE 2007-BLG-050.

BATISTA V., DONG S., 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., PARK B.-G., 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 C., DIETERS S., DOMINIK M., DOMINIS PRESTER D., DONATOWICZ J., FOUQUE P., GREENHILL J., HOFFMAN M., HORNE K., JORGENSEN 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 L., KUBIAK M., SZYMANSKI M.K., PIETRZYNSKI G., SOSZYNSKI 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 T., SAKO T., SKULJAN L., SULLIVAN D., SUMI T., SWEATMAN W.L., TRISTRAM P.J. and YOCK P.C.M.

Abstract (from CDS):

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 θE=0.48±0.01mas and the parallax πE=0.12±0.03, leading to an estimate of the lens mass M=0.50±0.14M☉ and its distance to the observer DL=5.5±0.4kpc. This is only the second determination of a reasonably precise (<30%) mass estimate for an isolated unseen object, using any method. This allows us to calculate the planetary detection efficiency in physical units (r{perpendicular},mp), where r{perpendicular} is the projected planet-star separation and mp is the planet mass. When computing planet detection efficiency, we did not find any planetary signature, i.e. none of the planetary configurations provides a Δχ2 improvement higher than 60, and our detection efficiency results reveal significant sensitivity to Neptune-mass planets, and to a lesser extent Earth-mass planets in some configurations. Indeed, Jupiter and Neptune-mass planets are excluded with a high confidence for a large projected separation range between the planet and the lens star, respectively [0.6-10] and [1.4-4]AU, and Earth-mass planets are excluded with a 10% confidence in the lensing zone, i.e. [1.8-3.1]AU.

Abstract Copyright: ∼

Journal keyword(s): gravitational lensing - techniques: photometric - stars: individual: OGLE 2007-BLG-050 - planetary systems

CDS comments: Paragraphe 1.2 OGLE 2007-BLG-071 is a probable misprint for EWS 2005-BLG-71. OGLE 2003-BLG-267 is EWS 2003-BUL-170 in Jaroszynski et al. 2005.

Simbad objects: 17

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