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1. TOI-1173 A $b$: The First Inflated Super-Neptune in a Wide Binary System

Author: Galarza, Jhon Yana, Ferreira, Thiago, Lorenzo-Oliveira, Diego, Simon, Joshua D., Reggiani, Henrique, Piro, Anthony L., McWilliam, Andrew, Netto, Yuri, Valio, Adriana, Ciardi, David R., Galarza, Jhon Yana, Ferreira, Thiago, Lorenzo-Oliveira, Diego, Simon, Joshua D., Reggiani, Henrique, Piro, Anthony L., McWilliam, Andrew, Netto, Yuri, Valio, Adriana, and Ciardi, David R.
Abstract: Among Neptunian mass planets exoplanets ($20-50$ M$_\oplus$), puffy hot Neptunes are extremely rare, and their unique combination of low mass and extended radii implies very low density ($\rho < 0.3$ g cm$^{-3}$). Over the last decade, only a few puffy planets have been detected and precisely characterized with both transit and radial velocity observations, most notably including WASP-107 $b$, TOI-1420 $b$, and WASP-193 $b$. In this paper, we report the discovery of TOI-1173 A $b$, a low-density ($\rho = 0.269_{-0.024}^{+0.028}$ g cm$^{-3}$) super-Neptune with $P = 7.06$ days in a nearly circular orbit around the primary G-dwarf star in the wide binary system TOI-1173 A/B. Using radial velocity observations with the MAROON-X spectrograph and transit photometry from TESS, we determined a planet mass of $M_{\rm{p}} = 26.1\pm1.9\ M_{\oplus}$ and radius of $R_{\rm{p}} = 8.10\pm0.17\ R_{\oplus}$. TOI-1173 A $b$ is the first puffy Super-Neptune planet detected in a wide binary system (separation $\sim 11,400$ AU). We explored several mechanisms to understand the puffy nature of TOI-1173 A $b$, and showed that tidal heating is the most promising explanation. Furthermore, we demonstrate that TOI-1173 A $b$ likely has maintained its orbital stability over time and may have undergone von-Zeipel-Lidov-Kozai migration followed by tidal circularization given its present-day architecture, with important implications for planet migration theory and induced engulfment into the host star. Further investigation of the atmosphere of TOI-1173 A $b$ will shed light on the origin of close-in low-density Neptunian planets in field and binary systems, while spin-orbit analyses may elucidate the dynamical evolution of the system., Comment: Article submitted and is under revision to the AAS Astrophysical Journal. Welcome any comments and suggestions!
Published: 2024

2. The TESS-Keck Survey XXI: 13 New Planets and Homogeneous Properties for 21 Subgiant Systems

Author: Chontos, Ashley, Huber, Daniel, Grunblatt, Samuel K., Saunders, Nicholas, Winn, Joshua N., McCormack, Mason, Knudstrup, Emil, Albrecht, Simon H., Crossfield, Ian J. M., Rodriguez, Joseph E., Ciardi, David R., Collins, Karen A., Jenkins, Jon M., Bieryla, Allyson, Batalha, Natalie M., Beard, Corey, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Howard, Andrew W., Isaacson, Howard, Kane, Stephen R., Lubin, Jack, MacDougall, Mason G., Močnik, Teo, Murphy, Joseph M. Akana, Petigura, Erik A., Pidhorodetska, Daria, Polanski, Alex S., Robertson, Paul, Rubenzahl, Ryan A., Turtelboom, Emma V., Weiss, Lauren M., Van Zandt, Judah, Rocker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Quinn, Samuel N., Shporer, Avi, Eisner, Nora L., Goeke, Robert F., Levine, Alan M., Ting, Eric B., Howell, Steve, Schlieder, Joshua E., Benni, Paul, Boyle, Andrew W., Gan, Tianjun, Girardin, Eric, Gonzalez, Erica, Gregorio, Joao, Horne, Keith, Livingston, John, Lund, Michael B., Mann, Christopher R., Massey, Bob, Matthews, Elisabeth C., McLeod, Kim K., Palle, Enric, Popowicz, Adam, Relles, Howard M., Schwarz, Richard P., Sefako, Ramotholo, Srdoc, Grego, Tan, Thiam-Guan, Wang, Gavin, Ziegler, Carl, Chontos, Ashley, Huber, Daniel, Grunblatt, Samuel K., Saunders, Nicholas, Winn, Joshua N., McCormack, Mason, Knudstrup, Emil, Albrecht, Simon H., Crossfield, Ian J. M., Rodriguez, Joseph E., Ciardi, David R., Collins, Karen A., Jenkins, Jon M., Bieryla, Allyson, Batalha, Natalie M., Beard, Corey, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Howard, Andrew W., Isaacson, Howard, Kane, Stephen R., Lubin, Jack, MacDougall, Mason G., Močnik, Teo, Murphy, Joseph M. Akana, Petigura, Erik A., Pidhorodetska, Daria, Polanski, Alex S., Robertson, Paul, Rubenzahl, Ryan A., Turtelboom, Emma V., Weiss, Lauren M., Van Zandt, Judah, Rocker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Quinn, Samuel N., Shporer, Avi, Eisner, Nora L., Goeke, Robert F., Levine, Alan M., Ting, Eric B., Howell, Steve, Schlieder, Joshua E., Benni, Paul, Boyle, Andrew W., Gan, Tianjun, Girardin, Eric, Gonzalez, Erica, Gregorio, Joao, Horne, Keith, Livingston, John, Lund, Michael B., Mann, Christopher R., Massey, Bob, Matthews, Elisabeth C., McLeod, Kim K., Palle, Enric, Popowicz, Adam, Relles, Howard M., Schwarz, Richard P., Sefako, Ramotholo, Srdoc, Grego, Tan, Thiam-Guan, Wang, Gavin, and Ziegler, Carl
Abstract: We present a dedicated transit and radial velocity survey of planets orbiting subgiant stars observed by the TESS Mission. Using $\sim$$16$ nights on Keck/HIRES, we confirm and characterize $12$ new transiting planets -- $\rm TOI-329\,b$, $\rm HD\,39688\,b$ ($\rm TOI-480$), $\rm TOI-603\,b$, $\rm TOI-1199\,b$, $\rm TOI-1294\,b$, $\rm TOI-1439\,b$, $\rm TOI-1605\,b$, $\rm TOI-1828\,b$, $\rm HD\,148193\,b$ ($\rm TOI-1836$), $\rm TOI-1885\,b$, $\rm HD\,83342\,b$ ($\rm TOI-1898$), $\rm TOI-2019\,b$ -- and provide updated properties for 9 previously confirmed TESS subgiant systems ($\rm TOI-197$, $\rm TOI-954$, $\rm TOI-1181$, $\rm TOI-1296$, $\rm TOI-1298$, $\rm TOI-1601$, $\rm TOI-1736$, $\rm TOI-1842$, $\rm TOI-2145$). We also report the discovery of an outer, non-transiting planet, $\rm TOI-1294\,c$ ($P=160.1\pm2.5$ days, $M_{\mathrm{p}}=148.3^{+18.2}_{-16.4} \,M_{\oplus}$), and three additional stars with long-term RV trends. We find that at least $19\pm8\%$ of subgiants in our sample of $21$ stars have outer companions, comparable to main-sequence stars. We perform a homogeneous analysis of the stars and planets in the sample, with median uncertainties of $3\%$, $8\%$ and $15\%$ for planet radii, masses and ages, doubling the number of known planets orbiting subgiant stars with bulk densities measured to better than $10\%$. We observe a dearth of giant planets around evolved stars with short orbital periods, consistent with tidal dissipation theories that predict the rapid inspiral of planets as their host stars leave the main sequence. We note the possible evidence for two distinct classes of hot Jupiter populations, indicating multiple formation channels to explain the observed distributions around evolved stars. Finally, continued RV monitoring of planets in this sample will provide a more comprehensive understanding of demographics for evolved planetary systems., Comment: 22 pages, 9 figures, 9 tables
Published: 2024

3. The TESS-Keck Survey. XIX. A Warm Transiting Sub-Saturn Mass Planet and a non-Transiting Saturn Mass Planet Orbiting a Solar Analog

Author: Hill, Michelle L., Kane, Stephen R., Dalba, Paul A., MacDougall, Mason, Fetherolf, Tara, Li, Zhexing, Pidhorodetska, Daria, Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Petigura, Erik A, Robertson, Paul, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Giacalone, Steven, Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew W., Mocnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Turtelboom, Emma V., Van Zandt, Judah, Bieryla, Allyson, Ciardi, David R., Eastman, Jason D., Falk, Ben, Hesse, Katharine M., Latham, David W., Livingston, John, Matson, Rachel A., Matthews, Elisabeth, Ricker, George R., Rudat, Alexander, Schlieder, Joshua E., Seager, S., Winn, Joshua N., Hill, Michelle L., Kane, Stephen R., Dalba, Paul A., MacDougall, Mason, Fetherolf, Tara, Li, Zhexing, Pidhorodetska, Daria, Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Petigura, Erik A, Robertson, Paul, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Giacalone, Steven, Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew W., Mocnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Turtelboom, Emma V., Van Zandt, Judah, Bieryla, Allyson, Ciardi, David R., Eastman, Jason D., Falk, Ben, Hesse, Katharine M., Latham, David W., Livingston, John, Matson, Rachel A., Matthews, Elisabeth, Ricker, George R., Rudat, Alexander, Schlieder, Joshua E., Seager, S., and Winn, Joshua N.
Abstract: The Transiting Exoplanet Survey Satellite (TESS) continues to dramatically increase the number of known transiting exoplanets, and is optimal for monitoring bright stars amenable to radial velocity (RV) and atmospheric follow-up observations. TOI-1386 is a solar-type (G5V) star that was detected via TESS photometry to exhibit transit signatures in three sectors with a period of 25.84 days. We conducted follow-up RV observations using Keck/HIRES as part of the TESS-Keck Survey (TKS), collecting 64 RV measurements of TOI-1386 with the HIRES spectrograph over 2.5 years. Our combined fit of the TOI-1386 photometry and RV data confirm the planetary nature of the detected TESS signal, and provide a mass and radius for planet b of $0.148\pm0.019$ $M_J$ and $0.540\pm0.017$ $R_J$, respectively, marking TOI-1386 b as a warm sub-Saturn planet. Our RV data further reveal an additional outer companion, TOI-1386 c, with an estimated orbital period of 227.6 days and a minimum mass of $0.309\pm0.038$ $M_J$. The dynamical modeling of the system shows that the measured system architecture is long-term stable, although there may be substantial eccentricity oscillations of the inner planet due to the dynamical influence of the outer planet., Comment: Accepted for publication in The Astronomical Journal. 15 pages, 7 figures
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. The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc

Author: Clark, Catherine A., van Belle, Gerard T., Horch, Elliott P., Ciardi, David R., von Braun, Kaspar, Skiff, Brian A., Winters, Jennifer G., Lund, Michael B., Everett, Mark E., Hartman, Zachary D., Llama, Joe, Clark, Catherine A., van Belle, Gerard T., Horch, Elliott P., Ciardi, David R., von Braun, Kaspar, Skiff, Brian A., Winters, Jennifer G., Lund, Michael B., Everett, Mark E., Hartman, Zachary D., and Llama, Joe
Abstract: M dwarfs are ubiquitous in our galaxy, and the rate at which they host stellar companions, and the properties of these companions, provides a window into the formation and evolution of the star(s), and of any planets that they may host. The Pervasive Overview of 'Kompanions' of Every M dwarf in Our Neighborhood (POKEMON) speckle survey of nearby M dwarfs is volume-limited from M0V through M9V out to 15 pc, with additional targets at larger distances. In total, 1125 stars were observed, and 455 of these are within the volume-limited, 15-pc sample of M-dwarf primaries. When we combine the speckle observations with known companions from the literature, we find that the stellar multiplicity rate of M dwarfs within 15 pc is 23.5% plus or minus 2.0%, and that the companion rate is 28.8% plus or minus 2.1%. We also find that the projected separation distribution for multiples that are known to host planets peaks at 198 au, while the distribution for multiples that are not yet known to host planets peaks at 5.57 au. This result suggests that the presence of close-in stellar companions inhibits the formation of M-dwarf planetary systems, similar to what has been found for FGK stars., Comment: 18 pages, 5 figures. Accepted for publication in the Astronomical Journal
Published: 2024

6. Migration and Evolution of giant ExoPlanets (MEEP) I: Nine Newly Confirmed Hot Jupiters from the TESS Mission

Author: Schulte, Jack, Rodriguez, Joseph E., Bieryla, Allyson, Quinn, Samuel N., Collins, Karen A., Yee, Samuel W., Nine, Andrew C., Soares-Furtado, Melinda, Latham, David W., Eastman, Jason D., Barkaoui, Khalid, Ciardi, David R., Dragomir, Diana, Everett, Mark E., Giacalone, Steven, Mireles, Ismael, Murgas, Felipe, Narita, Norio, Shporer, Avi, Strakhov, Ivan A., Striegel, Stephanie, Vaňko, Martin, Vowell, Noah, Wang, Gavin, Ziegler, Carl, Bellaver, Michael, Benni, Paul, Bergeron, Serge, Boffin, Henri M. J., Briceño, César, Clark, Catherine A., Collins, Kevin I., de Leon, Jerome P., Dressing, Courtney D., Evans, Phil, Esparza-Borges, Emma, Fedewa, Jeremy, Fukui, Akihiko, Gan, Tianjun, Gerasimov, Ivan S., Hartman, Joel D., Gill, Holden, Gillon, Michaël, Horne, Keith, Horta, Ferran Grau, Howell, Steve B., Isogai, Keisuke, Jehin, Emmanuël, Jenkins, Jon M., Karjalainen, Raine, Kielkopf, John F., Lester, Kathryn V., Littlefield, Colin, Lund, Michael B., Mann, Andrew W., McCormack, Mason, Michaels, Edward J., Painter, Shane, Palle, Enric, Parviainen, Hannu, Peterson, David-Michael, Pozuelos, Francisco J., Raup, Zachary, Reed, Phillip, Relles, Howard M., Ricker, George R., Savel, Arjun B., Schwarz, Richard P., Seager, Sara, Sefako, Ramotholo, Srdoc, Gregor, Stockdale, Chris, Sullivan, Hannah, Timmermans, Mathilde, Winn, Joshua N., Schulte, Jack, Rodriguez, Joseph E., Bieryla, Allyson, Quinn, Samuel N., Collins, Karen A., Yee, Samuel W., Nine, Andrew C., Soares-Furtado, Melinda, Latham, David W., Eastman, Jason D., Barkaoui, Khalid, Ciardi, David R., Dragomir, Diana, Everett, Mark E., Giacalone, Steven, Mireles, Ismael, Murgas, Felipe, Narita, Norio, Shporer, Avi, Strakhov, Ivan A., Striegel, Stephanie, Vaňko, Martin, Vowell, Noah, Wang, Gavin, Ziegler, Carl, Bellaver, Michael, Benni, Paul, Bergeron, Serge, Boffin, Henri M. J., Briceño, César, Clark, Catherine A., Collins, Kevin I., de Leon, Jerome P., Dressing, Courtney D., Evans, Phil, Esparza-Borges, Emma, Fedewa, Jeremy, Fukui, Akihiko, Gan, Tianjun, Gerasimov, Ivan S., Hartman, Joel D., Gill, Holden, Gillon, Michaël, Horne, Keith, Horta, Ferran Grau, Howell, Steve B., Isogai, Keisuke, Jehin, Emmanuël, Jenkins, Jon M., Karjalainen, Raine, Kielkopf, John F., Lester, Kathryn V., Littlefield, Colin, Lund, Michael B., Mann, Andrew W., McCormack, Mason, Michaels, Edward J., Painter, Shane, Palle, Enric, Parviainen, Hannu, Peterson, David-Michael, Pozuelos, Francisco J., Raup, Zachary, Reed, Phillip, Relles, Howard M., Ricker, George R., Savel, Arjun B., Schwarz, Richard P., Seager, Sara, Sefako, Ramotholo, Srdoc, Gregor, Stockdale, Chris, Sullivan, Hannah, Timmermans, Mathilde, and Winn, Joshua N.
Abstract: Hot Jupiters were many of the first exoplanets discovered in the 1990s, but in the decades since their discovery, the mysteries surrounding their origins remain. Here, we present nine new hot Jupiters (TOI-1855 b, TOI-2107 b, TOI-2368 b, TOI-3321 b, TOI-3894 b, TOI-3919 b, TOI-4153 b, TOI-5232 b, and TOI-5301 b) discovered by NASA's TESS mission and confirmed using ground-based imaging and spectroscopy. These discoveries are the first in a series of papers named the Migration and Evolution of giant ExoPlanets (MEEP) survey and are part of an ongoing effort to build a complete sample of hot Jupiters orbiting FGK stars, with a limiting Gaia $G$-band magnitude of 12.5. This effort aims to use homogeneous detection and analysis techniques to generate a set of precisely measured stellar and planetary properties that is ripe for statistical analysis. The nine planets presented in this work occupy a range of masses (0.55 Jupiter masses (M$_{\rm{J}}$) $<$ M$_{\rm{P}}$ $<$ 3.88 M$_{\rm{J}}$) and sizes (0.967 Jupiter radii (R$_{\rm{J}}$) $<$ R$_{\rm{P}}$ $<$ 1.438 R$_{\rm{J}}$) and orbit stars that range in temperature from 5360 K $<$ Teff $<$ 6860 K with Gaia $G$-band magnitudes ranging from 11.1 to 12.7. Two of the planets in our sample have detectable orbital eccentricity: TOI-3919 b ($e = 0.259^{+0.033}_{-0.036}$) and TOI-5301 b ($e = 0.33^{+0.11}_{-0.10}$). These eccentric planets join a growing sample of eccentric hot Jupiters that are consistent with high-eccentricity tidal migration, one of the three most prominent theories explaining hot Jupiter formation and evolution., Comment: 35 pages, 7 tables, and 14 figures. Submitted to AAS Journals on 2023 Dec 28
Published: 2024

7. TESS Hunt for Young and Maturing Exoplanets (THYME) XI: An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400Myr Ursa Major Moving Group

Author: Capistrant, Benjamin K., Soares-Furtado, Melinda, Vanderburg, Andrew, Jankowski, Alyssa, Mann, Andrew W., Ross, Gabrielle, Srdoc, Gregor, Hinkel, Natalie R., Becker, Juliette, Magliano, Christian, Limbach, Mary Anne, Stephan, Alexander P., Nine, Andrew C., Tofflemire, Benjamin M., Kraus, Adam L., Giacalone, Steven, Winn, Joshua N., Bieryla, Allyson, Bouma, Luke G., Ciardi, David R., Collins, Karen A., Covone, Giovanni, de Beurs, Zoë L., Huang, Chelsea X., Quinn, Samuel N., Seager, Sara, Vanderspek, Roland K., Jenkins, Jon M., Kreidberg, Laura, Latham, David W., Shporer, Avi, Twicken, Joseph D., Wohler, Bill, Yarza, Ricardo, Ziegler, Carl, Capistrant, Benjamin K., Soares-Furtado, Melinda, Vanderburg, Andrew, Jankowski, Alyssa, Mann, Andrew W., Ross, Gabrielle, Srdoc, Gregor, Hinkel, Natalie R., Becker, Juliette, Magliano, Christian, Limbach, Mary Anne, Stephan, Alexander P., Nine, Andrew C., Tofflemire, Benjamin M., Kraus, Adam L., Giacalone, Steven, Winn, Joshua N., Bieryla, Allyson, Bouma, Luke G., Ciardi, David R., Collins, Karen A., Covone, Giovanni, de Beurs, Zoë L., Huang, Chelsea X., Quinn, Samuel N., Seager, Sara, Vanderspek, Roland K., Jenkins, Jon M., Kreidberg, Laura, Latham, David W., Shporer, Avi, Twicken, Joseph D., Wohler, Bill, Yarza, Ricardo, and Ziegler, Carl
Abstract: Young terrestrial worlds are critical test beds to constrain prevailing theories of planetary formation and evolution. We present the discovery of HD 63433d - a nearby (22pc), Earth-sized planet transiting a young sunlike star (TOI-1726, HD 63433). HD 63433d is the third planet detected in this multiplanet system. The kinematic, rotational, and abundance properties of the host star indicate that it belongs to the young (414 $\pm$ 23 Myr) Ursa Major moving group, whose membership we update using new data from Gaia DR3 and TESS. Our transit analysis of the TESS light curves indicates that HD 63433 d has a radius of 1.1 $R_\oplus$ and closely orbits its host star with a period of 4.2 days. To date, HD 63433 d is the smallest confirmed exoplanet with an age less than 500 Myr, and the nearest young Earth-sized planet. Furthermore, the apparent brightness of the stellar host (V $\approx$ 6.9 mag) makes this transiting multiplanet system favorable to further investigations, including spectroscopic follow-up to probe atmospheric loss in a young Earth-sized world., Comment: 24 pages, 7 figures, 6 tables. Accepted for publication in AJ. The first two authors contributed equally to the manuscript
Published: 2024

8. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST

Author: Hord, Benjamin J., Kempton, Eliza M.-r., Evans-soma, Thomas M., Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, De Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, De Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-acosta, Sergio B., Fiołka, Jerzy, Forés-toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Grau Horta, Ferran, Gregorio, Joao, Greklek-mckeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Helm, Ian, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppi, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, Mcleod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Natarajan, Krupa, Dyregaard Nielsen, Louise, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Plavchan, Peter, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, Jp, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, Zucker, Shay, Hord, Benjamin J., Kempton, Eliza M.-r., Evans-soma, Thomas M., Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, De Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, De Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-acosta, Sergio B., Fiołka, Jerzy, Forés-toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Grau Horta, Ferran, Gregorio, Joao, Greklek-mckeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Helm, Ian, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppi, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, Mcleod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Natarajan, Krupa, Dyregaard Nielsen, Louise, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Plavchan, Peter, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, Jp, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, and Zucker, Shay
Published: 2024

9. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST

Author: Hord, Benjamin J., Kempton, Eliza M.-r., Evans-soma, Thomas M., Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, De Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, De Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-acosta, Sergio B., Fiołka, Jerzy, Forés-toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Grau Horta, Ferran, Gregorio, Joao, Greklek-mckeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Helm, Ian, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppi, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, Mcleod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Natarajan, Krupa, Dyregaard Nielsen, Louise, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Plavchan, Peter, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, Jp, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, Zucker, Shay, Hord, Benjamin J., Kempton, Eliza M.-r., Evans-soma, Thomas M., Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, De Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, De Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-acosta, Sergio B., Fiołka, Jerzy, Forés-toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Grau Horta, Ferran, Gregorio, Joao, Greklek-mckeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Helm, Ian, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppi, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, Mcleod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Natarajan, Krupa, Dyregaard Nielsen, Louise, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Plavchan, Peter, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, Jp, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, and Zucker, Shay
Published: 2024

10. Characterization of a Set of Small Planets with TESS and CHEOPS and an Analysis of Photometric Performance

Author: Oddo, Dominic, Dragomir, Diana, Brandeker, Alexis, Osborn, Hugh P., Collins, Karen, Stassun, Keivan G., Astudillo-Defru, Nicola, Bieryla, Allyson, Howell, Steve B., Ciardi, David R., Quinn, Samuel, Almenara, Jose M., Briceño, César, Collins, Kevin I., Colón, Knicole D., Conti, Dennis M., Crouzet, Nicolas, Furlan, Elise, Gan, Tianjun, Gnilka, Crystal L., Goeke, Robert F., Gonzales, Erica, Harris, Mallory, Jenkins, Jon M., Jensen, Eric L. N., Latham, David, Law, Nicholas, Lund, Michael B., Mann, Andrew W., Massey, Bob, Murgas, Felipe, Ricker, George, Relles, Howard M., Rowden, Pamela, Schwarz, Richard P., Schlieder, Joshua, Shporer, Avi, Seager, Sara, Srdoc, Gregor, Torres, Guillermo, Twicken, Joseph D., Vanderspek, Roland, Winn, Joshua N., Ziegler, Carl, Oddo, Dominic, Dragomir, Diana, Brandeker, Alexis, Osborn, Hugh P., Collins, Karen, Stassun, Keivan G., Astudillo-Defru, Nicola, Bieryla, Allyson, Howell, Steve B., Ciardi, David R., Quinn, Samuel, Almenara, Jose M., Briceño, César, Collins, Kevin I., Colón, Knicole D., Conti, Dennis M., Crouzet, Nicolas, Furlan, Elise, Gan, Tianjun, Gnilka, Crystal L., Goeke, Robert F., Gonzales, Erica, Harris, Mallory, Jenkins, Jon M., Jensen, Eric L. N., Latham, David, Law, Nicholas, Lund, Michael B., Mann, Andrew W., Massey, Bob, Murgas, Felipe, Ricker, George, Relles, Howard M., Rowden, Pamela, Schwarz, Richard P., Schlieder, Joshua, Shporer, Avi, Seager, Sara, Srdoc, Gregor, Torres, Guillermo, Twicken, Joseph D., Vanderspek, Roland, Winn, Joshua N., and Ziegler, Carl
Abstract: The radius valley carries implications for how the atmospheres of small planets form and evolve, but this feature is visible only with highly precise characterizations of many small planets. We present the characterization of nine planets and one planet candidate with both NASA TESS and ESA CHEOPS observations, which adds to the overall population of planets bordering the radius valley. While five of our planets—TOI 118 b, TOI 262 b, TOI 455 b, TOI 560 b, and TOI 562 b—have already been published, we vet and validate transit signals as planetary using follow-up observations for four new TESS planets, including TOI 198 b, TOI 244 b, TOI 444 b, and TOI 470 b. While a three times increase in primary mirror size should mean that one CHEOPS transit yields an equivalent model uncertainty in transit depth as about nine TESS transits in the case that the star is equally as bright in both bands, we find that our CHEOPS transits typically yield uncertainties equivalent to between two and 12 TESS transits, averaging 5.9 equivalent transits. Therefore, we find that while our fits to CHEOPS transits provide overall lower uncertainties on transit depth and better precision relative to fits to TESS transits, our uncertainties for these fits do not always match expected predictions given photon-limited noise. We find no correlations between number of equivalent transits and any physical parameters, indicating that this behavior is not strictly systematic, but rather might be due to other factors such as in-transit gaps during CHEOPS visits or nonhomogeneous detrending of CHEOPS light curves.
Published: 2023
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11. The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems

Author: Murphy, Joseph M Akana, Murphy, Joseph M Akana, Batalha, Natalie M, Scarsdale, Nicholas, Isaacson, Howard, Ciardi, David R, Gonzales, Erica J, Giacalone, Steven, Twicken, Joseph D, Dattilo, Anne, Fetherolf, Tara, Rubenzahl, Ryan A, Crossfield, Ian JM, Dressing, Courtney D, Fulton, Benjamin, Howard, Andrew W, Huber, Daniel, Kane, Stephen R, Petigura, Erik A, Robertson, Paul, Roy, Arpita, Weiss, Lauren M, Beard, Corey, Chontos, Ashley, Dai, Fei, Rice, Malena, Van Zandt, Judah, Lubin, Jack, Blunt, Sarah, Polanski, Alex S, Behmard, Aida, Dalba, Paul A, Hill, Michelle L, Rosenthal, Lee J, Brinkman, Casey L, Mayo, Andrew W, Turtelboom, Emma V, Angelo, Isabel, Močnik, Teo, MacDougall, Mason G, Pidhorodetska, Daria, Tyler, Dakotah, Kosiarek, Molly R, Holcomb, Rae, Louden, Emma M, Hirsch, Lea A, Gilbert, Emily A, Anderson, Jay, Valenti, Jeff A, Murphy, Joseph M Akana, Murphy, Joseph M Akana, Batalha, Natalie M, Scarsdale, Nicholas, Isaacson, Howard, Ciardi, David R, Gonzales, Erica J, Giacalone, Steven, Twicken, Joseph D, Dattilo, Anne, Fetherolf, Tara, Rubenzahl, Ryan A, Crossfield, Ian JM, Dressing, Courtney D, Fulton, Benjamin, Howard, Andrew W, Huber, Daniel, Kane, Stephen R, Petigura, Erik A, Robertson, Paul, Roy, Arpita, Weiss, Lauren M, Beard, Corey, Chontos, Ashley, Dai, Fei, Rice, Malena, Van Zandt, Judah, Lubin, Jack, Blunt, Sarah, Polanski, Alex S, Behmard, Aida, Dalba, Paul A, Hill, Michelle L, Rosenthal, Lee J, Brinkman, Casey L, Mayo, Andrew W, Turtelboom, Emma V, Angelo, Isabel, Močnik, Teo, MacDougall, Mason G, Pidhorodetska, Daria, Tyler, Dakotah, Kosiarek, Molly R, Holcomb, Rae, Louden, Emma M, Hirsch, Lea A, Gilbert, Emily A, Anderson, Jay, and Valenti, Jeff A
Abstract: With JWST’s successful deployment and unexpectedly high fuel reserves, measuring the masses of sub-Neptunes transiting bright, nearby stars will soon become the bottleneck for characterizing the atmospheres of small exoplanets via transmission spectroscopy. Using a carefully curated target list and observations from more than 2 yr of APF-Levy and Keck-HIRES Doppler monitoring, the TESS-Keck Survey is working toward alleviating this pressure. Here we present mass measurements for 11 transiting planets in eight systems that are particularly suited to atmospheric follow-up with JWST. We also report the discovery and confirmation of a temperate super-Jovian-mass planet on a moderately eccentric orbit. The sample of eight host stars, which includes one subgiant, spans early-K to late-F spectral types (T eff = 5200-6200 K). We homogeneously derive planet parameters using a joint photometry and radial velocity modeling framework, discuss the planets’ possible bulk compositions, and comment on their prospects for atmospheric characterization.
Published: 2023

12. A systematic validation of hot Neptunes in TESS data

Author: Magliano, Christian, Covone, Giovanni, Dobal, Richa, Cacciapuoti, Luca, Tonietti, Luca, Giacalone, Steven, Vines, Jose, Inno, Laura, Jenkins, James S., Lissauer, Jack J., Bieryla, Allyson, Oliva, Fabrizio, Pagano, Isabella, Kostov, Veselin, Ziegler, Carl, Ciardi, David R., Gonzales, Erica J., Dressing, Courtney D., Buchhave, Lars A., Howell, Steve B., Matson, Rachel A., Matthews, Elisabeth, Rotundi, Alessandra, Alves, Douglas, Fiscale, Stefano, Ienco, Riccardo M., Pena, Pablo, Gallo, Francesco, Tomajoli, Maria T. Muscari, Magliano, Christian, Covone, Giovanni, Dobal, Richa, Cacciapuoti, Luca, Tonietti, Luca, Giacalone, Steven, Vines, Jose, Inno, Laura, Jenkins, James S., Lissauer, Jack J., Bieryla, Allyson, Oliva, Fabrizio, Pagano, Isabella, Kostov, Veselin, Ziegler, Carl, Ciardi, David R., Gonzales, Erica J., Dressing, Courtney D., Buchhave, Lars A., Howell, Steve B., Matson, Rachel A., Matthews, Elisabeth, Rotundi, Alessandra, Alves, Douglas, Fiscale, Stefano, Ienco, Riccardo M., Pena, Pablo, Gallo, Francesco, and Tomajoli, Maria T. Muscari
Abstract: We statistically validated a sample of hot Neptune candidates applying a two-step vetting technique using dave and triceratops. We performed a systematic validation of 250 transit-like events in the Transiting Exoplanet Survey Satellite archive in the parameter region defined by P≤4d and 3R⊕≤R≤5R⊕⁠. Through our analysis, we identified 18 hot Neptune-sized candidates, with a false positive probability
Published: 2023

13. TOI-1695 b:A Water World Orbiting an Early-M Dwarf in the Planet Radius Valley

Author: Cherubim, Collin, Cloutier, Ryan, Charbonneau, David, Stockdale, Chris, Stassun, Keivan G., Schwarz, Richard P., Safonov, Boris, Mortier, Annelies, Lewin, Pablo, Latham, David W., Horne, Keith, Haywood, Raphaëlle D., Gonzales, Erica, Goliguzova, Maria V., Collins, Karen A., Ciardi, David R., Bieryla, Allyson, Belinski, Alexandre A., Wohler, Bill, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Sozzetti, Alessandro, Ségransan, Damien, Sasselov, Dimitar, Ricker, George R., Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Pepe, Francesco, Molinari, Emilio, Micela, Giuseppina, Mayor, Michel, Lovis, Christophe, López-Morales, Mercedes, Jenkins, Jon M., Essack, Zahra, Dumusque, Xavier, Doty, John P., Colón, Knicole D., Cameron, Andrew Collier, Buchhave, Lars A., Cherubim, Collin, Cloutier, Ryan, Charbonneau, David, Stockdale, Chris, Stassun, Keivan G., Schwarz, Richard P., Safonov, Boris, Mortier, Annelies, Lewin, Pablo, Latham, David W., Horne, Keith, Haywood, Raphaëlle D., Gonzales, Erica, Goliguzova, Maria V., Collins, Karen A., Ciardi, David R., Bieryla, Allyson, Belinski, Alexandre A., Wohler, Bill, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Sozzetti, Alessandro, Ségransan, Damien, Sasselov, Dimitar, Ricker, George R., Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Pepe, Francesco, Molinari, Emilio, Micela, Giuseppina, Mayor, Michel, Lovis, Christophe, López-Morales, Mercedes, Jenkins, Jon M., Essack, Zahra, Dumusque, Xavier, Doty, John P., Colón, Knicole D., Cameron, Andrew Collier, and Buchhave, Lars A.
Abstract: Characterizing the bulk compositions of transiting exoplanets within the M dwarf radius valley offers a unique means to establish whether the radius valley emerges from an atmospheric mass-loss process or is imprinted by planet formation itself. We present the confirmation of such a planet orbiting an early-M dwarf (T mag = 11.0294 ± 0.0074, M s = 0.513 ± 0.012 M ⊙, R s = 0.515 ± 0.015 R ⊙, and T eff = 3690 ± 50 K): TOI-1695 b (P = 3.13 days and R p = 1.90 − 0.14 + 0.16 R ⊕ ). TOI-1695 b’s radius and orbital period situate the planet between model predictions from thermally driven mass loss versus gas depleted formation, offering an important test case for radius valley emergence models around early-M dwarfs. We confirm the planetary nature of TOI-1695 b based on five sectors of TESS data and a suite of follow-up observations including 49 precise radial velocity measurements taken with the HARPS-N spectrograph. We measure a planetary mass of 6.36 ± 1.00 M ⊕, which reveals that TOI-1695 b is inconsistent with a purely terrestrial composition of iron and magnesium silicate, and instead is likely a water-rich planet. Our finding that TOI-1695 b is not terrestrial is inconsistent with the planetary system being sculpted by thermally driven mass loss. We present a statistical analysis of seven well-characterized planets within the M dwarf radius valley demonstrating that a thermally driven mass-loss scenario is unlikely to explain this population.
Published: 2023

14. TOI-5126: A hot super-Neptune and warm Neptune pair discovered by $\textit{TESS}$ and $\textit{CHEOPS}$

Author: Fairnington, Tyler R., Nabbie, Emma, Huang, Chelsea X., Zhou, George, Foo, Orion, Millholland, Sarah, Wright, Duncan, Belinski, Alexandre A., Bieryla, Allyson, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Everett, Mark, Howell, Steve B., Lissauer, Jack J., Lund, Michael B., Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Relles, Howard M., Safonov, Boris S., Schwarz, Richard P., Scott, Nicholas J., Srdoc, Gregor, Ricker, George, Vanderspek, Roland, Seager, Sara, Latham, David W., Winn, Joshua W., Jenkins, Jon M., Bouma, Luke G., Shporer, Avi, Ting, Eric B., Dragomir, Diana, Kunimoto, Michelle, Eisner, Nora L., Fairnington, Tyler R., Nabbie, Emma, Huang, Chelsea X., Zhou, George, Foo, Orion, Millholland, Sarah, Wright, Duncan, Belinski, Alexandre A., Bieryla, Allyson, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Everett, Mark, Howell, Steve B., Lissauer, Jack J., Lund, Michael B., Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Relles, Howard M., Safonov, Boris S., Schwarz, Richard P., Scott, Nicholas J., Srdoc, Gregor, Ricker, George, Vanderspek, Roland, Seager, Sara, Latham, David W., Winn, Joshua W., Jenkins, Jon M., Bouma, Luke G., Shporer, Avi, Ting, Eric B., Dragomir, Diana, Kunimoto, Michelle, and Eisner, Nora L.
Abstract: We present the confirmation of a hot super-Neptune with an exterior Neptune companion orbiting a bright (V = 10.1 mag) F-dwarf identified by the $\textit{Transiting Exoplanet Survey Satellite}$ ($\textit{TESS}$). The two planets, observed in sectors 45, 46 and 48 of the $\textit{TESS}$ extended mission, are $4.74^{+0.16}_{-0.14}$ $R_{\oplus}$ and $3.86^{+0.17}_{-0.16}$ $R_{\oplus}$ with $5.4588385^{+0.0000070}_{-0.0000072}$ d and $17.8999^{+0.0018}_{-0.0013}$ d orbital periods, respectively. We also obtained precise space based photometric follow-up of the system with ESAs $\textit{CHaracterising ExOplanets Satellite}$ ($\textit{CHEOPS}$) to constrain the radius and ephemeris of TOI-5126 b. TOI 5126 b is located in the "hot Neptune Desert" and is an ideal candidate for follow-up transmission spectroscopy due to its high predicted equilibrium temperature ($T_{eq} = 1442^{+46}_{-40}$ K) implying a cloud-free atmosphere. TOI-5126 c is a warm Neptune ($T_{eq}= 971^{+31}_{-27}$ K) also suitable for follow-up. Tentative transit timing variations (TTVs) have also been identified in analysis, suggesting the presence of at least one additional planet, however this signal may be caused by spot-crossing events, necessitating further precise photometric follow-up to confirm these signals., Comment: Accepted in MNRAS, 18 pages, 14 figures
Published: 2023

15. TESS Spots a Super-Puff: The Remarkably Low Density of TOI-1420b

Author: Yoshida, Stephanie, Vissapragada, Shreyas, Latham, David W., Bieryla, Allyson, Thorngren, Daniel P., Eastman, Jason D., López-Morales, Mercedes, Barkaoui, Khalid, Beichmam, Charles, Berlind, Perry, Buchave, Lars A., Calkins, Michael L., Ciardi, David R., Collins, Karen A., Cosentino, Rosario, Crossfield, Ian J. M., Dai, Fei, DiTomasso, Victoria, Dowling, Nicholas, Esquerdo, Gilbert A., Forés-Toribio, Raquel, Ghedina, Adriano, Goliguzova, Maria V., Golub, Eli, Gonzales, Erica J., Horta, Ferran Grau, Higuera, Jesus, Hoch, Nora, Horne, Keith, Howell, Steve B., Jenkins, Jon M., Klusmeyer, Jessica, Laloum, Didier, Lissauer, Jack J., Logsdon, Sarah E., Malavolta, Luca, Matson, Rachel A., Matthews, Elisabeth C., McLeod, Kim K., Medina, Jennifer V., Muñoz, Jose A., Osborn, Hugh P., Safonov, Boris, Schlieder, Joshua, Schmidt, Michael, Schweiker, Heidi, Seager, Sara, Sozzetti, Alessandro, Srdoc, Gregor, Stefánsson, Guđmundur, Strakhov, Ivan A., Striegel, Stephanie, Villaseñor, Joel, Winn, Joshua N., Yoshida, Stephanie, Vissapragada, Shreyas, Latham, David W., Bieryla, Allyson, Thorngren, Daniel P., Eastman, Jason D., López-Morales, Mercedes, Barkaoui, Khalid, Beichmam, Charles, Berlind, Perry, Buchave, Lars A., Calkins, Michael L., Ciardi, David R., Collins, Karen A., Cosentino, Rosario, Crossfield, Ian J. M., Dai, Fei, DiTomasso, Victoria, Dowling, Nicholas, Esquerdo, Gilbert A., Forés-Toribio, Raquel, Ghedina, Adriano, Goliguzova, Maria V., Golub, Eli, Gonzales, Erica J., Horta, Ferran Grau, Higuera, Jesus, Hoch, Nora, Horne, Keith, Howell, Steve B., Jenkins, Jon M., Klusmeyer, Jessica, Laloum, Didier, Lissauer, Jack J., Logsdon, Sarah E., Malavolta, Luca, Matson, Rachel A., Matthews, Elisabeth C., McLeod, Kim K., Medina, Jennifer V., Muñoz, Jose A., Osborn, Hugh P., Safonov, Boris, Schlieder, Joshua, Schmidt, Michael, Schweiker, Heidi, Seager, Sara, Sozzetti, Alessandro, Srdoc, Gregor, Stefánsson, Guđmundur, Strakhov, Ivan A., Striegel, Stephanie, Villaseñor, Joel, and Winn, Joshua N.
Abstract: We present the discovery of TOI-1420b, an exceptionally low-density ($\rho = 0.08\pm0.02$ g cm$^{-3}$) transiting planet in a $P = 6.96$ day orbit around a late G dwarf star. Using transit observations from TESS, LCOGT, OPM, Whitin, Wendelstein, OAUV, Ca l'Ou, and KeplerCam along with radial velocity observations from HARPS-N and NEID, we find that the planet has a radius of $R_p$ = 11.9 $\pm$ 0.3 $R_\Earth$ and a mass of $M_p$ = 25.1 $\pm$ 3.8 $M_\Earth$. TOI-1420b is the largest-known planet with a mass less than $50M_\Earth$, indicating that it contains a sizeable envelope of hydrogen and helium. We determine TOI-1420b's envelope mass fraction to be $f_{env} = 82^{+7}_{-6}\%$, suggesting that runaway gas accretion occurred when its core was at most $4-5\times$ the mass of the Earth. TOI-1420b is similar to the planet WASP-107b in mass, radius, density, and orbital period, so a comparison of these two systems may help reveal the origins of close-in low-density planets. With an atmospheric scale height of 1950 km, a transmission spectroscopy metric of 580, and a predicted Rossiter-McLaughlin amplitude of about $17$ m s$^{-1}$, TOI-1420b is an excellent target for future atmospheric and dynamical characterization.
Published: 2023

16. TOI-4600 b and c: Two long-period giant planets orbiting an early K dwarf

Author: Mireles, Ismael, Dragomir, Diana, Osborn, Hugh P., Hesse, Katharine, Collins, Karen A., Villanueva, Steven, Bieryla, Allyson, Ciardi, David R., Stassun, Keivan G., Harris, Mallory, Lissauer, Jack J., Schwarz, Richard P., Srdoc, Gregor, Barkaoui, Khalid, Riffeser, Arno, McLeod, Kim K., Pepper, Joshua, Grieves, Nolan, Passegger, Vera Maria, Ulmer-Moll, Solène, Rodriguez, Joseph E., Feliz, Dax L., Quinn, Samuel, Boyle, Andrew W., Fausnaugh, Michael, Kunimoto, Michelle, Rowden, Pamela, Vanderburg, Andrew, Wohler, Bill, Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Winn, Joshua N., Mireles, Ismael, Dragomir, Diana, Osborn, Hugh P., Hesse, Katharine, Collins, Karen A., Villanueva, Steven, Bieryla, Allyson, Ciardi, David R., Stassun, Keivan G., Harris, Mallory, Lissauer, Jack J., Schwarz, Richard P., Srdoc, Gregor, Barkaoui, Khalid, Riffeser, Arno, McLeod, Kim K., Pepper, Joshua, Grieves, Nolan, Passegger, Vera Maria, Ulmer-Moll, Solène, Rodriguez, Joseph E., Feliz, Dax L., Quinn, Samuel, Boyle, Andrew W., Fausnaugh, Michael, Kunimoto, Michelle, Rowden, Pamela, Vanderburg, Andrew, Wohler, Bill, Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, and Winn, Joshua N.
Abstract: We report the discovery and validation of two long-period giant exoplanets orbiting the early K dwarf TOI-4600 (V=12.6, T=11.9), first detected using observations from the Transiting Exoplanet Survey Satellite (TESS) by the TESS Single Transit Planet Candidate Working Group (TSTPC-WG). The inner planet, TOI-4600 b, has a radius of 6.80$\pm$0.31 R$_{\oplus}$ and an orbital period of 82.69 d. The outer planet, TOI-4600 c, has a radius of 9.42$\pm$0.42 R$_{\oplus}$ and an orbital period of 482.82 d, making it the longest-period confirmed or validated planet discovered by TESS to date. We combine TESS photometry and ground-based spectroscopy, photometry, and high-resolution imaging to validate the two planets. With equilibrium temperatures of 347 K and 191 K, respectively, TOI-4600 b and c add to the small but growing population of temperate giant exoplanets that bridge the gap between hot/warm Jupiters and the solar system's gas giants. TOI-4600 is a promising target for further transit and precise RV observations to measure masses and orbits for the planets as well as search for additional non-transiting planets. Additionally, with Transit Spectroscopy Metric (TSM) values of $\sim$30, both planets are amenable for atmospheric characterization with JWST. Altogether will lend insight into the formation and evolution of planet systems with multiple giant exoplanets., Comment: Accepted for publication in ApJL
Published: 2023

17. TOI-332 b: a super dense Neptune found deep within the Neptunian desert

Author: Osborn, Ares, Armstrong, David J., Fernández, Jorge Fernández, Knierim, Henrik, Adibekyan, Vardan, Collins, Karen A., Delgado-Mena, Elisa, Fridlund, Malcolm, da Silva, João Gomes, Hellier, Coel, Jackson, David G., King, George W., Lillo-Box, Jorge, Matson, Rachel A., Matthews, Elisabeth C., Santos, Nuno C., Sousa, Sérgio G., Stassun, Keivan G., Tan, Thiam-Guan, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Bayliss, Daniel, Bouma, Luke G., Ciardi, David R., Collins, Kevin I., Colón, Knicole D., Crossfield, Ian J. M., Demangeon, Olivier D. S., Díaz, Rodrigo F., Dorn, Caroline, Dumusque, Xavier, Keniger, Marcelo Aron Fetzner, Figueira, Pedro, Gan, Tianjun, Goeke, Robert F., Hadjigeorghiou, Andreas, Hawthorn, Faith, Helled, Ravit, Howell, Steve B., Nielsen, Louise D., Osborn, Hugh P., Quinn, Samuel N., Sefako, Ramotholo, Shporer, Avi, Strøm, Paul A., Twicken, Joseph D., Vanderburg, Andrew, Wheatley, Peter J., Osborn, Ares, Armstrong, David J., Fernández, Jorge Fernández, Knierim, Henrik, Adibekyan, Vardan, Collins, Karen A., Delgado-Mena, Elisa, Fridlund, Malcolm, da Silva, João Gomes, Hellier, Coel, Jackson, David G., King, George W., Lillo-Box, Jorge, Matson, Rachel A., Matthews, Elisabeth C., Santos, Nuno C., Sousa, Sérgio G., Stassun, Keivan G., Tan, Thiam-Guan, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Bayliss, Daniel, Bouma, Luke G., Ciardi, David R., Collins, Kevin I., Colón, Knicole D., Crossfield, Ian J. M., Demangeon, Olivier D. S., Díaz, Rodrigo F., Dorn, Caroline, Dumusque, Xavier, Keniger, Marcelo Aron Fetzner, Figueira, Pedro, Gan, Tianjun, Goeke, Robert F., Hadjigeorghiou, Andreas, Hawthorn, Faith, Helled, Ravit, Howell, Steve B., Nielsen, Louise D., Osborn, Hugh P., Quinn, Samuel N., Sefako, Ramotholo, Shporer, Avi, Strøm, Paul A., Twicken, Joseph D., Vanderburg, Andrew, and Wheatley, Peter J.
Abstract: To date, thousands of planets have been discovered, but there are regions of the orbital parameter space that are still bare. An example is the short period and intermediate mass/radius space known as the Neptunian desert, where planets should be easy to find but discoveries remain few. This suggests unusual formation and evolution processes are responsible for the planets residing here. We present the discovery of TOI-332 b, a planet with an ultra-short period of $0.78$ d that sits firmly within the desert. It orbits a K0 dwarf with an effective temperature of $5251 \pm 71$ K. TOI-332 b has a radius of $3.20^{+0.16}_{-0.12}$ R$_{\oplus}$, smaller than that of Neptune, but an unusually large mass of $57.2 \pm 1.6$ M$_{\oplus}$. It has one of the highest densities of any Neptune-sized planet discovered thus far at $9.6^{+1.1}_{-1.3}$ gcm$^{-3}$. A 4-layer internal structure model indicates it likely has a negligible hydrogen-helium envelope, something only found for a small handful of planets this massive, and so TOI-332 b presents an interesting challenge to planetary formation theories. We find that photoevaporation cannot account for the mass loss required to strip this planet of the Jupiter-like envelope it would have been expected to accrete. We need to look towards other scenarios, such as high-eccentricity migration, giant impacts, or gap opening in the protoplanetary disc, to try and explain this unusual discovery., Comment: 20 pages, 14 figures, 6 tables, accepted for publication in MNRAS
Published: 2023

18. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST

Author: Hord, Benjamin J., Kempton, Eliza M. -R., Mikal-Evans, Thomas, Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, de Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-Cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, de Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-Acosta, Sergio B., Fiołka, Jerzy, Forés-Toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Horta, Ferran Grau, Gregorio, Joao, Greklek-McKeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isaacson, Howard, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppe, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, McLeod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Nielsen, Louise Dyregaard, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-Guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, JP, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, Zucker, Shay, Hord, Benjamin J., Kempton, Eliza M. -R., Mikal-Evans, Thomas, Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, de Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-Cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, de Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-Acosta, Sergio B., Fiołka, Jerzy, Forés-Toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Horta, Ferran Grau, Gregorio, Joao, Greklek-McKeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isaacson, Howard, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppe, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, McLeod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Nielsen, Louise Dyregaard, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-Guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, JP, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, and Zucker, Shay
Abstract: JWST has ushered in an era of unprecedented ability to characterize exoplanetary atmospheres. While there are over 5,000 confirmed planets, more than 4,000 TESS planet candidates are still unconfirmed and many of the best planets for atmospheric characterization may remain to be identified. We present a sample of TESS planets and planet candidates that we identify as "best-in-class" for transmission and emission spectroscopy with JWST. These targets are sorted into bins across equilibrium temperature $T_{\mathrm{eq}}$ and planetary radius $R{_\mathrm{p}}$ and are ranked by transmission and emission spectroscopy metric (TSM and ESM, respectively) within each bin. In forming our target sample, we perform cuts for expected signal size and stellar brightness, to remove sub-optimal targets for JWST. Of the 194 targets in the resulting sample, 103 are unconfirmed TESS planet candidates, also known as TESS Objects of Interest (TOIs). We perform vetting and statistical validation analyses on these 103 targets to determine which are likely planets and which are likely false positives, incorporating ground-based follow-up from the TESS Follow-up Observation Program (TFOP) to aid the vetting and validation process. We statistically validate 23 TOIs, marginally validate 33 TOIs to varying levels of confidence, deem 29 TOIs likely false positives, and leave the dispositions for 4 TOIs as inconclusive. 14 of the 103 TOIs were confirmed independently over the course of our analysis. We provide our final best-in-class sample as a community resource for future JWST proposals and observations. We intend for this work to motivate formal confirmation and mass measurements of each validated planet and encourage more detailed analysis of individual targets by the community., Comment: Submitted to AJ. Machine-readable versions of Tables 2 and 3 are included. 40 pages, 7 figures, 3 tables
Published: 2023

19. The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems

Author: Murphy, Joseph M. Akana, Batalha, Natalie M., Scarsdale, Nicholas, Isaacson, Howard, Ciardi, David R., Gonzales, Erica J., Giacalone, Steven, Twicken, Joseph D., Dattilo, Anne, Fetherolf, Tara, Rubenzahl, Ryan A., Crossfield, Ian J. M., Dressing, Courtney D., Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Beard, Corey, Chontos, Ashley, Dai, Fei, Rice, Malena, Van Zandt, Judah, Lubin, Jack, Blunt, Sarah, Polanski, Alex S., Behmard, Aida, Dalba, Paul A., Hill, Michelle L., Rosenthal, Lee J., Brinkman, Casey L., Mayo, Andrew W., Turtelboom, Emma V., Angelo, Isabel, Močnik, Teo, MacDougall, Mason G., Pidhorodetska, Daria, Tyler, Dakotah, Kosiarek, Molly R., Holcomb, Rae, Louden, Emma M., Hirsch, Lea A., Anderson, Jay, Valenti, Jeff A., Murphy, Joseph M. Akana, Batalha, Natalie M., Scarsdale, Nicholas, Isaacson, Howard, Ciardi, David R., Gonzales, Erica J., Giacalone, Steven, Twicken, Joseph D., Dattilo, Anne, Fetherolf, Tara, Rubenzahl, Ryan A., Crossfield, Ian J. M., Dressing, Courtney D., Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Beard, Corey, Chontos, Ashley, Dai, Fei, Rice, Malena, Van Zandt, Judah, Lubin, Jack, Blunt, Sarah, Polanski, Alex S., Behmard, Aida, Dalba, Paul A., Hill, Michelle L., Rosenthal, Lee J., Brinkman, Casey L., Mayo, Andrew W., Turtelboom, Emma V., Angelo, Isabel, Močnik, Teo, MacDougall, Mason G., Pidhorodetska, Daria, Tyler, Dakotah, Kosiarek, Molly R., Holcomb, Rae, Louden, Emma M., Hirsch, Lea A., Anderson, Jay, and Valenti, Jeff A.
Abstract: With JWST's successful deployment and unexpectedly high fuel reserves, measuring the masses of sub-Neptunes transiting bright, nearby stars will soon become the bottleneck for characterizing the atmospheres of small exoplanets via transmission spectroscopy. Using a carefully curated target list and more than two years' worth of APF-Levy and Keck-HIRES Doppler monitoring, the TESS-Keck Survey is working toward alleviating this pressure. Here we present mass measurements for 11 transiting planets in eight systems that are particularly suited to atmospheric follow-up with JWST. We also report the discovery and confirmation of a temperate super-Jovian-mass planet on a moderately eccentric orbit. The sample of eight host stars, which includes one subgiant, spans early-K to late-F spectral types ($T_\mathrm{eff} =$ 5200--6200 K). We homogeneously derive planet parameters using a joint photometry and radial velocity modeling framework, discuss the planets' possible bulk compositions, and comment on their prospects for atmospheric characterization., Comment: Accepted for publication in The Astronomical Journal on 2023-Jun-22. 60 pages, 17 Tables, 28 Figures
Published: 2023

20. 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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21. 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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22. TOI-908: a planet at the edge of the Neptune desert transiting a G-type star

Author: Hawthorn, Faith, Bayliss, Daniel, Armstrong, David J., Fernández, Jorge Fernández, Osborn, Ares, Sousa, Sérgio G., Adibekyan, Vardan, Davoult, Jeanne, Collins, Karen A., Alibert, Yann, Barros, Susana C. C., Bouchy, François, Brogi, Matteo, Ciardi, David R., Daylan, Tansu, Mena, Elisa Delgado, Demangeon, Olivier D. S., Díaz, Rodrigo F., Gan, Tianjun, Horne, Keith, Hoyer, Sergio, Levine, Alan M., Lillo-Box, Jorge, Nielsen, Louise D., Osborn, Hugh P., Ricker, George R., Rodrigues, José, Santos, Nuno C., Schwarz, Richard P., Seager, Sara, Bell, Juan Serrano, Shporer, Avi, Stockdale, Chris, Strøm, Paul A., Tenenbaum, Peter, Udry, Stéphane, Wheatley, Peter J., Winn, Joshua N., Ziegler, Carl, Hawthorn, Faith, Bayliss, Daniel, Armstrong, David J., Fernández, Jorge Fernández, Osborn, Ares, Sousa, Sérgio G., Adibekyan, Vardan, Davoult, Jeanne, Collins, Karen A., Alibert, Yann, Barros, Susana C. C., Bouchy, François, Brogi, Matteo, Ciardi, David R., Daylan, Tansu, Mena, Elisa Delgado, Demangeon, Olivier D. S., Díaz, Rodrigo F., Gan, Tianjun, Horne, Keith, Hoyer, Sergio, Levine, Alan M., Lillo-Box, Jorge, Nielsen, Louise D., Osborn, Hugh P., Ricker, George R., Rodrigues, José, Santos, Nuno C., Schwarz, Richard P., Seager, Sara, Bell, Juan Serrano, Shporer, Avi, Stockdale, Chris, Strøm, Paul A., Tenenbaum, Peter, Udry, Stéphane, Wheatley, Peter J., Winn, Joshua N., and Ziegler, Carl
Abstract: We present the discovery of an exoplanet transiting TOI-908 (TIC-350153977) using data from TESS sectors 1, 12, 13, 27, 28 and 39. TOI-908 is a T = 10.7 mag G-dwarf ($T_{eff}$ = 5626 $\pm$ 61 K) solar-like star with a mass of 0.950 $\pm$ 0.010 $M_{\odot}$ and a radius of 1.028 $\pm$ 0.030 $R_{\odot}$. The planet, TOI-908 b, is a 3.18 $\pm$ 0.16 $R_{\oplus}$ planet in a 3.18 day orbit. Radial velocity measurements from HARPS reveal TOI-908 b has a mass of approximately 16.1 $\pm$ 4.1 $M_{\oplus}$ , resulting in a bulk planetary density of 2.7+0.2-0.4 g cm-3. TOI-908 b lies in a sparsely-populated region of parameter space known as the Neptune desert. The planet likely began its life as a sub-Saturn planet before it experienced significant photoevaporation due to X-rays and extreme ultraviolet radiation from its host star, and is likely to continue evaporating, losing a significant fraction of its residual envelope mass., Comment: 17 pages, 17 figures
Published: 2023
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23. 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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24. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author: Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., and Rose, Mark E.
Abstract: We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation
Published: 2023
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25. Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095

Author: Quintana, Elisa V., Gilbert, Emily A., Barclay, Thomas, Silverstein, Michele L., Schlieder, Joshua E., Cloutier, Ryan, Quinn, Samuel N., Rodriguez, Joseph E., Vanderburg, Andrew, Hord, Benjamin J., Louie, Dana R., Ostberg, Colby, Kane, Stephen R., Hoffman, Kelsey, Rowe, Jason F., Arney, Giada N., Saxena, Prabal, Richardson, Taran, Clement, Matthew S., Kartvedt, Nicholas M., Adams, Fred C., Alfred, Marcus, Berger, Travis, Bieryla, Allyson, Bonney, Paul, Boyd, Patricia, Cadieux, Charles, Caldwell, Douglas, Ciardi, David R., Charbonneau, David, Collins, Karen A., Colon, Knicole D., Conti, Dennis M., Di Sora, Mario, Domagal-Goldman, Shawn, Dotson, Jessie, Fauchez, Thomas, Günther, Maximilian N., Hedges, Christina, Isopi, Giovanni, Kohler, Erika, Kopparapu, Ravi, Kostov, Veselin B., Larsen, Jeffrey A., Lopez, Eric, Mallia, Franco, Mandell, Avi, Mullally, Susan E., Paudel, Rishi R., Powell, Brian P., Ricker, George R., Safonov, Boris S., Schwarz, Richard P., Sefako, Ramotholo, Stassun, Keivan G., Wilson, Robert, Winn, Joshua N., Vanderspek, Roland K., Quintana, Elisa V., Gilbert, Emily A., Barclay, Thomas, Silverstein, Michele L., Schlieder, Joshua E., Cloutier, Ryan, Quinn, Samuel N., Rodriguez, Joseph E., Vanderburg, Andrew, Hord, Benjamin J., Louie, Dana R., Ostberg, Colby, Kane, Stephen R., Hoffman, Kelsey, Rowe, Jason F., Arney, Giada N., Saxena, Prabal, Richardson, Taran, Clement, Matthew S., Kartvedt, Nicholas M., Adams, Fred C., Alfred, Marcus, Berger, Travis, Bieryla, Allyson, Bonney, Paul, Boyd, Patricia, Cadieux, Charles, Caldwell, Douglas, Ciardi, David R., Charbonneau, David, Collins, Karen A., Colon, Knicole D., Conti, Dennis M., Di Sora, Mario, Domagal-Goldman, Shawn, Dotson, Jessie, Fauchez, Thomas, Günther, Maximilian N., Hedges, Christina, Isopi, Giovanni, Kohler, Erika, Kopparapu, Ravi, Kostov, Veselin B., Larsen, Jeffrey A., Lopez, Eric, Mallia, Franco, Mandell, Avi, Mullally, Susan E., Paudel, Rishi R., Powell, Brian P., Ricker, George R., Safonov, Boris S., Schwarz, Richard P., Sefako, Ramotholo, Stassun, Keivan G., Wilson, Robert, Winn, Joshua N., and Vanderspek, Roland K.
Abstract: We report the detection and validation of two planets orbiting TOI-2095 (TIC 235678745). The host star is a 3700K M1V dwarf with a high proper motion. The star lies at a distance of 42 pc in a sparsely populated portion of the sky and is bright in the infrared (K=9). With data from 24 Sectors of observation during TESS's Cycles 2 and 4, TOI-2095 exhibits two sets of transits associated with super-Earth-sized planets. The planets have orbital periods of 17.7 days and 28.2 days and radii of 1.30 and 1.39 Earth radii, respectively. Archival data, preliminary follow-up observations, and vetting analyses support the planetary interpretation of the detected transit signals. The pair of planets have estimated equilibrium temperatures of approximately 400 K, with stellar insolations of 3.23 and 1.73 times that of Earth, placing them in the Venus zone. The planets also lie in a radius regime signaling the transition between rock-dominated and volatile-rich compositions. They are thus prime targets for follow-up mass measurements to better understand the properties of warm, transition radius planets. The relatively long orbital periods of these two planets provide crucial data that can help shed light on the processes that shape the composition of small planets orbiting M dwarfs., Comment: Submitted to AAS Journals
Published: 2023

26. Three long period transiting giant planets from TESS

Author: Brahm, Rafael, Ulmer-Moll, Solène, Hobson, Melissa J., Jordán, Andrés, Henning, Thomas, Trifonov, Trifon, Jones, Matías I., Schlecker, Martin, Espinoza, Nestor, Rojas, Felipe I., Torres, Pascal, Sarkis, Paula, Tala, Marcelo, Eberhardt, Jan, Kossakowski, Diana, Muñoz, Diego J., Hartman, Joel D., Boyle, Gavin, Suc, Vincent, Bouchy, François, Deline, Adrien, Chaverot, Guillaume, Grieves, Nolan, Lendl, Monika, Suarez, Olga, Triaud, Amaury H. M. J., Crouzet, Nicolas, Dransfield, Georgina, Guillot, Tristan, Cloutier, Ryan, Barkaoui, Khalid, Schwarz, Rick P., Stockdale, Chris, Harris, Mallory, Mireles, Ismael, Evans, Phil, Mann, Andrew W., Ziegler, Carl, Dragomir, Diana, Villanueva, Steven, Mordasini, Christoph, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Vezie, Michael, Youngblood, Allison, Daylan, Tansu, Collins, Karen A., Caldwell, Douglas A., Ciardi, David R., Palle, Enric, Murgas, Felipe, Brahm, Rafael, Ulmer-Moll, Solène, Hobson, Melissa J., Jordán, Andrés, Henning, Thomas, Trifonov, Trifon, Jones, Matías I., Schlecker, Martin, Espinoza, Nestor, Rojas, Felipe I., Torres, Pascal, Sarkis, Paula, Tala, Marcelo, Eberhardt, Jan, Kossakowski, Diana, Muñoz, Diego J., Hartman, Joel D., Boyle, Gavin, Suc, Vincent, Bouchy, François, Deline, Adrien, Chaverot, Guillaume, Grieves, Nolan, Lendl, Monika, Suarez, Olga, Triaud, Amaury H. M. J., Crouzet, Nicolas, Dransfield, Georgina, Guillot, Tristan, Cloutier, Ryan, Barkaoui, Khalid, Schwarz, Rick P., Stockdale, Chris, Harris, Mallory, Mireles, Ismael, Evans, Phil, Mann, Andrew W., Ziegler, Carl, Dragomir, Diana, Villanueva, Steven, Mordasini, Christoph, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Vezie, Michael, Youngblood, Allison, Daylan, Tansu, Collins, Karen A., Caldwell, Douglas A., Ciardi, David R., Palle, Enric, and Murgas, Felipe
Abstract: We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single transit events in the light curves generated from the full frame images of the Transiting Exoplanet Survey Satellite (TESS). Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of $M_P$= 0.30 $\pm$ 0.04 $M_J$ , a radius of $R_P$= 1.00 $\pm$ 0.02 $R_J$ , and a low eccentricity orbit (e=0.15 $\pm$ 0.05) with a period of P= 30.08364 $\pm$ 0.00005 d . TOI 2338b has a mass of $M_P$= 5.98 $\pm$ 0.20 $M_J$ , a radius of $R_P$= 1.00 $\pm$ 0.01 $R_J$ , and a highly eccentric orbit (e= 0.676 $\pm$ 0.002 ) with a period of P= 22.65398 $\pm$ 0.00002 d . Finally, TOI 2589b has a mass of $M_P$= 3.50 $\pm$ 0.10 $M_J$ , a radius of $R_P$= 1.08 $\pm$ 0.03 $R_J$ , and an eccentric orbit (e = 0.522 $\pm$ 0.006 ) with a period of P= 61.6277 $\pm$ 0.0002 d . TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star., Comment: 24 pages, 16 figures, accepted in AJ
Published: 2023
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27. Discovery of a massive giant planet with extreme density around a sub-giant star TOI-4603

Author: Khandelwal, Akanksha, Sharma, Rishikesh, Chakraborty, Abhijit, Chaturvedi, Priyanka, Ulmer-Moll, Solène, Ciardi, David R., Boyle, Andrew W., Baliwal, Sanjay, Bieryla, Allyson, Latham, David W., Prasad, Neelam J. S. S. V., Nayak, Ashirbad, Lendl, Monika, Mordasini, Christoph, Khandelwal, Akanksha, Sharma, Rishikesh, Chakraborty, Abhijit, Chaturvedi, Priyanka, Ulmer-Moll, Solène, Ciardi, David R., Boyle, Andrew W., Baliwal, Sanjay, Bieryla, Allyson, Latham, David W., Prasad, Neelam J. S. S. V., Nayak, Ashirbad, Lendl, Monika, and Mordasini, Christoph
Abstract: We present the discovery of a transiting massive giant planet around TOI-4603, a sub-giant F-type star from NASA's Transiting Exoplanet Survey Satellite (TESS). The newly discovered planet has a radius of $1.042^{+0.038}_{-0.035}$ $R_{J}$, and an orbital period of $7.24599^{+0.00022}_{-0.00021}$ days. Using radial velocity measurements with the PARAS {and TRES} spectrographs, we determined the planet's mass to be $12.89^{+0.58}_{-0.57}$ $M_{J}$, resulting in a bulk density of $14.1^{+1.7}_{-1.6}$ g ${cm^{-3}}$. This makes it one of the few massive giant planets with extreme density and lies in the transition mass region of massive giant planets and low-mass brown dwarfs, an important addition to the population of less than five objects in this mass range. The eccentricity of $0.325\pm0.020$ and an orbital separation of $0.0888\pm0.0010$ AU from its host star suggest that the planet is likely undergoing high eccentricity tidal (HET) migration. We find a fraction of heavy elements of $0.13^{+0.05}_{-0.06}$ and metal enrichment of the planet ($Z_{P}/Z_{star}$) of $4.2^{+1.6}_{-2.0}$. Detection of such systems will offer us to gain valuable insights into the governing mechanisms of massive planets and improve our understanding of their dominant formation and migration mechanisms., Comment: accepted for publication in A&A Letters
Published: 2023
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28. JWST Observations of the Enigmatic Y Dwarf WISE 1828+2650: I. Limits to a Binary Companion

Author: De Furio, Matthew, Lew, Ben W., Beichman, Charles A., Roellig, Thomas, Bryden, Geoffrey, Ciardi, David R., Meyer, Michael R., Rieke, Marcia J., Greenbaum, Alexandra Z., Leisenring, Jarron, Llop-Sayson, Jorge, Ygouf, Marie, Albert, Loïc, Boyer, Martha L., Eisenstein, Daniel J., Hodapp, Klaus W., Horner, Scott, Johnstone, Doug, Kelly, Douglas M., Misselt, Karl A., Rieke, George H., Stansberry, John A., Young, Erick T., De Furio, Matthew, Lew, Ben W., Beichman, Charles A., Roellig, Thomas, Bryden, Geoffrey, Ciardi, David R., Meyer, Michael R., Rieke, Marcia J., Greenbaum, Alexandra Z., Leisenring, Jarron, Llop-Sayson, Jorge, Ygouf, Marie, Albert, Loïc, Boyer, Martha L., Eisenstein, Daniel J., Hodapp, Klaus W., Horner, Scott, Johnstone, Doug, Kelly, Douglas M., Misselt, Karl A., Rieke, George H., Stansberry, John A., and Young, Erick T.
Abstract: The Y-dwarf WISE 1828+2650 is one of the coldest known Brown Dwarfs with an effective temperature of $\sim$300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of $\sim$5-10 Mj, making it a valuable laboratory for understanding the formation, evolution and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle with the near-impossibility of simultaneously fitting both the short (0.9-2.0 microns) and long wavelength (3-5 microns) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in 6 filters to address the binarity question and to provide new photometry to be used in model fitting. We also report Adaptive Optics imaging with the Keck 10 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 AU with either JWST or Keck. Companion articles will present low and high resolution spectra of WISE 1828+2650 obtained with both NIRSpec and MIRI., Comment: 15 pages, 9 figures, Accepted by ApJ on Feb. 21 2023
Published: 2023
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29. TOI-2525 b and c: A pair of massive warm giant planets with a strong transit timing variations revealed by TESS

Author: Trifonov, Trifon, Brahm, Rafael, Jordan, Andres, Hartogh, Christian, Henning, Thomas, Hobson, Melissa J., Schlecker, Martin, Howard, Saburo, Reichardt, Finja, Espinoza, Nestor, Lee, Man Hoi, Nesvorny, David, Rojas, Felipe I., Barkaoui, Khalid, Kossakowski, Diana, Boyle, Gavin, Dreizler, Stefan, Kuerster, Martin, Heller, Rene, Guillot, Tristan, Triaud, Amaury H. M. J., Abe, Lyu, Agabi, Abdelkrim, Bendjoya, Philippe, Crouzet, Nicolas, Dransfield, Georgina, Gasparetto, Thomas, Guenther, Maximilian N., Marie-Sainte, Wenceslas, Mekarnia, Djamel, Suarez, Olga, Teske, Johanna, Butler, R. Paul, Crane, Jeffrey D., Shectman, Stephen, Ricker, George R., Shporer, Avi, Vanderspek, Roland, Jenkins, Jon M., Wohler, Bill, Collins, Karen A., Collins, Kevin I., Ciardi, David R., Barclay, Thomas, Mireles, Ismael, Seager, Sara, Winn, Joshua N., Trifonov, Trifon, Brahm, Rafael, Jordan, Andres, Hartogh, Christian, Henning, Thomas, Hobson, Melissa J., Schlecker, Martin, Howard, Saburo, Reichardt, Finja, Espinoza, Nestor, Lee, Man Hoi, Nesvorny, David, Rojas, Felipe I., Barkaoui, Khalid, Kossakowski, Diana, Boyle, Gavin, Dreizler, Stefan, Kuerster, Martin, Heller, Rene, Guillot, Tristan, Triaud, Amaury H. M. J., Abe, Lyu, Agabi, Abdelkrim, Bendjoya, Philippe, Crouzet, Nicolas, Dransfield, Georgina, Gasparetto, Thomas, Guenther, Maximilian N., Marie-Sainte, Wenceslas, Mekarnia, Djamel, Suarez, Olga, Teske, Johanna, Butler, R. Paul, Crane, Jeffrey D., Shectman, Stephen, Ricker, George R., Shporer, Avi, Vanderspek, Roland, Jenkins, Jon M., Wohler, Bill, Collins, Karen A., Collins, Kevin I., Ciardi, David R., Barclay, Thomas, Mireles, Ismael, Seager, Sara, and Winn, Joshua N.
Abstract: TOI-2525 is a K-type star with an estimated mass of M = 0.849$_{-0.033}^{+0.024}$ M$_\odot$ and radius of R = 0.785$_{-0.007}^{+0.007}$ R$_\odot$ observed by the TESS mission in 22 sectors (within sectors 1 and 39). The TESS light curves yield significant transit events of two companions, which show strong transit timing variations (TTVs) with a semi-amplitude of a $\sim$6 hours. We performed TTV dynamical, and photo-dynamical light curve analysis of the TESS data, combined with radial velocity (RV) measurements from FEROS and PFS, and we confirmed the planetary nature of these companions. The TOI-2525 system consists of a transiting pair of planets comparable to Neptune and Jupiter with estimated dynamical masses of $m_{\rm b}$ = 0.088$_{-0.004}^{+0.005}$ M$_{\rm Jup.}$, and $m_{\rm c}$ = 0.709$_{-0.033}^{+0.034}$ M$_{\rm Jup.}$, radius of $r_b$ = 0.88$_{-0.02}^{+0.02}$ R$_{\rm Jup.}$ and $r_c$ = 0.98$_{-0.02}^{+0.02}$ R$_{\rm Jup.}$, and with orbital periods of $P_{\rm b}$ = 23.288$_{-0.002}^{+0.001}$ days and $P_{\rm c}$ = 49.260$_{-0.001}^{+0.001}$ days for the inner and the outer planet, respectively. The period ratio is close to the 2:1 period commensurability, but the dynamical simulations of the system suggest that it is outside the mean motion resonance (MMR) dynamical configuration. TOI-2525 b is among the lowest density Neptune-mass planets known to date, with an estimated median density of $\rho_{\rm b}$ = 0.174$_{-0.015}^{+0.016}$ g\,cm$^{-3}$. The TOI-2525 system is very similar to the other K-dwarf systems discovered by TESS, TOI-2202 and TOI-216, which are composed of almost identical K-dwarf primary and two warm giant planets near the 2:1 MMR., Comment: Accepted for publication in AJ
Published: 2023
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30. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author: Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, Winn, Joshua N., Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, and Winn, Joshua N.
Abstract: NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (vsin(i)=35.1±1.0km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of 2.76+0.24−0.23Mjup, 1.370±0.043Rjup and ∼4.63 days, respectively. The planet orbits a bright (V=9.1mag) F3-dwarf with M=1.40±0.05Msun, R=1.70±0.05Rsun, and logg=4.05±0.17. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of 18∘±11∘, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.
Published: 2023

31. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author: Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, Winn, Joshua N., Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, and Winn, Joshua N.
Abstract: NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (vsin(i)=35.1±1.0km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of 2.76+0.24−0.23Mjup, 1.370±0.043Rjup and ∼4.63 days, respectively. The planet orbits a bright (V=9.1mag) F3-dwarf with M=1.40±0.05Msun, R=1.70±0.05Rsun, and logg=4.05±0.17. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of 18∘±11∘, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.
Published: 2023

32. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author: Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, Winn, Joshua N., Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, and Winn, Joshua N.
Abstract: NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (vsin(i)=35.1±1.0km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of 2.76+0.24−0.23Mjup, 1.370±0.043Rjup and ∼4.63 days, respectively. The planet orbits a bright (V=9.1mag) F3-dwarf with M=1.40±0.05Msun, R=1.70±0.05Rsun, and logg=4.05±0.17. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of 18∘±11∘, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.
Published: 2023

33. Characterization of a set of small planets with TESS and CHEOPS and an analysis of photometric performance

Author: Oddo, Dominic, Dragomir, Diana, Brandeker, Alexis, Osborn, Hugh P., Collins, Karen, Stassun, Keivan, Astudillo-Defru, Nicola, Bieryla, Allyson, Howell, Steve B., Ciardi, David R., Quinn, Samuel, Almenara, Jose M., Briceno, Cesar, Collins, Kevin I., Colon, Knicole D., Conti, Dennis M., Crouzet, Nicolas, Furlan, Elise, Gan, Tianjun, Gnilka, Crystal L., Goeke, Robert F., Gonzales, Erica, Harris, Mallory, Jenkins, Jon M., Jensen, Eric L. N., Latham, David, Law, Nicholas, Lund, Michael B., Mann, Andrew W., Massey, Bob, Murgas, Felipe, Ricker, George, Relles, Howard M., Rowden, Pamela, Schwarz, Richard P., Schlieder, Joshua, Shporer, Avi, Seager, Sara, Srdoc, Gregor, Torres, Guillermo, Twicken, Joseph D., Vanderspek, Roland, Winn, Joshua N., Ziegler, Carl, Oddo, Dominic, Dragomir, Diana, Brandeker, Alexis, Osborn, Hugh P., Collins, Karen, Stassun, Keivan, Astudillo-Defru, Nicola, Bieryla, Allyson, Howell, Steve B., Ciardi, David R., Quinn, Samuel, Almenara, Jose M., Briceno, Cesar, Collins, Kevin I., Colon, Knicole D., Conti, Dennis M., Crouzet, Nicolas, Furlan, Elise, Gan, Tianjun, Gnilka, Crystal L., Goeke, Robert F., Gonzales, Erica, Harris, Mallory, Jenkins, Jon M., Jensen, Eric L. N., Latham, David, Law, Nicholas, Lund, Michael B., Mann, Andrew W., Massey, Bob, Murgas, Felipe, Ricker, George, Relles, Howard M., Rowden, Pamela, Schwarz, Richard P., Schlieder, Joshua, Shporer, Avi, Seager, Sara, Srdoc, Gregor, Torres, Guillermo, Twicken, Joseph D., Vanderspek, Roland, Winn, Joshua N., and Ziegler, Carl
Abstract: The radius valley carries implications for how the atmospheres of small planets form and evolve, but this feature is visible only with highly precise characterizations of many small planets. We present the characterization of nine planets and one planet candidate with both NASA TESS and ESA CHEOPS observations, which adds to the overall population of planets bordering the radius valley. While four of our planets - TOI 118 b, TOI 455 b, TOI 560 b, and TOI 562 b - have already been published, we vet and validate transit signals as planetary using follow-up observations for five new TESS planets, including TOI 198 b, TOI 244 b, TOI 262 b, TOI 444 b, and TOI 470 b. While a three times increase in primary mirror size should mean that one CHEOPS transit yields an equivalent model uncertainty in transit depth as about nine TESS transits in the case that the star is equally as bright in both bands, we find that our CHEOPS transits typically yield uncertainties equivalent to between two and 12 TESS transits, averaging 5.9 equivalent transits. Therefore, we find that while our fits to CHEOPS transits provide overall lower uncertainties on transit depth and better precision relative to fits to TESS transits, our uncertainties for these fits do not always match expected predictions given photon-limited noise. We find no correlations between number of equivalent transits and any physical parameters, indicating that this behavior is not strictly systematic, but rather might be due to other factors such as in-transit gaps during CHEOPS visits or nonhomogeneous detrending of CHEOPS light curves., Comment: Published in AJ; changed to reflect our vetting of TOI 262 b
Published: 2023
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34. TOI-332 b: a super dense Neptune found deep within the Neptunian desert

Author: Osborn, Ares; https://orcid.org/0000-0002-5899-7750, Armstrong, David J; https://orcid.org/0000-0002-5080-4117, Fernández Fernández, Jorge, Knierim, Henrik, Adibekyan, Vardan, Collins, Karen A, Delgado-Mena, Elisa, Fridlund, Malcolm; https://orcid.org/0000-0002-0855-8426, Gomes da Silva, João, Hellier, Coel, Jackson, David G; https://orcid.org/0000-0003-0343-7905, King, George W; https://orcid.org/0000-0002-3641-6636, Lillo-Box, Jorge, Matson, Rachel A; https://orcid.org/0000-0001-7233-7508, Matthews, Elisabeth C, Santos, Nuno C, Sousa, Sérgio G; https://orcid.org/0000-0001-9047-2965, Stassun, Keivan G; https://orcid.org/0000-0002-3481-9052, Tan, Thiam-Guan, Ricker, George R, Vanderspek, Roland, Latham, David W, Seager, Sara, Winn, Joshua N, Jenkins, Jon M, Bayliss, Daniel; https://orcid.org/0000-0001-6023-1335, Bouma, Luke G; https://orcid.org/0000-0002-0514-5538, Ciardi, David R, Collins, Kevin I, Colón, Knicole D, et al, Osborn, Ares; https://orcid.org/0000-0002-5899-7750, Armstrong, David J; https://orcid.org/0000-0002-5080-4117, Fernández Fernández, Jorge, Knierim, Henrik, Adibekyan, Vardan, Collins, Karen A, Delgado-Mena, Elisa, Fridlund, Malcolm; https://orcid.org/0000-0002-0855-8426, Gomes da Silva, João, Hellier, Coel, Jackson, David G; https://orcid.org/0000-0003-0343-7905, King, George W; https://orcid.org/0000-0002-3641-6636, Lillo-Box, Jorge, Matson, Rachel A; https://orcid.org/0000-0001-7233-7508, Matthews, Elisabeth C, Santos, Nuno C, Sousa, Sérgio G; https://orcid.org/0000-0001-9047-2965, Stassun, Keivan G; https://orcid.org/0000-0002-3481-9052, Tan, Thiam-Guan, Ricker, George R, Vanderspek, Roland, Latham, David W, Seager, Sara, Winn, Joshua N, Jenkins, Jon M, Bayliss, Daniel; https://orcid.org/0000-0001-6023-1335, Bouma, Luke G; https://orcid.org/0000-0002-0514-5538, Ciardi, David R, Collins, Kevin I, Colón, Knicole D, and et al
Abstract: To date, thousands of planets have been discovered, but there are regions of the orbital parameter space that are still bare. An example is the short period and intermediate mass/radius space known as the ‘Neptunian desert’, where planets should be easy to find but discoveries remain few. This suggests unusual formation and evolution processes are responsible for the planets residing here. We present the discovery of TOI-332 b, a planet with an ultra-short period of 0.78 d that sits firmly within the desert. It orbits a K0 dwarf with an effective temperature of 5251 ± 71 K. TOI-332 b has a radius of $3.20^{+0.16}_{-0.12}$ R⊕, smaller than that of Neptune, but an unusually large mass of 57.2 ± 1.6 M⊕. It has one of the highest densities of any Neptune-sized planet discovered thus far at $9.6^{+1.1}_{-1.3}$ g cm−3. A 4-layer internal structure model indicates it likely has a negligible hydrogen-helium envelope, something only found for a small handful of planets this massive, and so TOI-332 b presents an interesting challenge to planetary formation theories. We find that photoevaporation cannot account for the mass-loss required to strip this planet of the Jupiter-like envelope it would have been expected to accrete. We need to look towards other scenarios, such as high-eccentricity migration, giant impacts, or gap opening in the protoplanetary disc, to try and explain this unusual discovery.
Published: 2023

35. High-Resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-In Stellar Companions to Exoplanet Host Stars

Author: Littlefield, Colin, Howell, Steve B., Ciardi, David R., Lester, Kathryn V., Everett, Mark E., Furlan, Elise, Matson, Rachel A., Fajardo-Acosta, Sergio B., Gnilka, Crystal L., Littlefield, Colin, Howell, Steve B., Ciardi, David R., Lester, Kathryn V., Everett, Mark E., Furlan, Elise, Matson, Rachel A., Fajardo-Acosta, Sergio B., and Gnilka, Crystal L.
Abstract: The large number of exoplanets discovered with the Transiting Exoplanet Survey Satellite (TESS) means that any observational biases from TESS could influence the derived stellar multiplicity statistics of exoplanet host stars. To investigate this problem, we obtained speckle interferometry of 207 control stars whose properties in the TESS Input Catalog (TIC) closely match those of an exoplanetary host star in the TESS Object of Interest (TOI) catalog, with the objective of measuring the fraction of these stars that have companions within $\sim1.2"$. Our main result is the identification of a bias in the creation of the control sample that prevents the selection of binaries with $0.1" \lesssim \rho \lesssim 1.2"$ and $\Delta$mag $\lesssim3$. This bias is the result of large astrometric residuals that cause binaries with these parameters to fail the quality checks used to create the TIC, which in turn causes them to have incomplete stellar parameters (and uncertainties) in the TIC. Any stellar multiplicity study that relies exclusively upon TIC stellar parameters to identify its targets will struggle to select unresolved binaries in this parameter space. Left uncorrected, this selection bias disproportionately excludes high-mass-ratio binaries, causing the mass-ratio distribution of the companions to deviate significantly from the uniform distribution expected of FGK-type field binaries. After accounting for this bias, the companion rate of the FGK control stars is consistent with the canonical $46\pm2\%$ rate from Raghavan et al. 2010, and the mass-ratio distribution agrees with that of binary TOI host stars. There is marginal evidence that the control-star companions have smaller projected orbital separations than TOI host stars from previous studies., Comment: AJ accepted for publication
Published: 2023

36. The POKEMON Speckle Survey of Nearby M Dwarfs. II. Observations of 1125 Targets

Author: Clark, Catherine A., van Belle, Gerard T., Horch, Elliott P., Lund, Michael B., Ciardi, David R., von Braun, Kaspar, Winters, Jennifer G., Everett, Mark E., Hartman, Zachary D., Llama, Joe, Clark, Catherine A., van Belle, Gerard T., Horch, Elliott P., Lund, Michael B., Ciardi, David R., von Braun, Kaspar, Winters, Jennifer G., Everett, Mark E., Hartman, Zachary D., and Llama, Joe
Abstract: Stellar multiplicity is correlated with many stellar properties, yet multiplicity measurements have proven difficult for the M dwarfs -- the most common type of star in our galaxy -- due to their faintness and the fact that a reasonably-complete inventory of later M dwarfs did not exist until recently. We have therefore carried out the Pervasive Overview of "Kompanions" of Every M dwarf in Our Neighborhood (POKEMON) survey, which made use of the Differential Speckle Survey Instrument on the 4.3-meter Lowell Discovery Telescope, along with the NN-EXPLORE Exoplanet Stellar Speckle Imager on the 3.5-meter WIYN telescope. The POKEMON sample is volume-limited from M0V through M9V out to 15 pc, with additional brighter targets at larger distances. In total, 1125 targets were observed. New discoveries were presented in the first paper in the series. In this second paper in the series, we present all detected companions, gauge our astrometric and photometric precision, and compare our filtered and filterless speckle observations. We find that the majority (58.9%) of the companions we detect in our speckle images are not resolved in Gaia, demonstrating the need for high-resolution imaging in addition to long-term astrometric monitoring. Additionally, we find that the majority (73.2%) of simulated stellar companions would be detectable by our speckle observations. Specifically within 100 au, we find that 70.3% of simulated companions are recovered. Finally, we discuss future directions of the POKEMON survey., Comment: 24 pages, 11 figures. Accepted for publication in the Astronomical Journal
Published: 2023

37. TOI-1696: a nearby M4 dwarf with a $3R_\oplus$ planet in the Neptunian desert

Author: Mori, Mayuko, Livingston, John H., de Leon, Jerome, Narita, Norio, Hirano, Teruyuki, Fukui, Akihiko, Collins, Karen A., Fujita, Naho, Hori, Yasunori, Ishikawa, Hiroyuki Tako, Kawauchi, Kiyoe, Stassun, Keivan G., Watanabe, Noriharu, Giacalone, Steven, Gore, Rebecca, Schroeder, Ashley, Dressing, Courtney D., Bieryla, Allyson, Jensen, Eric L. N., Massey, Bob, Shporer, Avi, Kuzuhara, Masayuki, Charbonneau, David, Ciardi, David R., Doty, John P., Esparza-Borges, Emma, Harakawa, Hiroki, Hodapp, Klaus, Ikoma, Masahiro, Ikuta, Kai, Isogai, Keisuke, Jenkins, Jon M., Kagetani, Taiki, Kimura, Tadahiro, Kodama, Takanori, Kotani, Takayuki, Krishnamurthy, Vigneshwaran, Kudo, Tomoyuki, Kurita, Seiya, Kurokawa, Takashi, Kusakabe, Nobuhiko, Latham, David W., McLean, Brian, Murgas, Felipe, Nishikawa, Jun, Nishiumi, Taku, Omiya, Masashi, Osborn, Hugh P., Palle, Enric, Parviainen, Hannu, Ricker, George R., Seager, Sara, Serizawa, Takuma, Tamura, Motohide, Teng, Huan-Yu, Terada, Yuka, Twicken, Joseph D., Ueda, Akitoshi, Vanderspek, Roland, Vievard, Sébastien, Winn, Joshua N., Zou, Yujie, Mori, Mayuko, Livingston, John H., de Leon, Jerome, Narita, Norio, Hirano, Teruyuki, Fukui, Akihiko, Collins, Karen A., Fujita, Naho, Hori, Yasunori, Ishikawa, Hiroyuki Tako, Kawauchi, Kiyoe, Stassun, Keivan G., Watanabe, Noriharu, Giacalone, Steven, Gore, Rebecca, Schroeder, Ashley, Dressing, Courtney D., Bieryla, Allyson, Jensen, Eric L. N., Massey, Bob, Shporer, Avi, Kuzuhara, Masayuki, Charbonneau, David, Ciardi, David R., Doty, John P., Esparza-Borges, Emma, Harakawa, Hiroki, Hodapp, Klaus, Ikoma, Masahiro, Ikuta, Kai, Isogai, Keisuke, Jenkins, Jon M., Kagetani, Taiki, Kimura, Tadahiro, Kodama, Takanori, Kotani, Takayuki, Krishnamurthy, Vigneshwaran, Kudo, Tomoyuki, Kurita, Seiya, Kurokawa, Takashi, Kusakabe, Nobuhiko, Latham, David W., McLean, Brian, Murgas, Felipe, Nishikawa, Jun, Nishiumi, Taku, Omiya, Masashi, Osborn, Hugh P., Palle, Enric, Parviainen, Hannu, Ricker, George R., Seager, Sara, Serizawa, Takuma, Tamura, Motohide, Teng, Huan-Yu, Terada, Yuka, Twicken, Joseph D., Ueda, Akitoshi, Vanderspek, Roland, Vievard, Sébastien, Winn, Joshua N., and Zou, Yujie
Abstract: We present the discovery and validation of a temperate sub-Neptune around the nearby mid-M dwarf TIC 470381900 (TOI-1696), with a radius of $3.09 \pm 0.11 \,R_\oplus$ and an orbital period of $2.5 \,\rm{days}$, using a combination of TESS and follow-up observations using ground-based telescopes. Joint analysis of multi-band photometry from TESS, MuSCAT, MuSCAT3, Sinistro, and KeplerCam confirmed the transit signal to be achromatic as well as refined the orbital ephemeris. High-resolution imaging with Gemini/'Alopeke and high-resolution spectroscopy with the Subaru/IRD confirmed that there are no stellar companions or background sources to the star. The spectroscopic observations with IRD and IRTF/SpeX were used to determine the stellar parameters, and found the host star is an M4 dwarf with an effective temperature of $T_{eff} = 3185 \pm 76\,\rm{K}$ and a metallicity of [Fe/H] $=0.336 \pm 0.060 \,\rm{dex}$. The radial velocities measured from IRD set a $2$-$\sigma$ upper limit on the planetary mass to be $48.8 \,M_\oplus$. The large radius ratio ($R_p/R_\star \sim 0.1$) and the relatively bright NIR magnitude ($J=12.2 \,\rm{mag}$) make this planet an attractive target for further followup observations. TOI-1696b is one of the planets belonging to the Neptunian desert with the highest transmission spectroscopy metric discovered to date, making it an interesting candidate for atmospheric characterizations with JWST., Comment: 25 pages, 18 figures, 3 tables, Submitted to AJ
Published: 2022

38. A Dearth of Close-In Stellar Companions to M-dwarf TESS Objects of Interest

Author: Clark, Catherine A., van Belle, Gerard T., Ciardi, David R., Lund, Michael B., Howell, Steve B., Everett, Mark E., Beichman, Charles A., Winters, Jennifer G., Clark, Catherine A., van Belle, Gerard T., Ciardi, David R., Lund, Michael B., Howell, Steve B., Everett, Mark E., Beichman, Charles A., and Winters, Jennifer G.
Abstract: TESS has proven to be a powerful resource for finding planets, including those that orbit the most prevalent stars in our galaxy: the M dwarfs. Identification of stellar companions (both bound and unbound) has become a standard component of the transiting planet confirmation process in order to assess the level of light curve dilution and the possibility of the target being a false positive. Studies of stellar companions have also enabled investigations into stellar multiplicity in planet-hosting systems, which has wide-ranging implications for both exoplanet detection and characterization, as well as for the formation and evolution of planetary systems. Speckle and AO imaging are some of the most efficient and effective tools for revealing close-in stellar companions; we therefore present observations of 58 M-dwarf TOIs obtained using a suite of speckle imagers at the 3.5-m WIYN telescope, the 4.3-m Lowell Discovery Telescope, and the 8.1-m Gemini North and South telescopes. These observations, as well as near-infrared adaptive optics images obtained for a subset (14) of these TOIs, revealed only two close-in stellar companions. Upon surveying the literature, and cross-matching our sample with Gaia, SUPERWIDE, and the catalog from El-Badry et al. (2021), we reveal an additional 15 widely-separated common proper motion companions. We also evaluate the potential for undetected close-in companions. Taking into consideration the sensitivity of the observations, our findings suggest that the orbital period distribution of stellar companions to planet-hosting M dwarfs is shifted to longer periods compared to the expected distribution for field M dwarfs., Comment: 28 pages: 24 pages of text with 9 figures, 4 pages of figures in the appendix. Accepted for publication in the Astronomical Journal
Published: 2022

39. A close-in puffy Neptune with hidden friends: The enigma of TOI 620

Author: Reefe, Michael A., Luque, Rafael, Gaidos, Eric, Beard, Corey, Plavchan, Peter P., Cointepas, Marion, Cale, Bryson L., Palle, Enric, Parviainen, Hannu, Feliz, Dax L., Eastman, Jason, Stassun, Keivan, Gagné, Jonathan, Jenkins, Jon M., Boyd, Patricia T., Kidwell, Richard C., McDermott, Scott, Collins, Karen A., Fong, William, Guerrero, Natalia, Almenara-Villa, Jose-Manuel, Bean, Jacob, Beichman, Charles A., Berberian, John, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brady, Madison, Bryant, Edward M., Cacciapuoti, Luca, Cañas, Caleb I., Ciardi, David R., Collins, Kevin I., Crossfield, Ian, Dressing, Courtney D., Eigmueller, Philipp, Mufti, Mohammed El, Esparza-Borges, Emma, Fukui, Akihiko, Gao, Peter, Geneser, Claire, Gnilka, Crystal L., Gonzales, Erica, Gupta, Arvind F., Halverson, Sam, Hearty, Fred, Howell, Steve B., Irwin, Jonathan, Kanodia, Shubham, Kasper, David, Kodama, Takanori, Kostov, Veselin, Latham, David W., Lendl, Monika, Lin, Andrea, Livingston, John H., Lubin, Jack, Mahadevan, Suvrath, Matson, Rachel, Matthews, Elisabeth, Murgas, Felipe, Narita, Norio, Newman, Patrick, Ninan, Joe, Osborn, Ares, Quinn, Samuel N., Robertson, Paul, Roy, Arpita, Schlieder, Joshua, Schwab, Christian, Seifahrt, Andreas, Smith, Gareth D., Sohani, Ahmad, Stefánsson, Guðmundur, Stevens, Daniel, Stürmer, Julian, Tanner, Angelle, Terrien, Ryan, Teske, Johanna, Vermilion, David, Wang, Sharon X., Wittrock, Justin, Wright, Jason T., Zechmeister, Mathias, Zohrabi, Farzaneh, Reefe, Michael A., Luque, Rafael, Gaidos, Eric, Beard, Corey, Plavchan, Peter P., Cointepas, Marion, Cale, Bryson L., Palle, Enric, Parviainen, Hannu, Feliz, Dax L., Eastman, Jason, Stassun, Keivan, Gagné, Jonathan, Jenkins, Jon M., Boyd, Patricia T., Kidwell, Richard C., McDermott, Scott, Collins, Karen A., Fong, William, Guerrero, Natalia, Almenara-Villa, Jose-Manuel, Bean, Jacob, Beichman, Charles A., Berberian, John, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brady, Madison, Bryant, Edward M., Cacciapuoti, Luca, Cañas, Caleb I., Ciardi, David R., Collins, Kevin I., Crossfield, Ian, Dressing, Courtney D., Eigmueller, Philipp, Mufti, Mohammed El, Esparza-Borges, Emma, Fukui, Akihiko, Gao, Peter, Geneser, Claire, Gnilka, Crystal L., Gonzales, Erica, Gupta, Arvind F., Halverson, Sam, Hearty, Fred, Howell, Steve B., Irwin, Jonathan, Kanodia, Shubham, Kasper, David, Kodama, Takanori, Kostov, Veselin, Latham, David W., Lendl, Monika, Lin, Andrea, Livingston, John H., Lubin, Jack, Mahadevan, Suvrath, Matson, Rachel, Matthews, Elisabeth, Murgas, Felipe, Narita, Norio, Newman, Patrick, Ninan, Joe, Osborn, Ares, Quinn, Samuel N., Robertson, Paul, Roy, Arpita, Schlieder, Joshua, Schwab, Christian, Seifahrt, Andreas, Smith, Gareth D., Sohani, Ahmad, Stefánsson, Guðmundur, Stevens, Daniel, Stürmer, Julian, Tanner, Angelle, Terrien, Ryan, Teske, Johanna, Vermilion, David, Wang, Sharon X., Wittrock, Justin, Wright, Jason T., Zechmeister, Mathias, and Zohrabi, Farzaneh
Abstract: We present the validation of a transiting low-density exoplanet orbiting the M2.5 dwarf TOI 620 discovered by the NASA TESS mission. We utilize photometric data from both TESS and ground-based follow-up observations to validate the ephemerides of the 5.09-day transiting signal and vet false positive scenarios. High-contrast imaging data are used to resolve the stellar host and exclude stellar companions at separations $\gtrsim 0.2''$. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with multiple PRV spectrographs to confirm the planetary nature of the transiting exoplanet. We calculate a 5$\sigma$ upper limit of $M_P < 7.1$ M$_\oplus$ and $\rho_P < 0.74$ g cm$^{-3}$, and we identify a non-transiting 17.7-day candidate. We also find evidence for a substellar (1-20 M$_{\rm J}$) companion with a projected separation $\lesssim 20$ au from a combined analysis of Gaia, AO imaging, and RVs. With the discovery of this outer companion, we carry out a detailed exploration of the possibilities that TOI 620 b might instead be a circum-secondary planet or a pair of eclipsing binary stars orbiting the host in a hierarchical triple system. We find, under scrutiny, that we can exclude both of these scenarios from the multi-wavelength transit photometry, thus validating TOI 620 b as a low-density exoplanet transiting the central star in this system. The low density of TOI 620 b makes it one of the most amenable exoplanets for atmospheric characterization, such as with JWST and Ariel, validated or confirmed by the TESS mission to date., Comment: 64 pages, 34 figures, 22 tables. Accepted for publication in the Astronomical Journal
Published: 2022

40. Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2-18

Author: Christiansen, Jessie L., Bhure, Sakhee, Zink, Jon K., Hardegree-Ullman, Kevin K., Adkins, Britt Duffy, Hedges, Christina, Morton, Timothy D., Bieryla, Allyson, Ciardi, David R., Cochran, William D., Dressing, Courtney D., Everett, Mark E., Isaacson, Howard, Livingston, John H., Ziegler, Carl, Berlind, Perry, Calkins, Michael L., Esquerdo, Gilbert A., Latham, David W., Endl, Michael, MacQueen, Phillip J., Fulton, Benjamin J., Hirsch, Lea A., Howard, Andrew W., Weiss, Lauren M., Allen, Bridgette E., Berberyann, Arthur, Ciardi, Krys N., Dunlavy, Ava, Glassford, Sofia H., Dai, Fei, Hirano, Teruyuki, Tamura, Motohide, Beichman, Charles, Gonzales, Erica J., Schlieder, Joshua E., Barclay, Thomas, Crossfield, Ian J. M., Gilbert, Emily A., Matthews, Elisabeth C., Giacalone, Steven, Petigura, Erik A., Christiansen, Jessie L., Bhure, Sakhee, Zink, Jon K., Hardegree-Ullman, Kevin K., Adkins, Britt Duffy, Hedges, Christina, Morton, Timothy D., Bieryla, Allyson, Ciardi, David R., Cochran, William D., Dressing, Courtney D., Everett, Mark E., Isaacson, Howard, Livingston, John H., Ziegler, Carl, Berlind, Perry, Calkins, Michael L., Esquerdo, Gilbert A., Latham, David W., Endl, Michael, MacQueen, Phillip J., Fulton, Benjamin J., Hirsch, Lea A., Howard, Andrew W., Weiss, Lauren M., Allen, Bridgette E., Berberyann, Arthur, Ciardi, Krys N., Dunlavy, Ava, Glassford, Sofia H., Dai, Fei, Hirano, Teruyuki, Tamura, Motohide, Beichman, Charles, Gonzales, Erica J., Schlieder, Joshua E., Barclay, Thomas, Crossfield, Ian J. M., Gilbert, Emily A., Matthews, Elisabeth C., Giacalone, Steven, and Petigura, Erik A.
Abstract: The NASA K2 mission, salvaged from the hardware failures of the Kepler telescope, has continued Kepler's planet-hunting success. It has revealed nearly 500 transiting planets around the ecliptic plane, many of which are the subject of further study, and over 1000 additional candidates. Here we present the results of an ongoing project to follow-up and statistically validate new K2 planets, in particular to identify promising new targets for further characterization. By analyzing the reconnaissance spectra, high-resolution imaging, centroid variations, and statistical likelihood of the signals of 91 candidates, we validate 60 new planets in 46 systems. These include: a number of planets amenable to transmission spectroscopy (K2-384 f, K2-387 b, K2-390 b, K2-403 b, and K2-398 c), emission spectroscopy (K2-371 b, K2-370 b, and K2-399 b), and both (K2-405 b and K2-406 b); several systems with planets in or close to mean motion resonances (K2-381, K2-398) including a compact, TRAPPIST-1-like system of five small planets orbiting a mid-M dwarf (K2-384); an ultra-short period sub-Saturn in the hot Saturn desert (K2-399 b); and a super-Earth orbiting a moderately bright (V=11.93), metal-poor ([Fe/H]=-0.579+/-0.080) host star (K2-408 b). In total we validate planets around 4 F stars, 26 G stars, 13 K stars, and 3 M dwarfs. In addition, we provide a list of 37 vetted planet candidates that should be prioritized for future follow-up observation in order to be confirmed or validated., Comment: 50 pages, 14 figures, 7 tables, accepted in AJ; replaced to fix error in planet name (thanks Travis!) and error in figure label
Published: 2022

41. NEID Rossiter-McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star

Author: Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Stefánsson, Gudmundur K., Bender, Chad F., Blake, Cullen H., Ford, Eric B., Halverson, Samuel, Kanodia, Shubham, Mahadevan, Suvrath, McElwain, Michael W., Ninan, Joe P., Robertson, Paul, Roy, Arpita, Schwab, Christian, Stevens, Daniel J., Terrien, Ryan C., Vanderburg, Andrew, Kraus, Adam L., Douglas, Stephanie, Newton, Elisabeth, Rampalli, Rayna, Krolikowski, Daniel M., Collins, Karen A., Rodriguez, Joseph E., Feliz, Dax L., Srdoc, Gregor, Ziegler, Carl, Barkaoui, Khalid, Pozuelos, Francisco J., Jehin, Emmanuel, Gillon, Michaël, Benkhaldoun, Zouhair, Lewin, Pablo, Forés-Toribio, Raquel, Muñoz, Jose A., McLeod, Kim K., Özyurt, Fiona Powers, Horta, Ferran Grau, Murgas, Felipe, Latham, David W., Quinn, Samuel N., Bieryla, Allyson, Howell, Steve B., Gnilka, Crystal L., Ciardi, David R., Lund, Michael B., Dressing, Courtney D., Giacalone, Steven, Savel, Arjun B., Strakhov, Ivan A., Belinski, Alexander A., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Torres, Guillermo, Paegert, Martin, Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Stefánsson, Gudmundur K., Bender, Chad F., Blake, Cullen H., Ford, Eric B., Halverson, Samuel, Kanodia, Shubham, Mahadevan, Suvrath, McElwain, Michael W., Ninan, Joe P., Robertson, Paul, Roy, Arpita, Schwab, Christian, Stevens, Daniel J., Terrien, Ryan C., Vanderburg, Andrew, Kraus, Adam L., Douglas, Stephanie, Newton, Elisabeth, Rampalli, Rayna, Krolikowski, Daniel M., Collins, Karen A., Rodriguez, Joseph E., Feliz, Dax L., Srdoc, Gregor, Ziegler, Carl, Barkaoui, Khalid, Pozuelos, Francisco J., Jehin, Emmanuel, Gillon, Michaël, Benkhaldoun, Zouhair, Lewin, Pablo, Forés-Toribio, Raquel, Muñoz, Jose A., McLeod, Kim K., Özyurt, Fiona Powers, Horta, Ferran Grau, Murgas, Felipe, Latham, David W., Quinn, Samuel N., Bieryla, Allyson, Howell, Steve B., Gnilka, Crystal L., Ciardi, David R., Lund, Michael B., Dressing, Courtney D., Giacalone, Steven, Savel, Arjun B., Strakhov, Ivan A., Belinski, Alexander A., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Torres, Guillermo, and Paegert, Martin
Abstract: Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, $V_{\rm mag} {\sim} 10.9$), a young K-type dwarf hosting an 8.2-day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of Pleiades cluster (${\sim}120$ Myr) and Praesepe cluster (${\sim}670$ Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter-McLaughlin (RM) effect from both radial velocity (RV) and Doppler Tomography (DT) signals. The 3$\sigma$ upper bounds of the projected stellar obliquity $|\lambda|$ from both models are below 60$^\circ$. The large host star separation ($a/R_\star {\sim} 17$), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment ($a/R_\star {\gtrsim} 10$) and reveals an aligned or slightly misaligned system., Comment: 14 pages, 6 figures, 1 table, accepted for publication in ApJL; see independent work by Subjak et al. for RV follow-up of TOI-1268
Published: 2022
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42. 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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43. 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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44. Validation of 13 Hot and Potentially Terrestrial TESS Planets

Author: Giacalone, Steven, Dressing, Courtney D., Hedges, Christina, Kostov, Veselin B., Collins, Karen A., Jensen, Eric L. N., Yahalomi, Daniel A., Bieryla, Allyson, Ciardi, David R., Howell, Steve B., Lillo-Box, Jorge, Barkaoui, Khalid, Winters, Jennifer G., Matthews, Elisabeth, Livingston, John H., Quinn, Samuel N., Safonov, Boris S., Cadieux, Charles, Furlan, E., Crossfield, Ian J. M., Mandell, Avi M., Gilbert, Emily A., Kruse, Ethan, Quintana, Elisa V., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Adkins, Britt Duffy, Baker, David, Barclay, Thomas, Barrado, David, Batalha, Natalie M., Belinski, Alexander A., Benkhaldoun, Zouhair, Buchhave, Lars A., Cacciapuoti, Luca, Charbonneau, David, Chontos, Ashley, Christiansen, Jessie L., Cloutier, Ryan, Collins, Kevin I., Conti, Dennis M., Cutting, Neil, Dixon, Scott, Doyon, René, Mufti, Mohammed El, Esparza-Borges, Emma, Essack, Zahra, Fukui, Akihiko, Gan, Tianjun, Gary, Kaz, Ghachoui, Mourad, Gillon, Michaël, Girardin, Eric, Glidden, Ana, Gonzales, Erica J., Guerra, Pere, Horch, Elliott P., Helminiak, Krzysztof G., Howard, Andrew W., Huber, Daniel, Irwin, Jonathan M., Isopi, Giovanni, Jehin, Emmanuël, Kagetani, Taiki, Kane, Stephen R., Kawauchi, Kiyoe, Kielkopf, John F., Lewin, Pablo, Luker, Lindy, Lund, Michael B., Mallia, Franco, Mao, Shude, Massey, Bob, Matson, Rachel A., Mireles, Ismael, Mori, Mayuko, Murgas, Felipe, Narita, Norio, O`Dwyer, Tanner, Petigura, Erik A., Polanski, Alex S., Pozuelos, Francisco J., Palle, Enric, Parviainen, Hannu, Plavchan, Peter P., Relles, Howard M., Robertson, Paul, Rose, Mark E., Rowden, Pamela, Roy, Arpita, Savel, Arjun B., Schlieder, Joshua E., Schnaible, Chloe, Schwarz, Richard P., Sefako, Ramotholo, Selezneva, Aleksandra, Skinner, Brett, Stockdale, Chris, Strakhov, Ivan A., Tan, Thiam-Guan, Torres, Guillermo, Tronsgaard, René, Twicken, Joseph D., Vermilion, David, Waite, Ian A., Walter, Bradley, Wang, Gavin, Ziegler, Carl, Zou, Yujie, Giacalone, Steven, Dressing, Courtney D., Hedges, Christina, Kostov, Veselin B., Collins, Karen A., Jensen, Eric L. N., Yahalomi, Daniel A., Bieryla, Allyson, Ciardi, David R., Howell, Steve B., Lillo-Box, Jorge, Barkaoui, Khalid, Winters, Jennifer G., Matthews, Elisabeth, Livingston, John H., Quinn, Samuel N., Safonov, Boris S., Cadieux, Charles, Furlan, E., Crossfield, Ian J. M., Mandell, Avi M., Gilbert, Emily A., Kruse, Ethan, Quintana, Elisa V., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Adkins, Britt Duffy, Baker, David, Barclay, Thomas, Barrado, David, Batalha, Natalie M., Belinski, Alexander A., Benkhaldoun, Zouhair, Buchhave, Lars A., Cacciapuoti, Luca, Charbonneau, David, Chontos, Ashley, Christiansen, Jessie L., Cloutier, Ryan, Collins, Kevin I., Conti, Dennis M., Cutting, Neil, Dixon, Scott, Doyon, René, Mufti, Mohammed El, Esparza-Borges, Emma, Essack, Zahra, Fukui, Akihiko, Gan, Tianjun, Gary, Kaz, Ghachoui, Mourad, Gillon, Michaël, Girardin, Eric, Glidden, Ana, Gonzales, Erica J., Guerra, Pere, Horch, Elliott P., Helminiak, Krzysztof G., Howard, Andrew W., Huber, Daniel, Irwin, Jonathan M., Isopi, Giovanni, Jehin, Emmanuël, Kagetani, Taiki, Kane, Stephen R., Kawauchi, Kiyoe, Kielkopf, John F., Lewin, Pablo, Luker, Lindy, Lund, Michael B., Mallia, Franco, Mao, Shude, Massey, Bob, Matson, Rachel A., Mireles, Ismael, Mori, Mayuko, Murgas, Felipe, Narita, Norio, O`Dwyer, Tanner, Petigura, Erik A., Polanski, Alex S., Pozuelos, Francisco J., Palle, Enric, Parviainen, Hannu, Plavchan, Peter P., Relles, Howard M., Robertson, Paul, Rose, Mark E., Rowden, Pamela, Roy, Arpita, Savel, Arjun B., Schlieder, Joshua E., Schnaible, Chloe, Schwarz, Richard P., Sefako, Ramotholo, Selezneva, Aleksandra, Skinner, Brett, Stockdale, Chris, Strakhov, Ivan A., Tan, Thiam-Guan, Torres, Guillermo, Tronsgaard, René, Twicken, Joseph D., Vermilion, David, Waite, Ian A., Walter, Bradley, Wang, Gavin, Ziegler, Carl, and Zou, Yujie
Abstract: The James Webb Space Telescope (JWST) will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii ($R_{\rm p} \sim 0.6 - 2.0 R_\oplus$) and orbit stars of various magnitudes ($K_s = 5.78 - 10.78$, $V = 8.4 - 15.69$) and effective temperatures ($T_{\rm eff }\sim 3000 - 6000$ K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools -- DAVE and TRICERATOPS -- to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest ($133 \pm 26$ Myr) solar twin with a known planet to date. TOI-2260 is a young ($321 \pm 96$ Myr) G dwarf that is among the most metal-rich ([Fe/H] = $0.22 \pm 0.06$ dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of $\sim 2600$ K, TOI-2260 b is also the fourth hottest known planet with $R_{\rm p} < 2 \, R_\oplus$.
Published: 2022
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45. TESS Giants Transiting Giants II: The hottest Jupiters orbiting evolved stars

Author: Grunblatt, Samuel K., Saunders, Nicholas, Sun, Meng, Chontos, Ashley, Soares-Furtado, Melinda, Eisner, Nora, Pereira, Filipe, Komacek, Thaddeus, Huber, Daniel, Collins, Karen, Wang, Gavin, Stockdale, Chris, Quinn, Samuel N., Tronsgaard, Rene, Zhou, George, Nowak, Grzegorz, Deeg, Hans J., Ciardi, David R., Boyle, Andrew, Rice, Malena, Dai, Fei, Blunt, Sarah, Van Zandt, Judah, Beard, Corey, Murphy, Joseph M. Akana, Dalba, Paul A., Lubin, Jack, Polanski, Alex, Brinkman, Casey Lynn, Howard, Andrew W., Buchhave, Lars A., Angus, Ruth, Ricker, George R., Jenkins, Jon M., Wohler, Bill, Goeke, Robert F., Levine, Alan M., Colon, Knicole D., Huang, Chelsea X., Kunimoto, Michelle, Shporer, Avi, Latham, David W., Seager, Sara, Vanderspek, Roland K., Winn, Joshua N., Grunblatt, Samuel K., Saunders, Nicholas, Sun, Meng, Chontos, Ashley, Soares-Furtado, Melinda, Eisner, Nora, Pereira, Filipe, Komacek, Thaddeus, Huber, Daniel, Collins, Karen, Wang, Gavin, Stockdale, Chris, Quinn, Samuel N., Tronsgaard, Rene, Zhou, George, Nowak, Grzegorz, Deeg, Hans J., Ciardi, David R., Boyle, Andrew, Rice, Malena, Dai, Fei, Blunt, Sarah, Van Zandt, Judah, Beard, Corey, Murphy, Joseph M. Akana, Dalba, Paul A., Lubin, Jack, Polanski, Alex, Brinkman, Casey Lynn, Howard, Andrew W., Buchhave, Lars A., Angus, Ruth, Ricker, George R., Jenkins, Jon M., Wohler, Bill, Goeke, Robert F., Levine, Alan M., Colon, Knicole D., Huang, Chelsea X., Kunimoto, Michelle, Shporer, Avi, Latham, David W., Seager, Sara, Vanderspek, Roland K., and Winn, Joshua N.
Abstract: Giant planets on short-period orbits are predicted to be inflated and eventually engulfed by their host stars. However, the detailed timescales and stages of these processes are not well known. Here we present the discovery of three hot Jupiters (P $<$ 10 d) orbiting evolved, intermediate-mass stars ($M_\star$ $\approx$ 1.5 M$_\odot$, 2 R$_\odot$ $<$ $R_\star < $ 5 R$_\odot$). By combining \tess photometry with ground-based photometry and radial velocity measurements, we report masses and radii for these three planets between 0.4 and 1.8 M$_\mathrm{J}$ and 0.8 and 1.8 R$_\mathrm{J}$. \planet has the shortest period (P=\period) of any planet discovered around a red giant star to date. Both \planettwo and \planetthree appear to be inflated, but \planet does not show any sign of inflation. The large radii and relatively low masses of \planettwo and \planetthree place them among the lowest density hot Jupiters currently known, while \planet is conversely one of the highest. All three planets have orbital eccentricities below 0.2. The large spread in radii for these systems implies that planet inflation has a complex dependence on planet mass, radius, incident flux, and orbital properties. We predict that \planet has the shortest orbital decay timescale of any planet currently known, but do not detect any orbital decay in this system. Transmission spectroscopy of \planettwo would provide a favorable opportunity for the detection of water, carbon dioxide and carbon monoxide features in the atmosphere of a planet orbiting an evolved star, and could yield new information about planet formation and atmospheric evolution., Comment: 22 pages, 15 figures, accepted for publication in the Astronomical Journal
Published: 2022
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46. A pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 characterized 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, Floren, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sebastien, Sousa, Sergio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Barczy, Tamas, Navascues, David Barrado, 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, Sebastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colon, 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, Michael, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Gudel, 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., des Etangs, Alain Lecavelier, 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, Mekarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Goran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Palle, 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, Francois-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Segransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabo, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stephane, Van Eylen, Vincent, Van Grootel, Valerie, 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, Floren, Hans-Gustav, Guterman, Pascal, Adibekyan, Vardan, Hooton, Matthew J., Hoyer, Sergio, Leleu, Adrien, Mustill, Alexander James, Salmon, Sebastien, Sousa, Sergio G., Suarez, Olga, Abe, Lyu, Agabi, Abdelkrim, Alonso, Roi, Anglada, Guillem, Asquier, Joel, Barczy, Tamas, Navascues, David Barrado, 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, Sebastien, Ciardi, David R., Cloutier, Ryan, Cochran, William D., Collins, Karen A., Colon, 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, Michael, Gnilka, Crystal L., Grieves, Nolan, Grziwa, Sascha, Gudel, 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., des Etangs, Alain Lecavelier, 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, Mekarnia, Djamel, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Goran, Osborn, Hugh P., Osborne, Hannah L. M., Ottensamer, Roland, Pagano, Isabella, Palle, 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, Francois-Xavier, Schwarz, Richard P., Scott, Nicholas J., Seager, Sara, Segransan, Damien, Serrano, Luisa Maria, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabo, Gyula, Thomas, Nicolas, Ting, Eric B., Triaud, Amaury H. M. J., Udry, Stephane, Van Eylen, Vincent, Van Grootel, Valerie, Vanderspek, Roland K., Viotto, Valentina, Walton, Nicholas, and Winn, Joshua N.
Abstract: We report the discovery and characterization of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in the Transiting Exoplanet Survey Satellite (TESS) photometry. To characterize the system, we performed and retrieved the CHaracterising ExOPlanets Satellite (CHEOPS), TESS, and ground-based photometry, the High Accuracy Radial velocity Planet Searcher (HARPS) high-resolution spectroscopy, and Gemini speckle imaging. We characterize the host star and determine T-eff,T-* = 4734 +/- 67 K, R-* = 0.726 +/- 0.007 R-circle dot, and M-* = 0.748 +/- 0.032 M-circle dot. We present a novel detrending method based on point spread function 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-b = 6.44387 +/- 0.00003 d, a radius of R-b = 2.59 +/- 0.04 R-circle plus, and a mass of M-b = 13.5(-1.8)(+1.7) M-circle plus, whilst TOI-1064 c has an orbital period of P-c = 12.22657(-0.00004)(+0.00005) d, a radius of R-c = 2.65 +/- 0.04 R-circle plus, and a 3 sigma upper mass limit of 8.5 M-circle plus. From the high-precision photometry we obtain radius uncertainties of similar to 1.6 per cent, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterized 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 radial velocities 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 allow us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that m
Published: 2022

47. The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI-1246

Author: Turtelboom, Emma, Weiss, Lauren M., Dressing, Courtney D., Nowak, Grzegorz, Palle, 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., Mocnik, 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, Martin, 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., Lariviere, Maude, Lester, Kathryn, 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, Ricker, George R., Vanderspek, Roland, Seager, S., Winn, Joshua N., Turtelboom, Emma, Weiss, Lauren M., Dressing, Courtney D., Nowak, Grzegorz, Palle, 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., Mocnik, 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, Martin, 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., Lariviere, Maude, Lester, Kathryn, 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, Ricker, George R., Vanderspek, Roland, Seager, S., and Winn, Joshua N.
Abstract: Multiplanet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf (V = 11.6, K = 9.9) and four transiting sub-Neptunes identified by TESS with orbital periods of 4.31, 5.90, 18.66, and 37.92 days. 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 (2.97 +/- 0.06 R (circle plus), 2.47 +/- 0.08 R (circle plus), 3.46 +/- 0.09 R (circle plus), and 3.72 +/- 0.16 R (circle plus)) and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets (8.1 +/- 1.1 M (circle plus), 8.8 +/- 1.2 M (circle plus), 5.3 +/- 1.7 M (circle plus), and 14.8 +/- 2.3 M (circle plus)). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance (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 five systems with measured masses and radii for all four transiting planets. The planet densities range from 0.70 +/- 0.24 to 3.21 +/- 0.44 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 +/- 3.6 M (circle plus). This planet candidate is exterior to TOI-1246 e, with a candidate period of 93.8 days, and we discuss the implications if it is confirmed to be planetary in nature.
Published: 2022

48. TESS Hunt for Young and Maturing Exoplanets (THYME) IX: a 27 Myr extended population of Lower-Centaurus Crux with a transiting two-planet system

Author: Wood, Mackenna L., Mann, Andrew W., Barber, Madyson G., Bush, Jonathan L., Kraus, Adam L., Tofflemire, Benjamin M., Vanderburg, Andrew, Newton, Elisabeth R., Feiden, Gregory A., Zhou, George, Bouma, Luke G., Quinn, Samuel N., Armstrong, David J., Osborn, Ares, Adibekyan, Vardan, Mena, Elisa Delgado, Sousa, Sergio G., Gagné, Jonathan, Fields, Matthew J., Milburn, Reilly P., Thao, Pa Chia, Schmidt, Stephen P., Gnilka, Crystal L., Howell, Steve B., Law, Nicholas M., Ziegler, Carl, Briceño, César, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Schlieder, Joshua E., Osborn, Hugh P., Twicken, Joseph D., Ciardi, David R., Huang, Chelsea X., Wood, Mackenna L., Mann, Andrew W., Barber, Madyson G., Bush, Jonathan L., Kraus, Adam L., Tofflemire, Benjamin M., Vanderburg, Andrew, Newton, Elisabeth R., Feiden, Gregory A., Zhou, George, Bouma, Luke G., Quinn, Samuel N., Armstrong, David J., Osborn, Ares, Adibekyan, Vardan, Mena, Elisa Delgado, Sousa, Sergio G., Gagné, Jonathan, Fields, Matthew J., Milburn, Reilly P., Thao, Pa Chia, Schmidt, Stephen P., Gnilka, Crystal L., Howell, Steve B., Law, Nicholas M., Ziegler, Carl, Briceño, César, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Schlieder, Joshua E., Osborn, Hugh P., Twicken, Joseph D., Ciardi, David R., and Huang, Chelsea X.
Abstract: We report the discovery and characterization of a nearby (~ 85 pc), older (27 +/- 3 Myr), distributed stellar population near Lower-Centaurus-Crux (LCC), initially identified by searching for stars co-moving with a candidate transiting planet from TESS (HD 109833; TOI 1097). We determine the association membership using Gaia kinematics, color-magnitude information, and rotation periods of candidate members. We measure it's age using isochrones, gyrochronology, and Li depletion. While the association is near known populations of LCC, we find that it is older than any previously found LCC sub-group (10-16 Myr), and distinct in both position and velocity. In addition to the candidate planets around HD 109833 the association contains four directly-imaged planetary-mass companions around 3 stars, YSES-1, YSES-2, and HD 95086, all of which were previously assigned membership in the younger LCC. Using the Notch pipeline, we identify a second candidate transiting planet around HD 109833. We use a suite of ground-based follow-up observations to validate the two transit signals as planetary in nature. HD 109833 b and c join the small but growing population of <100 Myr transiting planets from TESS. HD 109833 has a rotation period and Li abundance indicative of a young age (< 100 Myr), but a position and velocity on the outskirts of the new population, lower Li levels than similar members, and a CMD position below model predictions for 27 Myr. So, we cannot reject the possibility that HD 109833 is a young field star coincidentally nearby the population., Comment: 23 pages, 15 figures, Accepted for publication in AJ
Published: 2022
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49. SImMER: A Pipeline for Reducing and Analyzing Images of Stars

Author: Savel, Arjun B., Hirsch, Lea A., Gill, Holden, Dressing, Courtney D., Ciardi, David R., Savel, Arjun B., Hirsch, Lea A., Gill, Holden, Dressing, Courtney D., and Ciardi, David R.
Abstract: We present the first public version of SImMER, an open-source Python reduction pipeline for astronomical images of point sources. Current capabilities include dark-subtraction, flat-fielding, sky-subtraction, image registration, FWHM measurement, contrast curve calculation, and table and plot generation. SImMER supports observations taken with the ShARCS camera on the Shane 3-m telescope and the PHARO camera on the Hale 5.1-m telescope. The modular nature of SImMER allows users to extend the pipeline to accommodate additional instruments with relative ease. One of the core functions of the pipeline is its image registration module, which is flexible enough to reduce saturated images and images of similar-brightness, resolved stellar binaries. Furthermore, SImMER can compute contrast curves for reduced images and produce publication-ready plots. The code is developed online at \url{https://github.com/arjunsavel/SImMER} and is both pip- and conda-installable. We develop tutorials and documentation alongside the code and host them online. With SImMER, we aim to provide a community resource for accurate and reliable data reduction and analysis., Comment: 12 pages, 5 figures. Accepted to PASP
Published: 2022
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50. A systematic validation of hot Neptunes in TESS data

Author: Magliano, Christian, Covone, Giovanni, Dobal, Richa, Cacciapuoti, Luca, Tonietti, Luca, Giacalone, Steven, Vines, Jose I., Inno, Laura, Jenkins, James S., Lissauer, Jack J., Bieryla, Allyson, Oliva, Fabrizio, Pagano, Isabella, Kostov, Veselin, Ziegler, Carl, Ciardi, David R., Gonzales, Erica J., Dressing, Courtney D., Buchhave, Lars A., Howell, Steve B., Matson, Rachel A., Matthews, Elisabeth, Rotundi, Alessandra, Alves, Douglas, Fiscale, Stefano, Ienco, Riccardo M., Pena, Pablo, Gallo, Francesco, Tomajoli, Maria T. Muscari, Magliano, Christian, Covone, Giovanni, Dobal, Richa, Cacciapuoti, Luca, Tonietti, Luca, Giacalone, Steven, Vines, Jose I., Inno, Laura, Jenkins, James S., Lissauer, Jack J., Bieryla, Allyson, Oliva, Fabrizio, Pagano, Isabella, Kostov, Veselin, Ziegler, Carl, Ciardi, David R., Gonzales, Erica J., Dressing, Courtney D., Buchhave, Lars A., Howell, Steve B., Matson, Rachel A., Matthews, Elisabeth, Rotundi, Alessandra, Alves, Douglas, Fiscale, Stefano, Ienco, Riccardo M., Pena, Pablo, Gallo, Francesco, and Tomajoli, Maria T. Muscari
Abstract: We statistically validated a sample of hot Neptune candidates applying a two-step vetting technique using DAVE and TRICERATOPS. We performed a systematic validation of 250 transit-like events in the Transiting Exoplanet Survey Satellite (TESS) archive in the parameter region defined by $P\leq 4$ d and $3R_\oplus\leq R\leq 5R_\oplus$. Through our analysis, we identified 18 hot Neptune-sized candidates, with a false positive probability $<50\%$. Nine of these planet candidates still need to be confirmed. For each of the nine targets we retrieved the stellar parameters using ARIADNE and derived constraints on the planetary parameters by fitting the lightcurves with the juliet package. Within this sample of nine candidates, we statistically validated (i.e, with false positive probability < $0.3\%$) two systems (TOI-277 b and TOI-1288 b) by re-processing the candidates with TRICERATOPS along with follow-up observations. These new validated exoplanets expand the known hot Neptunes population and are high-priority targets for future radial velocities follow-up., Comment: 24 pages, 20 figures. Accepted for publication on MNRAS
Published: 2022
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