Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-mass 
Microlensing Planet OGLE-2017-BLG-1140Lb

Calchi Novati, S.; Skowron, J.; Jung, Y. K.; Beichman, C.; Bryden, G.; Carey, S.; Gaudi, B. S.; Henderson, C. B.; Shvartzvald, Y.; Yee, J. C.; Zhu, W.; Team, Spitzer; Udalski, A.; Szymański, M. K.; Mróz, P.; Poleski, R.; Soszyński, I.; Kozłowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Pawlak, M.; Rybicki, K.; Iwanek, P.; Collaboration, OGLE; Albrow, M. D.; Chung, S. -J.; Gould, A.; Han, C.; Hwang, K. -H.; Ryu, Y. -H.; Shin, I. -G.; Zang, W.; Cha, S. -M.; Kim, D. -J.; Kim, H. -W.; Kim, S. -L.; Lee, C. -U.; Lee, D. -J.; Lee, Y.; Park, B. -G.; Pogge, R. W.; Collaboration, KMTNet

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Journal Article

Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-mass Microlensing Planet OGLE-2017-BLG-1140Lb

MPS-Authors

Calchi Novati, S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Skowron, J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Jung, Y. K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Beichman, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bryden, G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Carey, S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gaudi, B. S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Henderson, C. B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Shvartzvald, Y.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Yee, J. C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zhu, W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Team, Spitzer
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Udalski, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Szymański, M. K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mróz, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Poleski, R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Soszyński, I.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kozłowski, S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pietrukowicz, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ulaczyk, K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pawlak, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rybicki, K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Iwanek, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Collaboration, OGLE
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Albrow, M. D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chung, S. -J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gould, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Han, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hwang, K. -H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ryu, Y. -H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Shin, I. -G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zang, W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cha, S. -M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kim, D. -J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kim, H. -W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kim, S. -L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lee, C. -U.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lee, D. -J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lee, Y.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Park, B. -G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pogge, R. W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Collaboration, KMTNet
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018AJ....155..261C
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Citation

Calchi Novati, S., Skowron, J., Jung, Y. K., Beichman, C., Bryden, G., Carey, S., et al. (2018). Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-mass Microlensing Planet OGLE-2017-BLG-1140Lb. The Astronomical Journal, 155.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CE98-8

Abstract

We analyze the combined Spitzer and ground-based data for OGLE-2017-BLG-1140 and show that the event was generated by a Jupiter- class ({m}_p≃ 1.6 {M}_{{J}{{u}}{{p}}}) planet orbiting a mid-late M dwarf (M≃ 0.2 {M}_☉) that lies {D}_LS}≃ 1.0 {kpc} in the foreground of the microlensed Galactic-bar source star. The planet-host projected separation is {a}_\perp≃ 1.0 {au}, i.e., well beyond the snow line. By measuring the source proper motion {{\boldsymbol{μ }}}_s from ongoing long-term OGLE imaging and combining this with the lens-source relative proper motion {{\boldsymbol{μ }}}_rel} derived from the microlensing solution, we show that the lens proper motion {{\boldsymbol{μ }}}_l={{\boldsymbol{μ }}}_rel}+{{\boldsymbol{μ }}}_s is consistent with the lens lying in the Galactic disk, although a bulge lens is not ruled out. We show that while the Spitzer and ground-based data are comparably well fitted by planetary (i.e., binary-lens (2L1S)) and binary-source (1L2S) models, the combination of Spitzer and ground-based data decisively favors the planetary model. This is a new channel to resolve the 2L1S/1L2S degeneracy, which can be difficult to break in some cases.