The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Yee, Samuel W.; Winn, Joshua N.; Hartman, J. D.; Rodriguez, Joseph E.; Zhou, George; Quinn, Samuel N.; Latham, David W.; Bieryla, Allyson; Collins, Karen A.; Angelo, Isabel; Barkaoui, Khalid; Benni, Paul; W., Boyle, Andrew; Brahm, R.; Butler, R. Paul; Ciardi, David R.; Collins, Kevin I.; Conti, Dennis M.; Crane, Jeffrey D.; Dai, Fei; Dressing, Courtney D.; Eastman, Jason D.; Essack, Zahra; Forés-Toribio, Raquel; Furlan, Elise; Gan, Tianjun; Giacalone, Steven; Gill, Holden; Girardin, Éric; Henning, Thomas; Addison, Brett C.; Horner, Jonathan; Howard, Andrew W.; Howell, Steve B.; Huang, Chelsea X.; Isaacson, Howard; Jenkins, Jon M.; Jensen, Eric L. N.; Jordán, Andrés; Kane, Stephen R.; Kielkopf, John F.; Lasota, Slawomir; Levine, Alan M.; Lubin, Jack; Mann, Andrew W.; Massey, Bob; McLeod, Kim K.; Mengel, M. W.; Muñoz, J. A.; Murgas, F.; Πάλλη, Ε.; Plavchan, Peter; Radford, Don J.; Ricker, G.; Rowden, Pamela; Safonov, Boris; Savel, Arjun B.; Schwarz, Richard P.; Sefako, R.; Shporer, Avi; Srdoč, Gregor; Strakhov, Ivan A.; Teske, Johanna; Tinney, C. G.; Tyler, Dakotah; Wittenmyer, Robert A.; Zhang, Hui; Ziegler, Carl

doi:10.3847/1538-3881/ac73ff

“…the desert's upper boundary on stellar properties may yield more insight into the problem. This will require a large, statistically uniform sample of hot Jupiters, which will soon be provided by TESS (Yee et al 2021(Yee et al , 2022. Additional observations aimed at constraining the presence of long-period planetary companions, for instance with Gaia astrometry, could also help to differentiate between these hypotheses.…”

Section: Discussionmentioning

confidence: 99%

The Upper Edge of the Neptune Desert Is Stable Against Photoevaporation

Vissapragada¹,

Knutson²,

et al. 2022

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Transit surveys indicate that there is a deficit of Neptune-sized planets on close-in orbits. If this “Neptune desert” is entirely cleared out by atmospheric mass loss, then planets at its upper edge should only be marginally stable against photoevaporation, exhibiting strong outflow signatures in tracers like the metastable helium triplet. We test this hypothesis by carrying out a 12-night photometric survey of the metastable helium feature with Palomar/WIRC, targeting seven gas-giant planets orbiting K-type host stars. Eight nights of data are analyzed here for the first time along with reanalyses of four previously published data sets. We strongly detect helium absorption signals for WASP-69b, HAT-P-18b, and HAT-P-26b; tentatively detect signals for WASP-52b and NGTS-5b; and do not detect signals for WASP-177b and WASP-80b. We interpret these measured excess absorption signals using grids of Parker wind models to derive mass-loss rates, which are in good agreement with predictions from the hydrodynamical outflow code ATES for all planets except WASP-52b and WASP-80b, where our data suggest that the outflows are much smaller than predicted. Excluding these two planets, the outflows for the rest of the sample are consistent with a mean energy-limited outflow efficiency of ε = 0.41 − 0.13 + 0.16 . Even when we make the relatively conservative assumption that gas-giant planets experience energy-limited outflows at this efficiency for their entire lives, photoevaporation would still be too inefficient to carve the upper boundary of the Neptune desert. We conclude that this feature of the exoplanet population is a pristine tracer of giant planet formation and migration mechanisms.

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“…Rice et al (2022) suggest that this discontinuity may only exist for the low eccentricity population, a trend that would provide strong evidence for high-eccentricity migration as the dominant migration mechanism for hot Jupiters. This hypothesis is also supported by the current population of TESS discovered giant planets (Rodriguez et al 2023;Yee et al 2022). If BDs and giant planets undergo similar migratory processes, then they could exhibit the same discontinuity in stellar obliquity.…”

Section: Placing Hip 33609 In Contextmentioning

confidence: 58%

HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star

Vowell

¹

,

Rodriguez

²

,

Quinn

³

et al. 2023

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We present the discovery and characterization of HIP 33609 b, a transiting warm brown dwarf orbiting a late B star, discovered by NASA's Transiting Exoplanet Survey Satellite as TOI-588 b. HIP 33609 b is a large (R b = 1.580 − 0.070 + 0.074 R J) brown dwarf on a highly eccentric (e = 0.560 − 0.031 + 0.029 ) orbit with a 39 days period. The host star is a bright (V = 7.3 mag), T eff = 10,400 − 660 + 800 K star with a mass of M * = 2.383 − 0.095 + 0.10 M ⊙ and radius of R * = 1.863 − 0.082 + 0.087 R ⊙, making it the hottest transiting brown dwarf host star discovered to date. We obtained radial velocity measurements from the CHIRON spectrograph confirming the companion's mass of M b = 68.0 − 7.1 + 7.4 M J as well as the host star's rotation rate ( v sin i * = 55.6 ± 1.8 km s−1). We also present the discovery of a new comoving group of stars, designated as MELANGE-6, and determine that HIP 33609 is a member. We use a combination of rotation periods and isochrone models fit to the cluster members to estimate an age of 150 ± 25 Myr. With a measured mass, radius, and age, HIP 33609 b becomes a benchmark for substellar evolutionary models.

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“…We have confirmed and characterized 20 new short-period giant planets detected by the TESS mission, based on extensive ground-based photometric, spectroscopic, and imaging observations. These objects join a host of other giant planets that have been discovered by TESS over the last few years (e.g., Rodriguez et al 2019;Zhou et al 2019;Brahm et al 2020;Davis et al 2020;Nielsen et al 2020;Ikwut-Ukwa et al 2021;Rodriguez et al 2021;Sha et al 2021;Wong et al 2021;Knudstrup et al 2022;Psaridi et al 2022;Rodriguez et al 2022;Yee et al 2022), showcasing how TESS is rapidly transforming our knowledge of hot Jupiters by providing a uniform, all-sky sample of these planets. Yee et al (2021) found that the sample of known transiting hot Jupiters was only ∼40% complete at a magnitude-limit of G < 12.5.…”

Section: Discussionmentioning

confidence: 99%

The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets*

Yee

¹

,

Winn

²

,

Hartman

³

et al. 2023

ApJS

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NASA’s Transiting Exoplanet Survey Satellite (TESS) mission promises to improve our understanding of hot Jupiters by providing an all-sky, magnitude-limited sample of transiting hot Jupiters suitable for population studies. Assembling such a sample requires confirming hundreds of planet candidates with additional follow-up observations. Here we present 20 hot Jupiters that were detected using TESS data and confirmed to be planets through photometric, spectroscopic, and imaging observations coordinated by the TESS Follow-up Observing Program. These 20 planets have orbital periods shorter than 7 days and orbit relatively bright FGK stars (10.9 < G < 13.0). Most of the planets are comparable in mass to Jupiter, although there are four planets with masses less than that of Saturn. TOI-3976b, the longest-period planet in our sample (P = 6.6 days), may be on a moderately eccentric orbit (e = 0.18 ± 0.06), while observations of the other targets are consistent with them being on circular orbits. We measured the projected stellar obliquity of TOI-1937A b, a hot Jupiter on a 22.4 hr orbit with the Rossiter–McLaughlin effect, finding the planet’s orbit to be well aligned with the stellar spin axis (∣λ∣ = 4.°0 ± 3.°5). We also investigated the possibility that TOI-1937 is a member of the NGC 2516 open cluster but ultimately found the evidence for cluster membership to be ambiguous. These objects are part of a larger effort to build a complete sample of hot Jupiters to be used for future demographic and detailed characterization work.

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The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Cited by 12 publications

References 188 publications

The Upper Edge of the Neptune Desert Is Stable Against Photoevaporation

The Upper Edge of the Neptune Desert Is Stable Against Photoevaporation

HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star

The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets*

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