14 research outputs found
The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets
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 twenty 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 (TFOP). These twenty planets have orbital periods
shorter than 7 days and orbit relatively bright FGK stars ().
Most of the planets are comparable in mass to Jupiter, although there are four
planets with masses less than that of Saturn. TOI-3976 b, the longest period
planet in our sample ( days), may be on a moderately eccentric orbit
(), 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 hour orbit with the Rossiter-McLaughlin
effect, finding the planet's orbit to be well-aligned with the stellar spin
axis (). 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.Comment: 67 pages, 11 tables, 13 figures, 2 figure sets. Resubmitted to ApJS
after revision
Another Shipment of Six Short-Period Giant Planets from TESS
We present the discovery and characterization of six short-period, transiting
giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS) --
TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642),
TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), & TOI-2497 (TIC 97568467).
All six planets orbit bright host stars (8.9 <G< 11.8, 7.7 <K< 10.1). Using a
combination of time-series photometric and spectroscopic follow-up observations
from the TESS Follow-up Observing Program (TFOP) Working Group, we have
determined that the planets are Jovian-sized (R = 1.00-1.45 R),
have masses ranging from 0.92 to 5.35 M, and orbit F, G, and K stars
(4753 T 7360 K). We detect a significant orbital eccentricity
for the three longest-period systems in our sample: TOI-2025 b (P = 8.872 days,
= ), TOI-2145 b (P = 10.261 days, =
), and TOI-2497 b (P = 10.656 days, =
). TOI-2145 b and TOI-2497 b both orbit subgiant host
stars (3.8 g 4.0), but these planets show no sign of inflation
despite very high levels of irradiation. The lack of inflation may be explained
by the high mass of the planets; M (TOI-2145
b) and M (TOI-2497 b). These six new discoveries
contribute to the larger community effort to use {\it TESS} to create a
magnitude-complete, self-consistent sample of giant planets with
well-determined parameters for future detailed studies.Comment: 20 Pages, 6 Figures, 8 Tables, Accepted by MNRA
A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation
Progressive osseous heteroplasia: a model for the imprinting effects of GNAS inactivating mutations in humans.
International audienceCONTEXT: Heterozygous GNAS inactivating mutations are known to induce pseudohypoparathyroidism type 1a when maternally inherited and pseudopseudohypoparathyroidism when paternally inherited. Progressive osseous heteroplasia (POH) is a rare disease of ectopic bone formation, and studies in different families have shown that POH is also caused by paternally inherited GNAS mutations. OBJECTIVE: Our purpose was to characterize parental origin of the mutated allele in de novo cases of POH and to draw phenotype/genotype correlations according to maternal or paternal transmission of a same GNAS mutation. DESIGN AND SETTING: We conducted a retrospective study on patients addressed to our referral center for the rare diseases of calcium and phosphorus metabolism. PATIENTS AND METHODS: We matched 10 cases of POH with cases of pseudohypoparathyroidism type 1a carrying the same GNAS mutations. MAIN OUTCOME MEASURES: The parental origin of the mutated allele was studied using informative intragenic polymorphisms and subcloning of PCR products. RESULTS: Paternal origin of GNAS mutations was clearly demonstrated in eight POH cases including one patient with mutation in exon 1. Genotype/phenotype analyses suggest that there is no direct correlation between the ossifying process and the position of the inactivating GNAS mutation. It is, however, more severe in patients in whom origin of the mutation is paternal. Severe intrauterine growth retardation was clearly evidenced in paternally inherited mutations. CONCLUSIONS: Clinical heterogeneity makes genetic counseling a delicate matter, especially in which paternal inheritance is concerned because it can lead to either a mild expression of pseudopseudohypoparathyroidism or a severe expression of POH
TOI-1518b: A Misaligned Ultra-hot Jupiter with Iron in Its Atmosphere
We present the discovery of TOI-1518b-an ultra-hot Jupiter orbiting a bright star (V=8.95). The transiting planet is confirmed using high-resolution optical transmission spectra from EXPRES. It is inflated, with Rp=1.875±0.053 RJ, and exhibits several interesting properties, including a misaligned orbit ( - 240.34+0.98 0.93 degrees) and nearly grazing transit ( = - b 0.9036+0.0053 0.0061). The planet orbits a fast-rotating F0 host star (Teff;7300 K) in 1.9 days and experiences intense irradiation. Notably, the TESS data show a clear secondary eclipse with a depth of 364±28 ppm and a significant phase-curve signal, from which we obtain a relative day-night planetary flux difference of roughly 320 ppm and a 5.2s detection of ellipsoidal distortion on the host star. Prompted by recent detections of atomic and ionized species in ultrahot Jupiter atmospheres, we conduct an atmospheric cross-correlation analysis. We detect neutral iron (5.2s), at = - K 157+ p 44 68 km s-1 and = - - V 16+ sys 4 2, adding another object to the small sample of highly irradiated gas-giant planets with Fe detections in transmission. Detections so far favor particularly inflated gas giants with radii 1.78 RJ, which may be due to observational bias. With an equilibrium temperature of Teq=2492±38 K and a measured dayside brightness temperature of 3237±59 K (assuming zero geometric albedo), TOI-1518b is a promising candidate for future emission spectroscopy to probe for a thermal inversion
TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b
We present the discovery of TOI-1420b, an exceptionally low-density ( ρ = 0.08 ± 0.02 g cm ^−3 ) transiting planet in a P = 6.96 days orbit around a late G-dwarf star. Using transit observations from TESS, LCOGT, Observatoire Privé du Mont, Whitin, Wendelstein, OAUV, Ca l’Ou, and KeplerCam, along with radial velocity observations from HARPS-N and NEID, we find that the planet has a radius of R _p = 11.9 ± 0.3 R _⊕ and a mass of M _p = 25.1 ± 3.8 M _⊕ . TOI-1420b is the largest known planet with a mass less than 50 M _⊕ , indicating that it contains a sizeable envelope of hydrogen and helium. We determine TOI-1420b’s envelope mass fraction to be , suggesting that runaway gas accretion occurred when its core was at most four to five times the mass of the Earth. TOI-1420b is similar to the planet WASP-107b in mass, radius, density, and orbital period, so a comparison of these two systems may help reveal the origins of close-in low-density planets. With an atmospheric scale height of 1950 km, a transmission spectroscopy metric of 580, and a predicted Rossiter–McLaughlin amplitude of about 17 m s ^−1 , TOI-1420b is an excellent target for future atmospheric and dynamical characterization
The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope
We report the discovery of TOI-2180 b, a 2.8 giant planet
orbiting a slightly evolved G5 host star. This planet transited only once in
Cycle 2 of the primary Transiting Exoplanet Survey Satellite (TESS) mission.
Citizen scientists identified the 24 hr single-transit event shortly after the
data were released, allowing a Doppler monitoring campaign with the Automated
Planet Finder telescope at Lick Observatory to begin promptly. The radial
velocity observations refined the orbital period of TOI-2180 b to be
260.80.6 days, revealed an orbital eccentricity of 0.3680.007, and
discovered long-term acceleration from a more distant massive companion. We
conducted ground-based photometry from 14 sites spread around the globe in an
attempt to detect another transit. Although we did not make a clear transit
detection, the nondetections improved the precision of the orbital period. We
predict that TESS will likely detect another transit of TOI-2180 b in Sector 48
of its extended mission. We use giant planet structure models to retrieve the
bulk heavy-element content of TOI-2180 b. When considered alongside other giant
planets with orbital periods over 100 days, we find tentative evidence that the
correlation between planet mass and metal enrichment relative to stellar is
dependent on orbital properties. Single-transit discoveries like TOI-2180 b
highlight the exciting potential of the TESS mission to find planets with long
orbital periods and low irradiation fluxes despite the selection biases
associated with the transit method.Comment: Published in A
A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Astronomers do not have a complete picture of the effects of wide-binary
companions (semimajor axes greater than 100 AU) on the formation and evolution
of exoplanets. We investigate these effects using new data from Gaia EDR3 and
the TESS mission to characterize wide-binary systems with transiting
exoplanets. We identify a sample of 67 systems of transiting exoplanet
candidates (with well-determined, edge-on orbital inclinations) that reside in
wide visual binary systems. We derive limits on orbital parameters for the
wide-binary systems and measure the minimum difference in orbital inclination
between the binary and planet orbits. We determine that there is statistically
significant difference in the inclination distribution of wide-binary systems
with transiting planets compared to a control sample, with the probability that
the two distributions are the same being 0.0037. This implies that there is an
overabundance of planets in binary systems whose orbits are aligned with those
of the binary. The overabundance of aligned systems appears to primarily have
semimajor axes less than 700 AU. We investigate some effects that could cause
the alignment and conclude that a torque caused by a misaligned binary
companion on the protoplanetary disk is the most promising explanation.Comment: 30 pages, 19 figures, 2 csv files included in Arxiv source; accepted
for publication in A