2013ApJ...779...91F

Query : 2013ApJ...779...91F

2013ApJ...779...91F - Astrophys. J., 779, 91 (2013/December-3)

MOA-2010-BLG-328Lb: a Sub-Neptune orbiting very late M dwarf?

FURUSAWA K., UDALSKI A., SUMI T., BENNETT D.P., BOND I.A., GOULD A., JORGENSEN U.G., SNODGRASS C., DOMINIS PRESTER D., ALBROW M.D., ABE F., BOTZLER C.S., CHOTE P., FREEMAN M., FUKUI A., HARRIS P., ITOW Y., LING C.H., MASUDA K., MATSUBARA Y., MIYAKE N., MURAKI Y., OHNISHI K., RATTENBURY N.J., SAITO TO., SULLIVAN D.J., SUZUKI D., SWEATMAN W.L., TRISTRAM P.J., WADA K., YOCK P.C.M. (The MOA Collaboration), SZYMANSKI M.K., SOSZYNSKI I., KUBIAK M., POLESKI R., ULACZYK K., PIETRZYNSKI G., WYRZYKOWSKI L. (The OGLE Collaboration), CHOI J.-Y., CHRISTIE G.W., DEPOY D.L., DONG S., DRUMMOND J., GAUDI B.S., HAN C., HUNG L.-W., HWANG K.-H., LEE C.-U., McCORMICK J., MOORHOUSE D., NATUSCH T., NOLA M., OFEK E., POGGE R.W., SHIN I.-G., SKOWRON J., THORNLEY G., YEE J.C. (The {mu}FUN Collaboration), ALSUBAI K.A., BOZZA V., BROWNE P., BURGDORF M.J., CALCHI NOVATI S., DODDS P., DOMINIK M., FINET F., GERNER T., HARDIS S., HARPSOE K., HINSE T.C., HUNDERTMARK M., KAINS N., KERINS E., LIEBIG C., MANCINI L., MATHIASEN M., PENNY M.T., PROFT S., RAHVAR S., RICCI D., SCARPETTA G., SCHAFER S., SCHONEBECK F., SOUTHWORTH J., SURDEJ J., WAMBSGANSS J. (The MiNDSTEp Consortium), STREET R.A., BRAMICH D.M., STEELE I.A., TSAPRAS Y. (The RoboNet Collaboration), HORNE K., DONATOWICZ J., SAHU K.C., BACHELET E., BATISTA V., BEATTY T.G., BEAULIEU J.-P., BENNETT C.S., BLACK C., BOWENS-RUBIN R., BRILLANT S., CALDWELL J.A.R., CASSAN A., COLE A.A., CORRALES E., COUTURES C., DIETERS S., FOUQUE P., GREENHILL J., HENDERSON C.B., KUBAS D., MARQUETTE J.-B., MARTIN R., MENZIES J.W., SHAPPEE B., WILLIAMS A., WOUTERS D., VAN SADERS J., ZELLEM R., ZUB M. (The PLANET Collaboration)

Abstract (from CDS):

We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh= 0.11±0.01 M☉ and Mp= 9.2±2.2 M⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL= 0.81±0.10 kpc with projected separation r= 0.92±0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.

Abstract Copyright: ∼

Journal keyword(s): gravitational lensing: micro - planetary systems

Simbad objects: 4

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Number of rows : 4
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME EWS 2006-BLG-109b Pl 17 52 34.55 -30 05 15.7           ~ 46 1
2 MOA 2010-BLG-328 * 17 57 59.120 -30 42 54.63           ~ 14 0
3 MOA 2010-BLG-328b Pl 17 57 59.120 -30 42 54.63           ~ 4 0
4 NAME Galactic Bulge reg ~ ~           ~ 4794 0

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