14 research outputs found

    TOI-836 : a super-Earth and mini-Neptune transiting a nearby K-dwarf

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    Funding: TGW, ACC, and KH acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1.We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T = 8.5 mag), high proper motion (∌200 mas yr−1), low metallicity ([Fe/H]≈−0.28) K-dwarf with a mass of 0.68 ± 0.05 M⊙ and a radius of 0.67 ± 0.01 R⊙. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a 1.70 ± 0.07 R⊕ super-Earth in a 3.82 day orbit, placing it directly within the so-called ‘radius valley’. The outer planet, TOI-836 c, is a 2.59 ± 0.09 R⊕ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of 4.5 ± 0.9 M⊕, while TOI-836 c has a mass of 9.6 ± 2.6 M⊕. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet.Publisher PDFPeer reviewe

    TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

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    We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T=8.5T = 8.5 mag), high proper motion (∌ 200\sim\,200 mas yr−1^{-1}), low metallicity ([Fe/H]≈ −0.28\approx\,-0.28) K-dwarf with a mass of 0.68±0.050.68\pm0.05 M⊙_{\odot} and a radius of 0.67±0.010.67\pm0.01 R⊙_{\odot}. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a 1.70±0.071.70\pm0.07 R⊕_{\oplus} super-Earth in a 3.82 day orbit, placing it directly within the so-called 'radius valley'. The outer planet, TOI-836 c, is a 2.59±0.092.59\pm0.09 R⊕_{\oplus} mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of 4.5±0.94.5\pm0.9 M⊕_{\oplus} , while TOI-836 c has a mass of 9.6±2.69.6\pm2.6 M⊕_{\oplus}. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet

    Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

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    peer reviewedHIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes

    TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

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    A close-in puffy Neptune with hidden friends : the enigma of TOI 620

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    We present the validation of a transiting low-density exoplanet orbiting the M2.5 dwarf TOI 620 discovered by the NASA Transiting Exoplanet Survey Satellite (TESS) mission. We utilize photometric data from both TESS and ground-based follow-up observations to validate the ephemerides of the 5.09 day transiting signal and vet false-positive scenarios. High-contrast imaging data are used to resolve the stellar host and exclude stellar companions at separations ≳0farcs2. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with multiple precision radial velocity (PRV) spectrographs to confirm the planetary nature of the transiting exoplanet. We calculate a 5σ upper limit of MP < 7.1 M⊕ and ρP < 0.74 g cm−3, and we identify a nontransiting 17.7 day candidate. We also find evidence for a substellar (1–20 MJ) companion with a projected separation â‰Č20 au from a combined analysis of Gaia, adaptive optics imaging, and RVs. With the discovery of this outer companion, we carry out a detailed exploration of the possibilities that TOI 620 b might instead be a circum-secondary planet or a pair of eclipsing binary stars orbiting the host in a hierarchical triple system. We find, under scrutiny, that we can exclude both of these scenarios from the multiwavelength transit photometry, thus validating TOI 620 b as a low-density exoplanet transiting the central star in this system. The low density of TOI 620 b makes it one of the most amenable exoplanets for atmospheric characterization, such as with the James Webb Space Telescope and Ariel, validated or confirmed by the TESS mission to date

    TOI-836:A super-Earth and mini-Neptune transiting a nearby K-dwarf

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    We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T=8.5mag), high proper motion (∌200 mas yr−1), low metallicity ([Fe/H]≈−0.28) K-dwarf with a mass of 0.68±0.05 M⊙ and aradius of 0.67±0.01 R⊙. We obtain photometric follow-upobservations with a variety of facilities, and we use these data-sets todetermine that the inner planet, TOI-836 b, is a 1.70±0.07 R⊕super-Earth in a 3.82 day orbit, placing it directly within the so-called'radius valley'. The outer planet, TOI-836 c, is a 2.59±0.09 R⊕mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal thatTOI-836 b has a mass of 4.5±0.9 M⊕ , while TOI-836 c has a massof 9.6±2.6 M⊕. Photometric observations show Transit TimingVariations (TTVs) on the order of 20 minutes for TOI-836 c, although there areno detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused byan undetected exterior planet
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