HATS-71b: A giant planet transiting an M3 dwarf star in TESS Sector 1

Bakos, G. Á.; Bayliss, Daniel; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J. D.; Henning, Th.; Jordán, Andrés; Mancini, L.; Penev, K.; Sarkis, P.; Suc, V.; Val-Borro, Miguel de; Zhou, G.; Butler, R. Paul; Crane, Jeffrey D.; Durkan, S.; Shectman, Stephen; Kim, J.; Lázár, J.; Papp, I.; Sári, P.; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Chacon, A. D.; Fürész, Gábor; Goeke, B.; Li, J.; Quinn, Samuel N.; Quintana, Elisa V.; Tenenbaum, P.; Teske, Johanna; Vezie, Michael; Yu, Li; Stockdale, Chris; Evans, P.; Relles, Howard M.

doi:10.48550/arxiv.1812.09406

Cited by 11 publications

(12 citation statements)

References 36 publications

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“…8. The planets are 1) Kepler-45b (Johnson et al 2012), 2) NGTS-1b (Bayliss et al 2018), 3) HATS-6b (Hartman et al 2015), 4) HATS-71Ab (Bakos et al 2018), and 5) GJ 674b (Bonfils et al 2007); and the brown dwarfs are I) LP 261-75b (Reid & Walkowicz 2006), II) AD 3116b (Gillen et al 2017), and III) NLTT 41135b (Irwin et al 2010) (excluding objects with periods larger than 200 days and radii larger than 2 R Jup , although the recent discovery of GJ 3512 (Morales et al 2019) with an orbital period of 204 days deserves to be mentioned). At the moment these objects or their host stars do not seem to share any clear common characteristics.…”

Section: Discussionmentioning

confidence: 99%

MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf

Parviainen

Πάλλη

Osorio

et al. 2020

A&A

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Context. We report the discovery of TOI 263.01 (TIC 120916706), a transiting substellar object (R = 0.87 R Jup ) orbiting a faint M3.5 V dwarf (V = 18.97) on a 0.56 d orbit.Aims. We set out to determine the nature of the TESS planet candidate TOI 263.01 using ground-based multicolour transit photometry. The host star is faint, which makes RV confirmation challenging, but the large transit depth makes the candidate suitable for validation through multicolour photometry.Methods. Our analysis combines three transits observed simultaneously in r , i , and z s bands using the MuSCAT2 multicolour imager, three LCOGT-observed transit light curves in g , r , and i bands, a TESS light curve from Sector 3, and a low-resolution spectrum for stellar characterisation observed with the ALFOSC spectrograph. We model the light curves with PyTransit using a transit model that includes a physics-based light contamination component that allows us to estimate the contamination from unresolved sources from the multicolour photometry. This allows us to derive the true planet-star radius ratio marginalised over the contamination allowed by the photometry, and, combined with the stellar radius, gives us a reliable estimate of the object's absolute radius. Results. The ground-based photometry strongly excludes contamination from unresolved sources with a significant colour difference to TOI 263. Further, contamination from sources of same stellar type as the host is constrained to levels where the true radius ratio posterior has a median of 0.217 and a 99 percentile of 0.286. The median and maximum radius ratios correspond to absolute planet radii of 0.87 and 1.41 R Jup , respectively, which confirms the substellar nature of the planet candidate. The object is either a giant planet or a brown dwarf (BD) located deep inside the socalled "brown dwarf desert". Both possibilities offer a challenge to current planet/BD formation models and makes TOI 263.01 an object deserving of in-depth follow-up studies.

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Section: Discussionmentioning

confidence: 99%

MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf

Parviainen

Πάλλη

Osorio

et al. 2020

A&A

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“…We perform a global fit to the light curves, radial velocities, spectroscopically measured stellar atmospheric parameters, broad-band photometry, and parallax from Gaia DR2, using the methods described in Hartman et al (2019), with modifications as summarized most recently by Bakos et al (2018). The fit is carried out using a modified version of the lfit program which is included in the fitsh software package (Pál 2012).…”

Section: Transiting Planet Modellingmentioning

confidence: 99%

HATS-74Ab, HATS-75b, HATS-76b and HATS-77b: Four Transiting Giant Planets around K and M Dwarfs

Jordán,

Hartman,

Bayliss

et al. 2021

Preprint

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“…We purposely ignored M dwarfs in our study because these stars are not expected to form many hot Jupiters (Obermeier et al 2016;Mordasini et al 2012). Up to now only a few Jupiter size planets were discovered around M dwarfs (Bayliss et al 2018;Bakos et al 2018;Hartman et al 2015;Johnson et al 2012). Note that all of them have T eq < 1000 K which is outside of the temperature range considered in this work.…”

Section: Chemical Kinetic Modelmentioning

confidence: 99%

Stellar impact on disequilibrium chemistry and on observed spectra of hot Jupiter atmospheres

Shulyak,

Lara,

Rengel

et al. 2020

Preprint

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Aims. In this work we study the effect of disequilibrium processes (photochemistry and vertical transport) on mixing ratio profiles of neutral species and on the simulated spectra of a hot Jupiter exoplanet that orbits stars of different spectral types. We additionally address the impact of stellar activity that should be present to a different degree in all stars with convective envelopes. Methods. We used the VULCAN chemical kinetic code to compute number densities of species in irradiated planetary atmospheres. The temperature-pressure profile of the atmosphere was computed with the HELIOS code. We also utilized the τ-REx forward model to predict the spectra of planets in primary and secondary eclipses. In order to account for the stellar activity we made use of the observed solar XUV spectrum taken from Virtual Planetary Laboratory (VPL) as a proxy for an active sun-like star. Results. We find large changes in mixing ratios of most chemical species in planets orbiting A-type stars that radiate strong XUV flux inducing a very effective photodissociation. For some species, these changes can propagate very deep into the planetary atmosphere to pressures of around 1 bar. To observe disequilibrium chemistry we favor hot Jupiters with temperatures T eq = 1000 K and ultra-hot Jupiters with T eq ≈ 3000 K that also have temperature inversion in their atmospheres. On the other hand, disequilibrium calculations predict no noticeable changes in spectra of planets with intermediate temperatures. We also show that stellar activity similar to the one of the modern Sun drives important changes in mixing ratio profiles of atmospheric species. However, these changes take place at very high atmospheric altitudes and thus do not affect predicted spectra. Finally, we estimate that the effect of disequilibrium chemistry in planets orbiting nearby bright stars could be robustly detected and studied with future missions with spectroscopic capabilities in infrared such as, e.g., JWST and ARIEL.

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HATS-71b: A giant planet transiting an M3 dwarf star in TESS Sector 1

Cited by 11 publications

References 36 publications

MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf

MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf

HATS-74Ab, HATS-75b, HATS-76b and HATS-77b: Four Transiting Giant Planets around K and M Dwarfs

Stellar impact on disequilibrium chemistry and on observed spectra of hot Jupiter atmospheres

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