39 research outputs found
A Low-Mass Pre-Main-Sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
We report the discovery of 2M1222-57 as a low-mass, pre-main-sequence (PMS)
eclipsing binary (EB) in the Lower Centaurus Crux (LCC) association for which,
using Gaia parallaxes and proper motions with a neural-net age estimator, we
determine an age of 16.22.2 Myr. The broadband spectral energy
distribution (SED) shows clear excess at ~10 um indicative of a circumbinary
disk, and new speckle-imaging observations reveal a faint, tertiary companion
separated by ~100 AU. H-alpha emission is modulated on the orbital period,
consistent with theoretical models of orbitally pulsed accretion streams
reaching from the inner disk edge to the central stars. From a joint analysis
of spectroscopically determined radial velocities and TESS light curves,
together with additional tight constraints provided by the SED and the Gaia
parallax, we measure masses for the eclipsing stars of 0.74 Msun and 0.67 Msun;
radii of 0.98 Rsun and 0.94 Rsun; and effective temperatures of 3750 K and 3645
K. The masses and radii of both stars are measured to an accuracy of ~1%. The
measured radii are inflated, and the temperatures suppressed, relative to
predictions of standard PMS evolutionary models at the age of LCC; also, the Li
abundances are ~2 dex less depleted than predicted by those models. However,
models that account for the global and internal effects of surface magnetic
fields are able to simultaneously reproduce the measured radii, temperatures,
and Li abundances at an age of 17.00.5 Myr. Altogether, the 2M1222-57
system presents very strong evidence that magnetic activity in young stars
alters both their global properties and the physics of their interiors.Comment: 23 pages, 19 figures, accepted by Ap
Visual Orbits & Alignments of Planet Hosting Binary Systems
Roughly half of Solar-type planet hosts have stellar companions, so
understanding how these binary companions affect the formation and evolution of
planets is an important component to understanding planetary systems overall.
Measuring the dynamical properties of planet host binaries enables a valuable
test of planet formation in multi-star systems and requires knowledge of the
binary orbital parameters. Using high resolution imaging, we have measured the
relative astrometry and visual orbits of 13 binary systems where one of the
stars is known to host a transiting exoplanet. Our results indicate that the
mutual inclination between the orbits of the binary hosts and the transiting
planets are well aligned. Our results for close binary systems (a<100 AU)
complement past work for wide planet host binaries from Gaia.Comment: Accepted for publication in A
Revised Properties and Dynamical History for the HD 17156 System
From the thousands of known exoplanets, those that transit bright host stars
provide the greatest accessibility toward detailed system characterization. The
first known such planets were generally discovered using the radial velocity
technique, then later found to transit. HD 17156b is particularly notable among
these initial discoveries because it diverged from the typical hot Jupiter
population, occupying a 21.2 day eccentric () orbit, offering
preliminary insights into the evolution of planets in extreme orbits. Here we
present new data for this system, including ground and space-based photometry,
radial velocities, and speckle imaging, that further constrain the system
properties and stellar/planetary multiplicity. These data include photometry
from the Transiting Exoplanet Survey Satellite (TESS) that cover five transits
of the known planet. We show that the system does not harbor any additional
giant planets interior to 10 AU. The lack of stellar companions and the age of
the system indicate that the eccentricity of the known planet may have resulted
from a previous planet-planet scattering event. We provide the results from
dynamical simulations that suggest possible properties of an additional planet
that culminated in ejection from the system, leaving a legacy of the observed
high eccentricity for HD 17156b.Comment: 15 pages, 7 figures, accepted for publication in the Astronomical
Journa
The NASA High-Resolution Speckle Interferometric Imaging Program: Validation and Characterization of Exoplanets and Their Stellar Hosts
Starting in 2008, NASA has provided the exoplanet community an observational program aimed at obtaining the highest resolution imaging available as part of its mission to validate and characterize exoplanets, as well as their stellar environments, in search of life in the Universe. Our current program uses speckle interferometry in the optical (320–1,000 nm) with new instruments on the 3.5-m WIYN and both 8-m Gemini telescopes. Starting with Kepler and K2 follow-up, we now support TESS and other space- and ground-based exoplanet related discovery and characterization projects. The importance of high-resolution imaging for exoplanet research comes via identification of nearby stellar companions that can dilute the transit signal and confound derived exoplanet and stellar parameters. Our observations therefore provide crucial information allowing accurate planet and stellar properties to be determined. Our community program obtains high-resolution imagery, reduces the data, and provides all final data products, without any exclusive use period, to the community via the Exoplanet Follow-Up Observation Program (ExoFOP) website maintained by the NASA Exoplanet Science Institute. This paper describes the need for high-resolution imaging and gives details of the speckle imaging program, highlighting some of the major scientific discoveries made along the way
Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
© 2024. The Author(s). Published by the American Astronomical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/Multiplanet systems exhibit a diversity of architectures that diverge from the solar system and contribute to the topic of exoplanet demographics. Radial velocity (RV) surveys form a crucial component of exoplanet surveys, as their long observational baselines allow for searches for more distant planetary orbits. This work provides a significantly revised architecture for the multiplanet system HD 134606 using both HARPS and UCLES RVs. We confirm the presence of previously reported planets b, c, and d with periods of 12.0897 − 0.0018 + 0.0019 , 58.947 − 0.054 + 0.056 , and 958.7 − 5.9 + 6.3 days and masses of 9.14 − 0.63 + 0.65 , 11.0 ± 1, and 44.5 ± 2.9 Earth masses, respectively, with the planet d orbit significantly revised to over double that originally reported. We report two newly detected super-Earths, e and f, with periods of 4.31943 − 0.00068 + 0.00075 and 26.9 − 0.017 + 0.019 days and masses of 2.31 − 0.35 + 0.36 and 5.52 − 0.73 + 0.74 Earth masses, respectively. In addition, we identify a linear trend in the RV time series, and the cause of this acceleration is deemed to be a newly detected massive companion with a very long orbital period. HD 134606 now displays four low-mass planets in a compact region near the star, one gas giant further out in the habitable zone, an additional companion in the outer regime, and a low-mass M dwarf stellar companion at large separation, making it an intriguing target for system formation/evolution studies. The location of planet d in the habitable zone proves to be an exciting candidate for future space-based direct imaging missions, whereas continued RV observations of this system are recommended for understanding the nature of the massive, long-period companion.Peer reviewe
TESS Discovery of Twin Planets near 2:1 Resonance around Early M-Dwarf TOI 4342
With data from the Transiting Exoplanet Survey Satellite (TESS), we showcase
improvements to the MIT Quick-Look Pipeline (QLP) through the discovery and
validation of a multi-planet system around M-dwarf TOI 4342 (,
, , K,
pc). With updates to QLP, including a new multi-planet search, as well as
faster cadence data from TESS' First Extended Mission, we discovered two
sub-Neptunes ( and ; = 5.538 days and = 10.689 days)
and validated them with ground-based photometry, spectra, and speckle imaging.
Both planets notably have high transmission spectroscopy metrics (TSMs) of 36
and 32, making TOI 4342 one of the best systems for comparative atmospheric
studies. This system demonstrates how improvements to QLP, along with faster
cadence Full-Frame Images (FFIs), can lead to the discovery of new multi-planet
systems.Comment: accepted for publication in A
Three low-mass companions around aged stars discovered by TESS
We report the discovery of three transiting low-mass companions to aged
stars: a brown dwarf (TOI-2336b) and two objects near the hydrogen burning mass
limit (TOI-1608b and TOI-2521b). These three systems were first identified
using data from the Transiting Exoplanet Survey Satellite (TESS). TOI-2336b has
a radius of , a mass of and an orbital
period of 7.71 days. TOI-1608b has a radius of , a mass of
and an orbital period of 2.47 days. TOI-2521b has a radius
of , a mass of and an orbital period of
5.56 days. We found all these low-mass companions are inflated. We fitted a
relation between radius, mass and incident flux using the sample of known
transiting brown dwarfs and low-mass M dwarfs. We found a positive correlation
between the flux and the radius for brown dwarfs and for low-mass stars that is
weaker than the correlation observed for giant planets.Comment: 20 pages, 13 figures; submitted to MNRA
TESS Hunt for Young and Maturing Exoplanets (THYME) IX: a 27 Myr extended population of Lower-Centaurus Crux with a transiting two-planet system
We report the discovery and characterization of a nearby (~ 85 pc), older (27
+/- 3 Myr), distributed stellar population near Lower-Centaurus-Crux (LCC),
initially identified by searching for stars co-moving with a candidate
transiting planet from TESS (HD 109833; TOI 1097). We determine the association
membership using Gaia kinematics, color-magnitude information, and rotation
periods of candidate members. We measure it's age using isochrones,
gyrochronology, and Li depletion. While the association is near known
populations of LCC, we find that it is older than any previously found LCC
sub-group (10-16 Myr), and distinct in both position and velocity. In addition
to the candidate planets around HD 109833 the association contains four
directly-imaged planetary-mass companions around 3 stars, YSES-1, YSES-2, and
HD 95086, all of which were previously assigned membership in the younger LCC.
Using the Notch pipeline, we identify a second candidate transiting planet
around HD 109833. We use a suite of ground-based follow-up observations to
validate the two transit signals as planetary in nature. HD 109833 b and c join
the small but growing population of <100 Myr transiting planets from TESS. HD
109833 has a rotation period and Li abundance indicative of a young age (< 100
Myr), but a position and velocity on the outskirts of the new population, lower
Li levels than similar members, and a CMD position below model predictions for
27 Myr. So, we cannot reject the possibility that HD 109833 is a young field
star coincidentally nearby the population.Comment: 23 pages, 15 figures, Accepted for publication in A
TOI-733 b -- a planet in the small-planet radius valley orbiting a Sun-like star
We report the discovery of a hot ( 1055 K) planet in
the small planet radius valley transiting the Sun-like star TOI-733, as part of
the KESPRINT follow-up program of TESS planets carried out with the HARPS
spectrograph. TESS photometry from sectors 9 and 36 yields an orbital period of
= days and a radius of
= .
Multi-dimensional Gaussian process modelling of the radial velocity
measurements from HARPS and activity indicators, gives a semi-amplitude of
= m s, translating into a planet mass of
= . These
parameters imply that the planet is of moderate density ( =
g cm) and place it in the transition
region between rocky and volatile-rich planets with H/He-dominated envelopes on
the mass-radius diagram. Combining these with stellar parameters and
abundances, we calculate planet interior and atmosphere models, which in turn
suggest that TOI-733 b has a volatile-enriched, most likely secondary outer
envelope, and may represent a highly irradiated ocean world - one of only a few
such planets around G-type stars that are well-characterised.Comment: Accepted for publication in A&