arXiv:1603.07597v1 [astro-ph.EP] 24 Mar 2016 D rltim(i ohlu- n eim4 respectively, helium-4, and typically deuteriu helium-3 for fuse to who only (Li) dwarfs lithium brown or fusio sit (D) natural limits no these exhibit Between who all. objects planetary of regime the ta.21)ad75–80 and 2011) al. et h oenlwraduprlmt o rw wrsae11–16 are dwarfs brown for limits p upper giant and gas lower of most modern t structure The of the and resembles inside consist course, core of they structure, gas because Jupiter-li electron surprising of degenarate contraction not hydrogen-forming the is to This similar planets. quite is event (Bara this simp contract they phase and this down after because life-cycle their in event iloso er,s hyaecle tr;blw13 below stars; called are million they for so – years, elements of heavier billions or helium hydrogen, of fusion netgtdsm eae g,i a on htahdoe g hydrogen a 80 that over found was sphere it ago, decades some investigated 2007). Lodato plane & harbour (Payne can Earth-masses studi they 5 not about although are to hosts, up they ha planet and as can as clear; they objects enough not system; host well is planetary as habitability a both whose in known moons objects well additional not as is well their habitability Galaxy; the on of sys evolution pact dynamical planetary and of chemical evolution the in in formation, planet in derstood separate a right? form own as they their do stars in or they objects (2001), are celestial al of or giant et class Trentham suggest, gaseous in (2015) find they can Rauer Are we & dwarfs? Hatzes brown as classify planets we shall How Introduction 1. r1 rniigbn d rw wrsaekon(al ) de extended 1), (Table we 1 known and Only are dwarfs 2015). 2014 brown al. Ge fide bona et & transiting Csizmadia Ma 13 see or in (Johnston CoRoT-33b, o listed with single closer are list on (65 are their stars au host rest 2 their the than orbit bit dwarfs systems, brown binary 66 Only in 2015). are 400 than M h oo eayBook 2016 25, Legacy March CoRoT The jup xlrto ftebondafrgm rudslrlk sta solar-like around regime dwarf brown the of Exploration hntemnmmms-ii ohl ula uinwas fusion nuclear hold to mass-limit minimum the When un- well not is role their problem, classification the Beyond h ubro nw rw wrsi vr20 n more and 2200 over is dwarfs brown known of number The eedn neatitra hmclcmoiin(Spiegel composition chemical internal exact in depending ae ailvlct measurements. velocity radial based Results. Methods. Aims. ob 0 be to Ruther Berlin, e-mail: 12489 Planetenforschung, für Institut DLR, e words. Key umr fteCRTbondafivsiain r presen are investigations dwarf brown CoRoT the of summary A . 20 [email protected] oo eetdtretastn rw wrsaon n d G and F around dwarfs brown transiting three detected CoRoT ± rniigbondaf rudslrlk tr eestudie were stars like solar around dwarfs brown Transiting M 0 jup in lntfrain–tast–bondwarf brown – transit – formation planet giant . 5 rudslrlk tr hc scmail ihteval the with compatible is which stars solar-like around 15% ∼ a nuhms ohl ula uin– fusion nuclear hold to mass enough has 0 M . yswihsud eyepisodic very a sounds which Myrs 1 jup ff ta.20) hi vlto after evolution Their 2003). al. et e hpe o corot-book-csizmadia_language_corrected no. chapter (Bara ff ta.20) respectively. 2002), al. et e M jup efind we z Csizmadia Sz. ycool ly egas ke lanets. odt ,Germany, 2, fordstr tems, CoRoT ABSTRACT at n to s im- but his ed ve as ly m ts r- 2 - l 07 ae ta.20;Wteme ta.20;Sahlmann 2009; al. et Wittenmyer 2007; Lafrenière al. 2000; et by Butler Patel confirmed & 2007; and (Marcy al. found method this was velocity desert and It radial planets the desert’. dwarf and dwarf stars ’brown than the brown exhib rate called systems, the occurence binary smaller of in much objects a companion habitant as dwarfs, first Brown the CoRoT-3b: 2.1. a ae n yoeadi h etscinw ocnrt on concentrate we section next the in rates. and occurence ind one the the by discuss e one we (Csizmadia Hereafter cases 2015). missions ual al. space et occure both Santerne dwarf 2015; by brown al. similar derived Th found the size-range. that were this surprising rates in not and is periods Jupiter-siz it short for fore at bias same detection the are the jects that Notice years). four edn nhww on h ttso O-8bwoems is mass whose KOI-189b of status the 78 count we how on pending )snebt iso bevdaottesm ubro stars of di number for same but the Tabl 150,000) about (see Kepler observed (ca. by mission detected both dwarfs since brown 1) four co the is This to discoveries. parable dwarf brown three reported has CoRoT CoRoT by found dwarfs Brown 2. stars. those solar-like of around especially systems binary dwarfs, in brown are of which knowledge our of opment and precision good with cases. important radius are and they therefore mass provide Trans values. can composition systems chemical and ma model-independent afor luminosity o and radius, the precise study very in need the impacts we For issues and tioned stars). structure ma FGK internal as evolved evolution, (defined their slightly stars just solar-like or orbit sequence remaining orbits The dwarfs dwarf 2010). one brown brown al. least et eclipsing a Irwin At where 41135Ab, 1). (NLTT known M-dwarf Table an is (see system other whic binary each in eclipsing known orbit systems dwarfs binary brown eclipsing two two least at are There yuigtepooerctm-eiso oo,adground and CoRoT, of time-series photometric the using by d ± ted. eew umrz h otiuino oo otedevel- the to CoRoT of contribution the summarize we Here uie-ass oi sa h rw wr trboundary. star - dwarf brown the at is it so Jupiter-masses, 5 afsas h cuec aeo rw wrswsfound was dwarfs brown of rate occurence The stars. warf 1 eotie yKepler-data. by obtained ue ff rn ieitras(010dy vs days (30–150 time-intervals erent sby rs dob- ed emen- ivid- iting ere- nce m- ss, in et et is it 1 h e f t The CoRoT Lecacy Book al. 2011), as well as by adaptive optics direct imaging (Metchev vestigation can confirm this suspicion, then it seems that tidal & Hillenbrand 2009). interaction between stars and close-in brown dwarfs are strong The discovery of CoRoT-3b definitely means a breakthrough enough to synchronize their stars or trap it in some resonance. and a significant milestone in brown dwarf research (Deleuil et We further discuss this in the light of CoRoT-33b. al. 2008). It was the first object in the brown dwarf desert whose mass and radius were measured from its transiting nature. It was also a surprise because nobody expected the existence of a 2.3. CoRoT-33b, a key object for tidal evolution brown dwarf so close – only 7.8 stellar-radii – to a solar-like star This system was reported in Csizmadia et al. (2015). CoRoT- (Porb = 4.26 days) because radial velocity surveys did not de- 33A could be the presently-known most metal-rich brown dwarf tect any similar object before the discovery of CoRoT-3b (only host star because its metallicity is a [Fe/H] = +0.44 ± 0.1 two suspected objects between a minimum mass of 10 and 20 (the other candidate for this title is HAT-P-13A with [Fe/H] = Jupiter-masses were known at that time, see Deleuil et al. 2008). +0.43 ± 0.1, see Bakos et al. 2009). The host stars of the brown Therefore it was not clear then, that CoRoT-3b is a brown dwarf dwarfs in binary systems seem to be metal-poor (Ma & Ge or a ’super-planet’. A super-planet could be formed via core- 2014), therefore this system helps to extend the sample to the accretion whose mass can be up to 25 Mjup without deuterium- tails of the distribution. burning or such a high-mass object can be formed via collision The host star seems to be older than 4.6 Gyr and likely it of several smaller planetesimals or planets (Deleuil et al. 2008 is even older (maybe as old as 11-12 Gyr). The rotation period and references therein). The origin of CoRoT-3b is still under is too small for a G9V star when we compare it to the braking- debate. Notice that model calculations of Mordasini et al. (2009) mechanisms of the single-star scenarios of Bouvier et al. (1997). predict that high mass planets and brown dwarfs can form up to The measured v sin i, stellar radius, as well as the observablespot 40 Mjup via core-accretion but none of these objects get closer modulation on the light curve show that Prot = 8.95 days. An- than 1 au to their host star (cf. Fig. 9 of Mordasini et al. 2009). other interesting feature of CoRoT-33b, whose mass is 59 Mjup, Although Armitage & Bonnell (2002) proposed a very effective is its eccentric orbit (e = 0.07). Since the orbital period is just migration process for brown dwarfs, it is questionable that it is 5.82 d, the circularization time-scale for such a system is much really so effective that the majority of them are engulfed by their shorter than the age of the system. Even more interestingly, the host stars and this is the cause of the rarity of close-in brown orbital period of the brown dwarf is within 3% of a 3:2 commen- dwarfs. Therefore, if CoRoT-3b (∼ 22 Mjup) and NLTT 41135b surability with the rotational period of the star. (∼ 34Mjup) formed via core-accretion, then it is an intriguing Béky et al. (2014) listed six hot Jupiters where strange com- question how they moved so close to their host stars. mensurabilities can be observed between the stellar rotational At the time of the detection of CoRoT-3b, the authors rate and orbital periods of the planetary companions. They also thought that this object confirms the suspicion that ”transiting gi- suspected that these are just random coincidences between the ant planets (M > 4Mjup) can be found preferentially aroundmore stellar rotational period and the planetary companions’ orbital massive stars than the Sun” (Deleuil et al 2008). The discovery periods(maybea stellar spot at a certain latitude may mimic such of NLTT 41135b, a ∼ 34Mjup gaseous giant planet (or a brown a coincidence due to the differential rotation of the star). How- dwarf) around an M-dwarf is a remarkable counter-example (Ir- ever, several host stars of brown dwarfs rotate faster – even if we win et al. 2010). take into account the normal rate for stellar differential rotation – than we expect from their ages, so such random coincidences 2.2. CoRoT-15b, an oversized brown dwarf cannot explain the observed phenomenain star-brown dwarf sys- tems in general. More likely, we see a long-term interaction be- CoRoT-15b was the second detected transiting brown dwarf tween the star and the close-in, high mass brown dwarf system. (Bouchy et al. 2011a). Its most exciting feature is its high radius This interaction consists of tidal interaction as well as magnetic +0.30 ± relative to its mass (1.12−0.15 Rjup, a mass of 63.3 4.1 Mjup). braking effects. Such a combination of star - planet/brown dwarf Notice that brown dwarfs contract slowly until the equilibrium interaction can explain the observed properties – even the eccen- size in most of their lifetime: but at the beginning they can have tric orbit – of CoRoT-33 and other systems. Details of this phys- as large radius as 4-5 Jupiter radii, but at the age of the Uni- ical mechanism and the results can be found in Ferraz-Mello et verse and at the mass of CoRoT-15b the radius should be around al. (2015). 0.8 Jupiter-radii. The radius-variation is very fast in the first 5 Gyrs (Baraffe et al. 2003). The estimated age of the host star is between 1.14–3.35 Gyr using STAREVOL and 1.9 ± 1.7 Gyr 3. Distance-occurance rate relationship? obtained by CESAM. These do not contradict each other but The CoRoT data allowed us to determine the relative frequency the age is not well constrained - this is a point where PLATO ratio of brown dwarfs to hot Jupiters in the P < 10 days orbital with its well-measured (better than 10%) ages will play a role period range. Using the true frequency of hot Jupiters as given in the study of brown dwarfs and of planets (Rauer et al. 2014). in Wright et al. (2012), an 0.20 ± 0.15% true occurence rate of Therefore Bouchy et al. (2011a) left the question open as to why brown dwarfs was found around solar-like stars for P < 10 days this brown dwarf has large radius: either the system is young, or (Csizmadia et al. 2015). It is also suspected that this occurence cold spots on the brown dwarf surface help to inflate the radius rate follows a power-law up to at least 1000 au orbital separa- or atmospheric processes blow up it with disequilibrium chem- tions: istry. The irradiation effects were found to be negligible in the inflation-process of brown dwarfs. a β f = α (1) Interestingly, CoRoT-15b may be a double-synchronoussys- 1au tem: the orbital period of the brown dwarf and the rotational pe- riod of the star can be equal to each other, but the precision of where f is the occurence rate of brown dwarfs around solar like the rotational period measurement is not enough to make this stars below 1000 au orbital separation and first estimates give, +0.8 ± statement conclusive (Bouchy et al. 2011a). If subsequent in- α = 0.55−0.55%, β = 0.23 0.06 (Csizmadia et al 2015). The 2 Exploration of the brown dwarf regime around solar-like stars by CoRoT occurence rate-separation relationship considers radial velocity, may detect a limited number of microlensing brown dwarfs as microlensing and direct imaging results, too (see the discussion a by-product. Gaia is also able to detect brown dwarfs via its and referencesin Csizmadia et al. 2015).Although ground-based primary technique, namely via astrometry. transit surveys like HAT, WASP etc. did not report this frequency CHEOPS targets known planets and candidates detected by rate so far, the analysis of Kepler data is fully compatible with radial velocity technique (RV). CHEOPS may search for the pos- the CoRoT-results and also supports the aformentioned relation- sible transits of these RV-detected objects which would allow to ship (Santerne et al. 2015). The meaning of this possible rela- determine the inclination and hence their true masses instead of tionship and its connection to formation theories of planetary a lower mass limit; also, their radius becomes known. One can systems is not studied yet. However, it is worth mentioning that propose that CHEOPS may extend its program by checking the models by Mordasini et al. (2009) predicted the formation of possible transits of RV-detected brown dwarf candidates. brown dwarfs via core accretion up to 40 Mjup but none of these There also are several ongoing ground-based surveys which objects get closer than 1 au according to their Fig. 9. Observa- are able to find transiting (NGTS, WASP, HAT, for instance) or tional results of CoRoT, Kepler and ground based surveys (Table microlensing brown dwarfs. However, the low efficiency or ob- 1) shows that somehow these brown dwarfs moved inward sig- servational biases of ground based survey are hard to understand nificantly. and requires further study and a careful check of the existing data for undetected brown dwarfs. The same is to apply to space- based observatories’ data. 4. Summary and future prospects for transiting brown dwarf hunting References CoRoT detected three transiting brown dwarfs, including the Anderson,D. R., Collier Cameron, A., et al. 2011, ApJ, 726, L19 first known such object. All three are very close to their host Armitage, P. J. & Bonnell, I. A. 2002, MNRAS, 330, 11 stars (Porb < 10 days). Two of them (CoRoT-15b and -33b) show Bakos, G. Á. Howard, A. W., Noyes, R. W., et al. 2009, ApJ, interesting commensurabilities between the orbital period of the 707, 446 transiting object and the rotational period of the host star (maybe Baraffe, I., Chabrier, G., Allard, F., & Hauschildt, P. H. 2002, 1:1 in the case of 15b and a strict 3:2 in the case of 33b). Well- A&A, 382, 563 measured masses and first estimates of the radii were reported. Baraffe, I., Chabrier, G., Barman, T. S., et al. 2003, A&A, 402, CoRoT-33b also has an eccentric orbit and all three objects can 701 be subject of future tidal evolution studies. The occurence rate Béky B., Holman, M. J., Kipping, D. M., & Noyes, R. W. 2014, of brown dwarfs was estimated for the ten days orbital period ± ApJ, 788, 1 range and it was found to be 0.2% 0.15% and this was con- Bonomo, A. S., Sozzetti, A., Santerne, A., et al. 2015, A&A, firmed by an analysis of the Kepler-data later (Santerne et al. 575, A85 2015). The presence of such close-in brown dwarfs is a chal- Bouchy,F., Deleuil, M., Guillot, T., et al. 2011a, A&A, 525, A68 lange for presently known formation theories. Bouchy, F., Bonomo, A. S., Santerne, A., et al. 2011b, A&A, Transiting brown dwarfs are gold-mines for their studies. 533, A83 The mass and radius (hence their mean density) can be mea- Bouvier, J., Forestini, M., & Allain, S. 1997, A&A, 326, 1023 sured in a model-independentway for them, and the random and Csizmadia Sz., Hatzes, A., Gandolfi, D., et al. 2015, A&A, 584, systematic uncertainties of their parameters in such binary sys- A13 tems are dominated mostly by the stellar parameters (in double- David, T. J., Hillenbrand, L. A., Cody, A. M., Carpenter, J. M.,& lined systems this kind of uncertainty does not appear). This will Howard, A. W. 2015, ApJ, submitted (ArXiv.org:1510.08087) be improved by the next generation of instruments which will Deleuil, M., Deeg, H. J., Alonso, R., et al. 2008, A&A, 491, 889 be more sensitive for secondary eclipses and phase curves, like Díaz, R. F., Damiani, C., Deleuil, M., et al. 2013, A&A, 551, L9 PLATO. Since the age can be measured by isochrone fitting or Díaz, R. F., Montagnier,J. L., Bonomo, A. A., et al. 2014, A&A, by asteroseismology in the future (Rauer et al. 2014), the pre- 572, A109 dicted contraction rate of brown dwarfs and thus the theoretical Ferraz-Mello, S., Tadeu dos Santos, M., Folonier, H., et al. 2015, models of them (Baraffe et al. 2003) can be checked. ApJ, 807, 78 Although almost a dozen transiting brown dwarfs are known, Hatzes, A., Rauer, H. 2015, ApJ, 810, L25 this is still too small a sample for such studies. Since the size of Irwin, J., Buchhave, L., Berta, Z., et al. 2010, ApJ, 718, 1553 brown dwarfs is in the Jupiter-sized range or it can be bigger (up Johnson, J. A., Apps, K., Gazak, J. Z., et al. 2011, ApJ, 730, 79 to several Jupiter-radii) for young ones, they can easily be de- Johnston, W. R. 2015, tected from ground, too. However, interestingly, several brown http://www.johnstonsarchive.net/astro/browndwarflist.html, dwarfs are grazing transiters (like NLTT 41135b or CoRoT-33b) checked on 14 June 2015 and that decreases the observed transit depth making the dis- Kenworthy,M., Lacour, S., Kraus, A., et al. 2014, MNRAS, 446, covery hard from ground. For some yet unkown reason, space 411 observatories detected higher brown dwarf/hot Jupiter ratio than Lafrenière, D., Doyon, R., Marois, Ch., et al. 2007, ApJ, 670, what we can suspect from ground based surveys if we simply di- 1367 vide the number of the observed brown dwarfs by the number of Ma, G., & Ge, J. 2014, MNRAS, 439, 2781 hot Jupiters. It is quite unlikely that space observatories missed Marcy, G. W., & Butler, R. P. 2000, PASP, 112, 137 hot Jupiters, more probably this may be a selection effect of the Metchev, S. A., & Hillenbrand, L. A. 2009, ApJS, 181, 62 ground based surveys. Montet, B. J., Johnson, J. A., Muirhead, Ph. S., et al. 2015, ApJ, We foresee several ongoing or planned space missions which 800, 134 are able to detect transiting brown dwarfs, like Gaia (launched Mordasini, C., Alibert, Y., & Benz, W. 2009, A&A, 501, 1139 2013), CHEOPS and TESS (to be launched 2017), PLATO (to Moutou, C., Bonomo, A. S., Bruno, G., et al. 2013, A&A, 558, be launched in 2024). Also, EUCLID (to be launched in 2022) L6 3 The CoRoT Lecacy Book , ⊙ 01M 15), 8: . 0 ± ed after the 6 5 6 7 14 10 30 . 0 en et al. (2012), ff 4 3 ] Ref. . . 2 6 = 07 18 08 18 . . 3 2 1 0 2 ...... 3 2 1.1 12 5 17 8 11 51 52 8 5 7 2 3 2 5.6 2 5.2 9 4.1 8 . . 0 0 + − 23 15 0.06 1 0.08 1 27 4 29 3 + − + 6 1 − + − ± ± ± a 16 a 16 M a 16 a 15 a 13 cm ± ± ± + − / / / / / 5 ± ± / ± ± ± ± . masses are TTV masses, 29 [g h-mass brown dwarf or a 59 09 38 24 13.0 . . 12.40 ρ 157.4 g: 2). 004 2 05 1 53 55 02 90.9 014 170 021 107.6 021 109 07 26.4 022 75.6 023 97.3 038 029 ...... 27 17 12 07 12 10 30 15 09 10 . . Jup ...... 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 R a n + − 0.33 0.26 0.25 0.35 + − + − + − + − + − / / ± ± ± ± ± ± ± ± ± ± ± ± 0.28 n 0.26 n 0.44 n 13 22 24 79 12 0.195 n . . . . . BD 116 75 10 82 01 . 1 1 . . . . R 485 798 889 833 807 998 . 1 0 . . . . . 0 1 58 2 47 2 8 6.5 8 1 1 0 8 5.0 69 0 93 1 . 1 1 89 0 4 0 0 0 4 0 h h h ...... 93 91 8 7 1 5 3 2 h . . Jup 1 ...... 0 0 6 n 4 2 2 2 2 0 4 0 2 1 3 H] value is reported in the reference. Notice that 0 0 1 1 1 1 1 1 8 86 74 41 . / + − M + − = − + − ± . . . ± ± ± ± ± ± ± ± ± ± ± ± ± ± / 8 0 1 . . . 13 00 [M 7 7 6 6 3 7 9 0 18 15 18 . 66 ...... BD 79 22 14 38 . 96 . . . . . < < < < b: 18 27 0042 25 0042 23 002 64 002 62 0016 59 057 20 032 62 0037 78 022 023 ...... 01 007 . . 0 0 0 0 0 0 0 0 0 0 0.0060 56 0.0060 35 0 0 a a a a 20 a 33 a rd et al. (2012), 6: Bouchy et al. (2011b), 7: Bonomo et al. (20 + − / / / / / / + − e M a of the component A is given here. Star B has ± ± ± ± ± ± ± ± ± ± 0.015 40 0.031 39 01 ne one can find the questionable systems. Periods are truncat . 121 < < . : Kenworthy et al. (2014), 14: Irwin et al. (2010), 15: Ste 030 698 112 056 . . . . 3227 3227 0700 2746 . . . . 900 n 788 0 ± 713 0 . 720 087 0 087 0 713 0 720 360 0 451 0 451 0 . 889 n 779 0.3225 819 0 . 779 0.3225 . 217 0 156 0 60 256 0.0 21 . 060 0 63 ...... (days) structured (protoplanetary?) disc, see Mamajek et al. (201 4 4 9 9 4 Díaz et al. (2014) concluded that KOI-189b can be either a hig P d: b 04 31.330 n . 0.10 5 0.26 12 0.079 1 0.12 11 0.14 21 0.08 12 0.12 11 0.2 3 0 0.11 166 0.10 4 0.10 21 0.12 30 H] 0.06 a 5.729 n a 38.558 n a 3725 a 18.648 n ± ± ± ± ± ± ± ± / / / / / ± ± ± ± ± ± n 0.1 o brown dwarfs orbit each other. 41 0.44 0.03 0.18 0.10 0.04 0.14 . + 0.052 + + + + + + aka KOI-423b. + c: 80 -0.24 80 21 49 97 -0.08 75 60 0 20 40 -0.07 60 130 0.0 2 140 -0.29 200 100 140 -0.02 100 200 [K] [Fe + − ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± rown dwarfs orbit each other. Identical to V2384 Orionis. star T 5810 5225 6516 6260 6350 15) 11 4400 007 3431 019 6201 15 5400 008 3130 09 6740 020 5237 ⊙ 045 035 015 3230 . . . 020 5400 . . . . 15 10 08 11 10 31 14 ...... 14 0 0 0 0 0 0 0 0 0 R 0 0 0 0 0 0 0 . 0.017 4952 0.10 6350 ), 3: Bouchy et al. (2011a), 4: Csizmadia et al. (2015) 5: Sive 0 0 + − / + − 0 − + − + − ± ± ± ± ± ± ± ± ± ± ± H] to the same scale. / 39 15 94 46 star . . . . 13), 11: Johnson et al. (2011), 12: Anderson et al. (2011), 13 471 rsion of the one published in Csizmadia et al. (2015). 99 59 56 R . 1 21 . 87 . . the brown dwarf orbits companion A of a binary system, and dat . . 380 295 378 841 1.40 . . . . 0 0 is the mean density of the brown dwarf component. Below the li e: ρ ⊙ 019 0 026 1 16 0 063 1 06 1 009 0 04 0 09 1 12 1 033 0 051 0.733 ...... 03 04 07 06 06 07 026 022 ...... 0 0 0 0 0 0 0 0 0 0 0 M 0 0 0 0 0 0 0 0 / + − + − + − ± ± ± ± ± ± ± ± ± ± ± star 96 10 29 188 . . . . 65 94 86 37 32 the host star is young (16 Myr) and surrounded by a multiring- 1 . . . . . M 381 166 335 370 925 764 ...... f: 0 a 0 / 15.5V 0.83 0.73 5145 n 16.0V 0.89 0.98 5858 n 16.0V 0.89 0.98 5858 n 19.21R 12.4V 0.9 0 n 13.88V 0 14.43R 1 12.29K 0 f a a full name is EPIC 203 868 608. Similar system to 2M0535-05: tw i i e e g g c c g g i: d ]; we did not convert the inhomogeneous [Fe H 30 K (Johnson et al. 2011). / ± Fe Kepler-57b EPIC 2038b Kepler-53c EPIC 2038a NLTT41135b 8.44V 0 LHS 6343C WASP-30b 11.91V1 Kepler-53b Name2M0535-05a Mag 1SWASP J1407b Kepler-27c LHS 6343C KELT-1b 10.63V1 KOI-205b 0 KOI-415b 12.66K 0 2M0535-05b CoRoT-33b 14.25R 0 Kepler-39b Kepler-39b CoRoT-3b 13.29V 1 CoRoT-15b 15.4R 1 KOI-189b KOI-205b 14.47i 0 upper limit. 2M0535-05 is an extreme young eclipsing system in which two b [ Basic data of known transiting brown dwarfs. en et al. (2013), 17: Montet et al. (2015), 18: David et al. (20 h: ≅ a: References: 1: Stassun et al. (2006), 2: Deleuil et al. (2008 ff 3030 ] H = / ff e M very low mass star, too, therefore its status is uncertain. [ T 16: Ste Notes. not RV. Díaz et al. (2014), 9: Díaz et al. (2013), 10: Moutou et al. (20 Table 1. Notes. third decimal place. This table is an extended and updated ve

4 Exploration of the brown dwarf regime around solar-like stars by CoRoT

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