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Three super-Earths and a possible water world from TESS and ESPRESSO

Fuente: arXiv

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Main Authors:	Hobson, M. J., Bouchy, F., Lavie, B., Lovis, C., Adibekyan, V., Prieto, C. Allende, Alibert, Y., Barros, S. C. C., Castro-González, A., Cristiani, S., D'Odorico, V., Damasso, M., Di Marcantonio, P., Dumusque, X., Ehrenreich, D., Figueira, P., Santos, R. Génova, Hernández, J. I. González, Lillo-Box, J., Curto, G. Lo, Martins, C. J. A. P., Mehner, A., Micela, G., Molaro, P., Nunes, N. J., Palle, E., Pepe, F., Rebolo, R., Rodrigues, J., Santos, N., Sousa, S. G., Sozzetti, A., Mascareño, A. Suárez, Tabernero, H. M., Udry, S., Osorio, M. -R. Zapatero, Armstrong, D. J., Ciardi, D. R., Collins, K. A., Collins, K. I., Everett, M., Gandolfi, D., Howell, S. B., Jenkins, J. M., Kielkopf, J., Livingston, J. H., Lund, M. B., Mireles, I., Ricker, G. R., Schwarz, R. P., Seager, S., Tan, T. -G., Ting, E. B., Winn, J. N.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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_version_	1866914925382729728
author	Hobson, M. J. Bouchy, F. Lavie, B. Lovis, C. Adibekyan, V. Prieto, C. Allende Alibert, Y. Barros, S. C. C. Castro-González, A. Cristiani, S. D'Odorico, V. Damasso, M. Di Marcantonio, P. Dumusque, X. Ehrenreich, D. Figueira, P. Santos, R. Génova Hernández, J. I. González Lillo-Box, J. Curto, G. Lo Martins, C. J. A. P. Mehner, A. Micela, G. Molaro, P. Nunes, N. J. Palle, E. Pepe, F. Rebolo, R. Rodrigues, J. Santos, N. Sousa, S. G. Sozzetti, A. Mascareño, A. Suárez Tabernero, H. M. Udry, S. Osorio, M. -R. Zapatero Armstrong, D. J. Ciardi, D. R. Collins, K. A. Collins, K. I. Everett, M. Gandolfi, D. Howell, S. B. Jenkins, J. M. Kielkopf, J. Livingston, J. H. Lund, M. B. Mireles, I. Ricker, G. R. Schwarz, R. P. Seager, S. Tan, T. -G. Ting, E. B. Winn, J. N.
author_facet	Hobson, M. J. Bouchy, F. Lavie, B. Lovis, C. Adibekyan, V. Prieto, C. Allende Alibert, Y. Barros, S. C. C. Castro-González, A. Cristiani, S. D'Odorico, V. Damasso, M. Di Marcantonio, P. Dumusque, X. Ehrenreich, D. Figueira, P. Santos, R. Génova Hernández, J. I. González Lillo-Box, J. Curto, G. Lo Martins, C. J. A. P. Mehner, A. Micela, G. Molaro, P. Nunes, N. J. Palle, E. Pepe, F. Rebolo, R. Rodrigues, J. Santos, N. Sousa, S. G. Sozzetti, A. Mascareño, A. Suárez Tabernero, H. M. Udry, S. Osorio, M. -R. Zapatero Armstrong, D. J. Ciardi, D. R. Collins, K. A. Collins, K. I. Everett, M. Gandolfi, D. Howell, S. B. Jenkins, J. M. Kielkopf, J. Livingston, J. H. Lund, M. B. Mireles, I. Ricker, G. R. Schwarz, R. P. Seager, S. Tan, T. -G. Ting, E. B. Winn, J. N.
contents	Since 2018, the ESPRESSO spectrograph at the VLT has been hunting for planets in the Southern skies via the RV method. One of its goals is to follow up candidate planets from transit surveys such as the TESS mission, particularly small planets. We analyzed photometry from TESS and ground-based facilities, high-resolution imaging, and RVs from ESPRESSO, HARPS, and HIRES, to confirm and characterize three new planets: TOI-260 b, transiting a late K-dwarf, and TOI-286 b and c, orbiting an early K-dwarf. We also update parameters for the known super-Earth TOI-134 b , hosted by an M-dwarf. TOI-260 b has a $13.475853^{+0.000013}_{-0.000011}$ d period, $4.23 \pm1.60 \mathrm{M_\oplus}$ mass and $1.71\pm0.08\mathrm{R_\oplus}$ radius. For TOI-286 b we find a $4.5117244^{+0.0000031}_{-0.0000027}$ d period, $4.53\pm0.78\mathrm{M_\oplus}$ mass and $1.42\pm0.10\mathrm{R_\oplus}$ radius; for TOI-286 c, a $39.361826^{+0.000070}_{-0.000081}$ d period, $3.72\pm2.22\mathrm{M_\oplus}$ mass and $1.88\pm 0.12\mathrm{R_\oplus}$ radius. For TOI-134 b we obtain a $1.40152604^{+0.00000074}_{-0.00000082}$ d period, $4.07\pm0.45\mathrm{M_\oplus}$ mass, and $1.63\pm0.14\mathrm{R_\oplus}$ radius. Circular models are preferred for all, although for TOI-260 b the eccentricity is not well-constrained. We compute bulk densities and place the planets in the context of composition models. TOI-260 b lies within the radius valley, and is most likely a rocky planet. However, the uncertainty on the eccentricity and thus on the mass renders its composition hard to determine. TOI-286 b and c span the radius valley, with TOI-286 b lying below it and having a likely rocky composition, while TOI-286 c is within the valley, close to the upper border, and probably has a significant water fraction. With our updated parameters for TOI-134 b, we obtain a lower density than previous findings, giving a rocky or Earth-like composition.
format	Preprint
id	arxiv_https___arxiv_org_abs_2406_06278
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Three super-Earths and a possible water world from TESS and ESPRESSO Hobson, M. J. Bouchy, F. Lavie, B. Lovis, C. Adibekyan, V. Prieto, C. Allende Alibert, Y. Barros, S. C. C. Castro-González, A. Cristiani, S. D'Odorico, V. Damasso, M. Di Marcantonio, P. Dumusque, X. Ehrenreich, D. Figueira, P. Santos, R. Génova Hernández, J. I. González Lillo-Box, J. Curto, G. Lo Martins, C. J. A. P. Mehner, A. Micela, G. Molaro, P. Nunes, N. J. Palle, E. Pepe, F. Rebolo, R. Rodrigues, J. Santos, N. Sousa, S. G. Sozzetti, A. Mascareño, A. Suárez Tabernero, H. M. Udry, S. Osorio, M. -R. Zapatero Armstrong, D. J. Ciardi, D. R. Collins, K. A. Collins, K. I. Everett, M. Gandolfi, D. Howell, S. B. Jenkins, J. M. Kielkopf, J. Livingston, J. H. Lund, M. B. Mireles, I. Ricker, G. R. Schwarz, R. P. Seager, S. Tan, T. -G. Ting, E. B. Winn, J. N. Earth and Planetary Astrophysics Since 2018, the ESPRESSO spectrograph at the VLT has been hunting for planets in the Southern skies via the RV method. One of its goals is to follow up candidate planets from transit surveys such as the TESS mission, particularly small planets. We analyzed photometry from TESS and ground-based facilities, high-resolution imaging, and RVs from ESPRESSO, HARPS, and HIRES, to confirm and characterize three new planets: TOI-260 b, transiting a late K-dwarf, and TOI-286 b and c, orbiting an early K-dwarf. We also update parameters for the known super-Earth TOI-134 b , hosted by an M-dwarf. TOI-260 b has a $13.475853^{+0.000013}_{-0.000011}$ d period, $4.23 \pm1.60 \mathrm{M_\oplus}$ mass and $1.71\pm0.08\mathrm{R_\oplus}$ radius. For TOI-286 b we find a $4.5117244^{+0.0000031}_{-0.0000027}$ d period, $4.53\pm0.78\mathrm{M_\oplus}$ mass and $1.42\pm0.10\mathrm{R_\oplus}$ radius; for TOI-286 c, a $39.361826^{+0.000070}_{-0.000081}$ d period, $3.72\pm2.22\mathrm{M_\oplus}$ mass and $1.88\pm 0.12\mathrm{R_\oplus}$ radius. For TOI-134 b we obtain a $1.40152604^{+0.00000074}_{-0.00000082}$ d period, $4.07\pm0.45\mathrm{M_\oplus}$ mass, and $1.63\pm0.14\mathrm{R_\oplus}$ radius. Circular models are preferred for all, although for TOI-260 b the eccentricity is not well-constrained. We compute bulk densities and place the planets in the context of composition models. TOI-260 b lies within the radius valley, and is most likely a rocky planet. However, the uncertainty on the eccentricity and thus on the mass renders its composition hard to determine. TOI-286 b and c span the radius valley, with TOI-286 b lying below it and having a likely rocky composition, while TOI-286 c is within the valley, close to the upper border, and probably has a significant water fraction. With our updated parameters for TOI-134 b, we obtain a lower density than previous findings, giving a rocky or Earth-like composition.
title	Three super-Earths and a possible water world from TESS and ESPRESSO
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2406.06278