Mass and density of the transiting hot and rocky super-Earth LHS 1478 b (TOI-1640 b)

Soto, M. G.; Anglada‐Escudé, G.; Molaverdikhani, Karan; Kemmer, J.; Rodríguez‐López, C.; Lillo-Box, J.; Πάλλη, Ε.; Espinoza, N.; Caballero, J. A.; Quirrenbach, A.; Ribas, I.; Reiners, A.; Narita, Norio; Hirano, Teruyuki; Amado, P. J.; Béjar, V. J. S.; Bluhm, P.; Burke, Christopher J.; Caldwell, Douglas A.; Charbonneau, David; Cloutier, Ryan; Collins, Karen A.; Cortés-Contreras, M.; Girardin, Éric; Guerra, P.; Harakawa, Hiroki; Hatzes, A. P.; Irwin, Jonathan; Jenkins, Jon M.; Jensen, Eric L. N.; Kawauchi, Kiyoe; Kotani, Takayuki; Kudo, Tomoyuki; Kunimoto, Michelle; Kuzuhara, Masayuki; Latham, David W.; Montes, D.; Morales, J. C.; Mori, M.; Nelson, Richard P.; Omiya, Masashi; Pedraz, S.; Passegger, V. M.; Rackham, Benjamin V.; Rudat, Alexander; Schlieder, Joshua E.; Schöfer, P.; Schweitzer, A.; Selezneva, A.; Stockdale, Chris; Tamura, Motohide; Trifonov, T.; Vanderspek, R.; Watanabe, David

doi:10.1051/0004-6361/202140618

Cited by 24 publications

(2 citation statements)

References 74 publications

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“…The value agrees with the mass derived using all three spectrographs and is closer to the new best-fit mass than the initial published values using only HIRES or HARPS-N. The combination of HARPS-N, HIRES, and MAROON-X data allowed us to measure the mass of TOI-561 b with a fractional uncertainty of 9.6%, placing it among the most precisely known RV masses for planets with R p < 1.5 R ⊕ (see Dai et al 2019;Soto et al 2021;Trifonov et al 2021, for other examples).…”

Section: Keplerian Orbital Fitsupporting

confidence: 81%

TOI-561 b: A Low-density Ultra-short-period “Rocky” Planet around a Metal-poor Star

Brinkman

Weiss

Dai³

et al. 2023

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TOI-561 is a galactic thick-disk star hosting an ultra-short-period (0.45-day-orbit) planet with a radius of 1.37 R ⊕, making it one of the most metal-poor ([Fe/H] = −0.41) and oldest (≈10 Gyr) sites where an Earth-sized planet has been found. We present new simultaneous radial velocity (RV) measurements from Gemini-N/MAROON-X and Keck/HIRES, which we combined with literature RVs to derive a mass of M b = 2.24 ± 0.20 M ⊕. We also used two new sectors of TESS photometry to improve the radius determination, finding R b = 1.37 ± 0.04 R ⊕ and confirming that TOI-561 b is one of the lowest-density super-Earths measured to date (ρ b = 4.8 ± 0.5 g cm−3). This density is consistent with an iron-poor rocky composition reflective of the host star’s iron and rock-building element abundances; however, it is also consistent with a low-density planet with a volatile envelope. The equilibrium temperature of the planet (∼2300 K) suggests that this envelope would likely be composed of high mean molecular weight species, such as water vapor, carbon dioxide, or silicate vapor, and is likely not primordial. We also demonstrate that the composition determination is sensitive to the choice of stellar parameters and that further measurements are needed to determine whether TOI-561 b is a bare rocky planet, a rocky planet with an optically thin atmosphere, or a rare example of a nonprimordial envelope on a planet with a radius smaller than 1.5 R ⊕.

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Section: Keplerian Orbital Fitsupporting

confidence: 81%

TOI-561 b: A Low-density Ultra-short-period “Rocky” Planet around a Metal-poor Star

Brinkman

Weiss

Dai³

et al. 2023

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“…The TESS Primary Mission has already yielded the detections of several such systems (e.g., Vanderspek et al 2019;Gan et al 2020;Wells et al 2021;Fukui et al 2021). Some of those planets also have precise mass constraints through spectroscopic measurements thanks to the brightness of their host stars (e.g., Luque et al 2019;Shporer et al 2020;Cloutier et al 2020;Soto et al 2021). However, it is challenging to achieve a high enough signal-to-noise ratio (SNR) and obtain precise radial velocities for mid-to-late M dwarfs as they are, in general, faint at optical wavelengths.…”

Section: Introductionmentioning

confidence: 99%

TESS discovery of a sub-Neptune orbiting a mid-M dwarf TOI-2136

Gan¹,

Soubkiou²,

Wang³

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present the discovery of TOI-2136 b, a sub-Neptune planet transiting a nearby M4.5V-type star every 7.85 days, identified through photometric measurements from the TESS mission. The host star is located 33 pc away with a radius of R* = 0.34 ± 0.02 R⊙, a mass of 0.34 ± 0.02 M⊙ and an effective temperature of 3342 ± 100 K. We estimate its stellar rotation period to be 75 ± 5 days based on archival long-term photometry. We confirm and characterize the planet based on a series of ground-based multi-wavelength photometry, high-angular-resolution imaging observations, and precise radial velocities from CFHT/SPIRou. Our joint analysis reveals that the planet has a radius of 2.20 ± 0.17 R⊕ and a mass of 6.4 ± 2.4 M⊕. The mass and radius of TOI-2136 b is consistent with a broad range of compositions, from water-ice to gas-dominated worlds. TOI-2136 b falls close to the radius valley for M dwarfs predicted by thermally driven atmospheric mass loss models, making it an interesting target for future studies of its interior structure and atmospheric properties.

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Follow-up of non-transiting planets detected by Kepler

Lillo-Box

Millholland

Laughlin

2021

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Context. The direct detection of new extrasolar planets from high-precision photometry data is commonly based on the observation of the transit signal of the planet as it passes in front of its star. Close-in planets, however, leave additional imprints in the light curve even if they do not transit. These are the so-called phase curve variations that include ellipsoidal, reflection and beaming effects. Aims. In a previous paper, we scrutinized the Kepler database looking for these phase variations from non-transiting planets. They found 60 candidates whose signals were compatible with planetary companions. In this paper, we perform a ground-based follow-up of a subsample of these systems with the aim of confirming and characterizing these planets and thus validating the detection technique. Methods. We used the CAFE and HERMES instruments to monitor the radial velocity (RV) of ten non-transiting planet candidates along their orbits. We additionally used AstraLux to obtain high-resolution images of some of these candidates to discard blended binaries that contaminate the Kepler light curves by mimicking planetary signals. Results. Among the ten systems, we confirm three new hot-Jupiters (KIC 8121913 b, KIC 10068024 b, and KIC 5479689 b) with masses in the range 0.5–2 MJup and set mass constraints within the planetary regime for the other three candidates (KIC 8026887 b, KIC 5878307 b, and KIC 11362225 b), thus strongly suggestive of their planetary nature. Conclusions. For the first time, we validate the technique of detecting non-transiting planets via their phase curve variations. We present the new planetary systems and their properties. We find good agreement between the RV-derived masses and the photometric masses in all cases except KIC 8121913 b, which shows a significantly lower mass derived from the ellipsoidal modulations than from beaming and RV data.

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Mass and density of the transiting hot and rocky super-Earth LHS 1478 b (TOI-1640 b)

Cited by 24 publications

References 74 publications

TOI-561 b: A Low-density Ultra-short-period “Rocky” Planet around a Metal-poor Star

TOI-561 b: A Low-density Ultra-short-period “Rocky” Planet around a Metal-poor Star

TESS discovery of a sub-Neptune orbiting a mid-M dwarf TOI-2136

Follow-up of non-transiting planets detected by Kepler

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