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310 results on '"Wittenmyer, Robert A"'

1. Eccentricity Distribution Beyond the Snow Line and Implications for Planetary Habitability

Author: Kane, Stephen R., Wittenmyer, Robert A., Kane, Stephen R., and Wittenmyer, Robert A.
Abstract: A fundamental question in the study of planetary system demographics is: how common is the solar system architecture? The primary importance of this question lies in the potential of planetary systems to create habitable environments, and dissecting the various components of solar system evolution that contributed to a sustainable temperate surface for Earth. One important factor in that respect is volatile delivery to the inner system and the dependence on giant planets beyond the snow line as scattering agents, particularly as such cold giant planets are relatively rare. Here, we provide an investigation of the eccentricity distribution for giant planet populations both interior and exterior to their system snow lines. We show that the median eccentricity for cold giants is 0.23, compared with a far more circular orbital regime for inner planets. We further present the results of a dynamical simulation that explores the particle scattering potential for a Jupiter analog in comparison with a Jupiter whose eccentricity matches that of the median cold giant eccentricity. These simulations demonstrate that the capacity for such an eccentric cold giant system to scatter volatiles interior to the snow line is significantly increased compared with the Jupiter analog case, resulting in a far greater volume of Earth-crossing volatiles. Thus, many of the known systems with cold giant planets may harbor water worlds interior to the snow line., Comment: 10 pages, 2 figures, accepted for publication in the Astrophysical Journal Letters
Published: 2024

2. Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System

Author: Li, Zhexing, Kane, Stephen R., Brandt, Timothy D., Fetherolf, Tara, Robertson, Paul, Zhao, Jinglin, Dalba, Paul A., Wittenmyer, Robert A., Butler, R. Paul, Diaz, Matias R., Howell, Steve B., Bailey, Jeremy, Carter, Brad, Furlan, Elise, Gnilka, Crystal L., Jones, Hugh R. A., O'Toole, Simon, Tinney, Chris, Li, Zhexing, Kane, Stephen R., Brandt, Timothy D., Fetherolf, Tara, Robertson, Paul, Zhao, Jinglin, Dalba, Paul A., Wittenmyer, Robert A., Butler, R. Paul, Diaz, Matias R., Howell, Steve B., Bailey, Jeremy, Carter, Brad, Furlan, Elise, Gnilka, Crystal L., Jones, Hugh R. A., O'Toole, Simon, and Tinney, Chris
Abstract: Multi-planet systems exhibit a diversity of architectures that diverge from the solar system and contribute to the topic of exoplanet demographics. Radial velocity (RV) surveys form a crucial component of exoplanet surveys, as their long observational baselines allow searches for more distant planetary orbits. This work provides a significantly revised architecture for the multi-planet system HD 134606 using both HARPS and UCLES RVs. We confirm the presence of previously reported planets b, c, and d with periods $12.0897^{+0.0019}_{-0.0018}$, $58.947^{+0.056}_{-0.054}$, and $958.7^{+6.3}_{-5.9}$ days, and masses $9.14^{+0.65}_{-0.63}$, $11.0\pm1$, and $44.5\pm2.9$ Earth masses respectively, with the planet d orbit significantly revised to over double that originally reported. We report two newly detected super-Earths, e and f, with periods $4.31943^{+0.00075}_{-0.00068}$ and $26.9^{+0.019}_{-0.017}$ days, and masses $2.31^{+0.36}_{-0.35}$ and $5.52^{+0.74}_{-0.73}$ Earth masses, respectively. In addition, we identify a linear trend in the RV time series, and the cause of this acceleration is deemed to be a newly detected sub-stellar companion at large separation. HD 134606 now displays four low mass planets in a compact region near the star, one gas giant further out in the Habitable Zone, an additional massive companion in the outer regime, and a low mass M dwarf stellar companion at large separation, making it an intriguing target for system formation/evolution studies. The location of planet d in the Habitable Zone proves to be an exciting candidate for future space-based direct imaging missions, whereas continued RV observations of this system are recommended for understanding the nature of the massive, long period companion., Comment: 23 pages, 10 figures, 4 tables, accepted for publication in the Astronomical Journal
Published: 2024

3. Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System

Author: Li, Zhexing, Kane, Stephen R., Brandt, Timothy D., Fetherolf, Tara, Robertson, Paul, Zhao, Jinglin, Dalba, Paul A., Wittenmyer, Robert A., Butler, R. Paul, Díaz, Matías R., Howell, Steve B., Bailey, Jeremy, Carter, Brad, Furlan, Elise, Gnilka, Crystal L., Horner, Jonathan, Jones, Hugh R. A., O’Toole, Simon, Tinney, Chris, Li, Zhexing, Kane, Stephen R., Brandt, Timothy D., Fetherolf, Tara, Robertson, Paul, Zhao, Jinglin, Dalba, Paul A., Wittenmyer, Robert A., Butler, R. Paul, Díaz, Matías R., Howell, Steve B., Bailey, Jeremy, Carter, Brad, Furlan, Elise, Gnilka, Crystal L., Horner, Jonathan, Jones, Hugh R. A., O’Toole, Simon, and Tinney, Chris
Abstract: Multiplanet systems exhibit a diversity of architectures that diverge from the solar system and contribute to the topic of exoplanet demographics. Radial velocity (RV) surveys form a crucial component of exoplanet surveys, as their long observational baselines allow for searches for more distant planetary orbits. This work provides a significantly revised architecture for the multiplanet system HD 134606 using both HARPS and UCLES RVs.
Published: 2024

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

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

5. TOI-1994b: A Low Mass Eccentric Brown Dwarf Transiting A Subgiant Star

Author: Page, Emma, Pepper, Joshua, Wright, Duncan, Rodriguez, Joseph E., Wittenmyer, Robert A., Kane, Stephen R., Addison, Brett, Bedding, Timothy, Bowler, Brendan P., Barclay, Thomas, Collins, Karen A., Evans, Phil, Horner, Jonathan, Jensen, Eric L. N., Johnson, Marshall C., Kielkopf, John, Mireles, Ismael, Plavchan, Peter, Quinn, Samuel N., Seager, S., Stassun, Keivan G., Striegel, Stephanie, Winn, Joshua N., Zhou, George, Ziegler, Carl, Page, Emma, Pepper, Joshua, Wright, Duncan, Rodriguez, Joseph E., Wittenmyer, Robert A., Kane, Stephen R., Addison, Brett, Bedding, Timothy, Bowler, Brendan P., Barclay, Thomas, Collins, Karen A., Evans, Phil, Horner, Jonathan, Jensen, Eric L. N., Johnson, Marshall C., Kielkopf, John, Mireles, Ismael, Plavchan, Peter, Quinn, Samuel N., Seager, S., Stassun, Keivan G., Striegel, Stephanie, Winn, Joshua N., Zhou, George, and Ziegler, Carl
Abstract: We present the discovery of TOI-1994b, a low-mass brown dwarf transiting a hot subgiant star on a moderately eccentric orbit. TOI-1994 has an effective temperature of $7700^{+720}_{-410}$ K, V magnitude of 10.51 mag and log(g) of $3.982^{+0.067}_{-0.065}$. The brown dwarf has a mass of $22.1^{+2.6}_{-2.5}$ $M_J$, a period of 4.034 days, an eccentricity of $0.341^{+0.054}_{-0.059}$, and a radius of $1.220^{+0.082}_{-0.071}$ $R_J$. TOI-1994b is more eccentric than other transiting brown dwarfs with similar masses and periods. The population of low mass brown dwarfs may have properties similar to planetary systems if they were formed in the same way, but the short orbital period and high eccentricity of TOI-1994b may contrast this theory. An evolved host provides a valuable opportunity to understand the influence stellar evolution has on the substellar companion's fundamental properties. With precise age, mass, and radius, the global analysis and characterization of TOI-1994b augments the small number of transiting brown dwarfs and allows the testing of substellar evolution models., Comment: 12 pages, 7 figures, Submitted to AAS Journals
Published: 2023

6. Three Saturn-mass planets transiting F-type stars revealed with TESS and HARPS

Author: Psaridi, Angelica, Bouchy, François, Lendl, Monika, Akinsanmi, Babatunde, Stassun, Keivan G., Smalley, Barry, Armstrong, David J., Howard, Saburo, Ulmer-Moll, Solène, Grieves, Nolan, Barkaoui, Khalid, Rodriguez, Joseph E., Bryant, Edward M., Suárez, Olga, Guillot, Tristan, Evans, Phil, Attia, Omar, Wittenmyer, Robert A., Yee, Samuel W., Collins, Karen A., Zhou, George, Galland, Franck, Parc, Léna, Udry, Stéphane, Figueira, Pedro, Ziegler, Carl, Mordasini, Christoph, Winn, Joshua N., Seager, Sara, Jenkins, Jon M., Twicken, Joseph D., Brahm, Rafael, Jones, Matías I., Abe, Lyu, Addison, Brett, Briceño, César, Briegal, Joshua T., Collins, Kevin I., Daylan, Tansu, Eigmüller, Phillip, Furesz, Gabor, Guerrero, Natalia M., Hagelberg, Janis, Heitzmann, Alexis, Hounsell, Rebekah, Huang, Chelsea X., Krenn, Andreas, Law, Nicholas M., Mann, Andrew W., McCormac, James, Mékarnia, Djamel, Mounzer, Dany, Nielsen, Louise D., Osborn, Ares, Reinarz, Yared, Sefako, Ramotholo R., Steiner, Michal, Strøm, Paul A., Triaud, Amaury H. M. J., Vanderspek, Roland, Vanzi, Leonardo, Vines, Jose I., Watson, Christopher A., Wright, Duncan J., Zapata, Abner, Psaridi, Angelica, Bouchy, François, Lendl, Monika, Akinsanmi, Babatunde, Stassun, Keivan G., Smalley, Barry, Armstrong, David J., Howard, Saburo, Ulmer-Moll, Solène, Grieves, Nolan, Barkaoui, Khalid, Rodriguez, Joseph E., Bryant, Edward M., Suárez, Olga, Guillot, Tristan, Evans, Phil, Attia, Omar, Wittenmyer, Robert A., Yee, Samuel W., Collins, Karen A., Zhou, George, Galland, Franck, Parc, Léna, Udry, Stéphane, Figueira, Pedro, Ziegler, Carl, Mordasini, Christoph, Winn, Joshua N., Seager, Sara, Jenkins, Jon M., Twicken, Joseph D., Brahm, Rafael, Jones, Matías I., Abe, Lyu, Addison, Brett, Briceño, César, Briegal, Joshua T., Collins, Kevin I., Daylan, Tansu, Eigmüller, Phillip, Furesz, Gabor, Guerrero, Natalia M., Hagelberg, Janis, Heitzmann, Alexis, Hounsell, Rebekah, Huang, Chelsea X., Krenn, Andreas, Law, Nicholas M., Mann, Andrew W., McCormac, James, Mékarnia, Djamel, Mounzer, Dany, Nielsen, Louise D., Osborn, Ares, Reinarz, Yared, Sefako, Ramotholo R., Steiner, Michal, Strøm, Paul A., Triaud, Amaury H. M. J., Vanderspek, Roland, Vanzi, Leonardo, Vines, Jose I., Watson, Christopher A., Wright, Duncan J., and Zapata, Abner
Abstract: While the sample of confirmed exoplanets continues to increase, the population of transiting exoplanets around early-type stars is still limited. These planets allow us to investigate the planet properties and formation pathways over a wide range of stellar masses and study the impact of high irradiation on hot Jupiters orbiting such stars. We report the discovery of TOI-615b, TOI-622b, and TOI-2641b, three Saturn-mass planets transiting main sequence, F-type stars. The planets were identified by the Transiting Exoplanet Survey Satellite (TESS) and confirmed with complementary ground-based and radial velocity observations. TOI-615b is a highly irradiated ($\sim$1277 $F_{\oplus}$) and bloated Saturn-mass planet (1.69$^{+0.05}_{-0.06}$$R_{Jup}$ and 0.43$^{+0.09}_{-0.08}$$M_{Jup}$) in a 4.66 day orbit transiting a 6850 K star. TOI-622b has a radius of 0.82$^{+0.03}_{-0.03}$$R_{Jup}$ and a mass of 0.30$^{+0.07}_{-0.08}$~$M_{Jup}$ in a 6.40 day orbit. Despite its high insolation flux ($\sim$600 $F_{\oplus}$), TOI-622b does not show any evidence of radius inflation. TOI-2641b is a 0.39$^{+0.02}_{-0.04}$$M_{Jup}$ planet in a 4.88 day orbit with a grazing transit (b = 1.04$^{+0.05}_{-0.06 }$) that results in a poorly constrained radius of 1.61$^{+0.46}_{-0.64}$$R_{Jup}$. Additionally, TOI-615b is considered attractive for atmospheric studies via transmission spectroscopy with ground-based spectrographs and $\textit{JWST}$. Future atmospheric and spin-orbit alignment observations are essential since they can provide information on the atmospheric composition, formation and migration of exoplanets across various stellar types., Comment: 16 pages, 17 figures, submitted to A&A
Published: 2023
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7. Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions

Author: Laliotis, Katherine, Burt, Jennifer A., Mamajek, Eric E., Li, Zhexing, Perdelwitz, Volker, Zhao, Jinglin, Butler, R. Paul, Holden, Bradford, Rosenthal, Lee, Fulton, B. J., Feng, Fabo, Kane, Stephen R., Bailey, Jeremy, Carter, Brad, Crane, Jeffrey D., Furlan, Elise, Gnilka, Crystal L., Howell, Steve B., Laughlin, Gregory, Shectman, Stephen A., Teske, Johanna K., Tinney, C. G., Vogt, Steven S., Wang, Sharon Xuesong, Wittenmyer, Robert A., Laliotis, Katherine, Burt, Jennifer A., Mamajek, Eric E., Li, Zhexing, Perdelwitz, Volker, Zhao, Jinglin, Butler, R. Paul, Holden, Bradford, Rosenthal, Lee, Fulton, B. J., Feng, Fabo, Kane, Stephen R., Bailey, Jeremy, Carter, Brad, Crane, Jeffrey D., Furlan, Elise, Gnilka, Crystal L., Howell, Steve B., Laughlin, Gregory, Shectman, Stephen A., Teske, Johanna K., Tinney, C. G., Vogt, Steven S., Wang, Sharon Xuesong, and Wittenmyer, Robert A.
Abstract: Directly imaging temperate rocky planets orbiting nearby, Sun-like stars with a 6-m-class IR/O/UV space telescope, recently dubbed the Habitable Worlds Observatory, is a high priority goal of the Astro2020 Decadal Survey. To prepare for future direct imaging surveys, the list of potential targets should be thoroughly vetted to maximize efficiency and scientific yield. We present an analysis of archival radial velocity data for southern stars from the NASA/NSF Extreme Precision Radial Velocity Working Group's list of high priority target stars for future direct imaging missions (drawn from the HabEx, LUVOIR, and Starshade studies). For each star, we constrain the region of companion mass and period parameter space we are already sensitive to based on the observational baseline, sampling, and precision of the archival RV data. Additionally, for some of the targets we report new estimates of magnetic activity cycle periods, rotation periods, improved orbital parameters for previously known exoplanets, and new candidate planet signals that require further vetting or observations to confirm. Our results show that for many of these stars we are not yet sensitive to even Saturn-mass planets in the habitable zone, let alone smaller planets, highlighting the need for future EPRV vetting efforts before the launch of a direct imaging mission. We present evidence that the candidate temperate super-Earth exoplanet HD 85512 b is most likely due to the star's rotation, and report an RV acceleration for delta Pav which supports the existence of a distant giant planet previously inferred from astrometry., Comment: 58 pages, 11 figures, 4 figure sets to be included in the online journal Accepted for publication in AJ
Published: 2023
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8. TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting An Extremely Eccentric Exoplanet

Author: Jiang, Chen, Wu, Tao, Feinstein, Adina D., Stassun, Keivan G., Bedding, Timothy R., Veras, Dimitri, Corsaro, Enrico, Buzasi, Derek L., Stello, Dennis, Li, Yaguang, Mathur, Savita, Garcia, Rafael A., Breton, Sylvain N., Lundkvist, Mia S., Mikolajczyk, Przemyslaw J., Gehan, Charlotte, Campante, Tiago L., Bossini, Diego, Kane, Stephen R., Ong, Jia Mian Joel, Yildiz, Mutlu, Kayhan, Cenk, Orhan, Zeynep Celik, Ortel, Sibel, Zhang, Xinyi, Cunha, Margarida S., de Moura, Bruno Lustosa, Yu, Jie, Huber, Daniel, Ou, Jian-wen, Wittenmyer, Robert A., Gizon, Laurent, Chaplin, William J., Jiang, Chen, Wu, Tao, Feinstein, Adina D., Stassun, Keivan G., Bedding, Timothy R., Veras, Dimitri, Corsaro, Enrico, Buzasi, Derek L., Stello, Dennis, Li, Yaguang, Mathur, Savita, Garcia, Rafael A., Breton, Sylvain N., Lundkvist, Mia S., Mikolajczyk, Przemyslaw J., Gehan, Charlotte, Campante, Tiago L., Bossini, Diego, Kane, Stephen R., Ong, Jia Mian Joel, Yildiz, Mutlu, Kayhan, Cenk, Orhan, Zeynep Celik, Ortel, Sibel, Zhang, Xinyi, Cunha, Margarida S., de Moura, Bruno Lustosa, Yu, Jie, Huber, Daniel, Ou, Jian-wen, Wittenmyer, Robert A., Gizon, Laurent, and Chaplin, William J.
Abstract: The Transiting Exoplanet Survey Satellite (TESS) mission searches for new exoplanets. The observing strategy of TESS results in high-precision photometry of millions of stars across the sky, allowing for detailed asteroseismic studies of individual systems. In this work, we present a detailed asteroseismic analysis of the giant star HD 76920 hosting a highly eccentric giant planet ($e = 0.878$) with an orbital period of 415 days, using 5 sectors of TESS light curve that cover around 140 days of data. Solar-like oscillations in HD 76920 are detected around $52 \, \mu$Hz by TESS for the first time. By utilizing asteroseismic modeling that takes classical observational parameters and stellar oscillation frequencies as constraints, we determine improved measurements of the stellar mass ($1.22 \pm 0.11\, M_\odot$), radius ($8.68 \pm 0.34\,R_\odot$), and age ($5.2 \pm 1.4\,$Gyr). With the updated parameters of the host star, we update the semi-major axis and mass of the planet as $a=1.165 \pm 0.035$ au and $M_{\rm p}\sin{i} = 3.57 \pm 0.22\,M_{\rm Jup}$. With an orbital pericenter of $0.142 \pm 0.005$ au, we confirm that the planet is currently far away enough from the star to experience negligible tidal decay until being engulfed in the stellar envelope. We also confirm that this event will occur within about 100\,Myr, depending on the stellar model used., Comment: 18 pages, 7 figures, 4 tables
Published: 2023
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9. Multi-epoch detections of the extended atmosphere and transmission spectra of KELT-9b with a 1.5 m telescope

Author: Lowson, Nataliea, Zhou, George, Wright, Duncan J., Huang, Chelsea X., Mendonca, Joao M., Cabot, Samuel H. C., Pudmenzky, Christa, Wittenmyer, Robert A., Latham, David W., Bieryla, Allyson, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., Lowson, Nataliea, Zhou, George, Wright, Duncan J., Huang, Chelsea X., Mendonca, Joao M., Cabot, Samuel H. C., Pudmenzky, Christa, Wittenmyer, Robert A., Latham, David W., Bieryla, Allyson, Esquerdo, Gilbert A., Berlind, Perry, and Calkins, Michael L.
Abstract: Irradiated Jovian atmospheres are complex, dynamic, and can undergo temporal variations due to the close proximity of their parent stars. Of the Jovian planets that have been catalogued to date, KELT-9b is the hottest Gas Giant known, with an equilibrium temperature of 4050 K. We probe the temporal variability of transmission spectroscopic signatures from KELT-9b via a set of archival multi-year ground-based transit observations, performed with the TRES facility on the 1.5 m reflector at the Fred Lawrence Whipple Observatory. Our observations confirm past detections of Fe I, Fe II and Mg I over multiple epochs, in addition to excess absorption at H-alpha, which is an indicator for ongoing mass-loss. From our multi-year dataset, the H-alpha light curve consistently deviates from a standard transit, and follows a 'W' shape that is deeper near ingress and egress, and shallower mid-transit. To search for and quantify any seasonal variations that may be present, we parameterise a 'cometary tail' model to fit for the H-alpha transit. We find no detectable variations between the different observed epochs. Though a 'cometary tail' describes the H-alpha flux variations well, we note that such a scenario requires a high density of neutral hydrogen in the n = 2 excited state far beyond the planetary atmosphere. Other scenarios, such as centre-to-limb variations larger than that expected from 1-D atmosphere models, may also contribute to the observed H-alpha transit shape. These multi-epoch observations highlight the capabilities of small telescopes to provide temporal monitoring of the dynamics of exoplanet atmospheres., Comment: 19 pages, 11 figures, accepted for publication in AJ
Published: 2023
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10. 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

11. Flares, Rotation, and Planets of the AU Mic System from TESS Observations

Author: Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Gilbert, Emily A, Barclay, Thomas, Quintana, Elisa V, Walkowicz, Lucianne M, Vega, Laura D, Schlieder, Joshua E, Monsue, Teresa, Cale, Bryson L, Collins, Kevin I, Gaidos, Eric, El Mufti, Mohammed, Reefe, Michael A, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A, Wittrock, Justin M, Jenkins, Jon M, Latham, David W, Ricker, George R, Rose, Mark E, Seager, S, Vanderspek, Roland K, Winn, Joshua N, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Gilbert, Emily A, Barclay, Thomas, Quintana, Elisa V, Walkowicz, Lucianne M, Vega, Laura D, Schlieder, Joshua E, Monsue, Teresa, Cale, Bryson L, Collins, Kevin I, Gaidos, Eric, El Mufti, Mohammed, Reefe, Michael A, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A, Wittrock, Justin M, Jenkins, Jon M, Latham, David W, Ricker, George R, Rose, Mark E, Seager, S, Vanderspek, Roland K, and Winn, Joshua N
Abstract: Abstract AU Mic is a young (∼24 Myr), pre-main-sequence M dwarf star that was observed in the first month of science observations of the Transiting Exoplanet Survey Satellite (TESS) and reobserved 2 years later. This target has photometric variability from a variety of sources that is readily apparent in the TESS light curves; spots induce modulation in the light curve, flares are present throughout (manifesting as sharp rises with slow exponential decay phases), and transits of AU Mic b may be seen by eye as dips in the light curve. We present a combined analysis of both TESS Sector 1 and Sector 27 AU Mic light curves including the new 20 s cadence data from TESS Year 3. We compare flare rates between both observations and analyze the spot evolution, showing that the activity levels increase slightly from Sector 1 to Sector 27. Furthermore, the 20 s data collection allows us to detect more flares, smaller flares, and better resolve flare morphology in white light as compared to the 2 minute data collection mode. We also refine the parameters for AU Mic b by fitting three additional transits of AU Mic b from Sector 27 using a model that includes stellar activity. We show that the transits exhibit clear transit timing variations with an amplitude of ∼80 s. We also detect three transits of a 2.8 R ⊕ planet, AU Mic c, which has a period of 18.86 days.
Published: 2023

12. 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

13. 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

14. HD 83443c: A highly eccentric giant planet on a 22-year orbit

Author: Errico, Adriana, Wittenmyer, Robert A., Horner, Jonathan, Li, Zhexing, Brandt, Gregory Mirek, Kane, Stephen R., Fetherolf, Tara, Holt, Timothy R., Carter, Brad, Butler, Jake T. Clark. Robert . P., Tinney, Chris G., Ballard, Sarah, Bowler, Brendan P., Kielkopf, John, Liu, Huigen, Plavchan, Peter P., Shporer, Avi, Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Errico, Adriana, Wittenmyer, Robert A., Horner, Jonathan, Li, Zhexing, Brandt, Gregory Mirek, Kane, Stephen R., Fetherolf, Tara, Holt, Timothy R., Carter, Brad, Butler, Jake T. Clark. Robert . P., Tinney, Chris G., Ballard, Sarah, Bowler, Brendan P., Kielkopf, John, Liu, Huigen, Plavchan, Peter P., Shporer, Avi, Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Abstract: We report the discovery of a highly eccentric long-period Jovian planet orbiting the hot-Jupiter host HD\,83443. By combining radial velocity data from four instruments (AAT/UCLES, Keck/HIRES, HARPS, Minerva-Australis) spanning more than two decades, we find evidence for a planet with m~sin~$i=1.35^{+0.07}_{-0.06}$\,\mj, moving on an orbit with $a=8.0\pm$0.8\,au and eccentricity $e=0.76\pm$0.05. We combine our radial velocity analysis with \textit{Gaia} eDR3 /\textit{Hipparcos} proper motion anomalies and derive a dynamical mass of $1.5^{+0.5}_{-0.2} M_{\rm Jup}$. We perform a detailed dynamical simulation that reveals locations of stability within the system that may harbor additional planets, including stable regions within the habitable zone of the host star. HD\,83443 is a rare example of a system hosting a hot Jupiter and an exterior planetary companion. The high eccentricity of HD\,83443c suggests that a scattering event may have sent the hot Jupiter to its close orbit while leaving the outer planet on a wide and eccentric path.
Published: 2022

15. Precise radial velocities of giant stars XVI. Planet occurrence rates from the combined analysis of the Lick, EXPRESS, and PPPS giant star surveys

Author: Wolthoff, Vera, Reffert, Sabine, Quirrenbach, Andreas, Jones, Matías I., Wittenmyer, Robert A., Jenkins, James S., Wolthoff, Vera, Reffert, Sabine, Quirrenbach, Andreas, Jones, Matías I., Wittenmyer, Robert A., and Jenkins, James S.
Abstract: RV surveys of evolved stars allow us to probe a higher stellar mass range compared to main-sequence samples. Differences between the planet populations can be caused by either the differing stellar mass or stellar evolution. To properly disentangle the effects of both, the planet population around giant stars needs to be characterized as accurately as possible. Our goal is to investigate the giant planet occurrence rate around evolved stars and determine its dependence on stellar mass, metallicity, and orbital period. We combine data from the Lick, EXPRESS, and PPPS giant star surveys, yielding a sample of 482 evolved stars and 37 planets. We homogeneously rederived the stellar parameters and accounted for varying observational coverage, precision, and stellar noise properties by computing detection maps via injection and retrieval of synthetic planetary signals. We then computed occurrence rates as a function of period, stellar mass, and metallicity, corrected for incompleteness. Our findings agree with previous studies that found a positive planet-metallicity correlation for evolved stars and identified a peak in the occurrence rate as a function of stellar mass, but our results place it at a slightly smaller mass of 1.68Msun. The period dependence of the occurrence rate seems to follow a broken power-law or log-normal peaking at 700-800 days, roughly corresponding to 1.6AU for a 1Msun star and 2.0AU for a 2Msun star. This peak could be a remnant from halted migration around intermediate-mass stars, caused by stellar evolution, or an artifact from contamination by false positives. The global occurrence rate of giant planetary systems is 10.7% for the entire sample, while the subsets of RGB and HB stars exhibit 14.2% and 6.6%, respectively. However, we demonstrate that the different stellar mass distributions suffice to explain the apparent change of occurrence with evolutionary stage., Comment: 17 pages, 13 figures, accepted for publication in A&A
Published: 2022

16. Combined APOGEE-GALAH stellar catalogues using the Cannon

Author: Nandakumar, Govind, Hayden, Michael R., Sharma, Sanjib, Buder, Sven, Asplund, Martin, Bland-Hawthorn, Joss, De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Martell, Sarah L., Schlesinger, Katharine J., Lin, Jane, Simpson, Jeffrey D., Zucker, Daniel B., Zwitter, Tomaž, Nordlander, Thomas, Casagrande, Luca, Lind, Karin, Côtar, Klemen, Stello, Dennis, Wittenmyer, Robert A., Tepper-Garcia, Thor, Nandakumar, Govind, Hayden, Michael R., Sharma, Sanjib, Buder, Sven, Asplund, Martin, Bland-Hawthorn, Joss, De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Martell, Sarah L., Schlesinger, Katharine J., Lin, Jane, Simpson, Jeffrey D., Zucker, Daniel B., Zwitter, Tomaž, Nordlander, Thomas, Casagrande, Luca, Lind, Karin, Côtar, Klemen, Stello, Dennis, Wittenmyer, Robert A., and Tepper-Garcia, Thor
Abstract: APOGEE and GALAH are two high resolution multi-object spectroscopic surveys that provide fundamental stellar parameters and multiple elemental abundance estimates for about half a million stars in the Milky Way. Both surveys observe in different wavelength regimes and use different data reduction pipelines leading to significant offsets and trends in stellar parameters and abundances for the common stars observed in both surveys. Such systematic differences/offsets in stellar parameters and abundances make it difficult to effectively utilize them to investigate Galactic abundance trends in spite of the unique advantage provided by their complementary sky coverage and different Milky Way components they observe. Hence, we use the Cannon data-driven method selecting a training set of 4418 common stars observed by both surveys. This enables the construction of two catalogues, one with the APOGEE-scaled and the other with the GALAH-scaled stellar parameters. Using repeat observations in APOGEE and GALAH, we find high precision in metallicity (∼0.02–0.4 dex) and alpha abundances (∼0.02–0.03 dex) for spectra with good signal-to-noise ratio (SNR > 80 for APOGEE and SNR > 40 for GALAH). We use open and globular clusters to validate our parameter estimates and find small scatter in metallicity (0.06 dex) and alpha abundances (0.03 dex) in APOGEE-scaled case. The final catalogues have been cross-matched with the Gaia EDR3 catalogue to enable their use to carry out detailed chemo-dynamic studies of the Milky Way from perspectives of APOGEE and GALAH.
Published: 2022
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17. The GALAH Survey : improving our understanding of confirmed and candidate planetary systems with large stellar surveys

Author: Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, Nordlander, Thomas, Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, and Nordlander, Thomas
Abstract: Pioneering photometric, astrometric, and spectroscopic surveys is helping exoplanetary scientists better constrain the fundamental properties of stars within our galaxy and the planets these stars host. In this study, we use the third data release from the stellar spectroscopic GALAH Survey, coupled with astrometric data of eDR3 from the Gaia satellite, and other data from NASA's Exoplanet Archive, to refine our understanding of 279 confirmed and candidate exoplanet host stars and their exoplanets. This homogenously analysed data set comprises 105 confirmed exoplanets, along with 146 K2 candidates, 95 TESS Objects of Interest (TOIs), and 52 Community TOIs (CTOIs). Our analysis significantly shifts several previously (unknown) planet parameters while decreasing the uncertainties for others. Our radius estimates suggest that 35 planet candidates are more likely brown dwarfs or stellar companions due to their new radius values. We are able to refine the radii and masses of WASP-47 e, K2-106 b, and CoRoT-7 b to their most precise values yet to less than 2.3 per cent and 8.5 per cent, respectively. We also use stellar rotational values from GALAH to show that most planet candidates will have mass measurements that will be tough to obtain with current ground-based spectrographs. With GALAH's chemical abundances, we show through chemo-kinematics that there are five planet hosts that are associated with the galaxy's thick disc, including NGTS-4, K2-183, and K2-337. Finally, we show that there is no statistical difference between the chemical properties of hot Neptune and hot rocky exoplanet hosts, with the possibility that short-period rocky worlds might be the remnant cores of hotter, gaseous worlds.
Published: 2022
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18. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author: Clark, Jake, Addison, Brett, Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph, Wright, Duncan, Clerte, Mathieu, Brown, Carolyn, Fetherolf, Tara, Wittenmyer, Robert, Plavchan, Peter, Kane, Stephen, Horner, Jonathan, Kielkopf, John, Shporer, Avi, Tinney, C., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan, Mengel, Matthew, Zhou, George, Lee, Annette, David, Avelyn, Heim, Jessica, Lee, Michele, Sevilla, Veronica, Zafar, Naqsh, Hinkel, Natalie, Allen, Bridgette, Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward, Christiansen, Jessie, Ciardi, David, Ciardi, Krys, Collins, Karen, Dallant, Jules, Davis, Allen, Diaz, Matias, Dressing, Courtney, Esquerdo, Gilbert, Harre, Jan-Vincent, Howell, Steve, Jenkins, Jon, Jensen, Eric, Jones, Matias, Jordan, Andres, Latham, David, Lund, Michael, McCormac, James, Nielsen, Louise, Otegi, Jon, Quinn, Samuel, Radford, Don, Ricker, George, Schwarz, Richard, Seager, Sara, Smith, Alexis, Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephane, Vanderspek, Roland, Gunther, Maximilian, Wang, Songhu, Wingham, Geof, Winn, Joshua, Clark, Jake, Addison, Brett, Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph, Wright, Duncan, Clerte, Mathieu, Brown, Carolyn, Fetherolf, Tara, Wittenmyer, Robert, Plavchan, Peter, Kane, Stephen, Horner, Jonathan, Kielkopf, John, Shporer, Avi, Tinney, C., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan, Mengel, Matthew, Zhou, George, Lee, Annette, David, Avelyn, Heim, Jessica, Lee, Michele, Sevilla, Veronica, Zafar, Naqsh, Hinkel, Natalie, Allen, Bridgette, Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward, Christiansen, Jessie, Ciardi, David, Ciardi, Krys, Collins, Karen, Dallant, Jules, Davis, Allen, Diaz, Matias, Dressing, Courtney, Esquerdo, Gilbert, Harre, Jan-Vincent, Howell, Steve, Jenkins, Jon, Jensen, Eric, Jones, Matias, Jordan, Andres, Latham, David, Lund, Michael, McCormac, James, Nielsen, Louise, Otegi, Jon, Quinn, Samuel, Radford, Don, Ricker, George, Schwarz, Richard, Seager, Sara, Smith, Alexis, Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephane, Vanderspek, Roland, Gunther, Maximilian, Wang, Songhu, Wingham, Geof, and Winn, Joshua
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 ($v\sin{(i)}= 35.1\pm1.0$km/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 $2.76^{+0.24}_{-0.23}$Mjup, $1.370\pm0.043$Rjup and $\sim4.63$ days, respectively. The planet orbits a bright ($V = 9.1$mag) F3-dwarf with $M=1.40\pm0.05$Msun, $R=1.70\pm0.05$Rsun, and $\log g=4.05\pm0.17$. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of $18^{\circ}\pm11^{\circ}$, 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., Comment: 18 pages, 9 figures, and 4 tables. Submitted to the Astronomical Journal
Published: 2022
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19. A dense mini-Neptune orbiting the bright young star HD 18599

Author: Vines, Jose I., Jenkins, James S., Berdiñas, Zaira, Soto, Maritza G., Díaz, Matías R., Alves, Douglas R., Tuomi, Mikko, Wittenmyer, Robert A., de Leon, Jerome Pitogo, Peña, Pablo, Lissauer, Jack J., Ballard, Sarah, Bedding, Timothy, Bowler, Brendan P., Horner, Jonathan, Jones, Hugh R. A., Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Shporer, Avi, Tinney, C. G., Wright, Hui Zhang Duncan J., Addison, Brett, Mengel, Matthew W., Okumura, Jack, Samadi-Ghadim, Anya, Vines, Jose I., Jenkins, James S., Berdiñas, Zaira, Soto, Maritza G., Díaz, Matías R., Alves, Douglas R., Tuomi, Mikko, Wittenmyer, Robert A., de Leon, Jerome Pitogo, Peña, Pablo, Lissauer, Jack J., Ballard, Sarah, Bedding, Timothy, Bowler, Brendan P., Horner, Jonathan, Jones, Hugh R. A., Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Shporer, Avi, Tinney, C. G., Wright, Hui Zhang Duncan J., Addison, Brett, Mengel, Matthew W., Okumura, Jack, and Samadi-Ghadim, Anya
Abstract: Very little is known about the young planet population because the detection of small planets orbiting young stars is obscured by the effects of stellar activity and fast rotation which mask planets within radial velocity and transit data sets. The few planets that have been discovered in young clusters generally orbit stars too faint for any detailed follow-up analysis. Here we present the characterization of a new mini-Neptune planet orbiting the bright (V=9) and nearby K2 dwarf star, HD 18599. The planet candidate was originally detected in TESS light curves from Sectors 2, 3, 29, and 30, with an orbital period of 4.138~days. We then used HARPS and FEROS radial velocities, to find the companion mass to be 25.5$\pm$4.6~M$_\oplus$. When we combine this with the measured radius from TESS, of 2.70$\pm$0.05~R$_\oplus$, we find a high planetary density of 7.1$\pm$1.4~g cm$^{-3}$. The planet exists on the edge of the Neptune Desert and is the first young planet (300 Myr) of its type to inhabit this region. Structure models argue for a bulk composition to consist of 23% H$_2$O and 77% Rock and Iron. Future follow-up with large ground- and space-based telescopes can enable us to begin to understand in detail the characteristics of young Neptunes in the galaxy., Comment: Accepted in MNRAS
Published: 2022
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20. A sub-Neptune transiting the young field star HD 18599 at 40 pc

Author: de Leon, Jerome P., Livingston, John H., Jenkins, James S., Vines, Jose I., Wittenmyer, Robert A., Clark, Jake T., Winn, Joshua I. M., Addison, Brett, Ballard, Sarah, Bayliss, Daniel, Beichman, Charles, Benneke, Björn, Berardo, David Anthony, Bowler, Brendan P., Brown, Tim, Bryant, Edward M., Christiansen, Jessie, Ciardi, David, Collins, Karen A., Collins, Kevin I., Crossfield, Ian, Deming, Drake, Dragomir, Diana, Dressing, Courtney D., Fukui, Akihiko, Gan, Tianjun, Giacalone, Steven, Gill, Samuel, Alvarez, Erica Gonz\' alez, Hesse, Katharine, Horner, Jonathan, Howell, Steve B., Jenkins, Jon M., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kreidberg, Laura, Latham, David W., Liu, Huigen, Lund, Michael B., Matson, Rachel, Matthews, Elisabeth, Mengel, Matthew W., Morales, Farisa, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Okumura, Jack, Plavchan, Peter, Quinn, Sam, Rabus, Markus, Ricker, George, Rudat, Alexander, Schlieder, Joshua, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Smith, Alexis M. S., Sphorer, Avi, Stassun, Keivan, Tamura, Motohide, Tan, Thiam Guan, Tinney, C. G., Vanderspek, Roland, Gorjian, Varoujan, Werner, Michael W., West, Richard G., Wright, Duncan, Zhang, Hui, Zhou, George, de Leon, Jerome P., Livingston, John H., Jenkins, James S., Vines, Jose I., Wittenmyer, Robert A., Clark, Jake T., Winn, Joshua I. M., Addison, Brett, Ballard, Sarah, Bayliss, Daniel, Beichman, Charles, Benneke, Björn, Berardo, David Anthony, Bowler, Brendan P., Brown, Tim, Bryant, Edward M., Christiansen, Jessie, Ciardi, David, Collins, Karen A., Collins, Kevin I., Crossfield, Ian, Deming, Drake, Dragomir, Diana, Dressing, Courtney D., Fukui, Akihiko, Gan, Tianjun, Giacalone, Steven, Gill, Samuel, Alvarez, Erica Gonz\' alez, Hesse, Katharine, Horner, Jonathan, Howell, Steve B., Jenkins, Jon M., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kreidberg, Laura, Latham, David W., Liu, Huigen, Lund, Michael B., Matson, Rachel, Matthews, Elisabeth, Mengel, Matthew W., Morales, Farisa, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Okumura, Jack, Plavchan, Peter, Quinn, Sam, Rabus, Markus, Ricker, George, Rudat, Alexander, Schlieder, Joshua, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Smith, Alexis M. S., Sphorer, Avi, Stassun, Keivan, Tamura, Motohide, Tan, Thiam Guan, Tinney, C. G., Vanderspek, Roland, Gorjian, Varoujan, Werner, Michael W., West, Richard G., Wright, Duncan, Zhang, Hui, and Zhou, George
Abstract: Transiting exoplanets orbiting young nearby stars are ideal laboratories for testing theories of planet formation and evolution. However, to date only a handful of stars with age <1 Gyr have been found to host transiting exoplanets. Here we present the discovery and validation of a sub-Neptune around HD 18599, a young (300 Myr), nearby (d=40 pc) K star. We validate the transiting planet candidate as a bona fide planet using data from the TESS, Spitzer, and Gaia missions, ground-based photometry from IRSF, LCO, PEST, and NGTS, speckle imaging from Gemini, and spectroscopy from CHIRON, NRES, FEROS, and Minerva-Australis. The planet has an orbital period of 4.13 d, and a radius of 2.7Rearth. The RV data yields a 3-sigma mass upper limit of 30.5Mearth which is explained by either a massive companion or the large observed jitter typical for a young star. The brightness of the host star (V~9 mag) makes it conducive to detailed characterization via Doppler mass measurement which will provide a rare view into the interior structure of young planets., Comment: submitted to MNRAS
Published: 2022
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21. 3-D selection of 167 sub-stellar companions to nearby stars

Author: Feng, Fabo, Butler, R. Paul, Vogt, Steven S., Clement, Matthew S., Tinney, C. G., Cui, Kaiming, Aizawa, Masataka, Jones, Hugh R. A., Bailey, J., Burt, Jennifer, Carter, B. D., Crane, Jeffrey D., Dotti, Francesco Flammini, Holden, Bradford, Ma, Bo, Ogihara, Masahiro, Oppenheimer, Rebecca, O'Toole, S. J., Shectman, Stephen A., Wittenmyer, Robert A., Wang, Sharon X., Wright, D. J., Xuan, Yifan, Feng, Fabo, Butler, R. Paul, Vogt, Steven S., Clement, Matthew S., Tinney, C. G., Cui, Kaiming, Aizawa, Masataka, Jones, Hugh R. A., Bailey, J., Burt, Jennifer, Carter, B. D., Crane, Jeffrey D., Dotti, Francesco Flammini, Holden, Bradford, Ma, Bo, Ogihara, Masahiro, Oppenheimer, Rebecca, O'Toole, S. J., Shectman, Stephen A., Wittenmyer, Robert A., Wang, Sharon X., Wright, D. J., and Xuan, Yifan
Abstract: We analyze 5108 AFGKM stars with at least five high precision radial velocity points as well as Gaia and Hipparcos astrometric data utilizing a novel pipeline developed in previous work. We find 914 radial velocity signals with periods longer than 1000\,d. Around these signals, 167 cold giants and 68 other types of companions are identified by combined analyses of radial velocity, astrometry, and imaging data. Without correcting for detection bias, we estimate the minimum occurrence rate of the wide-orbit brown dwarfs to be 1.3\%, and find a significant brown dwarf valley around 40 $M_{\rm Jup}$. We also find a power-law distribution in the host binary fraction beyond 3 au similar to that found for single stars, indicating no preference of multiplicity for brown dwarfs. Our work also reveals nine sub-stellar systems (GJ 234 B, GJ 494 B, HD 13724 b, HD 182488 b, HD 39060 b and c, HD 4113 C, HD 42581 d, HD 7449 B, and HD 984 b) that have previously been directly imaged, and many others that are observable at existing facilities. Depending on their ages we estimate that an additional 10-57 sub-stellar objects within our sample can be detected with current imaging facilities, extending the imaged cold (or old) giants by an order of magnitude., Comment: 39 pages, 14 figures, 5 tables, published in The Astrophysical Journal Supplement Series
Published: 2022
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22. TOI-4562 b: A highly eccentric temperate Jupiter analog orbiting a young field star

Author: Heitzmann, Alexis, Zhou, George, Quinn, Samuel N., Huang, Chelsea X., Dong, Jiayin, Bouma, Luke G., Dawson, Rebekah I., Marsden, Stephen C., Wright, Duncan, Petit, Pascal, Collins, Karen A., Barkaoui, Khalid, Wittenmyer, Robert A., Gillen, Edward, Brahm, Rafael, Hobson, Melissa, Hellier, Coel, Ziegler, Carl, Briceño, César, Law, Nicholas, Mann, Andrew W., Howell, Steve B., Gnilka, Crystal L., Littlefield, Colin, Latham, David W., Lissauer, Jack J., Newton, Elisabeth R., Krolikowski, Daniel M., Kerr, Ronan, Rampalli, Rayna, Douglas, Stephanie T., Eisner, Nora L., Guedj, Nathalie, Sun, Guoyou, Smit, Martin, Huten, Marc, Eschweiler, Thorsten, Abe, Lyu, Guillot, Tristan, Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Winn, Joshua N., Ciardi, David R., Vanderburg, Andrew M., Burke, Christopher J., Rodriguez, David R., Daylan, Tansu, Heitzmann, Alexis, Zhou, George, Quinn, Samuel N., Huang, Chelsea X., Dong, Jiayin, Bouma, Luke G., Dawson, Rebekah I., Marsden, Stephen C., Wright, Duncan, Petit, Pascal, Collins, Karen A., Barkaoui, Khalid, Wittenmyer, Robert A., Gillen, Edward, Brahm, Rafael, Hobson, Melissa, Hellier, Coel, Ziegler, Carl, Briceño, César, Law, Nicholas, Mann, Andrew W., Howell, Steve B., Gnilka, Crystal L., Littlefield, Colin, Latham, David W., Lissauer, Jack J., Newton, Elisabeth R., Krolikowski, Daniel M., Kerr, Ronan, Rampalli, Rayna, Douglas, Stephanie T., Eisner, Nora L., Guedj, Nathalie, Sun, Guoyou, Smit, Martin, Huten, Marc, Eschweiler, Thorsten, Abe, Lyu, Guillot, Tristan, Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Winn, Joshua N., Ciardi, David R., Vanderburg, Andrew M., Burke, Christopher J., Rodriguez, David R., and Daylan, Tansu
Abstract: We report the discovery of TOI-4562 b (TIC-349576261), a Jovian planet orbiting a young F7V-type star, younger than the Praesepe/Hyades clusters (< $700$ Myr). This planet stands out because of its unusually long orbital period for transiting planets with known masses ($P_{\mathrm{orb}}$ = $225.11781^{+0.00025}_{-0.00022}$ days), and because it has a substantial eccentricity ($e$ = $0.76^{+0.02}_{-0.02}$). The location of TOI-4562 near the southern continuous viewing zone of TESS allowed observations throughout 25 sectors, enabling an unambiguous period measurement from TESS alone. Alongside the four available TESS transits, we performed follow-up photometry using the South African Astronomical Observatory node of the Las Cumbres Observatory, and spectroscopy with the CHIRON spectrograph on the 1.5 m SMARTS telescope. We measure a radius of $1.118_{+0.013}^{-0.014}$ $R_{\mathrm{J}}$ and a mass of $2.30^{+0.48}_{-0.47}$ $M_{\mathrm{J}}$ for TOI-4562 b. The radius of the planet is consistent with contraction models describing the early evolution of the size of giant planets. We detect tentative transit timing variations at the $\sim$ 20 min level from five transit events, favouring the presence of a companion that could explain the dynamical history of this system if confirmed by future follow-up observations. With its current orbital configuration, tidal timescales are too long for TOI-4562 b to become a hot-Jupiter via high eccentricity migration, though it is not excluded that interactions with the possible companion could modify TOI-4562 b eccentricity and trigger circularization. The characterisation of more such young systems is essential to set constraints on models describing giant planet evolution., Comment: 24 pages, 12 figures, 4 tables. Accepted in The Astronomical Journal (24/01/2023)
Published: 2022
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23. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

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

Author: Yee, Samuel W., Winn, Joshua N., Hartman, Joel D., Rodriguez, Joseph E., Zhou, George, Quinn, Samuel N., Latham, David W., Bieryla, Allyson, Collins, Karen A., Addison, Brett C., Angelo, Isabel, Barkaoui, Khalid, Benni, Paul, Boyle, Andrew W., Brahm, Rafael, Butler, R. Paul, Ciardi, David R., Collins, Kevin I., Conti, Dennis M., Crane, Jeffrey D., Dai, Fei, Dressing, Courtney D., Eastman, Jason D., Essack, Zahra, Forés-Toribio, Raquel, Furlan, Elise, Gan, Tianjun, Giacalone, Steven, Gill, Holden, Girardin, Eric, Henning, Thomas, Henze, Christopher E., Hobson, Melissa J., Horner, Jonathan, Howard, Andrew W., Howell, Steve B., Huang, Chelsea X., Isaacson, Howard, Jenkins, Jon M., Jensen, Eric L. N., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Lasota, Slawomir, Levine, Alan M., Lubin, Jack, Mann, Andrew W., Massey, Bob, McLeod, Kim K., Mengel, Matthew W., Muñoz, Jose A., Murgas, Felipe, Palle, Enric, Plavchan, Peter, Popowicz, Adam, Radford, Don J., Ricker, George R., Rowden, Pamela, Safonov, Boris S., Savel, Arjun B., Schwarz, Richard P., Seager, S., Sefako, Ramotholo, Shporer, Avi, Srdoc, Gregor, Strakhov, Ivan S., Teske, Johanna K., Tinney, C. G., Tyler, Dakotah, Wittenmyer, Robert A., Zhang, Hui, Ziegler, Carl, Yee, Samuel W., Winn, Joshua N., Hartman, Joel D., Rodriguez, Joseph E., Zhou, George, Quinn, Samuel N., Latham, David W., Bieryla, Allyson, Collins, Karen A., Addison, Brett C., Angelo, Isabel, Barkaoui, Khalid, Benni, Paul, Boyle, Andrew W., Brahm, Rafael, Butler, R. Paul, Ciardi, David R., Collins, Kevin I., Conti, Dennis M., Crane, Jeffrey D., Dai, Fei, Dressing, Courtney D., Eastman, Jason D., Essack, Zahra, Forés-Toribio, Raquel, Furlan, Elise, Gan, Tianjun, Giacalone, Steven, Gill, Holden, Girardin, Eric, Henning, Thomas, Henze, Christopher E., Hobson, Melissa J., Horner, Jonathan, Howard, Andrew W., Howell, Steve B., Huang, Chelsea X., Isaacson, Howard, Jenkins, Jon M., Jensen, Eric L. N., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Lasota, Slawomir, Levine, Alan M., Lubin, Jack, Mann, Andrew W., Massey, Bob, McLeod, Kim K., Mengel, Matthew W., Muñoz, Jose A., Murgas, Felipe, Palle, Enric, Plavchan, Peter, Popowicz, Adam, Radford, Don J., Ricker, George R., Rowden, Pamela, Safonov, Boris S., Savel, Arjun B., Schwarz, Richard P., Seager, S., Sefako, Ramotholo, Shporer, Avi, Srdoc, Gregor, Strakhov, Ivan S., Teske, Johanna K., Tinney, C. G., Tyler, Dakotah, Wittenmyer, Robert A., Zhang, Hui, and Ziegler, Carl
Abstract: We report the discovery of ten short-period giant planets (TOI-2193A b, TOI-2207 b, TOI-2236 b, TOI-2421 b, TOI-2567 b, TOI-2570 b, TOI-3331 b, TOI-3540A b, TOI-3693 b, TOI-4137 b). All of the planets were identified as planet candidates based on periodic flux dips observed by NASA's Transiting Exoplanet Survey Satellite (TESS). The signals were confirmed to be from transiting planets using ground-based time-series photometry, high angular resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The ten newly discovered planets orbit relatively bright F and G stars ($G < 12.5$,~$T_\mathrm{eff}$ between 4800 and 6200 K). The planets' orbital periods range from 2 to 10~days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421 b is notable for being a Saturn-mass planet and TOI-2567 b for being a ``sub-Saturn'', with masses of $0.322\pm 0.073$ and $0.195\pm 0.030$ Jupiter masses, respectively. In most cases, we have little information about the orbital eccentricities. Two exceptions are TOI-2207 b, which has an 8-day period and a detectably eccentric orbit ($e = 0.17\pm0.05$), and TOI-3693 b, a 9-day planet for which we can set an upper limit of $e < 0.052$. The ten planets described here are the first new planets resulting from an effort to use TESS data to unify and expand on the work of previous ground-based transit surveys in order to create a large and statistically useful sample of hot Jupiters., Comment: 44 pages, 15 tables, 21 figures; revised version submitted to AJ
Published: 2022
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25. Another Shipment of Six Short-Period Giant Planets from TESS

Author: Rodriguez, Joseph E., Quinn, Samuel N., Vanderburg, Andrew, Zhou, George, Eastman, Jason D., Thygesen, Erica, Cale, Bryson, Ciardi, David R., Reed, Phillip A., Oelkers, Ryan J., Collins, Karen A., Bieryla, Allyson, Latham, David W., Gaudi, B. Scott, Hellier, Coel, Sokolovsky, Kirill, Schulte, Jack, Srdoc, Gregor, Kielkopf, John, Horta, Ferran Grau, Massey, Bob, Evans, Phil, Stephens, Denise C., McLeod, Kim K., Chazov, Nikita, Krushinsky, Vadim, Ghachoui, Mourad, Safonov, Boris, Dedrick, Cayla M., Conti, Dennis, Laloum, Didier, Giacalone, Steven, Ziegler, Carl, Serra, Pere Guerra, Nogues, Ramon Naves, Murgas, Felipe, Michaels, Edward J., Ricker, George R., Vanderspek, Roland K., Winn, Joshua N., Jenkins, Jon M., Addison, Brett, Alfaro, Owen, Anderson, D. R., Ayad, Elias, Bedding, Timothy, Belinsky, Alexandr A., Benkhaldoun, Zouhair, Berlind, Perry, Blake, Cullen H., Bowen, Michael J., Bowler, Brendan P., Boyle, Andrew W., Branson, Dalton, Briceno, Cesar, Calkins, Michael L., Campbell, Emma, Chomiuk, Laura, Collins, Kevin I., Cornachione, Matthew A., Daassou, Ahmed, Dressing, Courtney D., Esquerdo, Gilbert A., Feliz, Dax L., Fong, William, Gan, Tianjun, Gill, Holden, Goliguzova, Maria V., Hansen, Jarrod, Hintz, Eric G., Horner, Jonathan, Huang, Chelsea X., James, David J., Jensen, Jacob S., Johnson, Samson A., Kane, Stephen R., Barkaoui, Khalid, Kim, Myung-Jin, Kim, Kingsley, Kuhn, Rudolf B., Law, Nicholas, Lewin, Pablo, Liu, Huigen, Lund, Michael B., Mann, Andrew W., McCrady, Nate, Mengel, Matthew W., Mink, Jessica, Murphy, Lauren, Narita, Norio, Newman, Patrick, Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Palle, Enric, Pepper, Joshua, Plavchan, Peter, Popov, Alexander A., Rabus, Markus, Ranshaw, Jessica, Rodriguez, Jennifer, Roh, Dong-Goo, Reefe, Michael A, Savel, Arjun B., Schwarz, Richard P., Shporer, Avi, Siverd, Robert J., Sliski, David H., Stassun, Keivan G., Stevens, Daniel J., Soubkiou, Abderahmane, Ting, Eric B., Tinney, C. G., Vowell, Noah, Walton, Payton, West, R. G., Wilson, Maurice L., Wittenmyer, Robert A., Wittrock, Justin M., Wright, Jason T., Zhang, Hui, Zobel, Evan, Rodriguez, Joseph E., Quinn, Samuel N., Vanderburg, Andrew, Zhou, George, Eastman, Jason D., Thygesen, Erica, Cale, Bryson, Ciardi, David R., Reed, Phillip A., Oelkers, Ryan J., Collins, Karen A., Bieryla, Allyson, Latham, David W., Gaudi, B. Scott, Hellier, Coel, Sokolovsky, Kirill, Schulte, Jack, Srdoc, Gregor, Kielkopf, John, Horta, Ferran Grau, Massey, Bob, Evans, Phil, Stephens, Denise C., McLeod, Kim K., Chazov, Nikita, Krushinsky, Vadim, Ghachoui, Mourad, Safonov, Boris, Dedrick, Cayla M., Conti, Dennis, Laloum, Didier, Giacalone, Steven, Ziegler, Carl, Serra, Pere Guerra, Nogues, Ramon Naves, Murgas, Felipe, Michaels, Edward J., Ricker, George R., Vanderspek, Roland K., Winn, Joshua N., Jenkins, Jon M., Addison, Brett, Alfaro, Owen, Anderson, D. R., Ayad, Elias, Bedding, Timothy, Belinsky, Alexandr A., Benkhaldoun, Zouhair, Berlind, Perry, Blake, Cullen H., Bowen, Michael J., Bowler, Brendan P., Boyle, Andrew W., Branson, Dalton, Briceno, Cesar, Calkins, Michael L., Campbell, Emma, Chomiuk, Laura, Collins, Kevin I., Cornachione, Matthew A., Daassou, Ahmed, Dressing, Courtney D., Esquerdo, Gilbert A., Feliz, Dax L., Fong, William, Gan, Tianjun, Gill, Holden, Goliguzova, Maria V., Hansen, Jarrod, Hintz, Eric G., Horner, Jonathan, Huang, Chelsea X., James, David J., Jensen, Jacob S., Johnson, Samson A., Kane, Stephen R., Barkaoui, Khalid, Kim, Myung-Jin, Kim, Kingsley, Kuhn, Rudolf B., Law, Nicholas, Lewin, Pablo, Liu, Huigen, Lund, Michael B., Mann, Andrew W., McCrady, Nate, Mengel, Matthew W., Mink, Jessica, Murphy, Lauren, Narita, Norio, Newman, Patrick, Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Palle, Enric, Pepper, Joshua, Plavchan, Peter, Popov, Alexander A., Rabus, Markus, Ranshaw, Jessica, Rodriguez, Jennifer, Roh, Dong-Goo, Reefe, Michael A, Savel, Arjun B., Schwarz, Richard P., Shporer, Avi, Siverd, Robert J., Sliski, David H., Stassun, Keivan G., Stevens, Daniel J., Soubkiou, Abderahmane, Ting, Eric B., Tinney, C. G., Vowell, Noah, Walton, Payton, West, R. G., Wilson, Maurice L., Wittenmyer, Robert A., Wittrock, Justin M., Wright, Jason T., Zhang, Hui, and Zobel, Evan
Abstract: We present the discovery and characterization of six short-period, transiting giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS) -- TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), & TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9
Published: 2022
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26. A Mini-Neptune from TESS and CHEOPS Around the 120 Myr Old AB Dor member HIP 94235

Author: Zhou, George, Wirth, Christopher P., Huang, Chelsea X., Venner, Alexander, Franson, Kyle, Quinn, Samuel N., Bouma, L. G., Kraus, Adam L., Mann, Andrew W., Newton, Elisabeth. R., Dragomir, Diana, Heitzmann, Alexis, Lowson, Nataliea, Douglas, Stephanie T., Battley, Matthew, Gillen, Edward, Triaud, Amaury, Latham, David W., Howell, Steve B., Hartman, J. D., Tofflemire, Benjamin M., Wittenmyer, Robert A., Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Winn, Joshua N., Daylan, Tansu, Fausnaugh, Michael, Kunimoto, Michelle, Zhou, George, Wirth, Christopher P., Huang, Chelsea X., Venner, Alexander, Franson, Kyle, Quinn, Samuel N., Bouma, L. G., Kraus, Adam L., Mann, Andrew W., Newton, Elisabeth. R., Dragomir, Diana, Heitzmann, Alexis, Lowson, Nataliea, Douglas, Stephanie T., Battley, Matthew, Gillen, Edward, Triaud, Amaury, Latham, David W., Howell, Steve B., Hartman, J. D., Tofflemire, Benjamin M., Wittenmyer, Robert A., Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Winn, Joshua N., Daylan, Tansu, Fausnaugh, Michael, and Kunimoto, Michelle
Abstract: The TESS mission has enabled discoveries of the brightest transiting planet systems around young stars. These systems are the benchmarks for testing theories of planetary evolution. We report the discovery of a mini-Neptune transiting a bright star in the AB Doradus moving group. HIP 94235 (TOI-4399, TIC 464646604) is a Vmag=8.31 G-dwarf hosting a 3.00 -0.28/+0.32 Rearth mini-Neptune in a 7.7 day period orbit. HIP 94235 is part of the AB Doradus moving group, one of the youngest and closest associations. Due to its youth, the host star exhibits significant photometric spot modulation, lithium absorption, and X-ray emission. Three 0.06% transits were observed during Sector-27 of the TESS Extended Mission, though these transit signals are dwarfed by the 2% peak-to-peak photometric variability exhibited by the host star. Follow-up observations with CHEOPS confirmed the transit signal and prevented the erosion of the transit ephemeris. HIP 94235 is part of a 50 AU G-M binary system. We make use of diffraction limited observations spanning 11 years, and astrometric accelerations from Hipparchos and Gaia, to constrain the orbit of HIP 94235 B. HIP 94235 is one of the tightest stellar binaries to host an inner planet. As part of a growing sample of bright, young planet systems, HIP 94235 b is ideal for follow-up transit observations, such as those that investigate the evaporative processes driven by high-energy radiation that may sculpt the valleys and deserts in the Neptune population., Comment: Accepted for publication in AJ
Published: 2022
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27. HD 83443c: A highly eccentric giant planet on a 22-year orbit

Author: Errico, Adriana, Wittenmyer, Robert A., Horner, Jonathan, Li, Zhexing, Brandt, Gregory Mirek, Kane, Stephen R., Fetherolf, Tara, Holt, Timothy R., Carter, Brad, Butler, Jake T. Clark. Robert . P., Tinney, Chris G., Ballard, Sarah, Bowler, Brendan P., Kielkopf, John, Liu, Huigen, Plavchan, Peter P., Shporer, Avi, Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Errico, Adriana, Wittenmyer, Robert A., Horner, Jonathan, Li, Zhexing, Brandt, Gregory Mirek, Kane, Stephen R., Fetherolf, Tara, Holt, Timothy R., Carter, Brad, Butler, Jake T. Clark. Robert . P., Tinney, Chris G., Ballard, Sarah, Bowler, Brendan P., Kielkopf, John, Liu, Huigen, Plavchan, Peter P., Shporer, Avi, Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Abstract: We report the discovery of a highly eccentric long-period Jovian planet orbiting the hot-Jupiter host HD\,83443. By combining radial velocity data from four instruments (AAT/UCLES, Keck/HIRES, HARPS, Minerva-Australis) spanning more than two decades, we find evidence for a planet with m~sin~$i=1.35^{+0.07}_{-0.06}$\,\mj, moving on an orbit with $a=8.0\pm$0.8\,au and eccentricity $e=0.76\pm$0.05. We combine our radial velocity analysis with \textit{Gaia} eDR3 /\textit{Hipparcos} proper motion anomalies and derive a dynamical mass of $1.5^{+0.5}_{-0.2} M_{\rm Jup}$. We perform a detailed dynamical simulation that reveals locations of stability within the system that may harbor additional planets, including stable regions within the habitable zone of the host star. HD\,83443 is a rare example of a system hosting a hot Jupiter and an exterior planetary companion. The high eccentricity of HD\,83443c suggests that a scattering event may have sent the hot Jupiter to its close orbit while leaving the outer planet on a wide and eccentric path.
Published: 2022
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28. Precise radial velocities of giant stars XVI. Planet occurrence rates from the combined analysis of the Lick, EXPRESS, and PPPS giant star surveys

Author: Wolthoff, Vera, Reffert, Sabine, Quirrenbach, Andreas, Jones, Matías I., Wittenmyer, Robert A., Jenkins, James S., Wolthoff, Vera, Reffert, Sabine, Quirrenbach, Andreas, Jones, Matías I., Wittenmyer, Robert A., and Jenkins, James S.
Abstract: RV surveys of evolved stars allow us to probe a higher stellar mass range compared to main-sequence samples. Differences between the planet populations can be caused by either the differing stellar mass or stellar evolution. To properly disentangle the effects of both, the planet population around giant stars needs to be characterized as accurately as possible. Our goal is to investigate the giant planet occurrence rate around evolved stars and determine its dependence on stellar mass, metallicity, and orbital period. We combine data from the Lick, EXPRESS, and PPPS giant star surveys, yielding a sample of 482 evolved stars and 37 planets. We homogeneously rederived the stellar parameters and accounted for varying observational coverage, precision, and stellar noise properties by computing detection maps via injection and retrieval of synthetic planetary signals. We then computed occurrence rates as a function of period, stellar mass, and metallicity, corrected for incompleteness. Our findings agree with previous studies that found a positive planet-metallicity correlation for evolved stars and identified a peak in the occurrence rate as a function of stellar mass, but our results place it at a slightly smaller mass of 1.68Msun. The period dependence of the occurrence rate seems to follow a broken power-law or log-normal peaking at 700-800 days, roughly corresponding to 1.6AU for a 1Msun star and 2.0AU for a 2Msun star. This peak could be a remnant from halted migration around intermediate-mass stars, caused by stellar evolution, or an artifact from contamination by false positives. The global occurrence rate of giant planetary systems is 10.7% for the entire sample, while the subsets of RGB and HB stars exhibit 14.2% and 6.6%, respectively. However, we demonstrate that the different stellar mass distributions suffice to explain the apparent change of occurrence with evolutionary stage., Comment: 17 pages, 13 figures, accepted for publication in A&A
Published: 2022
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29. The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at $\approx$2 AU

Author: Zeng, Yunlin, Brandt, Timothy D., Li, Gongjie, Dupuy, Trent J., Li, Yiting, Brandt, G. Mirek, Farihi, Jay, Horner, Jonathan, Wittenmyer, Robert A., Butler, R. Paul., Tinney, Christopher G., Carter, Bradley D., Wright, Duncan J., Jones, Hugh R. A., O'Toole, Simon J., Zeng, Yunlin, Brandt, Timothy D., Li, Gongjie, Dupuy, Trent J., Li, Yiting, Brandt, G. Mirek, Farihi, Jay, Horner, Jonathan, Wittenmyer, Robert A., Butler, R. Paul., Tinney, Christopher G., Carter, Bradley D., Wright, Duncan J., Jones, Hugh R. A., and O'Toole, Simon J.
Abstract: Gliese 86 is a nearby K dwarf hosting a giant planet on a $\approx$16-day orbit and an outer white dwarf companion on a $\approx$century-long orbit. In this study we combine radial velocity data (including new measurements spanning more than a decade) with high angular resolution imaging and absolute astrometry from Hipparcos and Gaia to measure the current orbits and masses of both companions. We then simulate the evolution of the Gl 86 system to constrain its primordial orbit when both stars were on the main sequence; the closest approach between the two stars was then about $9\,$AU. Such a close separation limited the size of the protoplanetary disk of Gl 86 A and dynamically hindered the formation of the giant planet around it. Our measurements of Gl 86 B and Gl 86 Ab's orbits reveal Gl 86 as a system in which giant planet formation took place in a disk truncated at $\approx$2$\,$AU. Such a disk would be just big enough to harbor the dust mass and total mass needed to assemble Gl 86 Ab's core and envelope, assuming a high disk accretion rate and a low viscosity. Inefficient accretion of the disk onto Gl 86 Ab, however, would require a disk massive enough to approach the Toomre stability limit at its outer truncation radius. The orbital architecture of the Gl 86 system shows that giant planets can form even in severely truncated disks and provides an important benchmark for planet formation theory., Comment: 17 pages, 10 figures
Published: 2021

30. TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs

Author: Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Werner, Michael W., Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Werner, Michael W., Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Abstract: We validate the presence of a two-planet system orbiting the 0.2--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P = 6.397438 \pm 0.000037$ days, $e=0.294^{0.13}_{0.062}$) initially discovered in the Sector 8 \tess\ mission observations, and a transiting mini-Neptune (TOI 560 c, $P = 18.8779 \pm 0.0016$ days) discovered in the Sector 34 observations, in a rare 1:3 orbital resonance. We utilize photometric data from \tess\, \textit{Spitzer}, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets and vet false positive scenarios. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We place upper limits on the masses of both planets of $<$2.1 and $<$4.1 M$_{Nep}$ for b and c, respectively. We apply a Gaussian Processes (GP) model to the \tess\ light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by $<$6 hours before June 2027., Comment: AAS Journals, submitted
Published: 2021

31. TOI-1842b: A Transiting Warm Saturn Undergoing Re-Inflation around an Evolving Subgiant

Author: Wittenmyer, Robert A., Clark, Jake T., Trifonov, Trifon, Addison, Brett C., Wright, Duncan J., Stassun, Keivan G., Horner, Jonathan, Lowson, Nataliea, Kielkopf, John, Kane, Stephen R., Plavchan, Peter, Shporer, Avi, Zhang, Hui, Bowler, Brendan P., Mengel, Matthew W., Okumura, Jack, Rabus, Markus, Johnson, Marshall C., Harbeck, Daniel, Tronsgaard, Rene, Buchhave, Lars A., Collins, Karen A., Collins, Kevin I., Gan, Tianjun, Jensen, Eric L. N., Howell, Steve B., Furlan, E., Gnilka, Crystal L., Lester, Kathryn V., Matson, Rachel A., Scott, Nicholas J., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Rudat, Alexander, Quintana, Elisa V., Rodriguez, David R., Caldwell, Douglas A., Quinn, Samuel N., Essack, Zahra, Bouma, Luke G., Wittenmyer, Robert A., Clark, Jake T., Trifonov, Trifon, Addison, Brett C., Wright, Duncan J., Stassun, Keivan G., Horner, Jonathan, Lowson, Nataliea, Kielkopf, John, Kane, Stephen R., Plavchan, Peter, Shporer, Avi, Zhang, Hui, Bowler, Brendan P., Mengel, Matthew W., Okumura, Jack, Rabus, Markus, Johnson, Marshall C., Harbeck, Daniel, Tronsgaard, Rene, Buchhave, Lars A., Collins, Karen A., Collins, Kevin I., Gan, Tianjun, Jensen, Eric L. N., Howell, Steve B., Furlan, E., Gnilka, Crystal L., Lester, Kathryn V., Matson, Rachel A., Scott, Nicholas J., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Rudat, Alexander, Quintana, Elisa V., Rodriguez, David R., Caldwell, Douglas A., Quinn, Samuel N., Essack, Zahra, and Bouma, Luke G.
Abstract: The imminent launch of space telescopes designed to probe the atmospheres of exoplanets has prompted new efforts to prioritise the thousands of transiting planet candidates for follow-up characterisation. We report the detection and confirmation of TOI-1842b, a warm Saturn identified by TESS and confirmed with ground-based observations from Minerva-Australis, NRES, and the Las Cumbres Observatory Global Telescope. This planet has a radius of $1.04^{+0.06}_{-0.05}\,R_{Jup}$, a mass of $0.214^{+0.040}_{-0.038}\,M_{Jup}$, an orbital period of $9.5739^{+0.0002}_{-0.0001}$ days, and an extremely low density ($\rho$=0.252$\pm$0.091 g cm$^{-3}$). TOI-1842b has among the best known combinations of large atmospheric scale height (893 km) and host-star brightness ($J=8.747$ mag), making it an attractive target for atmospheric characterisation. As the host star is beginning to evolve off the main sequence, TOI-1842b presents an excellent opportunity to test models of gas giant re-inflation. The primary transit duration of only 4.3 hours also makes TOI-1842b an easily-schedulable target for further ground-based atmospheric characterisation., Comment: Accepted for publication in AJ
Published: 2021
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32. The GALAH Survey: Improving our understanding of confirmed and candidate planetary systems with large stellar surveys

Author: Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, Nordlander, Thomas, Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, and Nordlander, Thomas
Abstract: Pioneering photometric, astrometric, and spectroscopic surveys are helping exoplanetary scientists better constrain the fundamental properties of stars within our galaxy, and the planets these stars host. In this study, we use the third data release from the stellar spectroscopic GALAH Survey, coupled with astrometric data of eDR3 from the \textit{Gaia} satellite, and other data from NASA's Exoplanet Archive, to refine our understanding of 279 confirmed and candidate exoplanet host stars and their exoplanets. This homogenously analysed data set comprises 105 confirmed exoplanets, along with 146 K2 candidates, 95 TESS Objects of Interest (TOIs) and 52 Community TOIs (CTOIs). Our analysis significantly shifts several previously (unknown) planet parameters while decreasing the uncertainties for others; Our radius estimates suggest that 35 planet candidates are more likely brown dwarfs or stellar companions due to their new radius values. We are able to refine the radii and masses of WASP-47 e, K2-106 b, and CoRoT-7 b to their most precise values yet, to less than 2.3\% and 8.5\% respectively. We also use stellar rotational values from GALAH to show that most planet candidates will have mass measurements that will be tough to obtain with current ground-based spectrographs. With GALAH's chemical abundances, we show through chemo-kinematics that there are five planet-hosts that are associated with the galaxy's thick disc, including NGTS-4, K2-183 and K2-337. Finally, we show there is no statistical difference between the chemical properties of hot Neptune and hot rocky exoplanet hosts, with the possibility that short-period rocky worlds might be the remnant cores of hotter, gaseous worlds., Comment: 21 pages with 11 figures and 5 tables. Accepted into MNRAS with appendix tables available within this arXiv submission
Published: 2021
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33. Diving Beneath the Sea of Stellar Activity: Chromatic Radial Velocities of the Young AU Mic Planetary System

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

Author: Gilbert, Emily A., Barclay, Thomas, Quintana, Elisa V., Walkowicz, Lucianne M., Vega, Laura D., Schlieder, Joshua E., Monsue, Teresa, Cale, Bryson, Collins, Kevin I., Gaidos, Eric, Mufti, Mohammed El, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A., Wittrock, Justin M., Jenkins, Jon M., Latham, David W., Ricker, George R., Rose, Mark E., Seager, S., Vanderspek, Roland K., Winn, Joshua N., Gilbert, Emily A., Barclay, Thomas, Quintana, Elisa V., Walkowicz, Lucianne M., Vega, Laura D., Schlieder, Joshua E., Monsue, Teresa, Cale, Bryson, Collins, Kevin I., Gaidos, Eric, Mufti, Mohammed El, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A., Wittrock, Justin M., Jenkins, Jon M., Latham, David W., Ricker, George R., Rose, Mark E., Seager, S., Vanderspek, Roland K., and Winn, Joshua N.
Abstract: AU Mic is a young ($\sim$24 Myr), pre-Main Sequence M~dwarf star that was observed in the first month of science observations of the Transiting Exoplanet Survey Satellite (TESS) and re-observed two years later. This target has photometric variability from a variety of sources that is readily apparent in the TESS light curves; spots induce modulation in the light curve, flares are present throughout (manifesting as sharp rises with slow exponential decay phases), and transits of AU Mic b may be seen by eye as dips in the light curve. We present a combined analysis of both TESS Sector 1 and Sector 27 AU Mic light curves including the new 20-second cadence data from TESS Year 3. We compare flare rates between both observations and analyze the spot evolution, showing that the activity levels increase slightly from Sector 1 to Sector 27. Furthermore, the 20-second data collection allows us to detect more flares, smaller flares, and better resolve flare morphology in white light as compared to the 2-minute data collection mode. We also refine the parameters for AU Mic b by fitting three additional transits of AU Mic b from Sector 27 using a model that includes stellar activity. We show that the transits exhibit clear transit timing variations (TTVs) with an amplitude of $\sim$80 seconds. We also detect three transits of a 2.8 $R_\oplus$ planet, AU Mic c, which has a period of 18.86 days., Comment: 18 pages, 13 figures, 5 tables, accepted to AJ
Published: 2021
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35. TOI-3362b: A Proto-Hot Jupiter Undergoing High-Eccentricity Tidal Migration

Author: Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Rodriguez, Joseph E., Eastman, Jason D., Collins, Karen A., Quinn, Samuel N., Shporer, Avi, Triaud, Amaury H. M. J., Wang, Songhu, Beatty, Thomas, Jackson, Jonathon, Collins, Kevin I., Abe, Lyu, Suarez, Olga, Crouzet, Nicolas, MeKarnia, Djamel, Dransfield, Georgina, Jensen, Eric L. N., Stockdale, Chris, Barkaoui, Khalid, Heitzmann, Alexis, Wright, Duncan J., Addison, Brett C., Wittenmyer, Robert A., Okumura, Jack, Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Liu, Huigen, Plavchan, Peter, Mengel, Matthew W., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Christiansen, Jessie L., Paegert, Martin, Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Rodriguez, Joseph E., Eastman, Jason D., Collins, Karen A., Quinn, Samuel N., Shporer, Avi, Triaud, Amaury H. M. J., Wang, Songhu, Beatty, Thomas, Jackson, Jonathon, Collins, Kevin I., Abe, Lyu, Suarez, Olga, Crouzet, Nicolas, MeKarnia, Djamel, Dransfield, Georgina, Jensen, Eric L. N., Stockdale, Chris, Barkaoui, Khalid, Heitzmann, Alexis, Wright, Duncan J., Addison, Brett C., Wittenmyer, Robert A., Okumura, Jack, Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Liu, Huigen, Plavchan, Peter, Mengel, Matthew W., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Christiansen, Jessie L., and Paegert, Martin
Abstract: High-eccentricity tidal migration is a possible way for giant planets to be emplaced in short-period orbits. If it commonly operates, one would expect to catch proto-Hot Jupiters on highly elliptical orbits that are undergoing high-eccentricity tidal migration. As of yet, few such systems have been discovered. Here, we introduce TOI-3362b (TIC-464300749b), an 18.1-day, 5 $M_{\rm Jup}$ planet orbiting a main-sequence F-type star that is likely undergoing high-eccentricity tidal migration. The orbital eccentricity is 0.815$^{+0.023}_{-0.032}$. With a semi-major axis of 0.153$^{+0.002}_{-0.003}$ au, the planet's orbit is expected to shrink to a final orbital radius of 0.051$^{+0.008}_{-0.006}$ au after complete tidal circularization. Several mechanisms could explain the extreme value of the planet's eccentricity, such as planet-planet scattering and secular interactions. Such hypotheses can be tested with follow-up observations of the system, e.g., measuring the stellar obliquity and searching for companions in the system with precise, long-term radial velocity observations. The variation in the planet's equilibrium temperature as it orbits the host star and the tidal heating at periapse make this planet an intriguing target for atmospheric modeling and observation. Because the planet's orbital period of 18.1 days is near the limit of TESS's period sensitivity, even a few such discoveries suggest that proto-Hot Jupiters may be quite common., Comment: 14 pages, 4 figures, 2 tables. submitted to ApJL, revised in response to referee report
Published: 2021
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36. TOI-431/HIP 26013: a super-Earth and a sub-Neptune transiting a bright, early K dwarf, with a third RV planet

Author: Osborn, Ares, Armstrong, David J., Cale, Bryson, Brahm, Rafael, Wittenmyer, Robert A., Dai, Fei, Crossfield, Ian J. M., Bryant, Edward M., Adibekyan, Vardan, Cloutier, Ryan, Collins, Karen A., Mena, E. Delgado, Fridlund, Malcolm, Hellier, Coel, Howell, Steve B., King, George W., Lillo-Box, Jorge, Otegi, Jon, Sousa, S., Stassun, Keivan G., Matthews, Elisabeth C., Ziegler, Carl, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Acton, Jack S., Addison, Brett C., Anderson, David R., Ballard, Sarah, Barrado, David, Barros, Susana C. C., Batalha, Natalie, Bayliss, Daniel, Barclay, Thomas, Benneke, Björn, Berberian Jr., John, Bouchy, Francois, Bowler, Brendan P., Briceño, César, Burke, Christopher J., Burleigh, Matthew R., Casewell, Sarah L., Ciardi, David, Collins, Kevin I., Cooke, Benjamin F., Demangeon, Olivier D. S., Díaz, Rodrigo F., Dorn, C., Dragomir, Diana, Dressing, Courtney, Dumusque, Xavier, Espinoza, Néstor, Figueira, P., Fulton, Benjamin, Furlan, E., Gaidos, E., Geneser, C., Gill, Samuel, Goad, Michael R., Gonzales, Erica J., Gorjian, Varoujan, Günther, Maximilian N., Helled, Ravit, Henderson, Beth A., Henning, Thomas, Hogan, Aleisha, Hojjatpanah, Saeed, Horner, Jonathan, Howard, Andrew W., Hoyer, Sergio, Huber, Dan, Isaacson, Howard, Jenkins, James S., Jensen, Eric L. N., Jordán, Andrés, Kane, Stephen R., Kidwell Jr., Richard C., Kielkopf, John, Law, Nicholas, Lendl, Monika, Lund, M., Matson, Rachel A., Mann, Andrew W., McCormac, James, Mengel, Matthew W., Morales, Farisa Y., Nielsen, Louise D., Okumura, Jack, Osborn, Hugh P., Petigura, Erik A., Plavchan, Peter, Pollacco, Don, Quintana, Elisa V., Raynard, Liam, Robertson, Paul, Rose, Mark E., Roy, Arpita, Reefe, Michael, Santerne, Alexandre, Santos, Nuno C., Sarkis, Paula, Schlieder, J., Schwarz, Richard P., Scott, Nicholas J., Shporer, Avi, Smith, A. M. S., Stibbard, C., Stockdale, Chris, Strøm, Paul A., Twicken, Joseph D., Tan, Thiam-Guan, Tanner, A., Teske, J., Tilbrook, Rosanna H., Tinney, C. G., Udry, Stephane, Villaseñor, Jesus Noel, Vines, Jose I., Wang, Sharon X., Weiss, Lauren M., West, Richard G., Wheatley, Peter J., Wright, Duncan J., Zhang, Hui, Zohrabi, F., Osborn, Ares, Armstrong, David J., Cale, Bryson, Brahm, Rafael, Wittenmyer, Robert A., Dai, Fei, Crossfield, Ian J. M., Bryant, Edward M., Adibekyan, Vardan, Cloutier, Ryan, Collins, Karen A., Mena, E. Delgado, Fridlund, Malcolm, Hellier, Coel, Howell, Steve B., King, George W., Lillo-Box, Jorge, Otegi, Jon, Sousa, S., Stassun, Keivan G., Matthews, Elisabeth C., Ziegler, Carl, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Acton, Jack S., Addison, Brett C., Anderson, David R., Ballard, Sarah, Barrado, David, Barros, Susana C. C., Batalha, Natalie, Bayliss, Daniel, Barclay, Thomas, Benneke, Björn, Berberian Jr., John, Bouchy, Francois, Bowler, Brendan P., Briceño, César, Burke, Christopher J., Burleigh, Matthew R., Casewell, Sarah L., Ciardi, David, Collins, Kevin I., Cooke, Benjamin F., Demangeon, Olivier D. S., Díaz, Rodrigo F., Dorn, C., Dragomir, Diana, Dressing, Courtney, Dumusque, Xavier, Espinoza, Néstor, Figueira, P., Fulton, Benjamin, Furlan, E., Gaidos, E., Geneser, C., Gill, Samuel, Goad, Michael R., Gonzales, Erica J., Gorjian, Varoujan, Günther, Maximilian N., Helled, Ravit, Henderson, Beth A., Henning, Thomas, Hogan, Aleisha, Hojjatpanah, Saeed, Horner, Jonathan, Howard, Andrew W., Hoyer, Sergio, Huber, Dan, Isaacson, Howard, Jenkins, James S., Jensen, Eric L. N., Jordán, Andrés, Kane, Stephen R., Kidwell Jr., Richard C., Kielkopf, John, Law, Nicholas, Lendl, Monika, Lund, M., Matson, Rachel A., Mann, Andrew W., McCormac, James, Mengel, Matthew W., Morales, Farisa Y., Nielsen, Louise D., Okumura, Jack, Osborn, Hugh P., Petigura, Erik A., Plavchan, Peter, Pollacco, Don, Quintana, Elisa V., Raynard, Liam, Robertson, Paul, Rose, Mark E., Roy, Arpita, Reefe, Michael, Santerne, Alexandre, Santos, Nuno C., Sarkis, Paula, Schlieder, J., Schwarz, Richard P., Scott, Nicholas J., Shporer, Avi, Smith, A. M. S., Stibbard, C., Stockdale, Chris, Strøm, Paul A., Twicken, Joseph D., Tan, Thiam-Guan, Tanner, A., Teske, J., Tilbrook, Rosanna H., Tinney, C. G., Udry, Stephane, Villaseñor, Jesus Noel, Vines, Jose I., Wang, Sharon X., Weiss, Lauren M., West, Richard G., Wheatley, Peter J., Wright, Duncan J., Zhang, Hui, and Zohrabi, F.
Abstract: We present the bright (V$_{mag} = 9.12$), multi-planet system TOI-431, characterised with photometry and radial velocities. We estimate the stellar rotation period to be $30.5 \pm 0.7$ days using archival photometry and radial velocities. TOI-431b is a super-Earth with a period of 0.49 days, a radius of 1.28 $\pm$ 0.04 R$_{\oplus}$, a mass of $3.07 \pm 0.35$ M$_{\oplus}$, and a density of $8.0 \pm 1.0$ g cm$^{-3}$; TOI-431d is a sub-Neptune with a period of 12.46 days, a radius of $3.29 \pm 0.09$ R$_{\oplus}$, a mass of $9.90^{+1.53}_{-1.49}$ M$_{\oplus}$, and a density of $1.36 \pm 0.25$ g cm$^{-3}$. We find a third planet, TOI-431c, in the HARPS radial velocity data, but it is not seen to transit in the TESS light curves. It has an $M \sin i$ of $2.83^{+0.41}_{-0.34}$ M$_{\oplus}$, and a period of 4.85 days. TOI-431d likely has an extended atmosphere and is one of the most well-suited TESS discoveries for atmospheric characterisation, while the super-Earth TOI-431b may be a stripped core. These planets straddle the radius gap, presenting an interesting case-study for atmospheric evolution, and TOI-431b is a prime TESS discovery for the study of rocky planet phase curves., Comment: 21 pages, 11 figures, 3 appendices, accepted for publication in MNRAS
Published: 2021
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37. HD 183579b: A Warm Sub-Neptune Transiting a Solar Twin Detected by TESS

Author: Gan, Tianjun, Bedell, Megan, Wang, Sharon Xuesong, Foreman-Mackey, Daniel, Meléndez, Jorge, Mao, Shude, Stassun, Keivan G., Howell, Steve B., Ziegler, Carl, Wittenmyer, Robert A., Hellier, Coel, Collins, Karen A., Shporer, Avi, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Ballard, Sarah, Barclay, Thomas, Bean, Jacob L., Bowler, Brendan P., Briceño, César, Crossfield, Ian J. M., Dittman, Jason, Horner, Jonathan, Jensen, Eric L. N., Kane, Stephen R., Kielkopf, John, Kreidberg, Laura, Law, Nicholas, Mann, Andrew W., Mengel, Matthew W., Morgan, Edward H., Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Plavchan, Peter, Schwarz, Richard P., Shiao, Bernie, Smith, Jeffrey C., Spina, Lorenzo, Tinney, C. G., Torres, Guillermo, Twicken, Joseph D., Vezie, Michael, Wang, Gavin, Wright, Duncan J., Zhang, Hui, Gan, Tianjun, Bedell, Megan, Wang, Sharon Xuesong, Foreman-Mackey, Daniel, Meléndez, Jorge, Mao, Shude, Stassun, Keivan G., Howell, Steve B., Ziegler, Carl, Wittenmyer, Robert A., Hellier, Coel, Collins, Karen A., Shporer, Avi, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Ballard, Sarah, Barclay, Thomas, Bean, Jacob L., Bowler, Brendan P., Briceño, César, Crossfield, Ian J. M., Dittman, Jason, Horner, Jonathan, Jensen, Eric L. N., Kane, Stephen R., Kielkopf, John, Kreidberg, Laura, Law, Nicholas, Mann, Andrew W., Mengel, Matthew W., Morgan, Edward H., Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Plavchan, Peter, Schwarz, Richard P., Shiao, Bernie, Smith, Jeffrey C., Spina, Lorenzo, Tinney, C. G., Torres, Guillermo, Twicken, Joseph D., Vezie, Michael, Wang, Gavin, Wright, Duncan J., and Zhang, Hui
Abstract: We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright ($V=8.75$ mag, $K=7.15$ mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located $56.8\pm0.1$ pc away with a radius of $R_{\ast}=0.97\pm0.02\ R_{\odot}$ and a mass of $M_{\ast}=1.03\pm0.05\ M_{\odot}$. We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of $R_{p}=3.53\pm0.13\ R_{\oplus}$ on a $17.47$ day orbit with a mass of $M_{p}=11.2\pm5.4\ M_{\oplus}$ ($3\sigma$ mass upper limit of $27.4\ M_{\oplus}$). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin sample, without a statistically significant refractory element depletion., Comment: 20 pages, 15 figures, accepted for publication in MNRAS
Published: 2021
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38. TOI-1431b/MASCARA-5b: A Highly Irradiated Ultra-Hot Jupiter Orbiting One of the Hottest & Brightest Known Exoplanet Host Stars

Author: Addison, Brett Christopher, Knudstrup, Emil, Wong, Ian, Hebrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier, Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, Rene, Antoci, Victoria, Buchhave, Lars A., Gunther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hanse, Jens, Palle, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., McLean, Brian, Addison, Brett Christopher, Knudstrup, Emil, Wong, Ian, Hebrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier, Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, Rene, Antoci, Victoria, Buchhave, Lars A., Gunther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hanse, Jens, Palle, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., and McLean, Brian
Abstract: We present the discovery of a highly irradiated and moderately inflated ultra-hot Jupiter, TOI-1431b/MASCARA-5b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky CAmeRA (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of $K=294.1\pm1.1$ m s$^{-1}$. A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of $M_{p}=3.12\pm0.18$ $\rm{M_J}$ ($990\pm60$ M$_{\oplus}$), an inflated radius of $R_{p}=1.49\pm0.05$ $\rm{R_J}$ ($16.7\pm0.6$ R$_{\oplus}$), and an orbital period of $P=2.650237\pm0.000003$ d. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright ($\mathrm{V}=8.049$ mag) and young ($0.29^{+0.32}_{-0.19}$ Gyr) Am type star with $T_{\rm eff}=7690^{+400}_{-250}$ $\rm{K}$, resulting in a highly irradiated planet with an incident flux of $\langle F \rangle=7.24^{+0.68}_{-0.64}\times$10$^9$ erg s$^{-1}$ cm$^{-2}$ ($5300^{+500}_{-470}\mathrm{S_{\oplus}}$) and an equilibrium temperature of $T_{eq}=2370\pm70$ K. TESS photometry also reveals a secondary eclipse with a depth of $127^{+4}_{-5}$ppm as well as the full phase curve of the planet's thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as $T_\mathrm{day}=3004\pm64$ K and $T_\mathrm{night}=2583\pm63$ K, the second hottest measured nightside temperature. The planet's low day/night temperature contrast ($\sim$420 K) suggests very efficient heat transport between the dayside and nightside hemispheres., Comment: Accepted for publication in the Astronomical Journal. 39 pages, 18 figures, and 4 tables
Published: 2021
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39. The GALAH plus survey : Third data release

Author: Buder, Sven, Sharma, Sanjib, Kos, Janez, Amarsi, Anish, Nordlander, Thomas, Lind, Karin, Martell, Sarah L., Asplund, Martin, Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Hayden, Michael R., Lewis, Geraint F., Lin, Jane, Schlesinger, Katharine J., Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaz, Beeson, Kevin L., Buck, Tobias, Casagrande, Luca, Clark, Jake T., Cotar, Klemen, Da Costa, Gary S., de Grijs, Richard, Feuillet, Diane, Horner, Jonathan, Kafle, Prajwal R., Khanna, Shourya, Kobayashi, Chiaki, Liu, Fan, Montet, Benjamin T., Nandakumar, Govind, Nataf, David M., Ness, Melissa K., Spina, Lorenzo, Tepper-Garcia, Thor, Ting, Yuan-Sen, Traven, Gregor, Vogrincic, Rok, Wittenmyer, Robert A., Wyse, Rosemary F. G., Zerjal, Marusa, Buder, Sven, Sharma, Sanjib, Kos, Janez, Amarsi, Anish, Nordlander, Thomas, Lind, Karin, Martell, Sarah L., Asplund, Martin, Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Hayden, Michael R., Lewis, Geraint F., Lin, Jane, Schlesinger, Katharine J., Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaz, Beeson, Kevin L., Buck, Tobias, Casagrande, Luca, Clark, Jake T., Cotar, Klemen, Da Costa, Gary S., de Grijs, Richard, Feuillet, Diane, Horner, Jonathan, Kafle, Prajwal R., Khanna, Shourya, Kobayashi, Chiaki, Liu, Fan, Montet, Benjamin T., Nandakumar, Govind, Nataf, David M., Ness, Melissa K., Spina, Lorenzo, Tepper-Garcia, Thor, Ting, Yuan-Sen, Traven, Gregor, Vogrincic, Rok, Wittenmyer, Robert A., Wyse, Rosemary F. G., and Zerjal, Marusa
Abstract: The ensemble of chemical element abundance measurements for stars, along with precision distances and orbit properties, provides high-dimensional data to study the evolution of the Milky Way. With this third data release of the Galactic Archaeology with HERMES (GALAH) survey, we publish 678 423 spectra for 588 571 mostly nearby stars (81.2 per cent of stars are within <2 kpc), observed with the HERMES spectrograph at the Anglo-Australian Telescope. This release (hereafter GALAH+ DR3) includes all observations from GALAH Phase 1 (bright, main, and faint survey, 70 per cent), K2-HERMES (17 per cent), TESS-HERMES (5 per cent), and a subset of ancillary observations (8 per cent) including the bulge and >75 stellar clusters. We derive stellar parameters T-eff, logg, [Fe/H], v(mic), v(broad), and v(rad) using our modified version of the spectrum synthesis code Spectroscopy Made Easy (SME) and 1D MARCS model atmospheres. We break spectroscopic degeneracies in our spectrum analysis with astrometry from Gaia DR2 and photometry from 2MASS. We report abundance ratios [X/Fe] for 30 different elements (11 of which are based on non-LTE computations) covering five nucleosynthetic pathways. We describe validations for accuracy and precision, flagging of peculiar stars/measurements and recommendations for using our results. Our catalogue comprises 65 per cent dwarfs, 34 per cent giants, and 1 per cent other/unclassified stars. Based on unflagged chemical composition and age, we find 62 per cent young low-alpha, 9 per cent young high-alpha, 27 per cent old high-alpha, and 2 per cent stars with [Fe/H] <= -1. Based on kinematics, 4 per cent are halo stars. Several Value-Added-Catalogues, including stellar ages and dynamics, updated after Gaia eDR3, accompany this release and allow chrono-chemodynamic analyses, as we showcase.
Published: 2021
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40. TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs

Author: El Mufti, Mohammed, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villaseñor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Akana Murphy, Joseph M., Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J., Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceño, César, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Werner, Michael W., Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, El Mufti, Mohammed, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villaseñor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Akana Murphy, Joseph M., Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J., Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceño, César, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Werner, Michael W., Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Abstract: We validate the presence of a two-planet system orbiting the 0.2--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, P = 6.397438 ± 0.000037 days, e = 0.294^(0.13)_(0.062)) initially discovered in the Sector 8 TESS mission observations, and a transiting mini-Neptune (TOI 560 c, P = 18.8779 ± 0.0016 days) discovered in the Sector 34 observations, in a rare 1:3 orbital resonance. We utilize photometric data from TESS Spitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets and vet false positive scenarios. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We place upper limits on the masses of both planets of <2.1 and <4.1 M_(Nep) for b and c, respectively. We apply a Gaussian Processes (GP) model to the TESS light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by <6 hours before June 2027.
Published: 2021

41. The GALAH Survey: Using galactic archaeology to refine our knowledge of TESS target stars

Author: Clark, Jake T., Clerté, Mathieu, Hinkel, Natalie R., Unterborn, Cayman T., Wittenmyer, Robert, Horner, Jonathan, Wright, Duncan, Carter, Bradley, Morton, Timothy D, Spina, Lorenzo, Asplund, Martin, Buder, Sven, Duong, Ly, Freeman, Kenneth, Ting, Yuan-Sen, Lin, Jane, Nordlander, Thomas, Clark, Jake T., Clerté, Mathieu, Hinkel, Natalie R., Unterborn, Cayman T., Wittenmyer, Robert, Horner, Jonathan, Wright, Duncan, Carter, Bradley, Morton, Timothy D, Spina, Lorenzo, Asplund, Martin, Buder, Sven, Duong, Ly, Freeman, Kenneth, Ting, Yuan-Sen, Lin, Jane, and Nordlander, Thomas
Abstract: An unprecedented number of exoplanets are being discovered by the Transiting Exoplanet Survey Satellite (TESS). Determining the orbital parameters of these exoplanets, and especially their mass and radius, will depend heavily upon the measured physical characteristics of their host stars. We have cross-matched spectroscopic, photometric, and astrometric data from GALAH Data Release 2, the TESS Input Catalog and Gaia Data Release 2, to create a curated, self-consistent catalogue of physical and chemical properties for 47 285 stars. Using these data, we have derived isochrone masses and radii that are precise to within 5 per cent. We have revised the parameters of three confirmed, and twelve candidate, TESS planetary systems. These results cast doubt on whether CTOI-20125677 is indeed a planetary system, since the revised planetary radii are now comparable to stellar sizes. Our GALAH-TESS catalogue contains abundances for up to 23 elements. We have specifically analysed the molar ratios for C/O, Mg/Si, Fe/Si, and Fe/Mg, to assist in determining the composition and structure of planets with Rp < 4R⊕. From these ratios, 36 per cent fall within 2$\sigma$ sigma of the Sun/Earth values, suggesting that these stars may host rocky exoplanets with geological compositions similar to planets found within our own Solar system.
Published: 2021

42. TOI-1431b/MASCARA-5b: A Highly Irradiated Ultrahot Jupiter Orbiting One of the Hottest and Brightest Known Exoplanet Host Stars

Author: Addison, Brett C., Knudstrup, Emil, Wong, Ian, Hébrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier D. S., Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, René, Antoci, Victoria, Buchhave, Lars A., Günther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hansen, Jens, Pallé, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., McLean, Brian, Addison, Brett C., Knudstrup, Emil, Wong, Ian, Hébrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier D. S., Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, René, Antoci, Victoria, Buchhave, Lars A., Günther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Rabus, Markus, Johnson, Marshall C., Otten, Gilles P. P. L., Talens, Geert Jan, Cabot, Samuel H. C., Fischer, Debra A., Grundahl, Frank, Andersen, Mads Fredslund, Jessen-Hansen, Jens, Pallé, Pere, Shporer, Avi, Ciardi, David R., Clark, Jake T., Wittenmyer, Robert A., Wright, Duncan J., Horner, Jonathan, Collins, Karen A., Jensen, Eric L. N., Kielkopf, John F., Schwarz, Richard P., Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan Volkan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus D., Smith, Jeffrey C., Wang, Songhu, Eastman, Jason D., Stassun, Keivan G., Latham, David W., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Louie, Dana R., Bouma, Luke G., Twicken, Joseph D., Levine, Alan M., and McLean, Brian
Abstract: We present the discovery of a highly irradiated and moderately inflated ultrahot Jupiter, TOI-1431b/MASCARA-5 b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky Camera (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of K = 294.1 ± 1.1 m s−1. A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of Mp = 3.12 ± 0.18 MJ (990 ± 60 M⊕), an inflated radius of Rp = 1.49 ± 0.05 RJ (16.7 ± 0.6 R⊕), and an orbital period of P = 2.650237 ± 0.000003 days. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright (V = 8.049 mag) and young ( Gyr) Am type star with K, resulting in a highly irradiated planet with an incident flux of 109 erg s−1 cm−2 () and an equilibrium temperature of Teq = 2370 ± 70 K. TESS photometry also reveals a secondary eclipse with a depth of ppm as well as the full phase curve of the planet's thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as Tday = 3004 ± 64 K and Tnight = 2583 ± 63 K, the second hottest measured nightside temperature. The planet's low day/night temperature contrast (∼420 K) suggests very efficient heat transport between the dayside and nightside hemispheres. Given the host star brightness and estimated secondary eclipse depth of ∼1000 ppm in the K band, the secondary eclipse is potentially detectable at near-IR wavelengths with ground-based facilities, and the planet is ideal for intensive atmospheric characterization thr
Published: 2021

43. TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs

Author: Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., Okumura, Jack, Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Abstract: We validate the presence of a two-planet system orbiting the 0.15--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P = 6.3980661^{+0.0000095}_{-0.0000097}$ days, $e=0.294^{+0.13}_{-0.062}$, $M= 0.94^{+0.31}_{-0.23}M_{Nep}$) initially discovered in the Sector 8 \tess\ mission observations, and a transiting mini-Neptune (TOI 560 c, $P = 18.8805^{+0.0024}_{-0.0011}$ days, $M= 1.32^{+0.29}_{-0.32}M_{Nep}$) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from \tess\, \textit{Spitzer}, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false positive scenarios, and detect the photo-eccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We detect the masses of both planets at $> 3-\sigma$ significance. We apply a Gaussian process (GP) model to the \tess\ light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of NIR RVs in mitigating stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by $<$6 hours before June 2027., Comment: AAS Journals, Accepted for publication
Published: 2021

44. The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at $\approx$2 AU

Author: Zeng, Yunlin, Brandt, Timothy D., Li, Gongjie, Dupuy, Trent J., Li, Yiting, Brandt, G. Mirek, Farihi, Jay, Horner, Jonathan, Wittenmyer, Robert A., Butler, R. Paul., Tinney, Christopher G., Carter, Bradley D., Wright, Duncan J., Jones, Hugh R. A., O'Toole, Simon J., Zeng, Yunlin, Brandt, Timothy D., Li, Gongjie, Dupuy, Trent J., Li, Yiting, Brandt, G. Mirek, Farihi, Jay, Horner, Jonathan, Wittenmyer, Robert A., Butler, R. Paul., Tinney, Christopher G., Carter, Bradley D., Wright, Duncan J., Jones, Hugh R. A., and O'Toole, Simon J.
Abstract: Gliese 86 is a nearby K dwarf hosting a giant planet on a $\approx$16-day orbit and an outer white dwarf companion on a $\approx$century-long orbit. In this study we combine radial velocity data (including new measurements spanning more than a decade) with high angular resolution imaging and absolute astrometry from Hipparcos and Gaia to measure the current orbits and masses of both companions. We then simulate the evolution of the Gl 86 system to constrain its primordial orbit when both stars were on the main sequence; the closest approach between the two stars was then about $9\,$AU. Such a close separation limited the size of the protoplanetary disk of Gl 86 A and dynamically hindered the formation of the giant planet around it. Our measurements of Gl 86 B and Gl 86 Ab's orbits reveal Gl 86 as a system in which giant planet formation took place in a disk truncated at $\approx$2$\,$AU. Such a disk would be just big enough to harbor the dust mass and total mass needed to assemble Gl 86 Ab's core and envelope, assuming a high disk accretion rate and a low viscosity. Inefficient accretion of the disk onto Gl 86 Ab, however, would require a disk massive enough to approach the Toomre stability limit at its outer truncation radius. The orbital architecture of the Gl 86 system shows that giant planets can form even in severely truncated disks and provides an important benchmark for planet formation theory., Comment: 17 pages, 10 figures
Published: 2021
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45. TOI-1842b: A Transiting Warm Saturn Undergoing Re-Inflation around an Evolving Subgiant

Author: Wittenmyer, Robert A., Clark, Jake T., Trifonov, Trifon, Addison, Brett C., Wright, Duncan J., Stassun, Keivan G., Horner, Jonathan, Lowson, Nataliea, Kielkopf, John, Kane, Stephen R., Plavchan, Peter, Shporer, Avi, Zhang, Hui, Bowler, Brendan P., Mengel, Matthew W., Okumura, Jack, Rabus, Markus, Johnson, Marshall C., Harbeck, Daniel, Tronsgaard, Rene, Buchhave, Lars A., Collins, Karen A., Collins, Kevin I., Gan, Tianjun, Jensen, Eric L. N., Howell, Steve B., Furlan, E., Gnilka, Crystal L., Lester, Kathryn V., Matson, Rachel A., Scott, Nicholas J., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Rudat, Alexander, Quintana, Elisa V., Rodriguez, David R., Caldwell, Douglas A., Quinn, Samuel N., Essack, Zahra, Bouma, Luke G., Wittenmyer, Robert A., Clark, Jake T., Trifonov, Trifon, Addison, Brett C., Wright, Duncan J., Stassun, Keivan G., Horner, Jonathan, Lowson, Nataliea, Kielkopf, John, Kane, Stephen R., Plavchan, Peter, Shporer, Avi, Zhang, Hui, Bowler, Brendan P., Mengel, Matthew W., Okumura, Jack, Rabus, Markus, Johnson, Marshall C., Harbeck, Daniel, Tronsgaard, Rene, Buchhave, Lars A., Collins, Karen A., Collins, Kevin I., Gan, Tianjun, Jensen, Eric L. N., Howell, Steve B., Furlan, E., Gnilka, Crystal L., Lester, Kathryn V., Matson, Rachel A., Scott, Nicholas J., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Rudat, Alexander, Quintana, Elisa V., Rodriguez, David R., Caldwell, Douglas A., Quinn, Samuel N., Essack, Zahra, and Bouma, Luke G.
Abstract: The imminent launch of space telescopes designed to probe the atmospheres of exoplanets has prompted new efforts to prioritise the thousands of transiting planet candidates for follow-up characterisation. We report the detection and confirmation of TOI-1842b, a warm Saturn identified by TESS and confirmed with ground-based observations from Minerva-Australis, NRES, and the Las Cumbres Observatory Global Telescope. This planet has a radius of $1.04^{+0.06}_{-0.05}\,R_{Jup}$, a mass of $0.214^{+0.040}_{-0.038}\,M_{Jup}$, an orbital period of $9.5739^{+0.0002}_{-0.0001}$ days, and an extremely low density ($\rho$=0.252$\pm$0.091 g cm$^{-3}$). TOI-1842b has among the best known combinations of large atmospheric scale height (893 km) and host-star brightness ($J=8.747$ mag), making it an attractive target for atmospheric characterisation. As the host star is beginning to evolve off the main sequence, TOI-1842b presents an excellent opportunity to test models of gas giant re-inflation. The primary transit duration of only 4.3 hours also makes TOI-1842b an easily-schedulable target for further ground-based atmospheric characterisation., Comment: Accepted for publication in AJ
Published: 2021
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46. The GALAH Survey: Improving our understanding of confirmed and candidate planetary systems with large stellar surveys

Author: Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, Nordlander, Thomas, Clark, Jake T., Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Hinkel, Natalie R., Clerté, Mathieu, Carter, Brad D., Buder, Sven, Hayden, Michael R., Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaž, Munari, Ulisse, and Nordlander, Thomas
Abstract: Pioneering photometric, astrometric, and spectroscopic surveys are helping exoplanetary scientists better constrain the fundamental properties of stars within our galaxy, and the planets these stars host. In this study, we use the third data release from the stellar spectroscopic GALAH Survey, coupled with astrometric data of eDR3 from the \textit{Gaia} satellite, and other data from NASA's Exoplanet Archive, to refine our understanding of 279 confirmed and candidate exoplanet host stars and their exoplanets. This homogenously analysed data set comprises 105 confirmed exoplanets, along with 146 K2 candidates, 95 TESS Objects of Interest (TOIs) and 52 Community TOIs (CTOIs). Our analysis significantly shifts several previously (unknown) planet parameters while decreasing the uncertainties for others; Our radius estimates suggest that 35 planet candidates are more likely brown dwarfs or stellar companions due to their new radius values. We are able to refine the radii and masses of WASP-47 e, K2-106 b, and CoRoT-7 b to their most precise values yet, to less than 2.3\% and 8.5\% respectively. We also use stellar rotational values from GALAH to show that most planet candidates will have mass measurements that will be tough to obtain with current ground-based spectrographs. With GALAH's chemical abundances, we show through chemo-kinematics that there are five planet-hosts that are associated with the galaxy's thick disc, including NGTS-4, K2-183 and K2-337. Finally, we show there is no statistical difference between the chemical properties of hot Neptune and hot rocky exoplanet hosts, with the possibility that short-period rocky worlds might be the remnant cores of hotter, gaseous worlds., Comment: 21 pages with 11 figures and 5 tables. Accepted into MNRAS with appendix tables available within this arXiv submission
Published: 2021
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47. Diving Beneath the Sea of Stellar Activity: Chromatic Radial Velocities of the Young AU Mic Planetary System

Author: Cale, Bryson, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Gaidos, Eric, Gagné, Jonathan, Gao, Peter, Kane, Stephen R., Béjar, Víctor J. S., Lodieu, Nicolas, Anglada-Escudé, Guillem, Ribas, Ignasi, Pallé, Enric, Quirrenbach, Andreas, Amado, Pedro J., Reiners, Ansgar, Caballero, José A., Osorio, María Rosa Zapatero, Dreizler, Stefan, Howard, Andrew W., Fulton, Benjamin J., Wang, Sharon Xuesong, Collins, Kevin I., Mufti, Mohammed El, Wittrock, Justin, Gilbert, Emily A., Barclay, Thomas, Klein, Baptiste, Martioli, Eder, Wittenmyer, Robert, Wright, Duncan, Addison, Brett, Hirano, Teruyuki, Tamura, Motohide, Kotani, Takayuki, Narita, Norio, Vermilion, David, Lee, Rena A., Geneser, Claire, Teske, Johanna, Quinn, Samuel N., Latham, David W., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Zohrabi, Farzaneh, Stibbards, Caitlin, Kotnana, Srihan, Jenkins, Jon, Twicken, Joseph D., Henze, Christopher, Kidwell Jr., Richard, Burke, Christopher, n}or, Joel Villase{\~, Boyd, Patricia, Cale, Bryson, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Gaidos, Eric, Gagné, Jonathan, Gao, Peter, Kane, Stephen R., Béjar, Víctor J. S., Lodieu, Nicolas, Anglada-Escudé, Guillem, Ribas, Ignasi, Pallé, Enric, Quirrenbach, Andreas, Amado, Pedro J., Reiners, Ansgar, Caballero, José A., Osorio, María Rosa Zapatero, Dreizler, Stefan, Howard, Andrew W., Fulton, Benjamin J., Wang, Sharon Xuesong, Collins, Kevin I., Mufti, Mohammed El, Wittrock, Justin, Gilbert, Emily A., Barclay, Thomas, Klein, Baptiste, Martioli, Eder, Wittenmyer, Robert, Wright, Duncan, Addison, Brett, Hirano, Teruyuki, Tamura, Motohide, Kotani, Takayuki, Narita, Norio, Vermilion, David, Lee, Rena A., Geneser, Claire, Teske, Johanna, Quinn, Samuel N., Latham, David W., Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Zohrabi, Farzaneh, Stibbards, Caitlin, Kotnana, Srihan, Jenkins, Jon, Twicken, Joseph D., Henze, Christopher, Kidwell Jr., Richard, Burke, Christopher, n}or, Joel Villase{\~, and Boyd, Patricia
Abstract: We present updated radial-velocity (RV) analyses of the AU Mic system. AU Mic is a young (22 Myr) early M dwarf known to host two transiting planets - $P_{b}\sim8.46$ days, $R_{b}=4.38_{-0.18}^{+0.18}\ R_{\oplus}$, $P_{c}\sim18.86$ days, $R_{c}=3.51_{-0.16}^{+0.16}\ R_{\oplus}$. With visible RVs from CARMENES-VIS, CHIRON, HARPS, HIRES, {\sc {\textsc{Minerva}}}-Australis, and TRES, as well as near-infrared (NIR) RVs from CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a $5\sigma$ upper limit to the mass of AU Mic c of $M_{c}\leq20.13\ M_{\oplus}$ and present a refined mass of AU Mic b of $M_{b}=20.12_{-1.57}^{+1.72}\ M_{\oplus}$. Used in our analyses is a new RV modeling toolkit to exploit the wavelength dependence of stellar activity present in our RVs via wavelength-dependent Gaussian processes. By obtaining near-simultaneous visible and near-infrared RVs, we also compute the temporal evolution of RV-``color'' and introduce a regressional method to aid in isolating Keplerian from stellar activity signals when modeling RVs in future works. Using a multi-wavelength Gaussian process model, we demonstrate the ability to recover injected planets at $5\sigma$ significance with semi-amplitudes down to $\approx$ 10\,m\,s$^{-1}$ with a known ephemeris, more than an order of magnitude below the stellar activity amplitude. However, we find that the accuracy of the recovered semi-amplitudes is $\sim$50\% for such signals with our model.
Published: 2021
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48. TOI-3362b: A Proto-Hot Jupiter Undergoing High-Eccentricity Tidal Migration

Author: Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Rodriguez, Joseph E., Eastman, Jason D., Collins, Karen A., Quinn, Samuel N., Shporer, Avi, Triaud, Amaury H. M. J., Wang, Songhu, Beatty, Thomas, Jackson, Jonathon, Collins, Kevin I., Abe, Lyu, Suarez, Olga, Crouzet, Nicolas, MeKarnia, Djamel, Dransfield, Georgina, Jensen, Eric L. N., Stockdale, Chris, Barkaoui, Khalid, Heitzmann, Alexis, Wright, Duncan J., Addison, Brett C., Wittenmyer, Robert A., Okumura, Jack, Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Liu, Huigen, Plavchan, Peter, Mengel, Matthew W., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Christiansen, Jessie L., Paegert, Martin, Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Rodriguez, Joseph E., Eastman, Jason D., Collins, Karen A., Quinn, Samuel N., Shporer, Avi, Triaud, Amaury H. M. J., Wang, Songhu, Beatty, Thomas, Jackson, Jonathon, Collins, Kevin I., Abe, Lyu, Suarez, Olga, Crouzet, Nicolas, MeKarnia, Djamel, Dransfield, Georgina, Jensen, Eric L. N., Stockdale, Chris, Barkaoui, Khalid, Heitzmann, Alexis, Wright, Duncan J., Addison, Brett C., Wittenmyer, Robert A., Okumura, Jack, Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Liu, Huigen, Plavchan, Peter, Mengel, Matthew W., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Christiansen, Jessie L., and Paegert, Martin
Abstract: High-eccentricity tidal migration is a possible way for giant planets to be emplaced in short-period orbits. If it commonly operates, one would expect to catch proto-Hot Jupiters on highly elliptical orbits that are undergoing high-eccentricity tidal migration. As of yet, few such systems have been discovered. Here, we introduce TOI-3362b (TIC-464300749b), an 18.1-day, 5 $M_{\rm Jup}$ planet orbiting a main-sequence F-type star that is likely undergoing high-eccentricity tidal migration. The orbital eccentricity is 0.815$^{+0.023}_{-0.032}$. With a semi-major axis of 0.153$^{+0.002}_{-0.003}$ au, the planet's orbit is expected to shrink to a final orbital radius of 0.051$^{+0.008}_{-0.006}$ au after complete tidal circularization. Several mechanisms could explain the extreme value of the planet's eccentricity, such as planet-planet scattering and secular interactions. Such hypotheses can be tested with follow-up observations of the system, e.g., measuring the stellar obliquity and searching for companions in the system with precise, long-term radial velocity observations. The variation in the planet's equilibrium temperature as it orbits the host star and the tidal heating at periapse make this planet an intriguing target for atmospheric modeling and observation. Because the planet's orbital period of 18.1 days is near the limit of TESS's period sensitivity, even a few such discoveries suggest that proto-Hot Jupiters may be quite common., Comment: 14 pages, 4 figures, 2 tables. submitted to ApJL, revised in response to referee report
Published: 2021
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49. Flares, Rotation, and Planets of the AU Mic System from TESS Observations

Author: Gilbert, Emily A., Barclay, Thomas, Quintana, Elisa V., Walkowicz, Lucianne M., Vega, Laura D., Schlieder, Joshua E., Monsue, Teresa, Cale, Bryson, Collins, Kevin I., Gaidos, Eric, Mufti, Mohammed El, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A., Wittrock, Justin M., Jenkins, Jon M., Latham, David W., Ricker, George R., Rose, Mark E., Seager, S., Vanderspek, Roland K., Winn, Joshua N., Gilbert, Emily A., Barclay, Thomas, Quintana, Elisa V., Walkowicz, Lucianne M., Vega, Laura D., Schlieder, Joshua E., Monsue, Teresa, Cale, Bryson, Collins, Kevin I., Gaidos, Eric, Mufti, Mohammed El, Reefe, Michael, Plavchan, Peter, Tanner, Angelle, Wittenmyer, Robert A., Wittrock, Justin M., Jenkins, Jon M., Latham, David W., Ricker, George R., Rose, Mark E., Seager, S., Vanderspek, Roland K., and Winn, Joshua N.
Abstract: AU Mic is a young ($\sim$24 Myr), pre-Main Sequence M~dwarf star that was observed in the first month of science observations of the Transiting Exoplanet Survey Satellite (TESS) and re-observed two years later. This target has photometric variability from a variety of sources that is readily apparent in the TESS light curves; spots induce modulation in the light curve, flares are present throughout (manifesting as sharp rises with slow exponential decay phases), and transits of AU Mic b may be seen by eye as dips in the light curve. We present a combined analysis of both TESS Sector 1 and Sector 27 AU Mic light curves including the new 20-second cadence data from TESS Year 3. We compare flare rates between both observations and analyze the spot evolution, showing that the activity levels increase slightly from Sector 1 to Sector 27. Furthermore, the 20-second data collection allows us to detect more flares, smaller flares, and better resolve flare morphology in white light as compared to the 2-minute data collection mode. We also refine the parameters for AU Mic b by fitting three additional transits of AU Mic b from Sector 27 using a model that includes stellar activity. We show that the transits exhibit clear transit timing variations (TTVs) with an amplitude of $\sim$80 seconds. We also detect three transits of a 2.8 $R_\oplus$ planet, AU Mic c, which has a period of 18.86 days., Comment: 18 pages, 13 figures, 5 tables, accepted to AJ
Published: 2021
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50. HD 183579b: A Warm Sub-Neptune Transiting a Solar Twin Detected by TESS

Author: Gan, Tianjun, Bedell, Megan, Wang, Sharon Xuesong, Foreman-Mackey, Daniel, Meléndez, Jorge, Mao, Shude, Stassun, Keivan G., Howell, Steve B., Ziegler, Carl, Wittenmyer, Robert A., Hellier, Coel, Collins, Karen A., Shporer, Avi, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Ballard, Sarah, Barclay, Thomas, Bean, Jacob L., Bowler, Brendan P., Briceño, César, Crossfield, Ian J. M., Dittman, Jason, Horner, Jonathan, Jensen, Eric L. N., Kane, Stephen R., Kielkopf, John, Kreidberg, Laura, Law, Nicholas, Mann, Andrew W., Mengel, Matthew W., Morgan, Edward H., Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Plavchan, Peter, Schwarz, Richard P., Shiao, Bernie, Smith, Jeffrey C., Spina, Lorenzo, Tinney, C. G., Torres, Guillermo, Twicken, Joseph D., Vezie, Michael, Wang, Gavin, Wright, Duncan J., Zhang, Hui, Gan, Tianjun, Bedell, Megan, Wang, Sharon Xuesong, Foreman-Mackey, Daniel, Meléndez, Jorge, Mao, Shude, Stassun, Keivan G., Howell, Steve B., Ziegler, Carl, Wittenmyer, Robert A., Hellier, Coel, Collins, Karen A., Shporer, Avi, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Ballard, Sarah, Barclay, Thomas, Bean, Jacob L., Bowler, Brendan P., Briceño, César, Crossfield, Ian J. M., Dittman, Jason, Horner, Jonathan, Jensen, Eric L. N., Kane, Stephen R., Kielkopf, John, Kreidberg, Laura, Law, Nicholas, Mann, Andrew W., Mengel, Matthew W., Morgan, Edward H., Okumura, Jack, Osborn, Hugh P., Paegert, Martin, Plavchan, Peter, Schwarz, Richard P., Shiao, Bernie, Smith, Jeffrey C., Spina, Lorenzo, Tinney, C. G., Torres, Guillermo, Twicken, Joseph D., Vezie, Michael, Wang, Gavin, Wright, Duncan J., and Zhang, Hui
Abstract: We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright ($V=8.75$ mag, $K=7.15$ mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located $56.8\pm0.1$ pc away with a radius of $R_{\ast}=0.97\pm0.02\ R_{\odot}$ and a mass of $M_{\ast}=1.03\pm0.05\ M_{\odot}$. We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of $R_{p}=3.53\pm0.13\ R_{\oplus}$ on a $17.47$ day orbit with a mass of $M_{p}=11.2\pm5.4\ M_{\oplus}$ ($3\sigma$ mass upper limit of $27.4\ M_{\oplus}$). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin sample, without a statistically significant refractory element depletion., Comment: 20 pages, 15 figures, accepted for publication in MNRAS
Published: 2021
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