Jennifer Burt’s research while affiliated with Jet Propulsion Laboratory and other places

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Publications (141)


The NCORES Program: Precise planetary masses, null results, and insight into the planet mass distribution near the radius gap
  • Article

January 2025

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2 Reads

Monthly Notices of the Royal Astronomical Society

David J Armstrong

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Ares Osborn

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[...]

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Peter J Wheatley

NCORES was a large observing program on the ESO HARPS spectrograph, dedicated to measuring the masses of Neptune-like and smaller transiting planets discovered by the TESS satellite using the radial velocity technique. This paper presents an overview of the programme, its scientific goals and published results, covering 35 planets in 18 planetary systems. We present spectrally derived stellar characterisation and mass constraints for five additional TOIs where radial velocity observations found only marginally significant signals (TOI-510.01, M_p = 1.08^{+0.58}_{-0.55}M_{\hbox{\oplus }}), or found no signal (TOIs 271.01, 641.01, 697.01 and 745.01). A newly detected non-transiting radial velocity candidate is presented orbiting TOI-510 on a 10.0d orbit, with a minimum mass of 4.82^{+1.29}_{-1.26}M_{\hbox{\oplus }}, although uncertainties on the system architecture and true orbital period remain. Combining the NCORES sample with archival known planets we investigate the distribution of planet masses and compositions around and below the radius gap, finding that the population of planets below the gap is consistent with a rocky composition and ranges up to a sharp cut-off at 10M⊕. We compare the observed distribution to models of pebble- and planetesimal-driven formation and evolution, finding good broad agreement with both models while highlighting interesting areas of potential discrepancy. Increased numbers of precisely measured planet masses in this parameter space are required to distinguish between pebble and planetesimal accretion.


The NCORES Program: Precise planetary masses, null results, and insight into the planet mass distribution near the radius gap
  • Preprint
  • File available

January 2025

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6 Reads

NCORES was a large observing program on the ESO HARPS spectrograph, dedicated to measuring the masses of Neptune-like and smaller transiting planets discovered by the TESS satellite using the radial velocity technique. This paper presents an overview of the programme, its scientific goals and published results, covering 35 planets in 18 planetary systems. We present spectrally derived stellar characterisation and mass constraints for five additional TOIs where radial velocity observations found only marginally significant signals (TOI-510.01, Mp=1.080.55+0.58MM_p=1.08^{+0.58}_{-0.55}M_\oplus), or found no signal (TOIs 271.01, 641.01, 697.01 and 745.01). A newly detected non-transiting radial velocity candidate is presented orbiting TOI-510 on a 10.0d orbit, with a minimum mass of 4.821.26+1.29M4.82^{+1.29}_{-1.26}M_\oplus, although uncertainties on the system architecture and true orbital period remain. Combining the NCORES sample with archival known planets we investigate the distribution of planet masses and compositions around and below the radius gap, finding that the population of planets below the gap is consistent with a rocky composition and ranges up to a sharp cut-off at 10M10M_\oplus. We compare the observed distribution to models of pebble- and planetesimal-driven formation and evolution, finding good broad agreement with both models while highlighting interesting areas of potential discrepancy. Increased numbers of precisely measured planet masses in this parameter space are required to distinguish between pebble and planetesimal accretion.

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Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581*

December 2024

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35 Reads

The Astronomical Journal

We report the validation of multiple planets transiting the nearby ( d = 12.8 pc) K5V dwarf HD 101581 (GJ 435, TOI–6276, TIC 397362481). This system consists of at least two Earth-size planets whose orbits are near a mutual 4:3 mean-motion resonance, HD 101581 b ( R p = 0.956 − 0.061 + 0.063 R ⊕ , P = 4.47 days) and HD 101581c ( R p = 0.990 − 0.070 + 0.070 R ⊕ , P = 6.21 days). Both planets were discovered in Sectors 63 and 64 TESS observations and statistically validated with supporting ground-based follow-up. We also identify a signal that probably originates from a third transiting planet, TOI-6276.03 ( R p = 0.982 − 0.098 + 0.114 R ⊕ , P = 7.87 days). These planets are remarkably uniform in size and their orbits are evenly spaced, representing a prime example of the “peas-in-a-pod” architecture seen in other compact multiplanet systems. At V = 7.77, HD 101581 is the brightest star known to host multiple transiting planets smaller than 1.5 R ⊕ . HD 101581 is a promising system for atmospheric characterization and comparative planetology of small planets.


Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift

December 2024

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2 Reads

The Astronomical Journal

Ultraviolet flare emission can drive photochemistry in exoplanet atmospheres and even serve as the primary source of uncertainty in atmospheric retrievals. Additionally, flare energy budgets are not well understood due to a paucity of simultaneous observations. We present new near-UV (NUV) and optical observations of flares from three M dwarfs obtained at 20 s cadence with Swift and the Transiting Exoplanet Survey Satellite (TESS), along with a reanalysis of flares from two M dwarfs in order to explore the energy budget and timing of flares at NUV-optical wavelengths. We find a 9000 K blackbody underestimates the NUV flux by ≥2× for 54 ± 14% of flares and 14.8× for one flare. We report time lags between the bands of 0.5–6.6 minutes and develop a method to predict the qualitative flare shape and time lag to 36% ± 30% accuracy. The scatter present in optical-NUV relations is reduced by a factor of 2.0 ± 0.6 when comparing the total NUV energy with the TESS energy during the FWHM duration due to the exclusion of the T eff ≈ 5000 K tail. We show the NUV light curve can be used to remove flares from the optical light curve and consistently detect planets with 20% smaller transits than is possible without flare detrending. Finally, we demonstrate a 10× increase in the literature number of multiwavelength flares with the Early eVolution Explorer (EVE), an astrophysics Small Explorer concept to observe young clusters with simultaneous NUV and optical bands in order to detect young planets, assess their photochemical radiation environments, and observe accretion.


Figure 3. RV observations from PFS (green), UCLES (blue), and HARPS (orange). PUCHEROS+ RVs are not included due to the large uncertainties (∼50 m s −1 ). While the expected RV semi-amplitudes of the three planets are too small to be resolved (< 0.4 m s −1 ), the observations do not feature large RV variations corresponding to stellar-mass companions.
Figure 4. The field within 60 ′′ of HD 101581 in blue (far left), infrared (center left), and red (center right) filters from the SERC and AAO-SES Surveys, and from LCO/CTIO observations taken shortly after the end of the TESS observations in 2023 (right). The location of HD 101581 at the time of each image is marked with a blue cross, while the location at the start of TESS Sector 63 in 2023 March is marked in orange. The width of a TESS pixel (21 ′′ ) is marked in the top left of each panel. HD 101581 has moved ∼ 32 ′′ between 1977 and 2023. v sin i < 10 km s −1 , with measurements of lower v sin i limited by the resolution of the spectrograph. Perdelwitz et al. (2024) used the SPECIES codebase (Soto & Jenkins 2018) to extract parameters from the archival HARPS spectra for 3612 stars including HD 101581, finding T eff = 4709 ± 62 K, log g = 4.11 ± 0.13, [Fe/H] = −0.58 ± 0.05 dex, and v sin i = 2.47 ± 0.30 km s −1 . The T eff and log g values from the Hypatia, PUCHEROS+, and HARPS results all agree within 1σ, while the HARPS-based measurement of metallicity is slightly lower (1.6σ) than that from PUCHEROS+. Both analyses conclude that HD 101581 is a metal-poor star.
Figure 7. Plots of the transit model fits, with residuals after subtracting the median models provided in the lower panel of each phase diagram. Black points show observations with offsets subtracted and jitter terms added in quadrature with uncertainties, while colored circles represent binned data. Colored lines represent median model values. In each planet's phase diagram, the best-fit models for the other two planets have been subtracted from the data.
Figure 10. Estimated TSM and ESM values (Kempton et al. 2018) for known terrestrial planets (Rp < 1.5 R⊕) with TSM > 10, based on their properties given in the NASA Exoplanet Archive Planetary Systems Composite Data Table (NASA Exoplanet Archive 2024). Planets are colored by equilibrium temperature assuming zero albedo. Sub-Earths (Rp < 1 R⊕) are plotted with a black outline. The top-right box indicates the TSM/ESM parameter space in which the planets lie. The planets orbiting HD 101581 are among the best sub-Earths for characterization with both transmission and emission spectroscopy.
Figure 11. Instellation flux as a function of planet escape velocity, in log-log scale. Based on data from the NASA Exoplanet Archive (2024) downloaded on June 30, 2024. The empirical "cosmic shoreline" and the water vapor greenhouse runaway threshold (Zahnle & Catling 2017) are shown as cyan and yellow shaded regions, respectively. Planets are categorized into terrestrial planets (magenta), sub-Neptunes (blue), Neptune-like planets (green), and gas giants (yellow) based on radius, see legend. The red rectangles represent escape velocities calculated based on HD 101581 planets' mean estimated masses assuming Hypatia Catalog metallicity. Because only radius, but not mass, is known, we further plot light red regions covering all possible interior compositions, ranging from pure iron to pure silicates. Height of the rectangles represent uncertainties in insolation.

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Two Earth-size Planets and an Earth-size Candidate Transiting the Nearby Star HD 101581

December 2024

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33 Reads

We report the validation of multiple planets transiting the nearby (d=12.8d = 12.8 pc) K5V dwarf HD 101581 (GJ 435, TOI-6276, TIC 397362481). The system consists of at least two Earth-size planets whose orbits are near a mutual 4:3 mean-motion resonance, HD 101581 b (Rp=0.9560.061+0.063 RR_{p} = 0.956_{-0.061}^{+0.063}~R_{\oplus}, P=4.47P = 4.47 days) and HD 101581 c (Rp=0.9900.070+0.070 RR_{p} = 0.990_{-0.070}^{+0.070}~R_{\oplus}, P=6.21P = 6.21 days). Both planets were discovered in Sectors 63 and 64 TESS observations and statistically validated with supporting ground-based follow-up. We also identify a signal that probably originates from a third transiting planet, TOI-6276.03 (Rp=0.9820.098+0.114 RR_{p} = 0.982_{-0.098}^{+0.114}~R_{\oplus}, P=7.87P = 7.87 days). These planets are remarkably uniform in size and their orbits are evenly spaced, representing a prime example of the "peas-in-a-pod" architecture seen in other compact multi-planet systems. At V=7.77V = 7.77, HD 101581 is the brightest star known to host multiple transiting planets smaller than 1.5 R1.5~R_{\oplus}. HD 101581 is a promising system for atmospheric characterization and comparative planetology of small planets.


A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet

December 2024

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12 Reads

The Astronomical Journal

Characterizing outer companions to hot Jupiters plays a crucial role in deciphering their origins. We present the discovery of a long-period giant planet, HD 118203 c ( m c = 11.79 − 0.63 + 0.69 M J , a c = 6.28 − 0.11 + 0.10 au) exterior to a close-in eccentric hot Jupiter HD 118203 b ( P b = 6.135 days, m b = 2.14 ± 0.12 M J , r b = 1.14 ± 0.029 R J , e b = 0.31 ± 0.007) based on 20 yr radial velocities (RVs). Using Rossiter–McLaughlin (RM) observations from the Keck Planet Finder, we measured a low sky-projected spin–orbit angle λ b = − 11 ° 7 − 10.0 + 7.6 for HD 118203 b and detected stellar oscillations in the host star, confirming its evolved status. Combining the RM observation with the stellar inclination measurement, we constrained the true spin–orbit angle of HD 118203 b as Ψ b < 33.°5 (2 σ ), indicating the orbit normal of the hot Jupiter nearly aligned with the stellar spin axis. Furthermore, by combining RVs and Hipparcos-Gaia astrometric acceleration, we constrained the line-of-sight mutual inclination between the hot Jupiter and the outer planet to be 9 .° 8 − 9.3 + 16.2 at the 2 σ level. HD 118203 is one of first hot Jupiter systems where both the true spin–orbit angle of the hot Jupiter and the mutual inclination between inner and outer planets have been determined. Our results are consistent with a system-wide alignment, with low mutual inclinations between the outer giant planet, the inner hot Jupiter, and the host star. This alignment, along with the moderate eccentricity of HD 118203 c, implies that the system may have undergone coplanar high-eccentricity tidal migration. Under this framework, our dynamical analysis suggests an initial semimajor axis of 0.3–3.2 au for the proto–hot Jupiter.


Preparing for the Early eVolution Explorer: Characterizing the photochemical inputs and transit detection efficiencies of young planets using multiwavelength flare observations by TESS and Swift

November 2024

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3 Reads

Ultraviolet flare emission can drive photochemistry in exoplanet atmospheres and even serve as the primary source of uncertainty in atmospheric retrievals. Additionally, flare energy budgets are not well-understood due to a paucity of simultaneous observations. We present new near-UV (NUV) and optical observations of flares from three M dwarfs obtained at 20 s cadence with Swift and TESS, along with a re-analysis of flares from two M dwarfs in order to explore the energy budget and timing of flares at NUV--optical wavelengths. We find a 9000 K blackbody underestimates the NUV flux by \geq2×\times for 54±\pm14% of flares and 14.8×\times for one flare. We report time lags between the bands of 0.5--6.6 min and develop a method to predict the qualitative flare shape and time lag to 36±\pm30% accuracy. The scatter present in optical-NUV relations is reduced by a factor of 2.0±\pm0.6 when comparing the total NUV energy with the TESS energy during the FWHM duration due to the exclusion of the TeffT_\mathrm{eff}\approx5000 K tail. We show the NUV light curve can be used to remove flares from the optical light curve and consistently detect planets with 20% smaller transits than is possible without flare detrending. Finally, we demonstrate a 10×\times increase in the literature number of multi-wavelength flares with the Early eVolution Explorer (EVE), an astrophysics Small Explorer concept to observe young clusters with simultaneous NUV and optical bands in order to detect young planets, assess their photochemical radiation environments, and observe accretion.


Hic Sunt Dracones: Uncovering Dynamical Perturbers Within the Habitable Zone

October 2024

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1 Read

The continuing exploration of neighboring planetary systems is providing deeper insights into the relative prevalence of various system architectures, particularly with respect to the solar system. However, a full assessment of the dynamical feasibility of possible terrestrial planets within the Habitable Zones (HZ) of nearby stars requires detailed knowledge of the masses and orbital solutions of any known planets within these systems. Moreover, the presence of as yet undetected planets in or near the HZ will be crucial for providing a robust target list for future direct imaging surveys. In this work, we quantify the distribution of uncertainties on planetary masses and semi-major axes for 1062 confirmed planets, finding median uncertainties of 11.1% and 2.2%, respectively. We show the dependence of these uncertainties on stellar mass and orbital period, and discuss the effects of these uncertainties on dynamical analyses and the locations of mean motion resonance. We also calculate the expected radial velocity (RV) semi-amplitude for a Neptune-mass planet in the middle of the HZ for each of the proposed Habitable Worlds Observatory target stars. We find that for more than half of these stars, the RV semi-amplitude is less than 1.5 m/s, rendering them unlikely to be detected in archival RV data sets and highlighting the need for further observations to understand the dynamical viability of the HZ for these systems. We provide specific recommendations regarding stellar characterization and RV survey strategies that work toward the detection of presently unseen perturbers within the HZ.


Figure 4: Final TOI-700's RV and FWHM time-series model and data after correcting for inferred offsets. The plot shows (from top to bottom): RV data with full, stellar, and planetary models; RV data with the stellar signal subtracted; RV residuals; FWHM data with the stellar model; and FWHM residuals. Black symbols and error bars represent measurements, with transparent error bars accounting for jitter. Solid lines show the inferred full model, with shaded areas indicating 1-and 2-sigma intervals.
Precise Masses Reveal that TOI-700 c is Low Density and TOI-700 d is Rocky

September 2024

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31 Reads

The search for life in the Universe has a significant focus on M dwarf stars, as they are the most common stellar type, and their small sizes and low masses make it easier to detect and characterize small, temperate planets. However, M dwarfs, especially those with the lowest masses, emit frequent flares for long portions of their lifetimes that may erode planetary atmospheres. Demographic studies have shown that planets the size of Earth in the Habitable Zone — the region where liquid water could likely exist on planetary surfaces — are common. But only a handful of such worlds have been measured to be rocky, and all of them orbit active, lower-mass M-dwarfs, so the survival of their atmospheres is questionable. Here, we report new exoplanet mass measurements from radial velocity observations with the VLT/ESPRESSO spectrograph of TOI-700, a relatively quiet, early M dwarf star that hosts 4 small planets, including 2 in the star's Habitable Zone. We find that TOI-700 c (2.65 R_Earth) is a low-mass (2.5 M_Earth) planet, which must have a hydrogen/helium dominated atmosphere given its low bulk density (0.73 g/cc). Furthermore, the small (1.16 R_Earth), Habitable Zone planet, TOI-700 d, has a mass of 2.4 M_Earth, implying a rocky composition. Given that TOI-700 c and d have similar masses, the presence of TOI-700 c, a puffy sub-Neptune, orbiting interior to the Habitable Zone planets, implies that d might be able to maintain a heavier, secondary atmosphere as these planets were subjected to the same stellar history.


Figure 2. Sensitivity curve of I-band delta-magnitude vs. on-sky separation, with a 4″ square image cutout inlaid. Centered on the star, the inset image shows the speckle autocorrelation function (ACF) of TOI-3261 observed with the High-Resolution Camera on the SOAR 4.1 m telescope. It has a pixel scale of 0.01575″ per pixel.
Figure 3. Stellar spectral energy distribution with an ATLAS9 model (T eff = 5000 K, [Fe/H] = 0 dex, log(g) = 4 dex) overlaid. Individual points represent photometric data from the Gaia DR2 Crossmatch Catalog. Horizontal errors denote the bandpass widths.
Observation Log
ARES Fit Results for TOI-3261
Stellar and Planet Parameters for TOI-3261
Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b

August 2024

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43 Reads

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5 Citations

The Astronomical Journal

The recent discoveries of Neptune-sized ultra-short-period planets (USPs) challenge existing planet formation theories. It is unclear whether these residents of the Hot Neptune Desert have similar origins to smaller, rocky USPs, or if this discrete population is evidence of a different formation pathway altogether. We report the discovery of TOI-3261b, an ultrahot Neptune with an orbital period P = 0.88 day. The host star is a V = 13.2 mag, slightly supersolar metallicity ([Fe/H] ≃0.15), inactive K1.5 main-sequence star at d = 300 pc. Using data from the Transiting Exoplanet Survey Satellite and the Las Cumbres Observatory Global Telescope, we find that TOI-3261b has a radius of 3.82 − 0.35 + 0.42 R ⊕ . Moreover, radial velocities from ESPRESSO and HARPS reveal a mass of 30.3 − 2.4 + 2.2 M ⊕ , more than twice the median mass of Neptune-sized planets on longer orbits. We investigate multiple mechanisms of mass loss that can reproduce the current-day properties of TOI-3261b, simulating the evolution of the planet via tidal stripping and photoevaporation. Thermal evolution models suggest that TOI-3261b should retain an envelope potentially enriched with volatiles constituting ∼5% of its total mass. This is the second highest envelope mass fraction among ultrahot Neptunes discovered to date, making TOI-3261b an ideal candidate for atmospheric follow-up observations.


Citations (42)


... These planets challenge conventional theories of planet formation and evolution. Remarkably, some of these "ultrahot Neptunes" are relatively low-density (≲ 3 g cm −3 ), with voluminous envelopes of hydrogen and helium (e.g., LTT 9779 b and TOI-3261 b; Jenkins et al. 2020;Nabbie et al. 2024). These planets have somehow resisted total envelope loss despite their relatively low core masses (here, "core" refers to the bulk non-gaseous part of the planet). ...

Reference:

The Hottest Neptunes Orbit Metal-Rich Stars
Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b

The Astronomical Journal

... Inaccurate masses may also bias mass-radius relations for small planets (J. Burt et al. 2018) and propagate the issue to future Doppler observing proposals that make use of their results for exposure time estimation and/or target selection (J. A. Burt et al. 2024). ...

TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target

The Astrophysical Journal Letters

... The importance of ephemeris maintenance and refinement is epitomized by the automatic ephemeris fitting in ETD, which is based on quality-weighted sets of the uploaded transit observations. Amateur data have been taken into account in several publications presenting improved transit ephemeris; e.g. for planets found by CoRoT (Klagyivik et al. 2021), TESS (Peluso et al. 2023) or WASP (Noguer et al. 2024). Transit re-observations may also give rise to the detection of transit timing variations (TTVs) -these are deviations from strict periodicity that indicate non-linear ephemeris. ...

Enhancing Exoplanet Ephemerides by Leveraging Professional and Citizen Science Data: A Test Case with WASP-77 A b
  • Citing Article
  • July 2024

Publications of the Astronomical Society of the Pacific

... Lafarga et al. 2020). Unfortunately, the correlation between RV activity contamination and activity indicators is not always well governed by a simple relationship (i.e., time delays between the datasets; A. Burrows et al. 2024). Further, many analyses today utilize data from multiple instruments, and it is common that different instruments do not track the same activity indicators. ...

The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity*

The Astronomical Journal

... Accessed 2024 June 9) to reconstruct their sample. We found only one meaningful discrepancy: the putative super-Earth HD 26965 b was initially reported by B.Ma et al. (2018), but was recently found to be spurious (K.Laliotis et al. 2023). The removal of this planet would also exclude HD 26965 from the BL24 sample. ...

Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions*

The Astronomical Journal

... by providing more data to constrain the stellar activity signal, but resources for follow-up are precious, especially for targets that are key to pushing forward our understanding of exoplanets and their habitability. This provides a strong motivation for RV scheduling frameworks to incorporate stellar variability modeling (R. Cloutier et al. 2018;P. Newman et al. 2023). Such a framework would be particularly relevant to the case of TESS follow-up, where the host stars are sufficiently bright for RV observation. The orbital periods of TESS-discovered planets are also likely to be on similar timescales to the stellar rotation period, particularly those in the habitable zone (A. Vanderburg et al. 2016). ...

Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys

The Astronomical Journal

... The RV semi-amplitudes of an Earth mass planet orbiting at the Earth Equivalent Irradiation Distance around likely HWO target stars (Mamajek & Stapelfeldt 2024) ranges from 5 -50 cm s −1 , notably smaller than the current state of the art. Achieving the 10% mass uncertainty recommended in this study will therefore require that the uncertainties of the relative RV measurements be ≤ 10 cm s −1 over time scales of years to decades so that systematic errors do not dominate the planet signals (Luhn et al. 2023). ...

Impact of Correlated Noise on the Mass Precision of Earth-analog Planets in Radial Velocity Surveys

The Astronomical Journal

... A preliminary version of this retrieval code has been applied to solve for the possible interior compositions of recently discovered super-Earth TOI-1075 b (Z. Essack et al. 2023). ...

TOI-1075 b: A Dense, Massive, Ultra-short-period Hot Super-Earth Straddling the Radius Gap

The Astronomical Journal

... This means TOI-2490b experiences a 1000 K change in temperature from closest to furthest approach in its orbit. This can be compared to HD 80606b, a 4.16 +0.005 −0.005 J , 1.03 ± 0.02 J hot Jupiter with a 111.43 d period (Pearson et al. 2022). It has an orbital eccentricity of 0.93 and semi-major axis of 0.449 AU (Tsai et al. 2023). ...

Utilizing a Global Network of Telescopes to Update the Ephemeris for the Highly Eccentric Planet HD 80606 b and to Ensure the Efficient Scheduling of JWST

The Astronomical Journal

... While TESS has significantly increased the sample of well-characterized transiting warm Jupiters (e.g. Dawson et al. 2021;Grieves et al. 2022;Brahm et al. 2023;Battley et al. 2024), an important fraction of them might still be undiscovered because they are presented as single transiters in TESS data (e.g. Gill et al. 2020c). ...

Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b
  • Citing Article
  • March 2021

The Astronomical Journal