SIMBAD references

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 M_h= 0.11±0.01 M_☉ and M_p= 9.2±2.2 M_⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D_L= 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

Full paper

View the references in ADS

To bookmark this query, right click on this link: simbad:2013ApJ...779...91F and select 'bookmark this link' or equivalent in the popup menu