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109 results on '"Mengel, Matthew W."'

1. HD 21520 b: a warm sub-Neptune transiting a bright G dwarf

Author

Nies, Molly, Mireles, Ismael, Bouchy, François, Dragomir, Diana, Nicholson, Belinda A., Eisner, Nora L., Sousa, Sergio G., Collins, Karen A., Howell, Steve B., Ziegler, Carl, Hellier, Coel, Addison, Brett, Ballard, Sarah, Bowler, Brendan P., Briceño, César, Clark, Catherine A., Conti, Dennis M., Dumusque, Xavier, Edwards, Billy, Gnilka, Crystal L., Hobson, Melissa, Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Lavie, Baptiste, Law, Nicholas, Lendl, Monika, Littlefield, Colin, Liu, Huigen, Mann, Andrew W., Mengel, Matthew W., Oddo, Dominic, Okumura, Jack, Palle, Enric, Plavchan, Peter, Psaridi, Angelica, Santos, Nuno C., Schwarz, Richard P., Shporer, Avi, Wittenmyer, Robert A., Wright, Duncan J., Zhang, Hui, Watanabe, David, Medina, Jennifer V., Villaseñor, Joel, Ting, Eric B., Christiansen, Jessie L., Winn, Joshua N., Stassun, Keivan G., Seager, S., Latham, David W., and Ricker, George R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery and validation of HD 21520 b, a transiting planet found with TESS and orbiting a bright G dwarf (V=9.2, $T_{eff} = 5871 \pm 62$ K, $R_{\star} = 1.04\pm 0.02\, R_{\odot}$). HD 21520 b was originally alerted as a system (TOI-4320) consisting of two planet candidates with periods of 703.6 and 46.4 days. However, our analysis supports instead a single-planet system with an orbital period of $25.1292\pm0.0001$ days and radius of $2.70 \pm 0.09\, R_{\oplus}$. Three full transits in sectors 4, 30 and 31 match this period and have transit depths and durations in agreement with each other, as does a partial transit in sector 3. We also observe transits using CHEOPS and LCOGT. SOAR and Gemini high-resolution imaging do not indicate the presence of any nearby companions, and MINERVA-Australis and CORALIE radial velocities rule out an on-target spectroscopic binary. Additionally, we use ESPRESSO radial velocities to obtain a tentative mass measurement of $7.9^{+3.2}_{-3.0}\, M_{\oplus}$, with a 3-$\sigma$ upper limit of 17.7 $M_{\oplus}$. Due to the bright nature of its host and likely significant gas envelope of the planet, HD 21520 b is a promising candidate for further mass measurements and for atmospheric characterization., Comment: Submitted to MNRAS

Published
2024

2. 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., and Addison, Brett C.

Subjects
Astrophysics - Earth and Planetary Astrophysics
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

3. 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, and Zhou, George

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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4. 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, and Samadi-Ghadim, Anya

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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5. 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, and Ziegler, Carl

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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6. 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, and Zobel, Evan

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
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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7. 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, and Kunimoto, Michelle

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
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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8. 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., and Okumura, Jack

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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9. 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., and Okumura, Jack

Subjects
Astrophysics - Earth and Planetary Astrophysics
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

10. 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, and Bouma, Luke G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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11. 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., and Paegert, Martin

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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12. 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, and Zohrabi, F.

Subjects
Astrophysics - Earth and Planetary Astrophysics
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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13. 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., and Zhang, Hui

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
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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14. A transiting warm giant planet around the young active star TOI-201

Author

Hobson, Melissa J., Brahm, Rafael, Jordán, Andres, Espinoza, Nestor, Kossakowski, Diana, Henning, Thomas, Rojas, Felipe, Schlecker, Martin, Sarkis, Paula, Trifonov, Trifon, Thorngren, Daniel, Binnenfeld, Avraham, Shahaf, Sahar, Zucker, Shay, Ricker, George R., Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Addison, Brett, Bouchy, Francois, Bowler, Brendan P., Briegal, Joshua T., Bryant, Edward M., Collins, Karen A., Daylan, Tansu, Grieves, Nolan, Horner, Jonathan, Huang, Chelsea, Kane, Stephen R., Kielkopf, John, McLean, Brian, Mengel, Matthew W., Nielsen, Louise D., Okumura, Jack, Plavchan, Peter, Shporer, Avi, Smith, Alexis M. S., Tilbrook, Rosanna, Tinney, C. G., Twicken, Joseph D., Udry, Stephane, Unger, Nicolas, West, Richard, Wittenmyer, Robert A., Wohler, Bill, and Wright, Duncan J.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in \textit{TESS} photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using ground-based photometry from NGTS and radial velocities from FEROS, HARPS, CORALIE, and \textsc{Minerva}-Australis. TOI-201 b orbits a young ($\mathrm{0.87^{+0.46}_{-0.49} \, Gyr}$) and bright(V=9.07 mag) F-type star with a $\mathrm{52.9781 \, d}$ period. The planet has a mass of $\mathrm{0.42^{+0.05}_{-0.03}\, M_J}$, a radius of $\mathrm{1.008^{+0.012}_{-0.015}\, R_J}$, and an orbital eccentricity of $0.28^{+0.06}_{-0.09}$; it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b is important for constraining formation and evolution theories for giant planets., Comment: 21 pages, 11 figures, accepted to AJ

Published
2021
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15. TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full Frame Images

Author

Rodriguez, Joseph E., Quinn, Samuel N., Zhou, George, Vanderburg, Andrew, Nielsen, Louise D., Wittenmyer, Robert A., Brahm, Rafael, Reed, Phillip A., Huang, Chelsea X., Vach, Sydney, Ciardi, David R., Oelkers, Ryan J., Stassun, Keivan G., Hellier, Coel, Gaudi, B. Scott, Eastman, Jason D., Collins, Karen A., Bieryla, Allyson, Christian, Sam, Latham, David W., Carleo, Ilaria, Wright, Duncan J., Matthews, Elisabeth, Gonzales, Erica J., Ziegler, Carl, Dressing, Courtney D., Howell, Steve B., Tan, Thiam-Guan, Wittrock, Justin, Plavchan, Peter, McLeod, Kim K., Baker, David, Wang, Gavin, Radford, Don, Schwarz, Richard P., Esposito, Massimiliano, Ricker, George R., Vanderspek, Roland K., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett, Anderson, D. R., Barclay, Thomas, Beatty, Thomas G., Berlind, Perry, Bouchy, Francois, Bowen, Michael, Bowler, Brendan P., Brasseur, C. E., Briceño, César, Caldwell, Douglas A., Calkins, Michael L., Chaturvedi, Priyanka, Chaverot, Guillaume, Chimaladinne, Sudhish, Christiansen, Jessie L., Collins, Kevin, Crossfield, Ian J. M., Eastridge, Kevin, Espinoza, N'estor, Esquerdo, Gilbert A., Feliz, Dax, Fenske, Tyler, Fong, William, Gan, Tianjun, Giacalone, Steven, Gill, Holden, Gordon, Lindsey, Granados, Alex, Grieves, Nolan, Guenther, Eike W., Guerrero, Natalia, Henning, Thomas, Henze, Christopher E., Hesse, Katharine, Hobson, Melissa J., Horner, Jonathan, James, David J., Jensen, Eric L. N., Jimenez, Mary, Jordán, Andrés, Kane, Stephen R., Kielkopf, John, Kim, Kingsley, Kuhn, Rudolf B., Latouf, Natasha, Law, Nicholas M., Levine, Alan M., Lund, Michael B., Mann, Andrew W., Mao, Shude, Matson, Rachel A., McDermott, Scott, Mengel, Matthew W., Mink, Jessica, Newman, Patrick, O'Dwyer, Tanner, Okumura, Jack, Palle, Enric, Pepper, Joshua, Quintana, Elisa V., Sarkis, Paula, Savel, Arjun, Schlieder, Joshua E., Schnaible, Chloe, Shporer, Avi, Sefako, Ramotholo, Seidel, Julia, Siverd, Robert J., Skinner, Brett, Stalport, Manu, Stevens, Daniel J., Stibbards, Caitlin, Tinney, C. G., West, R. G., Yahalomi, Daniel A., and Zhang, Hui

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

We present the discovery and characterization of five hot and warm Jupiters -- TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960) -- based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the $TESS$ Follow-up Observing Program (TFOP) Working Group. The planets are all Jovian size (R$_{\rm P}$ = 1.01-1.77 R$_{\rm J}$) and have masses that range from 0.85 to 6.33 M$_{\rm J}$. The host stars of these systems have F and G spectral types (5595 $\le$ T$_{\rm eff}$ $\le$ 6460 K) and are all relatively bright (9 $ 1.7R$_{\rm J}$, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive hot Jupiter discovered to date by $TESS$ with a measured mass of $6.31^{+0.28}_{-0.30}$ M$_{\rm J}$ and a statistically significant, non-zero orbital eccentricity of e = $0.074^{+0.021}_{-0.022}$. This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-Solar analogue. NASA's $TESS$ mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals., Comment: 25 Pages, 7 Figures, 5 Tables, Accepted to The Astronomical Journal

Published
2021
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16. TOI-954 b and K2-329 b: Short-Period Saturn-Mass Planets that Test whether Irradiation Leads to Inflation

Author

Sha, Lizhou, Huang, Chelsea X., Shporer, Avi, Rodriguez, Joseph E., Vanderburg, Andrew, Brahm, Rafael, Hagelberg, Janis, Matthews, Elisabeth C., Ziegler, Carl, Livingston, John H., Stassun, Keivan G., Wright, Duncan J., Crane, Jeffrey D., Espinoza, Néstor, Bouchy, François, Bakos, Gáspár Á., Collins, Karen A., Zhou, George, Bieryla, Allyson, Hartman, Joel D., Wittenmyer, Robert A., Nielsen, Louise D., Plavchan, Peter, Bayliss, Daniel, Sarkis, Paula, Tan, Thiam-Guan, Cloutier, Ryan, Mancini, Luigi, Jordán, Andrés, Wang, Sharon, Henning, Thomas, Narita, Norio, Penev, Kaloyan, Teske, Johanna K., Kane, Stephen R., Mann, Andrew W., Addison, Brett C., Tamura, Motohide, Horner, Jonathan, Barbieri, Mauro, Burt, Jennifer A., Díaz, Matías R., Crossfield, Ian J. M., Dragomir, Diana, Drass, Holger, Feinstein, Adina D., Zhang, Hui, Hart, Rhodes, Kielkopf, John F., Jensen, Eric L. N., Montet, Benjamin T., Ottoni, Gaël, Schwarz, Richard P., Rojas, Felipe, Nespral, David Lopez Fdez, Torres, Pascal, Mengel, Matthew W., Udry, Stéphane, Zapata, Abner, Snoddy, Erin, Okumura, Jack, Ricker, George R., Vanderspek, Roland K., Latham, David W., Winn, Joshua N., Seager, Sara, Jenkins, Jon M., Colón, Knicole D., Henze, Christopher E., Krishnamurthy, Akshata, Ting, Eric B., Vezie, Michael, and Villanueva, Steven

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of two short-period Saturn-mass planets, one transiting the G subgiant TOI-954 (TIC 44792534, $ V = 10.343 $, $ T = 9.78 $) observed in TESS sectors 4 and 5, and one transiting the G dwarf K2-329 (EPIC 246193072, $ V = 12.70 $, $ K = 10.67 $) observed in K2 campaigns 12 and 19. We confirm and characterize these two planets with a variety of ground-based archival and follow-up observations, including photometry, reconnaissance spectroscopy, precise radial velocity, and high-resolution imaging. Combining all available data, we find that TOI-954 b has a radius of $0.852_{-0.062}^{+0.053} \, R_{\mathrm{J}}$ and a mass of $0.174_{-0.017}^{+0.018} \, M_{\mathrm{J}}$ and is in a 3.68 day orbit, while K2-329 b has a radius of $0.774_{-0.024}^{+0.026} \, R_{\mathrm{J}}$ and a mass of $0.260_{-0.022}^{+0.020} \, M_{\mathrm{J}}$ and is in a 12.46 day orbit. As TOI-954 b is 30 times more irradiated than K2-329 b but more or less the same size, these two planets provide an opportunity to test whether irradiation leads to inflation of Saturn-mass planets and contribute to future comparative studies that explore Saturn-mass planets at contrasting points in their lifetimes., Comment: 28 pages, 9 figures, 11 tables, accepted by AJ, ancillary data also available at https://github.com/vulpicastor/toi954-data

Published
2020
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17. TOI-481 b & TOI-892 b: Two long period hot Jupiters from the Transiting Exoplanet Survey Satellite

Author

Brahm, Rafael, Nielsen, Louise D., Wittenmyer, Robert A., Wang, Songhu, Rodriguez, Joseph E., Espinoza, Néstor, Jones, Matías I., Jordán, Andrés, Henning, Thomas, Hobson, Melissa, Kossakowski, Diana, Rojas, Felipe, Sarkis, Paula, Schlecker, Martin, Trifonov, Trifon, Shahaf, Sahar, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Bakos, Gáspár Á., Bhatti, Waqas, Bayliss, Daniel, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Bowler, Brendan P., Briceño, César, Brown, Timothy M., Bryant, Edward M., Caldwell, Douglas A., Charbonneau, David, Collins, Karen A., Davis, Allen B., Esquerdo, Gilbert A., Fulton, Benjamin J., Guerrero, Natalia M., Henze, Christopher E., Hogan, Aleisha, Horner, Jonathan, Huang, Chelsea X., Irwin, Jonathan, Kane, Stephen R., Kielkopf, John, Mann, Andrew W., Mazeh, Tsevi, McCormac, James, McCully, Curtis, Mengel, Matthew W., Mireles, Ismael, Okumura, Jack, Plavchan, Peter, Quinn, Samuel N., Rabus, Markus, Saesen, Sophie, Schlieder, Joshua E., Segransan, Damien, Shiao, Bernie, Shporer, Avi, Siverd, Robert J., Stassun, Keivan G., Suc, Vincent, Tan, Thiam-Guan, Torres, Pascal, Tinney, Chris G., Udry, Stephane, Vanzi, Leonardo, Vezie, Michael, Vines, Jose I., Vuckovic, Maja, Wright, Duncan J., Yahalomi, Daniel A., Zapata, Abner, Zhang, Hui, and Ziegler, Carl

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

We present the discovery of two new 10-day period giant planets from the Transiting Exoplanet Survey Satellite ($TESS$) mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii ($0.99\pm0.01$ $\rm R_{J}$ and $1.07\pm0.02$ $\rm R_{J}$, respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses ($1.53\pm0.03$ $\rm M_{J}$ versus $0.95\pm0.07$ $\rm M_{J}$, respectively). Both planets orbit metal-rich stars ([Fe/H]= $+0.26\pm 0.05$ dex and [Fe/H] = $+0.24 \pm 0.05$ dex, for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a $\rm M_{\star}$ = $1.14\pm0.02$ $\rm M_{\odot}$, $\rm R_{\star}$ = $1.66\pm0.02$ $\rm R_{\odot}$ G-type star ($T_{\rm eff}$ = $5735 \pm 72$ K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892, on the other hand, is a F-type dwarf star ($T_{\rm eff}$ = $6261 \pm 80$ K), which has a mass of $\rm M_{\star}$ = $1.28\pm0.03$ $\rm M_{\odot}$, and a radius of $\rm R_{\star}$ = $1.39\pm0.02$ $\rm R_{\odot}$. TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters., Comment: 19 pages, 10 figures, accepted for publication in AJ

Published
2020
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18. AU Mic b is the Youngest Planet to have a Spin-Orbit Alignment Measurement

Author

Addison, Brett C., Horner, Jonathan, Wittenmyer, Robert A., Heitzmann, Alexis, Plavchan, Peter, Wright, Duncan J., Nicholson, Belinda A., Marshall, Jonathan P., Clark, Jake T., Gunther, Maximilian N., Kane, Stephen R., Hirano, Teruyuki, Wang, Songhu, Kielkopf, John, Shporer, Avi, Tinney, C. G., Zhang, Hui, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Okumura, Jack, Gaidos, Eric, and Wang, Xian-Yu

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

We report measurements of the sky-projected spin-orbit angle for AU\,Mic\,b, a Neptune-size planet orbiting a very young ($\sim20$\,Myr) nearby pre-main sequence M dwarf star which also hosts a bright, edge-on, debris disk. The planet was recently discovered from preliminary analysis of radial velocity observations and confirmed to be transiting its host star from photometric data from the NASA's \textit{TESS} mission. We obtained radial velocity measurements of AU\,Mic over the course of two partially observable transits and one full transit of planet b from high-resolution spectroscopic observations made with the {\textsc{Minerva}}-Australis telescope array. Only a marginal detection of the Rossiter--McLaughlin effect signal was obtained from the radial velocities, in part due to AU Mic being an extremely active star and the lack of full transit coverage plus sufficient out-of-transit baseline. As such, a precise determination of the obliquity for AU\,Mic\,b is not possible in this study and we find a sky-projected spin-orbit angle of $\lambda = 47{^{+26}_{-54}}^{\circ}$. This result is consistent with both the planet's orbit being aligned or highly misaligned with the spin-axis of its host star. Our measurement independently agrees with, but is far less precise than observations carried out on other instruments around the same time that measure a low obliquity orbit for the planet. AU\,Mic is the youngest exoplanetary system for which the projected spin-orbit angle has been measured, making it a key data point in the study of the formation and migration of exoplanets -- particularly given that the system is also host to a bright debris disk., Comment: 15 pages, 6 figures, 3 tables. Published in the Astronomical Journal on 10/09/2021

Published
2020
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19. TOI-257b (HD 19916b): A Warm sub-Saturn Orbiting an Evolved F-type Star

Author

Addison, Brett C., Wright, Duncan J., Nicholson, Belinda A., Cale, Bryson, Mocnik, Teo, Huber, Daniel, Plavchan, Peter, Wittenmyer, Robert A., Vanderburg, Andrew, Chaplin, William J., Chontos, Ashley, Clark, Jake T., Eastman, Jason D., Ziegler, Carl, Brahm, Rafael, Carter, Bradley D., Clerte, Mathieu, Espinoza, Néstor, Horner, Jonathan, Bentley, John, Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Laychock, Emilie, Mengel, Matthew W., Okumura, Jack, Stassun, Keivan G., Bedding, Timothy R., Bowler, Brendan P., Burnelis, Andrius, Blanco-Cuaresma, Sergi, Collins, Michaela, Crossfield, Ian, Davis, Allen B., Evensberget, Dag, Heitzmann, Alexis, Howell, Steve B., Law, Nicholas, Mann, Andrew W., Marsden, Stephen C., Matson, Rachel A., O'Connor, James, Shporer, Avi, Stevens, Catherine, Tinney, C. G., Tylor, Christopher, Wang, Songhu, Zhang, Hui, Henning, Thomas, Kossakowski, Diana, Ricker, George, Sarkis, Paula, Schlecker, Martin, Torres, Pascal, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Mireles, Ismael, Rowden, Pam, Pepper, Joshua, Daylan, Tansu, Schlieder, Joshua E., Collins, Karen A., Collins, Kevin I., Tan, Thiam-Guan, Ball, Warrick H., Basu, Sarbani, Buzasi, Derek L., Campante, Tiago L., Corsaro, Enrico, González-Cuesta, Lucía, Davies, Guy R., de Almeida, Leandro, Nascimento, Jr., Jose-Dias do, a, Rafael A. Garcí, Guo, Zhao, Handberg, Rasmus, Hekker, Saskia, Hey, Daniel R., Kallinger, Thomas, Kawaler, Steven D., Kayhan, Cenk, Kuszlewicz, James S., Lund, Mikkel N., Lyttle, Alexander, Mathur, Savita, Miglio, Andrea, Mosser, Benoit, Nielsen, Martin B., Serenelli, Aldo M., Aguirre, Victor Silva, and Themeßl, Nathalie

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

We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of $M_P=0.138\pm0.023$\,$\rm{M_J}$ ($43.9\pm7.3$\,$M_{\rm \oplus}$), a radius of $R_P=0.639\pm0.013$\,$\rm{R_J}$ ($7.16\pm0.15$\,$R_{\rm \oplus}$), bulk density of $0.65^{+0.12}_{-0.11}$ (cgs), and period $18.38818^{+0.00085}_{-0.00084}$\,$\rm{days}$. TOI-257b orbits a bright ($\mathrm{V}=7.612$\,mag) somewhat evolved late F-type star with $M_*=1.390\pm0.046$\,$\rm{M_{\odot}}$, $R_*=1.888\pm0.033$\,$\rm{R_{\odot}}$, $T_{\rm eff}=6075\pm90$\,$\rm{K}$, and $v\sin{i}=11.3\pm0.5$\,km\,s$^{-1}$. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a $\sim71$\,day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars ($\sim100$) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems., Comment: 24 pages, 20 figures, 6 tables. Published in MNRAS

Published
2020
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20. KELT-25b and KELT-26b: A Hot Jupiter and a Substellar Companion Transiting Young A-stars Observed by TESS

Author

Martínez, Romy Rodríguez, Gaudi, B. Scott, Rodriguez, Joseph E., Zhou, George, Labadie-Bartz, Jonathan, Quinn, Samuel N., Penev, Kaloyan Minev, Tan, Thiam-Guan, Latham, David W., Paredes, Leonardo A., Kielkopf, John, Addison, Brett C., Wright, Duncan J., Teske, Johanna K., Howell, Steve B., Ciardi, David R., Ziegler, Carl, Stassun, Keivan G., Johnson, Marshall C., Eastman, Jason D., Siverd, Robert J., Beatty, Thomas G., Bouma, Luke G., Pepper, Joshua, Lund, Michael B., Villanueva, Steven, Stevens, Daniel J., Jensen, Eric L. N., Kilby, Coleman, Cohen, David H., Bayliss, Daniel, Bieryla, Allyson, Cargile, Phillip A., Collins, Karen A., Conti, Dennis M., Colon, Knicole D., Curtis, Ivan A., DePoy, Darren L., Evans, Phil A., Feliz, Dax, Gregorio, Joao, Rothenberg, Jason, James, David J., Penny, Matthew T., Reed, Phillip A., Relles, Howard M., Stephens, Denise C., Joner, Michael D., Kuhn, Rudolf B., Stockdale, Chris, Trueblood, Mark, Trueblood, Patricia, Yao, Xinyu, Zambelli, Roberto, Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Henry, Todd J., James, Hodari-Sadiki, Jao, Wei-Chun, Wang, Sharon X., Butler, R. Paul, Crane, Jeffrey D., Thompson, Ian B., Schectman, Stephen, Wittenmyer, Robert A., Bedding, Timothy R., Okumura, Jack, Plavchan, Peter, Bowler, Brendan P., Horner, Jonathan, Kane, Stephen R., Mengel, Matthew W., Morton, Timothy D., Tinney, C. G., Zhang, Hui, Scott, Nicholas J., Matson, Rachel A., Everett, Mark E., Tokovinin, Andrei, Mann, Andrew W., Dragomir, Diana, Guenther, Maximilian N., Ting, Eric B., Fausnaugh, Michael, Glidden, Ana, Quintana, Elisa V., Manner, Mark, Marshall, Jennifer L., McLeod, Kim K., and Khakpash, Somayeh

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

We present the discoveries of KELT-25b (TIC 65412605, TOI-626.01) and KELT-26b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A-stars. The transit signals were initially detected by the KELT survey, and subsequently confirmed by \textit{TESS} photometry. KELT-25b is on a 4.40-day orbit around the V = 9.66 star CD-24 5016 ($T_{\rm eff} = 8280^{+440}_{-180}$ K, $M_{\star}$ = $2.18^{+0.12}_{-0.11}$ $M_{\odot}$), while KELT-26b is on a 3.34-day orbit around the V = 9.95 star HD 134004 ($T_{\rm eff}$ =$8640^{+500}_{-240}$ K, $M_{\star}$ = $1.93^{+0.14}_{-0.16}$ $M_{\odot}$), which is likely an Am star. We have confirmed the sub-stellar nature of both companions through detailed characterization of each system using ground-based and \textit{TESS} photometry, radial velocity measurements, Doppler Tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of $R_{\rm P}$ = $1.64^{+0.039}_{-0.043}$ $R_{\rm J}$, and a 3-sigma upper limit on the companion's mass of $\sim64~M_{\rm J}$. For KELT-26b, we infer a planetary mass and radius of $M_{\rm P}$ = $1.41^{+0.43}_{-0.51}$ $M_{\rm J}$ and $R_{\rm P}$ = $1.940^{+0.060}_{-0.058}$ $R_{\rm J}$. From Doppler Tomographic observations, we find KELT-26b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the \textit{TESS} data. KELT-25b appears to be in a well-aligned, prograde orbit, and the system is likely a member of a cluster or moving group., Comment: 24 pages, 18 figures, 8 tables

Published
2019
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21. TOI-677 b: A Warm Jupiter (P=11.2d) on an eccentric orbit transiting a late F-type star

Author

Jordán, Andrés, Brahm, Rafael, Espinoza, Néstor, Henning, Thomas, Jones, Matías I., Kossakowski, Diana, Sarkis, Paula, Trifonov, Trifon, Rojas, Felipe, Torres, Pascal, Drass, Holger, Nandakumar, Sangeetha, Barbieri, Mauro, Davis, Allen, Wang, Songhu, Bayliss, Daniel, Bouma, Luke, Dragomir, Diana, Eastman, Jason D., Daylan, Tansu, Guerrero, Natalia, Barclay, Thomas, Ting, Eric B., Henze, Christopher E., Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua, Jenkins, Jon M., Wittenmyer, Robert A., Bowler, Brendan P., Crossfield, Ian, Horner, Jonathan, Kane, Stephen R., Kielkopf, John F., Morton, Timothy D., Plavchan, Peter, Tinney, C. G., Addison, Brett, Mengel, Matthew W., Okumura, Jack, Shahaf, Sahar, Mazeh, Tsevi, Rabus, Markus, Shporer, Avi, Ziegler, Carl, Mann, Andrew W., and Hart, Rhodes

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

We report the discovery of TOI-677 b, first identified as a candidate in light curves obtained within Sectors 9 and 10 of the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed with radial velocities. TOI-677 b has a mass of M_p = 1.236$^{+0.069}_{-0.067}$ M_J, a radius of R_p = 1.170 +- 0.03 R_J,and orbits its bright host star (V=9.8 mag) with an orbital period of 11.23660 +- 0.00011 d, on an eccentric orbit with e = 0.435 +- 0.024. The host star has a mass of M_* = 1.181 +- 0.058 M_sun, a radius of R_* = 1.28 +- 0.03 R_sun, an age of 2.92$^{+0.80}_{-0.73}$ Gyr and solar metallicity, properties consistent with a main sequence late F star with T_eff = 6295 +- 77 K. We find evidence in the radial velocity measurements of a secondary long term signal which could be due to an outer companion. The TOI-677 b system is a well suited target for Rossiter-Mclaughlin observations that can constrain migration mechanisms of close-in giant planets., Comment: Submitted to AAS journals, 15 pages, 8 figures

Published
2019
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22. Do non-dipolar magnetic fields contribute to spin-down torques?

Author

See, Victor, Matt, Sean P., Finley, Adam J., Folsom, Colin P., Saikia, Sudeshna Boro, Donati, Jean-Francois, Fares, Rim, Hébrard, Élodie M., Jardine, Moira M., Jeffers, Sandra V., Marsden, Stephen C., Mengel, Matthew W., Morin, Julien, Petit, Pascal, Vidotto, Aline A., Waite, Ian A., and Collaboration, The BCool

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Main sequence low-mass stars are known to spin-down as a consequence of their magnetised stellar winds. However, estimating the precise rate of this spin-down is an open problem. The mass-loss rate, angular momentum-loss rate and the magnetic field properties of low-mass stars are fundamentally linked making this a challenging task. Of particular interest is the stellar magnetic field geometry. In this work, we consider whether non-dipolar field modes contribute significantly to the spin-down of low-mass stars. We do this using a sample of stars that have all been previously mapped with Zeeman-Doppler imaging. For a given star, as long as its mass-loss rate is below some critical mass-loss rate, only the dipolar fields contribute to its spin-down torque. However, if it has a larger mass-loss rate, higher order modes need to be considered. For each star, we calculate this critical mass-loss rate, which is a simple function of the field geometry. Additionally, we use two methods of estimating mass-loss rates for our sample of stars. In the majority of cases, we find that the estimated mass-loss rates do not exceed the critical mass-loss rate and hence, the dipolar magnetic field alone is sufficient to determine the spin-down torque. However, we find some evidence that, at large Rossby numbers, non-dipolar modes may start to contribute., Comment: 15 pages, 6 figures, 3 tables, accepted to ApJ

Published
2019
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23. TESS Hunt for Young and Maturing Exoplanets (THYME): A planet in the 45 Myr Tucana-Horologium association

Author

Newton, Elisabeth R., Mann, Andrew W., Tofflemire, Benjamin M., Pearce, Logan, Rizzuto, Aaron C., Vanderburg, Andrew, Martinez, Raquel A., Wang, Jason J., Ruffio, Jean-Baptiste, Kraus, Adam L., Johnson, Marshall C., Thao, Pa Chia, Wood, Mackenna L., Rampalli, Rayna, Nielsen, Eric L., Collins, Karen A., Dragomir, Diana, Hellier, Coel, Anderson, D. R., Barclay, Thomas, Brown, Carolyn, Feiden, Gregory, Hart, Rhodes, Isopi, Giovanni, Kielkopf, John F., Mallia, Franco, Nelson, Peter, Rodriguez, Joseph E., Stockdale, Chris, Waite, Ian A., Wright, Duncan J., Lissauer, Jack, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Bouma, Luke G., Burke, Christopher J., Davies, Misty, Fausnaugh, Michael, Li, Jie, Morris, Robert L., Mukai, Koji, Villaseñor, Joel, Villeneuva, Steven, De Rosa, Robert J., Macintosh, Bruce, Mengel, Matthew W., Okumura, Jack, and Wittenmyer, Robert A.

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

Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana-Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from SOAR/Goodman, SALT/HRS and LCO/NRES; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/GPI. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is $5.70\pm0.17$ Earth radii and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15 degrees to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V=8.5) for detailed characterization using radial velocities and transmission spectroscopy., Comment: Accepted to ApJ Letters 2019 June 11

Published
2019
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24. TESS Spots a Compact System of Super-Earths around the Naked-Eye Star HR 858

Author

Vanderburg, Andrew, Huang, Chelsea X., Rodriguez, Joseph E., Becker, Juliette C., Ricker, George R., Vanderspek, Roland K., Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett, Bieryla, Allyson, Briceño, Cesar, Bowler, Brendan P., Brown, Timothy M., Burke, Christopher J., Burt, Jennifer A., Caldwell, Douglas A., Clark, Jake T., Crossfield, Ian, Dittmann, Jason A., Dynes, Scott, Fulton, Benjamin J., Guerrero, Natalia, Harbeck, Daniel, Horner, Jonathan, Kane, Stephen R., Kielkopf, John, Kraus, Adam L., Kreidberg, Laura, Law, Nicolas, Mann, Andrew W., Mengel, Matthew W., Morton, Timothy D., Okumura, Jack, Pearce, Logan A., Plavchan, Peter, Quinn, Samuel N., Rabus, Markus, Rose, Mark E., Rowden, Pam, Shporer, Avi, Siverd, Robert J., Smith, Jeffrey C., Stassun, Keivan, Tinney, C. G., Wittenmyer, Rob, Wright, Duncan J., Zhang, Hui, Zhou, George, and Ziegler, Carl A.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Transiting Exoplanet Survey Satellite (TESS) observations have revealed a compact multi-planet system around the sixth-magnitude star HR 858 (TIC 178155732, TOI 396), located 32 parsecs away. Three planets, each about twice the size of Earth, transit this slightly-evolved, late F-type star, which is also a member of a visual binary. Two of the planets may be in mean motion resonance. We analyze the TESS observations, using novel methods to model and remove instrumental systematic errors, and combine these data with follow-up observations taken from a suite of ground-based telescopes to characterize the planetary system. The HR 858 planets are enticing targets for precise radial velocity observations, secondary eclipse spectroscopy, and measurements of the Rossiter-McLaughlin effect., Comment: Accepted for publication in ApJ Ltters. 11 pages, 4 figures, 2 tables. The systematics-corrected TESS light curve is included in the arXiv source code

Published
2019
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25. Estimating magnetic filling factors from Zeeman-Doppler magnetograms

Author

See, Victor, Matt, Sean P., Folsom, Colin P., Saikia, Sudeshna Boro, Donati, Jean-Francois, Fares, Rim, Finley, Adam J., Hebrard, Elodie M., Jardine, Moira M., Jeffers, Sandra V., Lehmann, Lisa T., Marsden, Stephen C., Mengel, Matthew W., Morin, Julien, Petit, Pascal, Vidotto, Aline A., Waite, Ian A., and collaboration, The BCool

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Low-mass stars are known to have magnetic fields that are believed to be of dynamo origin. Two complementary techniques are principally used to characterise them. Zeeman-Doppler imaging (ZDI) can determine the geometry of the large-scale magnetic field while Zeeman broadening can assess the total unsigned flux including that associated with small-scale structures such as spots. In this work, we study a sample of stars that have been previously mapped with ZDI. We show that the average unsigned magnetic flux follows an activity-rotation relation separating into saturated and unsaturated regimes. We also compare the average photospheric magnetic flux recovered by ZDI, $\langle B_V\rangle$, with that recovered by Zeeman broadening studies, $\langle B_I\rangle$. In line with previous studies, $\langle B_V\rangle$ ranges from a few % to $\sim$20% of $\langle B_I\rangle$. We show that a power law relationship between $\langle B_V\rangle$ and $\langle B_I\rangle$ exists and that ZDI recovers a larger fraction of the magnetic flux in more active stars. Using this relation, we improve on previous attempts to estimate filling factors, i.e. the fraction of the stellar surface covered with magnetic field, for stars mapped only with ZDI. Our estimated filling factors follow the well-known activity-rotation relation which is in agreement with filling factors obtained directly from Zeeman broadening studies. We discuss the possible implications of these results for flux tube expansion above the stellar surface and stellar wind models., Comment: 8 pages (main text), 3 additional pages (appendix), 4 figures, 2 tables

Published
2019
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26. Minerva-Australis I: Design, Commissioning, & First Photometric Results

Author

Addison, Brett, Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Mengel, Matthew W., Johns, Daniel, Marti, Connor, Nicholson, Belinda, Okumura, Jack, Bowler, Brendan, Crossfield, Ian, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Tinney, C. G., Zhang, Hui, Clark, Jake T., Clerte, Mathieu, Eastman, Jason D., Swift, Jon, Bottom, Michael, Muirhead, Philip, McCrady, Nate, Herzig, Erich, Hogstrom, Kristina, Wilson, Maurice, Sliski, David, Johnson, Samson A., Wright, Jason T., Blake, Cullen, Riddle, Reed, Lin, Brian, Cornachione, Matthew, Bedding, Timothy R., Stello, Dennis, Huber, Daniel, Marsden, Stephen, and Carter, Bradley D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Minerva-Australis telescope array is a facility dedicated to the follow-up, confirmation, characterisation, and mass measurement of bright transiting planets discovered by the Transiting Exoplanet Survey Satellite (TESS) -- a category in which it is almost unique in the southern hemisphere. It is located at the University of Southern Queensland's Mount Kent Observatory near Toowoomba, Australia. Its flexible design enables multiple 0.7m robotic telescopes to be used both in combination, and independently, for high-resolution spectroscopy and precision photometry of TESS transit planet candidates. Minerva-Australis also enables complementary studies of exoplanet spin-orbit alignments via Doppler observations of the Rossiter-McLaughlin effect, radial velocity searches for non-transiting planets, planet searches using transit timing variations, and ephemeris refinement for TESS planets. In this first paper, we describe the design, photometric instrumentation, software, and science goals of Minerva-Australis, and note key differences from its Northern hemisphere counterpart -- the Minerva array. We use recent transit observations of four planets--WASP-2b, WASP-44b, WASP-45b, and HD 189733b to demonstrate the photometric capabilities of Minerva-Australis., Comment: 33 pages, 7 figures, 5 tables. Published in PASP on November 2019

Published
2019
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27. MINERVA-Australis. I. Design, Commissioning, and First Photometric Results

Author

Addison, Brett, Wright, Duncan J., Wittenmyer, Robert A., Horner, Jonathan, Mengel, Matthew W., Johns, Daniel, Marti, Connor, Nicholson, Belinda, Soutter, Jack, Bowler, Brendan, Crossfield, Ian, Kane, Stephen R., Kielkopf, John, Plavchan, Peter, Tinney, C. G., Zhang, Hui, Clark, Jake T., Clerte, Mathieu, Eastman, Jason D., Swift, Jon, Bottom, Michael, Muirhead, Philip, McCrady, Nate, Herzig, Erich, Hogstrom, Kristina, Wilson, Maurice, Sliski, David, Johnson, Samson A., Wright, Jason T., Johnson, John Asher, Blake, Cullen, Riddle, Reed, Lin, Brian, Cornachione, Matthew, Bedding, Timothy R., Stello, Dennis, Huber, Daniel, Marsden, Stephen, and Carter, Bradley D.

Published
2019

28. 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, and Zhou, George

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, Space and Planetary Science, techniques: radial velocities, stars: individual: TOI-179, FOS: Physical sciences, Astronomy and Astrophysics, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
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, submitted to MNRAS

Published
2023

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

Author

Clark, Jake T., primary, Addison, Brett C., additional, Okumura, Jack, additional, Vach, Sydney, additional, Errico, Adriana, additional, Heitzmann, Alexis, additional, Rodriguez, Joseph E., additional, Wright, Duncan J., additional, Clerté, Mathieu, additional, Brown, Carolyn J., additional, Fetherolf, Tara, additional, Wittenmyer, Robert A., additional, Plavchan, Peter, additional, Kane, Stephen R., additional, Horner, Jonathan, additional, Kielkopf, John F., additional, Shporer, Avi, additional, Tinney, C. G., additional, Hui-Gen, Liu, additional, Ballard, Sarah, additional, Bowler, Brendan P., additional, Mengel, Matthew W., additional, Zhou, George, additional, Lee, Annette S., additional, David, Avelyn, additional, Heim, Jessica, additional, Lee, Michele E., additional, Sevilla, Verónica, additional, Zafar, Naqsh E., additional, Hinkel, Natalie R., additional, Allen, Bridgette E., additional, Bayliss, Daniel, additional, Berberyan, Arthur, additional, Berlind, Perry, additional, Bieryla, Allyson, additional, Bouchy, François, additional, Brahm, Rafael, additional, Bryant, Edward M., additional, Christiansen, Jessie L., additional, Ciardi, David R., additional, Ciardi, Krys N., additional, Collins, Karen A., additional, Dallant, Jules, additional, Davis, Allen B., additional, Díaz, Matías R., additional, Dressing, Courtney D., additional, Esquerdo, Gilbert A., additional, Harre, Jan-Vincent, additional, Howell, Steve B., additional, Jenkins, Jon M., additional, Jensen, Eric L. N., additional, Jones, Matías I., additional, Jordán, Andrés, additional, Latham, David W., additional, Lund, Michael B., additional, McCormac, James, additional, Nielsen, Louise D., additional, Otegi, Jon, additional, Quinn, Samuel N., additional, Radford, Don J., additional, Ricker, George R., additional, Schwarz, Richard P., additional, Seager, Sara, additional, Smith, Alexis M. S., additional, Stockdale, Chris, additional, Tan, Thiam-Guan, additional, Udry, Stéphane, additional, Vanderspek, Roland, additional, Günther, Maximilian N., additional, Wang, Songhu, additional, Wingham, Geof, additional, and Winn, Joshua N., additional

Published
2023
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30. Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

Author

Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, Winn, Joshua N., Clark, Jake T., Addison, Brett C., Okumura, Jack, Vach, Sydney, Heitzmann, Alexis, Rodriguez, Joseph E., Wright, Duncan J., Clerte, Mathieu, Brown, Carolyn J., Feterholf, Tara, Wittenmyer, Robert A., Plavchan, Peter, Kane, Stephen R., Horner, Jonathan, Kielkoff, John F., Shporer, Avi, Tinney, C. G., Hui-Gen, Liu, Ballard, Sarah, Bowler, Brendan P., Mengel, Matthew W., Zhou, George, Lee, Annette S., David, Avelyn, Heim, Jessica, Lee, Michele E., Sevilla, Veronica, Zafar, Naqsh E., Hinkel, Natalie R., Allen, Bridgette E., Bayliss, Daniel, Berberyan, Arthur, Berlind, Perry, Bieryla, Allyson, Bouchy, Francois, Brahm, Rafael, Bryant, Edward M., Christiansen, Jessie L., Ciardi, David R., Ciardi, Krys N., Collins, Karen A., Dallant, Jules, Davis, Allen B., Diaz, Matias R., Dressing, Courtney D., Esquerdo, Gilbert A., Harre, Jan-Vincent, Howell, Steve B., Jenkins, Jon M., Jensen, Eric L. N., Jones, Matias I., Jordan, Andres, Latham, David W., Lund, Michael B., McCormac, James, Nielsen, Louise D., Otegi, Jon, Quinn, Samuel N., Radford, Don J., Ricker, George R., Schwarz, Richard P., Seager, Sara, Smith, Alexis M. S., Stockdale, Chris, Tan, Thiam-Guan, Udry, Stephanie, Vanderspek, Roland, Gunther, Maximilian N., Wang, Songhu, Wingham, Geof, and Winn, Joshua N.

Abstract

NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (vsin(i)=35.1±1.0km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of 2.76+0.24−0.23Mjup, 1.370±0.043Rjup and ∼4.63 days, respectively. The planet orbits a bright (V=9.1mag) F3-dwarf with M=1.40±0.05Msun, R=1.70±0.05Rsun, and logg=4.05±0.17. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of 18∘±11∘, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.

Published
2023

31. Another shipment of six short-period giant planets from TESS

Author

Rodriguez, Joseph E, primary, Quinn, Samuel N, additional, Vanderburg, Andrew, additional, Zhou, George, additional, Eastman, Jason D, additional, Thygesen, Erica, additional, Cale, Bryson, additional, Ciardi, David R, additional, Reed, Phillip A, additional, Oelkers, Ryan J, additional, Collins, Karen A, additional, Bieryla, Allyson, additional, Latham, David W, additional, Gonzales, Erica J, additional, Scott Gaudi, B, additional, Hellier, Coel, additional, Jones, Matías I, additional, Brahm, Rafael, additional, Sokolovsky, Kirill, additional, Schulte, Jack, additional, Srdoc, Gregor, additional, Kielkopf, John, additional, Grau Horta, Ferran, additional, Massey, Bob, additional, Evans, Phil, additional, Stephens, Denise C, additional, McLeod, Kim K, additional, Chazov, Nikita, additional, Krushinsky, Vadim, additional, Ghachoui, Mourad, additional, Safonov, Boris S, additional, Dedrick, Cayla M, additional, Conti, Dennis, additional, Laloum, Didier, additional, Giacalone, Steven, additional, Ziegler, Carl, additional, Guerra Serra, Pere, additional, Naves Nogues, Ramon, additional, Murgas, Felipe, additional, Michaels, Edward J, additional, Ricker, George R, additional, Vanderspek, Roland K, additional, Seager, Sara, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Addison, Brett, additional, Alfaro, Owen, additional, Anderson, D R, additional, Aydi, Elias, additional, Beatty, Thomas G, additional, Bedding, Timothy R, additional, Belinski, Alexander A, additional, Benkhaldoun, Zouhair, additional, Berlind, Perry, additional, Blake, Cullen H, additional, Bowen, Michael J, additional, Bowler, Brendan P, additional, Boyle, Andrew W, additional, Branson, Dalton, additional, Briceño, César, additional, Calkins, Michael L, additional, Campbell, Emma, additional, Christiansen, Jessie L, additional, Chomiuk, Laura, additional, Collins, Kevin I, additional, Cornachione, Matthew A, additional, Daassou, Ahmed, additional, Dressing, Courtney D, additional, Esquerdo, Gilbert A, additional, Feliz, Dax L, additional, Fong, William, additional, Fukui, Akihiko, additional, Gan, Tianjun, additional, Gill, Holden, additional, Goliguzova, Maria V, additional, Hansen, Jarrod, additional, Henning, Thomas, additional, Hintz, Eric G, additional, Hobson, Melissa J, additional, Horner, Jonathan, additional, Huang, Chelsea X, additional, James, David J, additional, Jensen, Jacob S, additional, Johnson, Samson A, additional, Jordán, Andrés, additional, Kane, Stephen R, additional, Barkaoui, Khalid, additional, Kim, Myung-Jin, additional, Kim, Kingsley, additional, Kuhn, Rudolf B, additional, Law, Nicholas, additional, Lewin, Pablo, additional, Liu, Hui-Gen, additional, Lund, Michael B, additional, Mann, Andrew W, additional, McCrady, Nate, additional, Mengel, Matthew W, additional, Mink, Jessica, additional, Murphy, Lauren G, additional, Narita, Norio, additional, Newman, Patrick, additional, Okumura, Jack, additional, Osborn, Hugh P, additional, Paegert, Martin, additional, Palle, Enric, additional, Pepper, Joshua, additional, Plavchan, Peter, additional, Popov, Alexander A, additional, Rabus, Markus, additional, Ranshaw, Jessica, additional, Rodriguez, Jennifer A, additional, Roh, Dong-Goo, additional, Reefe, Michael A, additional, Savel, Arjun B, additional, Schwarz, Richard P, additional, Shporer, Avi, additional, Siverd, Robert J, additional, Sliski, David H, additional, Stassun, Keivan G, additional, Stevens, Daniel J, additional, Soubkiou, Abderahmane, additional, Ting, Eric B, additional, Tinney, C G, additional, Vowell, Noah, additional, Walton, Payton, additional, West, R G, additional, Wilson, Maurice L, additional, Wittenmyer, Robert A, additional, Wittrock, Justin M, additional, Wolf, Shania, additional, Wright, Jason T, additional, Zhang, Hui, additional, and Zobel, Evan, additional

Published
2023
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32. TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs

Author

El Mufti, Mohammed, primary, Plavchan, Peter P., additional, Isaacson, Howard, additional, Cale, Bryson L., additional, Feliz, Dax L., additional, Reefe, Michael A., additional, Hellier, Coel, additional, Stassun, Keivan, additional, Eastman, Jason, additional, Polanski, Alex, additional, Crossfield, Ian J. M., additional, Gaidos, Eric, additional, Kostov, Veselin, additional, Wittrock, Justin M., additional, Villaseñor, Joel, additional, Schlieder, Joshua E., additional, Bouma, Luke G., additional, Collins, Kevin I., additional, Zohrabi, Farzaneh, additional, Lee, Rena A., additional, Sohani, Ahmad, additional, Berberian, John, additional, Vermilion, David, additional, Newman, Patrick, additional, Geneser, Claire, additional, Tanner, Angelle, additional, Batalha, Natalie M., additional, Dressing, Courtney, additional, Fulton, Benjamin, additional, Howard, Andrew W., additional, Huber, Daniel, additional, Kane, Stephen R., additional, Petigura, Erik A., additional, Robertson, Paul, additional, Roy, Arpita, additional, Weiss, Lauren M., additional, Behmard, Aida, additional, Beard, Corey, additional, Chontos, Ashley, additional, Dai, Fei, additional, Dalba, Paul A., additional, Fetherolf, Tara, additional, Giacalone, Steven, additional, Hill, Michelle L., additional, Hirsch, Lea A., additional, Holcomb, Rae, additional, Lubin, Jack, additional, Mayo, Andrew, additional, Močnik, Teo, additional, Akana Murphy, Joseph M., additional, Rosenthal, Lee J., additional, Rubenzahl, Ryan A., additional, Scarsdale, Nicholas, additional, Stockdale, Christopher, additional, Collins, Karen, additional, Cloutier, Ryan, additional, Relles, Howard, additional, Tan, Thiam-Guan, additional, Scott, Nicholas J, additional, Hartman, Zach, additional, Matthews, Elisabeth, additional, Ciardi, David R., additional, Gonzales, Erica, additional, Matson, Rachel A., additional, Beichman, Charles, additional, Bieryla, Allyson, additional, Furlan, E., additional, Gnilka, Crystal L., additional, Howell, Steve B., additional, Ziegler, Carl, additional, Briceño, César, additional, Law, Nicholas, additional, Mann, Andrew W., additional, Rabus, Markus, additional, Johnson, Marshall C., additional, Christiansen, Jessie, additional, Kreidberg, Laura, additional, Berardo, David Anthony, additional, Deming, Drake, additional, Gorjian, Varoujan, additional, Morales, Farisa Y., additional, Benneke, Björn, additional, Dragomir, Diana, additional, Wittenmyer, Robert A., additional, Ballard, Sarah, additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kielkopf, John, additional, Liu, Huigen, additional, Shporer, Avi, additional, Tinney, C. G., additional, Zhang, Hui, additional, Wright, Duncan J., additional, Addison, Brett C., additional, Mengel, Matthew W., additional, and Okumura, Jack, additional

Published
2022
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33. A dense mini-Neptune orbiting the bright young star HD 18599

Author

Vines, Jose I, primary, Jenkins, James S, additional, Berdiñas, Zaira, additional, Soto, Maritza G, additional, Díaz, Matías R, additional, Alves, Douglas R, additional, Tuomi, Mikko, additional, Wittenmyer, Robert A, additional, de Leon, Jerome Pitogo, additional, Peña, Pablo, additional, Lissauer, Jack J, additional, Ballard, Sarah, additional, Bedding, Timothy, additional, Bowler, Brendan P, additional, Horner, Jonathan, additional, Jones, Hugh R A, additional, Kane, Stephen R, additional, Kielkopf, John, additional, Plavchan, Peter, additional, Shporer, Avi, additional, Tinney, C G, additional, Zhang, Hui, additional, Wright, Duncan J, additional, Addison, Brett, additional, Mengel, Matthew W, additional, Okumura, Jack, additional, and Samadi-Ghadim, Anya, additional

Published
2022
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34. The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Author

Yee, Samuel W., primary, Winn, Joshua N., additional, Hartman, Joel D., additional, Rodriguez, Joseph E., additional, Zhou, George, additional, Quinn, Samuel N., additional, Latham, David W., additional, Bieryla, Allyson, additional, Collins, Karen A., additional, Addison, Brett C., additional, Angelo, Isabel, additional, Barkaoui, Khalid, additional, Benni, Paul, additional, Boyle, Andrew W., additional, Brahm, Rafael, additional, Butler, R. Paul, additional, Ciardi, David R., additional, Collins, Kevin I., additional, Conti, Dennis M., additional, Crane, Jeffrey D., additional, Dai, Fei, additional, Dressing, Courtney D., additional, Eastman, Jason D., additional, Essack, Zahra, additional, Forés-Toribio, Raquel, additional, Furlan, Elise, additional, Gan, Tianjun, additional, Giacalone, Steven, additional, Gill, Holden, additional, Girardin, Eric, additional, Henning, Thomas, additional, Henze, Christopher E., additional, Hobson, Melissa J., additional, Horner, Jonathan, additional, Howard, Andrew W., additional, Howell, Steve B., additional, Huang, Chelsea X., additional, Isaacson, Howard, additional, Jenkins, Jon M., additional, Jensen, Eric L. N., additional, Jordán, Andrés, additional, Kane, Stephen R., additional, Kielkopf, John F., additional, Lasota, Slawomir, additional, Levine, Alan M., additional, Lubin, Jack, additional, Mann, Andrew W., additional, Massey, Bob, additional, McLeod, Kim K., additional, Mengel, Matthew W., additional, Muñoz, Jose A., additional, Murgas, Felipe, additional, Palle, Enric, additional, Plavchan, Peter, additional, Popowicz, Adam, additional, Radford, Don J., additional, Ricker, George R., additional, Rowden, Pamela, additional, Safonov, Boris S., additional, Savel, Arjun B., additional, Schwarz, Richard P., additional, Seager, S., additional, Sefako, Ramotholo, additional, Shporer, Avi, additional, Srdoc, Gregor, additional, Strakhov, Ivan S., additional, Teske, Johanna K., additional, Tinney, C. G., additional, Tyler, Dakotah, additional, Wittenmyer, Robert A., additional, Zhang, Hui, additional, and Ziegler, Carl, additional

Published
2022
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35. A Mini-Neptune from TESS and CHEOPS Around the 120 Myr Old AB Dor Member HIP 94235

Author

Zhou, George, primary, Wirth, Christopher P., additional, Huang, Chelsea X., additional, Venner, Alexander, additional, Franson, Kyle, additional, Quinn, Samuel N., additional, Bouma, L. G., additional, Kraus, Adam L., additional, Mann, Andrew W., additional, Newton, Elisabeth. R., additional, Dragomir, Diana, additional, Heitzmann, Alexis, additional, Lowson, Nataliea, additional, Douglas, Stephanie T., additional, Battley, Matthew, additional, Gillen, Edward, additional, Triaud, Amaury, additional, Latham, David W., additional, Howell, Steve B., additional, Hartman, J. D., additional, Tofflemire, Benjamin M., additional, Wittenmyer, Robert A., additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Plavchan, Peter, additional, Wright, Duncan J., additional, Addison, Brett C., additional, Mengel, Matthew W., additional, Okumura, Jack, additional, Ricker, George, additional, Vanderspek, Roland, additional, Seager, Sara, additional, Jenkins, Jon M., additional, Winn, Joshua N., additional, Daylan, Tansu, additional, Fausnaugh, Michael, additional, and Kunimoto, Michelle, additional

Published
2022
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36. HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit

Author

Errico, Adriana, primary, Wittenmyer, Robert A., additional, Horner, Jonathan, additional, Li, Zhexing, additional, Brandt, G. Mirek, additional, Kane, Stephen R., additional, Fetherolf, Tara, additional, Holt, Timothy R., additional, Carter, Brad, additional, Clark, Jake T., additional, Butler, R. P., additional, Tinney, C. G., additional, Ballard, Sarah, additional, Bowler, Brendan P., additional, Kielkopf, John, additional, Liu, Huigen, additional, Plavchan, Peter P., additional, Shporer, Avi, additional, Zhang, Hui, additional, Wright, Duncan J., additional, Addison, Brett C., additional, Mengel, Matthew W., additional, and Okumura, Jack, additional

Published
2022
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37. TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant

Author

Wittenmyer, Robert A., primary, Clark, Jake T., additional, Trifonov, Trifon, additional, Addison, Brett C., additional, Wright, Duncan J., additional, Stassun, Keivan G., additional, Horner, Jonathan, additional, Lowson, Nataliea, additional, Kielkopf, John, additional, Kane, Stephen R., additional, Plavchan, Peter, additional, Shporer, Avi, additional, Zhang, Hui, additional, Bowler, Brendan P., additional, Mengel, Matthew W., additional, Okumura, Jack, additional, Rabus, Markus, additional, Johnson, Marshall C., additional, Harbeck, Daniel, additional, Tronsgaard, René, additional, Buchhave, Lars A., additional, Collins, Karen A., additional, Collins, Kevin I., additional, Gan, Tianjun, additional, Jensen, Eric L. N., additional, Howell, Steve B., additional, Furlan, E., additional, Gnilka, Crystal L., additional, Lester, Kathryn V., additional, Matson, Rachel A., additional, Scott, Nicholas J., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Rudat, Alexander, additional, Quintana, Elisa V., additional, Rodriguez, David R., additional, Caldwell, Douglas A., additional, Quinn, Samuel N., additional, Essack, Zahra, additional, and Bouma, Luke G., additional

Published
2022
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38. TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration

Author

Dong, Jiayin, primary, Huang, Chelsea X., additional, Zhou, George, additional, Dawson, Rebekah I., additional, Rodriguez, Joseph E., additional, Eastman, Jason D., additional, Collins, Karen A., additional, Quinn, Samuel N., additional, Shporer, Avi, additional, Triaud, Amaury H. M. J., additional, Wang, Songhu, additional, Beatty, Thomas, additional, Jackson, Jonathon M., additional, Collins, Kevin I., additional, Abe, Lyu, additional, Suarez, Olga, additional, Crouzet, Nicolas, additional, Mékarnia, Djamel, additional, Dransfield, Georgina, additional, Jensen, Eric L. N., additional, Stockdale, Chris, additional, Barkaoui, Khalid, additional, Heitzmann, Alexis, additional, Wright, Duncan J., additional, Addison, Brett C., additional, Wittenmyer, Robert A., additional, Okumura, Jack, additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Liu, Huigen, additional, Plavchan, Peter, additional, Mengel, Matthew W., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Christiansen, Jessie L., additional, and Paegert, Martin, additional

Published
2021
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39. The Youngest Planet to Have a Spin-Orbit Alignment Measurement AU Mic b

Author

Addison, Brett C., primary, Horner, Jonathan, additional, Wittenmyer, Robert A., additional, Heitzmann, Alexis, additional, Plavchan, Peter, additional, Wright, Duncan J., additional, Nicholson, Belinda A., additional, Marshall, Jonathan P., additional, Clark, Jake T., additional, Günther, Maximilian N., additional, Kane, Stephen R., additional, Hirano, Teruyuki, additional, Wang, Songhu, additional, Kielkopf, John, additional, Shporer, Avi, additional, Tinney, C. G., additional, Zhang, Hui, additional, Ballard, Sarah, additional, Bedding, Timothy, additional, Bowler, Brendan P., additional, Mengel, Matthew W., additional, Okumura, Jack, additional, Gaidos, Eric, additional, and Wang, Xian-Yu, additional

Published
2021
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40. 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, primary, Armstrong, David J, additional, Cale, Bryson, additional, Brahm, Rafael, additional, Wittenmyer, Robert A, additional, Dai, Fei, additional, Crossfield, Ian J M, additional, Bryant, Edward M, additional, Adibekyan, Vardan, additional, Cloutier, Ryan, additional, Collins, Karen A, additional, Delgado Mena, E, additional, Fridlund, Malcolm, additional, Hellier, Coel, additional, Howell, Steve B, additional, King, George W, additional, Lillo-Box, Jorge, additional, Otegi, Jon, additional, Sousa, S, additional, Stassun, Keivan G, additional, Matthews, Elisabeth C, additional, Ziegler, Carl, additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David W, additional, Seager, S, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Acton, Jack S, additional, Addison, Brett C, additional, Anderson, David R, additional, Ballard, Sarah, additional, Barrado, David, additional, Barros, Susana C C, additional, Batalha, Natalie, additional, Bayliss, Daniel, additional, Barclay, Thomas, additional, Benneke, Björn, additional, Berberian, John, additional, Bouchy, Francois, additional, Bowler, Brendan P, additional, Briceño, César, additional, Burke, Christopher J, additional, Burleigh, Matthew R, additional, Casewell, Sarah L, additional, Ciardi, David, additional, Collins, Kevin I, additional, Cooke, Benjamin F, additional, Demangeon, Olivier D S, additional, Díaz, Rodrigo F, additional, Dorn, C, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Dumusque, Xavier, additional, Espinoza, Néstor, additional, Figueira, P, additional, Fulton, Benjamin, additional, Furlan, E, additional, Gaidos, E, additional, Geneser, C, additional, Gill, Samuel, additional, Goad, Michael R, additional, Gonzales, Erica J, additional, Gorjian, Varoujan, additional, Günther, Maximilian N, additional, Helled, Ravit, additional, Henderson, Beth A, additional, Henning, Thomas, additional, Hogan, Aleisha, additional, Hojjatpanah, Saeed, additional, Horner, Jonathan, additional, Howard, Andrew W, additional, Hoyer, Sergio, additional, Huber, Dan, additional, Isaacson, Howard, additional, Jenkins, James S, additional, Jensen, Eric L N, additional, Jordán, Andrés, additional, Kane, Stephen R, additional, Kidwell, Richard C, additional, Kielkopf, John, additional, Law, Nicholas, additional, Lendl, Monika, additional, Lund, M, additional, Matson, Rachel A, additional, Mann, Andrew W, additional, McCormac, James, additional, Mengel, Matthew W, additional, Morales, Farisa Y, additional, Nielsen, Louise D, additional, Okumura, Jack, additional, Osborn, Hugh P, additional, Petigura, Erik A, additional, Plavchan, Peter, additional, Pollacco, Don, additional, Quintana, Elisa V, additional, Raynard, Liam, additional, Robertson, Paul, additional, Rose, Mark E, additional, Roy, Arpita, additional, Reefe, Michael, additional, Santerne, Alexandre, additional, Santos, Nuno C, additional, Sarkis, Paula, additional, Schlieder, J, additional, Schwarz, Richard P, additional, Scott, Nicholas J, additional, Shporer, Avi, additional, Smith, A M S, additional, Stibbard, C, additional, Stockdale, Chris, additional, Strøm, Paul A, additional, Twicken, Joseph D, additional, Tan, Thiam-Guan, additional, Tanner, A, additional, Teske, J, additional, Tilbrook, Rosanna H, additional, Tinney, C G, additional, Udry, Stephane, additional, Villaseñor, Jesus Noel, additional, Vines, Jose I, additional, Wang, Sharon X, additional, Weiss, Lauren M, additional, West, Richard G, additional, Wheatley, Peter J, additional, Wright, Duncan J, additional, Zhang, Hui, additional, and Zohrabi, F, additional

Published
2021
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41. HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS

Author

Gan, Tianjun, primary, Bedell, Megan, additional, Wang, Sharon Xuesong, additional, Foreman-Mackey, Daniel, additional, Meléndez, Jorge, additional, Mao, Shude, additional, Stassun, Keivan G, additional, Howell, Steve B, additional, Ziegler, Carl, additional, Wittenmyer, Robert A, additional, Hellier, Coel, additional, Collins, Karen A, additional, Shporer, Avi, additional, Ricker, George R, additional, Vanderspek, Roland, additional, Latham, David W, additional, Seager, Sara, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Addison, Brett C, additional, Ballard, Sarah, additional, Barclay, Thomas, additional, Bean, Jacob L, additional, Bowler, Brendan P, additional, Briceño, César, additional, Crossfield, Ian J M, additional, Dittman, Jason, additional, Horner, Jonathan, additional, Jensen, Eric L N, additional, Kane, Stephen R, additional, Kielkopf, John, additional, Kreidberg, Laura, additional, Law, Nicholas, additional, Mann, Andrew W, additional, Mengel, Matthew W, additional, Morgan, Edward H, additional, Okumura, Jack, additional, Osborn, Hugh P, additional, Paegert, Martin, additional, Plavchan, Peter, additional, Schwarz, Richard P, additional, Shiao, Bernie, additional, Smith, Jeffrey C, additional, Spina, Lorenzo, additional, Tinney, C G, additional, Torres, Guillermo, additional, Twicken, Joseph D, additional, Vezie, Michael, additional, Wang, Gavin, additional, Wright, Duncan J, additional, and Zhang, Hui, additional

Published
2021
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42. 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

43. A Transiting Warm Giant Planet around the Young Active Star TOI-201

Author

Hobson, Melissa J., primary, Brahm, Rafael, additional, Jordán, Andrés, additional, Espinoza, Nestor, additional, Kossakowski, Diana, additional, Henning, Thomas, additional, Rojas, Felipe, additional, Schlecker, Martin, additional, Sarkis, Paula, additional, Trifonov, Trifon, additional, Thorngren, Daniel, additional, Binnenfeld, Avraham, additional, Shahaf, Sahar, additional, Zucker, Shay, additional, Ricker, George R., additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Addison, Brett, additional, Bouchy, François, additional, Bowler, Brendan P., additional, Briegal, Joshua T., additional, Bryant, Edward M., additional, Collins, Karen A., additional, Daylan, Tansu, additional, Grieves, Nolan, additional, Horner, Jonathan, additional, Huang, Chelsea, additional, Kane, Stephen R., additional, Kielkopf, John, additional, McLean, Brian, additional, Mengel, Matthew W., additional, Nielsen, Louise D., additional, Okumura, Jack, additional, Jones, Matias, additional, Plavchan, Peter, additional, Shporer, Avi, additional, Smith, Alexis M. S., additional, Tilbrook, Rosanna, additional, Tinney, C. G., additional, Twicken, Joseph D., additional, Udry, Stéphane, additional, Unger, Nicolas, additional, West, Richard, additional, Wittenmyer, Robert A., additional, Wohler, Bill, additional, Torres, Pascal, additional, and Wright, Duncan J., additional

Published
2021
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44. TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images

Author

Rodriguez, Joseph E., primary, Quinn, Samuel N., additional, Zhou, George, additional, Vanderburg, Andrew, additional, Nielsen, Louise D., additional, Wittenmyer, Robert A., additional, Brahm, Rafael, additional, Reed, Phillip A., additional, Huang, Chelsea X., additional, Vach, Sydney, additional, Ciardi, David R., additional, Oelkers, Ryan J., additional, Stassun, Keivan G., additional, Hellier, Coel, additional, Gaudi, B. Scott, additional, Eastman, Jason D., additional, Collins, Karen A., additional, Bieryla, Allyson, additional, Christian, Sam, additional, Latham, David W., additional, Carleo, Ilaria, additional, Wright, Duncan J., additional, Matthews, Elisabeth, additional, Gonzales, Erica J., additional, Ziegler, Carl, additional, Dressing, Courtney D., additional, Howell, Steve B., additional, Tan, Thiam-Guan, additional, Wittrock, Justin, additional, Plavchan, Peter, additional, McLeod, Kim K., additional, Baker, David, additional, Wang, Gavin, additional, Radford, Don J., additional, Schwarz, Richard P., additional, Esposito, Massimiliano, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Addison, Brett, additional, Anderson, D. R., additional, Barclay, Thomas, additional, Beatty, Thomas G., additional, Berlind, Perry, additional, Bouchy, Francois, additional, Bowen, Michael, additional, Bowler, Brendan P., additional, Brasseur, C. E., additional, Briceño, César, additional, Caldwell, Douglas A., additional, Calkins, Michael L., additional, Cartwright, Scott, additional, Chaturvedi, Priyanka, additional, Chaverot, Guillaume, additional, Chimaladinne, Sudhish, additional, Christiansen, Jessie L., additional, Collins, Kevin I., additional, Crossfield, Ian J. M., additional, Eastridge, Kevin, additional, Espinoza, Néstor, additional, Esquerdo, Gilbert A., additional, Feliz, Dax L., additional, Fenske, Tyler, additional, Fong, William, additional, Gan, Tianjun, additional, Giacalone, Steven, additional, Gill, Holden, additional, Gordon, Lindsey, additional, Granados, A., additional, Grieves, Nolan, additional, Guenther, Eike W., additional, Guerrero, Natalia, additional, Henning, Thomas, additional, Henze, Christopher E., additional, Hesse, Katharine, additional, Hobson, Melissa J., additional, Horner, Jonathan, additional, James, David J., additional, Jensen, Eric L. N., additional, Jimenez, Mary, additional, Jordán, Andrés, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Kim, Kingsley, additional, Kuhn, Rudolf B., additional, Latouf, Natasha, additional, Law, Nicholas M., additional, Levine, Alan M., additional, Lund, Michael B., additional, Mann, Andrew W., additional, Mao, Shude, additional, Matson, Rachel A., additional, Mengel, Matthew W., additional, Mink, Jessica, additional, Newman, Patrick, additional, O’Dwyer, Tanner, additional, Okumura, Jack, additional, Palle, Enric, additional, Pepper, Joshua, additional, Quintana, Elisa V., additional, Sarkis, Paula, additional, Savel, Arjun B., additional, Schlieder, Joshua E., additional, Schnaible, Chloe, additional, Shporer, Avi, additional, Sefako, Ramotholo, additional, Seidel, Julia V., additional, Siverd, Robert J., additional, Skinner, Brett, additional, Stalport, Manu, additional, Stevens, Daniel J., additional, Stibbards, Caitlin, additional, Tinney, C. G., additional, West, R. G., additional, Yahalomi, Daniel A., additional, and Zhang, Hui, additional

Published
2021
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45. TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to Inflation

Author

Sha, Lizhou, primary, Huang, Chelsea X., additional, Shporer, Avi, additional, Rodriguez, Joseph E., additional, Vanderburg, Andrew, additional, Brahm, Rafael, additional, Hagelberg, Janis, additional, Matthews, Elisabeth C., additional, Ziegler, Carl, additional, Livingston, John H., additional, Stassun, Keivan G., additional, Wright, Duncan J., additional, Crane, Jeffrey D., additional, Espinoza, Néstor, additional, Bouchy, François, additional, Bakos, Gáspár Á., additional, Collins, Karen A., additional, Zhou, George, additional, Bieryla, Allyson, additional, Hartman, Joel D., additional, Wittenmyer, Robert A., additional, Nielsen, Louise D., additional, Plavchan, Peter, additional, Bayliss, Daniel, additional, Sarkis, Paula, additional, Tan, Thiam-Guan, additional, Cloutier, Ryan, additional, Mancini, Luigi, additional, Jordán, Andrés, additional, Wang, Sharon, additional, Henning, Thomas, additional, Narita, Norio, additional, Penev, Kaloyan, additional, Teske, Johanna K., additional, Kane, Stephen R., additional, Mann, Andrew W., additional, Addison, Brett C., additional, Tamura, Motohide, additional, Horner, Jonathan, additional, Barbieri, Mauro, additional, Burt, Jennifer A., additional, Díaz, Matías R., additional, Crossfield, Ian J. M., additional, Dragomir, Diana, additional, Drass, Holger, additional, Feinstein, Adina D., additional, Zhang, Hui, additional, Hart, Rhodes, additional, Kielkopf, John F., additional, Jensen, Eric L. N., additional, Montet, Benjamin T., additional, Ottoni, Gaël, additional, Schwarz, Richard P., additional, Rojas, Felipe, additional, Nespral, David, additional, Torres, Pascal, additional, Mengel, Matthew W., additional, Udry, Stéphane, additional, Zapata, Abner, additional, Snoddy, Erin, additional, Okumura, Jack, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Latham, David W., additional, Winn, Joshua N., additional, Seager, Sara, additional, Jenkins, Jon M., additional, Colón, Knicole D., additional, Henze, Christopher E., additional, Krishnamurthy, Akshata, additional, Ting, Eric B., additional, Vezie, Michael, additional, and Villanueva, Steven, additional

Published
2021
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46. TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star

Author

Addison, Brett C, primary, Wright, Duncan J, additional, Nicholson, Belinda A, additional, Cale, Bryson, additional, Mocnik, Teo, additional, Huber, Daniel, additional, Plavchan, Peter, additional, Wittenmyer, Robert A, additional, Vanderburg, Andrew, additional, Chaplin, William J, additional, Chontos, Ashley, additional, Clark, Jake T, additional, Eastman, Jason D, additional, Ziegler, Carl, additional, Brahm, Rafael, additional, Carter, Bradley D, additional, Clerte, Mathieu, additional, Espinoza, Néstor, additional, Horner, Jonathan, additional, Bentley, John, additional, Jordán, Andrés, additional, Kane, Stephen R, additional, Kielkopf, John F, additional, Laychock, Emilie, additional, Mengel, Matthew W, additional, Okumura, Jack, additional, Stassun, Keivan G, additional, Bedding, Timothy R, additional, Bowler, Brendan P, additional, Burnelis, Andrius, additional, Blanco-Cuaresma, Sergi, additional, Collins, Michaela, additional, Crossfield, Ian, additional, Davis, Allen B, additional, Evensberget, Dag, additional, Heitzmann, Alexis, additional, Howell, Steve B, additional, Law, Nicholas, additional, Mann, Andrew W, additional, Marsden, Stephen C, additional, Matson, Rachel A, additional, O’Connor, James H, additional, Shporer, Avi, additional, Stevens, Catherine, additional, Tinney, C G, additional, Tylor, Christopher, additional, Wang, Songhu, additional, Zhang, Hui, additional, Henning, Thomas, additional, Kossakowski, Diana, additional, Ricker, George, additional, Sarkis, Paula, additional, Schlecker, Martin, additional, Torres, Pascal, additional, Vanderspek, Roland, additional, Latham, David W, additional, Seager, Sara, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Mireles, Ismael, additional, Rowden, Pam, additional, Pepper, Joshua, additional, Daylan, Tansu, additional, Schlieder, Joshua E, additional, Collins, Karen A, additional, Collins, Kevin I, additional, Tan, Thiam-Guan, additional, Ball, Warrick H, additional, Basu, Sarbani, additional, Buzasi, Derek L, additional, Campante, Tiago L, additional, Corsaro, Enrico, additional, González-Cuesta, L, additional, Davies, Guy R, additional, de Almeida, Leandro, additional, do Nascimento, Jose-Dias, additional, García, Rafael A, additional, Guo, Zhao, additional, Handberg, Rasmus, additional, Hekker, Saskia, additional, Hey, Daniel R, additional, Kallinger, Thomas, additional, Kawaler, Steven D, additional, Kayhan, Cenk, additional, S. Kuszlewicz, James, additional, Lund, Mikkel N, additional, Lyttle, Alexander, additional, Mathur, Savita, additional, Miglio, Andrea, additional, Mosser, Benoit, additional, Nielsen, Martin B, additional, Serenelli, Aldo M, additional, Aguirre, Victor Silva, additional, and Themeßl, Nathalie, additional

Published
2020
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47. TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite

Author

Brahm, Rafael, primary, Nielsen, Louise D., additional, Wittenmyer, Robert A., additional, Wang, Songhu, additional, Rodriguez, Joseph E., additional, Espinoza, Néstor, additional, Jones, Matías I., additional, Jordán, Andrés, additional, Henning, Thomas, additional, Hobson, Melissa, additional, Kossakowski, Diana, additional, Rojas, Felipe, additional, Sarkis, Paula, additional, Schlecker, Martin, additional, Trifonov, Trifon, additional, Shahaf, Sahar, additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Addison, Brett C., additional, Bakos, Gáspár Á., additional, Bhatti, Waqas, additional, Bayliss, Daniel, additional, Berlind, Perry, additional, Bieryla, Allyson, additional, Bouchy, Francois, additional, Bowler, Brendan P., additional, Briceño, César, additional, Brown, Timothy M., additional, Bryant, Edward M., additional, Caldwell, Douglas A., additional, Charbonneau, David, additional, Collins, Karen A., additional, Davis, Allen B., additional, Esquerdo, Gilbert A., additional, Fulton, Benjamin J., additional, Guerrero, Natalia M., additional, Henze, Christopher E., additional, Hogan, Aleisha, additional, Horner, Jonathan, additional, Huang, Chelsea X., additional, Irwin, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Mann, Andrew W., additional, Mazeh, Tsevi, additional, McCormac, James, additional, McCully, Curtis, additional, Mengel, Matthew W., additional, Mireles, Ismael, additional, Okumura, Jack, additional, Plavchan, Peter, additional, Quinn, Samuel N., additional, Rabus, Markus, additional, Saesen, Sophie, additional, Schlieder, Joshua E., additional, Segransan, Damien, additional, Shiao, Bernie, additional, Shporer, Avi, additional, Siverd, Robert J., additional, Stassun, Keivan G., additional, Suc, Vincent, additional, Tan, Thiam-Guan, additional, Torres, Pascal, additional, Tinney, Chris G., additional, Udry, Stephane, additional, Vanzi, Leonardo, additional, Vezie, Michael, additional, Vines, Jose I., additional, Vuckovic, Maja, additional, Wright, Duncan J., additional, Yahalomi, Daniel A., additional, Zapata, Abner, additional, Zhang, Hui, additional, and Ziegler, Carl, additional

Published
2020
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48. KELT-25 b and KELT-26 b: A Hot Jupiter and a Substellar Companion Transiting Young A Stars Observed by TESS*

Author

Martínez, Romy Rodríguez, primary, Gaudi, B. Scott, additional, Rodriguez, Joseph E., additional, Zhou, George, additional, Labadie-Bartz, Jonathan, additional, Quinn, Samuel N., additional, Penev, Kaloyan, additional, Tan, Thiam-Guan, additional, Latham, David W., additional, Paredes, Leonardo A., additional, Kielkopf, John F., additional, Addison, Brett, additional, Wright, Duncan J., additional, Teske, Johanna, additional, Howell, Steve B., additional, Ciardi, David, additional, Ziegler, Carl, additional, Stassun, Keivan G., additional, Johnson, Marshall C., additional, Eastman, Jason D., additional, Siverd, Robert J., additional, Beatty, Thomas G., additional, Bouma, Luke, additional, Bedding, Timothy, additional, Pepper, Joshua, additional, Winn, Joshua, additional, Lund, Michael B., additional, Villanueva, Steven, additional, Stevens, Daniel J., additional, Jensen, Eric L. N., additional, Kilby, Coleman, additional, Crane, Jeffrey D., additional, Tokovinin, Andrei, additional, Everett, Mark E., additional, Tinney, C. G., additional, Fausnaugh, Michael, additional, Cohen, David H., additional, Bayliss, Daniel, additional, Bieryla, Allyson, additional, Cargile, Phillip A., additional, Collins, Karen A., additional, Conti, Dennis M., additional, Colón, Knicole D., additional, Curtis, Ivan A., additional, Depoy, D. L., additional, Evans, Phil, additional, Feliz, Dax L., additional, Gregorio, Joao, additional, Rothenberg, Jason, additional, James, David J., additional, Joner, Michael D., additional, Kuhn, Rudolf B., additional, Manner, Mark, additional, Khakpash, Somayeh, additional, Marshall, Jennifer L., additional, McLeod, Kim K., additional, Penny, Matthew T., additional, Reed, Phillip A., additional, Relles, Howard M., additional, Stephens, Denise C., additional, Stockdale, Chris, additional, Trueblood, Mark, additional, Trueblood, Pat, additional, Yao, Xinyu, additional, Zambelli, Roberto, additional, Vanderspek, Roland, additional, Seager, Sara, additional, Jenkins, Jon M., additional, Henry, Todd J., additional, James, Hodari-Sadiki, additional, Jao, Wei-Chun, additional, Wang, Sharon Xuesong, additional, Butler, Paul, additional, Thompson, Ian, additional, Shectman, Stephen, additional, Wittenmyer, Robert, additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Mengel, Matthew W., additional, Morton, Timothy D., additional, Okumura, Jack, additional, Plavchan, Peter, additional, Zhang, Hui, additional, Scott, Nicholas J., additional, Matson, Rachel A., additional, Mann, Andrew W., additional, Dragomir, Diana, additional, Günther, Max, additional, Ting, Eric B., additional, Glidden, Ana, additional, and Quintana, Elisa V., additional

Published
2020
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49. TOI-677b: A Warm Jupiter (P= 11.2 days) on an Eccentric Orbit Transiting a Late F-type Star

Author

Jordán, Andrés, primary, Brahm, Rafael, additional, Espinoza, Néstor, additional, Henning, Thomas, additional, Jones, Matías I., additional, Kossakowski, Diana, additional, Sarkis, Paula, additional, Trifonov, Trifon, additional, Rojas, Felipe, additional, Torres, Pascal, additional, Drass, Holger, additional, Nandakumar, Sangeetha, additional, Barbieri, Mauro, additional, Davis, Allen, additional, Wang, Songhu, additional, Bayliss, Daniel, additional, Bouma, Luke, additional, Dragomir, Diana, additional, Eastman, Jason D., additional, Daylan, Tansu, additional, Guerrero, Natalia, additional, Barclay, Thomas, additional, Ting, Eric B., additional, Henze, Christopher E., additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua, additional, Jenkins, Jon M., additional, Wittenmyer, Robert A., additional, Bowler, Brendan P., additional, Crossfield, Ian, additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John F., additional, Morton, Timothy D., additional, Plavchan, Peter, additional, Tinney, C. G., additional, Addison, Brett, additional, Mengel, Matthew W., additional, Okumura, Jack, additional, Shahaf, Sahar, additional, Mazeh, Tsevi, additional, Rabus, Markus, additional, Shporer, Avi, additional, Ziegler, Carl, additional, Mann, Andrew W., additional, and Hart, Rhodes, additional

Published
2020
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50. TESS Spots a Compact System of Super-Earths around the Naked-eye Star HR 858

Author

Vanderburg, Andrew, primary, Huang, Chelsea X., additional, Rodriguez, Joseph E., additional, Becker, Juliette C., additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Addison, Brett, additional, Bieryla, Allyson, additional, Briceño, Cesar, additional, Bowler, Brendan P., additional, Brown, Timothy M., additional, Burke, Christopher J., additional, Burt, Jennifer A., additional, Caldwell, Douglas A., additional, Clark, Jake T., additional, Crossfield, Ian, additional, Dittmann, Jason A., additional, Dynes, Scott, additional, Fulton, Benjamin J., additional, Guerrero, Natalia, additional, Harbeck, Daniel, additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Kraus, Adam L., additional, Kreidberg, Laura, additional, Law, Nicolas, additional, Mann, Andrew W., additional, Mengel, Matthew W., additional, Morton, Timothy D., additional, Okumura, Jack, additional, Pearce, Logan A., additional, Plavchan, Peter, additional, Quinn, Samuel N., additional, Rabus, Markus, additional, Rose, Mark E., additional, Rowden, Pam, additional, Shporer, Avi, additional, Siverd, Robert J., additional, Smith, Jeffrey C., additional, Stassun, Keivan, additional, Tinney, C. G., additional, Wittenmyer, Rob, additional, Wright, Duncan J., additional, Zhang, Hui, additional, Zhou, George, additional, and Ziegler, Carl A., additional

Published
2019
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