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1. Validation of up to seven TESS planet candidates through multi-colour transit photometry using MuSCAT2 data

Author

Peláez-Torres, A., Esparza-Borges, E., Pallé, E., Parviainen, H., Murgas, F., Morello, G., Zapatero-Osorio, M. R., Korth, J., Narita, N., Fukui, A., Carleo, I., Luque, R., García, N. Abreu, Barkaoui, K., Boyle, A., Béjar, V. J. S., Calatayud-Borras, Y., Cheryasov, D. V., Christiansen, J. L., Ciardi, D. R., Enoc, G., Essack, Z., Fukuda, I., Furesz, G., Galán, D., Geraldía-González, S., Giacalone, S., Gill, H., Gonzales, E. J., Hayashi, Y., Ikuta, K., Isogai, K., Kagetani, T., Kawai, Y., Kawauchi, K., Klagyvik, P., Kodama, T., Kusakabe, N., Laza-Ramos, A., de Leon, J. P., Livingston, J. H., Lund, M. B., Madrigal-Aguado, A., Meni, P., Mori, M., Torres, S. Muñoz, Orell-Miquel, J., Puig, M., Ricker, G., Sánchez-Benavente, M., Savel, A. B., Schlieder, J. E., Schwarz, R. P., Sefako, R., Sosa-Guillén, P., Stangret, M., Stockdale, C., Tamura, M., Terada, Y., Twicken, J. D., Watanabe, N., Winn, J., Zheltoukhov, S. G., Ziegler, C., and Zou, Y.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TESS mission searches for transiting exoplanets by monitoring the brightness of hundreds of thousands of stars across the entire sky. M-type planet hosts are ideal targets for this mission due to their smaller size and cooler temperatures, which makes it easier to detect smaller planets near or within their habitable zones. Additionally, M~dwarfs have a smaller contrast ratio between the planet and the star, making it easier to measure the planet's properties accurately. Here, we report the validation analysis of 13 TESS exoplanet candidates orbiting around M dwarfs. We studied the nature of these candidates through a multi-colour transit photometry transit analysis using several ground-based instruments (MuSCAT2, MuSCAT3, and LCO-SINISTRO), high-spatial resolution observations, and TESS light curves. We present the validation of five new planetary systems: TOI-1883b, TOI-2274b, TOI2768b, TOI-4438b, and TOI-5319b, along with compelling evidence of a planetary nature for TOIs 2781b and 5486b. We also present an empirical definition for the Neptune desert boundaries. The remaining six systems could not be validated due to large true radius values overlapping with the brown dwarf regime or, alternatively, the presence of chromaticity in the MuSCAT2 light curves.

Published
2024

2. The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M dwarfs

Author

Hori, Y., Fukui, A., Hirano, T., Narita, N., de Leon, J. P., Ishikawa, H. T., Hartman, J. D., Morello, G., García, N. Abreu, Hernández, L. Álvarez, Béjar, V. J. S., Calatayud-Borras, Y., Carleo, I., Enoc, G., Esparza-Borges, E., Fukuda, I., Galán, D., Geraldía-González, S., Hayashi, Y., Ikoma, M., Ikuta, K., Isogai, K., Kagetani, T., Kawai, Y., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kusakabe, N., Laza-Ramos, A., Livingston, J. H., Luque, R., Miyakawa, K., Mori, M., Torres, S. Muñoz, Murgas, F., Orell-Miquel, J., Palle, E., Parviainen, H., Peláez-Torres, A., Puig-Subirá, M., Sánchez-Benavente, M., Sosa-Guillén, P., Stangret, M., Terada, Y., Watanabe, N., Bakos, G. Á., Barkaoui, K., Beichman, C., Benkhaldoun, Z., Boyle, A. W., Ciardi, D. R., Clark, C. A., Collins, K. A., Collins, K. I., Conti, D. M., Crossfield, I. J. M., Everett, M. E., Furlan, E., Ghachoui, M., Gillon, M., Gonzales, E. J., Higuera, J., Horne, K., Howell, S. B., Jehin, E., Lester, K. V., Lund, M. B., Matson, R., Matthews, E. C., Pozuelos, F. J., Safonov, B. S., Schlieder, J. E., Schwarz, R. P., Sefako, R., Srdoc, G., Strakhov, I. A., Waalkes, W. C., Ziegler, C., Charbonneau, D., Essack, Z., Timmermans, M., Guerrero, N. M., Harakawa, H., Hedges, C., Ishizuka, M., Jenkins, J. M., Konishi, M., Kotani, T., Kudo, T., Kurokawa, T., Kuzuhara, M., Nishikawa, J., Omiya, M., Ricker, G. R., Seager, S., Serizawa, T., Striegel, S., Tamura, M., Ueda, A., Vanderspek, R., Vievard, S., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Sub-Neptunes with $2-3R_\oplus$ are intermediate in size between rocky planets and Neptune-sized planets. The orbital properties and bulk compositions of transiting sub-Neptunes provide clues to the formation and evolution of close-in small planets. In this paper, we present the discovery and follow-up of four sub-Neptunes orbiting M dwarfs (TOI-782, TOI-1448, TOI-2120, and TOI-2406), three of which were newly validated by ground-based follow-up observations and statistical analyses. TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b have radii of $R_\mathrm{p} = 2.740^{+0.082}_{-0.079}\,R_\oplus$, $2.769^{+0.073}_{-0.068}\,R_\oplus$, $2.120\pm0.067\,R_\oplus$, and $2.830^{+0.068}_{-0.066}\,R_\oplus$ and orbital periods of $P = 8.02$, $8.11$, $5.80$, and $3.08$\,days, respectively. Doppler monitoring with Subaru/InfraRed Doppler instrument led to 2$\sigma$ upper limits on the masses of $<19.1\ M_\oplus$, $<19.5\ M_\oplus$, $<6.8\ M_\oplus$, and $<15.6\ M_\oplus$ for TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b, respectively. The mass-radius relationship of these four sub-Neptunes testifies to the existence of volatile material in their interiors. These four sub-Neptunes, which are located above the so-called ``radius valley'', are likely to retain a significant atmosphere and/or an icy mantle on the core, such as a water world. We find that at least three of the four sub-Neptunes (TOI-782 b, TOI-2120 b, and TOI-2406 b) orbiting M dwarfs older than 1 Gyr, are likely to have eccentricities of $e \sim 0.2-0.3$. The fact that tidal circularization of their orbits is not achieved over 1 Gyr suggests inefficient tidal dissipation in their interiors., Comment: Accepted for publication in AJ, 32 pages, 17 figures, 6 tables

Published
2024

3. A compact multi-planet system transiting HIP 29442 (TOI-469) discovered by TESS and ESPRESSO. Radial velocities lead to the detection of transits with low signal-to-noise ratio

Author

Damasso, M., Rodrigues, J., Castro-González, A., Lavie, B., Davoult, J., Osorio, M. R. Zapatero, Dou, J., Sousa, S. G., Owen, J. E., Sossi, P., Adibekyan, V., Osborn, H., Leinhardt, Z., Alibert, Y., Lovis, C., Mena, E. Delgado, Sozzetti, A., Barros, S. C. C., Bossini, D., Ziegler, C., Ciardi, D. R., Matthews, E. C., Carter, P. J., Lillo-Box, J., Mascareño, A. Suárez, Cristiani, S., Pepe, F., Rebolo, R., Santos, N. C., Prieto, C. Allende, Benatti, S., Bouchy, F., Briceño, C., Di Marcantonio, P., D'Odorico, V., Dumusque, X., Egger, J. A., Ehrenreich, D., Faria, J., Figueira, P., Santos, R. Génova, Gonzales, E. J., Hernández, J. I. González, Law, N., Curto, G. Lo, Mann, A. W., Martins, C. J. A. P., Mehner, A., Micela, G., Molaro, P., Nunes, N. J., Palle, E., Poretti, E., Schlieder, J. E., and Udry, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We followed-up with ESPRESSO the K0V star HIP 29442 (TOI-469), already known to host a validated sub-Neptune companion TOI-469.01. We aim to verify the planetary nature of TOI-469.01. We modelled radial velocity and photometric time series to measure the dynamical mass, radius, and ephemeris, and to characterise the internal structure and composition of TOI-469.01. We confirmed the planetary nature of TOI-469.01. Thanks to ESPRESSO we discovered two additional close-in companions. We also detected their low signal-to-noise transit signals in the TESS light curve. HIP 29442 is a compact multi-planet system, and the three planets have orbital periods $P_{\rm orb, b}=13.63083\pm0.00003$, $P_{\rm orb, c}=3.53796\pm0.00003$, and $P_{\rm orb, d}=6.42975^{+0.00009}_{-0.00010}$ days, and we measured their masses with high precision: $m_{\rm p, b}=9.6\pm0.8~M_{\oplus}$, $m_{\rm p, c}=4.5\pm0.3~M_{\oplus}$, and $m_{\rm p, d}=5.1\pm0.4~M_{\oplus}$. We measured radii and bulk densities of all the planets (the 3$\sigma$ confidence intervals are shown in parenthesis): $R_{\rm p, b}=3.48^{+0.07 (+0.19)}_{-0.08 (-0.28)} ~R_{\oplus}$ and $\rho_{\rm p, b}=1.3\pm0.2 (0.3) g~cm^{-3}$; $R_{\rm p, c}=1.58^{+0.10 (+0.30)}_{-0.11 (-0.34)}~R_{\oplus}$ and $\rho_{\rm p, c}=6.3^{+1.7 (+6.0)}_{-1.3 (-2.7)} g~cm^{-3}$; $R_{\rm p, d}=1.37\pm0.11^{(+0.32)}_{(-0.43)}~R_{\oplus}$ and $\rho_{\rm p, d}=11.0^{+3.4 (+21.0)}_{-2.4 (-6.3)} g~cm^{-3}$. We used the more conservative 3$\sigma$ confidence intervals for the radii as input to the interior structure modelling. We find that HIP 29442 $b$ appears as a typical sub-Neptune, likely surrounded by a gas layer of pure H-He with a mass of $0.27^{+0.24}_{-0.17} M_{\oplus}$ and a thickness of $1.4\pm0.5 R_{\oplus}$. For the innermost companions HIP 29442 $c$ HIP 29442 $d$, the model supports an Earth-like composition., Comment: Accepted for publication on A&A

Published
2023

4. TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets Around M Dwarf Stars and Revised Parameters for Three Others

Author

Hartman, J. D., Bakos, G. Á., Csubry, Z., Howard, A. W., Isaacson, H., Giacalone, S., Chontos, A., Narita, N., Fukui, A., de Leon, J. P., Watanabe, N., Mori, M., Kagetani, T., Fukuda, I., Kawai, Y., Ikoma, M., Palle, E., Murgas, F., Esparza-Borges, E., Parviainen, H., Bouma, L. G., Cointepas, M., Bonfils, X., Almenara, J. M., Collins, Karen A., Collins, Kevin I., Relles, Howard M., Barkaoui, Khalid, Schwarz, Richard P., Mourad, Ghachoui, Timmermans, Mathilde, Dransfield, Georgina, Burdanov, Artem, de Wit, Julien, Jehin, Emmanuël, Triaud, Amaury H. M. J., Gillon, Michaël, Benkhaldoun, Zouhair, Horne, Keith, Sefako, Ramotholo, Jordán, A., Brahm, R., Suc, V., Howell, Steve B., Furlan, E., Schlieder, J. E., Ciardi, D., Barclay, T., Gonzales, E. J., Crossfield, I., Dressing, C. D., Goliguzova, M., Tatarnikov, A., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Striegel, Stephanie, Shporer, Avi, Vanderburg, Andrew, Levine, Alan M., Kostov, Veselin B., and Watanabe, David

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery from the TESS mission of two giant planets transiting M dwarf stars: TOI 4201 b and TOI 5344 b. We also provide precise radial velocity measurements and updated system parameters for three other M dwarfs with transiting giant planets: TOI 519, TOI 3629 and TOI 3714. We measure planetary masses of 0.525 +- 0.064 M_J, 0.243 +- 0.020 M_J, 0.689 +- 0.030 M_J, 2.57 +- 0.15 M_J, and 0.412 +- 0.040 M_J for TOI 519 b, TOI 3629 b, TOI 3714 b, TOI 4201 b, and TOI 5344 b, respectively. The corresponding stellar masses are 0.372 +- 0.018 M_s, 0.635 +- 0.032 M_s, 0.522 +- 0.028 M_s, 0.625 +- 0.033 M_s and 0.612 +- 0.034 M_s. All five hosts have super-solar metallicities, providing further support for recent findings that, like for solar-type stars, close-in giant planets are preferentially found around metal-rich M dwarf host stars. Finally, we describe a procedure for accounting for systematic errors in stellar evolution models when those models are included directly in fitting a transiting planet system., Comment: 32 pages, 9 figures, 10 tables, submitted to AAS Journals; revised to add co-author

Published
2023

5. TESS discovery of a super-Earth orbiting the M dwarf star TOI-1680

Author

Ghachoui, M., Soubkiou, A., Wells, R. D., Rackham, B. V., Triaud, A. H. M. J., Sebastian, D., Giacalone, S., Stassun, K. G., Ciardi, D. R., Collins, K. A., Liu, A., Chew, Y. Gómez Maqueo, Gillon, M., Benkhaldoun, Z., Delrez, L., Eastman, J. D., Demangeon, O., Barkaoui, K., Burdanov, A., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Garcia, L., Gómez-Muñoz, M. A., Hooton, M. J., Jehin, E., Murray, C. A., Pedersen, P. P., Pozuelos, F. J., Queloz, D., Sabin, L., Schanche, N., Timmermans, M., Gonzales, E. J., Dressing, C. D., Aganze, C., Burgasser, A. J., Gerasimov, R., Hsu, C., Theissen, C. A., Charbonneau, D., Jenkins, J. M., Latham, D. W., Ricker, G., Seager, S., Shporer, A., Twicken, J. D., Vanderspek, R., Winn, J. N., Collins, K. I., Fukui, A., Gan, T., Narita, N., and Schwarz, R. P.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery by the TESS mission of a super-Earth on a 4.8-d orbit around an inactive M4.5 dwarf (TOI-1680) validated by ground-based facilities. The host star is located 37.14 pc away, with a radius of 0.2100+/-0.0064 R_sun, mass of 0.1800+/-0.0044 M_sun and an effective temperature of 3211+/-100 K. We validated and characterized the planet using TESS data, ground-based multi-wavelength photometry from TRAPPIST, SPECULOOS, and LCO, as well as high-resolution AO observations from Keck/NIRC2 and Shane. Our analyses have determined the following parameters for the planet: a radius of 1.466+0.063/-0.049 R_earth and an equilibrium temperature of 404+/-14 K, assuming no albedo and perfect heat redistribution. Assuming a mass based on mass-radius relations, this planet is a promising target for atmospheric characterization with the James Webb Space Telescope (JWST)., Comment: Accepted in A&A

Published
2023
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6. Two super-Earths at the edge of the habitable zone of the nearby M dwarf TOI-2095

Author

Murgas, F., Castro-González, A., Pallé, E., Pozuelos, F. J., Millholland, S., Foo, O., Korth, J., Marfil, E., Amado, P. J., Caballero, J. A., Christiansen, J. L., Ciardi, D. R., Collins, K. A., Di Sora, M., Fukui, A., Gan, T., Gonzales, E. J., Henning, Th., Herrero, E., Isopi, G., Jenkins, J. M., Lillo-Box, J., Lodieu, N., Luque, R., Mallia, F., Morales, J. C., Morello, G., Narita, N., Orell-Miquel, J., Parviainen, H., Pérez-Torres, M., Quirrenbach, A., Reiners, A., Ribas, I., Safonov, B. S., Seager, S., Schwarz, R. P., Schweitzer, A., Schlecker, M., Strakhov, I. A., Vanaverbeke, S., Watanabe, N., Winn, J. N., and Zechmeister, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The main scientific goal of TESS is to find planets smaller than Neptune around stars that are bright enough to allow for further characterization studies. Given our current instrumentation and detection biases, M dwarfs are prime targets in the search for small planets that are in (or near) the habitable zone of their host star. In this work, we use photometric observations and CARMENES radial velocity measurements to validate a pair of transiting planet candidates found by TESS. The data were fitted simultaneously, using a Bayesian Markov chain Monte Carlo (MCMC) procedure and taking into account the stellar variability present in the photometric and spectroscopic time series. We confirm the planetary origin of the two transiting candidates orbiting around TOI-2095 (LSPM J1902+7525). The star is a nearby M dwarf ($d = 41.90 \pm 0.03$ pc, $T_{\rm eff} = 3759 \pm 87$ K, $V = 12.6$ mag), with a stellar mass and radius of $M_\star = 0.44 \pm 0.02 \; M_\odot$ and $R_\star = 0.44 \pm 0.02 \; R_\odot$, respectively. The planetary system is composed of two transiting planets: TOI-2095b, with an orbital period of $P_b = 17.66484 \pm (7\times 10^{-5})$ days, and TOI-2095c, with $P_c = 28.17232 \pm (14\times 10^{-5})$ days. Both planets have similar sizes with $R_b = 1.25 \pm 0.07 \; R_\oplus$ and $R_c = 1.33 \pm 0.08 \; R_\oplus$ for planet b and planet c, respectively. Although we did not detect the induced RV variations of any planet with significance, our CARMENES data allow us to set stringent upper limits on the masses of these objects. We find $M_b < 4.1 \; M_\oplus$ for the inner and $M_c < 7.4 \; M_\oplus$ for the outer planet (95% confidence level). These two planets present equilibrium temperatures in the range of 300-350 K and are close to the inner edge of the habitable zone of their star., Comment: Accepted for publication in A&A. 29 pages

Published
2023
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7. Discovery of a hot, transiting, Earth-sized planet and a second temperate, non-transiting planet around the M4 dwarf GJ 3473 (TOI-488)

Author

Kemmer, J., Stock, S., Kossakowski, D., Kaminski, A., Molaverdikhani, K., Schlecker, M., Caballero, J. A., Amado, P. J., Astudillo-Defru, N., Bonfils, X., Ciardi, D., Collins, K. A., Espinoza, N., Fukui, A., Hirano, T., Jenkins, J. M., Latham, D. W., Matthews, E. C., Narita, N., Pallé, E., Parviainen, H., Quirrenbach, A., Reiners, A., Ribas, I., Ricker, G., Schlieder, J. E., Seager, S., V, R., Winn, J. N., Almenara, J. M., Béjar, V. J. S., Bluhm, P., Bouchy, F., Boyd, P., Christiansen, J. L., Cifuentes, C., Cloutier, R., Collins, K. I., Cortés-Contreras, M., Crossfield, I. J M., Crouzet, N., de Leon, J. P., Della-Rose, D. D., Delfosse, X., Dreizler, S., Esparza-Borges, E., Essack, Z., Forveille, Th., Figueira, P., Galadí-Enríquez, D., Gan, T., Glidden, A., Gonzales, E. J., Guerra, P., Harakawa, H., Hatzes, A. P., Henning, Th., Herrero, E., Hodapp, K., Hori, Y., Howell, S. B., Ikoma, M., Isogai, K., Jeffers, S. V., Kürster, M., Kawauchi, K., Kimura, T., Klagyivik, P., Kotani, T., Kurokawa, T., Kusakabe, N., Kuzuhara, M., Lafarga, M., Livingston, J. H., Luque, R., Matson, R., Morales, J. C., Mori, M., Muirhead, P. S., Murgas, F., Nishikawa, J., Nishiumi, T., Omiya, M., Reffert, S., López, C. Rodríguez, Santos, N. C., Schöfer, P., Schwarz, R. P., Shiao, B., Tamura, M., Terada, Y., Twicken, J. D., Ueda, A., Vievard, S., Watanabe, N., and Zechmeister, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the confirmation and characterisation of GJ 3473 b (G 50--16, TOI-488.01), a hot Earth-sized planet orbiting an M4 dwarf star, whose transiting signal ($P=1.1980035\pm0.0000018\mathrm{\,d}$) was first detected by the Transiting Exoplanet Survey Satellite (TESS). Through a joint modelling of follow-up radial velocity observations with CARMENES, IRD, and HARPS together with extensive ground-based photometric follow-up observations with LCOGT, MuSCAT, and MuSCAT2, we determined a precise planetary mass, $M_b = 1.86\pm0.30\,\mathrm{M_\oplus},$ and radius, $R_b = {1.264\pm0.050}\,\mathrm{R_\oplus}$. Additionally, we report the discovery of a second, temperate, non-transiting planet in the system, GJ 3473 c, which has a minimum mass, $M_c \sin{i} = {7.41\pm0.91}\,\mathrm{M_\oplus,}$ and orbital period, $P_c={15.509\pm0.033}\,\mathrm{d}$. The inner planet of the system, GJ 3473 b, is one of the hottest transiting Earth-sized planets known thus far, accompanied by a dynamical mass measurement, which makes it a particularly attractive target for thermal emission spectroscopy., Comment: 21 pages; accepted for publication in A&A

Published
2020
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8. The CARMENES search for exoplanets around M dwarfs. Two planets on the opposite sides of the radius gap transiting the nearby M dwarf LTT 3780

Author

Nowak, G., Luque, R., Parviainen, H., Pallé, E., Molaverdikhani, K., Béjar, V. J. S., Lillo-Box, J., Rodríguez-López, C., Caballero, J. A., Zechmeister, M., Passegger, V. M., Cifuentes, C., Schweitzer, A., Narita, N., Cale, B., Espinoza, N., Murgas, F., Hidalgo, D., Osorio, M. R. Zapatero, Pozuelos, F. J., Aceituno, F. J., Amado, P. J., Barkaoui, K., Barrado, D., Bauer, F. F., Benkhaldoun, Z., Caldwell, D. A., Barris, N. Casasayas, Chaturvedi, P., Chen, G., Collins, K. A., Collins, K. I., Cortés-Contreras, M., Crossfield, I. J. M., de León, J. P., Alonso, E. Díez, Dreizler, S., Mufti, M. El, Esparza-Borges, E., Essack, Z., Fukui, A., Gaidos, E., Gillon, M., Gonzales, E. J., Guerra, P., Hatzes, A., Henning, T., Herrero, E., Hesse, K., Hirano, T., Howell, S. B., Jeffers, S. V., Jehin, E., Jenkins, J. M., Kaminski, A., Kemmer, J., Kielkopf, J. F., Kossakowski, D., Kotani, T., Kürster, M., Lafarga, M., Latham, D. W., Law, N., Lissauer, J. J., Lodieu, N., Madrigal-Aguado, A., Mann, A. W., Massey, B., Matson, R. A., Matthews, E., Montanés-Rodríguez, P., Montes, D., Morales, J. C., Mori, M., Nagel, E., Oshagh, M., Pedraz, S., Plavchan, P., Pollacco, D., Quirrenbach, A., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rose, M. E., Schlecker, M., Schlieder, J. E., Seager, S., Stangret, M., Stock, S., Tamura, M., Tanner, A., Teske, J., Trifonov, T., Twicken, J. D., Vanderspek, R., Watanabe, D., Wittrock, J., Ziegler, C., and Zohrabi, F.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the discovery and characterisation of two transiting planets observed by the Transiting Exoplanet Survey Satellite (TESS) orbiting the nearby (d ~ 22 pc), bright (J ~ 9 mag) M3.5 dwarf LTT 3780 (TOI-732). We confirm both planets and their association with LTT 3780 via ground-based photometry and determine their masses using precise radial velocities measured with the CARMENES spectrograph. Precise stellar parameters determined from CARMENES high resolution spectra confirm that LTT 3780 is a mid-M dwarf with an effective temperature of T_eff = 3360 +\- 51 K, a surface gravity of log(g) = 4.81 +/- 0.04 (cgs), and an iron abundance of [Fe/H] = 0.09 +/- 0.16 dex, with an inferred mass of M_star = 0.379 +/- 0.016 M_sun and a radius of R_star = 0.382 +/- 0.012 R_sun. The ultra-short-period planet LTT 3780 b (P_b = 0.77 d) with a radius of 1.35^{+0.06}_{-0.06} R_earth, a mass of 2.34^{+0.24}_{-0.23} M_earth, and a bulk density of 5.24^{+0.94}_{-0.81} g cm^{-3} joins the population of Earth-size planets with rocky, terrestrial composition. The outer planet, LTT 3780 c, with an orbital period of 12.25 d, radius of 2.42^{+0.10}_{-0.10} R_earth, mass of 6.29^{+0.63}_{-0.61} M_earth, and mean density of 2.45^{+0.44}_{-0.37} g cm^{-3} belongs to the population of dense sub-Neptunes. With the two planets located on opposite sides of the radius gap, this planetary system is an excellent target for testing planetary formation, evolution and atmospheric models. In particular, LTT 3780 c is an ideal object for atmospheric studies with the James Webb Space Telescope., Comment: 21 pages, 15 figures, 4 tables, submitted to A&A

Published
2020
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9. TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others

Author

Hartman, J. D., primary, Bakos, G. Á., additional, Csubry, Z., additional, Howard, A. W., additional, Isaacson, H., additional, Giacalone, S., additional, Chontos, A., additional, Narita, N., additional, Fukui, A., additional, de Leon, J. P., additional, Watanabe, N., additional, Mori, M., additional, Kagetani, T., additional, Fukuda, I., additional, Kawai, Y., additional, Ikoma, M., additional, Palle, E., additional, Murgas, F., additional, Esparza-Borges, E., additional, Parviainen, H., additional, Bouma, L. G., additional, Cointepas, M., additional, Bonfils, X., additional, Almenara, J. M., additional, Collins, Karen A., additional, Collins, Kevin I., additional, Relles, Howard M., additional, Barkaoui, Khalid, additional, Schwarz, Richard P., additional, Mourad, Ghachoui, additional, Timmermans, Mathilde, additional, Dransfield, Georgina, additional, Burdanov, Artem, additional, de Wit, Julien, additional, Jehin, Emmanuël, additional, Triaud, Amaury H. M. J., additional, Gillon, Michaël, additional, Benkhaldoun, Zouhair, additional, Horne, Keith, additional, Sefako, Ramotholo, additional, Jordán, A., additional, Brahm, R., additional, Suc, V., additional, Howell, Steve B., additional, Furlan, E., additional, Schlieder, J. E., additional, Ciardi, D., additional, Barclay, T., additional, Gonzales, E. J., additional, Crossfield, I., additional, Dressing, C. D., additional, Goliguzova, M., additional, Tatarnikov, A., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Striegel, Stephanie, additional, Shporer, Avi, additional, Vanderburg, Andrew, additional, Levine, Alan M., additional, Kostov, Veselin B., additional, and Watanabe, David, additional

Published
2023
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10. Two super-Earths at the edge of the habitable zone of the nearby M dwarf TOI-2095

Author

Murgas, F., primary, Castro-González, A., additional, Pallé, E., additional, Pozuelos, F. J., additional, Millholland, S., additional, Foo, O., additional, Korth, J., additional, Marfil, E., additional, Amado, P. J., additional, Caballero, J. A., additional, Christiansen, J. L., additional, Ciardi, D. R., additional, Collins, K. A., additional, Di Sora, M., additional, Fukui, A., additional, Gan, T., additional, Gonzales, E. J., additional, Henning, Th., additional, Herrero, E., additional, Isopi, G., additional, Jenkins, J. M., additional, Lillo-Box, J., additional, Lodieu, N., additional, Luque, R., additional, Mallia, F., additional, Morales, J. C., additional, Morello, G., additional, Narita, N., additional, Orell-Miquel, J., additional, Parviainen, H., additional, Pérez-Torres, M., additional, Quirrenbach, A., additional, Reiners, A., additional, Ribas, I., additional, Safonov, B. S., additional, Seager, S., additional, Schwarz, R. P., additional, Schweitzer, A., additional, Schlecker, M., additional, Strakhov, I. A., additional, Vanaverbeke, S., additional, Watanabe, N., additional, Winn, J. N., additional, and Zechmeister, M., additional

Published
2023
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11. TESS discovery of a super-Earth orbiting the M-dwarf star TOI-1680

Author

Ghachoui, M., primary, Soubkiou, A., additional, Wells, R. D., additional, Rackham, B. V., additional, Triaud, A. H. M. J., additional, Sebastian, D., additional, Giacalone, S., additional, Stassun, K. G., additional, Ciardi, D. R., additional, Collins, K. A., additional, Liu, A., additional, Gómez Maqueo Chew, Y., additional, Gillon, M., additional, Benkhaldoun, Z., additional, Delrez, L., additional, Eastman, J. D., additional, Demangeon, O., additional, Barkaoui, K., additional, Burdanov, A., additional, Demory, B.-O., additional, de Wit, J., additional, Dransfield, G., additional, Ducrot, E., additional, Garcia, L., additional, Gómez-Muñoz, M. A., additional, Hooton, M. J., additional, Jehin, E., additional, Murray, C. A., additional, Pedersen, P. P., additional, Pozuelos, F. J., additional, Queloz, D., additional, Sabin, L., additional, Schanche, N., additional, Timmermans, M., additional, Gonzales, E. J., additional, Dressing, C. D., additional, Aganze, C., additional, Burgasser, A. J., additional, Gerasimov, R., additional, Hsu, C., additional, Theissen, C. A., additional, Charbonneau, D., additional, Jenkins, J. M., additional, Latham, D. W., additional, Ricker, G., additional, Seager, S., additional, Shporer, A., additional, Twicken, J. D., additional, Vanderspek, R., additional, Winn, J. N., additional, Collins, K. I., additional, Fukui, A., additional, Gan, T., additional, Narita, N., additional, and Schwarz, R. P., additional

Published
2023
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12. Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Author

Osborn, H P, primary, Nowak, G, additional, Hébrard, G, additional, Masseron, T, additional, Lillo-Box, J, additional, Pallé, E, additional, Bekkelien, A, additional, Florén, H-G, additional, Guterman, P, additional, Simon, A E, additional, Adibekyan, V, additional, Bieryla, A, additional, Borsato, L, additional, Brandeker, A, additional, Ciardi, D R, additional, Collier Cameron, A, additional, Collins, K A, additional, Egger, J A, additional, Gandolfi, D, additional, Hooton, M J, additional, Latham, D W, additional, Lendl, M, additional, Matthews, E C, additional, Tuson, A, additional, Ulmer-Moll, S, additional, Vanderburg, A, additional, Wilson, T G, additional, Ziegler, C, additional, Alibert, Y, additional, Alonso, R, additional, Anglada, G, additional, Arnold, L, additional, Asquier, J, additional, Barrado y Navascues, D, additional, Baumjohann, W, additional, Beck, T, additional, Belinski, A A, additional, Benz, W, additional, Biondi, F, additional, Boisse, I, additional, Bonfils, X, additional, Broeg, C, additional, Buchhave, L A, additional, Bárczy, T, additional, Barros, S C C, additional, Cabrera, J, additional, Cardona Guillen, C, additional, Carleo, I, additional, Castro-González, A, additional, Charnoz, S, additional, Christiansen, J, additional, Cortes-Zuleta, P, additional, Csizmadia, S, additional, Dalal, S, additional, Davies, M B, additional, Deleuil, M, additional, Delfosse, X, additional, Delrez, L, additional, Demory, B-O, additional, Dunlavey, A B, additional, Ehrenreich, D, additional, Erikson, A, additional, Fernandes, R B, additional, Fortier, A, additional, Forveille, T, additional, Fossati, L, additional, Fridlund, M, additional, Gillon, M, additional, Goeke, R F, additional, Goliguzova, M V, additional, Gonzales, E J, additional, Günther, M N, additional, Güdel, M, additional, Heidari, N, additional, Henze, C E, additional, Howell, S, additional, Hoyer, S, additional, Frey, J I, additional, Isaak, K G, additional, Jenkins, J M, additional, Kiefer, F, additional, Kiss, L, additional, Korth, J, additional, Maxted, P F L, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lovis, C, additional, Lund, M B, additional, Luque, R, additional, Magrin, D, additional, Almenara, J M, additional, Martioli, E, additional, Mecina, M, additional, Medina, J V, additional, Moldovan, D, additional, Morales-Calderón, M, additional, Morello, G, additional, Moutou, C, additional, Murgas, F, additional, Jensen, E L N, additional, Nascimbeni, V, additional, Olofsson, G, additional, Ottensamer, R, additional, Pagano, I, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Ribas, I, additional, Ricker, G, additional, Demangeon, O D S, additional, Smith, A M S, additional, Santos, N, additional, Scandariato, G, additional, Seager, S, additional, Sousa, S G, additional, Steller, M, additional, Szabó, G M, additional, Ségransan, D, additional, Thomas, N, additional, Udry, S, additional, Ulmer, B, additional, Van Grootel, V, additional, Vanderspek, R, additional, Walton, N, additional, and Winn, J N, additional

Published
2023
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13. Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Author

Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., Winn, J. N., Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., and Winn, J. N.

Abstract

HIP 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 <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

Published
2023

14. Discovery of a hot, transiting, Earth-sized planet and a second temperate, non-transiting planet around the M4 dwarf GJ 3473 (TOI-488)

Author

Kemmer, J., primary, Stock, S., additional, Kossakowski, D., additional, Kaminski, A., additional, Molaverdikhani, K., additional, Schlecker, M., additional, Caballero, J. A., additional, Amado, P. J., additional, Astudillo-Defru, N., additional, Bonfils, X., additional, Ciardi, D., additional, Collins, K. A., additional, Espinoza, N., additional, Fukui, A., additional, Hirano, T., additional, Jenkins, J. M., additional, Latham, D. W., additional, Matthews, E. C., additional, Narita, N., additional, Pallé, E., additional, Parviainen, H., additional, Quirrenbach, A., additional, Reiners, A., additional, Ribas, I., additional, Ricker, G., additional, Schlieder, J. E., additional, Seager, S., additional, Vanderspek, R., additional, Winn, J. N., additional, Almenara, J. M., additional, Béjar, V. J. S., additional, Bluhm, P., additional, Bouchy, F., additional, Boyd, P., additional, Christiansen, J. L., additional, Cifuentes, C., additional, Cloutier, R., additional, Collins, K. I., additional, Cortés-Contreras, M., additional, Crossfield, I. J M., additional, Crouzet, N., additional, de Leon, J. P., additional, Della-Rose, D. D., additional, Delfosse, X., additional, Dreizler, S., additional, Esparza-Borges, E., additional, Essack, Z., additional, Forveille, Th., additional, Figueira, P., additional, Galadí-Enríquez, D., additional, Gan, T., additional, Glidden, A., additional, Gonzales, E. J., additional, Guerra, P., additional, Harakawa, H., additional, Hatzes, A. P., additional, Henning, Th., additional, Herrero, E., additional, Hodapp, K., additional, Hori, Y., additional, Howell, S. B., additional, Ikoma, M., additional, Isogai, K., additional, Jeffers, S. V., additional, Kürster, M., additional, Kawauchi, K., additional, Kimura, T., additional, Klagyivik, P., additional, Kotani, T., additional, Kurokawa, T., additional, Kusakabe, N., additional, Kuzuhara, M., additional, Lafarga, M., additional, Livingston, J. H., additional, Luque, R., additional, Matson, R., additional, Morales, J. C., additional, Mori, M., additional, Muirhead, P. S., additional, Murgas, F., additional, Nishikawa, J., additional, Nishiumi, T., additional, Omiya, M., additional, Reffert, S., additional, Rodríguez López, C., additional, Santos, N. C., additional, Schöfer, P., additional, Schwarz, R. P., additional, Shiao, B., additional, Tamura, M., additional, Terada, Y., additional, Twicken, J. D., additional, Ueda, A., additional, Vievard, S., additional, Watanabe, N., additional, and Zechmeister, M., additional

Published
2020
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15. The CARMENES search for exoplanets around M dwarfs

Author

Nowak, G., primary, Luque, R., additional, Parviainen, H., additional, Pallé, E., additional, Molaverdikhani, K., additional, Béjar, V. J. S., additional, Lillo-Box, J., additional, Rodríguez-López, C., additional, Caballero, J. A., additional, Zechmeister, M., additional, Passegger, V. M., additional, Cifuentes, C., additional, Schweitzer, A., additional, Narita, N., additional, Cale, B., additional, Espinoza, N., additional, Murgas, F., additional, Hidalgo, D., additional, Zapatero Osorio, M. R., additional, Pozuelos, F. J., additional, Aceituno, F. J., additional, Amado, P. J., additional, Barkaoui, K., additional, Barrado, D., additional, Bauer, F. F., additional, Benkhaldoun, Z., additional, Caldwell, D. A., additional, Casasayas Barris, N., additional, Chaturvedi, P., additional, Chen, G., additional, Collins, K. A., additional, Collins, K. I., additional, Cortés-Contreras, M., additional, Crossfield, I. J. M., additional, de León, J. P., additional, Díez Alonso, E., additional, Dreizler, S., additional, El Mufti, M., additional, Esparza-Borges, E., additional, Essack, Z., additional, Fukui, A., additional, Gaidos, E., additional, Gillon, M., additional, Gonzales, E. J., additional, Guerra, P., additional, Hatzes, A., additional, Henning, Th., additional, Herrero, E., additional, Hesse, K., additional, Hirano, T., additional, Howell, S. B., additional, Jeffers, S. V., additional, Jehin, E., additional, Jenkins, J. M., additional, Kaminski, A., additional, Kemmer, J., additional, Kielkopf, J. F., additional, Kossakowski, D., additional, Kotani, T., additional, Kürster, M., additional, Lafarga, M., additional, Latham, D. W., additional, Law, N., additional, Lissauer, J. J., additional, Lodieu, N., additional, Madrigal-Aguado, A., additional, Mann, A. W., additional, Massey, B., additional, Matson, R. A., additional, Matthews, E., additional, Montañés-Rodríguez, P., additional, Montes, D., additional, Morales, J. C., additional, Mori, M., additional, Nagel, E., additional, Oshagh, M., additional, Pedraz, S., additional, Plavchan, P., additional, Pollacco, D., additional, Quirrenbach, A., additional, Reffert, S., additional, Reiners, A., additional, Ribas, I., additional, Ricker, G. R., additional, Rose, M. E., additional, Schlecker, M., additional, Schlieder, J. E., additional, Seager, S., additional, Stangret, M., additional, Stock, S., additional, Tamura, M., additional, Tanner, A., additional, Teske, J., additional, Trifonov, T., additional, Twicken, J. D., additional, Vanderspek, R., additional, Watanabe, D., additional, Wittrock, J., additional, Ziegler, C., additional, and Zohrabi, F., additional

Published
2020
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