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146 results on '"Pallé , Enric"'

1. ANDES, the high resolution spectrograph for the ELT:science goals, project overview, and future developments

Author: Vernet, Joël R., Bryant, Julia J., Motohara, Kentaro, Marconi, Alessandro, Abreu, Artur R., Adibekyan, Vardan, Alberti, Valentina, Albrecht, Simon, Alcaniz, Jailson, Aliverti, Matteo, Allende Prieto, Carlos, Alvarado-gomez, Julian, Alves, Catarina, Amado, Pedro J., Amate, Manuel, Andersen, Michael, Antoniucci, Simone, Artigau, E., Bailet, Christophe, Baker, Clark E., Baldini, Veronica, Balestra, Andrea, Barnes, S.a., Baron, Frédérique, Barros, Susana, Bauer, Svend-marian, Beaulieu, Mathilde, Bellido-tirado, Olga, Benneke, Björn, Bensby, Thomas, Bergin, Edwin, Berio, P., Biazzo, Katia, Bigot, Laurent, Bik, Arjan, Birkby, Jayne L., Blind, Nicolas, Boebion, Olivier, Boisse, Isabelle, Bolmont, Emeline, Bolton, J. S., Bonaglia, Marco, Bonfils, Xavier, Bonhomme, Lea, Borsa, Francesco, Bouret, Jean-claude, Brandeker, Alexis, Brandner, Wolfgang, Broeg, Christopher H., Brogi, Matteo, Brousseau, Denis, Brucalassi, Anna, Brynnel, Joar G., Buchhave, Lars A., Buscher, David F., Cabona, Lorenzo, Cabral, Alexandre, Calderone, Giorgio, Calvo-ortega, Rocío, Cantalloube, Faustine, Canto Martins, Bruno L., Carbonaro, Luca, Caujolle, Yan, Chauvin, Gaël, Chazelas, Bruno, Cheffot, Anne-laure L., Cheng, Yuk Shan, Chiavassa, Andrea, Christensen, Lise B., Cirami, Roberto, Cirasuolo, Michele, Cook, Neil J., Cooke, Ryan, Coretti, Igor, Covino, Stefano, Cowan, Nicolas B., Cresci, Giovanni, Cristiani, Stefano, Parro, Vanderlei Cunha, Cupani, Guido, D'odorico, Valentina, Dadi, Kamalesh, De Castro Leão, Izan C., De Cia, Annalisa, De Medeiros, Jose R., Debras, Florian, Debus, Michael, Delorme, Alain, Demangeon, Olivier, Derie, Frederic, Dessauges-zavadsky, M., Di Marcantonio, Paolo, Di Stefano, Simona, Dionies, Frank, Domiciano De Souza, Armando, Doyon, René, Dunn, Jennifer S., Egner, Sébastien E., Ehrenreich, David, Faria, Joao P., Ferruzzi, Debora, Feruglio, Chiara, Fisher, Martin, Fontana, Adriano, Frank, B S., Fuesslein, C., Fumagalli, M., Fusco, Thierry, Fynbo, Johan P. U., Gabella, O., Gaessler, W., Gallo, E., Gao, X., Genolet, L., Genoni, M., Giacobbe, P., Giro, E., Gonçalves, R. S., Gonzalez, O. A., González-hernández, J. I., Gouvret, C., Gracia Témich, F., Haehnelt, M. G., Haniff, C., Hatzes, A., Helled, R., Hoeijmakers, H. J., Hughes, I., Huke, Philipp, Ivanisenko, Y., Järvinen, A. S., Järvinen, S. P., Kaminski, A., Kern, J., Knoche, J., Kordt, A., Korhonen, H., Korn, A., Kouach, D., Kowzan, G., Kreidberg, L., Landoni, M., Lanotte, A. A., Lavail, A., Lavie, B., Lee, D., Lehmitz, M., Li, J., Li, W., Liske, J., Lovis, C., Lucatello, S., Lunney, D., Macintosh, M. J., Madhusudhan, N., Magrini, L., Maiolino, R., Maldonado, J., Malo, L., Man, A. W. S., Marquart, T., Marques, C. M. J., Marques, E. L., Martinez, P., Martins, A. M., Martins, C. J. A. P., Martins, J. H. C., Maslowski, P., Mason, C., Mason, E., Mccracken, R. A., Melo E Sousa, M. A. F., Mergo, P., Micela, G., Milaković, D., Mollière, P., Monteiro, M. A., Montgomery, D., Mordasini, C., Morin, J., Mucciarelli, A., Murphy, M. T., N'diaye, M., Nardetto, N., Neichel, B., Neri, N., Niedzielski, A. T., Niemczura, E., Nisini, B., Nortmann, L., Noterdaeme, P., Nunes, N. J., Oggioni, L., Olchewsky, F., Oliva, E., Önel, H., Origlia, L., Östlin, G., Ouellette, N. N.-q., Pallé, Enric, Papaderos, P., Pariani, G., Pasquini, L., Peñate Castro, J., Pepe, F., Peroux, C., Perreault Levasseur, L., Perruchot, Sandrine, Petit, P., Pfuhl, Oliver, Pino, L., Piqueras, Javier, Piskunov, N., Pollo, A., Poppenhaeger, K., Porru, M., Puschnig, J., Quirrenbach, A., Rauscher, Emily, Rebolo, R., Redaelli, E. M. A., Reffert, S., Reid, D. T., Reiners, A., Richter, P., Riva, M., Rivoire, S., Rodríguez-lópez, C., Roederer, I. U., Romano, D., Roth, M., Rousseau, S., Rowe, J., Saccardi, A., Salvadori, S., Sanna, N., Santos, N. C., Santos Diaz, P., Sanz-forcada, Jorge, Sarajlic, M., Sauvage, J.-f., Savio, D., Scaudo, A., Schäfer, S., Schiavon, R. P., Schmidt, T. M., Selmi, C., Simoes, R., Simonnin, A., Sivanandam, S., Sordet, M., Sordo, R., Sortino, F., Sosnowska, D., Sousa, S. G., Spang, A., Spiga, R., Stempels, E., Stevenson, J. R. Y., Strassmeier, Klaus G., Suárez Mascareño, A., Sulich, A., Sun, X., Tanvir, N. R., Tenegi-sanginés, F., Thibault, S., Thompson, S. J., Tisserand, P., Tozzi, A., Turbet, M., Véran, J.-p., Vallée, P., Vanni, I., Varas, R., Vega-moreno, A., Venn, K. A., Verma, A., Vernet, J., Viel, M., Wade, G., Waring, C., Weber, M., Weder, J., Wehbé, B., Weingrill, J., Woche, M., Xompero, M., Zackrisson, E., Zanutta, A., Zapatero Osorio, M. R., Zechmeister, M., Zimara, J., Vernet, Joël R., Bryant, Julia J., Motohara, Kentaro, Marconi, Alessandro, Abreu, Artur R., Adibekyan, Vardan, Alberti, Valentina, Albrecht, Simon, Alcaniz, Jailson, Aliverti, Matteo, Allende Prieto, Carlos, Alvarado-gomez, Julian, Alves, Catarina, Amado, Pedro J., Amate, Manuel, Andersen, Michael, Antoniucci, Simone, Artigau, E., Bailet, Christophe, Baker, Clark E., Baldini, Veronica, Balestra, Andrea, Barnes, S.a., Baron, Frédérique, Barros, Susana, Bauer, Svend-marian, Beaulieu, Mathilde, Bellido-tirado, Olga, Benneke, Björn, Bensby, Thomas, Bergin, Edwin, Berio, P., Biazzo, Katia, Bigot, Laurent, Bik, Arjan, Birkby, Jayne L., Blind, Nicolas, Boebion, Olivier, Boisse, Isabelle, Bolmont, Emeline, Bolton, J. S., Bonaglia, Marco, Bonfils, Xavier, Bonhomme, Lea, Borsa, Francesco, Bouret, Jean-claude, Brandeker, Alexis, Brandner, Wolfgang, Broeg, Christopher H., Brogi, Matteo, Brousseau, Denis, Brucalassi, Anna, Brynnel, Joar G., Buchhave, Lars A., Buscher, David F., Cabona, Lorenzo, Cabral, Alexandre, Calderone, Giorgio, Calvo-ortega, Rocío, Cantalloube, Faustine, Canto Martins, Bruno L., Carbonaro, Luca, Caujolle, Yan, Chauvin, Gaël, Chazelas, Bruno, Cheffot, Anne-laure L., Cheng, Yuk Shan, Chiavassa, Andrea, Christensen, Lise B., Cirami, Roberto, Cirasuolo, Michele, Cook, Neil J., Cooke, Ryan, Coretti, Igor, Covino, Stefano, Cowan, Nicolas B., Cresci, Giovanni, Cristiani, Stefano, Parro, Vanderlei Cunha, Cupani, Guido, D'odorico, Valentina, Dadi, Kamalesh, De Castro Leão, Izan C., De Cia, Annalisa, De Medeiros, Jose R., Debras, Florian, Debus, Michael, Delorme, Alain, Demangeon, Olivier, Derie, Frederic, Dessauges-zavadsky, M., Di Marcantonio, Paolo, Di Stefano, Simona, Dionies, Frank, Domiciano De Souza, Armando, Doyon, René, Dunn, Jennifer S., Egner, Sébastien E., Ehrenreich, David, Faria, Joao P., Ferruzzi, Debora, Feruglio, Chiara, Fisher, Martin, Fontana, Adriano, Frank, B S., Fuesslein, C., Fumagalli, M., Fusco, Thierry, Fynbo, Johan P. U., Gabella, O., Gaessler, W., Gallo, E., Gao, X., Genolet, L., Genoni, M., Giacobbe, P., Giro, E., Gonçalves, R. S., Gonzalez, O. A., González-hernández, J. I., Gouvret, C., Gracia Témich, F., Haehnelt, M. G., Haniff, C., Hatzes, A., Helled, R., Hoeijmakers, H. J., Hughes, I., Huke, Philipp, Ivanisenko, Y., Järvinen, A. S., Järvinen, S. P., Kaminski, A., Kern, J., Knoche, J., Kordt, A., Korhonen, H., Korn, A., Kouach, D., Kowzan, G., Kreidberg, L., Landoni, M., Lanotte, A. A., Lavail, A., Lavie, B., Lee, D., Lehmitz, M., Li, J., Li, W., Liske, J., Lovis, C., Lucatello, S., Lunney, D., Macintosh, M. J., Madhusudhan, N., Magrini, L., Maiolino, R., Maldonado, J., Malo, L., Man, A. W. S., Marquart, T., Marques, C. M. J., Marques, E. L., Martinez, P., Martins, A. M., Martins, C. J. A. P., Martins, J. H. C., Maslowski, P., Mason, C., Mason, E., Mccracken, R. A., Melo E Sousa, M. A. F., Mergo, P., Micela, G., Milaković, D., Mollière, P., Monteiro, M. A., Montgomery, D., Mordasini, C., Morin, J., Mucciarelli, A., Murphy, M. T., N'diaye, M., Nardetto, N., Neichel, B., Neri, N., Niedzielski, A. T., Niemczura, E., Nisini, B., Nortmann, L., Noterdaeme, P., Nunes, N. J., Oggioni, L., Olchewsky, F., Oliva, E., Önel, H., Origlia, L., Östlin, G., Ouellette, N. N.-q., Pallé, Enric, Papaderos, P., Pariani, G., Pasquini, L., Peñate Castro, J., Pepe, F., Peroux, C., Perreault Levasseur, L., Perruchot, Sandrine, Petit, P., Pfuhl, Oliver, Pino, L., Piqueras, Javier, Piskunov, N., Pollo, A., Poppenhaeger, K., Porru, M., Puschnig, J., Quirrenbach, A., Rauscher, Emily, Rebolo, R., Redaelli, E. M. A., Reffert, S., Reid, D. T., Reiners, A., Richter, P., Riva, M., Rivoire, S., Rodríguez-lópez, C., Roederer, I. U., Romano, D., Roth, M., Rousseau, S., Rowe, J., Saccardi, A., Salvadori, S., Sanna, N., Santos, N. C., Santos Diaz, P., Sanz-forcada, Jorge, Sarajlic, M., Sauvage, J.-f., Savio, D., Scaudo, A., Schäfer, S., Schiavon, R. P., Schmidt, T. M., Selmi, C., Simoes, R., Simonnin, A., Sivanandam, S., Sordet, M., Sordo, R., Sortino, F., Sosnowska, D., Sousa, S. G., Spang, A., Spiga, R., Stempels, E., Stevenson, J. R. Y., Strassmeier, Klaus G., Suárez Mascareño, A., Sulich, A., Sun, X., Tanvir, N. R., Tenegi-sanginés, F., Thibault, S., Thompson, S. J., Tisserand, P., Tozzi, A., Turbet, M., Véran, J.-p., Vallée, P., Vanni, I., Varas, R., Vega-moreno, A., Venn, K. A., Verma, A., Vernet, J., Viel, M., Wade, G., Waring, C., Weber, M., Weder, J., Wehbé, B., Weingrill, J., Woche, M., Xompero, M., Zackrisson, E., Zanutta, A., Zapatero Osorio, M. R., Zechmeister, M., and Zimara, J.
Published: 2024

2. Masses, revised radii, and a third planet candidate in the 'Inverted' planetary system around TOI-1266

Author: Cloutier, Ryan, Greklek-Mckeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris A., Cloutier, Ryan, Greklek-Mckeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris A.
Abstract: Is the population of close-in planets orbiting M dwarfs sculpted by thermally driven escape or is it a direct outcome of the planet formation process? A number of recent empirical results strongly suggest the latter. However, the unique architecture of the TOI-1266 system presents a challenge to models of planet formation and atmospheric escape given its seemingly ‘inverted’ architecture of a large sub-Neptune (Pb = 10.9 d, ⁠) orbiting interior to that of the system’s smaller planet (Pc = 18.8 d, ⁠). Here, we present revised planetary radii based on new TESS and diffuser-assisted ground-based transit observations, and characterize both planetary masses using a set of 145 radial velocity measurements from HARPS-N (⁠⁠). Our analysis also reveals a third planet candidate (Pd = 32.3 d, ⁠), which if real, would form a chain of near 5:3 period ratios, although the system is likely not in a mean motion resonance. Our results indicate that TOI-1266 b and c are among the lowest density sub-Neptunes around M dwarfs and likely exhibit distinct bulk compositions of a gas-enveloped terrestrial (Xenv,b = 5.5 ± 0.7 per cent) and a water-rich world (WMFc = 59 ± 14 per cent), which is supported by hydrodynamic escape models. If distinct bulk compositions are confirmed through atmospheric characterization, the system’s unique architecture would represent an interesting test case of inside-out sub-Neptune formation at pebble traps.
Published: 2024

3. Pre-perihelion Monitoring of Interstellar Comet 2I/Borisov

Author: Prodan, George P., Popescu, Marcel, Licandro, Javier, Akhlaghi, Mohammad, de León, Julia, Tatsumi, Eri, Pastrav, Bogdan Adrian, Hibbert, Jacob M., Văduvescu, Ovidiu, Simion, Nicolae Gabriel, Pallé, Enric, Narita, Norio, Fukui, Akihiko, Murgas, Felipe, Prodan, George P., Popescu, Marcel, Licandro, Javier, Akhlaghi, Mohammad, de León, Julia, Tatsumi, Eri, Pastrav, Bogdan Adrian, Hibbert, Jacob M., Văduvescu, Ovidiu, Simion, Nicolae Gabriel, Pallé, Enric, Narita, Norio, Fukui, Akihiko, and Murgas, Felipe
Abstract: The discovery of interstellar comet 2I/Borisov offered the unique opportunity to obtain a detailed analysis of an object coming from another planetary system, and leaving behind material in our interplanetary space. We continuously observed 2I/Borisov between October 3 and December 13, 2019 using the 1.52-m Telescopio Carlos S\'{a}nchez equipped with MuSCAT2 instrument, and the 2.54-m Isaac Newton Telescope with Wide Field Camera. We characterize its morphology and spectro-photometric features using the data gathered during this extended campaign. Simultaneous imaging in four bands ($g$, $r$, $i$, and $z_s$) reveals a homogeneous composition and a reddish hue, resembling Solar System comets, and as well a diffuse profile exhibiting familiar cometary traits. We discern a stationary trend fluctuating around a constant activity level throughout October and November 2019. Subsequently, a reduction in activity is observed in December. Dust production and mass loss calculations indicate approximately an average of 4 kg/s before perihelion, while after perihelion the net mass loss is about 0.6 kg/s. Our simulations indicate the most probable size of coma dust particles should be in the range 200-250 nm, and the terminal speed around 300 m/s. The spectrum acquired with the 4.2-m William Herschel Telescope shows the presence of a strong CN line for which we find a gas production rate of $1.2 \times 10^{24}~s^{-1}$. We also detected NH$_2$ and OI bands. The ratio between NH$_2$ and CN productions is $\log (NH_2/CN) =-0.2$. Overall, this observing campaign provides a new understanding of 2I/Borisov's unique characteristics and activity patterns., Comment: accepted to MNRAS on 12th Feb 2024
Published: 2024
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4. Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815

Author: Psaridi, Angelica, Osborn, Hugh, Bouchy, François, Lendl, Monika, Parc, Léna, Billot, Nicolas, Broeg, Christopher, Sousa, Sérgio G., Adibekyan, Vardan, Attia, Omar, Bonfanti, Andrea, Chakraborty, Hritam, Collins, Karen A., Davoult, Jeanne, Delgado-Mena, Elisa, Grieves, Nolan, Guillot, Tristan, Heitzmann, Alexis, Helled, Ravit, Hellier, Coel, Jenkins, Jon M., Knierim, Henrik, Krenn, Andreas, Lissauer, JackJ., Luque, Rafael, Rapetti, David, Santos, Nuno C., Suárez, Olga, Venturini, Julia, Wilkin, Francis P., Wilson, Thomas G., Winn, Joshua N., Ziegler, Carl, Zingales, Tiziano, Alibert, Yann, Brandeker, Alexis, Egger, Jo Ann, Gandolfi, Davide, Hooton, Matthew J., Tuson, Amy, Ulmer-Moll, Solène, Abe, Lyu, Allart, Romain, Alonso, Roi, Anderson, David R., Anglada, Guillem, Bárczy, Tamas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Benz, Willy, Bonfils, Xavier, Borsato, Luca, Bourrier, Vincent, Ciardi, David R., Cameron, Andrew Collier, Charnoz, Sébastien, Cointepas, Marion, Csizmadia, Szilárd, Cubillos, Patricio, Curto, Gaspare Lo, Davies, Melvyn B., Daylan, Tansu, Deleuil, Magali, Deline, Adrien, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dorn, Caroline, Dumusque, Xavier, Ehrenreich, David, Erikson, Anders, Etangs, Alain Lecavelier des, Ferreras, Elena Diana de Miguel, Fortier, Andrea, Fossati, Luca, Frensch, Yolanda G. C., Fridlund, Malcolm, Gillon, Michaël, Güdel, Manuel, Günther, Maximilian N., Hagelberg, Janis, Helling, Christiane, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo L., Lam, Kristine, Laskar, Jacques, Lavie, Baptiste, Lovis, Christophe, Magrin, Demetrio, Marafatto, Luca, Maxted, Pierre, McDermott, Scott, Mékarnia, Djamel, Mordasini, Christoph, Murgas, Felipe, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Ramos, Devin, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Seager, Sara, Ségransan, Damien, Scandariato, Gaetano, Simon, Attila, Smith, Alexis M. S., Stalport, Manu, Steller, Manfred, Szabó, Gyula, Thomas, Nicolas, Pritchard, Tyler A., Udry, Stéphane, Van Damme, Carlos Corral, Van Grootel, Valérie, Villaver, Eva, Walter, Ingo, Walton, Nicholas, Watkins, Cristilyn N., West, Richard G., Psaridi, Angelica, Osborn, Hugh, Bouchy, François, Lendl, Monika, Parc, Léna, Billot, Nicolas, Broeg, Christopher, Sousa, Sérgio G., Adibekyan, Vardan, Attia, Omar, Bonfanti, Andrea, Chakraborty, Hritam, Collins, Karen A., Davoult, Jeanne, Delgado-Mena, Elisa, Grieves, Nolan, Guillot, Tristan, Heitzmann, Alexis, Helled, Ravit, Hellier, Coel, Jenkins, Jon M., Knierim, Henrik, Krenn, Andreas, Lissauer, JackJ., Luque, Rafael, Rapetti, David, Santos, Nuno C., Suárez, Olga, Venturini, Julia, Wilkin, Francis P., Wilson, Thomas G., Winn, Joshua N., Ziegler, Carl, Zingales, Tiziano, Alibert, Yann, Brandeker, Alexis, Egger, Jo Ann, Gandolfi, Davide, Hooton, Matthew J., Tuson, Amy, Ulmer-Moll, Solène, Abe, Lyu, Allart, Romain, Alonso, Roi, Anderson, David R., Anglada, Guillem, Bárczy, Tamas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Benz, Willy, Bonfils, Xavier, Borsato, Luca, Bourrier, Vincent, Ciardi, David R., Cameron, Andrew Collier, Charnoz, Sébastien, Cointepas, Marion, Csizmadia, Szilárd, Cubillos, Patricio, Curto, Gaspare Lo, Davies, Melvyn B., Daylan, Tansu, Deleuil, Magali, Deline, Adrien, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dorn, Caroline, Dumusque, Xavier, Ehrenreich, David, Erikson, Anders, Etangs, Alain Lecavelier des, Ferreras, Elena Diana de Miguel, Fortier, Andrea, Fossati, Luca, Frensch, Yolanda G. C., Fridlund, Malcolm, Gillon, Michaël, Güdel, Manuel, Günther, Maximilian N., Hagelberg, Janis, Helling, Christiane, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo L., Lam, Kristine, Laskar, Jacques, Lavie, Baptiste, Lovis, Christophe, Magrin, Demetrio, Marafatto, Luca, Maxted, Pierre, McDermott, Scott, Mékarnia, Djamel, Mordasini, Christoph, Murgas, Felipe, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Ramos, Devin, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Seager, Sara, Ségransan, Damien, Scandariato, Gaetano, Simon, Attila, Smith, Alexis M. S., Stalport, Manu, Steller, Manfred, Szabó, Gyula, Thomas, Nicolas, Pritchard, Tyler A., Udry, Stéphane, Van Damme, Carlos Corral, Van Grootel, Valérie, Villaver, Eva, Walter, Ingo, Walton, Nicholas, Watkins, Cristilyn N., and West, Richard G.
Abstract: We present the discovery and characterization of two warm mini-Neptunes transiting the K3V star TOI-815 in a K-M binary system. Analysis of the spectra and rotation period reveal it to be a young star with an age of $200^{+400}_{-200}$Myr. TOI-815b has a 11.2-day period and a radius of 2.94$\pm$0.05$\it{R_{\rm\mathrm{\oplus}}}$ with transits observed by TESS, CHEOPS, ASTEP, and LCOGT. The outer planet, TOI-815c, has a radius of 2.62$\pm$0.10$\it{R_{\rm\mathrm{\oplus}}}$, based on observations of three non-consecutive transits with TESS, while targeted CHEOPS photometry and radial velocity follow-up with ESPRESSO were required to confirm the 35-day period. ESPRESSO confirmed the planetary nature of both planets and measured masses of 7.6$\pm$1.5 $\it{M_{\rm \mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=1.64$^{+0.33}_{-0.31}$gcm$^{-3}$) and 23.5$\pm$2.4$\it{M_{\rm\mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=7.2$^{+1.1}_{-1.0}$gcm$^{-3}$) respectively. Thus, the planets have very different masses, unlike the usual similarity of masses in compact multi-planet systems. Moreover, our statistical analysis of mini-Neptunes orbiting FGK stars suggests that weakly irradiated planets tend to have higher bulk densities compared to those suffering strong irradiation. This could be ascribed to their cooler atmospheres, which are more compressed and denser. Internal structure modeling of TOI-815b suggests it likely has a H-He atmosphere constituting a few percent of the total planet mass, or higher if the planet is assumed to have no water. In contrast, the measured mass and radius of TOI-815c can be explained without invoking any atmosphere, challenging planetary formation theories. Finally, we infer from our measurements that the star is viewed close to pole-on, which implies a spin-orbit misalignment at the 3$\sigma$ level., Comment: 24 pages, 27 figures, 6 tables
Published: 2024

5. Detection of Carbon Monoxide in the Atmosphere of WASP-39b Applying Standard Cross-Correlation Techniques to JWST NIRSpec G395H Data

Author: Esparza-Borges, Emma, López-Morales, Mercedes, Redai, Jéa I. Adams, Pallé, Enric, Kirk, James, Casasayas-Barris, Núria, Batalha, Natasha E., Rackham, Benjamin V., Bean, Jacob L., Casewell, S. L., Decin, Leen, Santos, Leonardo A. Dos, Muñoz, Antonio García, Harrington, Joseph, Heng, Kevin, Hu, Renyu, Mancini, Luigi, Molaverdikhani, Karan, Morello, Giuseppe, Nikolov, Nikolay K., Nixon, Matthew C., Redfield, Seth, Stevenson, Kevin B., Wakeford, Hannah R., Alam, Munazza K., Benneke, Björn, Blecic, Jasmina, Crouzet, Nicolas, Daylan, Tansu, Inglis, Julie, Kreidberg, Laura, de la Roche, Dominique J. M. Petit dit, Turner, Jake D., Esparza-Borges, Emma, López-Morales, Mercedes, Redai, Jéa I. Adams, Pallé, Enric, Kirk, James, Casasayas-Barris, Núria, Batalha, Natasha E., Rackham, Benjamin V., Bean, Jacob L., Casewell, S. L., Decin, Leen, Santos, Leonardo A. Dos, Muñoz, Antonio García, Harrington, Joseph, Heng, Kevin, Hu, Renyu, Mancini, Luigi, Molaverdikhani, Karan, Morello, Giuseppe, Nikolov, Nikolay K., Nixon, Matthew C., Redfield, Seth, Stevenson, Kevin B., Wakeford, Hannah R., Alam, Munazza K., Benneke, Björn, Blecic, Jasmina, Crouzet, Nicolas, Daylan, Tansu, Inglis, Julie, Kreidberg, Laura, de la Roche, Dominique J. M. Petit dit, and Turner, Jake D.
Abstract: Carbon monoxide was recently reported in the atmosphere of the hot Jupiter WASP-39b using the NIRSpec PRISM transit observation of this planet, collected as part of the JWST Transiting Exoplanet Community Early Release Science (JTEC ERS) Program. This detection, however, could not be confidently confirmed in the initial analysis of the higher resolution observations with NIRSpec G395H disperser. Here we confirm the detection of CO in the atmosphere of WASP-39b using the NIRSpec G395H data and cross-correlation techniques. We do this by searching for the CO signal in the unbinned transmission spectrum of the planet between 4.6 and 5.0 $\mu$m, where the contribution of CO is expected to be higher than that of other anticipated molecules in the planet's atmosphere. Our search results in a detection of CO with a cross-correlation function (CCF) significance of $6.6 \sigma$ when using a template with only ${\rm ^{12}C^{16}O}$ lines. The CCF significance of the CO signal increases to $7.5 \sigma$ when including in the template lines from additional CO isotopologues, with the largest contribution being from ${\rm ^{13}C^{16}O}$. Our results highlight how cross-correlation techniques can be a powerful tool for unveiling the chemical composition of exoplanetary atmospheres from medium-resolution transmission spectra, including the detection of isotopologues., Comment: Accepted for publication in The Astrophysical Journal Letters
Published: 2023

6. Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS

Author: Lowson, Nataliea, Zhou, George, Huang, Chelsea X., Wright, Duncan J., Edwards, Billy, Nabbie, Emma, Venner, Alex, Quinn, Samuel N., Collins, Karen A., Gillen, Edward, Battley, Matthew, Triaud, Amaury, Hellier, Coel, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Wohler, Bill, Shporer, Avi, Schwarz, Richard P., Murgas, Felipe, Pallé, Enric, Anderson, David R., West, Richard G., Wittenmyer, Robert A., Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Zhang, Hui, Fairnington, Tyler, Okumura, Jack, Mengel, Matthew W., Addison, Brett C., Lowson, Nataliea, Zhou, George, Huang, Chelsea X., Wright, Duncan J., Edwards, Billy, Nabbie, Emma, Venner, Alex, Quinn, Samuel N., Collins, Karen A., Gillen, Edward, Battley, Matthew, Triaud, Amaury, Hellier, Coel, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Wohler, Bill, Shporer, Avi, Schwarz, Richard P., Murgas, Felipe, Pallé, Enric, Anderson, David R., West, Richard G., Wittenmyer, Robert A., Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Zhang, Hui, Fairnington, Tyler, Okumura, Jack, Mengel, Matthew W., and Addison, Brett C.
Abstract: We report the discovery of two mini-Neptunes in near 2:1 resonance orbits ($P=7.610303$ d for HIP 113103 b and $P=14.245651$ d for HIP 113103 c) around the adolescent K-star HIP 113103 (TIC 121490076). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a $\sim$17.5 hour observation for the transits of both planets using ESA CHEOPS. We place $\leq4.5$ min and $\leq2.5$ min limits on the absence of transit timing variations over the three year photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of $R_{p}=1.829^{+0.096}_{-0.067}\,R_{\oplus}$, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius $R_{p}=2.40^{+0.10}_{-0.08}\,R_{\oplus}$ for HIP 113103 c, and close proximity of both planets to HIP 113103, it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST, HST, and Twinkle. It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population., Comment: 18 pages, 12 figures, published in the Monthly Notices of the Royal Astronomical Society
Published: 2023

7. An M dwarf accompanied by a close-in giant orbiter with SPECULOOS

Author: Triaud, Amaury H. M. J., Dransfield, Georgina, Kagetani, Taiki, Timmermans, Mathilde, Narita, Norio, Barkaoui, Khalid, Hirano, Teruyuki, Rackham, Benjamin V., Mori, Mayuko, Baycroft, Thomas, Benkhaldoun, Zouhair, Burgasser, Adam J., Caldwell, Douglas A., Collins, Karen A., Davis, Yasmin T., Delrez, Laetitia, Demory, Brice-Oliver, Ducrot, Elsa, Fukui, Akihiko, Muñoz, Clàudia Jano, Jehin, Emmanuël, García, Lionel J., Ghachoui, Mourad, Gillon, Michaël, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Ikoma, Masahiro, Kawauchi, Kiyoe, Kotani, Takayuki, Levine, Alan M., Pallé, Enric, Pedersen, Peter P., Pozuelos, Francisco J., Queloz, Didier, Scutt, Owen J., Seager, Sara, Sebastian, Daniel, Tamura, Motohide, Thompson, Samantha, Watanabe, Noriharu, de Wit, Julien, Winn, Joshua N., Zúñiga-Fernández, Sebastián, Triaud, Amaury H. M. J., Dransfield, Georgina, Kagetani, Taiki, Timmermans, Mathilde, Narita, Norio, Barkaoui, Khalid, Hirano, Teruyuki, Rackham, Benjamin V., Mori, Mayuko, Baycroft, Thomas, Benkhaldoun, Zouhair, Burgasser, Adam J., Caldwell, Douglas A., Collins, Karen A., Davis, Yasmin T., Delrez, Laetitia, Demory, Brice-Oliver, Ducrot, Elsa, Fukui, Akihiko, Muñoz, Clàudia Jano, Jehin, Emmanuël, García, Lionel J., Ghachoui, Mourad, Gillon, Michaël, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Ikoma, Masahiro, Kawauchi, Kiyoe, Kotani, Takayuki, Levine, Alan M., Pallé, Enric, Pedersen, Peter P., Pozuelos, Francisco J., Queloz, Didier, Scutt, Owen J., Seager, Sara, Sebastian, Daniel, Tamura, Motohide, Thompson, Samantha, Watanabe, Noriharu, de Wit, Julien, Winn, Joshua N., and Zúñiga-Fernández, Sebastián
Abstract: In the last decade, a dozen close-in giant planets have been discovered orbiting stars with spectral types ranging from M0 to M4, a mystery since known formation pathways do not predict the existence of such systems. Here, we confirm TOI-4860 b, a Jupiter-sized planet orbiting an M4.5 host, a star at the transition between fully and partially convective interiors. First identified with TESS data, we validate the transiting companion's planetary nature through multicolour photometry from the TRAPPIST-South/North, SPECULOOS, and MuSCAT3 facilities. Our analysis yields a radius of $0.76 \pm 0.02~ \rm R_{Jup}$ for the planet, a mass of $0.34~\rm M_\odot$ for the star, and an orbital period of 1.52 d. Using the newly commissioned SPIRIT InGaAs camera at the SPECULOOS-South Observatory, we collect infrared photometry in zYJ that spans the time of secondary eclipse. These observations do not detect a secondary eclipse, placing an upper limit on the brightness of the companion. The planetary nature of the companion is further confirmed through high-resolution spectroscopy obtained with the IRD spectrograph at Subaru Telescope, from which we measure a mass of $0.67 \pm 0.14~\rm M_{Jup}$ . Based on its overall density, TOI-4860 b appears to be rich in heavy elements, like its host star., Comment: Accepted for publication in MNRAS Letters
Published: 2023
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8. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906

Author: Tuson, Amy, Queloz, Didier, Osborn, Hugh P., Wilson, Thomas G., Hooton, Matthew J., Beck, Mathias, Lendl, Monika, Olofsson, Göran, Fortier, Andrea, Bonfanti, Andrea, Brandeker, Alexis, Buchhave, Lars A., Cameron, Andrew Collier, Ciardi, David R., Collins, Karen A., Gandolfi, Davide, Garai, Zoltan, Giacalone, Steven, da Silva, João Gomes, Howell, Steve B., Patel, Jayshil A., Persson, Carina M., Serrano, Luisa M., Sousa, Sérgio G., Ulmer-Moll, Solène, Vanderburg, Andrew, Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Borsato, Luca, Broeg, Christopher, Cabrera, Juan, Charnoz, Sébastien, Conti, Dennis M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dragomir, Diana, Dressing, Courtney D., Ehrenreich, David, Erikson, Anders, Essack, Zahra, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Furlan, Elise, Gill, Holden, Gillon, Michaël, Gnilka, Crystal L., Gonzales, Erica, Güdel, Manuel, Günther, Maximilian N., Hoyer, Sergio, Isaak, Kate G., Jenkins, Jon M., Kiss, Laszlo L., Laskar, Jacques, Latham, David W., Law, Nicholas, Etangs, Alain Lecavelier des, Curto, Gaspare Lo, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Mann, Andrew W., Maxted, Pierre F. L., Mayor, Michel, McDermott, Scott, Mecina, Marko, Mordasini, Christoph, Mortier, Annelies, Nascimbeni, Valerio, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Pritchard, Tyler, Ragazzoni, Roberto, Rando, Nicola, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Savel, Arjun B., Scandariato, Gaetano, Schwarz, Richard P., Seager, Sara, Ségransan, Damien, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula M., Thomas, Nicolas, Torres, Guillermo, Tronsgaard, René, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valérie, Vanderspek, Roland, Venturini, Julia, Walton, Nicholas A., Winn, Joshua N., Wohler, Bill, Tuson, Amy, Queloz, Didier, Osborn, Hugh P., Wilson, Thomas G., Hooton, Matthew J., Beck, Mathias, Lendl, Monika, Olofsson, Göran, Fortier, Andrea, Bonfanti, Andrea, Brandeker, Alexis, Buchhave, Lars A., Cameron, Andrew Collier, Ciardi, David R., Collins, Karen A., Gandolfi, Davide, Garai, Zoltan, Giacalone, Steven, da Silva, João Gomes, Howell, Steve B., Patel, Jayshil A., Persson, Carina M., Serrano, Luisa M., Sousa, Sérgio G., Ulmer-Moll, Solène, Vanderburg, Andrew, Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Borsato, Luca, Broeg, Christopher, Cabrera, Juan, Charnoz, Sébastien, Conti, Dennis M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dragomir, Diana, Dressing, Courtney D., Ehrenreich, David, Erikson, Anders, Essack, Zahra, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Furlan, Elise, Gill, Holden, Gillon, Michaël, Gnilka, Crystal L., Gonzales, Erica, Güdel, Manuel, Günther, Maximilian N., Hoyer, Sergio, Isaak, Kate G., Jenkins, Jon M., Kiss, Laszlo L., Laskar, Jacques, Latham, David W., Law, Nicholas, Etangs, Alain Lecavelier des, Curto, Gaspare Lo, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Mann, Andrew W., Maxted, Pierre F. L., Mayor, Michel, McDermott, Scott, Mecina, Marko, Mordasini, Christoph, Mortier, Annelies, Nascimbeni, Valerio, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Pritchard, Tyler, Ragazzoni, Roberto, Rando, Nicola, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Savel, Arjun B., Scandariato, Gaetano, Schwarz, Richard P., Seager, Sara, Ségransan, Damien, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula M., Thomas, Nicolas, Torres, Guillermo, Tronsgaard, René, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valérie, Vanderspek, Roland, Venturini, Julia, Walton, Nicholas A., Winn, Joshua N., and Wohler, Bill
Abstract: We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., Comment: 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS
Published: 2023
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9. A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654

Author: Dai, Fei, Schlaufman, Kevin C., Reggiani, Henrique, Bouma, Luke, Howard, Andrew W., Chontos, Ashley, Pidhorodetska, Daria, Van Zandt, Judah, Murphy, Joseph M. Akana, Rubenzahl, Ryan A., Polanski, Alex S., Lubin, Jack, Beard, Corey, Giacalone, Steven, Holcomb, Rae, Batalha, Natalie M., Crossfield, Ian, Dressing, Courtney, Fulton, Benjamin, Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Weiss, Lauren M., Belinski, Alexander A., Boyle, Andrew W., Burke, Christopher J., Castro-González, Amadeo, Ciardi, David R., Daylan, Tansu, Fukui, Akihiko, Gill, Holden, Guerrero, Natalia M., Hellier, Coel, Howell, Steve B., Lillo-Box, Jorge, Murgas, Felipe, Narita, Norio, Pallé, Enric, Rodriguez, David R., Savel, Arjun B., Shporer, Avi, Stassun, Keivan G., Striegel, Stephanie, Caldwell, Douglas A., Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua N., Dai, Fei, Schlaufman, Kevin C., Reggiani, Henrique, Bouma, Luke, Howard, Andrew W., Chontos, Ashley, Pidhorodetska, Daria, Van Zandt, Judah, Murphy, Joseph M. Akana, Rubenzahl, Ryan A., Polanski, Alex S., Lubin, Jack, Beard, Corey, Giacalone, Steven, Holcomb, Rae, Batalha, Natalie M., Crossfield, Ian, Dressing, Courtney, Fulton, Benjamin, Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Weiss, Lauren M., Belinski, Alexander A., Boyle, Andrew W., Burke, Christopher J., Castro-González, Amadeo, Ciardi, David R., Daylan, Tansu, Fukui, Akihiko, Gill, Holden, Guerrero, Natalia M., Hellier, Coel, Howell, Steve B., Lillo-Box, Jorge, Murgas, Felipe, Narita, Norio, Pallé, Enric, Rodriguez, David R., Savel, Arjun B., Shporer, Avi, Stassun, Keivan G., Striegel, Stephanie, Caldwell, Douglas A., Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland, and Winn, Joshua N.
Abstract: We report the discovery and Doppler mass measurement of a 7.4-day 2.3-$R_\oplus$ mini-Neptune around a metal-poor K dwarf BD+29 2654 (TOI-2018). Based on a high-resolution Keck/HIRES spectrum, the Gaia parallax, and multi-wavelength photometry from the ultraviolet to the mid-infrared, we found that the host star has $T_{\text{eff}}=4174^{+34}_{-42}$ K, $\log{g}=4.62^{+0.02}_{-0.03}$, $[\text{Fe/H}]=-0.58\pm0.18$, $M_{\ast}=0.57\pm0.02~M_{\odot}$, and $R_{\ast}=0.62\pm0.01~R_{\odot}$. Precise Doppler measurements with Keck/HIRES revealed a planetary mass of $M_{\text{p}}=9.2\pm2.1~M_{\oplus}$ for TOI-2018 b. TOI-2018 b has a mass and radius that are consistent with an Earth-like core with a $\sim1\%$-by-mass hydrogen/helium envelope, or an ice-rock mixture. The mass of TOI-2018 b is close to the threshold for run-away accretion and hence giant planet formation. Such a threshold is predicted to be around 10$M_\oplus$ or lower for a low-metallicity (low-opacity) environment. If TOI-2018 b is a planetary core that failed to undergo run-away accretion, it may underline the reason why giant planets are rare around low-metallicity host stars (one possibility is their shorter disk lifetimes). With a K-band magnitude of 7.1, TOI-2018 b may be a suitable target for transmission spectroscopy with the James Webb Space Telescope. The system is also amenable to metastable Helium observation; the detection of a Helium exosphere would help distinguish between a H/He enveloped planet and a water world., Comment: 10 figures, 5 tables, accepted to AAS Journals
Published: 2023
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10. Two Warm Neptunes transiting HIP 9618 revealed by TESS & Cheops

Author: Osborn, Hugh P., Nowak, Grzegorz, Hébrard, Guillaume, Masseron, Thomas, Lillo-Box, J., Pallé, Enric, Bekkelien, Anja, Florén, Hans-Gustav, Guterman, Pascal, Simon, Attila E., Adibekyan, V., Bieryla, Allyson, Borsato, Luca, Brandeker, Alexis, Ciardi, David R., Cameron, Andrew Collier, Collins, Karen A., Egger, Jo A., Gandolfi, Davide, Hooton, Matthew J., Latham, David W., Lendl, Monika, Matthews, Elisabeth C., Tuson, Amy, Ulmer-Moll, Solène, Vanderburg, Andrew, Wilson, Thomas G., Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Arnold, Luc, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Belinski, Alexandr A., Benz, Willy, Biondi, Federico, Boisse, Isabelle, Bonfils, Xavier, Broeg, Christopher, Buchhave, Lars A., Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Guillen, Carlos Cardona, Carleo, Ilaria, Castro-González, Amadeo, Charnoz, Sébastien, Christiansen, Jessie, Cortes-Zuleta, Pia, Csizmadia, Szilard, Dalal, Shweta, Davies, Melvyn B., Deleuil, Magali, Delfosse, Xavier, Delrez, Laetitia, Demory, Brice-Olivier, Dunlavey, Ava B., Ehrenreich, David, Erikson, Anders, Fernandes, Rachel B., Fortier, Andrea, Forveille, Thierry, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Goeke, Robert F., Goliguzova, Maria V., Gonzales, Erica J., Günther, M. N., Güdel, Manuel, Heidari, Neda, Henze, Christopher E., Howell, Steve, Hoyer, Sergio, Frey, Jonas Immanuel, Isaak, Kate G., Jenkins, Jon M., Kiefer, Flavien, Kiss, Laszlo, Korth, Judith, Maxted, Pierre F. L., Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Lund, Michael B., Luque, Rafa, Magrin, Demetrio, Almenara, Jose Manuel, Martioli, Eder, Mecina, Marko, Medina, Jennifer V., Moldovan, Daniel, Morales-Calderón, María, Morello, Giuseppe, Moutou, Claire, Murgas, Felipe, Jensen, Eric L. N., Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Ribas, Ignasi, Ricker, George, Demangeon, Olivier D. S., Smith, Alexis M. S., Santos, Nuno, Scandariato, Gaetano, Seager, Sara, Sousa, Sergio G., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valerie, Vanderspek, Roland, Walton, Nicholas, Winn, Joshua N., Osborn, Hugh P., Nowak, Grzegorz, Hébrard, Guillaume, Masseron, Thomas, Lillo-Box, J., Pallé, Enric, Bekkelien, Anja, Florén, Hans-Gustav, Guterman, Pascal, Simon, Attila E., Adibekyan, V., Bieryla, Allyson, Borsato, Luca, Brandeker, Alexis, Ciardi, David R., Cameron, Andrew Collier, Collins, Karen A., Egger, Jo A., Gandolfi, Davide, Hooton, Matthew J., Latham, David W., Lendl, Monika, Matthews, Elisabeth C., Tuson, Amy, Ulmer-Moll, Solène, Vanderburg, Andrew, Wilson, Thomas G., Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Arnold, Luc, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Belinski, Alexandr A., Benz, Willy, Biondi, Federico, Boisse, Isabelle, Bonfils, Xavier, Broeg, Christopher, Buchhave, Lars A., Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Guillen, Carlos Cardona, Carleo, Ilaria, Castro-González, Amadeo, Charnoz, Sébastien, Christiansen, Jessie, Cortes-Zuleta, Pia, Csizmadia, Szilard, Dalal, Shweta, Davies, Melvyn B., Deleuil, Magali, Delfosse, Xavier, Delrez, Laetitia, Demory, Brice-Olivier, Dunlavey, Ava B., Ehrenreich, David, Erikson, Anders, Fernandes, Rachel B., Fortier, Andrea, Forveille, Thierry, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Goeke, Robert F., Goliguzova, Maria V., Gonzales, Erica J., Günther, M. N., Güdel, Manuel, Heidari, Neda, Henze, Christopher E., Howell, Steve, Hoyer, Sergio, Frey, Jonas Immanuel, Isaak, Kate G., Jenkins, Jon M., Kiefer, Flavien, Kiss, Laszlo, Korth, Judith, Maxted, Pierre F. L., Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Lund, Michael B., Luque, Rafa, Magrin, Demetrio, Almenara, Jose Manuel, Martioli, Eder, Mecina, Marko, Medina, Jennifer V., Moldovan, Daniel, Morales-Calderón, María, Morello, Giuseppe, Moutou, Claire, Murgas, Felipe, Jensen, Eric L. N., Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Ribas, Ignasi, Ricker, George, Demangeon, Olivier D. S., Smith, Alexis M. S., Santos, Nuno, Scandariato, Gaetano, Seager, Sara, Sousa, Sergio G., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valerie, Vanderspek, Roland, Walton, Nicholas, and Winn, Joshua N.
Abstract: HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright ($G=9.0$ mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of $3.9 \pm 0.044$ $R_\oplus$ (HIP 9618 b) and $3.343 \pm 0.039$ $R_\oplus$ (HIP 9618 c). While the 20.77291 day period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-day gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE and CAFE revealed a mass of $10.0 \pm 3.1 M_\oplus$ for HIP 9618 b, which, according to our interior structure models, corresponds to a $6.8\pm1.4\%$ gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of $< 18M_\oplus$. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion ($0.08^{+0.12}_{-0.05} M_\odot$) orbiting at $26^{+19}_{-11}$ au. This detection makes HIP 9618 one of only five bright ($K<8$ mag) transiting multi-planet systems known to host a planet with $P>50$ d, opening the door for the atmospheric characterisation of warm ($T_{\rm eq}<750$ K) sub-Neptunes., Comment: 19 pages, 16 figures, 9 tables. Accepted at MNRAS. CHEOPS, RV and ground-based photometric data is available on CDS at https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/523/3069
Published: 2023
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11. Characterisation of the upper atmospheres of HAT-P-32 b, WASP-69 b, GJ 1214 b, and WASP-76 b through their He I triplet absorption

Author: Ministerio de Ciencia e Innovación (España), European Research Council, European Commission, Lampón, M., López-Puertas, Manuel, Sanz-Forcada, J., Czesla, S., Nortmann, L., Casasayas-Barris, N., Orell-Miquel, J., Sánchez-López, A., Danielski, Camilla, Pallé, Enric, Molaverdikhani, K., Henning, Thomas, Caballero, J. A., Amado, Pedro J., Quirrenbach, Andreas, Reiners, Ansgar, Ribas, Ignasi, Ministerio de Ciencia e Innovación (España), European Research Council, European Commission, Lampón, M., López-Puertas, Manuel, Sanz-Forcada, J., Czesla, S., Nortmann, L., Casasayas-Barris, N., Orell-Miquel, J., Sánchez-López, A., Danielski, Camilla, Pallé, Enric, Molaverdikhani, K., Henning, Thomas, Caballero, J. A., Amado, Pedro J., Quirrenbach, Andreas, Reiners, Ansgar, and Ribas, Ignasi
Abstract: Characterisation of atmospheres undergoing photo-evaporation is key to understanding the formation, evolution, and diversity of planets. However, only a few upper atmospheres that experience this kind of hydrodynamic escape have been characterised. Our aim is to characterise the upper atmospheres of the hot Jupiters HAT-P-32b and WASP-69 b, the warm sub-Neptune GJ 1214 b, and the ultra-hot Jupiter WASP-76 b through high-resolution observations of their He I triplet absorption. In addition, we also reanalyse the warm Neptune GJ 3470 b and the hot Jupiter HD 189733 b. We used a spherically symmetric 1D hydrodynamic model coupled with a non-local thermodynamic equilibrium model for calculating the He I triplet distribution along the escaping outflow. Comparing synthetic absorption spectra with observations, we constrained the main parameters of the upper atmosphere of these planets and classify them according to their hydrodynamic regime. Our results show that HAT-P-32 b photo-evaporates at (130 ± 70) ×1011 g s−1 with a hot (12 400 ± 2900 K) upper atmosphere; WASP-69 b loses its atmosphere at (0.9 ± 0.5) ×1011 g s−1 and 5250 ± 750 K; and GJ 1214b, with a relatively cold outflow of 3750 ± 750 K, photo-evaporates at (1.3 ± 1.1) ×1011 g s−1. For WASP-76 b, its weak absorption prevents us from constraining its temperature and mass-loss rate significantly; we obtained ranges of 6000–17 000 K and 23.5 ± 21.5 ×1011 g s−1. Our reanalysis of GJ 3470 b yields colder temperatures, 3400 ± 350 K, but practically the same mass-loss rate as in our previous results. Our reanalysis of HD 189733 b yields a slightly higher mass-loss rate, (1.4 ± 0.5) × 1011 g s−1, and temperature, 12 700 ± 900 K compared to previous estimates. We also found that HAT-P-32 b, WASP-69 b, and WASP-76 b undergo hydrodynamic escape in the recombination-limited regime, and that GJ 1214 b is in the photon-limited regime. Our results support that photo-evaporated outflows tend to be very light, H/He ≳ 98/2. The d
Published: 2023

12. The CARMENES search for exoplanets around M dwarfs: A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data

Author: Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Space Agency, Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Blanco-Pozo, J., Perger, M., Damasso, M., Anglada-Escudé, Guillem, Ribas, Ignasi, Baroch, David, Caballero, J. A., Cifuentes, C., Jeffers, Sandra V., Lafarga, M., Kaminski, Adrian, Kaur, Simranpreet, Nagel, Evangelos, Perdelwitz, Volker, Pérez-Torres, Miguel A., Sozzetti, Alessandro, Viganò, Daniele, Amado, Pedro J., Andreuzzi, G., Béjar, Victor J. S., Brown, E. L., Del Sordo, F., Dreizler, S., Galadí-Enriquez, D., Hatzes, Artie P., Kürster, M., Lanza, A. F., Melis, A., Molinari, Emilio, Montes, D., Murgia, M., Pallé, Enric, Peña-Moñino, Luis, Perrodin, D., Pilia, Maura, Poretti, Ennio, Quirrenbach, Andreas, Reiners, Ansgar, Schweitzer, Andreas, Zapatero Osorio, María Rosa, Zechmeister, Mathias, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Space Agency, Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Blanco-Pozo, J., Perger, M., Damasso, M., Anglada-Escudé, Guillem, Ribas, Ignasi, Baroch, David, Caballero, J. A., Cifuentes, C., Jeffers, Sandra V., Lafarga, M., Kaminski, Adrian, Kaur, Simranpreet, Nagel, Evangelos, Perdelwitz, Volker, Pérez-Torres, Miguel A., Sozzetti, Alessandro, Viganò, Daniele, Amado, Pedro J., Andreuzzi, G., Béjar, Victor J. S., Brown, E. L., Del Sordo, F., Dreizler, S., Galadí-Enriquez, D., Hatzes, Artie P., Kürster, M., Lanza, A. F., Melis, A., Molinari, Emilio, Montes, D., Murgia, M., Pallé, Enric, Peña-Moñino, Luis, Perrodin, D., Pilia, Maura, Poretti, Ennio, Quirrenbach, Andreas, Reiners, Ansgar, Schweitzer, Andreas, Zapatero Osorio, María Rosa, and Zechmeister, Mathias
Abstract: [Context] Detecting a planetary companion in a short-period orbit through radio emission from the interaction with its host star is a new prospect in exoplanet science. Recently, a tantalising signal was found close to the low-mass stellar system GJ 1151 using LOFAR observations., [Aims] We studied spectroscopic time-series data of GJ 1151 in order to search for planetary companions, investigate possible signatures of stellar magnetic activity, and to find possible explanations for the radio signal., [Methods] We used the combined radial velocities measured from spectra acquired with the CARMENES, HARPS-N, and HPF instruments, extracted activity indices from those spectra in order to mitigate the impact of stellar magnetic activity on the data, and performed a detailed analysis of Gaia astrometry and all available photometric time series coming from the MEarth and ASAS-SN surveys., [Results] We found a M > 10.6 M⊕ companion to GJ 1151 in a 390d orbit at a separation of 0.57 au. Evidence for a second modulation is also present; this could be due to long-term magnetic variability or a second (substellar) companion. The star shows episodes of elevated magnetic activity, one of which could be linked to the observed LOFAR radio emission. We show that it is highly unlikely that the detected GJ 1151 c, or any additional outer companion is the source of the detected signal. We cannot firmly rule out the suggested explanation of an undetected short-period planet that could be related to the radio emission, as we establish an upper limit of 1.2 M⊕ for the minimum mass.
Published: 2023

13. The CARMENES search for exoplanets around M dwarfs. A sub-Neptunian mass planet in the habitable zone of HN Lib

Author: Ministerio de Ciencia e Innovación (España), European Commission, González-Álvarez, E., Kemmer, J., Chaturvedi, P., Caballero, J. A., Quirrenbach, Andreas, Amado, Pedro J., Béjar, Victor J. S., Cifuentes, C., Herrero, E., Kossakowski, D., Reiners, Ansgar, Ribas, Ignasi, Rodríguez Martínez, Eloy, Rodríguez López, C., Sanz-Forcada, J., Shan, Y., Stock, S., Tabernero, H. M., Tal-Or, L., Zapatero Osorio, María Rosa, Hatzes, Artie P., Henning, Thomas, López González, Maria J., Montes, D., Morales, Juan Carlos, Pallé, Enric, Pedraz, S., Perger, M., Reffert, S., Sabotta, S., Schweitzer, Andreas, Zechmeister, Mathias, Ministerio de Ciencia e Innovación (España), European Commission, González-Álvarez, E., Kemmer, J., Chaturvedi, P., Caballero, J. A., Quirrenbach, Andreas, Amado, Pedro J., Béjar, Victor J. S., Cifuentes, C., Herrero, E., Kossakowski, D., Reiners, Ansgar, Ribas, Ignasi, Rodríguez Martínez, Eloy, Rodríguez López, C., Sanz-Forcada, J., Shan, Y., Stock, S., Tabernero, H. M., Tal-Or, L., Zapatero Osorio, María Rosa, Hatzes, Artie P., Henning, Thomas, López González, Maria J., Montes, D., Morales, Juan Carlos, Pallé, Enric, Pedraz, S., Perger, M., Reffert, S., Sabotta, S., Schweitzer, Andreas, and Zechmeister, Mathias
Abstract: We report the discovery of HN Lib b, a sub-Neptunian mass planet orbiting the nearby (d ≈ = 6.25 pc) M4.0 V star HN Lib detected by our CARMENES radial-velocity (RV) survey. We determined a planetary minimum mass of Mb sin i = 5.46 ± 0.75 M⊕ and an orbital period of Pb = 36.116 ± 0.029 d, using ~5 yr of CARMENES data, as well as archival RVs from HARPS and HIRES spanning more than 13 yr. The flux received by the planet equals half the instellation on Earth, which places it in the middle of the conservative habitable zone (HZ) of its host star. The RV data show evidence for another planet candidate with M[c] sin i = 9.7 ± 1.9 M⊕ and P[c] = 113.46 ± 0.20 d. The long-term stability of the signal and the fact that the best model for our data is a two-planet model with an independent activity component stand as strong arguments for establishing a planetary origin. However, we cannot rule out stellar activity due to its proximity to the rotation period of HN Lib, which we measured using CARMENES activity indicators and photometric data from a ground-based multi-site campaign as well as archival data. The discovery adds HN Lib b to the shortlist of super-Earth planets in the habitable zone of M dwarfs, but HN Lib [c] probably cannot be inhabited because, if confirmed, it would most likely be an icy giant. © The Authors 2023.
Published: 2023

14. Two temperate earth-mass planets orbiting the nearby star GJ 1002

Author: Ministerio de Ciencia e Innovación (España), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Superior de Investigaciones Científicas (España), Fundação para a Ciência e a Tecnologia (Portugal), Junta de Andalucía, Swiss National Science Foundation, Gobierno de Canarias, Suárez Mascareño, A., González-Álvarez, E., Zapatero Osorio, María Rosa, Lillo-Box, Jorge, Faria, J. P., Passegger, V.M., González Hernández, Jonay I., Figueira, Pedro, Sozzetti, Alessandro, Rebolo López, Rafael, Pepe, F., Santos, Nuno C., Cristiani, Stefano, Lovis, Christophe, Silva, André, Ribas, Ignasi, Amado, Pedro J., Caballero, J. A., Quirrenbach, Andreas, Reiners, Ansgar, Zechmeister, Mathias, Adibekyan, Vardan, Alibert, Y., Béjar, Victor J. S., Benatti, S., D'Odorico, Valentina, Damasso, M., Delisle, J. -B., Di Marcantonio, P., Dreizler, S., Ehrenreich, David, Hatzes, Artie P., Hara, N. C., Henning, Thomas, Kaminski, Adriaan, López González, Maria J., Martins, C.J.A.P., Micela, Giusi, Montes, D., Pallé, Enric, Pedraz, S., Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Tal-Or, L., Sousa, S. G., Udry, Stephane, Ministerio de Ciencia e Innovación (España), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Superior de Investigaciones Científicas (España), Fundação para a Ciência e a Tecnologia (Portugal), Junta de Andalucía, Swiss National Science Foundation, Gobierno de Canarias, Suárez Mascareño, A., González-Álvarez, E., Zapatero Osorio, María Rosa, Lillo-Box, Jorge, Faria, J. P., Passegger, V.M., González Hernández, Jonay I., Figueira, Pedro, Sozzetti, Alessandro, Rebolo López, Rafael, Pepe, F., Santos, Nuno C., Cristiani, Stefano, Lovis, Christophe, Silva, André, Ribas, Ignasi, Amado, Pedro J., Caballero, J. A., Quirrenbach, Andreas, Reiners, Ansgar, Zechmeister, Mathias, Adibekyan, Vardan, Alibert, Y., Béjar, Victor J. S., Benatti, S., D'Odorico, Valentina, Damasso, M., Delisle, J. -B., Di Marcantonio, P., Dreizler, S., Ehrenreich, David, Hatzes, Artie P., Hara, N. C., Henning, Thomas, Kaminski, Adriaan, López González, Maria J., Martins, C.J.A.P., Micela, Giusi, Montes, D., Pallé, Enric, Pedraz, S., Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Tal-Or, L., Sousa, S. G., and Udry, Stephane
Abstract: We report the discovery and characterisation of two Earth-mass planets orbiting in the habitable zone of the nearby M-dwarf GJ 1002 based on the analysis of the radial-velocity (RV) time series from the ESPRESSO and CARMENES spectrographs. The host star is the quiet M5.5 V star GJ 1002 (relatively faint in the optical, V ~ 13.8 mag, but brighter in the infrared, J ~ 8.3 mag), located at 4.84 pc from the Sun. We analyse 139 spectroscopic observations taken between 2017 and 2021. We performed a joint analysis of the time series of the RV and full-width half maximum (FWHM) of the cross-correlation function (CCF) to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with the stellar activity. We detect the signal of two planets orbiting GJ 1002. GJ 1002 b is a planet with a minimum mass mp sin i of 1.08 ± 0.13 M⊕ with an orbital period of 10.3465 ± 0.0027 days at a distance of 0.0457 ± 0.0013 au from its parent star, receiving an estimated stellar flux of 0.67 F⊕. GJ 1002 c is a planet with a minimum mass mp sin i of 1.36 ± 0.17 M⊕ with an orbital period of 20.202 ± 0.013 days at a distance of 0.0738 ± 0.0021 au from its parent star, receiving an estimated stellar flux of 0.257 F⊕. We also detect the rotation signature of the star, with a period of 126 ± 15 days. We find that there is a correlation between the temperature of certain optical elements in the spectrographs and changes in the instrumental profile that can affect the scientific data, showing a seasonal behaviour that creates spurious signals at periods longer than ~200 days. GJ 1002 is one of the few known nearby systems with planets that could potentially host habitable environments. The closeness of the host star to the Sun makes the angular sizes of the orbits of both planets (~9.7 mas and ~15.7 mas, respectively) large enough for their atmosphere to be studied via high-contrast high-resolution spectroscopy with instruments such as the future spectrog
Published: 2023

15. GJ 806 (TOI-4481): A bright nearby multi-planetary system with a transiting hot low-density super-Earth

Author: German Research Foundation, National Aeronautics and Space Administration (US), European Commission, Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), Ministerio de Ciencia e Innovación (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Generalitat de Catalunya, Japan Society for the Promotion of Science, Pallé, Enric, Morales, Juan Carlos, Sanz-Forcada, J., Caballero, J. A., Ribas, Ignasi, Pérez-Torres, Miguel A., Luque, Rafael, Aceituno, Francisco José, Amado, Pedro J., Anglada-Escudé, Guillem, Cifuentes, C., Herrero, E., Lillo-Box, Jorge, López González, Maria J., Rodríguez, C., Rodríguez-López, Cristina, Zapatero Osorio, María Rosa, German Research Foundation, National Aeronautics and Space Administration (US), European Commission, Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), Ministerio de Ciencia e Innovación (España), Agencia Estatal de Investigación (España), Junta de Andalucía, Generalitat de Catalunya, Japan Society for the Promotion of Science, Pallé, Enric, Morales, Juan Carlos, Sanz-Forcada, J., Caballero, J. A., Ribas, Ignasi, Pérez-Torres, Miguel A., Luque, Rafael, Aceituno, Francisco José, Amado, Pedro J., Anglada-Escudé, Guillem, Cifuentes, C., Herrero, E., Lillo-Box, Jorge, López González, Maria J., Rodríguez, C., Rodríguez-López, Cristina, and Zapatero Osorio, María Rosa
Abstract: One of the main scientific goals of the TESS mission is the discovery of transiting small planets around the closest and brightest stars in the sky. Here, using data from the CARMENES, MAROON-X, and HIRES spectrographs together with TESS, we report the discovery and mass determination of aplanetary system around the M1.5 V star GJ 806 (TOI-4481). GJ 806 is a bright (V ≈ 10.8mag, J ≈ 7.3 mag) and nearby (d = 12 pc) M dwarf that hosts at least two planets. The innermost planet, GJ 806 b, is transiting and has an ultra-short orbital period of 0.93 d, a radius of 1.331 ± 0.023 R⊕, a mass of 1.90 ± 0.17 M⊕, a mean density of 4.40 ± 0.45 g cm−3, and an equilibrium temperature of 940 ± 10 K. We detect a second, non-transiting, super-Earth planet in the system, GJ 806 c, with an orbital period of 6.6 d, a minimum mass of 5.80 ± 0.30 M⊕, and an equilibrium temperature of 490 ± 5 K. The radial velocity data also shows evidence for a third periodicity at 13.6 d, although the current dataset does not provide sufficient evidence to unambiguously distinguish between a third super-Earth mass (M sin i = 8.50 ± 0.45 M⊕) planet or stellar activity. Additionally, we report one transit observation of GJ 806 b taken with CARMENES in search of a possible extended atmosphere of H or He, but we can only place upper limits to its existence. This is not surprising as our evolutionary models support the idea that any possible primordial H/He atmosphere that GJ 806 b might have had would be long lost. However, the bulk density of GJ 806 b makes it likely that the planet hosts some type of volatile atmosphere. With transmission spectroscopy metrics (TSM) of 44 and emission spectroscopy metrics (ESM) of 24, GJ 806 b is to date the third-ranked terrestrial planet around an M dwarf suitable for transmission spectroscopy studies using JWST, and the most promising terrestrial planet for emission spectroscopy studies. GJ 806b is also an excellent target for the detection of radio emission via star-pl
Published: 2023

16. Masses, Revised Radii, and a Third Planet Candidate in the 'Inverted' Planetary System Around TOI-1266

Author: Cloutier, Ryan, Greklek-McKeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris A., Cloutier, Ryan, Greklek-McKeon, Michael, Wurmser, Serena, Cherubim, Collin, Gillis, Erik, Vanderburg, Andrew, Hadden, Sam, Cadieux, Charles, Artigau, Étienne, Vissapragada, Shreyas, Mortier, Annelies, López-Morales, Mercedes, Latham, David W., Knutson, Heather, Haywood, Raphaëlle D., Pallé, Enric, Doyon, René, Cook, Neil, Andreuzzi, Gloria, Cecconi, Massimo, Cosentino, Rosario, Ghedina, Adriano, Harutyunyan, Avet, Pinamonti, Matteo, Stalport, Manu, Damasso, Mario, Rescigno, Federica, Wilson, Thomas G., Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Dumusque, Xavier, Lovis, Christophe, Mayor, Michel, Molinari, Emilio, Pepe, Francesco, Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris A.
Abstract: Is the population of close-in planets orbiting M dwarfs sculpted by thermally driven escape or is it a direct outcome of the planet formation process? A number of recent empirical results strongly suggest the latter. However, the unique architecture of the TOI-1266 system presents a challenge to models of planet formation and atmospheric escape given its seemingly "inverted" architecture of a large sub-Neptune ($P_b=10.9$ days, $R_{p,b}=2.62\pm 0.11\, \mathrm{R}_{\oplus}$) orbiting interior to that of the system's smaller planet ($P_c=18.8$ days, $R_{p,c}=2.13\pm 0.12\, \mathrm{R}_{\oplus}$). Here we present revised planetary radii based on new TESS and diffuser-assisted ground-based transit observations, and characterize both planetary masses using a set of 145 radial velocity measurements from HARPS-N ($M_{p,b}=4.23\pm 0.69\, \mathrm{M}_{\oplus}, M_{p,c}=2.88\pm 0.80\, \mathrm{M}_{\oplus}$). Our analysis also reveals a third planet candidate ($P_d=32.3$ days, $M_{p,d}\sin{i} = 4.59^{+0.96}_{-0.94}\, \mathrm{M}_{\oplus}$), which if real, would form a chain of near 5:3 period ratios, although the system is likely not in a mean motion resonance. Our results indicate that TOI-1266 b and c are among the lowest density sub-Neptunes around M dwarfs and likely exhibit distinct bulk compositions of a gas-enveloped terrestrial ($X_{\mathrm{env},b}=5.5\pm 0.7$%) and a water-rich world (WMF$_c=59\pm 14$%), which is supported by hydrodynamic escape models. If distinct bulk compositions are confirmed through atmospheric characterization, the system's unique architecture would represent an interesting test case of inside-out sub-Neptune formation at pebble traps., Comment: Accepted for publication in MNRAS. 21 pages. Our spectroscopic time series are included in the arXiv source files as table6.csv
Published: 2023

17. Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

Author: Osborn, Hugh P., Bonfanti, Andrea, Gandolfi, Davide, Hedges, Christina, Leleu, Adrien, Fortier, Andrea, Futyan, David, Gutermann, Pascal, Maxted, Pierre F. L., Borsato, Luca, Collins, Karen A., da Silva, J. Gomes, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Lendl, Monika, Parviainen, Hannu, Salmon, Sébastien, Schanche, Nicole, Serrano, Luisa M., Sousa, Sergio G., Tuson, Amy, Ulmer-Moll, Solène, Van Grootel, Valerie, Wells, R. D., Wilson, Thomas G., Alibert, Yann, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Biondi, Federico, Bonfils, Xavier, Bouchy, Francois, Brandeker, Alexis, Broeg, Christopher, Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Charnoz, Sébastien, Cameron, Andrew Collier, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demory, Brice-Olivier, Ehrenreich, David, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Gómez-Muñoz, M. A., Güdel, Manuel, Heng, Kevin, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo, Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Magrin, Demetrio, Malavolta, Luca, McCormac, James, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Demangeon, Olivier D. S., Smith, Alexis M. S., Sabin, L., Santos, Nuno, Scandariato, Gaetano, Schroffenegger, U., Schwarz, Rick P., Shporer, Avi, Simon, Attila E., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Walter, Ingo, Walton, Nicholas, Osborn, Hugh P., Bonfanti, Andrea, Gandolfi, Davide, Hedges, Christina, Leleu, Adrien, Fortier, Andrea, Futyan, David, Gutermann, Pascal, Maxted, Pierre F. L., Borsato, Luca, Collins, Karen A., da Silva, J. Gomes, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Lendl, Monika, Parviainen, Hannu, Salmon, Sébastien, Schanche, Nicole, Serrano, Luisa M., Sousa, Sergio G., Tuson, Amy, Ulmer-Moll, Solène, Van Grootel, Valerie, Wells, R. D., Wilson, Thomas G., Alibert, Yann, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Biondi, Federico, Bonfils, Xavier, Bouchy, Francois, Brandeker, Alexis, Broeg, Christopher, Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Charnoz, Sébastien, Cameron, Andrew Collier, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demory, Brice-Olivier, Ehrenreich, David, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Gómez-Muñoz, M. A., Güdel, Manuel, Heng, Kevin, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo, Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Magrin, Demetrio, Malavolta, Luca, McCormac, James, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Demangeon, Olivier D. S., Smith, Alexis M. S., Sabin, L., Santos, Nuno, Scandariato, Gaetano, Schroffenegger, U., Schwarz, Rick P., Shporer, Avi, Simon, Attila E., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Walter, Ingo, and Walton, Nicholas
Abstract: Context: TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young ($340\pm80$ Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims: To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods: We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results: CHEOPS observations revealed a clear detection for TOI-2076 c at $P=21.01538^{+0.00084}_{-0.00074}$ d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the $P=35.12537\pm0.00067$ d alias. These observations also improved the radius precision of all three sub-Neptunes to $2.518\pm0.036$, $3.497\pm0.043$, and $3.232\pm0.063$ $R_\oplus$. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST., Comment: 18 pages, 7 figure, 8 tables. Accepted for publication in Astronomy & Astrophysics. Photometry available on CDS/Vizier. Python package presented for modelling duotransiting planet candidates available at https://github.com/hposborn/MonoTools. Modelling & figure-creation code available at https://github.com/hposborn/TOI2076
Published: 2022
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18. TOI-2119: A transiting brown dwarf orbiting an active M-dwarf from NASA's TESS mission

Author: Carmichael, Theron W., Irwin, Jonathan M., Murgas, Felipe, Pallé, Enric, Stassun, Keivan G., Collins, Karen A., de Leon, Jerome, Esparza-Borges, Emma, Fong, William, Fukui, Akihiko, Jenkins, Jon M., Kagetani, Taiki, Latham, David W., Lund, Michael B., Mann, Andrew W., Moldovan, Dan, Morgan, Edward H., Narita, Norio, Parviainen, Hannu, Quintana, Elisa V., Ricker, George R., Seager, Sara, Schwarz, Richard P., Twicken, Joseph D., Winn, Joshua N., Carmichael, Theron W., Irwin, Jonathan M., Murgas, Felipe, Pallé, Enric, Stassun, Keivan G., Collins, Karen A., de Leon, Jerome, Esparza-Borges, Emma, Fong, William, Fukui, Akihiko, Jenkins, Jon M., Kagetani, Taiki, Latham, David W., Lund, Michael B., Mann, Andrew W., Moldovan, Dan, Morgan, Edward H., Narita, Norio, Parviainen, Hannu, Quintana, Elisa V., Ricker, George R., Seager, Sara, Schwarz, Richard P., Twicken, Joseph D., and Winn, Joshua N.
Abstract: We report the discovery of TOI-2119b, a transiting brown dwarf (BD) that orbits and is completely eclipsed by an active M-dwarf star. Using light curve data from the Transiting Exoplanet Survey Satellite mission and follow up high-resolution Doppler spectroscopic observations, we find the BD has a radius of $R_b = 1.08 \pm 0.03{\rm R_J}$, a mass of $M_b = 64.4 \pm 2.3{\rm M_J}$, an orbital period of $P = 7.200865 \pm 0.00002$ days, and an eccentricity of $e=0.337\pm 0.002$. The host star has a mass of $M_\star = 0.53 \pm 0.02{\rm M_\odot}$, a radius of $R_\star= 0.50 \pm 0.01{\rm R_\odot}$, an effective temperature of $T_{\rm eff} = 3621 \pm 48{\rm K}$, and a metallicity of $\rm [Fe/H]=+0.06\pm 0.08$. TOI-2119b joins an emerging population of transiting BDs around M-dwarf host stars, with TOI-2119 being the ninth such system. These M-dwarf--brown dwarf systems occupy mass ratios near $q = M_b/M_\star \approx 0.1$, which separates them from the typical mass ratios for systems with transiting substellar objects and giant exoplanets that orbit more massive stars. TOI-2119 is also one of the most active M-dwarf stars known to host a transiting brown dwarf. The nature of the secondary eclipse of the BD by the star enables us to estimate the effective temperature of the substellar object to be $2030\pm 84 {\rm K}$, which is consistent with predictions by substellar evolutionary models., Comment: 13 pages, 13 figures, 4 tables, submitted to MNRAS
Published: 2022

19. A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Author: Espinoza, Néstor, Pallé, Enric, Kemmer, Jonas, Luque, Rafael, Caballero, José A., Cifuentes, Carlos, Herrero, Enrique, Béjar, Víctor J. Sánchez, Stock, Stephan, Molaverdikhani, Karan, Morello, Giuseppe, Kossakowski, Diana, Schlecker, Martin, Amado, Pedro J., Bluhm, Paz, Cortés-Contreras, Miriam, Henning, Thomas, Kreidberg, Laura, Kürster, Martin, Lafarga, Marina, Lodieu, Nicolas, Morales, Juan Carlos, Oshagh, Mahmoudreza, Passegger, Vera M., Pavlov, Alexey, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rodríguez, Eloy, López, Cristina Rodríguez, Schweitzer, Andreas, Trifonov, Trifon, Chaturvedi, Priyanka, Dreizler, Stefan, Jeffers, Sandra V., Kaminski, Adrian, López-González, María José, Lillo-Box, Jorge, Montes, David, Nowak, Grzegorz, Pedraz, Santos, Vanaverbeke, Siegfried, Osorio, Maria R. Zapatero, Zechmeister, Mathias, Collins, Karen A., Girardin, Eric, Guerra, Pere, Naves, Ramon, Crossfield, Ian J. M., Matthews, Elisabeth C., Howell, Steve B., Ciardi, David R., Gonzales, Erica, Matson, Rachel A., Beichman, Charles A., Schlieder, Joshua E., Barclay, Thomas, Vezie, Michael, Villaseñor, Jesus Noel, Daylan, Tansu, Mireies, Ismael, Dragomir, Diana, Twicken, Joseph D., Jenkins, Jon, Winn, Joshua N., Latham, David, Ricker, George, Seager, Sara, Espinoza, Néstor, Pallé, Enric, Kemmer, Jonas, Luque, Rafael, Caballero, José A., Cifuentes, Carlos, Herrero, Enrique, Béjar, Víctor J. Sánchez, Stock, Stephan, Molaverdikhani, Karan, Morello, Giuseppe, Kossakowski, Diana, Schlecker, Martin, Amado, Pedro J., Bluhm, Paz, Cortés-Contreras, Miriam, Henning, Thomas, Kreidberg, Laura, Kürster, Martin, Lafarga, Marina, Lodieu, Nicolas, Morales, Juan Carlos, Oshagh, Mahmoudreza, Passegger, Vera M., Pavlov, Alexey, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rodríguez, Eloy, López, Cristina Rodríguez, Schweitzer, Andreas, Trifonov, Trifon, Chaturvedi, Priyanka, Dreizler, Stefan, Jeffers, Sandra V., Kaminski, Adrian, López-González, María José, Lillo-Box, Jorge, Montes, David, Nowak, Grzegorz, Pedraz, Santos, Vanaverbeke, Siegfried, Osorio, Maria R. Zapatero, Zechmeister, Mathias, Collins, Karen A., Girardin, Eric, Guerra, Pere, Naves, Ramon, Crossfield, Ian J. M., Matthews, Elisabeth C., Howell, Steve B., Ciardi, David R., Gonzales, Erica, Matson, Rachel A., Beichman, Charles A., Schlieder, Joshua E., Barclay, Thomas, Vezie, Michael, Villaseñor, Jesus Noel, Daylan, Tansu, Mireies, Ismael, Dragomir, Diana, Twicken, Joseph D., Jenkins, Jon, Winn, Joshua N., Latham, David, Ricker, George, and Seager, Sara
Abstract: We report the discovery and characterization of TOI-1759~b, a temperate (400 K) sub-Neptune-sized exoplanet orbiting the M~dwarf TOI-1759 (TIC 408636441). TOI-1759 b was observed by TESS to transit on sectors 16, 17 and 24, with only one transit observed per sector, creating an ambiguity on the orbital period of the planet candidate. Ground-based photometric observations, combined with radial-velocity measurements obtained with the CARMENES spectrograph, confirm an actual period of $18.85019 \pm 0.00014$ d. A joint analysis of all available photometry and radial velocities reveal a radius of $3.17 \pm 0.10\,R_\oplus$ and a mass of $10.8 \pm 1.5\,M_\oplus$. Combining this with the stellar properties derived for TOI-1759 ($R_\star = 0.597 \pm 0.015\,R_\odot$; $M_\star = 0.606 \pm 0.020\,M_\odot$; $T_{\textrm{eff}} = 4065 \pm 51$ K), we compute a transmission spectroscopic metric (TSM) value of over 80 for the planet, making it a good target for transmission spectroscopy studies. TOI-1759 b is among the top five temperate, small exoplanets ($T_\textrm{eq} < 500$ K, $R_p < 4 \,R_\oplus$) with the highest TSM discovered to date. Two additional signals with periods of 80 d and $>$ 200 d seem to be present in our radial velocities. While our data suggest both could arise from stellar activity, the later signal's source and periodicity are hard to pinpoint given the $\sim 200$ d baseline of our radial-velocity campaign with CARMENES. Longer baseline radial-velocity campaigns should be performed in order to unveil the true nature of this long period signal., Comment: 22 pages, 10 figures, 7 tables. AJ in press
Published: 2022
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20. A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Author: Wilson, Thomas G., Goffo, Elisa, Alibert, Yann, Gandolfi, Davide, Bonfanti, Andrea, Persson, Carina M., Cameron, Andrew Collier, Fridlund, Malcolm, Fossati, Luca, Korth, Judith, Benz, Willy, Deline, Adrien, Florén, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sébastien, Sousa, Sérgio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Bárczy, Tamas, Navascues, David Barrado y, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Billot, Nicolas, Bonfils, Xavier, Brandeker, Alexis, Broeg, Christopher, Bryant, Edward M., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Charnoz, Sébastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colón, Knicole D., Crouzet, Nicolas, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Dragomir, Diana, Dransfield, Georgina, Ehrenreich, David, Erikson, Anders, Fortier, Andrea, Gan, Tianjun, Gill, Samuel, Gillon, Michaël, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Güdel, Manuel, Guillot, Tristan, Haldemann, Jonas, Heng, Kevin, Horne, Keith, Howell, Steve B., Isaak, Kate G., Jenkins, Jon M., Jensen, Eric L. N., Kiss, Laszlo, Lacedelli, Gaia, Lam, Kristine, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavelier des, Lendl, Monika, Lester, Kathryn V., Levine, Alan M., Livingston, John, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Marie-Sainte, Wenceslas, Maxted, Pierre F. L., Mayo, Andrew W., McLean, Brian, Mecina, Marko, Mékarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Ségransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stéphane, Van Eylen, Vincent, Van Grootel, Valérie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, Winn, Joshua N., Wilson, Thomas G., Goffo, Elisa, Alibert, Yann, Gandolfi, Davide, Bonfanti, Andrea, Persson, Carina M., Cameron, Andrew Collier, Fridlund, Malcolm, Fossati, Luca, Korth, Judith, Benz, Willy, Deline, Adrien, Florén, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sébastien, Sousa, Sérgio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Bárczy, Tamas, Navascues, David Barrado y, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Billot, Nicolas, Bonfils, Xavier, Brandeker, Alexis, Broeg, Christopher, Bryant, Edward M., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Charnoz, Sébastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colón, Knicole D., Crouzet, Nicolas, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Dragomir, Diana, Dransfield, Georgina, Ehrenreich, David, Erikson, Anders, Fortier, Andrea, Gan, Tianjun, Gill, Samuel, Gillon, Michaël, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Güdel, Manuel, Guillot, Tristan, Haldemann, Jonas, Heng, Kevin, Horne, Keith, Howell, Steve B., Isaak, Kate G., Jenkins, Jon M., Jensen, Eric L. N., Kiss, Laszlo, Lacedelli, Gaia, Lam, Kristine, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavelier des, Lendl, Monika, Lester, Kathryn V., Levine, Alan M., Livingston, John, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Marie-Sainte, Wenceslas, Maxted, Pierre F. L., Mayo, Andrew W., McLean, Brian, Mecina, Marko, Mékarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Ségransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stéphane, Van Eylen, Vincent, Van Grootel, Valérie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, and Winn, Joshua N.
Abstract: We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine $T_{\rm eff, \star}=4734\pm67$ K, $R_{\star}=0.726\pm0.007$ $R_{\odot}$, and $M_{\star}=0.748\pm0.032$ $M_{\odot}$. We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of $P_{\rm b}=6.44387\pm0.00003$ d, a radius of $R_{\rm b}=2.59\pm0.04$ $R_{\oplus}$, and a mass of $M_{\rm b}=13.5_{-1.8}^{+1.7}$ $M_{\oplus}$, whilst TOI-1064 c has an orbital period of $P_{\rm c}=12.22657^{+0.00005}_{-0.00004}$ d, a radius of $R_{\rm c}=2.65\pm0.04$ $R_{\oplus}$, and a 3$\sigma$ upper mass limit of 8.5 ${\rm M_{\oplus}}$. From the high-precision photometry we obtain radius uncertainties of $\sim$1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets., Comment: 30 pages, 24 figures, 6 tables including the Appendix; accepted for publication in MNRAS
Published: 2022
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21. Atmospheric characterization of terrestrial exoplanets in the mid-infrared : biosignatures, habitability, and diversity

Author: Quanz, Sascha P., Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, van Dishoeck, Ewine, Ehrenreich, David, Fortney, Jonathan, Glauser, Adrian, Grenfell, John Lee, Janson, Markus, Kraus, Stefan, Krause, Oliver, Labadie, Lucas, Lacour, Sylvestre, Line, Michael, Linz, Hendrik, Loicq, Jérôme, Miguel, Yamila, Pallé, Enric, Queloz, Didier, Rauer, Heike, Ribas, Ignasi, Rugheimer, Sarah, Selsis, Franck, Snellen, Ignas, Sozzetti, Alessandro, Stapelfeldt, Karl R., Udry, Stephane, Wyatt, Mark, Quanz, Sascha P., Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, van Dishoeck, Ewine, Ehrenreich, David, Fortney, Jonathan, Glauser, Adrian, Grenfell, John Lee, Janson, Markus, Kraus, Stefan, Krause, Oliver, Labadie, Lucas, Lacour, Sylvestre, Line, Michael, Linz, Hendrik, Loicq, Jérôme, Miguel, Yamila, Pallé, Enric, Queloz, Didier, Rauer, Heike, Ribas, Ignasi, Rugheimer, Sarah, Selsis, Franck, Snellen, Ignas, Sozzetti, Alessandro, Stapelfeldt, Karl R., Udry, Stephane, and Wyatt, Mark
Abstract: Exoplanet science is one of the most thriving fields of modern astrophysics. A major goal is the atmospheric characterization of dozens of small, terrestrial exoplanets in order to search for signatures in their atmospheres that indicate biological activity, assess their ability to provide conditions for life as we know it, and investigate their expected atmospheric diversity. None of the currently adopted projects or missions, from ground or in space, can address these goals. In this White Paper, submitted to ESA in response to the Voyage 2050 Call, we argue that a large space-based mission designed to detect and investigate thermal emission spectra of terrestrial exoplanets in the mid-infrared wavelength range provides unique scientific potential to address these goals and surpasses the capabilities of other approaches. While NASA might be focusing on large missions that aim to detect terrestrial planets in reflected light, ESA has the opportunity to take leadership and spearhead the development of a large mid-infrared exoplanet mission within the scope of the “Voyage 2050” long-term plan establishing Europe at the forefront of exoplanet science for decades to come. Given the ambitious science goals of such a mission, additional international partners might be interested in participating and contributing to a roadmap that, in the long run, leads to a successful implementation. A new, dedicated development program funded by ESA to help reduce development and implementation cost and further push some of the required key technologies would be a first important step in this direction. Ultimately, a large mid-infrared exoplanet imaging mission will be needed to help answer one of humankind’s most fundamental questions: “How unique is our Earth?”
Published: 2022
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22. Atmospheric characterization of terrestrial exoplanets in the mid-infrared: biosignatures, habitability, and diversity.

Author: Quanz, Sascha P, Quanz, Sascha P, Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, van Dishoeck, Ewine, Ehrenreich, David, Fortney, Jonathan, Glauser, Adrian, Grenfell, John Lee, Janson, Markus, Kraus, Stefan, Krause, Oliver, Labadie, Lucas, Lacour, Sylvestre, Line, Michael, Linz, Hendrik, Loicq, Jérôme, Miguel, Yamila, Pallé, Enric, Queloz, Didier, Rauer, Heike, Ribas, Ignasi, Rugheimer, Sarah, Selsis, Franck, Snellen, Ignas, Sozzetti, Alessandro, Stapelfeldt, Karl R, Udry, Stephane, Wyatt, Mark, Quanz, Sascha P, Quanz, Sascha P, Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, van Dishoeck, Ewine, Ehrenreich, David, Fortney, Jonathan, Glauser, Adrian, Grenfell, John Lee, Janson, Markus, Kraus, Stefan, Krause, Oliver, Labadie, Lucas, Lacour, Sylvestre, Line, Michael, Linz, Hendrik, Loicq, Jérôme, Miguel, Yamila, Pallé, Enric, Queloz, Didier, Rauer, Heike, Ribas, Ignasi, Rugheimer, Sarah, Selsis, Franck, Snellen, Ignas, Sozzetti, Alessandro, Stapelfeldt, Karl R, Udry, Stephane, and Wyatt, Mark
Abstract: Exoplanet science is one of the most thriving fields of modern astrophysics. A major goal is the atmospheric characterization of dozens of small, terrestrial exoplanets in order to search for signatures in their atmospheres that indicate biological activity, assess their ability to provide conditions for life as we know it, and investigate their expected atmospheric diversity. None of the currently adopted projects or missions, from ground or in space, can address these goals. In this White Paper, submitted to ESA in response to the Voyage 2050 Call, we argue that a large space-based mission designed to detect and investigate thermal emission spectra of terrestrial exoplanets in the mid-infrared wavelength range provides unique scientific potential to address these goals and surpasses the capabilities of other approaches. While NASA might be focusing on large missions that aim to detect terrestrial planets in reflected light, ESA has the opportunity to take leadership and spearhead the development of a large mid-infrared exoplanet mission within the scope of the "Voyage 2050" long-term plan establishing Europe at the forefront of exoplanet science for decades to come. Given the ambitious science goals of such a mission, additional international partners might be interested in participating and contributing to a roadmap that, in the long run, leads to a successful implementation. A new, dedicated development program funded by ESA to help reduce development and implementation cost and further push some of the required key technologies would be a first important step in this direction. Ultimately, a large mid-infrared exoplanet imaging mission will be needed to help answer one of humankind's most fundamental questions: "How unique is our Earth?"
Published: 2022

23. Atmospheric characterization of the ultra-hot Jupiter WASP-33b

Author: Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, German Research Foundation, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Research Council, Cont, D., Yan, F., Reiners, Ansgar, Nortmann, L., Molaverdikhani, K., Pallé, Enric, Henning, Thomas, Ribas, Ignasi, Quirrenbach, Andreas, Caballero, J. A., Amado, Pedro J., Czesla, S., Lesjak, F., López-Puertas, Manuel, Mollière, P., Montes, D., Morello, G., Nagel, Evangelos, Pedraz, S., Sánchez-López, A., Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, German Research Foundation, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Research Council, Cont, D., Yan, F., Reiners, Ansgar, Nortmann, L., Molaverdikhani, K., Pallé, Enric, Henning, Thomas, Ribas, Ignasi, Quirrenbach, Andreas, Caballero, J. A., Amado, Pedro J., Czesla, S., Lesjak, F., López-Puertas, Manuel, Mollière, P., Montes, D., Morello, G., Nagel, Evangelos, Pedraz, S., and Sánchez-López, A.
Abstract: Ultra-hot Jupiters are highly irradiated gas giant exoplanets on close-in orbits around their host stars. The dayside atmospheres of these objects strongly emit thermal radiation due to their elevated temperatures, making them prime targets for characterization by emission spectroscopy. We analyzed high-resolution spectra from CARMENES, HARPS-N, and ESPaDOnS taken over eight observation nights to study the emission spectrum of WASP-33b and draw conclusions about its atmosphere. By applying the cross-correlation technique, we detected the spectral signatures of Ti I, V I, and a tentative signal of Ti II for the first time via emission spectroscopy. These detections are an important finding because of the fundamental role of Ti- and V-bearing species in the planetary energy balance. Moreover, we assessed and confirm the presence of OH, Fe I, and Si I from previous studies. The spectral lines are all detected in emission, which unambiguously proves the presence of an inverted temperature profile in the planetary atmosphere. By performing retrievals on the emission lines of all the detected species, we determined a relatively weak atmospheric thermal inversion extending from approximately 3400 to 4000 K. We infer a supersolar metallicity close to 1.5 dex in the planetary atmosphere, and find that its emission signature undergoes significant line broadening with a Gaussian full width at half maximum of about 4.5 km s−1. Also, we find that the atmospheric temperature profile retrieved at orbital phases far from the secondary eclipse is about 300 to 700 K cooler than that measured close to the secondary eclipse, which is consistent with different day- and nightside temperatures. Moreover, retrievals performed on the emission lines of the individual chemical species lead to consistent results, which gives additional confidence to our retrieval method. Increasing the number of species included in the retrieval and expanding the set of retrieved atmospheric parameters will fu
Published: 2022

24. Density, not radius, separates rocky and water-rich small planets orbiting M dwarf stars

Author: Ministerio de Ciencia e Innovación (España), Luque, R., Pallé, Enric, Ministerio de Ciencia e Innovación (España), Luque, R., and Pallé, Enric
Abstract: Exoplanets smaller than Neptune are common around red dwarf stars (M dwarfs), with those that transit their host star constituting the bulk of known temperate worlds amenable for atmospheric characterization. We analyze the masses and radii of all known small transiting planets around M dwarfs, identifying three populations: rocky, water-rich, and gas-rich. Our results are inconsistent with the previously known bimodal radius distribution arising from atmospheric loss of a hydrogen/helium envelope. Instead, we propose that a density gap separates rocky from water-rich exoplanets. Formation models that include orbital migration can explain the observations: Rocky planets form within the snow line, whereas water-rich worlds form outside it and later migrate inward. © 2022 the authors, some rights reserved; exclusive licensee American Association for the Advancement of Science.
Published: 2022

25. Precise mass determination for the keystone sub-Neptune planet transiting the mid-type M dwarf G 9-40

Author: Ministerio de Ciencia e Innovación (España), European Commission, Luque, Alejandro, Nowak, G., Hirano, T., Kossakowski, D., Pallé, Enric, Nixon, M. C., Morello, G., Amado, Pedro J., Albrecht, S., Caballero, J. A., Cifuentes, C., Cochran, W.D., Deeg, H. J., Dreizler, S., Esparza-Borges, E., Fukui, A., Gandolfi, D., Goffo, E., Guenther, E. W., Hatzes, Artie P., Henning, Thomas, Kabath, P., Kawauchi, K., Korth, J., Kotani, T., Kudo, T., Kuzuhara, M., Lafarga, M., Lam, K. W. F., Livingston, J., Morales, Juan Carlos, Muresan, A., Murgas, F., Narita, N., Osborne, H. L. M., Parviainen, H., Passegger, V.M., Persson, C.M., Quirrenbach, Andreas, Redfield, S., Reffert, S., Reiners, Ansgar, Ribas, Ignasi, Serrano, L. M., Tamura, M., Van Eylen, V., Watanabe, N., Zapatero Osorio, María Rosa, Ministerio de Ciencia e Innovación (España), European Commission, Luque, Alejandro, Nowak, G., Hirano, T., Kossakowski, D., Pallé, Enric, Nixon, M. C., Morello, G., Amado, Pedro J., Albrecht, S., Caballero, J. A., Cifuentes, C., Cochran, W.D., Deeg, H. J., Dreizler, S., Esparza-Borges, E., Fukui, A., Gandolfi, D., Goffo, E., Guenther, E. W., Hatzes, Artie P., Henning, Thomas, Kabath, P., Kawauchi, K., Korth, J., Kotani, T., Kudo, T., Kuzuhara, M., Lafarga, M., Lam, K. W. F., Livingston, J., Morales, Juan Carlos, Muresan, A., Murgas, F., Narita, N., Osborne, H. L. M., Parviainen, H., Passegger, V.M., Persson, C.M., Quirrenbach, Andreas, Redfield, S., Reffert, S., Reiners, Ansgar, Ribas, Ignasi, Serrano, L. M., Tamura, M., Van Eylen, V., Watanabe, N., and Zapatero Osorio, María Rosa
Abstract: Context. Despite being a prominent subset of the exoplanet population discovered in the past three decades, the nature and provenance of sub-Neptune-sized planets is still one of the open questions in exoplanet science. Aims. For planets orbiting bright stars, precisely measuring the orbital and planet parameters of the system is the best approach to distinguish between competing theories regarding their formation and evolution. Methods. We obtained 69 new radial velocity observations of the mid-M dwarf G 9–40 with the CARMENES instrument to measure for the first time the mass of its transiting sub-Neptune planet, G 9–40 b, discovered in data from the K2 mission. Results. Combined with new observations from the TESS mission during Sectors 44, 45, and 46, we are able to measure the radius of the planet to an uncertainty of 3.4% (Rb = 1.900 ± 0.065 R⊕) and determine its mass with a precision of 16% (Mb = 4.00 ± 0.63 M⊕). The resulting bulk density of the planet is inconsistent with a terrestrial composition and suggests the presence of either a water-rich core or a significant hydrogen-rich envelope. Conclusions. G 9–40 b is referred to as a keystone planet due to its location in period-radius space within the radius valley. Several theories offer explanations for the origin and properties of this population and this planet is a valuable target for testing the dependence of those models on stellar host mass. By virtue of its brightness and small size of the host, it joins L 98-59 d as one of the two best warm (Teq ~ 400 K) sub-Neptunes for atmospheric characterization with JWST, which will probe cloud formation in sub-Neptune-sized planets and break the degeneracies of internal composition models. © R. Luque et al. 2022.
Published: 2022

26. Atmospheric characterization of terrestrial exoplanets in the mid-infrared: biosignatures, habitability, and diversity

Author: ETH Zurich, Swiss National Science Foundation, Quanz, Sascha P., Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, Dishoeck, Ewine van, Ehrenreich, David, Fortney, Jonathan J., Glauser, Adrian M., Linz, Hendrik, Loicq, Jerôme, Pallé, Enric, Rauer, Heike, Ribas, Ignasi, Selsis, Franck, Snellen, Ignas A. G., Sozzetti, Alessandro, Udry, Stephane, Wyatt, Mark, ETH Zurich, Swiss National Science Foundation, Quanz, Sascha P., Absil, Olivier, Benz, Willy, Bonfils, Xavier, Berger, Jean-Philippe, Defrère, Denis, Dishoeck, Ewine van, Ehrenreich, David, Fortney, Jonathan J., Glauser, Adrian M., Linz, Hendrik, Loicq, Jerôme, Pallé, Enric, Rauer, Heike, Ribas, Ignasi, Selsis, Franck, Snellen, Ignas A. G., Sozzetti, Alessandro, Udry, Stephane, and Wyatt, Mark
Abstract: Exoplanet science is one of the most thriving fields of modern astrophysics. A major goal is the atmospheric characterization of dozens of small, terrestrial exoplanets in order to search for signatures in their atmospheres that indicate biological activity, assess their ability to provide conditions for life as we know it, and investigate their expected atmospheric diversity. None of the currently adopted projects or missions, from ground or in space, can address these goals. In this White Paper, submitted to ESA in response to the Voyage 2050 Call, we argue that a large space-based mission designed to detect and investigate thermal emission spectra of terrestrial exoplanets in the mid-infrared wavelength range provides unique scientific potential to address these goals and surpasses the capabilities of other approaches. While NASA might be focusing on large missions that aim to detect terrestrial planets in reflected light, ESA has the opportunity to take leadership and spearhead the development of a large mid-infrared exoplanet mission within the scope of the “Voyage 2050” long-term plan establishing Europe at the forefront of exoplanet science for decades to come. Given the ambitious science goals of such a mission, additional international partners might be interested in participating and contributing to a roadmap that, in the long run, leads to a successful implementation. A new, dedicated development program funded by ESA to help reduce development and implementation cost and further push some of the required key technologies would be a first important step in this direction. Ultimately, a large mid-infrared exoplanet imaging mission will be needed to help answer one of humankind’s most fundamental questions: “How unique is our Earth?”
Published: 2022

27. Detecting life outside our solar system with a large high-contrast-imaging mission

Author: European Commission, European Research Council, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Netherlands Organization for Scientific Research, Knut and Alice Wallenberg Foundation, Snellen, Ignas A. G., Albrecht, S., Anglada-Escudé, Guillem, Benz, Willy, Carone, Ludmila, Claudi, Riccardo, Désert, Jean-Michel, Desidera, S., Gaudi, B. Scott, Henning, Thomas, Kreidberg, L., Launhardt, R., López-Puertas, Manuel, Micela, Giusi, Pallé, Enric, Pagano, Isabella, Piotto, Giampaolo, Rauer, Heike, Ribas, Ignasi, Selsis, Franck, Sozzetti, Alessandro, Vigan, A., Visser, Pieter de, European Commission, European Research Council, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Netherlands Organization for Scientific Research, Knut and Alice Wallenberg Foundation, Snellen, Ignas A. G., Albrecht, S., Anglada-Escudé, Guillem, Benz, Willy, Carone, Ludmila, Claudi, Riccardo, Désert, Jean-Michel, Desidera, S., Gaudi, B. Scott, Henning, Thomas, Kreidberg, L., Launhardt, R., López-Puertas, Manuel, Micela, Giusi, Pallé, Enric, Pagano, Isabella, Piotto, Giampaolo, Rauer, Heike, Ribas, Ignasi, Selsis, Franck, Sozzetti, Alessandro, Vigan, A., and Visser, Pieter de
Abstract: In this White Paper, which was submitted in response to the European Space Agency (ESA) Voyage 2050 Call, we recommend the ESA plays a proactive role in developing a global collaborative effort to construct a large high-contrast imaging space telescope, e.g. as currently under study by NASA. Such a mission will be needed to characterize a sizable sample of temperate Earth-like planets in the habitable zones of nearby Sun-like stars and to search for extraterrestrial biological activity. We provide an overview of relevant European expertise, and advocate ESA to start a technology development program towards detecting life outside the Solar System.
Published: 2022

28. The Gravitational-wave Optical Transient Observer (GOTO)

Author: Dyer, Martin J., Ackley, Kendall, Lyman, Joe, Ulaczyk, Krzysztof, Steeghs, Danny, Galloway, Duncan K., Dhillon, Vik S, O'Brien, Paul, Ramsay, Gavin, Noysena, Kanthanakorn, Kotak, Rubina, Breton, Rene, Nuttall, Laura, Pallé, Enric, Pollacco, Don, Dyer, Martin J., Ackley, Kendall, Lyman, Joe, Ulaczyk, Krzysztof, Steeghs, Danny, Galloway, Duncan K., Dhillon, Vik S, O'Brien, Paul, Ramsay, Gavin, Noysena, Kanthanakorn, Kotak, Rubina, Breton, Rene, Nuttall, Laura, Pallé, Enric, and Pollacco, Don
Abstract: The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. Each GOTO robotic mount holds eight 40 cm telescopes, giving an overall field of view of 40 square degrees. As of 2022 the first two GOTO mounts have been commissioned at the Roque de los Muchachos Observatory on La Palma, Canary Islands, and construction of the second node with two additional 8-telescope mounts has begin at Siding Spring Observatory in New South Wales, Australia. Once fully operational each GOTO mount will be networked to form a robotic, multi-site observatory, which will survey the entire visible sky every two nights and enable rapid follow-up detections of transient sources., Comment: 8 pages, 5 figures, submitted to SPIE Astronomical Telescopes + Instrumentation 2022
Published: 2022
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29. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

Author: Hawthorn, Faith, Bayliss, Daniel, Wilson, Thomas G., Bonfanti, Andrea, Adibekyan, Vardan, Alibert, Yann, Sousa, Sérgio G., Collins, Karen A., Bryant, Edward M., Osborn, Ares, Armstrong, David J., Abe, Lyu, Acton, Jack S., Addison, Brett C., Agabi, Karim, Alonso, Roi, Alves, Douglas R., Anglada-Escudé, Guillem, Bárczy, Tamas, Barclay, Thomas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Bendjoya, Philippe, Benz, Willy, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brandeker, Alexis, Broeg, Christopher, Brown, David J. A., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Caldwell, Douglas A., Casewell, Sarah L., Charbonneau, David, Charnoz, Sébastian, Cloutier, Ryan, Cameron, Andrew Collier, Collins, Kevin I., Conti, Dennis M., Crouzet, Nicolas, Czismadia, Szilárd, Davies, Melvyn B., Deleuil, Magali, Delgado-Mena, Elisa, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dransfield, Georgina, Dumusque, Xavier, Egger, Jo Ann, Ehrenreich, David, Eigmüller, Philipp, Erickson, Anders, Essack, Zahra, Fortier, Andrea, Fossati, Luca, Fridlund, Malcolm, Günther, Maximilian N., Güdel, Manuel, Gandolfi, Davide, Gillard, Harvey, Gillon, Michaël, Gnilka, Crystal, Goad, Michael R., Goeke, Robert F., Guillot, Tristan, Hadjigeorghiou, Andreas, Hellier, Coel, Henderson, Beth A., Heng, Kevin, Hooton, Matthew J., Horne, Keith, Howell, Steve B., Hoyer, Sergio, Irwin, Jonathan M., Jenkins, James S., Jenkins, Jon M., Jensen, Eric L. N., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kiss, Laszlo L., Lacedelli, Gaia, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavalier des, Leleu, Adrien, Lendl, Monika, Lillo-Box, Jorge, Lovis, Christophe, Mékarnia, Djamel, Massey, Bob, Masters, Tamzin, Maxted, Pierre F. L., Nascimbeni, Valerio, Nielsen, Louise D., O'Brien, Sean M., Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Persson, Carina M., Piotto, Giampaolo, Plavchan, Peter, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rauer, Heike, Ribas, Ignasi, Ricker, George, Ségransan, Damien, Salmon, Sébastien, Santerne, Alexandre, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Srdoc, Gregor, Steller, Manfred, Suarez, Olga, Szabó, Gyula M., Teske, Johanna, Thomas, Nicolas, Tilbrook, Rosanna H., Triaud, Amaury H. M. J., Udry, Stéphane, Van Grootel, Valérie, Walton, Nicholas, Wang, Sharon X., Wheatley, Peter J., Winn, Joshua N., Wittenmyer, Robert A., Zhang, Hui, Hawthorn, Faith, Bayliss, Daniel, Wilson, Thomas G., Bonfanti, Andrea, Adibekyan, Vardan, Alibert, Yann, Sousa, Sérgio G., Collins, Karen A., Bryant, Edward M., Osborn, Ares, Armstrong, David J., Abe, Lyu, Acton, Jack S., Addison, Brett C., Agabi, Karim, Alonso, Roi, Alves, Douglas R., Anglada-Escudé, Guillem, Bárczy, Tamas, Barclay, Thomas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Bendjoya, Philippe, Benz, Willy, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brandeker, Alexis, Broeg, Christopher, Brown, David J. A., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Caldwell, Douglas A., Casewell, Sarah L., Charbonneau, David, Charnoz, Sébastian, Cloutier, Ryan, Cameron, Andrew Collier, Collins, Kevin I., Conti, Dennis M., Crouzet, Nicolas, Czismadia, Szilárd, Davies, Melvyn B., Deleuil, Magali, Delgado-Mena, Elisa, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dransfield, Georgina, Dumusque, Xavier, Egger, Jo Ann, Ehrenreich, David, Eigmüller, Philipp, Erickson, Anders, Essack, Zahra, Fortier, Andrea, Fossati, Luca, Fridlund, Malcolm, Günther, Maximilian N., Güdel, Manuel, Gandolfi, Davide, Gillard, Harvey, Gillon, Michaël, Gnilka, Crystal, Goad, Michael R., Goeke, Robert F., Guillot, Tristan, Hadjigeorghiou, Andreas, Hellier, Coel, Henderson, Beth A., Heng, Kevin, Hooton, Matthew J., Horne, Keith, Howell, Steve B., Hoyer, Sergio, Irwin, Jonathan M., Jenkins, James S., Jenkins, Jon M., Jensen, Eric L. N., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kiss, Laszlo L., Lacedelli, Gaia, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavalier des, Leleu, Adrien, Lendl, Monika, Lillo-Box, Jorge, Lovis, Christophe, Mékarnia, Djamel, Massey, Bob, Masters, Tamzin, Maxted, Pierre F. L., Nascimbeni, Valerio, Nielsen, Louise D., O'Brien, Sean M., Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Persson, Carina M., Piotto, Giampaolo, Plavchan, Peter, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rauer, Heike, Ribas, Ignasi, Ricker, George, Ségransan, Damien, Salmon, Sébastien, Santerne, Alexandre, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Srdoc, Gregor, Steller, Manfred, Suarez, Olga, Szabó, Gyula M., Teske, Johanna, Thomas, Nicolas, Tilbrook, Rosanna H., Triaud, Amaury H. M. J., Udry, Stéphane, Van Grootel, Valérie, Walton, Nicholas, Wang, Sharon X., Wheatley, Peter J., Winn, Joshua N., Wittenmyer, Robert A., and Zhang, Hui
Abstract: We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright ($T = 8.5$ mag), high proper motion ($\sim\,200$ mas yr$^{-1}$), low metallicity ([Fe/H]$\approx\,-0.28$) K-dwarf with a mass of $0.68\pm0.05$ M$_{\odot}$ and a radius of $0.67\pm0.01$ R$_{\odot}$. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a $1.70\pm0.07$ R$_{\oplus}$ super-Earth in a 3.82 day orbit, placing it directly within the so-called 'radius valley'. The outer planet, TOI-836 c, is a $2.59\pm0.09$ R$_{\oplus}$ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of $4.5\pm0.9$ M$_{\oplus}$ , while TOI-836 c has a mass of $9.6\pm2.6$ M$_{\oplus}$. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet.
Published: 2022
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30. TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission

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 Physics, Subjak, Jan, Sharma, Rishikesh, Carmichael, Theron W., Johnson, Marshall C., Gonzales, Erica J., Matthews, Elisabeth C, Boffin, Henry M. J., Brahm, Rafael, Chaturvedi, Priyanka, Chakraborty, Abhijit, Ciardi, David R., Collins, Karen A., Esposito, Massimilaino, Fridlund, Malcolm, Gan, Tianjun, Gandolfi, Davide, García, Rafael A., Guenther, Eike, Hatze, Artie, Latham, David W., Mathis, Stéphane, Mathur, Savita, Persson, Carina M., Relles, Howard M., Schlieder, Joshua E., Barclay, Thomas, Dressing, Courtney D., Crossfield, Ian Jm, Howard, Andrew W., Rodler, Florian, Zhou, George, Quinn, Samuel N., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Stassun, Keivan G., Blažek, Martin, Skarka, Marek, Spokova, Magdalena, Zak, Jiri, Albrecht, Simon, Sobrino, Roi Alonso, Beck, Paul, Cabrera, Juan, Carleo, Ilaria, Cochran, WIlliam D., Csizmadia, Szilard, Dai, Fei, Deeg, Hans J., de Leon, Jerome P., Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Fukui, Akihiko, Georgeieva, Iskra, González-Cuesta, Lucía, Grziwa, Sascha, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Knudstrup, Emil, Korth, Judith, Lam, Kristine W. F., Livingston, John H., Lund, Mikkel N., Luque, Rafael, Rodríguez, Pilar Montanes, Murgas, Felipe, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Pallé, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Smith, Alexis M. S., Van Eylen, Vincent, Kabáth, Petr, 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 Physics, Subjak, Jan, Sharma, Rishikesh, Carmichael, Theron W., Johnson, Marshall C., Gonzales, Erica J., Matthews, Elisabeth C, Boffin, Henry M. J., Brahm, Rafael, Chaturvedi, Priyanka, Chakraborty, Abhijit, Ciardi, David R., Collins, Karen A., Esposito, Massimilaino, Fridlund, Malcolm, Gan, Tianjun, Gandolfi, Davide, García, Rafael A., Guenther, Eike, Hatze, Artie, Latham, David W., Mathis, Stéphane, Mathur, Savita, Persson, Carina M., Relles, Howard M., Schlieder, Joshua E., Barclay, Thomas, Dressing, Courtney D., Crossfield, Ian Jm, Howard, Andrew W., Rodler, Florian, Zhou, George, Quinn, Samuel N., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Stassun, Keivan G., Blažek, Martin, Skarka, Marek, Spokova, Magdalena, Zak, Jiri, Albrecht, Simon, Sobrino, Roi Alonso, Beck, Paul, Cabrera, Juan, Carleo, Ilaria, Cochran, WIlliam D., Csizmadia, Szilard, Dai, Fei, Deeg, Hans J., de Leon, Jerome P., Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Fukui, Akihiko, Georgeieva, Iskra, González-Cuesta, Lucía, Grziwa, Sascha, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Knudstrup, Emil, Korth, Judith, Lam, Kristine W. F., Livingston, John H., Lund, Mikkel N., Luque, Rafael, Rodríguez, Pilar Montanes, Murgas, Felipe, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Pallé, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Smith, Alexis M. S., Van Eylen, Vincent, and Kabáth, Petr
Abstract: © 2020. The American Astronomical Society. All rights reserved.. We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P = 3.6772 ± 0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD's radius . We obtained high-resolution spectroscopic observations with the FIES, Ondrejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be M b = 53.7 ± 1.2 a radius of R = 1.70 ± 0.05R o, an effective temperature of T eff = 7650 ± 160 K, and a relatively high metallicity of 0.61 ± 0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main-sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert is reforesting.
Published: 2022

31. K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant

Author: European Commission, Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), Swedish National Space Agency, Smith, A. M. S., Breton, S. N., Csizmadia, Sz, Dai, F., Gandolfi, D., García, R. A., Howard, A. W., Isaacson, H., Korth, J., Lam, K.W.F., Mathur, Savita, Nowak, G., Pérez Hernández, F., Persson, C.M., Albrecht, S. H., Barragán, O., Cabrera, J., Cochran, W. D., Deeg, H. J., Fridlund, M., Georgieva, I. Y., Goffo, E., Guenther, E. W., Hatzes, Artie P., Kabath, P., Livingston, J. H., Luque, R., Pallé, Enric, Redfield, S., Rodler, F., Serrano, L. M., Van Eylen, V., European Commission, Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), Swedish National Space Agency, Smith, A. M. S., Breton, S. N., Csizmadia, Sz, Dai, F., Gandolfi, D., García, R. A., Howard, A. W., Isaacson, H., Korth, J., Lam, K.W.F., Mathur, Savita, Nowak, G., Pérez Hernández, F., Persson, C.M., Albrecht, S. H., Barragán, O., Cabrera, J., Cochran, W. D., Deeg, H. J., Fridlund, M., Georgieva, I. Y., Goffo, E., Guenther, E. W., Hatzes, Artie P., Kabath, P., Livingston, J. H., Luque, R., Pallé, Enric, Redfield, S., Rodler, F., Serrano, L. M., and Van Eylen, V.
Abstract: We report new photometric and spectroscopic observations of the K2-99 planetary system. Asteroseismic analysis of the short-cadence light curve from K2’s Campaign 17 allows us to refine the stellar properties. We find K2-99 to be significantly smaller than previously thought, with R⋆ = 2.55 ± 0.02 R⊙. The new light curve also contains four transits of K2-99 b, which we use to improve our knowledge of the planetary properties. We find the planet to be a non-inflated warm Jupiter, with Rb = 1.06 ± 0.01 RJup⁠. 60 new radial velocity measurements from HARPS, HARPS-N, and HIRES enable the determination of the orbital parameters of K2-99 c, which were previously poorly constrained. We find that this outer planet has a minimum mass Mcsin ic = 8.4 ± 0.2 MJup⁠, and an eccentric orbit (ec = 0.210 ± 0.009) with a period of 522.2 ± 1.4 d. Upcoming TESS observations in 2022 have a good chance of detecting the transit of this planet, if the mutual inclination between the two planetary orbits is small. © 2022 The Author(s).
Published: 2022

32. A multi-planetary system orbiting the early-M dwarf TOI-1238

Author: European Commission, Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), González-Álvarez, E., Zapatero Osorio, María Rosa, Sanz-Forcada, J., Caballero, J. A., Reffert, S., Béjar, Victor J. S., Hatzes, Artie P., Herrero, E., Jeffers, Sandra V., Kemmer, J., López González, Maria J., Luque, R., Molaverdikhani, K., Morello, G., Nagel, Evangelos, Quirrenbach, Andreas, Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Schlecker, M., Schweitzer, Andreas, Stock, S., Passegger, V.M., Trifonov, T., Amado, Pedro J., Baker, D., Boyd, P. T., Cadieux, Charles, Charbonneau, David, Collins, Karen A., Doyon, R., Dreizler, S., Espinoza, Néstor, Fűrész, G., Furlan, E., Hesse, K., Howell, S.B., Jenkins, Jon M., Kidwell, R. C., Latham, David W., McLeod, K. K., Montes, D., Morales, Juan Carlos, O'Dwyer, T., Pallé, Enric, Pedraz, S., Reiners, Ansgar, Ribas, Ignasi, Quinn, S. N., Schnaible, C., Seager, S., Skinner, B., Smith, J. C., Schwarz, R. P., Shporer, A., Vanderspek, R., Winn, J. N., European Commission, Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), González-Álvarez, E., Zapatero Osorio, María Rosa, Sanz-Forcada, J., Caballero, J. A., Reffert, S., Béjar, Victor J. S., Hatzes, Artie P., Herrero, E., Jeffers, Sandra V., Kemmer, J., López González, Maria J., Luque, R., Molaverdikhani, K., Morello, G., Nagel, Evangelos, Quirrenbach, Andreas, Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Schlecker, M., Schweitzer, Andreas, Stock, S., Passegger, V.M., Trifonov, T., Amado, Pedro J., Baker, D., Boyd, P. T., Cadieux, Charles, Charbonneau, David, Collins, Karen A., Doyon, R., Dreizler, S., Espinoza, Néstor, Fűrész, G., Furlan, E., Hesse, K., Howell, S.B., Jenkins, Jon M., Kidwell, R. C., Latham, David W., McLeod, K. K., Montes, D., Morales, Juan Carlos, O'Dwyer, T., Pallé, Enric, Pedraz, S., Reiners, Ansgar, Ribas, Ignasi, Quinn, S. N., Schnaible, C., Seager, S., Skinner, B., Smith, J. C., Schwarz, R. P., Shporer, A., Vanderspek, R., and Winn, J. N.
Abstract: Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an insightful characterization of the planets, which in turn has repercussions for our understanding of the architecture of planetary systems and, therefore, their formation and evolution. Aims. Two transiting planet candidates with super-Earth radii around the nearby (d = 70.64 ± 0.06 pc) K7–M0 dwarf star TOI-1238 were announced by NASA’s Transiting Exoplanet Survey Satellite (TESS), which observed the field of TOI-1238 in four different sectors. We aim to validate their planetary nature using precise radial velocities taken with the CARMENES spectrograph. Methods. We obtained 55 CARMENES radial velocity measurements that span the 11 months between 9 May 2020 and 5 April 2021. For a better characterization of the parent star’s activity, we also collected contemporaneous optical photometric observations at the Joan Oró and Sierra Nevada observatories and retrieved archival photometry from the literature. We performed a combined TESS+CARMENES photometric and spectroscopic analysis by including Gaussian processes and Keplerian orbits to account for the stellar activity and planetary signals simultaneously. Results. We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on photometric and spectroscopic data. The combined analysis confirms the discovery of two transiting planets, TOI-1238 b and c, with orbital periods of 0.764597−0.000011+0.000013 d and 3.294736−0.000036+0.000034 d, masses of 3.76−1.07+1.15 M⊕ and 8.32−1.88+1.90 M⊕, and radii of 1.21−0.10+0.11 R⊕ and 2.11−0.14+0.14 R⊕. They orbit their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ± 0.001 au, respectively.The two planets are placed on opposi
Published: 2022

33. Detection of iron emission lines and a temperature inversion on the dayside of the ultra-hot Jupiter KELT-20b

Author: European Commission, European Research Council, Ministerio de Ciencia e Innovación (España), Yan, F., Reiners, Ansgar, Pallé, Enric, Shulyak, D., Stangret, M., Molaverdikhani, K., Nortmann, L., Mollière, P., Henning, Thomas, Casasayas-Barris, N., Cont, D., Chen, G., Czesla, S., Sánchez-López, A., López-Puertas, Manuel, Ribas, Ignasi, Quirrenbach, Andreas, Caballero, J. A., Amado, Pedro J., Galadí-Enriquez, D., Khalafinejad, S., Lara, Luisa María, Montes, D., Morello, G., Nagel, Evangelos, Sedaghati, E., Zapatero Osorio, María Rosa, Zechmeister, Mathias, European Commission, European Research Council, Ministerio de Ciencia e Innovación (España), Yan, F., Reiners, Ansgar, Pallé, Enric, Shulyak, D., Stangret, M., Molaverdikhani, K., Nortmann, L., Mollière, P., Henning, Thomas, Casasayas-Barris, N., Cont, D., Chen, G., Czesla, S., Sánchez-López, A., López-Puertas, Manuel, Ribas, Ignasi, Quirrenbach, Andreas, Caballero, J. A., Amado, Pedro J., Galadí-Enriquez, D., Khalafinejad, S., Lara, Luisa María, Montes, D., Morello, G., Nagel, Evangelos, Sedaghati, E., Zapatero Osorio, María Rosa, and Zechmeister, Mathias
Abstract: Ultra-hot Jupiters (UHJs) are gas giants with very high equilibrium temperatures. In recent years, multiple chemical species, including various atoms and ions, have been discovered in their atmospheres. Most of these observations have been performed with transmission spectroscopy, although UHJs are also ideal targets for emission spectroscopy due to their strong thermal radiation. We present high-resolution thermal emission spectroscopy of the transiting UHJ KELT-20b/MASCARA-2b. The observation was performed with the CARMENES spectrograph at orbital phases before and after the secondary eclipse. We detected atomic Fe using the cross-correlation technique. The detected Fe lines are in emission, which unambiguously indicates a temperature inversion on the dayside hemisphere. We furthermore retrieved the temperature structure with the detected Fe lines. The result shows that the atmosphere has a strong temperature inversion with a temperature of 4900 ± 700 K and a pressure of 10−4.8−1.1+1.0 bar at the upper layer of the inversion. A joint retrieval of the CARMENES data and the TESS secondary eclipse data returns a temperature of 2550−250+150 K and a pressure of 10−1.5−0.6+0.7 bar at the lower layer of the temperature inversion. The detection of such a strong temperature inversion is consistent with theoretical simulations that predict an inversion layer on the dayside of UHJs. The joint retrieval of the CARMENES and TESS data demonstrates the power of combing high-resolution emission spectroscopy with secondary eclipse photometry in characterizing atmospheric temperature structures. © ESO 2022.
Published: 2022

34. Benchmark tests of transmission spectroscopy using transiting white dwarfs

Author: Jiang, Chengzi, Chen, Guo, Pallé, Enric, Parviainen, Hannu, Murgas, Felipe, Ma, Yuehua, Jiang, Chengzi, Chen, Guo, Pallé, Enric, Parviainen, Hannu, Murgas, Felipe, and Ma, Yuehua
Abstract: Ground-based transit observations are affected by both telluric absorption and instrumental systematics. To account for these effects, a better understanding of the impact of different data analyses is needed to improve the accuracy of the retrieved transmission spectra. We propose validating ground-based low-resolution transmission spectroscopy using transiting white dwarfs. The advantage here is that we know beforehand what the final transmission spectrum should be: a featureless flat spectrum. We analyzed two transiting white dwarfs analogous to hot Jupiters. We used various noise models to account for the systematic noise in their spectroscopic light curves following common procedures of transmission spectroscopy analyses. We compared the derived transmission spectra with the broadband transit depth to determine whether there are any artificial offsets or spectral features arising from light-curve fitting. The results show a strong model dependence, and the transmission spectra exhibit considerable discrepancies when they are computed with different noise models, different reference stars, and different common-mode removal methods. Nonetheless, we can still derive relatively accurate transmission spectra based on a Bayesian model comparison. With current ground-based instrumentation, the systematics in transit light curves can easily contaminate a transmission spectrum, introducing a general offset or some spurious spectral features and thus leading to a biased interpretation on the planetary atmosphere. Therefore, it is necessary to determine the dependence of results on the adopted noise model through model comparison. The model inferences should be examined through multiple observations and different instruments. (Abridged), Comment: Accepted for pulication in A&A, 18 pages, 9 figures
Published: 2022
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35. The TESS-Keck Survey. XI. Mass Measurements for Four Transiting sub-Neptunes orbiting K dwarf TOI-1246

Author: Turtelboom, Emma V., Weiss, Lauren M., Dressing, Courtney D., Nowak, Grzegorz, Pallé, Enric, Beard, Corey, Blunt, Sarah, Brinkman, Casey, Chontos, Ashley, Claytor, Zachary R., Dai, Fei, Dalba, Paul A., Giacalone, Steven, Gonzales, Erica, Harada, Caleb K., Hill, Michelle L., Holcomb, Rae, Korth, Judith, Lubin, Jack, Masseron, Thomas, MacDougall, Mason, Mayo, Andrew W., Močnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rice, Malena, Rubenzahl, Ryan A., Scarsdale, Nicholas, Stassun, Keivan G., Tyler, Dakotah B., Van Zandt, Judah, Crossfield, Ian J. M., Deeg, Hans J., Fulton, Benjamin, Gandolfi, Davide, Howard, Andrew W., Huber, Dan, Isaacson, Howard, Kane, Stephen R., Lam, Kristine W. F., Luque, Rafael, Martín, Eduardo L., Morello, Giuseppe, Orell-Miquel, Jaume, Petigura, Erik A., Robertson, Paul, Roy, Arpita, Van Eylen, Vincent, Baker, David, Belinski, Alexander A., Bieryla, Allyson, Ciardi, David R., Collins, Karen A., Cutting, Neil, Della-Rose, Devin J., Ellingsen, Taylor B., Furlan, E., Gan, Tianjun, Gnilka, Crystal L., Guerra, Pere, Howell, Steve B., Jimenez, Mary, Latham, David W., Larivière, Maude, Lester, Kathryn V., Lillo-Box, Jorge, Luker, Lindy, Mann, Christopher R., Plavchan, Peter P., Safonov, Boris, Skinner, Brett, Strakhov, Ivan A., Wittrock, Justin M., Caldwell, Douglas A., Essack, Zahra, Jenkins, Jon M., Quintana, Elisa V., Ricker, George R., Vanderspek, Roland, Seager, S., Winn, Joshua N., Turtelboom, Emma V., Weiss, Lauren M., Dressing, Courtney D., Nowak, Grzegorz, Pallé, Enric, Beard, Corey, Blunt, Sarah, Brinkman, Casey, Chontos, Ashley, Claytor, Zachary R., Dai, Fei, Dalba, Paul A., Giacalone, Steven, Gonzales, Erica, Harada, Caleb K., Hill, Michelle L., Holcomb, Rae, Korth, Judith, Lubin, Jack, Masseron, Thomas, MacDougall, Mason, Mayo, Andrew W., Močnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rice, Malena, Rubenzahl, Ryan A., Scarsdale, Nicholas, Stassun, Keivan G., Tyler, Dakotah B., Van Zandt, Judah, Crossfield, Ian J. M., Deeg, Hans J., Fulton, Benjamin, Gandolfi, Davide, Howard, Andrew W., Huber, Dan, Isaacson, Howard, Kane, Stephen R., Lam, Kristine W. F., Luque, Rafael, Martín, Eduardo L., Morello, Giuseppe, Orell-Miquel, Jaume, Petigura, Erik A., Robertson, Paul, Roy, Arpita, Van Eylen, Vincent, Baker, David, Belinski, Alexander A., Bieryla, Allyson, Ciardi, David R., Collins, Karen A., Cutting, Neil, Della-Rose, Devin J., Ellingsen, Taylor B., Furlan, E., Gan, Tianjun, Gnilka, Crystal L., Guerra, Pere, Howell, Steve B., Jimenez, Mary, Latham, David W., Larivière, Maude, Lester, Kathryn V., Lillo-Box, Jorge, Luker, Lindy, Mann, Christopher R., Plavchan, Peter P., Safonov, Boris, Skinner, Brett, Strakhov, Ivan A., Wittrock, Justin M., Caldwell, Douglas A., Essack, Zahra, Jenkins, Jon M., Quintana, Elisa V., Ricker, George R., Vanderspek, Roland, Seager, S., and Winn, Joshua N.
Abstract: Multi-planet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf ($\rm{V=11.6,~K=9.9}$) and four transiting sub-Neptunes identified by TESS with orbital periods of $4.31~\rm{d},~5.90~\rm{d},~18.66~\rm{d}$, and $~37.92~\rm{d}$. We collected 130 radial velocity observations with Keck/HIRES and TNG/HARPS-N to measure planet masses. We refit the 14 sectors of TESS photometry to refine planet radii ($\rm{2.97 \pm 0.06~R_\oplus},\rm{2.47 \pm 0.08~R_\oplus}, \rm{3.46 \pm 0.09~R_\oplus}$, $\rm{3.72 \pm 0.16~R_\oplus}$), and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets ($\rm{8.1 \pm 1.1 M_\oplus}$, $\rm{8.8 \pm 1.2 M_\oplus}$, $\rm{5.3 \pm 1.7 M_\oplus}$, $\rm{14.8 \pm 2.3 M_\oplus}$). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance ($\rm{P_{e}/P_{d}=2.03}$) and exhibit transit timing variations. TOI-1246 is one of the brightest four-planet systems, making it amenable for continued observations. It is one of only six systems with measured masses and radii for all four transiting planets. The planet densities range from $\rm{0.70 \pm 0.24}$ to $3.21 \pm 0.44 \rm{g/cm^3}$, implying a range of bulk and atmospheric compositions. We also report a fifth planet candidate found in the RV data with a minimum mass of 25.6 $\pm$ 3.6 $\rm{M_\oplus}$. This planet candidate is exterior to TOI-1246 e with a candidate period of 93.8 d, and we discuss the implications if it is confirmed to be planetary in nature., Comment: Accepted at The Astronomical Journal; 33 pages, 10 figures
Published: 2022
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36. Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

Author: Osborn, Hugh P., Bonfanti, Andrea, Gandolfi, Davide, Hedges, Christina, Leleu, Adrien, Fortier, Andrea, Futyan, David, Gutermann, Pascal, Maxted, Pierre F. L., Borsato, Luca, Collins, Karen A., da Silva, J. Gomes, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Lendl, Monika, Parviainen, Hannu, Salmon, Sébastien, Schanche, Nicole, Serrano, Luisa M., Sousa, Sergio G., Tuson, Amy, Ulmer-Moll, Solène, Van Grootel, Valerie, Wells, R. D., Wilson, Thomas G., Alibert, Yann, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Biondi, Federico, Bonfils, Xavier, Bouchy, Francois, Brandeker, Alexis, Broeg, Christopher, Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Charnoz, Sébastien, Cameron, Andrew Collier, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demory, Brice-Olivier, Ehrenreich, David, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Gómez-Muñoz, M. A., Güdel, Manuel, Heng, Kevin, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo, Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Magrin, Demetrio, Malavolta, Luca, McCormac, James, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Demangeon, Olivier D. S., Smith, Alexis M. S., Sabin, L., Santos, Nuno, Scandariato, Gaetano, Schroffenegger, U., Schwarz, Rick P., Shporer, Avi, Simon, Attila E., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Walter, Ingo, Walton, Nicholas, Osborn, Hugh P., Bonfanti, Andrea, Gandolfi, Davide, Hedges, Christina, Leleu, Adrien, Fortier, Andrea, Futyan, David, Gutermann, Pascal, Maxted, Pierre F. L., Borsato, Luca, Collins, Karen A., da Silva, J. Gomes, Chew, Yilen Gómez Maqueo, Hooton, Matthew J., Lendl, Monika, Parviainen, Hannu, Salmon, Sébastien, Schanche, Nicole, Serrano, Luisa M., Sousa, Sergio G., Tuson, Amy, Ulmer-Moll, Solène, Van Grootel, Valerie, Wells, R. D., Wilson, Thomas G., Alibert, Yann, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Biondi, Federico, Bonfils, Xavier, Bouchy, Francois, Brandeker, Alexis, Broeg, Christopher, Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Charnoz, Sébastien, Cameron, Andrew Collier, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demory, Brice-Olivier, Ehrenreich, David, Erikson, Anders, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Gómez-Muñoz, M. A., Güdel, Manuel, Heng, Kevin, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo, Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Magrin, Demetrio, Malavolta, Luca, McCormac, James, Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piazza, Daniele, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Demangeon, Olivier D. S., Smith, Alexis M. S., Sabin, L., Santos, Nuno, Scandariato, Gaetano, Schroffenegger, U., Schwarz, Rick P., Shporer, Avi, Simon, Attila E., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Walter, Ingo, and Walton, Nicholas
Abstract: Context: TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young ($340\pm80$ Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims: To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods: We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results: CHEOPS observations revealed a clear detection for TOI-2076 c at $P=21.01538^{+0.00084}_{-0.00074}$ d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the $P=35.12537\pm0.00067$ d alias. These observations also improved the radius precision of all three sub-Neptunes to $2.518\pm0.036$, $3.497\pm0.043$, and $3.232\pm0.063$ $R_\oplus$. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST., Comment: 18 pages, 7 figure, 8 tables. Accepted for publication in Astronomy & Astrophysics. Photometry available on CDS/Vizier. Python package presented for modelling duotransiting planet candidates available at https://github.com/hposborn/MonoTools. Modelling & figure-creation code available at https://github.com/hposborn/TOI2076
Published: 2022
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37. TOI-2119: A transiting brown dwarf orbiting an active M-dwarf from NASA's TESS mission

Author: Carmichael, Theron W., Irwin, Jonathan M., Murgas, Felipe, Pallé, Enric, Stassun, Keivan G., Bartnik, Matthew, Collins, Karen A., de Leon, Jerome, Esparza-Borges, Emma, Fedewa, Jeremy, Fong, William, Fukui, Akihiko, Jenkins, Jon M., Kagetani, Taiki, Latham, David W., Lund, Michael B., Mann, Andrew W., Moldovan, Dan, Morgan, Edward H., Narita, Norio, Painter, Shane, Parviainen, Hannu, Quintana, Elisa V., Ricker, George R., Schulte, Jack, Schwarz, Richard P., Seager, Sara, Sokolovsky, Kirill, Twicken, Joseph D., Winn, Joshua N., Carmichael, Theron W., Irwin, Jonathan M., Murgas, Felipe, Pallé, Enric, Stassun, Keivan G., Bartnik, Matthew, Collins, Karen A., de Leon, Jerome, Esparza-Borges, Emma, Fedewa, Jeremy, Fong, William, Fukui, Akihiko, Jenkins, Jon M., Kagetani, Taiki, Latham, David W., Lund, Michael B., Mann, Andrew W., Moldovan, Dan, Morgan, Edward H., Narita, Norio, Painter, Shane, Parviainen, Hannu, Quintana, Elisa V., Ricker, George R., Schulte, Jack, Schwarz, Richard P., Seager, Sara, Sokolovsky, Kirill, Twicken, Joseph D., and Winn, Joshua N.
Abstract: We report the discovery of TOI-2119b, a transiting brown dwarf (BD) that orbits and is completely eclipsed by an active M-dwarf star. Using light curve data from the Transiting Exoplanet Survey Satellite mission and follow-up high-resolution Doppler spectroscopic observations, we find the BD has a radius of $R_b = 1.08 \pm 0.03{\rm R_J}$, a mass of $M_b = 64.4 \pm 2.3{\rm M_J}$, an orbital period of $P = 7.200865 \pm 0.00002$ days, and an eccentricity of $e=0.337\pm 0.002$. The host star has a mass of $M_\star = 0.53 \pm 0.02{\rm M_\odot}$, a radius of $R_\star= 0.50 \pm 0.01{\rm R_\odot}$, an effective temperature of $T_{\rm eff} = 3621 \pm 48$K, and a metallicity of $\rm [Fe/H]=+0.06\pm 0.08$. TOI-2119b joins an emerging population of transiting BDs around M-dwarf host stars, with TOI-2119 being the ninth such system. These M-dwarf--brown dwarf systems typically occupy mass ratios near $q = M_b/M_\star \approx 0.1-0.2$, which separates them from the typical mass ratios for systems with transiting substellar objects and giant exoplanets that orbit more massive stars. The nature of the secondary eclipse of the BD by the star enables us to estimate the effective temperature of the substellar object to be $2030\pm 84$K, which is consistent with predictions by substellar evolutionary models., Comment: 14 pages, 13 figures, 4 tables, accepted in MNRAS
Published: 2022
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38. A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Author: Espinoza, Néstor, Pallé, Enric, Kemmer, Jonas, Luque, Rafael, Caballero, José A., Cifuentes, Carlos, Herrero, Enrique, Béjar, Víctor J. Sánchez, Stock, Stephan, Molaverdikhani, Karan, Morello, Giuseppe, Kossakowski, Diana, Schlecker, Martin, Amado, Pedro J., Bluhm, Paz, Cortés-Contreras, Miriam, Henning, Thomas, Kreidberg, Laura, Kürster, Martin, Lafarga, Marina, Lodieu, Nicolas, Morales, Juan Carlos, Oshagh, Mahmoudreza, Passegger, Vera M., Pavlov, Alexey, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rodríguez, Eloy, López, Cristina Rodríguez, Schweitzer, Andreas, Trifonov, Trifon, Chaturvedi, Priyanka, Dreizler, Stefan, Jeffers, Sandra V., Kaminski, Adrian, López-González, María José, Lillo-Box, Jorge, Montes, David, Nowak, Grzegorz, Pedraz, Santos, Vanaverbeke, Siegfried, Osorio, Maria R. Zapatero, Zechmeister, Mathias, Collins, Karen A., Girardin, Eric, Guerra, Pere, Naves, Ramon, Crossfield, Ian J. M., Matthews, Elisabeth C., Howell, Steve B., Ciardi, David R., Gonzales, Erica, Matson, Rachel A., Beichman, Charles A., Schlieder, Joshua E., Barclay, Thomas, Vezie, Michael, Villaseñor, Jesus Noel, Daylan, Tansu, Mireies, Ismael, Dragomir, Diana, Twicken, Joseph D., Jenkins, Jon, Winn, Joshua N., Latham, David, Ricker, George, Seager, Sara, Espinoza, Néstor, Pallé, Enric, Kemmer, Jonas, Luque, Rafael, Caballero, José A., Cifuentes, Carlos, Herrero, Enrique, Béjar, Víctor J. Sánchez, Stock, Stephan, Molaverdikhani, Karan, Morello, Giuseppe, Kossakowski, Diana, Schlecker, Martin, Amado, Pedro J., Bluhm, Paz, Cortés-Contreras, Miriam, Henning, Thomas, Kreidberg, Laura, Kürster, Martin, Lafarga, Marina, Lodieu, Nicolas, Morales, Juan Carlos, Oshagh, Mahmoudreza, Passegger, Vera M., Pavlov, Alexey, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rodríguez, Eloy, López, Cristina Rodríguez, Schweitzer, Andreas, Trifonov, Trifon, Chaturvedi, Priyanka, Dreizler, Stefan, Jeffers, Sandra V., Kaminski, Adrian, López-González, María José, Lillo-Box, Jorge, Montes, David, Nowak, Grzegorz, Pedraz, Santos, Vanaverbeke, Siegfried, Osorio, Maria R. Zapatero, Zechmeister, Mathias, Collins, Karen A., Girardin, Eric, Guerra, Pere, Naves, Ramon, Crossfield, Ian J. M., Matthews, Elisabeth C., Howell, Steve B., Ciardi, David R., Gonzales, Erica, Matson, Rachel A., Beichman, Charles A., Schlieder, Joshua E., Barclay, Thomas, Vezie, Michael, Villaseñor, Jesus Noel, Daylan, Tansu, Mireies, Ismael, Dragomir, Diana, Twicken, Joseph D., Jenkins, Jon, Winn, Joshua N., Latham, David, Ricker, George, and Seager, Sara
Abstract: We report the discovery and characterization of TOI-1759~b, a temperate (400 K) sub-Neptune-sized exoplanet orbiting the M~dwarf TOI-1759 (TIC 408636441). TOI-1759 b was observed by TESS to transit on sectors 16, 17 and 24, with only one transit observed per sector, creating an ambiguity on the orbital period of the planet candidate. Ground-based photometric observations, combined with radial-velocity measurements obtained with the CARMENES spectrograph, confirm an actual period of $18.85019 \pm 0.00014$ d. A joint analysis of all available photometry and radial velocities reveal a radius of $3.17 \pm 0.10\,R_\oplus$ and a mass of $10.8 \pm 1.5\,M_\oplus$. Combining this with the stellar properties derived for TOI-1759 ($R_\star = 0.597 \pm 0.015\,R_\odot$; $M_\star = 0.606 \pm 0.020\,M_\odot$; $T_{\textrm{eff}} = 4065 \pm 51$ K), we compute a transmission spectroscopic metric (TSM) value of over 80 for the planet, making it a good target for transmission spectroscopy studies. TOI-1759 b is among the top five temperate, small exoplanets ($T_\textrm{eq} < 500$ K, $R_p < 4 \,R_\oplus$) with the highest TSM discovered to date. Two additional signals with periods of 80 d and $>$ 200 d seem to be present in our radial velocities. While our data suggest both could arise from stellar activity, the later signal's source and periodicity are hard to pinpoint given the $\sim 200$ d baseline of our radial-velocity campaign with CARMENES. Longer baseline radial-velocity campaigns should be performed in order to unveil the true nature of this long period signal., Comment: 22 pages, 10 figures, 7 tables. AJ in press
Published: 2022
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39. A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Author: Wilson, Thomas G., Goffo, Elisa, Alibert, Yann, Gandolfi, Davide, Bonfanti, Andrea, Persson, Carina M., Cameron, Andrew Collier, Fridlund, Malcolm, Fossati, Luca, Korth, Judith, Benz, Willy, Deline, Adrien, Florén, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sébastien, Sousa, Sérgio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Bárczy, Tamas, Navascues, David Barrado y, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Billot, Nicolas, Bonfils, Xavier, Brandeker, Alexis, Broeg, Christopher, Bryant, Edward M., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Charnoz, Sébastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colón, Knicole D., Crouzet, Nicolas, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Dragomir, Diana, Dransfield, Georgina, Ehrenreich, David, Erikson, Anders, Fortier, Andrea, Gan, Tianjun, Gill, Samuel, Gillon, Michaël, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Güdel, Manuel, Guillot, Tristan, Haldemann, Jonas, Heng, Kevin, Horne, Keith, Howell, Steve B., Isaak, Kate G., Jenkins, Jon M., Jensen, Eric L. N., Kiss, Laszlo, Lacedelli, Gaia, Lam, Kristine, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavelier des, Lendl, Monika, Lester, Kathryn V., Levine, Alan M., Livingston, John, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Marie-Sainte, Wenceslas, Maxted, Pierre F. L., Mayo, Andrew W., McLean, Brian, Mecina, Marko, Mékarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Ségransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stéphane, Van Eylen, Vincent, Van Grootel, Valérie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, Winn, Joshua N., Wilson, Thomas G., Goffo, Elisa, Alibert, Yann, Gandolfi, Davide, Bonfanti, Andrea, Persson, Carina M., Cameron, Andrew Collier, Fridlund, Malcolm, Fossati, Luca, Korth, Judith, Benz, Willy, Deline, Adrien, Florén, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sébastien, Sousa, Sérgio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Bárczy, Tamas, Navascues, David Barrado y, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Billot, Nicolas, Bonfils, Xavier, Brandeker, Alexis, Broeg, Christopher, Bryant, Edward M., Burleigh, Matthew R., Buttu, Marco, Cabrera, Juan, Charnoz, Sébastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colón, Knicole D., Crouzet, Nicolas, Csizmadia, Szilard, Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier, Demory, Brice-Olivier, Dragomir, Diana, Dransfield, Georgina, Ehrenreich, David, Erikson, Anders, Fortier, Andrea, Gan, Tianjun, Gill, Samuel, Gillon, Michaël, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Güdel, Manuel, Guillot, Tristan, Haldemann, Jonas, Heng, Kevin, Horne, Keith, Howell, Steve B., Isaak, Kate G., Jenkins, Jon M., Jensen, Eric L. N., Kiss, Laszlo, Lacedelli, Gaia, Lam, Kristine, Laskar, Jacques, Latham, David W., Etangs, Alain Lecavelier des, Lendl, Monika, Lester, Kathryn V., Levine, Alan M., Livingston, John, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Marie-Sainte, Wenceslas, Maxted, Pierre F. L., Mayo, Andrew W., McLean, Brian, Mecina, Marko, Mékarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Ségransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stéphane, Van Eylen, Vincent, Van Grootel, Valérie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, and Winn, Joshua N.
Abstract: We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine $T_{\rm eff, \star}=4734\pm67$ K, $R_{\star}=0.726\pm0.007$ $R_{\odot}$, and $M_{\star}=0.748\pm0.032$ $M_{\odot}$. We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of $P_{\rm b}=6.44387\pm0.00003$ d, a radius of $R_{\rm b}=2.59\pm0.04$ $R_{\oplus}$, and a mass of $M_{\rm b}=13.5_{-1.8}^{+1.7}$ $M_{\oplus}$, whilst TOI-1064 c has an orbital period of $P_{\rm c}=12.22657^{+0.00005}_{-0.00004}$ d, a radius of $R_{\rm c}=2.65\pm0.04$ $R_{\oplus}$, and a 3$\sigma$ upper mass limit of 8.5 ${\rm M_{\oplus}}$. From the high-precision photometry we obtain radius uncertainties of $\sim$1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets., Comment: 30 pages, 24 figures, 6 tables including the Appendix; accepted for publication in MNRAS
Published: 2022
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40. Rapid contraction of giant planets orbiting the 20-million-year-old star V1298 Tau

Author: Ministerio de Ciencia e Innovación (España), European Commission, Suárez Mascareño, A., Damasso, M., Lodieu, N., Sozzetti, Alessandro, Béjar, Victor J. S., Benatti, S., Zapatero Osorio, María Rosa, Micela, Giusi, Rebolo López, Rafael, Desidera, S., Murgas, F., Claudi, Riccardo, González Hernández, Jonay I., Malavolta, L., Del Burgo, C., D'Orazi, V., Amado, Pedro J., Locci, D., Tabernero, H. M., Marzari, F., Aguado, D. S., Turrini, D., Cardona Guillén, C., Toledo-Padrón, B., Maggio, Antonio, Aceituno, Jesús, Bauer, Florian Franz, Caballero, J. A., Chinchilla, P., Esparza-Borges, E., González-Álvarez, E., Granzer, Thomas, Luque, R., Martín, Eduardo Lorenzo, Nowak, G., Oshagh, M., Pallé, Enric, Parviainen, H., Quirrenbach, Andreas, Reiners, Ansgar, Ribas, Ignasi, Strassmeier, K. G., Weber, M., Mallonn, Matthias, Ministerio de Ciencia e Innovación (España), European Commission, Suárez Mascareño, A., Damasso, M., Lodieu, N., Sozzetti, Alessandro, Béjar, Victor J. S., Benatti, S., Zapatero Osorio, María Rosa, Micela, Giusi, Rebolo López, Rafael, Desidera, S., Murgas, F., Claudi, Riccardo, González Hernández, Jonay I., Malavolta, L., Del Burgo, C., D'Orazi, V., Amado, Pedro J., Locci, D., Tabernero, H. M., Marzari, F., Aguado, D. S., Turrini, D., Cardona Guillén, C., Toledo-Padrón, B., Maggio, Antonio, Aceituno, Jesús, Bauer, Florian Franz, Caballero, J. A., Chinchilla, P., Esparza-Borges, E., González-Álvarez, E., Granzer, Thomas, Luque, R., Martín, Eduardo Lorenzo, Nowak, G., Oshagh, M., Pallé, Enric, Parviainen, H., Quirrenbach, Andreas, Reiners, Ansgar, Ribas, Ignasi, Strassmeier, K. G., Weber, M., and Mallonn, Matthias
Abstract: Current theories of planetary evolution predict that infant giant planets have large radii and very low densities before they slowly contract to reach their final size after about several hundred million years1,2. These theoretical expectations remain untested so far as the detection and characterization of very young planets is extremely challenging due to the intense stellar activity of their host stars3,4. Only the recent discoveries of young planetary transiting systems allow initial constraints to be placed on evolutionary models5,6,7. With an estimated age of 20 million years, V1298 Tau is one of the youngest solar-type stars known to host transiting planets; it harbours a system composed of four planets, two Neptune-sized, one Saturn-sized and one Jupiter-sized8,9. Here we report a multi-instrument radial velocity campaign of V1298 Tau, which allowed us to determine the masses of two of the planets in the system. We find that the two outermost giant planets, V1298 Tau b and e (0.64 ± 0.19 and 1.16 ± 0.30 Jupiter masses, respectively), seem to contradict our knowledge of early-stages planetary evolution. According to models, they should reach their mass–radius combination only hundreds of millions of years after formation. This result suggests that giant planets can contract much more quickly than usually assumed. © 2021, The Author(s), under exclusive licence to Springer Nature Limited.
Published: 2022

41. The CARMENES search for exoplanets around M dwarfs: Two Saturn-mass planets orbiting active stars

Author: Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), Quirrenbach, Andreas, Passegger, V.M., Trifonov, T., Amado, Pedro J., Caballero, J. A., Reiners, Ansgar, Ribas, Ignasi, Aceituno, Jesús, Béjar, Victor J. S., Chaturvedi, P., González-Cuesta, L., Henning, Thomas, Herrero, E., Kaminski, A., Kürster, M., Lalitha, S., Lodieu, N., López González, Maria J., Montes, D., Pallé, Enric, Perger, M., Pollacco, D., Reffert, S., Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Shan, Y., Tal-Or, L., Zapatero Osorio, María Rosa, Zechmeister, Mathias, Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), Quirrenbach, Andreas, Passegger, V.M., Trifonov, T., Amado, Pedro J., Caballero, J. A., Reiners, Ansgar, Ribas, Ignasi, Aceituno, Jesús, Béjar, Victor J. S., Chaturvedi, P., González-Cuesta, L., Henning, Thomas, Herrero, E., Kaminski, A., Kürster, M., Lalitha, S., Lodieu, N., López González, Maria J., Montes, D., Pallé, Enric, Perger, M., Pollacco, D., Reffert, S., Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Shan, Y., Tal-Or, L., Zapatero Osorio, María Rosa, and Zechmeister, Mathias
Abstract: The CARMENES radial-velocity survey is currently searching for planets in a sample of 387 M dwarfs. Here we report on two Saturn-mass planets orbiting TYC 2187-512-1 (M* = 0.50 M⊙) and TZ Ari (M* = 0.15 M⊙), respectively. We obtained supplementary photometric time series, which we use along with spectroscopic information to determine the rotation periods of the two stars. In both cases, the radial velocities also show strong modulations at the respective rotation period. We thus modeled the radial velocities as a Keplerian orbit plus a Gaussian process representing the stellar variability. TYC 2187-512-1 is found to harbor a planet with a minimum mass of 0.33 MJup in a near-circular 692-day orbit. The companion of TZ Ari has a minimum mass of 0.21 MJup, orbital period of 771 d, and orbital eccentricity of 0.46. We provide an overview of all known giant planets in the CARMENES sample, from which we infer an occurrence rate of giant planets orbiting M dwarfs with periods up to 2 yr in the range between 2 and 6%. TZ Ari b is only the second giant planet discovered orbiting a host with mass less than 0.3 M⊙. These objects occupy an extreme location in the planet mass versus host mass plane. It is difficult to explain their formation in core-accretion scenarios, so they may possibly have been formed through a disk fragmentation process. © ESO 2022.
Published: 2022

42. TOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit

Author: Wong, Ian, Shporer, Avi, Zhou, George, Kitzmann, Daniel, Komacek, Thaddeus D., Tan, Xianyu, Tronsgaard, René, Buchhave, Lars A., Vissapragada, Shreyas, Greklek-McKeon, Michael, Rodriguez, Joseph E., Ahlers, John P., Quinn, Samuel N., Furlan, Elise, Howell, Steve B., Bieryla, Allyson, Heng, Kevin, Knutson, Heather A., Collins, Karen A., McLeod, Kim K., Berlind, Perry, Brown, Peyton, Calkins, Michael L., Leon, Jerome P. de, Esparza-Borges, Emma, Esquerdo, Gilbert A., Fukui, Akihiko, Gan, Tianjun, Girardin, Eric, Gnilka, Crystal L., Ikoma, Masahiro, Jensen, Eric L. N., Kielkopf, John, Kodama, Takanori, Kurita, Seiya, Lester, Kathryn V., Lewin, Pablo, Marino, Giuseppe, Murgas, Felipe, Narita, Norio, Pallé, Enric, Schwarz, Richard P., Stassun, Keivan G., Tamura, Motohide, Watanabe, Noriharu, Benneke, Björn, Ricker, George R., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Caldwell, Douglas A., Fong, William, Huang, Chelsea X., Mireles, Ismael, Schlieder, Joshua E., Shiao, Bernie, Villaseñor, Jesus Noel, Wong, Ian, Shporer, Avi, Zhou, George, Kitzmann, Daniel, Komacek, Thaddeus D., Tan, Xianyu, Tronsgaard, René, Buchhave, Lars A., Vissapragada, Shreyas, Greklek-McKeon, Michael, Rodriguez, Joseph E., Ahlers, John P., Quinn, Samuel N., Furlan, Elise, Howell, Steve B., Bieryla, Allyson, Heng, Kevin, Knutson, Heather A., Collins, Karen A., McLeod, Kim K., Berlind, Perry, Brown, Peyton, Calkins, Michael L., Leon, Jerome P. de, Esparza-Borges, Emma, Esquerdo, Gilbert A., Fukui, Akihiko, Gan, Tianjun, Girardin, Eric, Gnilka, Crystal L., Ikoma, Masahiro, Jensen, Eric L. N., Kielkopf, John, Kodama, Takanori, Kurita, Seiya, Lester, Kathryn V., Lewin, Pablo, Marino, Giuseppe, Murgas, Felipe, Narita, Norio, Pallé, Enric, Schwarz, Richard P., Stassun, Keivan G., Tamura, Motohide, Watanabe, Noriharu, Benneke, Björn, Ricker, George R., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Caldwell, Douglas A., Fong, William, Huang, Chelsea X., Mireles, Ismael, Schlieder, Joshua E., Shiao, Bernie, and Villaseñor, Jesus Noel
Published: 2021

43. TOI-2109b: An Ultrahot Gas Giant on a 16 hr Orbit

Author: Wong, Ian, Shporer, Avi, Zhou, George, Kitzmann, Daniel, Komacek, Thaddeus D., Tan, Xianyu, Tronsgaard, René, Buchhave, Lars A., Vissapragada, Shreyas, Greklek-McKeon, Michael, Rodriguez, Joseph E., Ahlers, John P., Quinn, Samuel N., Furlan, Elise, Howell, Steve B., Bieryla, Allyson, Heng, Kevin, Knutson, Heather A., Collins, Karen A., McLeod, Kim K., Berlind, Perry, Brown, Peyton, Calkins, Michael L., de Leon, Jerome P., Esparza-Borges, Emma, Esquerdo, Gilbert A., Fukui, Akihiko, Gan, Tianjun, Girardin, Eric, Gnilka, Crystal L., Ikoma, Masahiro, Jensen, Eric L. N., Kielkopf, John, Kodama, Takanori, Kurita, Seiya, Lester, Kathryn V., Lewin, Pablo, Marino, Giuseppe, Murgas, Felipe, Narita, Norio, Pallé, Enric, Schwarz, Richard P., Stassun, Keivan G., Tamura, Motohide, Watanabe, Noriharu, Benneke, Björn, Ricker, George R., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Caldwell, Douglas A., Fong, William, Huang, Chelsea X., Mireles, Ismael, Schlieder, Joshua E., Shiao, Bernie, Villaseñor, Jesus Noel, Wong, Ian, Shporer, Avi, Zhou, George, Kitzmann, Daniel, Komacek, Thaddeus D., Tan, Xianyu, Tronsgaard, René, Buchhave, Lars A., Vissapragada, Shreyas, Greklek-McKeon, Michael, Rodriguez, Joseph E., Ahlers, John P., Quinn, Samuel N., Furlan, Elise, Howell, Steve B., Bieryla, Allyson, Heng, Kevin, Knutson, Heather A., Collins, Karen A., McLeod, Kim K., Berlind, Perry, Brown, Peyton, Calkins, Michael L., de Leon, Jerome P., Esparza-Borges, Emma, Esquerdo, Gilbert A., Fukui, Akihiko, Gan, Tianjun, Girardin, Eric, Gnilka, Crystal L., Ikoma, Masahiro, Jensen, Eric L. N., Kielkopf, John, Kodama, Takanori, Kurita, Seiya, Lester, Kathryn V., Lewin, Pablo, Marino, Giuseppe, Murgas, Felipe, Narita, Norio, Pallé, Enric, Schwarz, Richard P., Stassun, Keivan G., Tamura, Motohide, Watanabe, Noriharu, Benneke, Björn, Ricker, George R., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Caldwell, Douglas A., Fong, William, Huang, Chelsea X., Mireles, Ismael, Schlieder, Joshua E., Shiao, Bernie, and Villaseñor, Jesus Noel
Abstract: We report the discovery of an ultrahot Jupiter with an extremely short orbital period of $0.67247414\,\pm\,0.00000028$ days ($\sim$16 hr). The $1.347 \pm 0.047$ $R_{\rm Jup}$ planet, initially identified by the Transiting Exoplanet Survey Satellite (TESS) mission, orbits TOI-2109 (TIC 392476080): a $T_{\rm eff} \sim 6500$ K F-type star with a mass of $1.447 \pm 0.077$ $M_{\rm Sun}$, a radius of $1.698 \pm 0.060$ $R_{\rm Sun}$, and a rotational velocity of $v\sin i_* = 81.9 \pm 1.7$ km s$^{-1}$. The planetary nature of TOI-2109b was confirmed through radial velocity measurements, which yielded a planet mass of $5.02 \pm 0.75$ $M_{\rm Jup}$. Analysis of the Doppler shadow in spectroscopic transit observations indicates a well-aligned system, with a sky-projected obliquity of $\lambda = 1\overset{\circ}{.}7 \pm 1\overset{\circ}{.}7$. From the TESS full-orbit light curve, we measured a secondary eclipse depth of $731 \pm 46$ ppm, as well as phase-curve variations from the planet's longitudinal brightness modulation and ellipsoidal distortion of the host star. Combining the TESS-band occultation measurement with a $K_s$-band secondary eclipse depth ($2012 \pm 80$ ppm) derived from ground-based observations, we find that the dayside emission of TOI-2109b is consistent with a brightness temperature of $3631 \pm 69$ K, making it the second hottest exoplanet hitherto discovered. By virtue of its extreme irradiation and strong planet-star gravitational interaction, TOI-2109b is an exceptionally promising target for intensive follow-up studies using current and near-future telescope facilities to probe for orbital decay, detect tidally driven atmospheric escape, and assess the impacts of H$_2$ dissociation and recombination on the global heat transport., Comment: 30 pages, 17 figures, published in AJ
Published: 2021
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44. TOI-2285b: A 1.7 Earth-radius Planet Near the Habitable Zone around a Nearby M Dwarf

Author: Fukui, Akihiko, Kimura, Tadahiro, Hirano, Teruyuki, Narita, Norio, Kodama, Takanori, Hori, Yasunori, Ikoma, Masahiro, Pallé, Enric, Murgas, Felipe, Parviainen, Hannu, Kawauchi, Kiyoe, Mori, Mayuko, Esparza-Borges, Emma, Bieryla, Allyson, Irwin, Jonathan, Safonov, Boris S., Stassun, Keivan G., Alvarez-Hernandez, Leticia, Béjar, Víctor J. S., Casasayas-Barris, Núria, Chen, Guo, Crouzet, Nicolas, de Leon, Jerome P., Isogai, Keisuke, Kagetani, Taiki, Klagyivik, Peter, Korth, Judith, Kurita, Seiya, Kusakabe, Nobuhiko, Livingston, John, Luque, Rafael, Madrigal-Aguado, Alberto, Morello, Giuseppe, Nishiumi, Taku, Orell-Miquel, Jaume, Oshagh, Mahmoudreza, Sánchez-Benavente, Manuel, Stangret, Monika, Terada, Yuka, Watanabe, Noriharu, Zou, Yujie, Tamura, Motohide, Kurokawa, Takashi, Kuzuhara, Masayuki, Nishikawa, Jun, Omiya, Masashi, Vievard, Sébastien, Ueda, Akitoshi, Latham, David W., Quinn, Samuel N., Strakhov, Ivan S., Belinski, Alexandr A., Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua N., Charbonneau, David, Ciardi, David R., Collins, Karen A., Doty, John P., Bachelet, Etienne, Harbeck, Daniel, Fukui, Akihiko, Kimura, Tadahiro, Hirano, Teruyuki, Narita, Norio, Kodama, Takanori, Hori, Yasunori, Ikoma, Masahiro, Pallé, Enric, Murgas, Felipe, Parviainen, Hannu, Kawauchi, Kiyoe, Mori, Mayuko, Esparza-Borges, Emma, Bieryla, Allyson, Irwin, Jonathan, Safonov, Boris S., Stassun, Keivan G., Alvarez-Hernandez, Leticia, Béjar, Víctor J. S., Casasayas-Barris, Núria, Chen, Guo, Crouzet, Nicolas, de Leon, Jerome P., Isogai, Keisuke, Kagetani, Taiki, Klagyivik, Peter, Korth, Judith, Kurita, Seiya, Kusakabe, Nobuhiko, Livingston, John, Luque, Rafael, Madrigal-Aguado, Alberto, Morello, Giuseppe, Nishiumi, Taku, Orell-Miquel, Jaume, Oshagh, Mahmoudreza, Sánchez-Benavente, Manuel, Stangret, Monika, Terada, Yuka, Watanabe, Noriharu, Zou, Yujie, Tamura, Motohide, Kurokawa, Takashi, Kuzuhara, Masayuki, Nishikawa, Jun, Omiya, Masashi, Vievard, Sébastien, Ueda, Akitoshi, Latham, David W., Quinn, Samuel N., Strakhov, Ivan S., Belinski, Alexandr A., Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua N., Charbonneau, David, Ciardi, David R., Collins, Karen A., Doty, John P., Bachelet, Etienne, and Harbeck, Daniel
Abstract: We report the discovery of TOI-2285b, a sub-Neptune-sized planet transiting a nearby (42 pc) M dwarf with a period of 27.3 days. We identified the transit signal from the Transiting Exoplanet Survey Satellite photometric data, which we confirmed with ground-based photometric observations using the multiband imagers MuSCAT2 and MuSCAT3. Combining these data with other follow-up observations including high resolution spectroscopy with the Tillinghast Reflector Echelle Spectrograph, high resolution imaging with the SPeckle Polarimeter, and radial velocity (RV) measurements with the InfraRed Doppler instrument, we find that the planet has a radius of 1.74 $\pm$ 0.08 $R_\oplus$, a mass of $<$ 19.5 $M_\oplus$ (95\% c.l.), and an insolation flux of 1.54 $\pm$ 0.14 times that of the Earth. Although the planet resides just outside the habitable zone for a rocky planet, if the planet harbors an H$_2$O layer under a hydrogen-rich atmosphere, then liquid water could exist on the surface of the H$_2$O layer depending on the planetary mass and water mass fraction. The bright host star in the near infrared ($K_s=9.0$) makes this planet an excellent target for further RV and atmospheric observations to improve our understanding on the composition, formation, and habitability of sub-Neptune-sized planets., Comment: 9 pages, 3 figures, published online in PASJ
Published: 2021
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45. TKS V. Twin sub-Neptunes Transiting the Nearby G Star HD 63935

Author: Scarsdale, Nicholas, Murphy, Joseph M. Akana, Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney D., Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Beard, Corey, Behmard, Aida, Chontos, Ashley, Christiansen, Jessie L., Ciardi, David R., Claytor, Zachary R., Collins, Karen A., Collins, Kevin I., Dai, Fei, Dalba, Paul A., Dragomir, Diana, Fetherolf, Tara, Fukui, Akihiko, Giacalone, Steven, Gonzales, Erica J., Hill, Michelle L., Hirsch, Lea A., Jensen, Eric L. N., Kosiarek, Molly R., de Leon, Jerome P., Lubin, Jack, Lund, Michael B., Luque, Rafael, Mayo, Andrew W., Močnik, Teo, Mori, Mayuko, Narita, Norio, Nowak, Grzegorz, Pallé, Enric, Rabus, Markus, Rosenthal, Lee J., Rubenzahl, Ryan A., Schlieder, Joshua E., Shporer, Avi, Stassun, Keivan G., Twicken, Joe, Wang, Gavin, Wohler, Bill, Yahalomi, Daniel A., Jenkins, Jon, Latham, David W., Ricker, George R., Seager, S., Vanderspek, Roland, Winn, Joshua N., Scarsdale, Nicholas, Murphy, Joseph M. Akana, Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney D., Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Beard, Corey, Behmard, Aida, Chontos, Ashley, Christiansen, Jessie L., Ciardi, David R., Claytor, Zachary R., Collins, Karen A., Collins, Kevin I., Dai, Fei, Dalba, Paul A., Dragomir, Diana, Fetherolf, Tara, Fukui, Akihiko, Giacalone, Steven, Gonzales, Erica J., Hill, Michelle L., Hirsch, Lea A., Jensen, Eric L. N., Kosiarek, Molly R., de Leon, Jerome P., Lubin, Jack, Lund, Michael B., Luque, Rafael, Mayo, Andrew W., Močnik, Teo, Mori, Mayuko, Narita, Norio, Nowak, Grzegorz, Pallé, Enric, Rabus, Markus, Rosenthal, Lee J., Rubenzahl, Ryan A., Schlieder, Joshua E., Shporer, Avi, Stassun, Keivan G., Twicken, Joe, Wang, Gavin, Wohler, Bill, Yahalomi, Daniel A., Jenkins, Jon, Latham, David W., Ricker, George R., Seager, S., Vanderspek, Roland, and Winn, Joshua N.
Abstract: We present the discovery of two nearly identically-sized sub-Neptune transiting planets orbiting HD 63935, a bright ($V=8.6$ mag), sun-like ($T_{eff}=5560K$) star at 49 pc. TESS identified the first planet, HD 63935 b (TOI-509.01), in Sectors 7 and 34. We identified the second signal (HD 63935 c) in Keck HIRES and Lick APF radial velocity data as part of our followup campaign. It was subsequently confirmed with TESS photometry in Sector 34 as TOI-509.02. Our analysis of the photometric and radial velocity data yields a robust detection of both planets with periods of $9.0600 \pm 0.007$ and $21.40 \pm 0.0019$ days, radii of $2.99 \pm 0.14$ and $2.90 \pm 0.13$ $R_\oplus$, and masses of $10.8 \pm 1.8$ and $11.1 \pm 2.4$ $M_\oplus$. We calculate densities for planets b and c consistent with a few percent of the planet mass in hydrogen/helium envelopes. We also describe our survey's efforts to choose the best targets for JWST atmospheric followup. These efforts suggest that HD 63935 b will have the most clearly visible atmosphere of its class. It is the best target for transmission spectroscopy (ranked by Transmission Spectroscopy Metric, a proxy for atmospheric observability) in the so-far uncharacterized parameter space comprising sub-Neptune-sized (2.6 $R_\oplus$ $<$ $R_p$ $<$ 4 $R_\oplus$), moderately-irradiated (100 $F_\oplus$ $<$ $F_p$ $<$ 1000 $F_\oplus$) planets around G-stars. Planet c is also a viable target for transmission spectroscopy, and given the indistinguishable masses and radii of the two planets, the system serves as a natural laboratory for examining the processes that shape the evolution of sub-Neptune planets., Comment: 22 pages, 12 figures, published in AJ
Published: 2021
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46. The strange case of Na I in the atmosphere of HD209458 b: Reconciling low- and high-resolution spectroscopic observations G

Author: Morello, Giuseppe, Casasayas-Barris, Núria, Orell-Miquel, Jaume, Pallé, Enric, Cracchiolo, Gianluca, Micela, Giuseppina, Morello, Giuseppe, Casasayas-Barris, Núria, Orell-Miquel, Jaume, Pallé, Enric, Cracchiolo, Gianluca, and Micela, Giuseppina
Abstract: Aims. We aim to investigate the origin of the discrepant results reported in the literature about the presence of Na I in the atmosphere of HD209458 b, based on low- and high-resolution transmission spectroscopy. Methods. We generated synthetic planetary atmosphere models and we compared them with the transmission light curves and spectra observed in previous studies. Our models account for the stellar limb-darkening and Rossiter-McLaughlin (RM) effects, and contemplate various possible scenarios for the planetary atmosphere. Results. We reconciled the discrepant results by identifying a range of planetary atmospheres that are consistent with previous low- and high-resolution spectroscopic observations. Either both datasets are interpreted as consistent with a total absence of Na I in the planetary atmosphere (with Hubble Space Telescope data being affected by limb darkening), or the terminator temperature of HD209458 b has to have an upper limit of about 1000K. In particular, we find that 1D transmission spectra with lower-than-equilibrium temperatures can also explain the previously reported detection of absorption signal at low resolution due to differential transit depth in adjacent bands, while the cores of the Na I D lines may be masked by the strong RM signal seen at high resolution. We also rule out high-altitude clouds, which would otherwise mask the absorption signal at low resolution, as the source of the discrepancies. Conclusions. This work highlights the synergies between different observing techniques, specifically low- and high-resolution spectroscopy, to fully characterise transiting exoplanet systems., Comment: Accepted version to be published on A&A
Published: 2021
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47. Diving Beneath the Sea of Stellar Activity: Chromatic Radial Velocities of the Young AU Mic Planetary System

Author: Cale, Bryson, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Gaidos, Eric, Gagné, Jonathan, Gao, Peter, Kane, Stephen R., Béjar, Víctor J. S., Lodieu, Nicolas, Anglada-Escudé, Guillem, Ribas, Ignasi, Pallé, Enric, Quirrenbach, Andreas, Amado, Pedro J., Reiners, Ansgar, Caballero, José A., Osorio, María Rosa Zapatero, Dreizler, Stefan, Howard, Andrew W., Fulton, Benjamin J., Wang, Sharon Xuesong, Collins, Kevin I., Mufti, Mohammed El, Wittrock, Justin, Gilbert, Emily A., Barclay, Thomas, Klein, Baptiste, Martioli, Eder, Wittenmyer, Robert, Wright, Duncan, Addison, Brett, Hirano, Teruyuki, Tamura, Motohide, Kotani, Takayuki, Narita, Norio, Vermilion, David, Lee, Rena A., Geneser, Claire, Teske, Johanna, Quinn, Samuel N., Latham, David W., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Zohrabi, Farzaneh, Stibbards, Caitlin, Kotnana, Srihan, Jenkins, Jon, Twicken, Joseph D., Henze, Christopher, Kidwell Jr., Richard, Burke, Christopher, n}or, Joel Villase{\~, Boyd, Patricia, Cale, Bryson, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Gaidos, Eric, Gagné, Jonathan, Gao, Peter, Kane, Stephen R., Béjar, Víctor J. S., Lodieu, Nicolas, Anglada-Escudé, Guillem, Ribas, Ignasi, Pallé, Enric, Quirrenbach, Andreas, Amado, Pedro J., Reiners, Ansgar, Caballero, José A., Osorio, María Rosa Zapatero, Dreizler, Stefan, Howard, Andrew W., Fulton, Benjamin J., Wang, Sharon Xuesong, Collins, Kevin I., Mufti, Mohammed El, Wittrock, Justin, Gilbert, Emily A., Barclay, Thomas, Klein, Baptiste, Martioli, Eder, Wittenmyer, Robert, Wright, Duncan, Addison, Brett, Hirano, Teruyuki, Tamura, Motohide, Kotani, Takayuki, Narita, Norio, Vermilion, David, Lee, Rena A., Geneser, Claire, Teske, Johanna, Quinn, Samuel N., Latham, David W., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Zohrabi, Farzaneh, Stibbards, Caitlin, Kotnana, Srihan, Jenkins, Jon, Twicken, Joseph D., Henze, Christopher, Kidwell Jr., Richard, Burke, Christopher, n}or, Joel Villase{\~, and Boyd, Patricia
Abstract: We present updated radial-velocity (RV) analyses of the AU Mic system. AU Mic is a young (22 Myr) early M dwarf known to host two transiting planets - $P_{b}\sim8.46$ days, $R_{b}=4.38_{-0.18}^{+0.18}\ R_{\oplus}$, $P_{c}\sim18.86$ days, $R_{c}=3.51_{-0.16}^{+0.16}\ R_{\oplus}$. With visible RVs from CARMENES-VIS, CHIRON, HARPS, HIRES, {\sc {\textsc{Minerva}}}-Australis, and TRES, as well as near-infrared (NIR) RVs from CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a $5\sigma$ upper limit to the mass of AU Mic c of $M_{c}\leq20.13\ M_{\oplus}$ and present a refined mass of AU Mic b of $M_{b}=20.12_{-1.57}^{+1.72}\ M_{\oplus}$. Used in our analyses is a new RV modeling toolkit to exploit the wavelength dependence of stellar activity present in our RVs via wavelength-dependent Gaussian processes. By obtaining near-simultaneous visible and near-infrared RVs, we also compute the temporal evolution of RV-``color'' and introduce a regressional method to aid in isolating Keplerian from stellar activity signals when modeling RVs in future works. Using a multi-wavelength Gaussian process model, we demonstrate the ability to recover injected planets at $5\sigma$ significance with semi-amplitudes down to $\approx$ 10\,m\,s$^{-1}$ with a known ephemeris, more than an order of magnitude below the stellar activity amplitude. However, we find that the accuracy of the recovered semi-amplitudes is $\sim$50\% for such signals with our model.
Published: 2021
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48. Wolf 503 b: Characterization of a Sub-Neptune Orbiting a Metal-Poor K Dwarf

Author: Polanski, Alex S., Crossfield, Ian J. M., Burt, Jennifer A., Nowak, Grzegorz, López-Morales, Mercedes, Mortier, Annelies, Poretti, Ennio, Behmard, Aida, Benneke, Björn, Blunt, Sarah, Bonomo, Aldo S., Butler, R. Paul, Chontos, Ashley, Cosentino, Rosario, Crane, Jeffrey D., Dumusque, Xavier, Fulton, Benjamin J., Ghedina, Adriano, Gorjian, Varoujan, Grunblatt, Samuel K., Harutyunyan, Avet, Howard, Andrew W., Isaacson, Howard, Kosiarek, Molly R., Latham, David W., Luque, Rafael, Fiorenzano, Aldo F. Martinez, Mayor, Michel, Mills, Sean M., Molinari, Emilio, Nagel, Evangelos, Pallé, Enric, Petigura, Erik A., Shectman, Stephen A., Sozzetti, Alessandro, Teske, Johanna K., Wang, Sharon Xuesong, Weiss, Lauren M., Polanski, Alex S., Crossfield, Ian J. M., Burt, Jennifer A., Nowak, Grzegorz, López-Morales, Mercedes, Mortier, Annelies, Poretti, Ennio, Behmard, Aida, Benneke, Björn, Blunt, Sarah, Bonomo, Aldo S., Butler, R. Paul, Chontos, Ashley, Cosentino, Rosario, Crane, Jeffrey D., Dumusque, Xavier, Fulton, Benjamin J., Ghedina, Adriano, Gorjian, Varoujan, Grunblatt, Samuel K., Harutyunyan, Avet, Howard, Andrew W., Isaacson, Howard, Kosiarek, Molly R., Latham, David W., Luque, Rafael, Fiorenzano, Aldo F. Martinez, Mayor, Michel, Mills, Sean M., Molinari, Emilio, Nagel, Evangelos, Pallé, Enric, Petigura, Erik A., Shectman, Stephen A., Sozzetti, Alessandro, Teske, Johanna K., Wang, Sharon Xuesong, and Weiss, Lauren M.
Abstract: Using radial velocity measurements from four instruments, we report the mass and density of a $2.043\pm0.069 ~\rm{R}_{\oplus}$ sub-Neptune orbiting the quiet K-dwarf Wolf 503 (HIP 67285). In addition, we present improved orbital and transit parameters by analyzing previously unused short-cadence $K2$ campaign 17 photometry and conduct a joint radial velocity-transit fit to constrain the eccentricity at $0.41\pm0.05$. The addition of a transit observation by $Spitzer$ also allows us to refine the orbital ephemeris in anticipation of further follow-up. Our mass determination, $6.26^{+0.69}_{-0.70}~\rm{M}_{\odot}$, in combination with the updated radius measurements, gives Wolf 503 b a bulk density of $\rho = 2.92\pm ^{+0.50}_{-0.44}$ $\rm{g}~\rm{cm}^{-3}$. Using interior composition models, we find this density is consistent with an Earth-like core with either a substantial $\rm{H}_2\rm{O}$ mass fraction ($45^{+19.12}_{-16.15}\%$) or a modest H/He envelope ($0.5\pm0.28\%$). The low H/He mass fraction, along with the old age of Wolf 503 ($11\pm2$ Gyrs), makes this sub-Neptune an opportune subject for testing theories of XUV-driven mass loss while the brightness of its host ($J=8.3$ mag) makes it an attractive target for transmission spectroscopy., Comment: Accepted to ApJ 2021 July 15
Published: 2021
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49. Transit detection of the long-period volatile-rich super-Earth $\nu^2$ Lupi d with $CHEOPS$

Author: Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Escudé, Guillem Anglada, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Cameron, Andrew Collier, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Muñoz, Antonio Garcia, Gillon, Michaël, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Etangs, Alain Lecavelier des, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, Walton, Nicholas A., Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Escudé, Guillem Anglada, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Cameron, Andrew Collier, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Muñoz, Antonio Garcia, Gillon, Michaël, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Etangs, Alain Lecavelier des, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, and Walton, Nicholas A.
Abstract: Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior, and orbital properties of the planetary companions. $\nu^2$ Lupi (HD 136352) is a naked-eye ($V = 5.78$) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6, and 107.6 days via radial velocity monitoring (Udry et al. 2019). The two inner planets (b and c) were recently found to transit (Kane et al. 2020), prompting a photometric follow-up by the brand-new $CHaracterising\:ExOPlanets\:Satellite\:(CHEOPS)$. Here, we report that the outer planet d is also transiting, and measure its radius and mass to be $2.56\pm0.09$ $R_{\oplus}$ and $8.82\pm0.94$ $M_{\oplus}$, respectively. With its bright Sun-like star, long period, and mild irradiation ($\sim$5.7 times the irradiation of Earth), $\nu^2$ Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b likely has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen-helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the $\nu^2$ Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets., Comment: Published in Nature Astronomy. 60 pages, 18 Figures, 6 Tables. This is the authors' version of the manuscript. The final authenticated version is available online at https://www.nature.com/articles/s41550-021-01381-5
Published: 2021
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50. Transit detection of the long-period volatile-rich super-Earth nu(2) Lupi d with CHEOPS

Author: Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Anglada-Escudé, Guillem, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Collier Cameron, Andrew, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Garcia Muñoz, Antonio, Gillon, Michael, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Lecavelier des Etangs, Alain, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, Walton, Nicholas A., Delrez, Laetitia, Ehrenreich, David, Alibert, Yann, Bonfanti, Andrea, Borsato, Luca, Fossati, Luca, Hooton, Matthew J., Hoyer, Sergio, Pozuelos, Francisco J., Salmon, Sébastien, Sulis, Sophia, Wilson, Thomas G., Adibekyan, Vardan, Bourrier, Vincent, Brandeker, Alexis, Charnoz, Sébastien, Deline, Adrien, Guterman, Pascal, Haldemann, Jonas, Hara, Nathan, Oshagh, Mahmoudreza, Sousa, Sergio G., Van Grootel, Valérie, Alonso, Roi, Anglada-Escudé, Guillem, Bárczy, Tamás, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Bekkelien, Anja, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Broeg, Christopher, Cabrera, Juan, Collier Cameron, Andrew, Davies, Melvyn B., Deleuil, Magali, Delisle, Jean-Baptiste, Demangeon, Olivier D. S., Demory, Brice-Olivier, Erikson, Anders, Fortier, Andrea, Fridlund, Malcolm, Futyan, David, Gandolfi, Davide, Garcia Muñoz, Antonio, Gillon, Michael, Guedel, Manuel, Heng, Kevin, Kiss, László, Laskar, Jacques, Lecavelier des Etangs, Alain, Lendl, Monika, Lovis, Christophe, Maxted, Pierre F. L., Nascimbeni, Valerio, Olofsson, Göran, Osborn, Hugh P., Pagano, Isabella, Pallé, Enric, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rauer, Heike, Ragazzoni, Roberto, Ribas, Ignasi, Santos, Nuno C., Scandariato, Gaetano, Ségransan, Damien, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Szabó, Gyula M., Thomas, Nicolas, Udry, Stéphane, and Walton, Nicholas A.
Abstract: Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior and orbital properties of the planetary companions. nu(2) Lupi (HD 136352) is a naked-eye (V = 5.78) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6 and 107.6 d via radial-velocity monitoring(1). The two inner planets (b and c) were recently found to transit(2), prompting a photometric follow-up by the brand new Characterising Exoplanets Satellite (CHEOPS). Here, we report that the outer planet d is also transiting, and measure its radius and mass to be 2.56 +/- 0.09 R-circle plus and 8.82 +/- 0.94 M-circle plus, respectively. With its bright Sun-like star, long period and mild irradiation (similar to 5.7 times the irradiation of Earth), nu(2) Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b probably has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen-helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the nu(2) Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets.
Published: 2021
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