TOI-530b: a giant planet transiting an M-dwarf detected by <i>TESS</i>

Gan, Tianjun; Lin, Zitao; Wang, Sharon Xuesong; Mao, Shude; Fouqué, P.; Stassun, Keivan G.; Giacalone, Steven; Fukui, A.; Murgas, F.; Ciardi, David R.; Howell, Steve B.; Collins, Karen A.; Shporer, Avi; Arnold, L.; Barclay, Thomas; Charbonneau, David; Christiansen, Jessie L.; Crossfield, Ian J. M.; Dressing, Courtney D.; Elliott, Ashley; Esparza-Borges, E.; Evans, P.; Gnilka, Crystal L.; Gonzales, Erica J.; Howard, Andrew W.; Isogai, Keisuke; Kawauchi, Kiyoe; Kurita, S.; Liu, Beibei; Livingston, John H.; Matson, Rachel A.; Narita, Norio; Πάλλη, Ε.; Parviainen, H.; Rackham, Benjamin V.; Rodríguez, David; Rose, Mark; Rudat, Alexander; Schlieder, Joshua E.; Scott, Nicholas J.; Vezie, Michael; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.

doi:10.1093/mnras/stab3708

Cited by 26 publications

(23 citation statements)

References 146 publications

(91 reference statements)

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“…There is a small but growing number of these planets (∼ 11, Fig. 1; hereafter the GGM-D sample) confirmed by NASA's TESS mission (Ricker et al 2015): TOI-1728 b (Kanodia et al 2020), TOI-1899 b (Cañas et al 2020), TOI-442 b (Dreizler et al 2020), TOI-674 b (Murgas et al 2021), TOI-532 b (Kanodia et al 2021), TOI-737 b, TOI-552 b (Jordán et al 2022), TOI-3629 b, TOI-3714 b (Cañas et al 2022), TOI-3757 b (Kanodia et al 2022), and TOI-530 b (Gan et al 2022); all with close-in orbits, thus making them perfect bodies to study tidal evolution around M-dwarf hosts.…”

Section: Introductionmentioning

confidence: 77%

Tidally induced migration of TESS gas giants orbiting M dwarfs

Alvarado-Montes

2022

Monthly Notices of the Royal Astronomical Society

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According to core-accretion formation models, the conditions under which gas giants will form around M dwarfs are very restrictive. Also, the correlation of the occurrence of these planets with the metallicity of host stars is still unknown due to the intrinsic faintness of M dwarfs in the optical and some intricacies in their spectra. Interestingly, NASA’s TESS mission has started to create a growing sample of these systems, with ten observed planets located in close-in orbits: contrary to what is expected for low stellar masses. Tidal interactions with the host star will play a key role in determining the fate of these planets, so by using the measured physical and orbital characteristics of these M-dwarf systems we numerically analyse the exchange of rotational and orbital angular momentum, while constraining the energy dissipation in each system to calculate whether host stars are spun up or spun down, depending on the relationship between the gain and loss of angular momentum by the stellar rotation. We also study the coupled orbital and physical evolution of their gas giant companion and calculate orbital circularization time-scales, as well as the time needed to undergo orbital decay from their current orbital position to the Roche limit. The thorough study of tidal processes occurring over short and long time-scales in star-planet systems like those studied here, can help constrain tidal dissipation rates inside the star and planet, complement tidal theories, and improve estimations of unconstrained properties of exoplanetary systems.

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Section: Introductionmentioning

confidence: 77%

Tidally induced migration of TESS gas giants orbiting M dwarfs

Alvarado-Montes

2022

Monthly Notices of the Royal Astronomical Society

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“…In this section, we outline our data analysis steps including modeling the space and ground light curves as well as the SPIRou radial velocities, which mainly follows Gan et al (2022). In short, we begin with fitting the TESS-only photometry and then take the posterior information as a prior to detrend the ground-based light curves (see Section 4.1).…”

Section: Analysis and Resultsmentioning

confidence: 99%

“…To determine the stellar type, we further compare our SpeX spectrum with the IRTF library (Rayner et al 2009) and find that TOI-2136 is consistent with a star of spectral type M4.5V (Figure 4). Lastly, following the procedure described in Gan et al (2022), we obtain the metallicity of TOI-2136 based on the relations defined in Mann et al (2013) for cool dwarfs with spectral types between K5 and M5. Our analysis yield metallicities of [Fe/H] = 0.03 ± 0.07 and [M/H] = −0.01 ± 0.08.…”

Section: Toi-2136 Bmentioning

confidence: 99%

“…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. The new-generation near-infrared spectrograph Spec-troPolarimètre InfraROUge spectrograph (SPIRou) on the Canada-France-Hawaii-Telescope (CFHT) opens a window to characterize planets around faint stars via high-precision velocimetry and spectropolarimetry (Donati et al 2020;Klein et al 2021;Gan et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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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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“…Although wobble suffers from "convolution" errors as it assumes simple multiplication of spectra, it should, in principle, perform as well as the division method presented in this work, which can reach or is close to the photon-limited precision in the majority of the common photometric bands. wobble has been very successful in the optical band, and it is yet to be seen whether it could tackle the more challenging NIR region (e.g., Gan et al 2022).…”

Section: Discussionmentioning

confidence: 99%

Characterizing and Mitigating the Impact of Telluric Absorption in Precise Radial Velocities

Wang

Latouf

Plavchan

et al. 2022

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Precise radial velocity (PRV) surveys are important for the search for Earth analogs around nearby bright stars, which induce a small stellar reflex motion with an RV amplitude of ∼10 cm s−1. Detecting such a small RV signal poses challenges to instrumentation, data analysis, and the precision of astrophysical models to mitigate stellar jitter. In this work, we investigate an important component in the PRV error budget—the spectral contamination from the Earth’s atmosphere (tellurics). We characterize the effects of telluric absorption on the RV precision and quantify its contribution to the RV error budget over time and across a wavelength range of 350 nm–2.5 μm. We use simulated solar spectra with telluric contamination injected, and we extract the RVs using two commonly adopted algorithms: dividing out a telluric model before performing cross-correlation or forward modeling the observed spectrum incorporating a telluric model. We assume various degrees of cleanness in removing the tellurics. We conclude that the RV errors caused by telluric absorption can be suppressed to close to or even below 1–10 cm s−1 in the blue optical region. At red through near-infrared wavelengths, however, the residuals of tellurics can induce an RV error on the meter-per-second level even under the most favorable assumptions for telluric removal, leading to significant systematic noise in the RV time series and periodograms. If the red-optical or near-infrared becomes critical in the mitigation of stellar activity, systematic errors from tellurics can be eliminated with a space mission such as EarthFinder.

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TOI-530b: a giant planet transiting an M-dwarf detected by TESS

Cited by 26 publications

References 146 publications

Tidally induced migration of TESS gas giants orbiting M dwarfs

Tidally induced migration of TESS gas giants orbiting M dwarfs

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

Characterizing and Mitigating the Impact of Telluric Absorption in Precise Radial Velocities

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