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Register a new userTwo intermediate-mass transiting brown dwarfs from the TESS mission
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We report the discovery of two intermediate-mass brown dwarfs (BDs), TOI-569b and TOI-1406b, from NASAs Transiting Exoplanet Survey Satellite mission. TOI-569b has an orbital period of $P = 6.55604 pm 0.00016$ days, a mass of $M_b = 64.1 pm 1.9 M_J$, and a radius of $R_b = 0.75 pm 0.02 R_J$. Its host star, TOI-569, has a mass of $M_star = 1.21 pm 0.03 M_odot$, a radius of $R_star = 1.47 pm 0.03 R_odot$, $rm [Fe/H] = +0.29 pm 0.09$ dex, and an effective temperature of $T_{rm eff} = 5768 pm 110K$. TOI-1406b has an orbital period of $P = 10.57415 pm 0.00063$ days, a mass of $M_b =46.0 pm 2.7 M_J$, and a radius of $R_b = 0.86 pm 0.03 R_J$. The host star for this BD has a mass of $M_star =1 .18 pm 0.09 M_odot$, a radius of $R_star = 1.35 pm 0.03 R_odot$, $ rm [Fe/H] = -0.08 pm 0.09$ dex and an effective temperature of $T_{rm eff} = 6290 pm 100K$. Both BDs are in circular orbits around their host stars and are older than 3 Gyr based on stellar isochrone models of the stars. TOI-569 is one of two slightly evolved stars known to host a transiting BD (the other being KOI-415). TOI-1406b is one of three known transiting BDs to occupy the mass range of $40-50 M_J$ and one of two to have a circular orbit at a period near 10 days (with the first being KOI-205b).Both BDs have reliable ages from stellar isochrones in addition to their well-constrained masses and radii, making them particularly valuable as tests for substellar isochrones in the BD mass-radius diagram.
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We report the discovery of two transiting brown dwarfs (BDs), TOI-811b and TOI-852b, from NASAs Transiting Exoplanet Survey Satellite mission. These two transiting BDs have similar masses, but very different radii and ages. Their host stars have similar masses, effective temperatures, and metallicities. The younger and larger transiting BD is TOI-811b at a mass of $M_b = 55.3 pm 3.2{rm M_J}$ and radius of $R_b = 1.35 pm 0.09{rm R_J}$ and it orbits its host star in a period of $P = 25.16551 pm 0.00004$ days. Its age of $93^{+61}_{-29}$ Myr, which we derive from an application of gyrochronology to its host star, is why this BDs radius is relatively large, not heating from its host star since this BD orbits at a longer orbital period than most known transiting BDs. This constraint on the youth of TOI-811b allows us to test substellar mass-radius isochrones where the radius of BDs changes rapidly with age. TOI-852b is a much older (4.0 Gyr from stellar isochrone models of the host star) and smaller transiting BD at a mass of $M_b = 53.7 pm 1.3{rm M_J}$, a radius of $R_b = 0.75 pm 0.03{rm R_J}$, and an orbital period of $P = 4.94561 pm 0.00008$ days. TOI-852b joins the likes of other old transiting BDs that trace out the oldest substellar mass-radius isochrones where contraction of the BDs radius asymptotically slows. Both host stars have a mass of $M_star = 1.32{rm M_odot}pm0.05$ and differ in their radii, $T_{rm eff}$, and [Fe/H] with TOI-811 having $R_star=1.27pm0.09{rm R_odot}$, $T_{rm eff} = 6107 pm 77$K, and $rm [Fe/H] = +0.40 pm 0.09$ and TOI-852 having $R_star=1.71pm0.04{rm R_odot}$, $T_{rm eff} = 5768 pm 84$K, and $rm [Fe/H] = +0.33 pm 0.09$. We take this opportunity to examine how TOI-811b and TOI-852b serve as test points for young and old substellar isochrones, respectively.
We report the discovery of an intermediate-mass transiting brown dwarf, TOI-503b, from the TESS mission. TOI-503b is the first brown dwarf discovered by TESS and orbits a metallic-line A-type star with a period of $P=3.6772 pm 0.0001$ days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the brown dwarfs radius ($R_b = 1.34^{+0.26}_{-0.15} R_J$). We obtained high-resolution spectroscopic observations with the FIES, Ondv{r}ejov, PARAS, Tautenburg, and TRES spectrographs and measured the mass of TOI-503b to be $M_b = 53.7 pm 1.2 M_J$. The host star has a mass of $M_star = 1.80 pm 0.06 M_odot$, a radius of $R_star = 1.70 pm 0.05 R_odot$, an effective temperature of $T_{rm eff} = 7650 pm 160$K, and a relatively high metallicity of $0.61pm 0.07$ dex. We used stellar isochrones to derive the age of the system to be $sim$180 Myr, which places its age between that of RIK 72b (a $sim$10 Myr old brown dwarf in the Upper Scorpius stellar association) and AD 3116b (a $sim$600 Myr old brown dwarf in the Praesepe cluster). We argue that this brown dwarf formed in-situ, based on the young age of the system and the long circularization timescale for this brown dwarf around its host star. TOI-503b joins a growing number of known short-period, intermediate-mass brown dwarfs orbiting main sequence stars, and is the second such brown dwarf known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the brown dwarf desert ($35-55 M_J sin{i}$) is reforesting and its mass range shrinking.
The lowest-mass stars, brown dwarfs and giant exoplanets span a minimum in the mass-radius relationship that probes the fundamental physics of extreme states of matter, magnetism, and fusion. This White Paper outlines scientific opportunities and the necessary resources for modeling and measuring the mass-radius relationship in this regime.
The number of brown dwarfs (BDs) now identified tops 700. Yet our understanding of these cool objects is still lacking, and models are struggling to accurately reproduce observations. What is needed is a method of calibrating the models, BDs whose properties (e.g. age, mass, distance, metallicity) that can be independently determined can provide such calibration. The ability to calculate properties based on observables is set to be of vital importance if we are to be able to measure the properties of fainter, more distant populations of BDs that near-future surveys will reveal, for which ground based spectroscopic studies will become increasingly difficult. We present here the state of the current population of age benchmark brown dwarfs.
The number of low-mass brown dwarfs and even free floating planetary mass objects in young nearby star-forming regions and associations is continuously increasing, offering the possibility to study the low-mass end of the IMF in greater detail. In this paper, we present six new candidates for (very) low-mass objects in the Taurus star-forming region one of which was recently discovered in parallel by Luhman et al. (2009). The underlying data we use is part of a new database from a deep near-infrared survey at the Calar Alto observatory. The survey is more than four magnitudes deeper than the 2MASS survey and covers currently ~1.5 square degree. Complementary optical photometry from SDSS were available for roughly 1.0 square degree. After selection of the candidates using different color indices, additional photometry from Spitzer/IRAC was included in the analysis. In greater detail we focus on two very faint objects for which we obtained J-band spectra. Based on comparison with reference spectra we derive a spectral type of L2+/-0.5 for one object, making it the object with the latest spectral type in Taurus known today. From models we find the effective temperature to be 2080+/-140 K and the mass 5-15 Jupiter masses. For the second source the J-band spectrum does not provide a definite proof of the young, low-mass nature of the object as the expected steep water vapor absorption at 1.33 micron is not present in the data. We discuss the probability that this object might be a background giant or carbon star. If it were a young Taurus member, however, a comparison to theoretical models suggests that it lies close to or even below the deuterium burning limit (<13 Jupiter masses) as well. A first proper motion analysis for both objects shows that they are good candidates for being Taurus members.
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