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73 results on '"Barkaoui K"'

1. TOI-1135 b: A young hot Saturn-size planet orbiting a solar-type star

Author: Mallorquín, M., Lodieu, N., Béjar, V. J. S., Osorio, M. R. Zapatero, Sanz-Forcada, J., Alarcon, M. R., Tabernero, H. M., Nagel, E., Collins, K. A., Ciardi, D. R., Serra-Ricart, M., Orell-Miquel, J., Barkaoui, K., Burdanov, A., de Wit, J., Everett, M. E., Gillon, M., Jensen, E. L. N., Murphy, L. G., Reed, P. A., Safonov, B., Strakhov, I. A., Ziegler, C., Mallorquín, M., Lodieu, N., Béjar, V. J. S., Osorio, M. R. Zapatero, Sanz-Forcada, J., Alarcon, M. R., Tabernero, H. M., Nagel, E., Collins, K. A., Ciardi, D. R., Serra-Ricart, M., Orell-Miquel, J., Barkaoui, K., Burdanov, A., de Wit, J., Everett, M. E., Gillon, M., Jensen, E. L. N., Murphy, L. G., Reed, P. A., Safonov, B., Strakhov, I. A., and Ziegler, C.
Abstract: Despite the thousands of planets in orbit around stars known to date, the mechanisms of planetary formation, migration, and atmospheric loss remain unresolved. In this work, we confirm the planetary nature of a young Saturn-size planet transiting a solar-type star every 8.03 d, TOI-1135\,b. The age of the parent star is estimated to be in the interval of 125--1000 Myr based on various activity and age indicators, including its stellar rotation period of 5.13\,$\pm$\,0.27 d and the intensity of photospheric lithium. We obtained follow-up photometry and spectroscopy, including precise radial velocity measurements using the CARMENES spectrograph, which together with the TESS data allowed us to fully characterise the parent star and its planet. As expected for its youth, the star is rather active and shows strong photometric and spectroscopic variability correlating with its rotation period. We modelled the stellar variability using Gaussian process regression. We measured the planetary radius at 9.02\,$\pm$\,0.23 R$_\oplus$ (0.81\,$\pm$\,0.02 R$_{\mathrm{Jup}}$) and determined a 3$\sigma$ upper limit of $<$\,51.4 M$_\oplus$ ($<$\,0.16 \,M$_{\rm{Jup}}$) on the planetary mass by adopting a circular orbit. Our results indicate that TOI-1135\,b is an inflated planet less massive than Saturn or Jupiter but with a similar radius, which could be in the process of losing its atmosphere by photoevaporation. This new young planet occupies a region of the mass-radius diagram where older planets are scarse, and it could be very helpful to understanding the lower frequency of planets with sizes between Neptune and Saturn., Comment: Accepted in A&A. 18 pages, 15 figures
Published: 2024

2. TOI-2266 b: a keystone super-Earth at the edge of the M dwarf radius valley

Author: Parviainen, Hannu, Murgas, Felipe, Esparza-Borges, Emma, Peláez-Torres, A., Palle, Enric, Luque, Rafael, Zapatero-Osorio, M. R., Korth, Judith, Fukui, Akihiko, Narita, Norio, Collins, K. A., Béjar, V. J. S., Morello, Guiseppe, Monelli, M., Garcia, N. Abreu, Chen, Guo, Crouzet, N., de Leon, J. P., Isogai, K., Kagetani, T., Kawauchi, K., Klagyivik, P., Kodama, T., Kusakabe, N., Livingston, J. H., Meni, P., Mori, M., Nowak, G., Tamura, M., Terada, Y., Watanabe, N., Ciardi, D. R., Lund, M. B., Christiansen, J. L., Dressing, C. D., Giacalone, S., Savel, A. B., Hirsch, L., Parsons, S. G., Brown, P., Collins, K. I., Barkaoui, K., Timmermans, M., Ghachoui, M., Soubkiou, A., Benkhaldoun, Z., McDermott, S., Pritchard, T., Rowden, P., Striegel, S., Gan, T., Horne, K., Jensen, E. L. N., Schwarz, R. P., Shporer, A., Srdoc, G., Seager, S., Winn, J. N., Jenkins, J. M., Ricker, G., Vanderspek, R., Dragomir, D., Parviainen, Hannu, Murgas, Felipe, Esparza-Borges, Emma, Peláez-Torres, A., Palle, Enric, Luque, Rafael, Zapatero-Osorio, M. R., Korth, Judith, Fukui, Akihiko, Narita, Norio, Collins, K. A., Béjar, V. J. S., Morello, Guiseppe, Monelli, M., Garcia, N. Abreu, Chen, Guo, Crouzet, N., de Leon, J. P., Isogai, K., Kagetani, T., Kawauchi, K., Klagyivik, P., Kodama, T., Kusakabe, N., Livingston, J. H., Meni, P., Mori, M., Nowak, G., Tamura, M., Terada, Y., Watanabe, N., Ciardi, D. R., Lund, M. B., Christiansen, J. L., Dressing, C. D., Giacalone, S., Savel, A. B., Hirsch, L., Parsons, S. G., Brown, P., Collins, K. I., Barkaoui, K., Timmermans, M., Ghachoui, M., Soubkiou, A., Benkhaldoun, Z., McDermott, S., Pritchard, T., Rowden, P., Striegel, S., Gan, T., Horne, K., Jensen, E. L. N., Schwarz, R. P., Shporer, A., Srdoc, G., Seager, S., Winn, J. N., Jenkins, J. M., Ricker, G., Vanderspek, R., and Dragomir, D.
Abstract: We validate the Transiting Exoplanet Survey Satellite (TESS) object of interest TOI-2266.01 (TIC 348911) as a small transiting planet (most likely a super-Earth) orbiting a faint M5 dwarf ($V=16.54$) on a 2.33~d orbit. The validation is based on an approach where multicolour transit light curves are used to robustly estimate the upper limit of the transiting object's radius. Our analysis uses SPOC-pipeline TESS light curves from Sectors 24, 25, 51, and 52, simultaneous multicolour transit photometry observed with MuSCAT2, MuSCAT3, and HiPERCAM, and additional transit photometry observed with the LCOGT telescopes. TOI-2266 b is found to be a planet with a radius of $1.54\pm\0.09\,R_\oplus$, which locates it at the edge of the transition zone between rocky planets, water-rich planets, and sub-Neptunes (the so-called M~dwarf radius valley). The planet is amenable to ground-based radial velocity mass measurement with red-sensitive spectrographs installed in large telescopes, such as MAROON-X and Keck Planet Finder (KPF), which makes it a valuable addition to a relatively small population of planets that can be used to probe the physics of the transition zone. Further, the planet's orbital period of 2.33 days places it inside a `keystone planet' wedge in the period-radius plane where competing planet formation scenarios make conflicting predictions on how the radius valley depends on the orbital period. This makes the planet also a welcome addition to the small population of planets that can be used to test small-planet formation scenarios around M~dwarfs., Comment: Accepted to A&A
Published: 2024

3. Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs

Author: Murgas, F., Pallé, E., Orell-Miquel, J., Carleo, I., Peña-Moñino, L., Pérez-Torres, M., Watkins, C. N., Jeffers, S. V., Azzaro, M., Barkaoui, K., Belinski, A. A., Caballero, J. A., Charbonneau, D., Cheryasov, D. V., Ciardi, D. R., Collins, K. A., Cortés-Contreras, M., de Leon, J., Duque-Arribas, C., Enoc, G., Esparza-Borges, E., Fukui, A., Geraldía-González, S., Gilbert, E. A., Hatzes, A. P., Hayashi, Y., Henning, Th., Herrero, E., Jenkins, J. M., Lillo-Box, J., Lodieu, N., Lund, M. B., Luque, R., Montes, D., Nagel, E., Narita, N., Parviainen, H., Polanski, A. S., Reffert, S., Schlecker, M., Schöfer, P., Schwarz, R. P., Schweitzer, A., Seager, S., Stassun, K. G., Tabernero, H. M., Terada, Y., Twicken, J. D., Vanaverbeke, S., Winn, J. N., Zambelli, R., Amado, P. J., Quirrenbach, A., Reiners, A., Ribas, I., Murgas, F., Pallé, E., Orell-Miquel, J., Carleo, I., Peña-Moñino, L., Pérez-Torres, M., Watkins, C. N., Jeffers, S. V., Azzaro, M., Barkaoui, K., Belinski, A. A., Caballero, J. A., Charbonneau, D., Cheryasov, D. V., Ciardi, D. R., Collins, K. A., Cortés-Contreras, M., de Leon, J., Duque-Arribas, C., Enoc, G., Esparza-Borges, E., Fukui, A., Geraldía-González, S., Gilbert, E. A., Hatzes, A. P., Hayashi, Y., Henning, Th., Herrero, E., Jenkins, J. M., Lillo-Box, J., Lodieu, N., Lund, M. B., Luque, R., Montes, D., Nagel, E., Narita, N., Parviainen, H., Polanski, A. S., Reffert, S., Schlecker, M., Schöfer, P., Schwarz, R. P., Schweitzer, A., Seager, S., Stassun, K. G., Tabernero, H. M., Terada, Y., Twicken, J. D., Vanaverbeke, S., Winn, J. N., Zambelli, R., Amado, P. J., Quirrenbach, A., Reiners, A., and Ribas, I.
Abstract: Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small ($R_\mathrm{p} < 2\; R_\oplus$) ultra-short-period (USP) planets are highly irradiated, probably have rocky compositions with high bulk densities, and are often found in multi-planet systems. Additionally, USP planets found around small stars are excellent candidates for characterization using present-day instrumentation. Of the current full sample of approximately 5500 confirmed exoplanets, only 130 are USP planets and around 40 have mass and radius measurements. Wolf 327 (TOI-5747) is an M dwarf ($R_\star = 0.406 \pm 0.015 \; R_\odot$, $M_\star = 0.405 \pm 0.019 \; M_\odot$, $T_{\mathrm{eff}}=3542 \pm 70$ K, and $V = 13$ mag) located at a distance $d = 28.5$ pc. NASA's planet hunter satellite, TESS, detected transits in this star with a period of 0.573 d (13.7 h) and with a transit depth of 818 ppm. Ground-based follow-up photometry, high resolution imaging, and radial velocity (RV) measurements taken with the CARMENES spectrograph confirm the presence of this new USP planet. Wolf 327b is a super-Earth with a radius of $R_\mathrm{p} = 1.24 \pm 0.06 \; R_\oplus$ and a mass of $M_\mathrm{p} = 2.53 \pm 0.46 \; M_\oplus$, yielding a bulk density of $7.24 \pm 1.66 $\,g cm$^{-3}$ and thus suggesting a rocky composition. Owing to its close proximity to its host star ($a = 0.01$ au), Wolf 327b has an equilibrium temperature of $996 \pm 22$ K. This planet has a mass and radius similar to K2-229b, a planet with an inferred Mercury-like internal composition. Planet interior models suggest that Wolf 327b has a large iron core, a small rocky mantle, and a negligible (if any) H/He atmosphere., Comment: 26 pages, 19 figures. Accepted for publication in A&A
Published: 2024

4. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, Bruno, Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Burwitz, V., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Waldemar Sybilski, P., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Bykowski, W., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Müller, Thomas G., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Ogloza, W., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Gonçalves, R., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Ferreira, J.F., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Ferreira, M., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Bento, M., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Urbaník, M., Holler, B.J., Er, H., Weber, C., Kalkan, S., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, Bruno, Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Burwitz, V., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Waldemar Sybilski, P., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Bykowski, W., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Müller, Thomas G., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Ogloza, W., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Gonçalves, R., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Ferreira, J.F., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Ferreira, M., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Bento, M., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Urbaník, M., Holler, B.J., Er, H., Weber, C., Kalkan, S., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., and Juravle, A.
Abstract: Context. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs’ fundamental physical properties with high precision, such as size and shape. Aims. This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also study the object’s topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fit ellipse, combined with the object’s rotational information from the literature, sets constraints on the object’s size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object’s limb. Results. The global limb has a semi-major axis of a′ = 412 ± 10 km, a semi-minor axis of b′= 385 ± 17 km, and the position angle of the minor axis is 121° ± 16°. From this instantaneous limb, we obtained 2002 MS4’s geometric albedo of pV = 0.1 ± 0.025, using HV = 3.63 ± 0.05 mag and a projected area-equivalent diameter of 796 ± 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25−5+4 k
Published: 2023

5. Two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., Zúñiga-fernández, S., Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-fernández, S.
Published: 2023

6. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS$_4$ measured from stellar occultations

Author: Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., Wake, D. A., Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., and Wake, D. A.
Abstract: This work aims at constraining the size, shape, and geometric albedo of the dwarf planet candidate 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also studied the object's topography by analyzing the obtained limb and the residuals between observed chords and the best-fitted ellipse. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with three to up to sixty-one positive chords. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fitted ellipse, combined with the object's rotational information from the literature, constrains the object's size, shape, and albedo. Additionally, we developed a new method to characterize topography features on the object's limb. The global limb has a semi-major axis of 412 $\pm$ 10 km, a semi-minor axis of 385 $\pm$ 17 km, and the position angle of the minor axis is 121 $^\circ$ $\pm$ 16$^\circ$. From this instantaneous limb, we obtained 2002 MS4's geometric albedo and the projected area-equivalent diameter. Significant deviations from the fitted ellipse in the northernmost limb are detected from multiple sites highlighting three distinct topographic features: one 11 km depth depression followed by a 25$^{+4}_{-5}$ km height elevation next to a crater-like depression with an extension of 322 $\pm$ 39 km and 45.1 $\pm$ 1.5 km deep. Our results present an object that is $\approx$138 km smaller in diameter than derived from thermal data, possibly indicating the presence of a so-far unknown satellite. However, within the error bars, the geometric albedo in the V-band agrees with the results published in the literature, even with the radiometric-derived albedo.
Published: 2023
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7. 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., Schwarz, R. P., 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.
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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8. TOI-2084 b and TOI-4184 b: two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-Reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-Gaxiola, S., Ghachoui, M., Chew, Y. Gómez Maqueo, Günther, M. N., McCormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-López, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., Zúñiga-Fernández, S., Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-Reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-Gaxiola, S., Ghachoui, M., Chew, Y. Gómez Maqueo, Günther, M. N., McCormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-López, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-Fernández, S.
Abstract: We present the discovery and validation of two TESS exoplanets orbiting nearby M dwarfs: TOI-2084b, and TOI-4184b. We characterized the host stars by combining spectra from Shane/Kast and Magellan/FIRE, SED (Spectral Energy Distribution) analysis, and stellar evolutionary models. In addition, we used Gemini-South/Zorro & -North/Alopeke high-resolution imaging, archival science images, and statistical validation packages to support the planetary interpretation. We performed a global analysis of multi-colour photometric data from TESS and ground-based facilities in order to derive the stellar and planetary physical parameters for each system. We find that TOI-2084b and TOI-4184b are sub-Neptune-sized planets with radii of Rp = 2.47 +/- 0.13R_Earth and Rp = 2.43 +/- 0.21R_Earth, respectively. TOI-2084b completes an orbit around its host star every 6.08 days, has an equilibrium temperature of T_eq = 527 +/- 8K and an irradiation of S_p = 12.8 +/- 0.8 S_Earth. Its host star is a dwarf of spectral M2.0 +/- 0.5 at a distance of 114pc with an effective temperature of T_eff = 3550 +/- 50 K, and has a wide, co-moving M8 companion at a projected separation of 1400 au. TOI-4184b orbits around an M5.0 +/- 0.5 type dwarf star (Kmag = 11.87) each 4.9 days, and has an equilibrium temperature of T_eq = 412 +/- 8 K and an irradiation of S_p = 4.8 +/- 0.4 S_Earth. TOI-4184 is a metal poor star ([Fe/H] = -0.27 +/- 0.09 dex) at a distance of 69 pc with an effective temperature of T_eff = 3225 +/- 75 K. Both planets are located at the edge of the sub-Jovian desert in the radius-period plane. The combination of the small size and the large infrared brightness of their host stars make these new planets promising targets for future atmospheric exploration with JWST., Comment: Accepted for publication in A&A
Published: 2023

9. TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet

Author: Korth, J., Gandolfi, D., Šubjak, J., Howard, S., Ataiee, S., Collins, K. A., Quinn, S. N., Mustill, A. J., Guillot, T., Lodieu, N., Smith, A. M. S., Esposito, M., Rodler, F., Muresan, A., Abe, L., Albrecht, S. H., Alqasim, A., Barkaoui, K., Beck, P. G., Burke, C. J., Butler, R. P., Conti, D. M., Collins, K. I., Crane, J. D., Dai, F., Deeg, H. J., Evans, P., Grziwa, S., Hatzes, A. P., Hirano, T., Horne, K., Huang, C. X., Jenkins, J. M., Kabáth, P., Kielkopf, J. F., Knudstrup, E., Latham, D. W., Livingston, J., Luque, R., Mathur, S., Murgas, F., Osborne, H. L. M., Pallé, E., Persson, C. M., Rodriguez, J. E., Rose, M., Rowden, P., Schwarz, R. P., Seager, S., Serrano, L. M., Sha, L., Shectman, S. A., Shporer, A., Srdoc, G., Stockdale, C., Tan, T. G., Teske, J. K., Van Eylen, V., Vanderburg, A., Vanderspek, R., Wang, S. X., Winn, J. N., Korth, J., Gandolfi, D., Šubjak, J., Howard, S., Ataiee, S., Collins, K. A., Quinn, S. N., Mustill, A. J., Guillot, T., Lodieu, N., Smith, A. M. S., Esposito, M., Rodler, F., Muresan, A., Abe, L., Albrecht, S. H., Alqasim, A., Barkaoui, K., Beck, P. G., Burke, C. J., Butler, R. P., Conti, D. M., Collins, K. I., Crane, J. D., Dai, F., Deeg, H. J., Evans, P., Grziwa, S., Hatzes, A. P., Hirano, T., Horne, K., Huang, C. X., Jenkins, J. M., Kabáth, P., Kielkopf, J. F., Knudstrup, E., Latham, D. W., Livingston, J., Luque, R., Mathur, S., Murgas, F., Osborne, H. L. M., Pallé, E., Persson, C. M., Rodriguez, J. E., Rose, M., Rowden, P., Schwarz, R. P., Seager, S., Serrano, L. M., Sha, L., Shectman, S. A., Shporer, A., Srdoc, G., Stockdale, C., Tan, T. G., Teske, J. K., Van Eylen, V., Vanderburg, A., Vanderspek, R., Wang, S. X., and Winn, J. N.
Abstract: The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c, on an 8.4-day orbit, accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We perform a photodynamical modeling of the HARPS and PFS RVs, and transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program. We determine the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 $\pm$ 0.97 M$_\oplus$ and Rb = 3.56 $\pm$ 0.13 R$_\oplus$, and Mc = 325.59 $\pm$ 5.59 M$_\oplus$ and Rc = 13.32+1.55-1.41 R$_\oplus$, respectively. We spectroscopically confirm TOI-1130 b that was previously only validated. We find that the two planets orbit with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small yet increasing population of hot Jupiters with an inner low-mass planet that challenges the pathway for hot Jupiter formation. We also detect a linear RV trend possibly due to the presence of an outer massive companion., Comment: 19 pages, Accepted to A&A
Published: 2023
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10. A super-Earth and a mini-Neptune near the 2:1 MMR straddling the radius valley around the nearby mid-M dwarf TOI-2096

Author: Pozuelos, F. J., Timmermans, M., Rackham, B. V., Garcia, L. J., Burgasser, A. J., Kane, S. R., Günther, M. N., Stassun, K. G., Van Grootel, V., Dévora-Pajares, M., Luque, R., Edwards, B., Niraula, P., Schanche, N., Wells, R. D., Ducrot, E., Howell, S., Sebastian, D., Barkaoui, K., Waalkes, W., Cadieux, C., Doyon, R., Boyle, R. P., Dietrich, J., Burdanov, A., Delrez, L., Demory, B. -O., de Wit, J., Dransfield, G., Gillon, M., Chew, Y. Gómez Maqueo, Hooton, M. J., Jehin, E., Murray, C. A., Pedersen, P. P., Queloz, D., Thompson, S. J., Triaud, A. H. M. J., Zúñiga-Fernández, S., Collins, K. A., Fausnaugh, M. M., Hedges, C., Hesse, K. M., Jenkins, J. M., Kunimoto, M., Latham, D. W., Shporer, A., Ting, E. B., Torres, G., Amado, P., Rodón, J. R., Rodríguez-López, C., Suárez, J. C., Alonso, R., Benkhaldoun, Z., Berta-Thompson, Z. K., Chinchilla, P., Ghachoui, M., Gómez-Muñoz, M. A., Rebolo, R., Sabin, L., Schroffenegger, U., Furlan, E., Gnilka, C., Lester, K., Scott, N., Aganze, C., Gerasimov, R., Hsu, C., Theissen, C., Apai, D., Chen, W. P., Gabor, P., Henning, T., Mancini, L., Pozuelos, F. J., Timmermans, M., Rackham, B. V., Garcia, L. J., Burgasser, A. J., Kane, S. R., Günther, M. N., Stassun, K. G., Van Grootel, V., Dévora-Pajares, M., Luque, R., Edwards, B., Niraula, P., Schanche, N., Wells, R. D., Ducrot, E., Howell, S., Sebastian, D., Barkaoui, K., Waalkes, W., Cadieux, C., Doyon, R., Boyle, R. P., Dietrich, J., Burdanov, A., Delrez, L., Demory, B. -O., de Wit, J., Dransfield, G., Gillon, M., Chew, Y. Gómez Maqueo, Hooton, M. J., Jehin, E., Murray, C. A., Pedersen, P. P., Queloz, D., Thompson, S. J., Triaud, A. H. M. J., Zúñiga-Fernández, S., Collins, K. A., Fausnaugh, M. M., Hedges, C., Hesse, K. M., Jenkins, J. M., Kunimoto, M., Latham, D. W., Shporer, A., Ting, E. B., Torres, G., Amado, P., Rodón, J. R., Rodríguez-López, C., Suárez, J. C., Alonso, R., Benkhaldoun, Z., Berta-Thompson, Z. K., Chinchilla, P., Ghachoui, M., Gómez-Muñoz, M. A., Rebolo, R., Sabin, L., Schroffenegger, U., Furlan, E., Gnilka, C., Lester, K., Scott, N., Aganze, C., Gerasimov, R., Hsu, C., Theissen, C., Apai, D., Chen, W. P., Gabor, P., Henning, T., and Mancini, L.
Abstract: Several planetary formation models have been proposed to explain the observed abundance and variety of compositions of super-Earths and mini-Neptunes. In this context, multitransiting systems orbiting low-mass stars whose planets are close to the radius valley are benchmark systems, which help to elucidate which formation model dominates. We report the discovery, validation, and initial characterization of one such system, TOI-2096, composed of a super-Earth and a mini-Neptune hosted by a mid-type M dwarf located 48 pc away. We first characterized the host star by combining different methods. Then, we derived the planetary properties by modeling the photometric data from TESS and ground-based facilities. We used archival data, high-resolution imaging, and statistical validation to support our planetary interpretation. We found that TOI-2096 corresponds to a dwarf star of spectral type M4. It harbors a super-Earth (R$\sim1.2 R_{\oplus}$) and a mini-Neptune (R$\sim1.90 R_{\oplus}$) in likely slightly eccentric orbits with orbital periods of 3.12 d and 6.39 d, respectively. These orbital periods are close to the first-order 2:1 mean-motion resonance (MMR), which may lead to measurable transit timing variations (TTVs). We computed the expected TTVs amplitude for each planet and found that they might be measurable with high-precision photometry delivering mid-transit times with accuracies of $\lesssim$2 min. Moreover, measuring the planetary masses via radial velocities (RVs) is also possible. Lastly, we found that these planets are among the best in their class to conduct atmospheric studies using the James Webb Space Telescope (JWST). The properties of this system make it a suitable candidate for further studies, particularly for mass determination using RVs and/or TTVs, decreasing the scarcity of systems that can be used to test planetary formation models around low-mass stars., Comment: 25 pages, 21 figures. Aceptted for publication in Astronomy & Astrophysics
Published: 2023
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11. TOI-2084 b and TOI-4184 b: Two new sub-Neptunes around M dwarf stars

Author: European Commission, European Research Council, Agencia Estatal de Investigación (España), Barkaoui, K., Pozuelos, Francisco José, European Commission, European Research Council, Agencia Estatal de Investigación (España), Barkaoui, K., and Pozuelos, Francisco José
Abstract: We present the discovery and validation of two TESS exoplanets orbiting nearby M dwarfs: TOI-2084 b, and TOI-4184b. We characterized the host stars by combining spectra from Shane/Kast and Magellan/FIRE, spectral energy distribution analysis, and stellar evolutionary models. In addition, we used Gemini-South/Zorro & -North/Alopeke high-resolution imaging, archival science images, and statistical validation packages to support the planetary interpretation. We performed a global analysis of multi-colour photometric data from TESS and ground-based facilities in order to derive the stellar and planetary physical parameters for each system. We find that TOI-2084 band TOI-4184 bare sub-Neptune-sized planets with radii of R = 2.47 ± 0.13R and R = 2.43 ± 0.21 R, respectively. TOI-2084 b completes an orbit around its host star every 6.08 days, has an equilibrium temperature of T = 527 ± 8 K and an irradiation of S = 12.8 ± 0.8 S. Its host star is a dwarf of spectral M2.0 ± 0.5 at a distance of 114 pc with an effective temperature of T = 3550 ± 50 K, and has a wide, co-moving M8 companion at a projected separation of 1400 au. TOI-4184 b orbits around an M5.0 ± 0.5 type dwarf star (K = 11.87) each 4.9 days, and has an equilibrium temperature of T = 412 ± 8 K and an irradiation of S = 4.8 ± 0.4 S. TOI-4184 is a metal poor star ([Fe/H] = 0.27 ± 0.09 dex) at a distance of 69 pc with an effective temperature of T = 3225 ± 75 K. Both planets are located at the edge of the sub-Jovian desert in the radius-period plane. The combination of the small size and the large infrared brightness of their host stars make these new planets promising targets for future atmospheric exploration with JWST. © 2023 Authors. All rights reserved.
Published: 2023

12. The GAPS Programme at TNG L -- TOI-4515 b: An eccentric warm Jupiter orbiting a 1.2 Gyr-old G-star

Author: Carleo, I., Malavolta, L., Desidera, S., Nardiello, D., Wang, Songhu, Turrini, D., Lanza, A. F., Baratella, M., Marzari, F., Benatti, S., Biazzo, K., Bieryla, A., Brahm, R., Bonavita, M., Collins, K. A., Hellier, C., Locci, D., Hobson, M. J., Maggio, A., Mantovan, G., Pinamonti, S. Messina M., Rodriguez, J. E., Sozzetti, A., Stassun, K., Wang, X. Y., Ziegler, C., Damasso, M., Giacobbe, P., Murgas, F., Parviainen, H., Andreuzzi, G., Barkaoui, K., Berlind, P., Bignamini, A., Borsa, F., Briceño, C., Brogi, M., Cabona, L., Calkins, M. L., Capuzzo-Dolcetta, R., Cecconi, M., Colon, K. D., Cosentino, R., Dragomir, D., Esquerdo, G. A., Henning, T., Ghedina, A., Goeke, R. F., Gratton, R., Horta, F. Grau, Gupta, A. F., Jenkins, J. M., Jordán, A., Knapic, C., Latham, D. W., Mireles, I., Law, N., Lorenzi, V., Lund, M. B., Maldonado, J., Mann, A. W., Molinari, E., Pallé, E., Paegert, M., Pedani, M., Quinn, S. N., Scandariato, G., Seager, S., Winn, J. N., Wohler, B., Zingales, T., Carleo, I., Malavolta, L., Desidera, S., Nardiello, D., Wang, Songhu, Turrini, D., Lanza, A. F., Baratella, M., Marzari, F., Benatti, S., Biazzo, K., Bieryla, A., Brahm, R., Bonavita, M., Collins, K. A., Hellier, C., Locci, D., Hobson, M. J., Maggio, A., Mantovan, G., Pinamonti, S. Messina M., Rodriguez, J. E., Sozzetti, A., Stassun, K., Wang, X. Y., Ziegler, C., Damasso, M., Giacobbe, P., Murgas, F., Parviainen, H., Andreuzzi, G., Barkaoui, K., Berlind, P., Bignamini, A., Borsa, F., Briceño, C., Brogi, M., Cabona, L., Calkins, M. L., Capuzzo-Dolcetta, R., Cecconi, M., Colon, K. D., Cosentino, R., Dragomir, D., Esquerdo, G. A., Henning, T., Ghedina, A., Goeke, R. F., Gratton, R., Horta, F. Grau, Gupta, A. F., Jenkins, J. M., Jordán, A., Knapic, C., Latham, D. W., Mireles, I., Law, N., Lorenzi, V., Lund, M. B., Maldonado, J., Mann, A. W., Molinari, E., Pallé, E., Paegert, M., Pedani, M., Quinn, S. N., Scandariato, G., Seager, S., Winn, J. N., Wohler, B., and Zingales, T.
Abstract: Context. Different theories have been developed to explain the origins and properties of close-in giant planets, but none of them alone can explain all of the properties of the warm Jupiters (WJs, Porb = 10 - 200 days). One of the most intriguing characteristics of WJs is that they have a wide range of orbital eccentricities, challenging our understanding of their formation and evolution. Aims. The investigation of these systems is crucial in order to put constraints on formation and evolution theories. TESS is providing a significant sample of transiting WJs around stars bright enough to allow spectroscopic follow-up studies. Methods. We carried out a radial velocity (RV) follow-up study of the TESS candidate TOI-4515 b with the high-resolution spectrograph HARPS-N in the context of the GAPS project, the aim of which is to characterize young giant planets, and the TRES and FEROS spectrographs. We then performed a joint analysis of the HARPS-N, TRES, FEROS, and TESS data in order to fully characterize this planetary system. Results. We find that TOI-4515 b orbits a 1.2 Gyr-old G-star, has an orbital period of Pb = 15.266446 +- 0.000013 days, a mass of Mb = 2.01 +- 0.05 MJ, and a radius of Rb = 1.09 +- 0.04 RJ. We also find an eccentricity of e = 0.46 +- 0.01, placing this planet among the WJs with highly eccentric orbits. As no additional companion has been detected, this high eccentricity might be the consequence of past violent scattering events., Comment: 20 pages, 16 figures
Published: 2023

13. A hot mini-Neptune and a temperate, highly eccentric sub-Saturn around the bright K-dwarf TOI-2134

Author: Rescigno, F., Hébrard, G., Vanderburg, A., Mann, A. W., Mortier, A., Morrell, S., Buchhave, L. A., Collins, K. A., Mann, C. R., Hellier, C., Haywood, R. D., West, R., Stalport, M., Heidari, N., Anderson, D., Huang, C. X., López-Morales, M., Cortés-Zuleta, P., Lewis, H. M., Dumusque, X., Boisse, I., Rowden, P., Cameron, A. Collier, Deleuil, M., Vezie, M., Pepe, F. A., Delfosse, X., Charbonneau, D., Rice, K., Demangeon, O., Quinn, S. N., Udry, S., Forveille, T., Winn, J. N., Sozzetti, A., Hoyer, S., Seager, S., Wilson, T. G., Dalal, S., Martioli, E., Striegel, S., Boschin, W., Dragomir, D., Fiorenzano, A. F. Martínez, Cosentino, R., Ghedina, A., Malavolta, L., Affer, L., Lakeland, B. S., Nicholson, B. A., Foschino, S., Wünsche, A., Barkaoui, K., Srdoc, G., Randolph, J., Guillet, B., Conti, D. M., Ghachoui, M., Gillon, M., Benkhaldoun, Z., Pozuelos, F. J., Timmermans, M., Girardin, E., Matutano, S., Bosch-Cabot, P., Muñoz, J. A., Forés-Toribio, R., Rescigno, F., Hébrard, G., Vanderburg, A., Mann, A. W., Mortier, A., Morrell, S., Buchhave, L. A., Collins, K. A., Mann, C. R., Hellier, C., Haywood, R. D., West, R., Stalport, M., Heidari, N., Anderson, D., Huang, C. X., López-Morales, M., Cortés-Zuleta, P., Lewis, H. M., Dumusque, X., Boisse, I., Rowden, P., Cameron, A. Collier, Deleuil, M., Vezie, M., Pepe, F. A., Delfosse, X., Charbonneau, D., Rice, K., Demangeon, O., Quinn, S. N., Udry, S., Forveille, T., Winn, J. N., Sozzetti, A., Hoyer, S., Seager, S., Wilson, T. G., Dalal, S., Martioli, E., Striegel, S., Boschin, W., Dragomir, D., Fiorenzano, A. F. Martínez, Cosentino, R., Ghedina, A., Malavolta, L., Affer, L., Lakeland, B. S., Nicholson, B. A., Foschino, S., Wünsche, A., Barkaoui, K., Srdoc, G., Randolph, J., Guillet, B., Conti, D. M., Ghachoui, M., Gillon, M., Benkhaldoun, Z., Pozuelos, F. J., Timmermans, M., Girardin, E., Matutano, S., Bosch-Cabot, P., Muñoz, J. A., and Forés-Toribio, R.
Abstract: We present the characterisation of an inner mini-Neptune in a 9.2292005$\pm$0.0000063 day orbit and an outer mono-transiting sub-Saturn planet in a 95.50$^{+0.36}_{-0.25}$ day orbit around the moderately active, bright (mv=8.9 mag) K5V star TOI-2134. Based on our analysis of five sectors of TESS data, we determine the radii of TOI-2134b and c to be 2.69$\pm$0.16 R$_{e}$ for the inner planet and 7.27$\pm$0.42 R$_{e}$ for the outer one. We acquired 111 radial-velocity spectra with HARPS-N and 108 radial-velocity spectra with SOPHIE. After careful periodogram analysis, we derive masses for both planets via Gaussian Process regression: 9.13$^{+0.78}_{-0.76}$ M$_{e}$ for TOI-2134b and 41.86$^{+7.69}_{-7.83}$ M$_{e}$ for TOI-2134c. We analysed the photometric and radial-velocity data first separately, then jointly. The inner planet is a mini-Neptune with density consistent with either a water-world or a rocky core planet with a low-mass H/He envelope. The outer planet has a bulk density similar to Saturn's. The outer planet is derived to have a significant eccentricity of 0.67$^{+0.05}_{-0.06}$ from a combination of photometry and RVs. We compute the irradiation of TOI-2134c as 1.45$\pm$0.10 times the bolometric flux received by Earth, positioning it for part of its orbit in the habitable sone of its system. We recommend further RV observations to fully constrain the orbit of TOI-2134c. With an expected Rossiter-McLaughlin (RM) effect amplitude of 7.2$\pm$1.3 m/s, we recommend TOI-2134c for follow-up RM analysis to study the spin-orbit architecture of the system. We calculate the Transmission Spectroscopy Metric, and both planets are suitable for bright-mode NIRCam atmospheric characterisation., Comment: 24 pages, 7 tables, 14 figures
Published: 2023
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14. The GAPS programme at TNG XLIX. TOI-5398, the youngest compact multi-planet system composed of an inner sub-Neptune and an outer warm Saturn

Author: Mantovan, G., Malavolta, L., Desidera, S., Zingales, T., Borsato, L., Piotto, G., Maggio, A., Locci, D., Polychroni, D., Turrini, D., Baratella, M., Biazzo, K., Nardiello, D., Stassun, K., Nascimbeni, V., Benatti, S., John, A. Anna, Watkins, C., Bieryla, A., Lissauer, J. J., Twicken, J. D., Lanza, A. F., Winn, J. N., Messina, S., Montalto, M., Sozzetti, A., Boffin, H., Cheryasov, D., Strakhov, I., Murgas, F., D'Arpa, M., Barkaoui, K., Benni, P., Bignamini, A., Bonomo, A., Borsa, F., Cabona, L., Cameron, A. C., Claudi, R., Cochran, W., Collins, K. A., Damasso, M., Dong, J., Endl, M., Fukui, A., Furész, G., Gandolfi, D., Ghedina, A., Jenkins, J., Kabáth, P., Latham, D. W., Lorenzi, V., Luque, R., Maldonado, J., McLeod, K., Molinaro, M., Narita, N., Nowak, G., Orell-Miquel, J., Pallé, E., Parviainen, H., Pedani, M., Quinn, S. N., Relles, H., Rowden, P., Scandariato, G., Schwarz, R., Seager, S., Shporer, A., Vanderburg, A., Wilson, T. G., Mantovan, G., Malavolta, L., Desidera, S., Zingales, T., Borsato, L., Piotto, G., Maggio, A., Locci, D., Polychroni, D., Turrini, D., Baratella, M., Biazzo, K., Nardiello, D., Stassun, K., Nascimbeni, V., Benatti, S., John, A. Anna, Watkins, C., Bieryla, A., Lissauer, J. J., Twicken, J. D., Lanza, A. F., Winn, J. N., Messina, S., Montalto, M., Sozzetti, A., Boffin, H., Cheryasov, D., Strakhov, I., Murgas, F., D'Arpa, M., Barkaoui, K., Benni, P., Bignamini, A., Bonomo, A., Borsa, F., Cabona, L., Cameron, A. C., Claudi, R., Cochran, W., Collins, K. A., Damasso, M., Dong, J., Endl, M., Fukui, A., Furész, G., Gandolfi, D., Ghedina, A., Jenkins, J., Kabáth, P., Latham, D. W., Lorenzi, V., Luque, R., Maldonado, J., McLeod, K., Molinaro, M., Narita, N., Nowak, G., Orell-Miquel, J., Pallé, E., Parviainen, H., Pedani, M., Quinn, S. N., Relles, H., Rowden, P., Scandariato, G., Schwarz, R., Seager, S., Shporer, A., Vanderburg, A., and Wilson, T. G.
Abstract: Short-period giant planets are frequently found to be solitary compared to other classes of exoplanets. Small inner companions to giant planets with $P \lesssim$ 15 days are known only in five compact systems: WASP-47, Kepler-730, WASP-132, TOI-1130, and TOI-2000. Here, we report the confirmation of TOI-5398, the youngest compact multi-planet system composed of a hot sub-Neptune (TOI-5398 c, $P_{\rm c}$ = 4.77271 days) orbiting interior to a short-period Saturn (TOI-5398 b, $P_{\rm b}$ = 10.590547 days) planet, both transiting around a 650 $\pm$ 150 Myr G-type star. As part of the GAPS Young Object project, we confirmed and characterised this compact system, measuring the radius and mass of both planets, thus constraining their bulk composition. Using multidimensional Gaussian processes, we simultaneously modelled stellar activity and planetary signals from TESS Sector 48 light curve and our HARPS-N radial velocity time series. We have confirmed the planetary nature of both planets, TOI-5398 b and TOI-5398 c, alongside a precise estimation of stellar parameters. Through the use of astrometric, photometric, and spectroscopic observations, our findings indicate that TOI-5398 is a young, active G dwarf star (650 $\pm$ 150 Myr), with a rotational period of $P_{\rm rot}$ = 7.34 days. The transit photometry and radial velocity measurements enabled us to measure both the radius and mass of planets b, $R_b = 10.30\pm0.40 R_{\oplus}$, $M_b = 58.7\pm5.7 M_{\oplus}$, and c, $R_c = 3.52 \pm 0.19 R_{\oplus}$, $M_c = 11.8\pm4.8 M_{\oplus}$. TESS observed TOI-5398 during sector 48 and no further observations are planned in the current Extended Mission, making our ground-based light curves crucial for ephemeris improvement. With a Transmission Spectroscopy Metric value of around 300, TOI-5398 b is the most amenable warm giant (10 < $P$ < 100 days) for JWST atmospheric characterisation., Comment: 29 pages, Paper accepted for publication in Astronomy & Astrophysics
Published: 2023

15. Two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., Zúñiga-fernández, S., Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-fernández, S.
Published: 2023

16. TOI-1442 b and TOI-2445 b: two ultra-short period super-Earths around M dwarfs

Author: Morello, G., Parviainen, H., Murgas, F., Pallé, E., Oshagh, M., Fukui, A., Hirano, T., Ishikawa, H. T., Narita, N., Collins, K. A., Barkaoui, K., Lewin, P., Cadieux, C., de Leon, J. P., Soubkiou, A., Crouzet, N., Esparza-Borges, E., Rodríguez, G. E. Fernández, Hori, Y., Ikoma, M., Isogai, K., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kotani, T., Krishnamurthy, V., Kurita, S., Laza-Ramos, A., Livingston, J. H., Luque, R., Madrigal-Aguado, A., Mori, M., Nishiumi, T., Orell-Miquel, J., Puig-Subirà, M., Sánchez-Benavente, M., Stangret, M., Tamura, M., Terada, Y., Watanabe, N., Zou, Y., Benkhaldoun, Z., Collins, K. I., Doyon, R., Garcia, L., Ghachoui, M., Gillon, M., Jehin, E., Jensen, E. L. N., Pozuelos, F. J., Schwarz, R. P., Timmermans, M., Morello, G., Parviainen, H., Murgas, F., Pallé, E., Oshagh, M., Fukui, A., Hirano, T., Ishikawa, H. T., Narita, N., Collins, K. A., Barkaoui, K., Lewin, P., Cadieux, C., de Leon, J. P., Soubkiou, A., Crouzet, N., Esparza-Borges, E., Rodríguez, G. E. Fernández, Hori, Y., Ikoma, M., Isogai, K., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kotani, T., Krishnamurthy, V., Kurita, S., Laza-Ramos, A., Livingston, J. H., Luque, R., Madrigal-Aguado, A., Mori, M., Nishiumi, T., Orell-Miquel, J., Puig-Subirà, M., Sánchez-Benavente, M., Stangret, M., Tamura, M., Terada, Y., Watanabe, N., Zou, Y., Benkhaldoun, Z., Collins, K. I., Doyon, R., Garcia, L., Ghachoui, M., Gillon, M., Jehin, E., Jensen, E. L. N., Pozuelos, F. J., Schwarz, R. P., and Timmermans, M.
Abstract: Context. Exoplanets with orbital periods of less than one day are know as Ultra-short period (USP) planets. They are relatively rare products of planetary formation and evolution processes, but especially favourable to current planet detection methods. At the time of writing, 120 USP planets have already been confirmed. Aims. We aim to confirm the planetary nature of two new transiting planet candidates announced by the NASA's Transiting Exoplanet Survey Satellite (TESS), registered as TESS Objects of Interest (TOIs) TOI-1442.01 and TOI-2445.01. Methods. We use the TESS data, ground-based photometric light-curves and Subaru/IRD spectrograph radial velocity (RV) measurements to validate both planetary candidates and to establish their physical properties. Results. TOI-1442 b is a hot super-Earth with an orbital period of $P = 0.4090682 \pm 0.0000004 \, d$, a radius of $R_{\mathrm{p}} = 1.15 \pm 0.06 \, R_{\oplus}$, equilibrium temperature of $T_{\mathrm{p,eq}} = 1357_{-42}^{+49} \, K$, and a mass $M_{\mathrm{p}} < 18 \, M_{\oplus}$ at 3$\sigma$. TOI-2445 b is also a hot super-Earth/mini-Neptune with an orbital period of $P = 0.3711286 \pm 0.0000004 \, d$, a radius of $R_{\mathrm{p}} = 1.33 \pm 0.09 \, R_{\oplus}$, equilibrium temperature of $T_{\mathrm{p,eq}} = 1330_{-56}^{+61} \, K$, and a mass $M_{\mathrm{p}} < 38 \, M_{\oplus}$ at 3$\sigma$. Their physical properties align with current empirical trends and formation theories of USP planets. More RV measurements will be useful to constrain the planetary masses and mean densities, as well as the predicted presence of outer planetary companions.
Published: 2022

17. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author: Oliveira, J. Marques, Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernández-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Pérez-Hoyos, S., Sánchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K. -L., Bode, H. -J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelínek, M., Štrobl, J., Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Pütz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J. -M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, G., Sanchez, R. Zanmar, Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Savio, R. Lo, Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., Abbeel, F. Van Den, André, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J. -P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J. -F., Metz, F., Erpelding, D., Nougayrède, P., Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Aissa, D. Baba, Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Reche, A. Román, Casanova, V., Briggs, E., Iglesias-Marzoa, R., Ibáñez, J. Abril, Martín, M. C. Díaz, González, H., García, J. L. Maestre, Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Gonçalves, R., Ferreira, M., Dias, F. Marques, Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., Moutamid, M. El, Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J. -P., Françoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Neilsen, G., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Oliveira, J. Marques, Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernández-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Pérez-Hoyos, S., Sánchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K. -L., Bode, H. -J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelínek, M., Štrobl, J., Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Pütz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J. -M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, G., Sanchez, R. Zanmar, Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Savio, R. Lo, Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., Abbeel, F. Van Den, André, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J. -P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J. -F., Metz, F., Erpelding, D., Nougayrède, P., Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Aissa, D. Baba, Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Reche, A. Román, Casanova, V., Briggs, E., Iglesias-Marzoa, R., Ibáñez, J. Abril, Martín, M. C. Díaz, González, H., García, J. L. Maestre, Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Gonçalves, R., Ferreira, M., Dias, F. Marques, Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., Moutamid, M. El, Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J. -P., Françoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Neilsen, G., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., and Downs, B.
Abstract: A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range $\sim$8 km to $\sim$190 km, corresponding to pressure levels from 9 {\mu}bar down to a few nanobars. Results. (i) A pressure of 1.18$\pm$0.03 {\mu}bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 {\mu}bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Comment: 52 pages, 26 figures in the main paper, 2 figures in appendix B, 9 figures in appendix C, 1 long table over 5 pages
Published: 2022
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18. A Possible Alignment between the Orbits of Planetary Systems and their Visual Binary Companions

Author: Christian, S., Vanderburg, A., Becker, J., Yahalomi, D. A., Pearce, L., Zhou, G., Collins, K. A., Kraus, A. L., Stassun, K. G., De, Beurs, Z., Ricker, G. R., Vanderspek, R. K., Latham, D. W., Winn, J. N., Seager, S., Jenkins, J. M., Abe, L., Agabi, K., Amado, P. J., Baker, D., Barkaoui, K., Benkhaldoun, Z., Benni, P., Berberian, J., Berlind, P., Bieryla, A., Esparza-Borges, E., Bowen, M., Brown, P., Buchhave, L. A., Burke, C. J., Buttu, M., Cadieux, C., Caldwell, D. A., Charbonneau, D., Chazov, N., Chimaladinne, S., Collins, K. I., Combs, D., Conti, D. M., Crouzet, N., De Leon, J. P., Deljookorani, S., Diamond, B., Doyon, R., Dragomir, D., Dransfield, G., Essack, Z., Evans, P., Fukui, A., Gan, T., Esquerdo, G. A., Gillon, M., Girardin, E., Guerra, P., Guillot, T., K. , Habich, E. K., Henriksen, A., Hoch, N., Isogai, K. I., Jehin, E., Jensen, E. L. N., Johnson, M. C., Livingston, J. H., Kielkopf, J. F., Kim, K., Kawauchi, K., Krushinsky, V., Kunzle, V., Laloum, D., Leger, D., Lewin, P., Mallia, F., Massey, B., Mori, M., McLeod, K. K., Mékarnia, D., Mireles, I., Mishevskiy, N., Tamura, M., Murgas, F., Narita, N., Naves, R., Nelson, P., Osborn, H. P., Palle, E., Parviainen, H., Plavchan, P., Pozuelos, F. J., Rabus, M., Relles, H. M., Rodríguez, López, C., Quinn, S. N., Schmider, F. -X., Schlieder, J. E., Schwarz, R. P., Shporer, A., Sibbald, L., Srdoc, G., Stibbards, C., Stickler, H., Suarez, O., Stockdale, C., Tan, T. -G., Terada, Y., Triaud, A., Tronsgaard, R., Waalkes, W. C., Wang, G., Watanabe, N., Wenceslas, M. -S., Wingham, G., Wittrock, J., Ziegler, C., Christian, S., Vanderburg, A., Becker, J., Yahalomi, D. A., Pearce, L., Zhou, G., Collins, K. A., Kraus, A. L., Stassun, K. G., De, Beurs, Z., Ricker, G. R., Vanderspek, R. K., Latham, D. W., Winn, J. N., Seager, S., Jenkins, J. M., Abe, L., Agabi, K., Amado, P. J., Baker, D., Barkaoui, K., Benkhaldoun, Z., Benni, P., Berberian, J., Berlind, P., Bieryla, A., Esparza-Borges, E., Bowen, M., Brown, P., Buchhave, L. A., Burke, C. J., Buttu, M., Cadieux, C., Caldwell, D. A., Charbonneau, D., Chazov, N., Chimaladinne, S., Collins, K. I., Combs, D., Conti, D. M., Crouzet, N., De Leon, J. P., Deljookorani, S., Diamond, B., Doyon, R., Dragomir, D., Dransfield, G., Essack, Z., Evans, P., Fukui, A., Gan, T., Esquerdo, G. A., Gillon, M., Girardin, E., Guerra, P., Guillot, T., K. , Habich, E. K., Henriksen, A., Hoch, N., Isogai, K. I., Jehin, E., Jensen, E. L. N., Johnson, M. C., Livingston, J. H., Kielkopf, J. F., Kim, K., Kawauchi, K., Krushinsky, V., Kunzle, V., Laloum, D., Leger, D., Lewin, P., Mallia, F., Massey, B., Mori, M., McLeod, K. K., Mékarnia, D., Mireles, I., Mishevskiy, N., Tamura, M., Murgas, F., Narita, N., Naves, R., Nelson, P., Osborn, H. P., Palle, E., Parviainen, H., Plavchan, P., Pozuelos, F. J., Rabus, M., Relles, H. M., Rodríguez, López, C., Quinn, S. N., Schmider, F. -X., Schlieder, J. E., Schwarz, R. P., Shporer, A., Sibbald, L., Srdoc, G., Stibbards, C., Stickler, H., Suarez, O., Stockdale, C., Tan, T. -G., Terada, Y., Triaud, A., Tronsgaard, R., Waalkes, W. C., Wang, G., Watanabe, N., Wenceslas, M. -S., Wingham, G., Wittrock, J., and Ziegler, C.
Abstract: Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation. © 2022. The Author(s). Published by the American Astronomical Society.
Published: 2022

19. Two temperate super-Earths transiting a nearby late-type M dwarf

Author: Delrez, L., Murray, C. A., Pozuelos, F. J., Narita, N., Ducrot, E., Timmermans, M., Watanabe, N., Burgasser, A. J., Hirano, T., Rackham, B. V., Stassun, K. G., Van Grootel, V., Aganze, C., Cointepas, M., Howell, S., Kaltenegger, L., Niraula, P., Sebastian, D., Almenara, J. M., Barkaoui, K., Baycroft, T. A., Bonfils, X., Bouchy, F., Burdanov, A., Caldwell, D. A., Charbonneau, D., Ciardi, D. R., Collins, K. A., Daylan, T., Demory, B. -O., de Wit, J., Dransfield, G., Fajardo-Acosta, S. B., Fausnaugh, M., Fukui, A., Furlan, E., Garcia, L. J., Gnilka, C. L., Chew, Y. Gómez Maqueo, Gómez-Muñoz, M. A., Günther, M. N., Harakawa, H., Heng, K., Hooton, M. J., Hori, Y., Ikoma, M., Jehin, E., Jenkins, J. M., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Kotani, T., Krishnamurthy, V., Kudo, T., Kunovac, V., Kusakabe, N., Latham, D. W., Littlefield, C., McCormac, J., Melis, C., Mori, M., Murgas, F., Palle, E., Pedersen, P. P., Queloz, D., Ricker, G., Sabin, L., Schanche, N., Schroffenegger, U., Seager, S., Shiao, B., Sohy, S., Standing, M. R., Tamura, M., Theissen, C. A., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Vievard, S., Wells, R. D., Winn, J. N., Zou, Y., Zúñiga-Fernández, S., Gillon, M., Delrez, L., Murray, C. A., Pozuelos, F. J., Narita, N., Ducrot, E., Timmermans, M., Watanabe, N., Burgasser, A. J., Hirano, T., Rackham, B. V., Stassun, K. G., Van Grootel, V., Aganze, C., Cointepas, M., Howell, S., Kaltenegger, L., Niraula, P., Sebastian, D., Almenara, J. M., Barkaoui, K., Baycroft, T. A., Bonfils, X., Bouchy, F., Burdanov, A., Caldwell, D. A., Charbonneau, D., Ciardi, D. R., Collins, K. A., Daylan, T., Demory, B. -O., de Wit, J., Dransfield, G., Fajardo-Acosta, S. B., Fausnaugh, M., Fukui, A., Furlan, E., Garcia, L. J., Gnilka, C. L., Chew, Y. Gómez Maqueo, Gómez-Muñoz, M. A., Günther, M. N., Harakawa, H., Heng, K., Hooton, M. J., Hori, Y., Ikoma, M., Jehin, E., Jenkins, J. M., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Kotani, T., Krishnamurthy, V., Kudo, T., Kunovac, V., Kusakabe, N., Latham, D. W., Littlefield, C., McCormac, J., Melis, C., Mori, M., Murgas, F., Palle, E., Pedersen, P. P., Queloz, D., Ricker, G., Sabin, L., Schanche, N., Schroffenegger, U., Seager, S., Shiao, B., Sohy, S., Standing, M. R., Tamura, M., Theissen, C. A., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Vievard, S., Wells, R. D., Winn, J. N., Zou, Y., Zúñiga-Fernández, S., and Gillon, M.
Abstract: In the age of JWST, temperate terrestrial exoplanets transiting nearby late-type M dwarfs provide unique opportunities for characterising their atmospheres, as well as searching for biosignature gases. We report here the discovery and validation of two temperate super-Earths transiting LP 890-9 (TOI-4306, SPECULOOS-2), a relatively low-activity nearby (32 pc) M6V star. The inner planet, LP 890-9b, was first detected by TESS (and identified as TOI-4306.01) based on four sectors of data. Intensive photometric monitoring of the system with the SPECULOOS Southern Observatory then led to the discovery of a second outer transiting planet, LP 890-9c (also identified as SPECULOOS-2c), previously undetected by TESS. The orbital period of this second planet was later confirmed by MuSCAT3 follow-up observations. With a mass of 0.118$\pm$0.002 $M_\odot$, a radius of 0.1556$\pm$0.0086 $R_\odot$, and an effective temperature of 2850$\pm$75 K, LP 890-9 is the second-coolest star found to host planets, after TRAPPIST-1. The inner planet has an orbital period of 2.73 d, a radius of $1.320_{-0.027}^{+0.053}$ $R_\oplus$, and receives an incident stellar flux of 4.09$\pm$0.12 $S_\oplus$. The outer planet has a similar size of $1.367_{-0.039}^{+0.055}$ $R_\oplus$ and an orbital period of 8.46 d. With an incident stellar flux of 0.906 $\pm$ 0.026 $S_\oplus$, it is located within the conservative habitable zone, very close to its inner limit. Although the masses of the two planets remain to be measured, we estimated their potential for atmospheric characterisation via transmission spectroscopy using a mass-radius relationship and found that, after the TRAPPIST-1 planets, LP 890-9c is the second-most favourable habitable-zone terrestrial planet known so far. The discovery of this remarkable system offers another rare opportunity to study temperate terrestrial planets around our smallest and coolest neighbours., Comment: 31 pages, 19 figures, 7 tables. Accepted for publication in A&A
Published: 2022
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20. A hot sub-Neptune in the desert and a temperate super-Earth around faint M dwarfs: Color validation of TOI-4479b and TOI-2081b

Author: Esparza-Borges, E., Parviainen, H., Murgas, F., Pallé, E., Maas, A., Morello, G., Zapatero-Osorio, M. R., Barkaoui, K., Narita, N., Fukui, A., Casasayas-Barris, N., Oshagh, M., Crouzet, N., Galán, D., Fernández, G. E., Kagetani, T., Kawauchi, K., Kodama, T., Korth, J., Kusakabe, N., Laza-Ramos, A., Luque, R., Livingston, J., Madrigal-Aguado, A., Mori, M., Orell-Miquel, J., Puig-Subirá, M., Stangret, M., Terada, Y., Watanabe, N., Zou, Y., Savel, A. Baliga, Belinski, A. A., Collins, K., Dressing, C. D., Giacalone, S., Gill, H., Goliguzova, M. V., Ikoma, M., Jenkins, J. M., Tamura, M., Twicken, J. D., Ricker, G. R., Schwarz, R. P., Seager, S., Shporer, A., Vanderspek, R., Winn, J., Esparza-Borges, E., Parviainen, H., Murgas, F., Pallé, E., Maas, A., Morello, G., Zapatero-Osorio, M. R., Barkaoui, K., Narita, N., Fukui, A., Casasayas-Barris, N., Oshagh, M., Crouzet, N., Galán, D., Fernández, G. E., Kagetani, T., Kawauchi, K., Kodama, T., Korth, J., Kusakabe, N., Laza-Ramos, A., Luque, R., Livingston, J., Madrigal-Aguado, A., Mori, M., Orell-Miquel, J., Puig-Subirá, M., Stangret, M., Terada, Y., Watanabe, N., Zou, Y., Savel, A. Baliga, Belinski, A. A., Collins, K., Dressing, C. D., Giacalone, S., Gill, H., Goliguzova, M. V., Ikoma, M., Jenkins, J. M., Tamura, M., Twicken, J. D., Ricker, G. R., Schwarz, R. P., Seager, S., Shporer, A., Vanderspek, R., and Winn, J.
Abstract: We report the discovery and validation of two TESS exoplanets orbiting faint M dwarfs: TOI-4479b and TOI-2081b. We have jointly analyzed space (TESS mission) and ground based (MuSCAT2, MuSCAT3 and SINISTRO instruments) lightcurves using our multi-color photometry transit analysis pipeline. This allowed us to compute contamination limits for both candidates and validate them as planet-sized companions. We found TOI-4479b to be a sub-Neptune-sized planet ($R_{p}=2.82^{+0.65}_{-0.63}~\rm R_{\oplus}$) and TOI-2081b to be a super-Earth-sized planet ($R_{p}=2.04^{+0.50}_{-0.54}~\rm R_{\oplus}$). Furthermore, we obtained that TOI-4479b, with a short orbital period of $1.15890^{+0.00002}_{-0.00001}~\rm days$, lies within the Neptune desert and is in fact the largest nearly ultra-short period planet around an M dwarf known to date. These results make TOI-4479b rare among the currently known exoplanet population around M dwarf stars, and an especially interesting target for spectroscopic follow-up and future studies of planet formation and evolution., Comment: Accepted for publication in Astronomy&Astrophysics
Published: 2022
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21. Confirmation and characterisation of three giant planets detected by TESS from the FIES/NOT and Tull/McDonald spectrographs

Author: Knudstrup, E., Serrano, L. M., Gandolfi, D., Albrecht, S. H., Cochran, W. D., Endl, M., Macqueen, P., Tronsgaard, R., Bieryla, A., Buchhave, Lars A., Stassun, K., Collins, K. A., Nowak, G., Deeg, H. J., Barkaoui, K., Safonov, B. S., Strakhov, I. A., Belinski, A. A., Twicken, J. D., Jenkins, J. M., Howard, A. W., Isaacson, H., Winn, J. N., Collins, K. I., Conti, D. M., Furesz, G., Gan, T., Kielkopf, John F., Massey, B., Murgas, F., Murphy, L. G., Palle, E., Quinn, S. N., Reed, P. A., Ricker, G. R., Seager, S., Shiao, B., Schwarz, R. P., Srdoc, G., Watanabe, D., Knudstrup, E., Serrano, L. M., Gandolfi, D., Albrecht, S. H., Cochran, W. D., Endl, M., Macqueen, P., Tronsgaard, R., Bieryla, A., Buchhave, Lars A., Stassun, K., Collins, K. A., Nowak, G., Deeg, H. J., Barkaoui, K., Safonov, B. S., Strakhov, I. A., Belinski, A. A., Twicken, J. D., Jenkins, J. M., Howard, A. W., Isaacson, H., Winn, J. N., Collins, K. I., Conti, D. M., Furesz, G., Gan, T., Kielkopf, John F., Massey, B., Murgas, F., Murphy, L. G., Palle, E., Quinn, S. N., Reed, P. A., Ricker, G. R., Seager, S., Shiao, B., Schwarz, R. P., Srdoc, G., and Watanabe, D.
Abstract: We report the confirmation and characterisation of TOI-1820~b, TOI-2025~b, and TOI-2158~b, three Jupiter-sized planets on short-period orbits around G-type stars detected by TESS. Through our ground-based efforts using the FIES and Tull spectrographs, we have confirmed these planets and characterised their orbits, and find periods of around $4.9$~d, $8.9$~d, and $8.6$~d for TOI-1820~b, TOI-2025~b, and TOI-2158~b, respectively. The sizes of the planets range from 0.96 to 1.14 Jupiter radii, and their masses are in the range from 0.8 to 4.4 Jupiter masses. For two of the systems, namely TOI-2025 and TOI-2158, we see a long-term trend in the radial velocities, indicating the presence of an outer companion in each of the two systems. For TOI-2025 we furthermore find the star to be well-aligned with the orbit, with a projected obliquity of $9^{+33}_{-31}$~$^\circ$. As these planets are all found in relatively bright systems (V$\sim$10.9-11.6 mag), they are well-suited for further studies, which could help shed light on the formation and migration of hot and warm Jupiters., Comment: Accepted for publication in A&A. 19 pages, 15 figures
Published: 2022
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22. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author: Oliveira, J. Marques, Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernández-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Pérez-Hoyos, S., Sánchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K. -L., Bode, H. -J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelínek, M., Štrobl, J., Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Pütz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J. -M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, G., Sanchez, R. Zanmar, Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Savio, R. Lo, Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., Abbeel, F. Van Den, André, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J. -P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J. -F., Metz, F., Erpelding, D., Nougayrède, P., Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Aissa, D. Baba, Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Reche, A. Román, Casanova, V., Briggs, E., Iglesias-Marzoa, R., Ibáñez, J. Abril, Martín, M. C. Díaz, González, H., García, J. L. Maestre, Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Gonçalves, R., Ferreira, M., Dias, F. Marques, Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., Moutamid, M. El, Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J. -P., Françoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Neilsen, G., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Oliveira, J. Marques, Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernández-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Pérez-Hoyos, S., Sánchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K. -L., Bode, H. -J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelínek, M., Štrobl, J., Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Pütz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J. -M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, G., Sanchez, R. Zanmar, Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Savio, R. Lo, Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., Abbeel, F. Van Den, André, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J. -P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J. -F., Metz, F., Erpelding, D., Nougayrède, P., Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Aissa, D. Baba, Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Reche, A. Román, Casanova, V., Briggs, E., Iglesias-Marzoa, R., Ibáñez, J. Abril, Martín, M. C. Díaz, González, H., García, J. L. Maestre, Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Gonçalves, R., Ferreira, M., Dias, F. Marques, Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., Moutamid, M. El, Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J. -P., Françoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Neilsen, G., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., and Downs, B.
Abstract: A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range $\sim$8 km to $\sim$190 km, corresponding to pressure levels from 9 {\mu}bar down to a few nanobars. Results. (i) A pressure of 1.18$\pm$0.03 {\mu}bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 {\mu}bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Comment: 52 pages, 26 figures in the main paper, 2 figures in appendix B, 9 figures in appendix C, 1 long table over 5 pages
Published: 2022
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23. TOI-1442 b and TOI-2445 b: two potentially rocky ultra-short period planets around M dwarfs

Author: Morello, G., Parviainen, H., Murgas, F., Pallé, E., Oshagh, M., Fukui, A., Hirano, T., Ishikawa, H. T., Mori, M., Narita, N., Collins, K. A., Barkaoui, K., Lewin, P., Cadieux, C., de Leon, J. P., Soubkiou, A., Garcia, N. Abreu, Crouzet, N., Esparza-Borges, E., Rodríguez, G. E. Fernández, Galán, D., Hori, Y., Ikoma, M., Isogai, K., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kotani, T., Krishnamurthy, V., Kurita, S., Laza-Ramos, A., Livingston, J. H., Luque, R., Madrigal-Aguado, A., Nishiumi, T., Orell-Miquel, J., Puig-Subirà, M., Sánchez-Benavente, M., Stangret, M., Tamura, M., Terada, Y., Watanabe, N., Zou, Y., Benkhaldoun, Z., Collins, K. I., Doyon, R., Garcia, L., Ghachoui, M., Gillon, M., Jehin, E., Pozuelos, F. J., Schwarz, R. P., Timmermans, M., Morello, G., Parviainen, H., Murgas, F., Pallé, E., Oshagh, M., Fukui, A., Hirano, T., Ishikawa, H. T., Mori, M., Narita, N., Collins, K. A., Barkaoui, K., Lewin, P., Cadieux, C., de Leon, J. P., Soubkiou, A., Garcia, N. Abreu, Crouzet, N., Esparza-Borges, E., Rodríguez, G. E. Fernández, Galán, D., Hori, Y., Ikoma, M., Isogai, K., Kagetani, T., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kotani, T., Krishnamurthy, V., Kurita, S., Laza-Ramos, A., Livingston, J. H., Luque, R., Madrigal-Aguado, A., Nishiumi, T., Orell-Miquel, J., Puig-Subirà, M., Sánchez-Benavente, M., Stangret, M., Tamura, M., Terada, Y., Watanabe, N., Zou, Y., Benkhaldoun, Z., Collins, K. I., Doyon, R., Garcia, L., Ghachoui, M., Gillon, M., Jehin, E., Pozuelos, F. J., Schwarz, R. P., and Timmermans, M.
Abstract: Context. Exoplanets with orbital periods of less than one day are known as ultra-short period (USP) planets. They are relatively rare products of planetary formation and evolution processes, but especially favourable for characterisation with current planet detection methods. At the time of writing, 125 USP planets have already been confirmed. Aims. Our aim is to validate the planetary nature of two new transiting planet candidates around M dwarfs announced by the NASA Transiting Exoplanet Survey Satellite (TESS), registered as TESS Objects of Interest (TOIs) TOI-1442.01 and TOI-2445.01. Methods. We used TESS data, ground-based photometric light curves, and Subaru/IRD spectrograph radial velocity (RV) measurements to validate both planetary candidates and to establish their physical properties. Results. TOI-1442 b is a validated exoplanet with an orbital period of $P$=0.4090682+/-0.0000004 d, a radius of $R_p$=1.15+/-0.06$R_{\oplus}$, and equilibrium temperature of $T_{p,eq}$=1357$_{-42}^{+49}$K. TOI-2445 b is also validated with an orbital period of $P$=0.3711286+/-0.0000004 d, a radius of $R_p$= 1.33+/-0.09$R_{\oplus}$, and equilibrium temperature of $T_{p,eq}$=1330$_{-56}^{+61}$K. Their physical properties align with current empirical trends and formation theories of USP planets. Based on the RV measurements, we set 3$\sigma$ upper mass limits of 8$M_{\oplus}$ and 20$M_{\oplus}$, thus confirming the non-stellar, sub-Jovian nature of both transiting objects. More RV measurements will be needed to constrain the planetary masses and mean densities, and the predicted presence of outer planetary companions. These targets extend the small sample of USP planets orbiting around M dwarfs up to 21 members. They are also among the 20 most suitable terrestrial planets for atmospheric characterisation via secondary eclipse with the JWST, according to a widespread emission spectroscopy metric., Comment: Published in A&A, 18 pages, 6 tables, 8 figures
Published: 2022
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24. A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266

Author: Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Demory, B-O, Pozuelos, FJ, Gómez Maqueo Chew, Y, Sabin, L, Petrucci, R, Schroffenegger, U, Grimm, SL, Sestovic, M, Gillon, M, McCormac, J, Barkaoui, K, Benz, W, Bieryla, A, Bouchy, F, Burdanov, A, Collins, KA, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Demory, B-O, Pozuelos, FJ, Gómez Maqueo Chew, Y, Sabin, L, Petrucci, R, Schroffenegger, U, Grimm, SL, Sestovic, M, Gillon, M, McCormac, J, Barkaoui, K, Benz, W, Bieryla, A, Bouchy, F, Burdanov, A, and Collins, KA
Published: 2021

25. Vetting of 384 TESS Objects of Interest with TRICERATOPS and Statistical Validation of 12 Planet Candidates

Author: Giacalone, S, Giacalone, S, Dressing, CD, Jensen, ELN, Collins, KA, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Barkaoui, K, Cadieux, C, Charbonneau, D, Collins, KI, Conti, DM, Doyon, R, Evans, P, Ghachoui, M, Gillon, M, Guerrero, NM, Hart, R, Jehin, E, Kielkopf, JF, McLean, B, Murgas, F, Palle, E, Parviainen, H, Pozuelos, FJ, Relles, HM, Shporer, A, Socia, Q, Stockdale, C, Tan, TG, Torres, G, Twicken, JD, Waalkes, WC, Waite, IA, Giacalone, S, Giacalone, S, Dressing, CD, Jensen, ELN, Collins, KA, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Barkaoui, K, Cadieux, C, Charbonneau, D, Collins, KI, Conti, DM, Doyon, R, Evans, P, Ghachoui, M, Gillon, M, Guerrero, NM, Hart, R, Jehin, E, Kielkopf, JF, McLean, B, Murgas, F, Palle, E, Parviainen, H, Pozuelos, FJ, Relles, HM, Shporer, A, Socia, Q, Stockdale, C, Tan, TG, Torres, G, Twicken, JD, Waalkes, WC, and Waite, IA
Abstract: We present TRICERATOPS, a new Bayesian tool that can be used to vet and validate TESS Objects of Interest (TOIs). We test the tool on 68 TOIs that have been previously confirmed as planets or rejected as astrophysical false positives. By looking in the false-positive probability (FPP)-nearby false-positive probability (NFPP) plane, we define criteria that TOIs must meet to be classified as validated planets (FPP < 0.015 and NFPP < 10-3), likely planets (FPP < 0.5 and NFPP < 10-3), and likely nearby false positives (NFPP > 10-1). We apply this procedure on 384 unclassified TOIs and statistically validate 12, classify 125 as likely planets, and classify 52 as likely nearby false positives. Of the 12 statistically validated planets, 9 are newly validated. TRICERATOPS is currently the only TESS vetting and validation tool that models transits from nearby contaminant stars in addition to the target star. We therefore encourage use of this tool to prioritize follow-up observations that confirm bona fide planets and identify false positives originating from nearby stars.
Published: 2021

26. HATS-74Ab, HATS-75b, HATS-76b and HATS-77b: Four Transiting Giant Planets around K and M Dwarfs

Author: Jordán, A., Hartman, J. D., Bayliss, D., Bakos, G. Á., Brahm, R., Bryant, E. M., Csubry, Z., Henning, Th., Hobson, M., Mancini, L., Penev, K., Rabus, M., Suc, V., de Val-Borro, M., Wallace, J., Barkaoui, K., Ciardi, D. R., Collins, K. A., Esparza-Borges, E., Furlan, E., Gan, T., Ghachoui, M., Gillon, M., Howell, S., Jehin, E., Fukui, A., Kawauchi, K., Livingston, J. H., Luque, R., Matson, R., Matthews, E. C., Osborn, H. P., Murgas, F., Palle, E., Waalkes, W. C., Jordán, A., Hartman, J. D., Bayliss, D., Bakos, G. Á., Brahm, R., Bryant, E. M., Csubry, Z., Henning, Th., Hobson, M., Mancini, L., Penev, K., Rabus, M., Suc, V., de Val-Borro, M., Wallace, J., Barkaoui, K., Ciardi, D. R., Collins, K. A., Esparza-Borges, E., Furlan, E., Gan, T., Ghachoui, M., Gillon, M., Howell, S., Jehin, E., Fukui, A., Kawauchi, K., Livingston, J. H., Luque, R., Matson, R., Matthews, E. C., Osborn, H. P., Murgas, F., Palle, E., and Waalkes, W. C.
Abstract: The relative rarity of giant planets around low mass stars compared with solar-type stars is a key prediction from core accretion planet formation theory. In this paper we report on the discovery of four gas giant planets that transit low mass late K and early M dwarfs. The planets HATS-74Ab (TOI 737b), HATS-75b (TOI 552b), HATS-76b (TOI 555b), and HATS-77b (TOI 730b), were all discovered from the HATSouth photometric survey and followed-up using TESS and other photometric facilities. We use the new ESPRESSO facility at the VLT to confirm and systems and measure their masses. We find that that planets have masses of 1.46 +- 0.14 MJ , 0.491 +- 0.039 MJ , 2.629 +- 0.089 MJ and 1.374 +0.100-0.074 MJ , respectively, and radii of 1.032 +- 0.021 RJ , 0.884 +- 0.013 RJ , 1.079 +- 0.031 RJ , and 1.165 +- 0.021 RJ, respectively. The planets all orbit close to their host stars with orbital periods ranging from 1.7319 d to 3.0876 d. With further work we aim to test core accretion theory by using these and further discoveries to quantify the occurrence rate of giant planets around low mass host stars., Comment: Accepted for publication in the Astronomical Journal
Published: 2021
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27. TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf

Author: Schanche, N., Pozuelos, F. J., Günther, M. N., Wells, R. D., Burgasser, A. J., Chinchilla, P., Delrez, L., Ducrot, E., Garcia, L. J., Chew, Y. Gómez Maqueo, Jofré, E., Rackham, B. V., Sebastian, D., Stassun, K. G., Stern, D., Timmermans, M., Barkaoui, K., Belinski, A., Benkhaldoun, Z., Benz, W., Charbonneau, D., Christiansen, Jessie L., Collins, Karen A., Demory, B. -O., Dévora-Pajares, M., de Wit, J., Dragomir, D., Dransfield, G., Furlan, E., Ghachou, M., Gillon, M., Gnilka, C., Gómez-Muñoz, M. A., Guerrero, N., Harris, M., Heng, K., Henze, C. E., Hesse, K., Howell, S. B., Jehin, E., Jenkins, J., Jensen, Eric L. N., Kunimoto, M., Latham, D. W., Lester, K., McLeod, Kim K., Mireles, I., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Quintana, E. V., Ricker, G., Rudat, A., Sabin, L., Safonov, B., Schroffenegger, U., Scott, N., Seager, S., Strakhov, I., Triaud, A. H. M. J., Vanderspek, R., Vezie, M., Winn, J., Schanche, N., Pozuelos, F. J., Günther, M. N., Wells, R. D., Burgasser, A. J., Chinchilla, P., Delrez, L., Ducrot, E., Garcia, L. J., Chew, Y. Gómez Maqueo, Jofré, E., Rackham, B. V., Sebastian, D., Stassun, K. G., Stern, D., Timmermans, M., Barkaoui, K., Belinski, A., Benkhaldoun, Z., Benz, W., Charbonneau, D., Christiansen, Jessie L., Collins, Karen A., Demory, B. -O., Dévora-Pajares, M., de Wit, J., Dragomir, D., Dransfield, G., Furlan, E., Ghachou, M., Gillon, M., Gnilka, C., Gómez-Muñoz, M. A., Guerrero, N., Harris, M., Heng, K., Henze, C. E., Hesse, K., Howell, S. B., Jehin, E., Jenkins, J., Jensen, Eric L. N., Kunimoto, M., Latham, D. W., Lester, K., McLeod, Kim K., Mireles, I., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Quintana, E. V., Ricker, G., Rudat, A., Sabin, L., Safonov, B., Schroffenegger, U., Scott, N., Seager, S., Strakhov, I., Triaud, A. H. M. J., Vanderspek, R., Vezie, M., and Winn, J.
Abstract: Thanks to the relative ease of finding and characterizing small planets around M dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs make such objects particularly compelling as they provide clues about the formation and evolution of these systems. In this study, we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit ($e \sim 0.5$), which would make it the most eccentric planet that is known to be transiting an M-dwarf star. We combined TESS and ground-based data obtained with the 1.0-m SAINT-EX, 0.60-m TRAPPIST-North and 1.2-m FLWO telescopes to find a planetary size of 2.2 $R_{\oplus}$ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. With its long period and high eccentricity, TOI-2257 b falls in a novel slice of parameter space. Despite the planet's low equilibrium temperature ($\sim$ 256 K), its host star's small size ($R_* = 0.311 \pm{0.015}$) and relative infrared brightness (K$_{mag}$ = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy., Comment: 18 pages, 12 figures, 2 appendices, Accepted for publication in Astronomy and Astrophysics
Published: 2021
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28. A large sub-Neptune transiting the thick-disk M4V TOI-2406

Author: Wells, R. D., Rackham, B. V., Schanche, N., Petrucci, R., Chew, Y. Gomez Maqueo, Demory, B. -O., Burgasser, A. J., Burn, R., Pozuelos, F. J., Gunther, M. N., Sabin, L., Schroffenegger, U., Gomez-Munoz, M. A., Stassun, K. G., Van Grootel, V., Howell, S. B., Sebastian, D., Triaud, A. H. M. J., Apai, D., Plauchu-Frayn, I., Guerrero, C. A., Guillen, P. F., Landa, A., Melgoza, G., Montalvo, F., Serrano, H., Riesgo, H., Barkaoui, K., Bixel, A., Burdanov, A., Chen, W. P., Chinchilla, P., Collins, K. A., Daylan, T., de Wit, J., Delrez, L., Devora-Pajares, M., Dietrich, J., Dransfield, G., Ducrot, E., Fausnaugh, M., Furlan, E., Gabor, P., Gan, T., Garcia, L., Ghachoui, M., Giacalone, S., Gibbs, A. B., Gillon, M., Gnilka, C., Gore, R., Guerrero, N., Henning, T., Hesse, K., Jehin, E., Jenkins, J. M., Latham, D. W., Lester, K., McCormac, J., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Ricker, G., Rodriguez, D. R., Schroeder, A., Schwarz, R. P., Scott, N., Seager, S., Theissen, C. A., Thompson, S., Timmermans, M., Twicken, J. D., Winn, J. N., Wells, R. D., Rackham, B. V., Schanche, N., Petrucci, R., Chew, Y. Gomez Maqueo, Demory, B. -O., Burgasser, A. J., Burn, R., Pozuelos, F. J., Gunther, M. N., Sabin, L., Schroffenegger, U., Gomez-Munoz, M. A., Stassun, K. G., Van Grootel, V., Howell, S. B., Sebastian, D., Triaud, A. H. M. J., Apai, D., Plauchu-Frayn, I., Guerrero, C. A., Guillen, P. F., Landa, A., Melgoza, G., Montalvo, F., Serrano, H., Riesgo, H., Barkaoui, K., Bixel, A., Burdanov, A., Chen, W. P., Chinchilla, P., Collins, K. A., Daylan, T., de Wit, J., Delrez, L., Devora-Pajares, M., Dietrich, J., Dransfield, G., Ducrot, E., Fausnaugh, M., Furlan, E., Gabor, P., Gan, T., Garcia, L., Ghachoui, M., Giacalone, S., Gibbs, A. B., Gillon, M., Gnilka, C., Gore, R., Guerrero, N., Henning, T., Hesse, K., Jehin, E., Jenkins, J. M., Latham, D. W., Lester, K., McCormac, J., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Ricker, G., Rodriguez, D. R., Schroeder, A., Schwarz, R. P., Scott, N., Seager, S., Theissen, C. A., Thompson, S., Timmermans, M., Twicken, J. D., and Winn, J. N.
Abstract: Large sub-Neptunes are uncommon around the coolest stars in the Galaxy and are rarer still around those that are metal-poor. However, owing to the large planet-to-star radius ratio, these planets are highly suitable for atmospheric study via transmission spectroscopy in the infrared, such as with JWST. Here we report the discovery and validation of a sub-Neptune orbiting the thick-disk, mid-M dwarf star TOI-2406. We first infer properties of the host star by analysing the star's near-infrared spectrum, spectral energy distribution, and Gaia parallax. We use multi-band photometry to confirm that the transit event is on-target and achromatic, and we statistically validate the TESS signal as a transiting exoplanet. We then determine physical properties of the planet through global transit modelling of the TESS and ground-based time-series data. We determine the host to be a metal-poor M4V star, located at a distance of 56 pc, with a sub-solar metallicity $(\mathrm{[Fe/H] = -0.38 \pm 0.07})$, and a member of the thick disk. The planet is a relatively large sub-Neptune for the M-dwarf planet population, with $\mathrm{R_p = 2.94 \pm 0.17} \mathrm{R_\oplus}$ and $\mathrm{P = 3.077}$ d, producing transits of 2% depth. We note the orbit has a non-zero eccentricity to 3$\mathrm{\sigma}$, prompting questions about the dynamical history of the system. This system is an interesting outcome of planet formation and presents a benchmark for large-planet formation around metal-poor, low-mass stars. The system warrants further study, in particular radial velocity follow-up to determine the planet mass and constrain possible bound companions. Furthermore, TOI-2406 b is a good target for future atmospheric study through transmission spectroscopy, particularly in the category of warm sub-Neptunes., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2021
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29. Massive search of spot- and facula-crossing events in 1598 exoplanetary transit lightcurves

Author: Baluev, R. V., Sokov, E. N., Sokova, I. A., Shaidulin, V. Sh., Veselova, A. V., Aitov, V. N., Mitiani, G. Sh., Valeev, A. F., Gadelshin, D. R., Gutaev, A. G., Beskin, G. M., Valyavin, G. G., Antonyuk, K., Barkaoui, K., Gillon, M., Jehin, E., Delrez, L., Guðmundsson, S., Dale, H. A., Fernández-Lajús, E., Di Sisto, R. P., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garlitz, J., Esseiva, N., Ogmen, Y., Bosch-Cabot, P., Selezneva, A., Hinse, T. C., Baluev, R. V., Sokov, E. N., Sokova, I. A., Shaidulin, V. Sh., Veselova, A. V., Aitov, V. N., Mitiani, G. Sh., Valeev, A. F., Gadelshin, D. R., Gutaev, A. G., Beskin, G. M., Valyavin, G. G., Antonyuk, K., Barkaoui, K., Gillon, M., Jehin, E., Delrez, L., Guðmundsson, S., Dale, H. A., Fernández-Lajús, E., Di Sisto, R. P., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garlitz, J., Esseiva, N., Ogmen, Y., Bosch-Cabot, P., Selezneva, A., and Hinse, T. C.
Abstract: We developed a dedicated statistical test for a massive detection of spot- and facula-crossing anomalies in multiple exoplanetary transit lightcurves, based on the frequentist $p$-value thresholding. This test was used to augment our algorithmic pipeline for transit lightcurves analysis. It was applied to $1598$ amateur and professional transit observations of $26$ targets being monitored in the EXPANSION project. We detected $109$ statistically significant candidate events revealing a roughly $2:1$ asymmetry in favor of spots-crossings over faculae-crossings. Although some candidate anomalies likely appear non-physical and originate from systematic errors, such asymmetry between negative and positive events should indicate a physical difference between the frequency of star spots and faculae. Detected spot-crossing events also reveal positive correlation between their amplitude and width, possibly owed to spot size correlation. However, the frequency of all detectable crossing events appears just about a few per cent, so they cannot explain excessive transit timing noise observed for several targets., Comment: 30 pages, 9 figures, 1 table; accepted by Acta Astronomica
Published: 2021
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30. Discovery of a Young Low-Mass Brown Dwarf Transiting a Fast-Rotating F-Type Star by the Galactic Plane eXoplanet (GPX) Survey

Author: Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., Henze, C. E., Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.
Abstract: We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of 19.7 ± 1.6 MJup and a radius of 1.47 ± 0.10 RJup, the first substellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright (V = 12.3 mag) fast-rotating F-type star with a projected rotational velocity v sin i∗ = 40 ± 10 km s−1. We use the isochrone placement algorithm to characterize the host star, which has effective temperature 7000 ± 200 K, mass 1.68 ± 0.10 M☉, radius 1.56 ± 0.10 R☉, and approximate age 0.27-0.15+0.09 Gyr. GPX-1 b has an orbital period of -1.75 d and a transit depth of 0.90 ± 0.03 per cent. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a substellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data are affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of the Doppler tomography. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Published: 2021

31. Vetting of 384 TESS Objects of Interest with TRICERATOPS and Statistical Validation of 12 Planet Candidates

Author: Giacalone, S, Giacalone, S, Dressing, CD, Jensen, ELN, Collins, KA, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Barkaoui, K, Cadieux, C, Charbonneau, D, Collins, KI, Conti, DM, Doyon, R, Evans, P, Ghachoui, M, Gillon, M, Guerrero, NM, Hart, R, Jehin, E, Kielkopf, JF, McLean, B, Murgas, F, Palle, E, Parviainen, H, Pozuelos, FJ, Relles, HM, Shporer, A, Socia, Q, Stockdale, C, Tan, TG, Torres, G, Twicken, JD, Waalkes, WC, Waite, IA, Giacalone, S, Giacalone, S, Dressing, CD, Jensen, ELN, Collins, KA, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Barkaoui, K, Cadieux, C, Charbonneau, D, Collins, KI, Conti, DM, Doyon, R, Evans, P, Ghachoui, M, Gillon, M, Guerrero, NM, Hart, R, Jehin, E, Kielkopf, JF, McLean, B, Murgas, F, Palle, E, Parviainen, H, Pozuelos, FJ, Relles, HM, Shporer, A, Socia, Q, Stockdale, C, Tan, TG, Torres, G, Twicken, JD, Waalkes, WC, and Waite, IA
Abstract: We present TRICERATOPS, a new Bayesian tool that can be used to vet and validate TESS Objects of Interest (TOIs). We test the tool on 68 TOIs that have been previously confirmed as planets or rejected as astrophysical false positives. By looking in the false-positive probability (FPP)-nearby false-positive probability (NFPP) plane, we define criteria that TOIs must meet to be classified as validated planets (FPP < 0.015 and NFPP < 10-3), likely planets (FPP < 0.5 and NFPP < 10-3), and likely nearby false positives (NFPP > 10-1). We apply this procedure on 384 unclassified TOIs and statistically validate 12, classify 125 as likely planets, and classify 52 as likely nearby false positives. Of the 12 statistically validated planets, 9 are newly validated. TRICERATOPS is currently the only TESS vetting and validation tool that models transits from nearby contaminant stars in addition to the target star. We therefore encourage use of this tool to prioritize follow-up observations that confirm bona fide planets and identify false positives originating from nearby stars.
Published: 2021

32. HATS-74Ab, HATS-75b, HATS-76b and HATS-77b: Four Transiting Giant Planets around K and M Dwarfs

Author: Jordán, A., Hartman, J. D., Bayliss, D., Bakos, G. Á., Brahm, R., Bryant, E. M., Csubry, Z., Henning, Th., Hobson, M., Mancini, L., Penev, K., Rabus, M., Suc, V., de Val-Borro, M., Wallace, J., Barkaoui, K., Ciardi, D. R., Collins, K. A., Esparza-Borges, E., Furlan, E., Gan, T., Ghachoui, M., Gillon, M., Howell, S., Jehin, E., Fukui, A., Kawauchi, K., Livingston, J. H., Luque, R., Matson, R., Matthews, E. C., Osborn, H. P., Murgas, F., Palle, E., Waalkes, W. C., Jordán, A., Hartman, J. D., Bayliss, D., Bakos, G. Á., Brahm, R., Bryant, E. M., Csubry, Z., Henning, Th., Hobson, M., Mancini, L., Penev, K., Rabus, M., Suc, V., de Val-Borro, M., Wallace, J., Barkaoui, K., Ciardi, D. R., Collins, K. A., Esparza-Borges, E., Furlan, E., Gan, T., Ghachoui, M., Gillon, M., Howell, S., Jehin, E., Fukui, A., Kawauchi, K., Livingston, J. H., Luque, R., Matson, R., Matthews, E. C., Osborn, H. P., Murgas, F., Palle, E., and Waalkes, W. C.
Abstract: The relative rarity of giant planets around low mass stars compared with solar-type stars is a key prediction from core accretion planet formation theory. In this paper we report on the discovery of four gas giant planets that transit low mass late K and early M dwarfs. The planets HATS-74Ab (TOI 737b), HATS-75b (TOI 552b), HATS-76b (TOI 555b), and HATS-77b (TOI 730b), were all discovered from the HATSouth photometric survey and followed-up using TESS and other photometric facilities. We use the new ESPRESSO facility at the VLT to confirm and systems and measure their masses. We find that that planets have masses of 1.46 +- 0.14 MJ , 0.491 +- 0.039 MJ , 2.629 +- 0.089 MJ and 1.374 +0.100-0.074 MJ , respectively, and radii of 1.032 +- 0.021 RJ , 0.884 +- 0.013 RJ , 1.079 +- 0.031 RJ , and 1.165 +- 0.021 RJ, respectively. The planets all orbit close to their host stars with orbital periods ranging from 1.7319 d to 3.0876 d. With further work we aim to test core accretion theory by using these and further discoveries to quantify the occurrence rate of giant planets around low mass host stars., Comment: Accepted for publication in the Astronomical Journal
Published: 2021
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33. TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf

Author: Schanche, N., Pozuelos, F. J., Günther, M. N., Wells, R. D., Burgasser, A. J., Chinchilla, P., Delrez, L., Ducrot, E., Garcia, L. J., Chew, Y. Gómez Maqueo, Jofré, E., Rackham, B. V., Sebastian, D., Stassun, K. G., Stern, D., Timmermans, M., Barkaoui, K., Belinski, A., Benkhaldoun, Z., Benz, W., Charbonneau, D., Christiansen, Jessie L., Collins, Karen A., Demory, B. -O., Dévora-Pajares, M., de Wit, J., Dragomir, D., Dransfield, G., Furlan, E., Ghachou, M., Gillon, M., Gnilka, C., Gómez-Muñoz, M. A., Guerrero, N., Harris, M., Heng, K., Henze, C. E., Hesse, K., Howell, S. B., Jehin, E., Jenkins, J., Jensen, Eric L. N., Kunimoto, M., Latham, D. W., Lester, K., McLeod, Kim K., Mireles, I., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Quintana, E. V., Ricker, G., Rudat, A., Sabin, L., Safonov, B., Schroffenegger, U., Scott, N., Seager, S., Strakhov, I., Triaud, A. H. M. J., Vanderspek, R., Vezie, M., Winn, J., Schanche, N., Pozuelos, F. J., Günther, M. N., Wells, R. D., Burgasser, A. J., Chinchilla, P., Delrez, L., Ducrot, E., Garcia, L. J., Chew, Y. Gómez Maqueo, Jofré, E., Rackham, B. V., Sebastian, D., Stassun, K. G., Stern, D., Timmermans, M., Barkaoui, K., Belinski, A., Benkhaldoun, Z., Benz, W., Charbonneau, D., Christiansen, Jessie L., Collins, Karen A., Demory, B. -O., Dévora-Pajares, M., de Wit, J., Dragomir, D., Dransfield, G., Furlan, E., Ghachou, M., Gillon, M., Gnilka, C., Gómez-Muñoz, M. A., Guerrero, N., Harris, M., Heng, K., Henze, C. E., Hesse, K., Howell, S. B., Jehin, E., Jenkins, J., Jensen, Eric L. N., Kunimoto, M., Latham, D. W., Lester, K., McLeod, Kim K., Mireles, I., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Quintana, E. V., Ricker, G., Rudat, A., Sabin, L., Safonov, B., Schroffenegger, U., Scott, N., Seager, S., Strakhov, I., Triaud, A. H. M. J., Vanderspek, R., Vezie, M., and Winn, J.
Abstract: Thanks to the relative ease of finding and characterizing small planets around M dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs make such objects particularly compelling as they provide clues about the formation and evolution of these systems. In this study, we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit ($e \sim 0.5$), which would make it the most eccentric planet that is known to be transiting an M-dwarf star. We combined TESS and ground-based data obtained with the 1.0-m SAINT-EX, 0.60-m TRAPPIST-North and 1.2-m FLWO telescopes to find a planetary size of 2.2 $R_{\oplus}$ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. With its long period and high eccentricity, TOI-2257 b falls in a novel slice of parameter space. Despite the planet's low equilibrium temperature ($\sim$ 256 K), its host star's small size ($R_* = 0.311 \pm{0.015}$) and relative infrared brightness (K$_{mag}$ = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy., Comment: 18 pages, 12 figures, 2 appendices, Accepted for publication in Astronomy and Astrophysics
Published: 2021
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34. A large sub-Neptune transiting the thick-disk M4V TOI-2406

Author: Wells, R. D., Rackham, B. V., Schanche, N., Petrucci, R., Chew, Y. Gomez Maqueo, Demory, B. -O., Burgasser, A. J., Burn, R., Pozuelos, F. J., Gunther, M. N., Sabin, L., Schroffenegger, U., Gomez-Munoz, M. A., Stassun, K. G., Van Grootel, V., Howell, S. B., Sebastian, D., Triaud, A. H. M. J., Apai, D., Plauchu-Frayn, I., Guerrero, C. A., Guillen, P. F., Landa, A., Melgoza, G., Montalvo, F., Serrano, H., Riesgo, H., Barkaoui, K., Bixel, A., Burdanov, A., Chen, W. P., Chinchilla, P., Collins, K. A., Daylan, T., de Wit, J., Delrez, L., Devora-Pajares, M., Dietrich, J., Dransfield, G., Ducrot, E., Fausnaugh, M., Furlan, E., Gabor, P., Gan, T., Garcia, L., Ghachoui, M., Giacalone, S., Gibbs, A. B., Gillon, M., Gnilka, C., Gore, R., Guerrero, N., Henning, T., Hesse, K., Jehin, E., Jenkins, J. M., Latham, D. W., Lester, K., McCormac, J., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Ricker, G., Rodriguez, D. R., Schroeder, A., Schwarz, R. P., Scott, N., Seager, S., Theissen, C. A., Thompson, S., Timmermans, M., Twicken, J. D., Winn, J. N., Wells, R. D., Rackham, B. V., Schanche, N., Petrucci, R., Chew, Y. Gomez Maqueo, Demory, B. -O., Burgasser, A. J., Burn, R., Pozuelos, F. J., Gunther, M. N., Sabin, L., Schroffenegger, U., Gomez-Munoz, M. A., Stassun, K. G., Van Grootel, V., Howell, S. B., Sebastian, D., Triaud, A. H. M. J., Apai, D., Plauchu-Frayn, I., Guerrero, C. A., Guillen, P. F., Landa, A., Melgoza, G., Montalvo, F., Serrano, H., Riesgo, H., Barkaoui, K., Bixel, A., Burdanov, A., Chen, W. P., Chinchilla, P., Collins, K. A., Daylan, T., de Wit, J., Delrez, L., Devora-Pajares, M., Dietrich, J., Dransfield, G., Ducrot, E., Fausnaugh, M., Furlan, E., Gabor, P., Gan, T., Garcia, L., Ghachoui, M., Giacalone, S., Gibbs, A. B., Gillon, M., Gnilka, C., Gore, R., Guerrero, N., Henning, T., Hesse, K., Jehin, E., Jenkins, J. M., Latham, D. W., Lester, K., McCormac, J., Murray, C. A., Niraula, P., Pedersen, P. P., Queloz, D., Ricker, G., Rodriguez, D. R., Schroeder, A., Schwarz, R. P., Scott, N., Seager, S., Theissen, C. A., Thompson, S., Timmermans, M., Twicken, J. D., and Winn, J. N.
Abstract: Large sub-Neptunes are uncommon around the coolest stars in the Galaxy and are rarer still around those that are metal-poor. However, owing to the large planet-to-star radius ratio, these planets are highly suitable for atmospheric study via transmission spectroscopy in the infrared, such as with JWST. Here we report the discovery and validation of a sub-Neptune orbiting the thick-disk, mid-M dwarf star TOI-2406. We first infer properties of the host star by analysing the star's near-infrared spectrum, spectral energy distribution, and Gaia parallax. We use multi-band photometry to confirm that the transit event is on-target and achromatic, and we statistically validate the TESS signal as a transiting exoplanet. We then determine physical properties of the planet through global transit modelling of the TESS and ground-based time-series data. We determine the host to be a metal-poor M4V star, located at a distance of 56 pc, with a sub-solar metallicity $(\mathrm{[Fe/H] = -0.38 \pm 0.07})$, and a member of the thick disk. The planet is a relatively large sub-Neptune for the M-dwarf planet population, with $\mathrm{R_p = 2.94 \pm 0.17} \mathrm{R_\oplus}$ and $\mathrm{P = 3.077}$ d, producing transits of 2% depth. We note the orbit has a non-zero eccentricity to 3$\mathrm{\sigma}$, prompting questions about the dynamical history of the system. This system is an interesting outcome of planet formation and presents a benchmark for large-planet formation around metal-poor, low-mass stars. The system warrants further study, in particular radial velocity follow-up to determine the planet mass and constrain possible bound companions. Furthermore, TOI-2406 b is a good target for future atmospheric study through transmission spectroscopy, particularly in the category of warm sub-Neptunes., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2021
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35. Massive search of spot- and facula-crossing events in 1598 exoplanetary transit lightcurves

Author: Baluev, R. V., Sokov, E. N., Sokova, I. A., Shaidulin, V. Sh., Veselova, A. V., Aitov, V. N., Mitiani, G. Sh., Valeev, A. F., Gadelshin, D. R., Gutaev, A. G., Beskin, G. M., Valyavin, G. G., Antonyuk, K., Barkaoui, K., Gillon, M., Jehin, E., Delrez, L., Guðmundsson, S., Dale, H. A., Fernández-Lajús, E., Di Sisto, R. P., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garlitz, J., Esseiva, N., Ogmen, Y., Bosch-Cabot, P., Selezneva, A., Hinse, T. C., Baluev, R. V., Sokov, E. N., Sokova, I. A., Shaidulin, V. Sh., Veselova, A. V., Aitov, V. N., Mitiani, G. Sh., Valeev, A. F., Gadelshin, D. R., Gutaev, A. G., Beskin, G. M., Valyavin, G. G., Antonyuk, K., Barkaoui, K., Gillon, M., Jehin, E., Delrez, L., Guðmundsson, S., Dale, H. A., Fernández-Lajús, E., Di Sisto, R. P., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garlitz, J., Esseiva, N., Ogmen, Y., Bosch-Cabot, P., Selezneva, A., and Hinse, T. C.
Abstract: We developed a dedicated statistical test for a massive detection of spot- and facula-crossing anomalies in multiple exoplanetary transit lightcurves, based on the frequentist $p$-value thresholding. This test was used to augment our algorithmic pipeline for transit lightcurves analysis. It was applied to $1598$ amateur and professional transit observations of $26$ targets being monitored in the EXPANSION project. We detected $109$ statistically significant candidate events revealing a roughly $2:1$ asymmetry in favor of spots-crossings over faculae-crossings. Although some candidate anomalies likely appear non-physical and originate from systematic errors, such asymmetry between negative and positive events should indicate a physical difference between the frequency of star spots and faculae. Detected spot-crossing events also reveal positive correlation between their amplitude and width, possibly owed to spot size correlation. However, the frequency of all detectable crossing events appears just about a few per cent, so they cannot explain excessive transit timing noise observed for several targets., Comment: 30 pages, 9 figures, 1 table; accepted by Acta Astronomica
Published: 2021
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36. A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266

Author: Demory, B-O, Demory, B-O, Pozuelos, FJ, Chew, Y Gómez Maqueo, Sabin, L, Petrucci, R, Schroffenegger, U, Grimm, SL, Sestovic, M, Gillon, M, McCormac, J, Barkaoui, K, Benz, W, Bieryla, A, Bouchy, F, Burdanov, A, Collins, KA, de Wit, J, Dressing, CD, Garcia, LJ, Giacalone, S, Guerra, P, Haldemann, J, Heng, K, Jehin, E, Jofré, E, Kane, SR, Lillo-Box, J, Maigné, V, Mordasini, C, Morris, BM, Niraula, P, Queloz, D, Rackham, BV, Savel, AB, Soubkiou, A, Srdoc, G, Stassun, KG, Triaud, AHMJ, Zambelli, R, Ricker, G, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Calvario-Velásquez, T, Herrera, JA Franco, Colorado, E, Zepeda, EO Cadena, Figueroa, L, Watson, AM, Lugo-Ibarra, EE, Carigi, L, Guisa, G, Herrera, J, Díaz, G Sierra, Suárez, JC, Barrado, D, Batalha, NM, Benkhaldoun, Z, Chontos, A, Dai, F, Essack, Z, Ghachoui, M, Huang, CX, Huber, D, Isaacson, H, Lissauer, JJ, Morales-Calderón, M, Robertson, P, Roy, A, Twicken, JD, Vanderburg, A, Weiss, LM, Demory, B-O, Demory, B-O, Pozuelos, FJ, Chew, Y Gómez Maqueo, Sabin, L, Petrucci, R, Schroffenegger, U, Grimm, SL, Sestovic, M, Gillon, M, McCormac, J, Barkaoui, K, Benz, W, Bieryla, A, Bouchy, F, Burdanov, A, Collins, KA, de Wit, J, Dressing, CD, Garcia, LJ, Giacalone, S, Guerra, P, Haldemann, J, Heng, K, Jehin, E, Jofré, E, Kane, SR, Lillo-Box, J, Maigné, V, Mordasini, C, Morris, BM, Niraula, P, Queloz, D, Rackham, BV, Savel, AB, Soubkiou, A, Srdoc, G, Stassun, KG, Triaud, AHMJ, Zambelli, R, Ricker, G, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Calvario-Velásquez, T, Herrera, JA Franco, Colorado, E, Zepeda, EO Cadena, Figueroa, L, Watson, AM, Lugo-Ibarra, EE, Carigi, L, Guisa, G, Herrera, J, Díaz, G Sierra, Suárez, JC, Barrado, D, Batalha, NM, Benkhaldoun, Z, Chontos, A, Dai, F, Essack, Z, Ghachoui, M, Huang, CX, Huber, D, Isaacson, H, Lissauer, JJ, Morales-Calderón, M, Robertson, P, Roy, A, Twicken, JD, Vanderburg, A, and Weiss, LM
Published: 2020

37. Discovery of a pre-cataclysmic binary with unusual chromaticity of the eclipsed white dwarf by the GPX survey

Author: Krushinsky, V., Benni, P., Burdanov, A., Antokhin, I., Antokhina, E., Jehin, E., Barkaoui, K., Fitzsimmons, A., Gibson, C., Gillon, M., Popov, A., Baştürk, Ö., Benkhaldoun, Z., Marchini, A., Papini, R., Salvaggio, F., Brazhko, V., Krushinsky, V., Benni, P., Burdanov, A., Antokhin, I., Antokhina, E., Jehin, E., Barkaoui, K., Fitzsimmons, A., Gibson, C., Gillon, M., Popov, A., Baştürk, Ö., Benkhaldoun, Z., Marchini, A., Papini, R., Salvaggio, F., and Brazhko, V.
Abstract: We report the discovery of a relatively bright eclipsing binary system, which consists of a white dwarf (WD) and a main-sequence K7 star with clear signs of chromospheric and spot activity. The light curve of this system shows ∼0.2 mag ellipsoidal variability with a period of 0.297549 d and a short total eclipse of the WD. Based on our analysis of the spectral and photometric data, we estimated the parameters of the system. The K7V star is tidally deformed but does not fill its Roche lobe (the filling factor is about 0.86). The orbital inclination is i = 73◦.1 ± 0◦.2, and the mass ratio is q = M2/M1 ≈ 0.88. The parameters of the K7V star are M2 ≈ 0.64 M☉, R2 = 0.645 ± 0.012R☉, and T2 ≈ 4070 K. The parameters of the WD are M1 ≈ 0.72 M☉, R1 = 0.013 ± 0.003R☉, and T1 = 8700 ± 1100 K. Photometric observations in different bands revealed that the maximum depth of the eclipse is in the SDSS r filter, which is unusual for a system of a WD and a late main-sequence star. We suspect that this system is a product of the evolution of a common-envelope binary star, and that the WD accretes the stellar wind from the secondary star (the so-called low-accretion-rate polar, hereafter LARP). © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Published: 2020

38. Two transiting hot Jupiters from the WASP survey: WASP-150b and WASP-176b

Author: Cooke, Benjamin F., Pollacco, Don, Almleaky, Y., Barkaoui, K., Benkhaldoun, Z., Blake, James A., Bouchy, François, Boumis, Panos, Brown, D. J. A., Bruni, Ivan, Burdanov, A., Cameron, Andrew Collier, Chote, Paul, Daassou, A., D'ago, Giuseppe, Dalal, Shweta, Damasso, Mario, Delrez, L., Doyle, A. P., Ducrot, E., Gillon, M., Hébrard, G., Hellier, C., Henning, Thomas, Jehin, E., Kiefer, Flavien, King, George W., Liakos, Alexios, Lopez, Théo, Mancini, Luigi, Mardling, Rosemary, Maxted, P. F. L., McCormac, James, Murray, C., Nielsen, Louise D., Osborn, Hugh, Palle, E., Pepe, Francesco, Pozuelos, F. J., Prieto-Arranz, J., Queloz, D., Schanche, Nicole, Ségransan, Damien, Smalley, Barry, Southworth, John, Thompson, S., Turner, Oliver, Udry, Stéphane, Velasco, S., West, Richard, Wheatley, Pete, Alikakos, John, Cooke, Benjamin F., Pollacco, Don, Almleaky, Y., Barkaoui, K., Benkhaldoun, Z., Blake, James A., Bouchy, François, Boumis, Panos, Brown, D. J. A., Bruni, Ivan, Burdanov, A., Cameron, Andrew Collier, Chote, Paul, Daassou, A., D'ago, Giuseppe, Dalal, Shweta, Damasso, Mario, Delrez, L., Doyle, A. P., Ducrot, E., Gillon, M., Hébrard, G., Hellier, C., Henning, Thomas, Jehin, E., Kiefer, Flavien, King, George W., Liakos, Alexios, Lopez, Théo, Mancini, Luigi, Mardling, Rosemary, Maxted, P. F. L., McCormac, James, Murray, C., Nielsen, Louise D., Osborn, Hugh, Palle, E., Pepe, Francesco, Pozuelos, F. J., Prieto-Arranz, J., Queloz, D., Schanche, Nicole, Ségransan, Damien, Smalley, Barry, Southworth, John, Thompson, S., Turner, Oliver, Udry, Stéphane, Velasco, S., West, Richard, Wheatley, Pete, and Alikakos, John
Abstract: We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric ($e$ = 0.38) hot Jupiter on a 5.6 day orbit around a $V$ = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4 $\rm M_{\odot}$ and 1.7 $\rm R_{\odot}$ respectively. WASP-150b has a mass and radius of 8.5 $\rm M_J$ and 1.1 $\rm R_J$, leading to a large planetary bulk density of 6.4 $\rm \rho_J$. WASP-150b is found to be $\sim3$ Gyr old, well below its circularisation timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a $V$ = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 $\rm M_{\odot}$ and 1.9 $\rm R_{\odot}$. WASP-176b has a mass and radius of 0.86 $\rm M_J$ and 1.5 $\rm R_J$ respectively, leading to a planetary bulk density of 0.23 $\rm \rho_J$., Comment: 15 pages, 14 figures. Accepted for publication in The Astronomical Journal
Published: 2020
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39. 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., Zohrabi, F., 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.
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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40. Three Short Period Jupiters from TESS

Author: Nielsen, L. D., Brahm, R., Bouchy, F., Espinoza, N., Turner, O., Rappaport, S., Pearce, L., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Acton, J. S., Bakos, G., Barclay, T., Barkaoui, K., Bhatti, W., Briceño, C., Bryant, E. M., Burleigh, M. R., Ciardi, D. R., Collins, K. A., Collins, K. I., Cooke, B. F., Csubry, Z., Santos, L. A. dos, Eigmüller, Ph., Fausnaugh, M. M., Gan, T., Gillon, M., Goad, M. R., Guerrero, N., Hagelberg, J., Hart, R., Henning, T., Huang, C. X., Jehin, E., Jenkins, J. S., Jordàn, A., Kielkopf, J. F., Kossakowski, D., Lavie, B., Law, N., Lendl, M., de Leon, J. P., Lovis, C., Mann, A. W., Marmier, M., McCormac, J., Mori, M., Moyano, M., Narita, N., Osip, D., Otegi, J. F., Pepe, F., Pozuelos, F. J., Raynard, L., Relles, H. M., Sarkis, P., Segransan, D., Seidel, J. V., Shporer, A., Stalport, M., Stockdale, C., Suc, V., Tamura, M., Tan, T. G., Tilbrook, R. H., Ting, E. B., Trifonov, T., Udry, S., Vanderburg, A., Wheatley, P. J., Wingham, G., Zhan, Z., Ziegler, C., Nielsen, L. D., Brahm, R., Bouchy, F., Espinoza, N., Turner, O., Rappaport, S., Pearce, L., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Acton, J. S., Bakos, G., Barclay, T., Barkaoui, K., Bhatti, W., Briceño, C., Bryant, E. M., Burleigh, M. R., Ciardi, D. R., Collins, K. A., Collins, K. I., Cooke, B. F., Csubry, Z., Santos, L. A. dos, Eigmüller, Ph., Fausnaugh, M. M., Gan, T., Gillon, M., Goad, M. R., Guerrero, N., Hagelberg, J., Hart, R., Henning, T., Huang, C. X., Jehin, E., Jenkins, J. S., Jordàn, A., Kielkopf, J. F., Kossakowski, D., Lavie, B., Law, N., Lendl, M., de Leon, J. P., Lovis, C., Mann, A. W., Marmier, M., McCormac, J., Mori, M., Moyano, M., Narita, N., Osip, D., Otegi, J. F., Pepe, F., Pozuelos, F. J., Raynard, L., Relles, H. M., Sarkis, P., Segransan, D., Seidel, J. V., Shporer, A., Stalport, M., Stockdale, C., Suc, V., Tamura, M., Tan, T. G., Tilbrook, R. H., Ting, E. B., Trifonov, T., Udry, S., Vanderburg, A., Wheatley, P. J., Wingham, G., Zhan, Z., and Ziegler, C.
Abstract: We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V=11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 Mjup planet in a grazing transit configuration with an impact parameter of b = 1.17 +0.10/-0.08. As a result the radius is poorly constrained, 2.03 +0.61/-0.49 Rjup. The planet's distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs' = 10^7 - 10^9. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 +/- 0.13 Mjup and a radius of 1.29 +/- 0.02 Rjup. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V=12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V=12.4 G-type star. It has a mass of 0.79 +/- 0.06 Mjup and a radius of 1.09 +0.08/-0.05 Rjup. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe/H] ranging from 0.18 - 0.24., Comment: Published in A&A
Published: 2020
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41. HATS-47b, HATS-48Ab, HATS-49b and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs

Author: Hartman, J. D., Jordán, Andrés, Bayliss, D., Bakos, G. Á., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., Henning, Th., Mancini, L., Penev, K., Rabus, M., Sarkis, P., Suc, V., de Val-Borro, M., Zhou, G., Crane, J. D., Shectman, S., Teske, J. K., Wang, S. X., Butler, R. P., Lázár, J., Papp, I., Sári, P., Anderson, D. R., Hellier, C., West, R. G., Barkaoui, K., Pozuelos, F. J., Jehin, E., Gillon, M., Nielsen, L., Lendl, M., Udry, S., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Christiansen, Jessie, Crossfield, Ian J. M., Henze, Christopher E., Jenkins, Jon M., Smith, Jeffrey C., Ting, Eric B., Hartman, J. D., Jordán, Andrés, Bayliss, D., Bakos, G. Á., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., Henning, Th., Mancini, L., Penev, K., Rabus, M., Sarkis, P., Suc, V., de Val-Borro, M., Zhou, G., Crane, J. D., Shectman, S., Teske, J. K., Wang, S. X., Butler, R. P., Lázár, J., Papp, I., Sári, P., Anderson, D. R., Hellier, C., West, R. G., Barkaoui, K., Pozuelos, F. J., Jehin, E., Gillon, M., Nielsen, L., Lendl, M., Udry, S., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Christiansen, Jessie, Crossfield, Ian J. M., Henze, Christopher E., Jenkins, Jon M., Smith, Jeffrey C., and Ting, Eric B.
Abstract: We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have masses of $0.369_{-0.021}^{+0.031}$ $M_{J}$, $0.243_{-0.030}^{+0.022}$ $M_{J}$, $0.353_{-0.027}^{+0.038}$ $M_{J}$ and $0.1254\pm0.0039$ $M_{J}$, respectively, and radii of $1.117\pm0.014$ $R_{J}$, $0.800\pm0.015$ $R_{J}$, $0.765\pm0.013$ $R_{J}$, and $0.7224\pm0.0032$ $R_{J}$, respectively. The planets orbit close to their host stars with orbital periods of $3.9228$ d, $3.1317$ d, $4.1480$ d and $7.3279$ d, respectively. The hosts are main sequence K dwarfs with masses of $0.674_{-0.012}^{+0.016}$ $M_{\odot}$, $0.7279\pm0.0066$ $M_{\odot}$, $0.7133\pm0.0075$ $M_{\odot}$, and $0.7311\pm0.0028$ $M_{\odot}$ and with $V$-band magnitudes of $V = 14.829\pm0.010$, $14.35\pm0.11$, $14.998\pm0.040$ and $12.469\pm0.010$. The Super-Neptune HATS-72b (a.k.a.\ WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI 1073.01), HATS-48A and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved $5.\!\!^{\prime\prime}4$ neighbor in Gaia~DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of $0.22$ $M_{\odot}$ and a current projected physical separation of $\sim$1,400 au., Comment: Accepted for publication in AJ. 32 pages, 14 figures, 7 tables
Published: 2020
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42. The CARMENES search for exoplanets around M dwarfs -- LP 714-47b (TOI 442.01): Populating the Neptune desert

Author: Dreizler, S., I., J., Crossfield, M., Kossakowski, D., Plavchan, P., S., Jeffers, V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., Caballero, A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., M., Osorio, R. Zapatero, Chaturvedi, P., A., Hatzes, P., Ricker, G., Vanderspek, R., D., Latham, W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., P., Amado, J., Barkaoui, K., Barbieri, M., N., Batalha, M., F., Bauer, F., Benneke, B., Benkhaldoun, Z., C, Beichman, Berberian, J., Burt, J., R., Butler, P., Caldwell, A., Chintada, A., Chontos, A., Christiansen, L., Ciardi, D. R., Cifuentes, C., K., Collins, A., Collins, I., Combs, D., Cortés-Contreras, M., Crane, D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., E., Flowers, E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., Howard, W., Howell, S., Huber, D., Isaacson, H., Jehin, E., L., Jensen, N., Kaminski, A., Kane, R., Kawauchi, K., Kielkopf, F., Klahr, H., Kosiarek, R., Kreidberg, L., Kürster, Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., Matson, A., Mocnik, T., Morales, C., Muirhead, S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., V., Passegger, M., Pollacco, D., Pozuelos, J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., Rose, E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., H., Şenavcı, V., Teske, J., Twicken, D., Villasenor, J., Wang, S. X., Weiss, M., Wittrock, J., Yılmaz, M., Zohrabi, F., Dreizler, S., I., J., Crossfield, M., Kossakowski, D., Plavchan, P., S., Jeffers, V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., Caballero, A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., M., Osorio, R. Zapatero, Chaturvedi, P., A., Hatzes, P., Ricker, G., Vanderspek, R., D., Latham, W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., P., Amado, J., Barkaoui, K., Barbieri, M., N., Batalha, M., F., Bauer, F., Benneke, B., Benkhaldoun, Z., C, Beichman, Berberian, J., Burt, J., R., Butler, P., Caldwell, A., Chintada, A., Chontos, A., Christiansen, L., Ciardi, D. R., Cifuentes, C., K., Collins, A., Collins, I., Combs, D., Cortés-Contreras, M., Crane, D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., E., Flowers, E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., Howard, W., Howell, S., Huber, D., Isaacson, H., Jehin, E., L., Jensen, N., Kaminski, A., Kane, R., Kawauchi, K., Kielkopf, F., Klahr, H., Kosiarek, R., Kreidberg, L., Kürster, Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., Matson, A., Mocnik, T., Morales, C., Muirhead, S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., V., Passegger, M., Pollacco, D., Pozuelos, J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., Rose, E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., H., Şenavcı, V., Teske, J., Twicken, D., Villasenor, J., Wang, S. X., Weiss, M., Wittrock, J., Yılmaz, M., and Zohrabi, F.
Abstract: We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, m_b = 30.8 +/- 1.5 M_earth , R_b = 4.7 +/- 0.3 R_earth ) located in the 'hot Neptune desert'. Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST- South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TUBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (T_eff = 3950 +/- 51 K) with a mass of 0.59 +/- 0.02 M_sun and a radius of 0.58 +/- 0.02 R_sun. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained., Comment: Accepted for publication in A&A. 24 pages, 21 figures, 5 tables
Published: 2020
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43. Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Author: Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštienė, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Horta, F. Grau, Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., Henze, C. E., Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštienė, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Horta, F. Grau, Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.
Abstract: We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of $19.7\pm 1.6$ $M_{\mathrm{Jup}}$ and a radius of $1.47\pm0.10$ $R_{\mathrm{Jup}}$, the first sub-stellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright ($V$ = 12.3 mag) fast-rotating F-type star with a projected rotational velocity $v\sin{ i_*}=40\pm10$ km/s. We use the isochrone placement algorithm to characterize the host star, which has effective temperature $7000\pm200$ K, mass $1.68\pm0.10$ $M_{\mathrm{Sun}}$, radius $1.56\pm0.10$ $R_{\mathrm{Sun}}$ and approximate age $0.27_{-0.15}^{+0.09}$ Gyr. GPX-1 b has an orbital period of $\sim$1.75 d, and a transit depth of $0.90\pm0.03$ %. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a sub-stellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data is affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of Doppler tomography., Comment: 13 pages, 13 figures, accepted to MNRAS in May 2021
Published: 2020
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44. A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266

Author: Demory, B. -O., Pozuelos, F. J., Chew, Y. Gomez Maqueo, Sabin, L., Petrucci, R., Schroffenegger, U., Grimm, S. L., Sestovic, M., Gillon, M., McCormac, J., Barkaoui, K., Benz, W., Bieryla, A., Bouchy, F., Burdanov, A., Collins, K. A., de Wit, J., Dressing, C. D., Garcia, L. J., Giacalone, S., Guerra, P., Haldemann, J., Heng, K., Jehin, E., Jofre, E., Kane, S. R., Lillo-Box, J., Maigne, V., Mordasini, C., Morris, B. M., Niraula, P., Queloz, D., Rackham, B. V., Savel, A. B., Soubkiou, A., Srdoc, G., Stassun, K. G., Triaud, A. H. M. J., Zambelli, R., Ricker, G., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Calvario-Velasquez, T., Herrera, J. A. Franco, Colorado, E., Zepeda, E. O. Cadena, Figueroa, L., Watson, A. M., Lugo-Ibarra, E. E., Carigi, L., Guisa, G., Herrera, J., Diaz, G. Sierra, Suarez, J. C., Barrado, D., Batalha, N. M., Benkhaldoun, Z., Chontos, A., Dai, F., Essack, Z., Ghachoui, M., Huang, C. X., Huber, D., Isaacson, H., Lissauer, J. J., Morales-Calderon, M., Robertson, P., Roy, A., Twicken, J. D., Vanderburg, A., Weiss, L. M., Demory, B. -O., Pozuelos, F. J., Chew, Y. Gomez Maqueo, Sabin, L., Petrucci, R., Schroffenegger, U., Grimm, S. L., Sestovic, M., Gillon, M., McCormac, J., Barkaoui, K., Benz, W., Bieryla, A., Bouchy, F., Burdanov, A., Collins, K. A., de Wit, J., Dressing, C. D., Garcia, L. J., Giacalone, S., Guerra, P., Haldemann, J., Heng, K., Jehin, E., Jofre, E., Kane, S. R., Lillo-Box, J., Maigne, V., Mordasini, C., Morris, B. M., Niraula, P., Queloz, D., Rackham, B. V., Savel, A. B., Soubkiou, A., Srdoc, G., Stassun, K. G., Triaud, A. H. M. J., Zambelli, R., Ricker, G., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Calvario-Velasquez, T., Herrera, J. A. Franco, Colorado, E., Zepeda, E. O. Cadena, Figueroa, L., Watson, A. M., Lugo-Ibarra, E. E., Carigi, L., Guisa, G., Herrera, J., Diaz, G. Sierra, Suarez, J. C., Barrado, D., Batalha, N. M., Benkhaldoun, Z., Chontos, A., Dai, F., Essack, Z., Ghachoui, M., Huang, C. X., Huber, D., Isaacson, H., Lissauer, J. J., Morales-Calderon, M., Robertson, P., Roy, A., Twicken, J. D., Vanderburg, A., and Weiss, L. M.
Abstract: We report the discovery and characterisation of a super-Earth and a sub-Neptune transiting the bright ($K=8.8$), quiet, and nearby (37 pc) M3V dwarf TOI-1266. We validate the planetary nature of TOI-1266 b and c using four sectors of TESS photometry and data from the newly-commissioned 1-m SAINT-EX telescope located in San Pedro M\'artir (Mexico). We also include additional ground-based follow-up photometry as well as high-resolution spectroscopy and high-angular imaging observations. The inner, larger planet has a radius of $R=2.37_{-0.12}^{+0.16}$ R$_{\oplus}$ and an orbital period of 10.9 days. The outer, smaller planet has a radius of $R=1.56_{-0.13}^{+0.15}$ R$_{\oplus}$ on an 18.8-day orbit. The data are found to be consistent with circular, co-planar and stable orbits that are weakly influenced by the 2:1 mean motion resonance. Our TTV analysis of the combined dataset enables model-independent constraints on the masses and eccentricities of the planets. We find planetary masses of $M_\mathrm{p}$ = $13.5_{-9.0}^{+11.0}$ $\mathrm{M_{\oplus}}$ ($<36.8$ $\mathrm{M_{\oplus}}$ at 2-$\sigma$) for TOI-1266 b and $2.2_{-1.5}^{+2.0}$ $\mathrm{M_{\oplus}}$ ($<5.7$ $\mathrm{M_{\oplus}}$ at 2-$\sigma$) for TOI-1266 c. We find small but non-zero orbital eccentricities of $0.09_{-0.05}^{+0.06}$ ($<0.21$ at 2-$\sigma$) for TOI-1266 b and $0.04\pm0.03$ ($<0.10$ at 2-$\sigma$) for TOI-1266 c. The equilibrium temperatures of both planets are of $413\pm20$ K and $344\pm16$ K, respectively, assuming a null Bond albedo and uniform heat redistribution from the day-side to the night-side hemisphere. The host brightness and negligible activity combined with the planetary system architecture and favourable planet-to-star radii ratios makes TOI-1266 an exquisite system for a detailed characterisation., Comment: In press. Accepted for publication in Astronomy and Astrophysics on 20 July 2020
Published: 2020
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45. Two transiting hot Jupiters from the WASP survey: WASP-150b and WASP-176b

Author: Cooke, Benjamin F., Pollacco, Don, Almleaky, Y., Barkaoui, K., Benkhaldoun, Z., Blake, James A., Bouchy, François, Boumis, Panos, Brown, D. J. A., Bruni, Ivan, Burdanov, A., Cameron, Andrew Collier, Chote, Paul, Daassou, A., D'ago, Giuseppe, Dalal, Shweta, Damasso, Mario, Delrez, L., Doyle, A. P., Ducrot, E., Gillon, M., Hébrard, G., Hellier, C., Henning, Thomas, Jehin, E., Kiefer, Flavien, King, George W., Liakos, Alexios, Lopez, Théo, Mancini, Luigi, Mardling, Rosemary, Maxted, P. F. L., McCormac, James, Murray, C., Nielsen, Louise D., Osborn, Hugh, Palle, E., Pepe, Francesco, Pozuelos, F. J., Prieto-Arranz, J., Queloz, D., Schanche, Nicole, Ségransan, Damien, Smalley, Barry, Southworth, John, Thompson, S., Turner, Oliver, Udry, Stéphane, Velasco, S., West, Richard, Wheatley, Pete, Alikakos, John, Cooke, Benjamin F., Pollacco, Don, Almleaky, Y., Barkaoui, K., Benkhaldoun, Z., Blake, James A., Bouchy, François, Boumis, Panos, Brown, D. J. A., Bruni, Ivan, Burdanov, A., Cameron, Andrew Collier, Chote, Paul, Daassou, A., D'ago, Giuseppe, Dalal, Shweta, Damasso, Mario, Delrez, L., Doyle, A. P., Ducrot, E., Gillon, M., Hébrard, G., Hellier, C., Henning, Thomas, Jehin, E., Kiefer, Flavien, King, George W., Liakos, Alexios, Lopez, Théo, Mancini, Luigi, Mardling, Rosemary, Maxted, P. F. L., McCormac, James, Murray, C., Nielsen, Louise D., Osborn, Hugh, Palle, E., Pepe, Francesco, Pozuelos, F. J., Prieto-Arranz, J., Queloz, D., Schanche, Nicole, Ségransan, Damien, Smalley, Barry, Southworth, John, Thompson, S., Turner, Oliver, Udry, Stéphane, Velasco, S., West, Richard, Wheatley, Pete, and Alikakos, John
Abstract: We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric ($e$ = 0.38) hot Jupiter on a 5.6 day orbit around a $V$ = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4 $\rm M_{\odot}$ and 1.7 $\rm R_{\odot}$ respectively. WASP-150b has a mass and radius of 8.5 $\rm M_J$ and 1.1 $\rm R_J$, leading to a large planetary bulk density of 6.4 $\rm \rho_J$. WASP-150b is found to be $\sim3$ Gyr old, well below its circularisation timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a $V$ = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 $\rm M_{\odot}$ and 1.9 $\rm R_{\odot}$. WASP-176b has a mass and radius of 0.86 $\rm M_J$ and 1.5 $\rm R_J$ respectively, leading to a planetary bulk density of 0.23 $\rm \rho_J$., Comment: 15 pages, 14 figures. Accepted for publication in The Astronomical Journal
Published: 2020
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46. 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., Zohrabi, F., 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.
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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47. Three Short Period Jupiters from TESS

Author: Nielsen, L. D., Brahm, R., Bouchy, F., Espinoza, N., Turner, O., Rappaport, S., Pearce, L., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Acton, J. S., Bakos, G., Barclay, T., Barkaoui, K., Bhatti, W., Briceño, C., Bryant, E. M., Burleigh, M. R., Ciardi, D. R., Collins, K. A., Collins, K. I., Cooke, B. F., Csubry, Z., Santos, L. A. dos, Eigmüller, Ph., Fausnaugh, M. M., Gan, T., Gillon, M., Goad, M. R., Guerrero, N., Hagelberg, J., Hart, R., Henning, T., Huang, C. X., Jehin, E., Jenkins, J. S., Jordàn, A., Kielkopf, J. F., Kossakowski, D., Lavie, B., Law, N., Lendl, M., de Leon, J. P., Lovis, C., Mann, A. W., Marmier, M., McCormac, J., Mori, M., Moyano, M., Narita, N., Osip, D., Otegi, J. F., Pepe, F., Pozuelos, F. J., Raynard, L., Relles, H. M., Sarkis, P., Segransan, D., Seidel, J. V., Shporer, A., Stalport, M., Stockdale, C., Suc, V., Tamura, M., Tan, T. G., Tilbrook, R. H., Ting, E. B., Trifonov, T., Udry, S., Vanderburg, A., Wheatley, P. J., Wingham, G., Zhan, Z., Ziegler, C., Nielsen, L. D., Brahm, R., Bouchy, F., Espinoza, N., Turner, O., Rappaport, S., Pearce, L., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Acton, J. S., Bakos, G., Barclay, T., Barkaoui, K., Bhatti, W., Briceño, C., Bryant, E. M., Burleigh, M. R., Ciardi, D. R., Collins, K. A., Collins, K. I., Cooke, B. F., Csubry, Z., Santos, L. A. dos, Eigmüller, Ph., Fausnaugh, M. M., Gan, T., Gillon, M., Goad, M. R., Guerrero, N., Hagelberg, J., Hart, R., Henning, T., Huang, C. X., Jehin, E., Jenkins, J. S., Jordàn, A., Kielkopf, J. F., Kossakowski, D., Lavie, B., Law, N., Lendl, M., de Leon, J. P., Lovis, C., Mann, A. W., Marmier, M., McCormac, J., Mori, M., Moyano, M., Narita, N., Osip, D., Otegi, J. F., Pepe, F., Pozuelos, F. J., Raynard, L., Relles, H. M., Sarkis, P., Segransan, D., Seidel, J. V., Shporer, A., Stalport, M., Stockdale, C., Suc, V., Tamura, M., Tan, T. G., Tilbrook, R. H., Ting, E. B., Trifonov, T., Udry, S., Vanderburg, A., Wheatley, P. J., Wingham, G., Zhan, Z., and Ziegler, C.
Abstract: We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V=11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 Mjup planet in a grazing transit configuration with an impact parameter of b = 1.17 +0.10/-0.08. As a result the radius is poorly constrained, 2.03 +0.61/-0.49 Rjup. The planet's distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs' = 10^7 - 10^9. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 +/- 0.13 Mjup and a radius of 1.29 +/- 0.02 Rjup. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V=12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V=12.4 G-type star. It has a mass of 0.79 +/- 0.06 Mjup and a radius of 1.09 +0.08/-0.05 Rjup. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe/H] ranging from 0.18 - 0.24., Comment: Published in A&A
Published: 2020
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48. HATS-47b, HATS-48Ab, HATS-49b and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs

Author: Hartman, J. D., Jordán, Andrés, Bayliss, D., Bakos, G. Á., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., Henning, Th., Mancini, L., Penev, K., Rabus, M., Sarkis, P., Suc, V., de Val-Borro, M., Zhou, G., Crane, J. D., Shectman, S., Teske, J. K., Wang, S. X., Butler, R. P., Lázár, J., Papp, I., Sári, P., Anderson, D. R., Hellier, C., West, R. G., Barkaoui, K., Pozuelos, F. J., Jehin, E., Gillon, M., Nielsen, L., Lendl, M., Udry, S., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Christiansen, Jessie, Crossfield, Ian J. M., Henze, Christopher E., Jenkins, Jon M., Smith, Jeffrey C., Ting, Eric B., Hartman, J. D., Jordán, Andrés, Bayliss, D., Bakos, G. Á., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., Henning, Th., Mancini, L., Penev, K., Rabus, M., Sarkis, P., Suc, V., de Val-Borro, M., Zhou, G., Crane, J. D., Shectman, S., Teske, J. K., Wang, S. X., Butler, R. P., Lázár, J., Papp, I., Sári, P., Anderson, D. R., Hellier, C., West, R. G., Barkaoui, K., Pozuelos, F. J., Jehin, E., Gillon, M., Nielsen, L., Lendl, M., Udry, S., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Christiansen, Jessie, Crossfield, Ian J. M., Henze, Christopher E., Jenkins, Jon M., Smith, Jeffrey C., and Ting, Eric B.
Abstract: We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have masses of $0.369_{-0.021}^{+0.031}$ $M_{J}$, $0.243_{-0.030}^{+0.022}$ $M_{J}$, $0.353_{-0.027}^{+0.038}$ $M_{J}$ and $0.1254\pm0.0039$ $M_{J}$, respectively, and radii of $1.117\pm0.014$ $R_{J}$, $0.800\pm0.015$ $R_{J}$, $0.765\pm0.013$ $R_{J}$, and $0.7224\pm0.0032$ $R_{J}$, respectively. The planets orbit close to their host stars with orbital periods of $3.9228$ d, $3.1317$ d, $4.1480$ d and $7.3279$ d, respectively. The hosts are main sequence K dwarfs with masses of $0.674_{-0.012}^{+0.016}$ $M_{\odot}$, $0.7279\pm0.0066$ $M_{\odot}$, $0.7133\pm0.0075$ $M_{\odot}$, and $0.7311\pm0.0028$ $M_{\odot}$ and with $V$-band magnitudes of $V = 14.829\pm0.010$, $14.35\pm0.11$, $14.998\pm0.040$ and $12.469\pm0.010$. The Super-Neptune HATS-72b (a.k.a.\ WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI 1073.01), HATS-48A and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved $5.\!\!^{\prime\prime}4$ neighbor in Gaia~DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of $0.22$ $M_{\odot}$ and a current projected physical separation of $\sim$1,400 au., Comment: Accepted for publication in AJ. 32 pages, 14 figures, 7 tables
Published: 2020
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49. WASP-South hot Jupiters: WASP-178b, WASP-184b, WASP-185b & WASP-192b

Author: Hellier, C., Anderson, D. R., Barkaoui, K., Benkhaldoun, Z., Bouchy, F., Burdanov, A., Cameron, A. Collier, Delrez, L., Gillon, M., Jehin, E., Nielsen, L. D., Maxted, P. F. L., Pepe, F., Pollacco, D., Pozuelos, F. J., Queloz, D., Segransan, D., Smalley, B., Triaud, A. H. M. J., Turner, O. D., Udry, S., West, R. G., Hellier, C., Anderson, D. R., Barkaoui, K., Benkhaldoun, Z., Bouchy, F., Burdanov, A., Cameron, A. Collier, Delrez, L., Gillon, M., Jehin, E., Nielsen, L. D., Maxted, P. F. L., Pepe, F., Pollacco, D., Pozuelos, F. J., Queloz, D., Segransan, D., Smalley, B., Triaud, A. H. M. J., Turner, O. D., Udry, S., and West, R. G.
Abstract: We report on four new transiting hot Jupiters discovered by the WASP-South survey. WASP-178b transits a V = 9.9, A1V star with Teff = 9350 +/- 150 K, the second-hottest transit host known. It has a highly bloated radius of 1.81 +/- 0.09 Rjup, in line with the known correlation between high irradiation and large size. With an estimated temperature of 2470 +/- 60 K, the planet is one of the best targets for studying ultra-hot Jupiters that is visible from the Southern hemisphere. The three host stars WASP-184, WASP-185 and WASP-192 are all post-main-sequence G0 stars of ages 4-8 Gyr. The larger stellar radii (1.3-1.7 Msun) mean that the transits are relatively shallow (0.7-0.9%) even though the planets have moderately inflated radii of 1.2-1.3 Rjup. WASP-185b has an eccentric orbit (e = 0.24) and a relatively long orbital period of 9.4 d. A star that is 4.6 arcsec from WASP-185 and 4.4 mag fainter might be physically associated., Comment: Version as Accepted for MNRAS (RV table added)
Published: 2019
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50. Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS

Author: Zhou, G., Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, David W., Quinn, S. N., Collins, K. A., Winn, J. N., Wong, I., Kovács, G., Csubry, Z., Bhatti, W., Penev, K., Bieryla, A., Esquerdo, G. A., Berlind, P., Calkins, M. L., de Val-Borro, M., Noyes, R. W., Lázár, J., Papp, I., Sári, P., Kovács, T., Buchhave, Lars A., Szklenár, T., Beky, B., Johnson, M. C., Cochran, W. D., Kniazev, A. Y., Stassun, K. G., Fulton, B. J., Shporer, A., Espinoza, N., Bayliss, D., Everett, M., Howell, S. B., Hellier, C., Anderson, D. R., Cameron, A. Collier, West, R. G., Brown, D. J. A., Schanche, N., Barkaoui, K., Pozuelos, F., Gillon, M., Jehin, E., Benkhaldoun, Z., Daassou, A., Ricker, G., Vanderspek, R., Seager, S., Jenkins, J. M., Lissauer, Jack J., Armstrong, J. D., Collins, K. I., Gan, T., Hart, R., Horne, K., Kielkopf, J. F., Nielsen, L. D., Nishiumi, T., Narita, N., Palle, E., Relles, H. M., Sefako, R., Tan, T. G., Davies, M., Goeke, Robert F., Guerrero, N., Haworth, K., Villanueva, S., Zhou, G., Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, David W., Quinn, S. N., Collins, K. A., Winn, J. N., Wong, I., Kovács, G., Csubry, Z., Bhatti, W., Penev, K., Bieryla, A., Esquerdo, G. A., Berlind, P., Calkins, M. L., de Val-Borro, M., Noyes, R. W., Lázár, J., Papp, I., Sári, P., Kovács, T., Buchhave, Lars A., Szklenár, T., Beky, B., Johnson, M. C., Cochran, W. D., Kniazev, A. Y., Stassun, K. G., Fulton, B. J., Shporer, A., Espinoza, N., Bayliss, D., Everett, M., Howell, S. B., Hellier, C., Anderson, D. R., Cameron, A. Collier, West, R. G., Brown, D. J. A., Schanche, N., Barkaoui, K., Pozuelos, F., Gillon, M., Jehin, E., Benkhaldoun, Z., Daassou, A., Ricker, G., Vanderspek, R., Seager, S., Jenkins, J. M., Lissauer, Jack J., Armstrong, J. D., Collins, K. I., Gan, T., Hart, R., Horne, K., Kielkopf, J. F., Nielsen, L. D., Nishiumi, T., Narita, N., Palle, E., Relles, H. M., Sefako, R., Tan, T. G., Davies, M., Goeke, Robert F., Guerrero, N., Haworth, K., and Villanueva, S.
Abstract: Wide field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69b (TOI 625.01) and HAT-P-70b (TOI 624.01), two new hot Jupiters around A stars from the HATNet survey which have also been observed by the Transiting Exoplanet Survey Satellite (TESS). HAT-P-69b has a mass of 3.58 +0.58/-0.58 MJup and a radius of 1.676 +0.051/-0.033 RJup, residing in a prograde 4.79-day orbit. HAT-P-70b has a radius of 1.87 +0.15/-0.10 RJup and a mass constraint of < 6.78 (3 sigma) MJup, and resides in a retrograde 2.74-day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than Tmag=10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41+/-0.10 % within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71+/-0.31% for G stars, 0.43+/-0.15% for F stars, and 0.26+/-0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass., Comment: Accepted for publication by AJ
Published: 2019
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