Know thy star, know thy planet: chemo-kinematically characterizing TESS targets

  title={Know thy star, know thy planet: chemo-kinematically characterizing TESS targets},
  author={Andreia Carrillo and Keith Hawkins and Brendan P. Bowler and William D. Cochran and Andrew M. Vanderburg},
  journal={Monthly Notices of the Royal Astronomical Society},
The Transiting Exoplanet Survey Satellite (TESS) has already begun to discover what will ultimately be thousands of exoplanets around nearby cool bright stars. These potential host stars must be well-understood to accurately characterize exoplanets at the individual and population levels. We present a catalogue of the chemo-kinematic properties of 2,218,434 stars in the TESS Candidate Target List using survey data from Gaia DR2, APOGEE, GALAH, RAVE, LAMOST, and photometrically-derived stellar… 

A low-eccentricity migration pathway for a 13-h-period Earth analogue in a four-planet system

It is commonly accepted that exoplanets with orbital periods shorter than one day, also known as ultra-short-period (USP) planets, formed further out within their natal protoplanetary disks before

Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment

We present a catalog of stellar companions to host stars of Transiting Exoplanet Survey Satellite Objects of Interest (TOIs) identified from a marginalized likelihood ratio test that incorporates

37 new validated planets in overlapping K2 campaigns

We analysed 68 candidate planetary systems first identified during Campaigns 5 and 6 (C5 and C6) of the NASA K2 mission. We set out to validate these systems by using a suite of follow-up

Searching for Extragalactic Exoplanetary Systems: The Curious Case of BD+20 2457

Planets and their host stars carry a long-term memory of their origin in their chemical compositions. Thus, identifying planets formed in different environments improves our understating of planetary

Characterization of 92 southern TESS candidate planet hosts and a new photometric [Fe/H] relation for cool dwarfs

We present the results of a medium resolution optical spectroscopic survey of 92 cool (3, 000 . Teff . 4, 500K) southern TESS candidate planet hosts, and describe our spectral fitting methodology

The TESS-Keck Survey. II. An Ultra-short-period Rocky Planet and Its Siblings Transiting the Galactic Thick-disk Star TOI-561

We report the discovery of TOI-561, a multiplanet system in the galactic thick disk that contains a rocky, ultra-short-period planet. This bright (V = 10.2) star hosts three small transiting planets

A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776

We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776, J = 8.5 mag, M = 0.54 ± 0.03 M ⊙) detected during Sector 10 observations of the

A Mini-Neptune and a Radius Valley Planet Orbiting the Nearby M2 Dwarf TOI-1266 in Its Venus Zone: Validation with the Habitable-zone Planet Finder

We report on the validation of two planets orbiting the nearby (36 pc) M2 dwarf TOI-1266 observed by the TESS mission. This system is one of a few M dwarf multiplanet systems with close-in planets

The GALAH+ survey: Third data release

The recent exponential increase in spectroscopic, astrometric & photometric data has highlighted the scientific opportunities afforded by obtaining an ensemble of chemical element abundances for

A giant planet candidate transiting a white dwarf.

These findings for the WD 1856+534 system indicate that giant planets can be scattered into tight orbits without being tidally disrupted, motivating the search for smaller transiting planets around white dwarfs.



Data-driven stellar parameters for southern TESS FGK targets

We present stellar parameter estimates for 939 457 southern FGK stars that are candidate targets for the Transiting Exoplanet Survey Satellite (TESS) mission. Using a data-driven method similar to

The GALAH survey: An abundance, age, and kinematic inventory of the solar neighbourhood made with TGAS

The overlap between the spectroscopic Galactic Archaeology with HERMES (GALAH) survey and Gaia provides a high-dimensional chemodynamical space of unprecedented size. We present a first analysis of a

Predicting the hypervelocity star population in Gaia

Hypervelocity stars (HVSs) are amongst the fastest objects in our Milky Way. These stars are predicted to come from the Galactic center (GC) and travel along unbound orbits across the Galaxy. In the

SkyMapper Southern Survey: First Data Release (DR1)

  • C. WolfC. Onken F. Yuan
  • Physics, Environmental Science
    Publications of the Astronomical Society of Australia
  • 2018
The end-user database is described, through which data are presented to the world community, and some illustrative science queries are provided, and the internal reproducibility of SkyMapper photometry is on the order of 1%, which is better than 0.2 arcsec based on comparison with Gaia first data release.

The New Galaxy: Signatures of Its Formation

▪ Abstract The formation and evolution of galaxies is one of the great outstanding problems of astrophysics. Within the broad context of hierachical structure formation, we have only a crude picture

Exploring the Milky Way stellar disk - A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood

Aims. The aim of this paper is to explore and map the age and abundance structure of the stars in the nearby Galactic disk. Methods. We have conducted a high-resolution spectroscopic study of 714 F

Characterizing TESS host stars

  • 2019

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)

Metallicity and Kinematics of the Galactic Halo from the LAMOST Sample Stars

We study the metallicity distribution and kinematic properties of 4680 A/F/G/K-type giant stars with 5 kpc selected from the LAMOST spectroscopic survey. The metallicity distribution of giant stars

Estimating Distances from Parallaxes

Astrometric surveys such as Gaia and LSST will measure parallaxes for hundreds of millions of stars. Yet they will not measure a single distance. Rather, a distance must be estimated from a parallax.