A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: Cold neptunes are common

Sumi, T.; Bennett, D. P.; Bond, I. A.; Udalski, A.; Batista, V.; Dominik, M.; Fouqué, P.; Kubas, D.; Gould, Andrew; Macintosh, Bruce; Cook, K. H.; Dong, Subo; Skuljan, L.; Cassan, A.; Abe, F.; Botzler, C. S.; Fukui, A.; Furusawa, K.; Hearnshaw, John; Itow, Y.; Kamiya, K.; Kilmartin, P. M.; Korpela, A.; Lin, Wei; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Nagayama, Takahiro; Ohnishi, Koji; Okumura, Teppei; Perrott, Y. C.; Rattenbury, N. J.; Saito, To.; Sako, T.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Yock, P. C. M.; Beaulieu, J. P.; Cole, A. A.; Coutures, C.; Durán, María Fernanda; Greenhill, J.; Jablonski, F.; Marboeuf, U.; Martioli, E.; Pedretti, E.; Pejcha, Ondřej; Rojo, P.; Albrow, M. D.; Brillant, S.; Bode, M. F.; Bramich, D. M.; Burgdorf, M.; Caldwell, J. A. R.; Calitz, H.; Corrales, E.; Dieters, S.; Prester, D. Dominis; Donatowicz, J.; Hill, K.; Hoffman, M.; Horne, K.; Jørgensen, U. G.; Kains, N.; Kane, Stephen R.; Marquette, J. B.; Martín, Roland; Meintjes, Pieter; Menzies, John; Pollard, K. R.; Sahu, Kailash C.; Snodgrass, C.; Steele, I. A.; Street, R. A.; Tsapras, Y.; Wambsganß, J.; Williams, A.; Zub, M.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Wyrzykowski, Ł.; Ulaczyk, K.; Allen, William H.; Christie, Grant; DePoy, D. L.; Gaudi, B. Scott; Han, Cheongho; Janczak, J.; Lee, Chung-Uk; McCormick, J.; Mallia, F.; Monard, B.; Natusch, T.; Park, B.-G.; Pogge, Richard W.; Santallo, R.

doi:10.1088/0004-637x/710/2/1641

Cited by 215 publications

(246 citation statements)

References 77 publications

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“…10 Jup and separation 0.5-10 AU, including constraints obtained by the two previous works by Sumi et al (2010) and Gould et al (2010), and found that there is one planet per star in the Galaxy. Clanton & Gaudi (2014) found that the planet abundances estimated by microlensing are consistent with those found by radial velocity.…”

Section: Introductionmentioning

confidence: 69%

“…In contrast, gravitational microlensing is sensitive to planets orbiting at a few AU away from the host stars down to Earth mass, which is complementary to other methods (Bennett & Rhie 1996). Sumi et al (2010) constructed the planet mass function beyond the snow line and found that Neptune-mass planets are ∼3 times more common than Jupiter-mass planets based on 10 microlensing planets. Gould et al (2010) estimated the planet abundance beyond the snow line based on six events and found that they are 7 times more likely than that at close orbits of 1 AU.…”

Section: Introductionmentioning

confidence: 99%

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Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

Hirao

Udalski

Sumi

et al. 2016

ApJ

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We report the discovery of a planet by the microlensing method, OGLE-2012-BLG-0724Lb. Although the duration of the planetary signal for this event was one of the shortest seen for a planetary event, the anomaly was well covered thanks to high-cadence observations taken by the survey groups OGLE and MOA. By analyzing the light curve, this planetary system is found to have a mass ratio ( ) = ´-q 1.58 0.15 10 3 . By conducting a Bayesian analysis, we estimate that the host star is an M dwarf with a mass of . Because the lens-source relative proper motion is relatively high, future highresolution images would detect the lens host star and determine the lens properties uniquely. This system is likely a Saturn-mass exoplanet around an M dwarf, and such systems are commonly detected by gravitational microlensing. This adds another example of a possible pileup of sub-Jupiters ( )in contrast to a lack of Jupiters ( -M 1 2 Jup ) around M dwarfs, supporting the prediction by core accretion models that Jupitermass or more massive planets are unlikely to form around M dwarfs.

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Section: Introductionmentioning

confidence: 69%

Section: Introductionmentioning

confidence: 99%

Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

Hirao

Udalski

Sumi

et al. 2016

ApJ

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“…The correlation between the planet frequency and the host star metallicity (Santos et al 2001(Santos et al , 2004) and the emerging fact that planets with an intermediate mass between Neptune's and Saturn's are exceedingly rare are both predicted in this theoretical frame. The recent extent of velocimetric surveys to lowmass main-sequence stars (M dwarfs; Mayor et al 2009a,b) has yielded new key evidence in favour of this formation mechanism: for instance, that low-mass planets (about the mass of Neptune) are frequent, while gas giants are seldom found around low-mass stars observed by radial velocity or microlensing techniques (Bonfils et al 2007;Sumi et al 2010). In contrast, the frequency of giant planets should not be affected by the stellar mass in the frame of gravitational instability, as long as circumstellar discs are massive enough to become unstable (Boss 2006).…”

Section: Introductionmentioning

confidence: 99%

Deep infrared imaging of close companions to austral A- and F-type stars

Ehrenreich

Lagrange

Montagnier

et al. 2010

A&A

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The search for substellar companions around stars with different masses along the main sequence is critical to understanding the different processes leading to the formation of low-mass stars, brown dwarfs, and planets. In particular, the existence of a large population of low-mass stars and brown dwarfs physically bound to early-type main-sequence stars could imply that the massive planets recently imaged at wide separations (10-100 AU) around A-type stars are disc-born objects in the low-mass tail of the binary distribution and are thus formed via gravitational instability rather than by core accretion. Our aim is to characterize the environment of early-type main-sequence stars by detecting substellar companions between 10 and 500 AU. The sample stars are also surveyed with radial velocimetry, providing a way to determine the impact of the imaged companions on planets at < ∼ 10 AU. High-contrast and high angular resolution near-infrared images of a sample of 38 southern A-and F-type stars were obtained between 2005 and 2009 with the instruments NaCo on the Very Large Telescope and PUEO on the Canada-France-Hawaii Telescope. Direct and saturated imaging were used in the J to K s bands to probe the faint circumstellar environments with contrasts of ∼5 × 10 −2 to 10 −4 at separations of 0. 2 and 1 , respectively. Using coronagraphic imaging, we achieved contrasts between 10 −5 and 10 −6 at separations >5 . Multiepoch observations were performed to distinguish comoving companions from background contaminants. This survey is sensitive to companions of A and F stars in the brown dwarf to low-mass star mass regime. About 41 companion candidates were imaged around 23 stars. Follow-up observations for 83% of these stars allowed us to identify a large number of background contaminants. We report detection of 7 low-mass stars with masses between 0.1 and 0.8 M in 6 multiple systems: the discovery of an M2 companion around the A5V star HD 14943 and detection of HD 41742B around the F4V star HD 41742 in a quadruple system. We resolve the known companion of the F6.5V star HD 49095 as a short-period binary system composed of 2 M/L dwarfs. We also resolve the companions to the astrometric binaries ι Crt (F6.5V) and 26 Oph (F3V), and identify an M3/M4 companion to the F4V star o Gru, associated with an X-ray source. The global multiplicity fraction measured in our sample of A and F stars is ≥16%. This has a probable impact on the radial velocity measurements performed on the sample stars.

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“…The default binary lens parametrization is not optimal for fitting all the microlensing events because the parameters α, q, and in many cases s are not directly constrained by the light curves, in the sense that the observable properties of the microlensing event are not directly relatable to these parameters (Cassan 2008;Sumi et al 2010;Skowron et al 2011;Kains et al 2012). …”

Section: Discussionmentioning

confidence: 99%

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Poleski

Udalski

Bond

et al. 2017

A&A

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We present the discovery of a substellar companion to the primary host lens in the microlensing event MOA-2012-BLG-006. The companion-to-host mass ratio is 0.016, corresponding to a companion mass ofThus, the companion is either a high-mass giant planet or a low-mass brown dwarf, depending on the mass of the primary M * . The companion signal was separated from the peak of the primary event by a time that was as much as four times longer than the event timescale. We therefore infer a relatively large projected separation of the companion from its host of ≈ 10 a.u.(M * /0.5M ) 1/2 for a wide range (3-7 kpc) of host star distances from the Earth. We also challenge a previous claim of a planetary companion to the lens star in microlensing event OGLE-2002-BLG-045.

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A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: Cold neptunes are common

Cited by 215 publications

References 77 publications

Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

Deep infrared imaging of close companions to austral A- and F-type stars

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

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