Microlensing Discovery of a Tight, Low-Mass-Ratio Planetary-Mass Object Around an Old Field Brown Dwarf

Han, Cheongho; Jung, Youn Kil; Udalski, A.; Sumi, T.; Gaudi, B. Scott; Gould, Andrew; Bennett, D. P.; Tsapras, Y.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Skowron, J.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, Ł.; Abe, F.; Bond, I. A.; Botzler, C. S.; Chote, P.; Freeman, Matthew; Fukui, A.; Furusawa, K.; Harris, P.; Itow, Y.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Ohnishi, Koji; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Sweatman, W. L.; Suzuki, D.; Tristram, P. J.; Wada, K.; Yock, P. C. M.; Batista, V.; Christie, Grant; Choi, J.-Y.; DePoy, D. L.; Dong, Subo; Hwang, Kyu-Ha; Kavka, A.; Lee, Chung-Uk; Monard, L. A. G.; Natusch, T.; Ngan, H.; Park, H.; Pogge, Richard W.; Porritt, I.; Shin, In-Gu; Tan, T. G.; Yee, Jennifer C.; Alsubai, K. A.; Bozza, V.; Bramich, D. M.; Browne, P.; Dominik, M.; Horne, K.; Hundertmark, M.; Ипатов, С. И.; Kains, N.; Liebig, C.; Snodgrass, C.; Steele, I. A.; Street, R. A.

doi:10.1088/0004-637x/778/1/38

Cited by 83 publications

(46 citation statements)

References 38 publications

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“…More massive, supra-Jupiter mass companions (e.g. Chauvin et al 2004;Joergens & Müller 2007;Todorov et al 2010;Han et al 2013) cannot be really considered to be formed in protoplanetary disks with the properties that we observe, and are most likely the result of a binary system formation in the substellar regime.…”

Section: Discussionmentioning

confidence: 80%

Brown dwarf disks with ALMA: Evidence for truncated dust disks in Ophiuchus

Testi

Natta

Scholz

et al. 2016

A&A

129

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Context. The study of the properties of disks around young brown dwarfs can provide important clues on the formation of these very low-mass objects and on the possibility of forming planetary systems around them. The presence of warm dusty disks around brown dwarfs is well known, based on near-and mid-infrared studies. Aims. High angular resolution observations of the cold outer disk are limited; we used ALMA to attempt a first survey of young brown dwarfs in the ρ Oph star-forming region. Methods. All 17 young brown dwarfs in our sample were observed at 890 µm in the continuum at ∼ 0. 5 angular resolution. The sensitivity of our observations was chosen to detect ∼ 0.5 M ⊕ of dust. Results. We detect continuum emission in 11 disks (∼ 65% of the total), and the estimated mass of dust in the detected disks ranges from ∼ 0.5 to ∼ 6 M ⊕ . These disk masses imply that planet formation around brown dwarfs may be relatively rare and that the supraJupiter mass companions found around some brown dwarfs are probably the result of a binary system formation. We find evidence that the two brightest disks in ρ Oph have sharp outer edges at R < ∼ 25 AU, in contrast to disks around Taurus brown dwarfs. This difference may suggest that the different environment in ρ Oph may lead to significant differences in disk properties. A comparison of the M disk /M * ratio for brown dwarf and solar-mass systems also shows a possible deficit of mass in brown dwarfs, which could support the evidence for dynamical truncation of disks in the substellar regime. These findings are still tentative and need to be put on firmer grounds by studying the gaseous disks around brown dwarfs and by performing a more systematic and unbiased survey of the disk population around the more massive stars.

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Section: Discussionmentioning

confidence: 80%

Brown dwarf disks with ALMA: Evidence for truncated dust disks in Ophiuchus

Testi

Natta

Scholz

et al. 2016

A&A

129

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“…The first gas giant was detected around a BD by Han et al (2013). Very recently, Gillon et al (2016) discovered 3 Earth-sized planets close to an object of mass 0.08 M (just above the theoretical limit of M ∼ 0.075 M between brown dwarfs and M-dwarfs, Chabrier & Baraffe 1997).…”

Section: Introductionmentioning

confidence: 96%

Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1

Bolmont

Selsis

Owen

et al. 2016

Mon. Not. R. Astron. Soc.

240

282

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Ultracool dwarfs (UCD; T eff <∼ 3000 K) cool to settle on the main sequence after ∼1 Gyr. For brown dwarfs, this cooling never stops. Their habitable zone (HZ) thus sweeps inward at least during the first Gyr of their lives. Assuming they possess water, planets found in the HZ of UCDs have experienced a runaway greenhouse phase too hot for liquid water prior to entering the HZ. It has been proposed that such planets are desiccated by this hot early phase and enter the HZ as dry worlds. Here we model the water loss during this pre-HZ hot phase taking into account recent upper limits on the XUV emission of UCDs and using 1D radiation-hydrodynamic simulations. We address the whole range of UCDs but also focus on the planets recently found around the 0.08 M dwarf TRAPPIST-1.Despite assumptions maximizing the FUV-photolysis of water and the XUV-driven escape of hydrogen, we find that planets can retain significant amounts of water in the HZ of UCDs, with a sweet spot in the 0.04 -0.06 M range. We also studied the TRAPPIST-1 system using observed constraints on the XUV-flux. We find that TRAPPIST-1b and c may have lost as much as 15 Earth Oceans and planet d -which might be inside the HZ -may have lost less than 1 Earth Ocean. Depending on their initial water contents, they could have enough water to remain habitable. TRAPPIST-1 planets are key targets for atmospheric characterization and could provide strong constraints on the water erosion around UCDs.

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“…In addition, Han et al (2013) discovered a ∼2M J planet at projected separation ∼0.9AU orbiting a ∼0.02M BD. While the mass ratio suggests a binary-like formation mechanism, the relatively close projected separation hints at possible in-disk formation.…”

Section: Introductionmentioning

confidence: 99%

An Earth-mass Planet in a 1 au Orbit around an Ultracool Dwarf

Shvartzvald

Yee

Novati

et al. 2017

ApJL

Self Cite

127

123

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We combine Spitzer and ground-based KMTNet microlensing observations to identify and precisely measure an Earth-mass (1.43 −0.46 kpc, it is the third consecutive case among the Spitzer "Galactic distribution" planets toward the Galactic bulge that lies in the Galactic disk as opposed to the bulge itself, hinting at a skewed distribution of planets. Together with previous microlensing discoveries, the seven Earth-size planets orbiting the ultracool dwarf TRAPPIST-1, and the detection of disks around young brown dwarfs, OGLE-2016-BLG-1195Lb suggests that such planets might be common around ultracool dwarfs. It therefore sheds light on the formation of both ultracool dwarfs and planetary systems at the limit of low-mass protoplanetary disks.

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Microlensing Discovery of a Tight, Low-Mass-Ratio Planetary-Mass Object Around an Old Field Brown Dwarf

Cited by 83 publications

References 38 publications

Brown dwarf disks with ALMA: Evidence for truncated dust disks in Ophiuchus

Brown dwarf disks with ALMA: Evidence for truncated dust disks in Ophiuchus

Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1

An Earth-mass Planet in a 1 au Orbit around an Ultracool Dwarf

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