Discovery and Mass Measurements of a Cold, 10 Earth Mass Planet and Its Host Star

Muraki, Y.; Han, Cheongho; Bennett, D. P.; Suzuki, D.; Monard, L. A. G.; Street, R. A.; Jørgensen, U. G.; Kundurthy, P.; Skowron, J.; Becker, A. C.; Albrow, M. D.; Fouqué, P.; Heyrovsky, David; Barry, Richard; Beaulieu, J. P.; Wellnitz, D. D.; Bond, I. A.; Sumi, T.; Dong, Subo; Gaudi, B. Scott; Bramich, D. M.; Dominik, M.; Abe, F.; Botzler, C. S.; Freeman, Matthew; Fukui, A.; Furusawa, K.; Hayashi, F.; Hearnshaw, John; Hosaka, S.; Itow, Y.; Kamiya, K.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nishimoto, K.; Ohnishi, Kouhei; Perrott, Y. C.; Rattenbury, N. J.; Saito, To.; Skuljan, L.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Wada, K.; Yock, P. C. M.; Christie, Grant; DePoy, D. L.; Gorbikov, E.; Gould, Andrew; Kaspi, S.; Lee, Chung-Uk; Mallia, F.; Maoz, Dan; McCormick, J.; Moorhouse, D.; Natusch, T.; Park, B.-G.; Pogge, Richard W.; Polishook, David; Shporer, Avi; Thornley, G.; Yee, Jennifer C.; Allan, A.; Browne, P.; Horne, K.; Kains, N.; Snodgrass, C.; Steele, I. A.; Tsapras, Y.; Batista, V.; Bennett, C. S.; Brillant, S.; Caldwell, J.; Cassan, A.; Cole, A. A.; Corrales, R.; Coutures, C.; Dieters, S.; Prester, D. Dominis; Donatowicz, J.; Greenhill, J.; Kubas, D.; Marquette, J. B.; Martín, Roland; Menzies, John; Sahu, K. C.; Waldman, I.; Williams, A.; Zub, M.; Bourhrous, H.; Matsuoka, Yoshiki; Nagayama, Takahiro; Oi, Nagisa; Randriamanakoto, Zara; Bozza, V.; Burgdorf, M.; Novati, S. Calchi; Dreizler, S.; Finet, F.; Glitrup, M.; Harpsøe, K.; Hinse, T. C.; Hundertmark, M.; Liebig, C.; Maier, G.; Mancini, L.; Mathiasen, M.; Rahvar, S.; Ricci, Davide; Scarpetta, G.; Skottfelt, J.; Surdej, Jean; Southworth, J.; Wambsganß, J.; Zimmer, F.; Udalski, A.; Poleski, R.; Wyrzykowski, Ł.; Ulaczyk, K.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.

doi:10.1088/0004-637x/741/1/22

Cited by 124 publications

(87 citation statements)

References 79 publications

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“…First, planetary events can contain additional groundbased, annual-parallax information due to sharp features in the light curve. This was first clearly noted by Muraki et al (2011) for MOA-2009-BLG-266. Second, planetary events lead to the measurement of (or strong constraints upon) θ E , which obviously aids in the determination of π rel =θ E π E .…”

Section: Zhu Et Al (2017b) Protocols: Is the Parallax Measured?mentioning

confidence: 71%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

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Section: Zhu Et Al (2017b) Protocols: Is the Parallax Measured?mentioning

confidence: 71%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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“…OGLE-05-169L b is a planet of ∼13 M ⊕ orbiting a lowmass star of 0.49 +0.23 −0.29 M (if it is a main-sequence star) with a semimajor axis of ∼2.7 AU (Gould et al 2006). Finally, MOA-2009-BLG-266L b is a planet with 10.4 ± 1.7 M ⊕ orbiting a star of 0.56 ± 0.09 M with a semimajor axis of 3.2 +1.9 −0.5 AU (Muraki et al 2011). This planet represents a detection of interest since its mass and that of its host star are known with good precision.…”

Section: Discussionmentioning

confidence: 99%

Terrestrial planets in high-mass disks without gas giants

Elía

Guilera

Brunini

2013

A&A

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Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, superEarths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M . Results. All our simulations form massive planets on wide orbits. For a 0.1 M disk, 2-3 super-Earths of 2.8 to 5.9 M ⊕ are formed between 2 and 5 AU. For disks of 0.125 and 0.15 M , our simulations produce a 10-17.1 M ⊕ planet between 1.6 and 2.7 AU, and other super-Earths are formed in outer regions. Moreover, six planets survive in the habitable zone (HZ). These planets have masses from 1.9 to 4.7 M ⊕ and significant water contents ranging from 560 to 7482 Earth oceans, where one Earth ocean represents the amount of water on Earth's surface, which equals 2.8 × 10 −4 M ⊕ . Of the six planets formed in the HZ, three are water worlds with 39%-44% water by mass. These planets start the simulations beyond the snow line, which explains their high water abundances. In general terms, the smaller the mass of the planets observed on wide orbits, the higher the possibility to find water worlds in the HZ. In fact, massive planets can act as a dynamical barrier that prevents the inward diffusion of water-rich embryos located beyond the snow line. Conclusions. Systems without gas giants that harbor super-Earths or Neptune-mass planets on wide orbits around solar-type stars are of astrobiological interest. These systems are likely to harbor super-Earths in the HZ with significant water contents, which missions such as Kepler and Darwin should be able to find.

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“…The microlensing parallax effect has been detected in a number of planetary microlensing events (Gaudi et al 2008;Bennett et al 2010;Muraki et al 2011), where it has allowed the lens system masses to be measured. Due to the Earth's orbital motion about the Sun, the apparent lens-source relative motion deviates from uniform linear motion.…”

Section: Search For a Microlensing Parallax Signalmentioning

confidence: 99%

“…In events where the lens-star brightness or the parallax effect is measured (Gould 1992;Gaudi et al 2008;Muraki et al 2011), the planetary mass and distance to the planetary system can be determined. Hence, this technique can be used to build statistics of the planetary mass as a function of the host-star mass.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

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We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong lightcurve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with -=  V I 1.48 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at =  D 6.9 1.1 kpc , and a projected star-planet separation of = -+ a 1.75 0.33 0.34 au. The lens-source relative proper motion is m =  6.5 1.1 rel mas yr −1 . The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6-8 yr after the peak magnification. So, by 2020-2022, we can hope to detect the lens star with deep, high-resolution images.

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Discovery and Mass Measurements of a Cold, 10 Earth Mass Planet and Its Host Star

Abstract: Muraki et al.

Cited by 124 publications

References 79 publications

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Terrestrial planets in high-mass disks without gas giants

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

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