EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

Hojjatpanah, S.; Santerne, A.; Dragomir, Diana; Zhou, George; Shporer, Avi; Colón, Knicole D.; Almenara, J. M.; Barrado, D.; Barros, S. C. C.; Bento, J.; Boisse, I.; Bouchy, F.; Brown, D. J. A.; Brown, Timothy M.; Cameron, A. Collier; Cochran, William D.; Deleuil, M.; Díaz, R. F.; Fulton, Benjamin J.; Horne, K.; Hébrard, G.; Lillo-Box, J.; Mawet, Dimitri; Ngo, Henry; Osborn, H.; Πάλλη, Ε.; Petigura, Erik A.; Pollacco, D.; Santos, N. C.; Sefako, Ramotholo; Siverd, Robert J.; Sousa, S. G.; Tsantaki, M.

doi:10.3847/1538-3881/153/1/15

Cited by 42 publications

(29 citation statements)

References 76 publications

(66 reference statements)

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“…Independently of any assumptions for the primary star, we obtain a surface gravity log g 2 = 5.50 +0.03 −0.13 for EBLM J0555-57Ab, comparable to that of the recently announced brown dwarf EPIC 201702477b (Bayliss et al 2017). We determine a mass function f (m) = 0.0003686 −0.0017 .…”

Section: Resultsmentioning

confidence: 77%

The EBLM project

Boetticher

Triaud

Queloz

et al. 2017

A&A

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We report the discovery of an eclipsing binary system with mass-ratio q ∼ 0.07. After identifying a periodic photometric signal received by WASP, we obtained CORALIE spectroscopic radial velocities and follow-up light curves with the Euler and TRAPPIST telescopes. From a joint fit of these data we determine that EBLM J0555-57 consists of a sun-like primary star that is eclipsed by a low-mass companion, on a weakly eccentric 7.8-day orbit. Using a mass estimate for the primary star derived from stellar models, we determine a companion mass of 85 ± 4 M Jup (0.081 M ) and a radius of 0.84 +0.14 −0.04 R Jup (0.084 R ) that is comparable to that of Saturn. EBLM J0555-57Ab has a surface gravity log g 2 = 5.50 +0.03 −0.13 and is one of the densest non-stellar-remnant objects currently known. These measurements are consistent with models of low-mass stars.Key words. binaries: eclipsing -binaries: spectroscopic -stars: low-mass -techniques: spectroscopic -techniques: photometricstars: individual: EBLM J0555-57AbEclipsing binary stars enable empirical measurements of the stellar mass-radius relation. The low-mass regime, down to the hydrogen-burning mass limit, is poorly constrained by measurements of mass and radius, but is of particular relevance to the study of exoplanets. Stars with masses below 0.25 M are the most common stellar objects (Kroupa 2001;Chabrier 2003;Henry et al. 2006) and prove to be excellent candidates for the detection of Earth-sized planets (Berta- Gillon et al. 2016Gillon et al. , 2017Luger et al. 2017) and their atmospheric characterization (de Wit et al. 2016). Determining the properties of exoplanets requires an accurate knowledge of their host star parameters, in particular the stellar mass. This motivates the study of low-mass eclipsing binaries (henceforth EBLMs; Triaud et al. 2013;Gómez Maqueo Chew et al. 2014), to empirically measure the mass-radius relation. In this context, we report our results on the eclipsing binary EBLM J0555-57. The system was detected by the Wide Angle Search for PlanetsThe photometry tables and radial velocities are only available at the CDS and on demand via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)

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Section: Resultsmentioning

confidence: 77%

The EBLM project

Boetticher

Triaud

Queloz

et al. 2017

A&A

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“…In fact, according to the NASA Exoplanet Archive (Akeson et al 2013), K2-115b is currently 27 the longest-period K2 transiting exoplanet with a well constrained mass (but see Bayliss et al 2017).…”

Section: Discussionmentioning

confidence: 99%

K2-114b and K2-115b: Two Transiting Warm Jupiters

Shporer

Zhou

Fulton

et al. 2017

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We report the first results from a search for transiting warm Jupiter exoplanets-gas giant planets receiving stellar irradiation below about 10 8 erg s −1 cm −2 , equivalent to orbital periods beyond about 10 days around Sun-like stars. We have discovered two transiting warm Jupiter exoplanets initially identified as transiting candidates in K2 photometry. K2-114b has a mass of , and an orbital period of 20.3days. Both planets are among the longest-period transiting gas giant planets with a measured mass, and they are orbiting relatively old host stars. Both planets are not inflated, as their radii are consistent with theoretical expectations. Their position in the planet radius-stellar irradiation diagram is consistent with the scenario where the radius-irradiation correlation levels off below about 10 8 erg s −1 cm −2 , suggesting that for warm Jupiters stellar irradiation does not play a significant role in determining the planet radius. We also report our identification of another K2 transiting warm Jupiter candidate, EPIC 212504617, as a false positive.

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“…We use a value of 5.84 ± 0.03 pc for GJ 570D from Hipparcos parallax measurements (van Leeuwen 2007) and 3.6224 ± 0.0037 pc for Indi (King et al 2010), respectively. Based on Table 6 from Bayliss et al (2017), who measured the transit radii of 12 brown dwarfs, we adopt a value of 1 Jupiter radius for R (see also Figure 1 in Burrows & Liebert (1993), that shows the predicted radii for brown dwarfs being around 1 Jupiter radius, independently of the object's mass). We note, however, that any error in either the distance or the assumed radius will be included in our retrieved calibration factor f .…”

Section: Atmospheric Retrieval Of Measured Brown Dwarf Spectramentioning

confidence: 99%

Supervised Machine Learning for Intercomparison of Model Grids of Brown Dwarfs: Application to GJ 570D and the Epsilon Indi B Binary System

Oreshenko

Kitzmann

Márquez-Neila

et al. 2019

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Self-consistent model grids of brown dwarfs involve complex physics and chemistry, and are often computed using proprietary computer codes, making it challenging to identify the reasons for discrepancies between model and data as well as between the models produced by different research groups. In the current study, we demonstrate a novel method for analyzing brown dwarf spectra, which combines the use of the Sonora, AMES-cond and HELIOS model grids with the supervised machine learning method of the random forest. Besides performing atmospheric retrieval, the random forest enables information content analysis of the three model grids as a natural outcome of the method, both individually on each grid and by comparing the grids against one another, via computing large suites of mock retrievals. Our analysis reveals that the different choices made in modeling the alkali line shapes hinder the use of the alkali lines as gravity indicators. Nevertheless, the spectrum longward of 1.2 µm encodes enough information on the surface gravity to allow its inference from retrieval. Temperature may be accurately and precisely inferred independent of the choice of model grid, but not the surface gravity. We apply random forest retrieval to three objects: the benchmark T7.5 brown dwarf GJ 570D; and Indi Ba (T1.5 brown dwarf) and Bb (T6 brown dwarf), which are part of a binary system and have measured dynamical masses. For GJ 570D, the inferred effective temperature and surface gravity are consistent with previous studies. For Indi Ba and Bb, the inferred surface gravities are broadly consistent with the values informed by the dynamical masses.

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EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

Cited by 42 publications

References 76 publications

The EBLM project

The EBLM project

K2-114b and K2-115b: Two Transiting Warm Jupiters

Supervised Machine Learning for Intercomparison of Model Grids of Brown Dwarfs: Application to GJ 570D and the Epsilon Indi B Binary System

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