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TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type starAddison, Brett C.Wright, Duncan J.Nicholson, Belinda A.Cale, BrysonMocnik, TeoHuber, DanielPlavchan, PeterWittenmyer, Robert A.Vanderburg, AndrewChaplin, William J.Chontos, AshleyClark, Jake T.Eastman, Jason D.Ziegler, CarlBrahm, RafaelCarter, Bradley D.Clerte, MathieuEspinoza, NéstorHorner, JonathanBentley, JohnJordán, AndrésKane, Stephen R.Kielkopf, John F.Laychock, EmilieMengel, Matthew W.Okumura, JackStassun, Keivan G.Bedding, Timothy R.Bowler, Brendan P.Burnelis, AndriusBlanco-Cuaresma, SergiCollins, MichaelaCrossfield, IanDavis, Allen B.Evensberget, DagHeitzmann, AlexisHowell, Steve B.Law, NicholasMann, Andrew W.Marsden, Stephen C.Matson, Rachel A.O'Connor, James H.Shporer, AviStevens, CatherineTinney, C. G.Tylor, ChristopherWang, SonghuZhang, HuiHenning, ThomasKossakowski, DianaRicker, GeorgeSarkis, PaulaSchlecker, MartinTorres, PascalVanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Mireles, IsmaelRowden, PamPepper, JoshuaDaylan, TansuSchlieder, Joshua E.Collins, Karen A.Collins, Kevin I.Tan, Thiam-GuanBall, Warrick H.Basu, SarbaniBuzasi, Derek L.Campante, Tiago L.Corsaro, EnricoGonzález-Cuesta, L.Davies, Guy R.de Almeida, LeandroDo Nascimento, Jose-Dias, Jr.García, Rafael A.Guo, ZhaoHandberg, RasmusHekker, SaskiaHey, Daniel R.Kallinger, ThomasKawaler, Steven D.Kayhan, CenkKuszlewicz, James S.Lund, Mikkel N.Lyttle, AlexanderMathur, SavitaMiglio, AndreaMosser, BenoitNielsen, Martin B.Serenelli, Aldo M.Aguirre, Victor SilvaThemeßl, NathalieDOI: info:10.1093/mnras/staa3960v. 5023704–3722
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. et al. 2021. "TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star." Monthly Notices of the Royal Astronomical Society 502:3704– 3722. https://doi.org/10.1093/mnras/staa3960
ID: 159268
Type: article
Authors: 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 H.; 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, L.; Davies, Guy R.; de Almeida, Leandro; Do Nascimento, Jose-Dias, Jr.; García, Rafael A.; 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; Themeßl, Nathalie
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 MP = 0.138 ± 0.023 $\rm {M_J}$ (43.9 ± 7.3 $\, M_{\rm \oplus}$ ), a radius of RP = 0.639 ± 0.013 $\rm {R_J}$ (7.16 ± 0.15 $\, \mathrm{ R}_{\rm \oplus}$ ), 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 (V = 7.612 mag) somewhat evolved late F-type star with M* = 1.390 ± 0.046 $\rm {M_{sun}}$ , R* = 1.888 ± 0.033 $\rm {R_{sun}}$ , Teff = 6075 ± 90 $\rm {K}$ , and vsin i = 11.3 ± 0.5 km s-1. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) 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.
TOI-811b and TOI-852b: New Transiting Brown Dwarfs with Similar Masses and Very Different Radii and Ages from the TESS MissionCarmichael, Theron W.Quinn, Samuel N.Zhou, GeorgeGrieves, NolanIrwin, Jonathan M.Stassun, Keivan G.Vanderburg, Andrew M.Winn, Joshua N.Bouchy, FrancoisBrasseur, Clara E.Briceño, CésarCaldwell, Douglas A.Charbonneau, DavidCollins, Karen A.Colon, Knicole D.Eastman, Jason D.Fausnaugh, MichaelFong, WilliamFűrész, GáborHuang, ChelseaJenkins, Jon M.Kielkopf, John F.Latham, David W.Law, NicholasLund, Michael B.Mann, Andrew W.Ricker, George R.Rodriguez, Joseph E.Schwarz, Richard P.Shporer, AviTenenbaum, PeterWood, Mackenna L.Ziegler, CarlDOI: info:10.3847/1538-3881/abd4e1v. 16197
Carmichael, Theron W., Quinn, Samuel N., Zhou, George, Grieves, Nolan, Irwin, Jonathan M., Stassun, Keivan G., Vanderburg, Andrew M., Winn, Joshua N., Bouchy, Francois, Brasseur, Clara E., Briceño, César, Caldwell, Douglas A., Charbonneau, David, Collins, Karen A., Colon, Knicole D., Eastman, Jason D., Fausnaugh, Michael, Fong, William, Fűrész, Gábor, Huang, Chelsea, Jenkins, Jon M., Kielkopf, John F., Latham, David W., Law, Nicholas, Lund, Michael B. et al. 2021. "TOI-811b and TOI-852b: New Transiting Brown Dwarfs with Similar Masses and Very Different Radii and Ages from the TESS Mission." The Astronomical Journal 161:97. https://doi.org/10.3847/1538-3881/abd4e1
ID: 159333
Type: article
Authors: Carmichael, Theron W.; Quinn, Samuel N.; Zhou, George; Grieves, Nolan; Irwin, Jonathan M.; Stassun, Keivan G.; Vanderburg, Andrew M.; Winn, Joshua N.; Bouchy, Francois; Brasseur, Clara E.; Briceño, César; Caldwell, Douglas A.; Charbonneau, David; Collins, Karen A.; Colon, Knicole D.; Eastman, Jason D.; Fausnaugh, Michael; Fong, William; Fűrész, Gábor; Huang, Chelsea; Jenkins, Jon M.; Kielkopf, John F.; Latham, David W.; Law, Nicholas; Lund, Michael B.; Mann, Andrew W.; Ricker, George R.; Rodriguez, Joseph E.; Schwarz, Richard P.; Shporer, Avi; Tenenbaum, Peter; Wood, Mackenna L.; Ziegler, Carl
Abstract: We report the discovery of two transiting brown dwarfs (BDs), TOI-811b and TOI-852b, from NASA's Transiting Exoplanet Survey Satellite mission. These two transiting BDs have similar masses but very different radii and ages. Their host stars have similar masses, effective temperatures, and metallicities. The younger and larger transiting BD is TOI-811b at a mass of Mb = 59.9 ± 13.0MJ and radius of Rb = 1.26 ± 0.06RJ, and it orbits its host star in a period of P = 25.16551 ± 0.00004 days. We derive the host star's age of ${93}_{-29}^{+61}$ Myr from an application of gyrochronology. The youth of this system, rather than external heating from its host star, is why this BD's radius is relatively large. This constraint on the youth of TOI-811b allows us to test substellar mass-radius evolutionary models at young ages where the radius of BDs changes rapidly. TOI-852b has a similar mass at Mb = 53.7 ± 1.4MJ but is much older (4 or 8 Gyr, based on bimodal isochrone results of the host star) and is also smaller with a radius of Rb = 0.83 ± 0.04RJ. TOI-852b's orbital period is P = 4.94561 ± 0.00008 days. TOI-852b joins the likes of other old transiting BDs that trace out the oldest substellar mass-radius evolutionary models where contraction of the BD's radius slows and approaches a constant value. Both host stars have a mass of M = 1.32M ± 0.05 and differ in their radii, Teff, and [Fe/H], with TOI-811 having R = 1.27 ± 0.09R, Teff = 6107 ± 77 K, and [Fe/H] = + 0.40 ± 0.09 and TOI-852 having R = 1.71 ± 0.04R, Teff = 5768 ± 84 K, and [Fe/H] = + 0.33 ± 0.09. We take this opportunity to examine how TOI-811b and TOI-852b serve as test points for young and old substellar isochrones, respectively.
Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216bDawson, Rebekah I.Huang, Chelsea X.Brahm, RafaelCollins, Karen A.Hobson, Melissa J.Jordán, AndrésDong, JiayinKorth, JudithTrifonov, TrifonAbe, LyuAgabi, AbdelkrimBruni, IvanButler, R. PaulBarbieri, MauroCollins, Kevin I.Conti, Dennis M.Crane, Jeffrey D.Crouzet, NicolasDransfield, GeorginaEvans, PhilEspinoza, NéstorGan, TianjunGuillot, TristanHenning, ThomasLissauer, Jack J.Jensen, Eric L. N.Sainte, Wenceslas MarieMékarnia, DjamelMyers, GordonNandakumar, SangeethaRelles, Howard M.Sarkis, PaulaTorres, PascalShectman, StephenSchmider, François-XavierShporer, AviStockdale, ChrisTeske, JohannaTriaud, Amaury H. M. J.Wang, Sharon XuesongZiegler, CarlRicker, G.Vanderspek, R.Latham, David W.Seager, S.Winn, J.Jenkins, Jon M.Bouma, L. G.Burt, Jennifer A.Charbonneau, DavidLevine, Alan M.McDermott, ScottMcLean, BrianRose, Mark E.Vanderburg, AndrewWohler, BillDOI: info:10.3847/1538-3881/abd8d0v. 161161
Dawson, Rebekah I., Huang, Chelsea X., Brahm, Rafael, Collins, Karen A., Hobson, Melissa J., Jordán, Andrés, Dong, Jiayin, Korth, Judith, Trifonov, Trifon, Abe, Lyu, Agabi, Abdelkrim, Bruni, Ivan, Butler, R. Paul, Barbieri, Mauro, Collins, Kevin I., Conti, Dennis M., Crane, Jeffrey D., Crouzet, Nicolas, Dransfield, Georgina, Evans, Phil, Espinoza, Néstor, Gan, Tianjun, Guillot, Tristan, Henning, Thomas, Lissauer, Jack J. et al. 2021. "Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b." The Astronomical Journal 161:161. https://doi.org/10.3847/1538-3881/abd8d0
ID: 159319
Type: article
Authors: Dawson, Rebekah I.; Huang, Chelsea X.; Brahm, Rafael; Collins, Karen A.; Hobson, Melissa J.; Jordán, Andrés; Dong, Jiayin; Korth, Judith; Trifonov, Trifon; Abe, Lyu; Agabi, Abdelkrim; Bruni, Ivan; Butler, R. Paul; Barbieri, Mauro; Collins, Kevin I.; Conti, Dennis M.; Crane, Jeffrey D.; Crouzet, Nicolas; Dransfield, Georgina; Evans, Phil; Espinoza, Néstor; Gan, Tianjun; Guillot, Tristan; Henning, Thomas; Lissauer, Jack J.; Jensen, Eric L. N.; Sainte, Wenceslas Marie; Mékarnia, Djamel; Myers, Gordon; Nandakumar, Sangeetha; Relles, Howard M.; Sarkis, Paula; Torres, Pascal; Shectman, Stephen; Schmider, François-Xavier; Shporer, Avi; Stockdale, Chris; Teske, Johanna; Triaud, Amaury H. M. J.; Wang, Sharon Xuesong; Ziegler, Carl; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, S.; Winn, J.; Jenkins, Jon M.; Bouma, L. G.; Burt, Jennifer A.; Charbonneau, David; Levine, Alan M.; McDermott, Scott; McLean, Brian; Rose, Mark E.; Vanderburg, Andrew; Wohler, Bill
Abstract: TOI-216 hosts a pair of warm, large exoplanets discovered by the TESS mission. These planets were found to be in or near the 2:1 resonance, and both of them exhibit transit timing variations (TTVs). Precise characterization of the planets' masses and radii, orbital properties, and resonant behavior can test theories for the origins of planets orbiting close to their stars. Previous characterization of the system using the first six sectors of TESS data suffered from a degeneracy between planet mass and orbital eccentricity. Radial-velocity measurements using HARPS, FEROS, and the Planet Finder Spectrograph break that degeneracy, and an expanded TTV baseline from TESS and an ongoing ground-based transit observing campaign increase the precision of the mass and eccentricity measurements. We determine that TOI-216c is a warm Jupiter, TOI-216b is an eccentric warm Neptune, and that they librate in 2:1 resonance with a moderate libration amplitude of ${60}_{-2}^{+2}$ deg, a small but significant free eccentricity of ${0.0222}_{-0.0003}^{+0.0005}$ for TOI-216b, and a small but significant mutual inclination of 1°2-3°9 (95% confidence interval). The libration amplitude, free eccentricity, and mutual inclination imply a disturbance of TOI-216b before or after resonance capture, perhaps by an undetected third planet.
TESS Discovery of a Super-Earth and Three Sub-Neptunes Hosted by the Bright, Sun-like Star HD 108236Daylan, TansuPinglé, KartikWright, JasmineGünther, Maximilian N.Stassun, Keivan G.Kane, Stephen R.Vanderburg, AndrewJontof-Hutter, DanielRodriguez, Joseph E.Shporer, AviHuang, Chelsea X.Mikal-Evans, ThomasBadenas-Agusti, MarionaCollins, Karen A.Rackham, Benjamin V.Quinn, Samuel N.Cloutier, RyanCollins, Kevin I.Guerra, PereJensen, Eric L. N.Kielkopf, John F.Massey, BobSchwarz, Richard P.Charbonneau, DavidLissauer, Jack J.Irwin, Jonathan M.Baştürk, ÖzgürFulton, BenjaminSoubkiou, AbderahmaneZouhair, BenkhaldounHowell, Steve B.Ziegler, CarlBriceño, CésarLaw, NicholasMann, Andrew W.Scott, NicFurlan, EliseCiardi, David R.Matson, RachelHellier, CoelAnderson, David R.Butler, R. PaulCrane, Jeffrey D.Teske, Johanna K.Shectman, Stephen A.Kristiansen, Martti H.Terentev, Ivan A.Schwengeler, Hans MartinRicker, George R.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Berta-Thompson, Zachory K.Bouma, Luke G.Fong, WilliamFuresz, GaborHenze, Christopher E.Morgan, Edward H.Quintana, ElisaTing, Eric B.Twicken, Joseph D.DOI: info:10.3847/1538-3881/abd73ev. 16185
Daylan, Tansu, Pinglé, Kartik, Wright, Jasmine, Günther, Maximilian N., Stassun, Keivan G., Kane, Stephen R., Vanderburg, Andrew, Jontof-Hutter, Daniel, Rodriguez, Joseph E., Shporer, Avi, Huang, Chelsea X., Mikal-Evans, Thomas, Badenas-Agusti, Mariona, Collins, Karen A., Rackham, Benjamin V., Quinn, Samuel N., Cloutier, Ryan, Collins, Kevin I., Guerra, Pere, Jensen, Eric L. N., Kielkopf, John F., Massey, Bob, Schwarz, Richard P., Charbonneau, David, Lissauer, Jack J. et al. 2021. "TESS Discovery of a Super-Earth and Three Sub-Neptunes Hosted by the Bright, Sun-like Star HD 108236." The Astronomical Journal 161:85. https://doi.org/10.3847/1538-3881/abd73e
ID: 159336
Type: article
Authors: Daylan, Tansu; Pinglé, Kartik; Wright, Jasmine; Günther, Maximilian N.; Stassun, Keivan G.; Kane, Stephen R.; Vanderburg, Andrew; Jontof-Hutter, Daniel; Rodriguez, Joseph E.; Shporer, Avi; Huang, Chelsea X.; Mikal-Evans, Thomas; Badenas-Agusti, Mariona; Collins, Karen A.; Rackham, Benjamin V.; Quinn, Samuel N.; Cloutier, Ryan; Collins, Kevin I.; Guerra, Pere; Jensen, Eric L. N.; Kielkopf, John F.; Massey, Bob; Schwarz, Richard P.; Charbonneau, David; Lissauer, Jack J.; Irwin, Jonathan M.; Baştürk, Özgür; Fulton, Benjamin; Soubkiou, Abderahmane; Zouhair, Benkhaldoun; Howell, Steve B.; Ziegler, Carl; Briceño, César; Law, Nicholas; Mann, Andrew W.; Scott, Nic; Furlan, Elise; Ciardi, David R.; Matson, Rachel; Hellier, Coel; Anderson, David R.; Butler, R. Paul; Crane, Jeffrey D.; Teske, Johanna K.; Shectman, Stephen A.; Kristiansen, Martti H.; Terentev, Ivan A.; Schwengeler, Hans Martin; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Berta-Thompson, Zachory K.; Bouma, Luke G.; Fong, William; Furesz, Gabor; Henze, Christopher E.; Morgan, Edward H.; Quintana, Elisa; Ting, Eric B.; Twicken, Joseph D.
Abstract: We report the discovery and validation of four extrasolar planets hosted by the nearby, bright, Sun-like (G3V) star HD 108236 using data from the Transiting Exoplanet Survey Satellite (TESS). We present transit photometry, reconnaissance, and precise Doppler spectroscopy, as well as high-resolution imaging, to validate the planetary nature of the objects transiting HD 108236, also known as the TESS Object of Interest (TOI) 1233. The innermost planet is a possibly rocky super-Earth with a period of ${3.79523}_{-0.00044}^{+0.00047}$ days and has a radius of 1.586 ± 0.098 R. The outer planets are sub-Neptunes, with potential gaseous envelopes, having radii of ${2.068}_{-0.091}^{+0.10}$ R, 2.72 ± 0.11 R, and ${3.12}_{-0.12}^{+0.13}$ R and periods of ${6.20370}_{-0.00052}^{+0.00064}$ days, ${14.17555}_{-0.0011}^{+0.00099}$ days, and ${19.5917}_{-0.0020}^{+0.0022}$ days, respectively. With V and Ks magnitudes of 9.2 and 7.6, respectively, the bright host star makes the transiting planets favorable targets for mass measurements and, potentially, for atmospheric characterization via transmission spectroscopy. HD 108236 is the brightest Sun-like star in the visual (V) band known to host four or more transiting exoplanets. The discovered planets span a broad range of planetary radii and equilibrium temperatures and share a common history of insolation from a Sun-like star (R = 0.888 ± 0.017 R, Teff = 5730 ± 50 K), making HD 108236 an exciting, opportune cosmic laboratory for testing models of planet formation and evolution.
A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113Osborn, H. P.Armstrong, D. J.Adibekyan, V.Collins, Karen A.Delgado-Mena, E.Howell, S. B.Hellier, C.King, G. W.Lillo-Box, J.Nielsen, L. D.Otegi, J. F.Santos, N. C.Ziegler, C.Anderson, D. R.Briceño, C.Burke, C.Bayliss, D.Barrado, D.Bryant, E. M.Brown, D. J. A.Barros, S. C. C.Bouchy, F.Caldwell, D. A.Conti, D. M.Díaz, R. F.Dragomir, D.Deleuil, M.Demangeon, O. D. S.Dorn, C.Daylan, T.Figueira, P.Helled, R.Hoyer, S.Jenkins, J. M.Jensen, E. L. N.Latham, David W.Law, N.Louie, D. R.Mann, A. W.Osborn, A.Pollacco, D. L.Rodriguez, D. R.Rackham, B. V.Ricker, G.Scott, N. J.Sousa, S. G.Seager, S.Stassun, K. G.Smith, J. C.Strøm, P.Udry, S.Villaseñor, J.Vanderspek, R.West, R.Wheatley, P. J.Winn, J. N.DOI: info:10.1093/mnras/stab182v. 5024842–4857
Osborn, H. P., Armstrong, D. J., Adibekyan, V., Collins, Karen A., Delgado-Mena, E., Howell, S. B., Hellier, C., King, G. W., Lillo-Box, J., Nielsen, L. D., Otegi, J. F., Santos, N. C., Ziegler, C., Anderson, D. R., Briceño, C., Burke, C., Bayliss, D., Barrado, D., Bryant, E. M., Brown, D. J. A., Barros, S. C. C., Bouchy, F., Caldwell, D. A., Conti, D. M., Díaz, R. F. et al. 2021. "A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113." Monthly Notices of the Royal Astronomical Society 502:4842– 4857. https://doi.org/10.1093/mnras/stab182
ID: 159269
Type: article
Authors: Osborn, H. P.; Armstrong, D. J.; Adibekyan, V.; Collins, Karen A.; Delgado-Mena, E.; Howell, S. B.; Hellier, C.; King, G. W.; Lillo-Box, J.; Nielsen, L. D.; Otegi, J. F.; Santos, N. C.; Ziegler, C.; Anderson, D. R.; Briceño, C.; Burke, C.; Bayliss, D.; Barrado, D.; Bryant, E. M.; Brown, D. J. A.; Barros, S. C. C.; Bouchy, F.; Caldwell, D. A.; Conti, D. M.; Díaz, R. F.; Dragomir, D.; Deleuil, M.; Demangeon, O. D. S.; Dorn, C.; Daylan, T.; Figueira, P.; Helled, R.; Hoyer, S.; Jenkins, J. M.; Jensen, E. L. N.; Latham, David W.; Law, N.; Louie, D. R.; Mann, A. W.; Osborn, A.; Pollacco, D. L.; Rodriguez, D. R.; Rackham, B. V.; Ricker, G.; Scott, N. J.; Sousa, S. G.; Seager, S.; Stassun, K. G.; Smith, J. C.; Strøm, P.; Udry, S.; Villaseñor, J.; Vanderspek, R.; West, R.; Wheatley, P. J.; Winn, J. N.
Abstract: We report the discovery of HD 110113 b (TESS object of interest-755.01), a transiting mini-Neptune exoplanet on a 2.5-d orbit around the solar-analogue HD 110113 (Teff = 5730 K). Using TESS photometry and High Accuracy Radial velocity Planet Searcher (HARPS) radial velocities gathered by the NCORES program, we find that HD 110113 b has a radius of 2.05 ± 0.12 R and a mass of 4.55 ± 0.62 M. The resulting density of $2.90^{+0.75}_{-0.59}$ g cm-3 is significantly lower than would be expected from a pure-rock world; therefore HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. The high incident flux places it within the so-called radius valley; however, HD 110113 b was able to hold on to a substantial (0.1-1 per cent) H-He atmosphere over its ∼4 Gyr lifetime. Through a novel simultaneous Gaussian process fit to multiple activity indicators, we were also able to fit for the strong stellar rotation signal with period 20.8 ± 1.2 d from the RVs and confirm an additional non-transiting planet, HD 110113 c, which has a mass of 10.5 ± 1.2 M and a period of $6.744^{+0.008}_{-0.009}$ d.
TIC 168789840: A Sextuply Eclipsing Sextuple Star SystemPowell, Brian P.Kostov, Veselin B.Rappaport, Saul A.Borkovits, TamásZasche, PetrTokovinin, AndreiKruse, EthanLatham, David W.Montet, Benjamin T.Jensen, Eric L. N.Jayaraman, RahulCollins, Karen A.Mašek, MartinHellier, CoelEvans, PhilTan, Thiam-GuanSchlieder, Joshua E.Torres, GuillermoSmale, Alan P.Friedman, Adam H.Barclay, ThomasGagliano, RobertQuintana, Elisa V.Jacobs, Thomas L.Gilbert, Emily A.Kristiansen, Martti H.Colón, Knicole D.LaCourse, Daryll M.Olmschenk, GregOmohundro, MarkSchnittman, Jeremy D.Schwengeler, Hans M.Barry, Richard K.Terentev, Ivan A.Boyd, PatriciaSchmitt, Allan R.Quinn, Samuel N.Vanderburg, AndrewPalle, EnricArmstrong, JamesRicker, George R.Vanderspek, RolandSeager, S.Winn, Joshua N.Jenkins, Jon M.Caldwell, Douglas A.Wohler, BillShiao, BernieBurke, Christopher J.Daylan, TansuVillaseñor, JoelDOI: info:10.3847/1538-3881/abddb5v. 161162
Powell, Brian P., Kostov, Veselin B., Rappaport, Saul A., Borkovits, Tamás, Zasche, Petr, Tokovinin, Andrei, Kruse, Ethan, Latham, David W., Montet, Benjamin T., Jensen, Eric L. N., Jayaraman, Rahul, Collins, Karen A., Mašek, Martin, Hellier, Coel, Evans, Phil, Tan, Thiam-Guan, Schlieder, Joshua E., Torres, Guillermo, Smale, Alan P., Friedman, Adam H., Barclay, Thomas, Gagliano, Robert, Quintana, Elisa V., Jacobs, Thomas L., Gilbert, Emily A. et al. 2021. "TIC 168789840: A Sextuply Eclipsing Sextuple Star System." The Astronomical Journal 161:162. https://doi.org/10.3847/1538-3881/abddb5
ID: 159318
Type: article
Authors: Powell, Brian P.; Kostov, Veselin B.; Rappaport, Saul A.; Borkovits, Tamás; Zasche, Petr; Tokovinin, Andrei; Kruse, Ethan; Latham, David W.; Montet, Benjamin T.; Jensen, Eric L. N.; Jayaraman, Rahul; Collins, Karen A.; Mašek, Martin; Hellier, Coel; Evans, Phil; Tan, Thiam-Guan; Schlieder, Joshua E.; Torres, Guillermo; Smale, Alan P.; Friedman, Adam H.; Barclay, Thomas; Gagliano, Robert; Quintana, Elisa V.; Jacobs, Thomas L.; Gilbert, Emily A.; Kristiansen, Martti H.; Colón, Knicole D.; LaCourse, Daryll M.; Olmschenk, Greg; Omohundro, Mark; Schnittman, Jeremy D.; Schwengeler, Hans M.; Barry, Richard K.; Terentev, Ivan A.; Boyd, Patricia; Schmitt, Allan R.; Quinn, Samuel N.; Vanderburg, Andrew; Palle, Enric; Armstrong, James; Ricker, George R.; Vanderspek, Roland; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Caldwell, Douglas A.; Wohler, Bill; Shiao, Bernie; Burke, Christopher J.; Daylan, Tansu; Villaseñor, Joel
Abstract: We report the discovery of a sextuply eclipsing sextuple star system from TESS data, TIC 168789840, also known as TYC 7037-89-1, the first known sextuple system consisting of three eclipsing binaries. The target was observed in Sectors 4 and 5 during Cycle 1, with lightcurves extracted from TESS Full Frame Image data. It was also previously observed by the WASP survey and ASAS-SN. The system consists of three gravitationally bound eclipsing binaries in a hierarchical structure of an inner quadruple system with an outer binary subsystem. Follow-up observations from several different observatories were conducted as a means of determining additional parameters. The system was resolved by speckle interferometry with a 0"42 separation between the inner quadruple and outer binary, inferring an estimated outer period of ∼2 kyr. It was determined that the fainter of the two resolved components is an 8.217 day eclipsing binary, which orbits the inner quadruple that contains two eclipsing binaries with periods of 1.570 days and 1.306 days. Markov Chain Monte Carlo (MCMC) analysis of the stellar parameters has shown that the three binaries of TIC 168789840 are "triplets," as each binary is quite similar to the others in terms of mass, radius, and Teff. As a consequence of its rare composition, structure, and orientation, this object can provide important new insight into the formation, dynamics, and evolution of multiple star systems. Future observations could reveal if the intermediate and outer orbital planes are all aligned with the planes of the three inner eclipsing binaries.
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame ImagesRodriguez, Joseph E.Quinn, Samuel N.Zhou, GeorgeVanderburg, AndrewNielsen, Louise D.Wittenmyer, Robert A.Brahm, RafaelReed, Phillip A.Huang, Chelsea X.Vach, SydneyCiardi, David R.Oelkers, Ryan J.Stassun, Keivan G.Hellier, CoelGaudi, B. ScottEastman, Jason D.Collins, Karen A.Bieryla, AllysonChristian, SamLatham, David W.Carleo, IlariaWright, Duncan J.Matthews, ElisabethGonzales, Erica J.Ziegler, CarlDressing, Courtney D.Howell, Steve B.Tan, Thiam-GuanWittrock, JustinPlavchan, PeterMcLeod, Kim K.Baker, DavidWang, GavinRadford, Don J.Schwarz, Richard P.Esposito, MassimilianoRicker, George R.Vanderspek, Roland K.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, BrettAnderson, D. R.Barclay, ThomasBeatty, Thomas G.Berlind, PerryBouchy, FrancoisBowen, MichaelBowler, Brendan P.Brasseur, C. E.Briceño, CésarCaldwell, Douglas A.Calkins, Michael L.Cartwright, ScottChaturvedi, PriyankaChaverot, GuillaumeChimaladinne, SudhishChristiansen, Jessie L.Collins, Kevin I.Crossfield, Ian J. M.Eastridge, KevinEspinoza, NéstorEsquerdo, Gilbert A.Feliz, Dax L.Fenske, TylerFong, WilliamGan, TianjunGiacalone, StevenGill, HoldenGordon, LindseyGranados, A.Grieves, NolanGuenther, Eike W.Guerrero, NataliaHenning, ThomasHenze, Christopher E.Hesse, KatharineHobson, Melissa J.Horner, JonathanJames, David J.Jensen, Eric L. N.Jimenez, MaryJordán, AndrésKane, Stephen R.Kielkopf, JohnKim, KingsleyKuhn, Rudolf B.Latouf, NatashaLaw, Nicholas M.Levine, Alan M.Lund, Michael B.Mann, Andrew W.Mao, ShudeMatson, Rachel A.Mengel, Matthew W.Mink, JessicaNewman, PatrickO'Dwyer, TannerOkumura, JackPalle, EnricPepper, JoshuaQuintana, Elisa V.Sarkis, PaulaSavel, Arjun B.Schlieder, Joshua E.Schnaible, ChloeShporer, AviSefako, RamotholoSeidel, Julia V.Siverd, Robert J.Skinner, BrettStalport, ManuStevens, Daniel J.Stibbards, CaitlinTinney, C. G.West, R. G.Yahalomi, Daniel A.Zhang, HuiDOI: info:10.3847/1538-3881/abe38av. 161194
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 et al. 2021. "TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images." The Astronomical Journal 161:194. https://doi.org/10.3847/1538-3881/abe38a
ID: 159316
Type: article
Authors: 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 J.; 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.; Cartwright, Scott; Chaturvedi, Priyanka; Chaverot, Guillaume; Chimaladinne, Sudhish; Christiansen, Jessie L.; Collins, Kevin I.; Crossfield, Ian J. M.; Eastridge, Kevin; Espinoza, Néstor; Esquerdo, Gilbert A.; Feliz, Dax L.; Fenske, Tyler; Fong, William; Gan, Tianjun; Giacalone, Steven; Gill, Holden; Gordon, Lindsey; Granados, A.; 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.; Mengel, Matthew W.; Mink, Jessica; Newman, Patrick; O'Dwyer, Tanner; Okumura, Jack; Palle, Enric; Pepper, Joshua; Quintana, Elisa V.; Sarkis, Paula; Savel, Arjun B.; Schlieder, Joshua E.; Schnaible, Chloe; Shporer, Avi; Sefako, Ramotholo; Seidel, Julia V.; Siverd, Robert J.; Skinner, Brett; Stalport, Manu; Stevens, Daniel J.; Stibbards, Caitlin; Tinney, C. G.; West, R. G.; Yahalomi, Daniel A.; Zhang, Hui
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 Working Group. The planets are all Jovian size (RP = 1.01-1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 P > 1.7 RJ, 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 ${6.31}_{-0.30}^{+0.28}$ MJ and a statistically significant, nonzero orbital eccentricity of e = ${0.074}_{-0.022}^{+0.021}$ . 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 analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESSSeager, SaraKnapp, MaryDemory, Brice-OlivierKrishnamurthy, AkshataHuang, Chelsea X.Agusti, Mariona BadenasShporer, AviWeisserman, DrewBecker, JulietteVanderburg, AndrewSmith, MatthewPong, Christopher M.Bailey, Vanessa P.Donner, AmandaDi Pasquale, PeterCampuzano, BrianSmith, ColinLuu, JasonBabuscia, AlessandraBocchino, Robert L., Jr.Loveland, JessicaColley, CodyGedenk, TobiasKulkarni, TejasHughes, KyleWhite, MaryKrajewski, JoelFesq, LorraineRicker, GeorgeVanderspek, RolandLatham, David W.Jenkins, Jon M.Winn, Joshua N.Caldwell, Douglas A.Collins, Karen A.Dragomir, DianaFausnaugh, MichaelGlidden, AnaSchlieder, Joshua E.Twicken, Joseph D.Wohler, BillDOI: info:10.3847/1538-3881/abcd3dv. 161117
Seager, Sara, Knapp, Mary, Demory, Brice-Olivier, Krishnamurthy, Akshata, Huang, Chelsea X., Agusti, Mariona Badenas, Shporer, Avi, Weisserman, Drew, Becker, Juliette, Vanderburg, Andrew, Smith, Matthew, Pong, Christopher M., Bailey, Vanessa P., Donner, Amanda, Di Pasquale, Peter, Campuzano, Brian, Smith, Colin, Luu, Jason, Babuscia, Alessandra, Bocchino, Robert L., Jr., Loveland, Jessica, Colley, Cody, Gedenk, Tobias, Kulkarni, Tejas, Hughes, Kyle et al. 2021. "HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS." The Astronomical Journal 161:117. https://doi.org/10.3847/1538-3881/abcd3d
ID: 159327
Type: article
Authors: Seager, Sara; Knapp, Mary; Demory, Brice-Olivier; Krishnamurthy, Akshata; Huang, Chelsea X.; Agusti, Mariona Badenas; Shporer, Avi; Weisserman, Drew; Becker, Juliette; Vanderburg, Andrew; Smith, Matthew; Pong, Christopher M.; Bailey, Vanessa P.; Donner, Amanda; Di Pasquale, Peter; Campuzano, Brian; Smith, Colin; Luu, Jason; Babuscia, Alessandra; Bocchino, Robert L., Jr.; Loveland, Jessica; Colley, Cody; Gedenk, Tobias; Kulkarni, Tejas; Hughes, Kyle; White, Mary; Krajewski, Joel; Fesq, Lorraine; Ricker, George; Vanderspek, Roland; Latham, David W.; Jenkins, Jon M.; Winn, Joshua N.; Caldwell, Douglas A.; Collins, Karen A.; Dragomir, Diana; Fausnaugh, Michael; Glidden, Ana; Schlieder, Joshua E.; Twicken, Joseph D.; Wohler, Bill
Abstract: HD 219134 is a K3V dwarf star with six reported radial-velocity discovered planets. The two innermost planets b and c show transits, raising the possibility of this system to be the nearest (6.53 pc), brightest (V = 5.57) example of a star with a compact multiple transiting planet system. Ground-based searches for transits of planets beyond b and c are not feasible because of the infrequent transits, long transit duration (∼5 hr), shallow transit depths (. We provide TESS updated transit times and periods for HD 219134 b and c, which are designated TOI 1469.01 and 1469.02 respectively.
TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to InflationSha, LizhouHuang, Chelsea X.Shporer, AviRodriguez, Joseph E.Vanderburg, AndrewBrahm, RafaelHagelberg, JanisMatthews, Elisabeth C.Ziegler, CarlLivingston, John H.Stassun, Keivan G.Wright, Duncan J.Crane, Jeffrey D.Espinoza, NéstorBouchy, FrançoisBakos, Gáspár Á.Collins, Karen A.Zhou, GeorgeBieryla, AllysonHartman, Joel D.Wittenmyer, Robert A.Nielsen, Louise D.Plavchan, PeterBayliss, DanielSarkis, PaulaTan, Thiam-GuanCloutier, RyanMancini, LuigiJordán, AndrésWang, SharonHenning, ThomasNarita, NorioPenev, KaloyanTeske, Johanna K.Kane, Stephen R.Mann, Andrew W.Addison, Brett C.Tamura, MotohideHorner, JonathanBarbieri, MauroBurt, Jennifer A.Díaz, Matías R.Crossfield, Ian J. M.Dragomir, DianaDrass, HolgerFeinstein, Adina D.Zhang, HuiHart, RhodesKielkopf, John F.Jensen, Eric L. N.Montet, Benjamin T.Ottoni, GaëlSchwarz, Richard P.Rojas, FelipeNespral, DavidTorres, PascalMengel, Matthew W.Udry, StéphaneZapata, AbnerSnoddy, ErinOkumura, JackRicker, George R.Vanderspek, Roland K.Latham, David W.Winn, Joshua N.Seager, SaraJenkins, Jon M.Colón, Knicole D.Henze, Christopher E.Krishnamurthy, AkshataTing, Eric B.Vezie, MichaelVillanueva, StevenDOI: info:10.3847/1538-3881/abd187v. 16182
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 et al. 2021. "TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to Inflation." The Astronomical Journal 161:82. https://doi.org/10.3847/1538-3881/abd187
ID: 159334
Type: article
Authors: 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; 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; Villanueva, Steven
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 ${0.852}_{-0.062}^{+0.053}\,{R}_{{\rm{J}}}$ and a mass of ${0.174}_{-0.017}^{+0.018}$ MJ and is in a 3.68 day orbit, while K2-329 b has a radius of ${0.774}_{-0.024}^{+0.026}\,{R}_{{\rm{J}}}$ and a mass of ${0.260}_{-0.022}^{+0.020}$ MJ 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.
TESS Hunt for Young and Maturing Exoplanets (THYME). V. A Sub-Neptune Transiting a Young Star in a Newly Discovered 250 Myr AssociationTofflemire, Benjamin M.Rizzuto, Aaron C.Newton, Elisabeth R.Kraus, Adam L.Mann, Andrew W.Vanderburg, AndrewNelson, TylerHawkins, KeithWood, Mackenna L.Zhou, GeorgeQuinn, Samuel N.Howell, Steve B.Collins, Karen A.Schwarz, Richard P.Stassun, Keivan G.Bouma, Luke G.Essack, ZahraOsborn, HughBoyd, Patricia T.Fűrész, GáborGlidden, AnaTwicken, Joseph D.Wohler, BillMcLean, BrianRicker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.DOI: info:10.3847/1538-3881/abdf53v. 161171
Tofflemire, Benjamin M., Rizzuto, Aaron C., Newton, Elisabeth R., Kraus, Adam L., Mann, Andrew W., Vanderburg, Andrew, Nelson, Tyler, Hawkins, Keith, Wood, Mackenna L., Zhou, George, Quinn, Samuel N., Howell, Steve B., Collins, Karen A., Schwarz, Richard P., Stassun, Keivan G., Bouma, Luke G., Essack, Zahra, Osborn, Hugh, Boyd, Patricia T., Fűrész, Gábor, Glidden, Ana, Twicken, Joseph D., Wohler, Bill, McLean, Brian, Ricker, George R. et al. 2021. "TESS Hunt for Young and Maturing Exoplanets (THYME). V. A Sub-Neptune Transiting a Young Star in a Newly Discovered 250 Myr Association." The Astronomical Journal 161:171. https://doi.org/10.3847/1538-3881/abdf53
ID: 159320
Type: article
Authors: Tofflemire, Benjamin M.; Rizzuto, Aaron C.; Newton, Elisabeth R.; Kraus, Adam L.; Mann, Andrew W.; Vanderburg, Andrew; Nelson, Tyler; Hawkins, Keith; Wood, Mackenna L.; Zhou, George; Quinn, Samuel N.; Howell, Steve B.; Collins, Karen A.; Schwarz, Richard P.; Stassun, Keivan G.; Bouma, Luke G.; Essack, Zahra; Osborn, Hugh; Boyd, Patricia T.; Fűrész, Gábor; Glidden, Ana; Twicken, Joseph D.; Wohler, Bill; McLean, Brian; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.
Abstract: The detection and characterization of young planetary systems offer a direct path to study the processes that shape planet evolution. We report on the discovery of a sub-Neptune-sized planet orbiting the young star HD 110082 (TOI-1098). Transit events we initially detected during TESS Cycle 1 are validated with time-series photometry from Spitzer. High-contrast imaging and high-resolution, optical spectra are also obtained to characterize the stellar host and confirm the planetary nature of the transits. The host star is a late-F dwarf (M = 1.2M) with a low-mass, M dwarf binary companion (M = 0.26M) separated by nearly one arcminute (∼6200 au). Based on its rapid rotation and Lithium absorption, HD 110082 is young, but is not a member of any known group of young stars (despite proximity to the Octans association). To measure the age of the system, we search for coeval, phase-space neighbors and compile a sample of candidate siblings to compare with the empirical sequences of young clusters and to apply quantitative age-dating techniques. In doing so, we find that HD 110082 resides in a new young stellar association we designate MELANGE-1, with an age of ${250}_{-70}^{+50}$ Myr. Jointly modeling the TESS and Spitzer light curves, we measure a planetary orbital period of 10.1827 days and radius of Rp = 3.2 ± 0.1R. HD 110082 b's radius falls in the largest 12% of field-age systems with similar host-star mass and orbital period. This finding supports previous studies indicating that young planets have larger radii than their field-age counterparts.
A nearby transiting rocky exoplanet that is suitable for atmospheric investigationTrifonov, T.Caballero, J. A.Morales, J. C.Seifahrt, A.Ribas, I.Reiners, A.Bean, J. L.Luque, R.Parviainen, H.Pallé, E.Stock, S.Zechmeister, M.Amado, P. J.Anglada-Escudé, G.Azzaro, M.Barclay, T.Béjar, V. J. S.Bluhm, P.Casasayas-Barris, N.Cifuentes, C.Collins, Karen A.Collins, K. I.Cortés-Contreras, M.de Leon, J.Dreizler, S.Dressing, C. D.Esparza-Borges, E.Espinoza, N.Fausnaugh, M.Fukui, A.Hatzes, A. P.Hellier, C.Henning, ThHenze, C. E.Herrero, E.Jeffers, S. V.Jenkins, J. M.Jensen, E. L. N.Kaminski, A.Kasper, D.Kossakowski, D.Kürster, M.Lafarga, M.Latham, David W.Mann, A. W.Molaverdikhani, K.Montes, D.Montet, B. T.Murgas, F.Narita, N.Oshagh, M.Passegger, V. M.Pollacco, D.Quinn, Samuel N.Quirrenbach, A.Ricker, G. R.Rodríguez López, C.Sanz-Forcada, J.Schwarz, R. P.Schweitzer, A.Seager, S.Shporer, A.Stangret, M.Stürmer, J.Tan, T. G.Tenenbaum, P.Twicken, J. D.Vanderspek, R.Winn, J. N.DOI: info:10.1126/science.abd7645v. 3711038–1041
Trifonov, T., Caballero, J. A., Morales, J. C., Seifahrt, A., Ribas, I., Reiners, A., Bean, J. L., Luque, R., Parviainen, H., Pallé, E., Stock, S., Zechmeister, M., Amado, P. J., Anglada-Escudé, G., Azzaro, M., Barclay, T., Béjar, V. J. S., Bluhm, P., Casasayas-Barris, N., Cifuentes, C., Collins, Karen A., Collins, K. I., Cortés-Contreras, M., de Leon, J., Dreizler, S. et al. 2021. "A nearby transiting rocky exoplanet that is suitable for atmospheric investigation." Science 371:1038– 1041. https://doi.org/10.1126/science.abd7645
ID: 159422
Type: article
Authors: Trifonov, T.; Caballero, J. A.; Morales, J. C.; Seifahrt, A.; Ribas, I.; Reiners, A.; Bean, J. L.; Luque, R.; Parviainen, H.; Pallé, E.; Stock, S.; Zechmeister, M.; Amado, P. J.; Anglada-Escudé, G.; Azzaro, M.; Barclay, T.; Béjar, V. J. S.; Bluhm, P.; Casasayas-Barris, N.; Cifuentes, C.; Collins, Karen A.; Collins, K. I.; Cortés-Contreras, M.; de Leon, J.; Dreizler, S.; Dressing, C. D.; Esparza-Borges, E.; Espinoza, N.; Fausnaugh, M.; Fukui, A.; Hatzes, A. P.; Hellier, C.; Henning, Th; Henze, C. E.; Herrero, E.; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kaminski, A.; Kasper, D.; Kossakowski, D.; Kürster, M.; Lafarga, M.; Latham, David W.; Mann, A. W.; Molaverdikhani, K.; Montes, D.; Montet, B. T.; Murgas, F.; Narita, N.; Oshagh, M.; Passegger, V. M.; Pollacco, D.; Quinn, Samuel N.; Quirrenbach, A.; Ricker, G. R.; Rodríguez López, C.; Sanz-Forcada, J.; Schwarz, R. P.; Schweitzer, A.; Seager, S.; Shporer, A.; Stangret, M.; Stürmer, J.; Tan, T. G.; Tenenbaum, P.; Twicken, J. D.; Vanderspek, R.; Winn, J. N.
Abstract: Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy.
KELT-9 b's Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin-Orbit MisalignmentAhlers, John P.Johnson, Marshall C.Stassun, Keivan G.Colón, Knicole D.Barnes, Jason W.Stevens, Daniel J.Beatty, ThomasGaudi, B. ScottCollins, Karen A.Rodriguez, Joseph E.Ricker, GeorgeVanderspek, RolandLatham, DavidSeager, SaraWinn, JoshuaJenkins, Jon M.Caldwell, Douglas A.Goeke, Robert F.Osborn, Hugh P.Paegert, MartinRowden, PamTenenbaum, PeterDOI: info:10.3847/1538-3881/ab8fa3v. 1604
Ahlers, John P., Johnson, Marshall C., Stassun, Keivan G., Colón, Knicole D., Barnes, Jason W., Stevens, Daniel J., Beatty, Thomas, Gaudi, B. Scott, Collins, Karen A., Rodriguez, Joseph E., Ricker, George, Vanderspek, Roland, Latham, David, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Caldwell, Douglas A., Goeke, Robert F., Osborn, Hugh P., Paegert, Martin, Rowden, Pam, and Tenenbaum, Peter. 2020. "KELT-9 b's Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin-Orbit Misalignment." The Astronomical Journal 160:4. https://doi.org/10.3847/1538-3881/ab8fa3
ID: 157618
Type: article
Authors: Ahlers, John P.; Johnson, Marshall C.; Stassun, Keivan G.; Colón, Knicole D.; Barnes, Jason W.; Stevens, Daniel J.; Beatty, Thomas; Gaudi, B. Scott; Collins, Karen A.; Rodriguez, Joseph E.; Ricker, George; Vanderspek, Roland; Latham, David; Seager, Sara; Winn, Joshua; Jenkins, Jon M.; Caldwell, Douglas A.; Goeke, Robert F.; Osborn, Hugh P.; Paegert, Martin; Rowden, Pam; Tenenbaum, Peter
Abstract: KELT-9 b is an ultra-hot Jupiter transiting a rapidly rotating, oblate early-A-type star in a polar orbit. We model the effect of rapid stellar rotation on KELT-9 b's transit light curve using photometry from the Transiting Exoplanet Survey Satellite to constrain the planet's true spin-orbit angle and to explore how KELT-9 b may be influenced by stellar gravity darkening. We constrain the host star's equatorial radius to be 1.089 ± 0.017 times as large as its polar radius and its local surface brightness to vary by ∼38% between its hot poles and cooler equator. We model the stellar oblateness and surface brightness gradient and find that it causes the transit light curve to lack the usual symmetry around the time of minimum light. We take advantage of the light-curve asymmetry to constrain KELT-9 b's true spin-orbit angle ( ${87^\circ }_{{-11}^{^\circ }}^{{+10}^{^\circ }}$ ), agreeing with Gaudi et al. that KELT-9 b is in a nearly polar orbit. We also apply a gravity-darkening correction to the spectral energy distribution model from Gaudi et al. and find that accounting for rapid rotation gives a better fit to available spectroscopy and yields a more reliable estimate for the star's polar effective temperature.
A remnant planetary core in the hot-Neptune desertArmstrong, David J.Lopez, Théo A.Adibekyan, VardanBooth, Richard A.Bryant, Edward M.Collins, Karen A.Deleuil, MagaliEmsenhuber, AlexandreHuang, Chelsea X.King, George W.Lillo-Box, JorgeLissauer, Jack J.Matthews, ElisabethMousis, OlivierNielsen, Louise D.Osborn, HughOtegi, JonSantos, Nuno C.Sousa, Sérgio G.Stassun, Keivan G.Veras, DimitriZiegler, CarlActon, Jack S.Almenara, Jose M.Anderson, David R.Barrado, DavidBarros, Susana C. C.Bayliss, DanielBelardi, ClaudiaBouchy, FrancoisBriceño, CésarBrogi, MatteoBrown, David J. A.Burleigh, Matthew R.Casewell, Sarah L.Chaushev, AlexanderCiardi, David R.Collins, Kevin I.Colón, Knicole D.Cooke, Benjamin F.Crossfield, Ian J. M.Díaz, Rodrigo F.Mena, Elisa DelgadoDemangeon, Olivier D. S.Dorn, CarolineDumusque, XavierEigmüller, PhilippFausnaugh, MichaelFigueira, PedroGan, TianjunGandhi, SiddharthGill, SamuelGonzales, Erica J.Goad, Michael R.Günther, Maximilian N.Helled, RavitHojjatpanah, SaeedHowell, Steve B.Jackman, JamesJenkins, James S.Jenkins, Jon M.Jensen, Eric L. N.Kennedy, Grant M.Latham, David W.Law, NicholasLendl, MonikaLozovsky, MichaelMann, Andrew W.Moyano, MaximilianoMcCormac, JamesMeru, FarzanaMordasini, ChristophOsborn, AresPollacco, DonQueloz, DidierRaynard, LiamRicker, George R.Rowden, PamelaSanterne, AlexandreSchlieder, Joshua E.Seager, SaraSha, LizhouTan, Thiam-GuanTilbrook, Rosanna H.Ting, EricUdry, StéphaneVanderspek, RolandWatson, Christopher A.West, Richard G.Wilson, Paul A.Winn, Joshua N.Wheatley, PeterVillasenor, Jesus NoelVines, Jose I.Zhan, ZhuchangDOI: info:10.1038/s41586-020-2421-7v. 583No. 781439–42
Armstrong, David J., Lopez, Théo A., Adibekyan, Vardan, Booth, Richard A., Bryant, Edward M., Collins, Karen A., Deleuil, Magali, Emsenhuber, Alexandre, Huang, Chelsea X., King, George W., Lillo-Box, Jorge, Lissauer, Jack J., Matthews, Elisabeth, Mousis, Olivier, Nielsen, Louise D., Osborn, Hugh, Otegi, Jon, Santos, Nuno C., Sousa, Sérgio G., Stassun, Keivan G., Veras, Dimitri, Ziegler, Carl, Acton, Jack S., Almenara, Jose M., Anderson, David R. et al. 2020. "A remnant planetary core in the hot-Neptune desert." Nature 583 (7814):39– 42. https://doi.org/10.1038/s41586-020-2421-7
ID: 156472
Type: article
Authors: Armstrong, David J.; Lopez, Théo A.; Adibekyan, Vardan; Booth, Richard A.; Bryant, Edward M.; Collins, Karen A.; Deleuil, Magali; Emsenhuber, Alexandre; Huang, Chelsea X.; King, George W.; Lillo-Box, Jorge; Lissauer, Jack J.; Matthews, Elisabeth; Mousis, Olivier; Nielsen, Louise D.; Osborn, Hugh; Otegi, Jon; Santos, Nuno C.; Sousa, Sérgio G.; Stassun, Keivan G.; Veras, Dimitri; Ziegler, Carl; Acton, Jack S.; Almenara, Jose M.; Anderson, David R.; Barrado, David; Barros, Susana C. C.; Bayliss, Daniel; Belardi, Claudia; Bouchy, Francois; Briceño, César; Brogi, Matteo; Brown, David J. A.; Burleigh, Matthew R.; Casewell, Sarah L.; Chaushev, Alexander; Ciardi, David R.; Collins, Kevin I.; Colón, Knicole D.; Cooke, Benjamin F.; Crossfield, Ian J. M.; Díaz, Rodrigo F.; Mena, Elisa Delgado; Demangeon, Olivier D. S.; Dorn, Caroline; Dumusque, Xavier; Eigmüller, Philipp; Fausnaugh, Michael; Figueira, Pedro; Gan, Tianjun; Gandhi, Siddharth; Gill, Samuel; Gonzales, Erica J.; Goad, Michael R.; Günther, Maximilian N.; Helled, Ravit; Hojjatpanah, Saeed; Howell, Steve B.; Jackman, James; Jenkins, James S.; Jenkins, Jon M.; Jensen, Eric L. N.; Kennedy, Grant M.; Latham, David W.; Law, Nicholas; Lendl, Monika; Lozovsky, Michael; Mann, Andrew W.; Moyano, Maximiliano; McCormac, James; Meru, Farzana; Mordasini, Christoph; Osborn, Ares; Pollacco, Don; Queloz, Didier; Raynard, Liam; Ricker, George R.; Rowden, Pamela; Santerne, Alexandre; Schlieder, Joshua E.; Seager, Sara; Sha, Lizhou; Tan, Thiam-Guan; Tilbrook, Rosanna H.; Ting, Eric; Udry, Stéphane; Vanderspek, Roland; Watson, Christopher A.; West, Richard G.; Wilson, Paul A.; Winn, Joshua N.; Wheatley, Peter; Villasenor, Jesus Noel; Vines, Jose I.; Zhan, Zhuchang
A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESSAstudillo-Defru, N.Cloutier, RyanWang, S. X.Teske, J.Brahm, R.Hellier, C.Ricker, G.Vanderspek, R.Latham, DavidSeager, S.Winn, J. N.Jenkins, J. M.Collins, Karen A.Stassun, K. G.Ziegler, C.Almenara, J. M.Anderson, D. R.Artigau, E.Bonfils, X.Bouchy, F.Briceño, C.Butler, R. P.Charbonneau, DavidConti, D. M.Crane, J.Crossfield, I. J. M.Davies, M.Delfosse, X.Díaz, R. F.Doyon, R.Dragomir, D.Eastman, Jason D.Espinoza, N.Essack, Z.Feng, F.Figueira, P.Forveille, T.Gan, T.Glidden, A.Guerrero, N.Hart, R.Henning, ThHorch, E. P.Isopi, G.Jenkins, J. S.Jordán, A.Kielkopf, J. F.Law, N.Lovis, C.Mallia, F.Mann, A. W.de Medeiros, J. R.Melo, C.Mennickent, R. E.Mignon, L.Murgas, F.Nusdeo, D. A.Pepe, F.Relles, Howard M.Rose, M.Santos, N. C.Ségransan, D.Shectman, S.Shporer, A.Smith, J. C.Torres, P.Udry, S.Villasenor, J.Winters, Jennifer G.Zhou, GeorgeDOI: info:10.1051/0004-6361/201937179v. 636A58
Astudillo-Defru, N., Cloutier, Ryan, Wang, S. X., Teske, J., Brahm, R., Hellier, C., Ricker, G., Vanderspek, R., Latham, David, Seager, S., Winn, J. N., Jenkins, J. M., Collins, Karen A., Stassun, K. G., Ziegler, C., Almenara, J. M., Anderson, D. R., Artigau, E., Bonfils, X., Bouchy, F., Briceño, C., Butler, R. P., Charbonneau, David, Conti, D. M., Crane, J. et al. 2020. "A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS." Astronomy and Astrophysics 636:A58. https://doi.org/10.1051/0004-6361/201937179
ID: 157118
Type: article
Authors: Astudillo-Defru, N.; Cloutier, Ryan; Wang, S. X.; Teske, J.; Brahm, R.; Hellier, C.; Ricker, G.; Vanderspek, R.; Latham, David; Seager, S.; Winn, J. N.; Jenkins, J. M.; Collins, Karen A.; Stassun, K. G.; Ziegler, C.; Almenara, J. M.; Anderson, D. R.; Artigau, E.; Bonfils, X.; Bouchy, F.; Briceño, C.; Butler, R. P.; Charbonneau, David; Conti, D. M.; Crane, J.; Crossfield, I. J. M.; Davies, M.; Delfosse, X.; Díaz, R. F.; Doyon, R.; Dragomir, D.; Eastman, Jason D.; Espinoza, N.; Essack, Z.; Feng, F.; Figueira, P.; Forveille, T.; Gan, T.; Glidden, A.; Guerrero, N.; Hart, R.; Henning, Th; Horch, E. P.; Isopi, G.; Jenkins, J. S.; Jordán, A.; Kielkopf, J. F.; Law, N.; Lovis, C.; Mallia, F.; Mann, A. W.; de Medeiros, J. R.; Melo, C.; Mennickent, R. E.; Mignon, L.; Murgas, F.; Nusdeo, D. A.; Pepe, F.; Relles, Howard M.; Rose, M.; Santos, N. C.; Ségransan, D.; Shectman, S.; Shporer, A.; Smith, J. C.; Torres, P.; Udry, S.; Villasenor, J.; Winters, Jennifer G.; Zhou, George
Abstract: We report the detection of a transiting super-Earth-sized planet (R = 1.39 ± 0.09 R) in a 1.4-day orbit around L 168-9 (TOI-134), a bright M1V dwarf (V = 11, K = 7.1) located at 25.15 ± 0.02 pc. The host star was observed in the first sector of the Transiting Exoplanet Survey Satellite (TESS) mission. For confirmation and planet mass measurement purposes, this was followed up with ground-based photometry, seeing-limited and high-resolution imaging, and precise radial velocity (PRV) observations using the HARPS and Magellan/PFS spectrographs. By combining the TESS data and PRV observations, we find the mass of L 168-9 b to be 4.60 ± 0.56 M and thus the bulk density to be 1.74-0.33+0.44 times higher than that of the Earth. The orbital eccentricity is smaller than 0.21 (95% confidence). This planet is a level one candidate for the TESS mission's scientific objective of measuring the masses of 50 small planets, and it is one of the most observationally accessible terrestrial planets for future atmospheric characterization.
Full Tables B.1 and B.2 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/cat/J/A+A/636/A58.
Partially based on observations made with the HARPS instrument on the ESO 3.6 m telescope under the program IDs 198.C-0838(A), 0101.C-0510(C), and 1102.C-0339(A) at Cerro La Silla (Chile).
This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc AwayBadenas-Agusti, MarionaGünther, Maximilian N.Daylan, TansuMikal-Evans, ThomasVanderburg, AndrewHuang, Chelsea X.Matthews, ElisabethRackham, Benjamin V.Bieryla, AllysonStassun, Keivan G.Kane, Stephen R.Shporer, AviFulton, Benjamin J.Hill, Michelle L.Nowak, GrzegorzRibas, IgnasiPallé, EnricJenkins, Jon M.Latham, David W.Seager, SaraRicker, George R.Vanderspek, Roland K.Winn, Joshua N.Abril-Pla, OriolCollins, Karen A.Serra, Pere GuerraNiraula, PrajwalRustamkulov, ZafarBarclay, ThomasCrossfield, Ian J. M.Howell, Steve B.Ciardi, David R.Gonzales, Erica J.Schlieder, Joshua E.Caldwell, Douglas A.Fausnaugh, MichaelMcDermott, ScottPaegert, MartinPepper, JoshuaRose, Mark E.Twicken, Joseph D.DOI: info:10.3847/1538-3881/aba0b5v. 160113
Badenas-Agusti, Mariona, Günther, Maximilian N., Daylan, Tansu, Mikal-Evans, Thomas, Vanderburg, Andrew, Huang, Chelsea X., Matthews, Elisabeth, Rackham, Benjamin V., Bieryla, Allyson, Stassun, Keivan G., Kane, Stephen R., Shporer, Avi, Fulton, Benjamin J., Hill, Michelle L., Nowak, Grzegorz, Ribas, Ignasi, Pallé, Enric, Jenkins, Jon M., Latham, David W., Seager, Sara, Ricker, George R., Vanderspek, Roland K., Winn, Joshua N., Abril-Pla, Oriol, Collins, Karen A. et al. 2020. "HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc Away." The Astronomical Journal 160:113. https://doi.org/10.3847/1538-3881/aba0b5
ID: 158027
Type: article
Authors: Badenas-Agusti, Mariona; Günther, Maximilian N.; Daylan, Tansu; Mikal-Evans, Thomas; Vanderburg, Andrew; Huang, Chelsea X.; Matthews, Elisabeth; Rackham, Benjamin V.; Bieryla, Allyson; Stassun, Keivan G.; Kane, Stephen R.; Shporer, Avi; Fulton, Benjamin J.; Hill, Michelle L.; Nowak, Grzegorz; Ribas, Ignasi; Pallé, Enric; Jenkins, Jon M.; Latham, David W.; Seager, Sara; Ricker, George R.; Vanderspek, Roland K.; Winn, Joshua N.; Abril-Pla, Oriol; Collins, Karen A.; Serra, Pere Guerra; Niraula, Prajwal; Rustamkulov, Zafar; Barclay, Thomas; Crossfield, Ian J. M.; Howell, Steve B.; Ciardi, David R.; Gonzales, Erica J.; Schlieder, Joshua E.; Caldwell, Douglas A.; Fausnaugh, Michael; McDermott, Scott; Paegert, Martin; Pepper, Joshua; Rose, Mark E.; Twicken, Joseph D.
Abstract: We present the discovery of three sub-Neptune-sized planets transiting the nearby and bright Sun-like star HD 191939 (TIC 269701147, TOI 1339), a Ks = 7.18 mag G8 V dwarf at a distance of only 54 pc. We validate the planetary nature of the transit signals by combining 5 months of data from the Transiting Exoplanet Survey Satellite with follow-up ground-based photometry, archival optical images, radial velocities, and high angular resolution observations. The three sub-Neptunes have similar radii ( ${R}_{{\rm{b}}}={3.42}_{-0.11}^{+0.11}$ , ${R}_{{\rm{c}}}={3.23}_{-0.11}^{+0.11}$ , and ${R}_{{\rm{d}}}={3.16}_{-0.11}^{+0.11}\,{R}_{\oplus }$ ), and their orbits are consistent with a stable, circular, and coplanar architecture near mean-motion resonances of 1:3 and 3:4 (Pb = 8.88, Pc = 28.58, and Pd = 38.35 days). The HD 191939 system is an excellent candidate for precise mass determinations of the planets with high-resolution spectroscopy due to the host star's brightness and low chromospheric activity. Moreover, the system's compact and near-resonant nature can provide an independent way to measure planetary masses via transit timing variations while also enabling dynamical and evolutionary studies. Finally, as a promising target for multiwavelength transmission spectroscopy of all three planets' atmospheres, HD 191939 can offer valuable insight into multiple sub-Neptunes born from a protoplanetary disk that may have resembled that of the early Sun.
Precise mass and radius of a transiting super-Earth planet orbiting the M dwarf TOI-1235: a planet in the radius gap?Bluhm, P.Luque, R.Espinoza, N.Pallé, E.Caballero, J. A.Dreizler, S.Livingston, J. H.Mathur, S.Quirrenbach, A.Stock, S.Van Eylen, V.Nowak, G.López, E. D.Csizmadia, SzZapatero Osorio, M. R.Schöfer, P.Lillo-Box, J.Oshagh, M.González-Álvarez, E.Amado, P. J.Barrado, D.Béjar, V. J. S.Cale, B.Chaturvedi, P.Cifuentes, C.Cochran, W. D.Collins, Karen A.Collins, K. I.Cortés-Contreras, M.Díez Alonso, E.El Mufti, M.Ercolino, A.Fridlund, M.Gaidos, E.García, R. A.Georgieva, I.González-Cuesta, L.Guerra, P.Hatzes, A. P.Henning, ThHerrero, E.Hidalgo, D.Isopi, G.Jeffers, S. V.Jenkins, J. M.Jensen, E. L. N.Kábath, P.Kaminski, A.Kemmer, J.Korth, J.Kossakowski, D.Kürster, M.Lafarga, M.Mallia, F.Montes, D.Morales, J. C.Morales-Calderón, M.Murgas, F.Narita, N.Passegger, V. M.Pedraz, S.Persson, C. M.Plavchan, P.Rauer, H.Redfield, S.Reffert, S.Reiners, A.Ribas, I.Ricker, G. R.Rodríguez-López, C.Santos, A. R. G.Seager, S.Schlecker, M.Schweitzer, A.Shan, Y.Soto, M. G.Subjak, J.Tal-Or, L.Trifonov, T.Vanaverbeke, S.Vanderspek, R.Wittrock, J.Zechmeister, M.Zohrabi, F.DOI: info:10.1051/0004-6361/202038160v. 639A132
Bluhm, P., Luque, R., Espinoza, N., Pallé, E., Caballero, J. A., Dreizler, S., Livingston, J. H., Mathur, S., Quirrenbach, A., Stock, S., Van Eylen, V., Nowak, G., López, E. D., Csizmadia, Sz, Zapatero Osorio, M. R., Schöfer, P., Lillo-Box, J., Oshagh, M., González-Álvarez, E., Amado, P. J., Barrado, D., Béjar, V. J. S., Cale, B., Chaturvedi, P., Cifuentes, C. et al. 2020. "Precise mass and radius of a transiting super-Earth planet orbiting the M dwarf TOI-1235: a planet in the radius gap?." Astronomy and Astrophysics 639:A132. https://doi.org/10.1051/0004-6361/202038160
ID: 157773
Type: article
Authors: Bluhm, P.; Luque, R.; Espinoza, N.; Pallé, E.; Caballero, J. A.; Dreizler, S.; Livingston, J. H.; Mathur, S.; Quirrenbach, A.; Stock, S.; Van Eylen, V.; Nowak, G.; López, E. D.; Csizmadia, Sz; Zapatero Osorio, M. R.; Schöfer, P.; Lillo-Box, J.; Oshagh, M.; González-Álvarez, E.; Amado, P. J.; Barrado, D.; Béjar, V. J. S.; Cale, B.; Chaturvedi, P.; Cifuentes, C.; Cochran, W. D.; Collins, Karen A.; Collins, K. I.; Cortés-Contreras, M.; Díez Alonso, E.; El Mufti, M.; Ercolino, A.; Fridlund, M.; Gaidos, E.; García, R. A.; Georgieva, I.; González-Cuesta, L.; Guerra, P.; Hatzes, A. P.; Henning, Th; Herrero, E.; Hidalgo, D.; Isopi, G.; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kábath, P.; Kaminski, A.; Kemmer, J.; Korth, J.; Kossakowski, D.; Kürster, M.; Lafarga, M.; Mallia, F.; Montes, D.; Morales, J. C.; Morales-Calderón, M.; Murgas, F.; Narita, N.; Passegger, V. M.; Pedraz, S.; Persson, C. M.; Plavchan, P.; Rauer, H.; Redfield, S.; Reffert, S.; Reiners, A.; Ribas, I.; Ricker, G. R.; Rodríguez-López, C.; Santos, A. R. G.; Seager, S.; Schlecker, M.; Schweitzer, A.; Shan, Y.; Soto, M. G.; Subjak, J.; Tal-Or, L.; Trifonov, T.; Vanaverbeke, S.; Vanderspek, R.; Wittrock, J.; Zechmeister, M.; Zohrabi, F.
Abstract: We report the confirmation of a transiting planet around the bright weakly active M0.5 V star TOI-1235 (TYC 4384-1735-1, V ≈ 11.5 mag), whose transit signal was detected in the photometric time series of sectors 14, 20, and 21 of the TESS space mission. We confirm the planetary nature of the transit signal, which has a period of 3.44 d, by using precise RV measurements with the CARMENES, HARPS-N, and iSHELL spectrographs, supplemented by high-resolution imaging and ground-based photometry. A comparison of the properties derived for TOI-1235 b with theoretical models reveals that the planet has a rocky composition, with a bulk density slightly higher than that of Earth. In particular, we measure a mass of Mp = 5.9 ± 0.6 M and a radius of Rp = 1.69 ± 0.08 R, which together result in a density of ρp = 6.7- 1.1+ 1.3 g cm-3. When compared with other well-characterized exoplanetary systems, the particular combination of planetary radius and mass places our discovery in the radius gap, which is a transition region between rocky planets and planets with significant atmospheric envelopes. A few examples of planets occupying the radius gap are known to date. While the exact location of the radius gap for M dwarfs is still a matter of debate, our results constrain it to be located at around 1.7 R or larger at the insolation levels received by TOI-1235 b (~60 S). This makes it an extremely interesting object for further studies of planet formation and atmospheric evolution.
Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602Bouma, L. G.Hartman, J. D.Brahm, R.Evans, P.Collins, Karen A.Zhou, GeorgeSarkis, P.Quinn, Samuel N.de Leon, J.Livingston, J.Bergmann, C.Stassun, K. G.Bhatti, W.Winn, J. N.Bakos, G. Á.Abe, L.Crouzet, N.Dransfield, G.Guillot, T.Marie-Sainte, W.Mékarnia, D.Triaud, A. H. M. J.Tinney, C. G.Henning, T.Espinoza, N.Jordán, A.Barbieri, M.Nandakumar, S.Trifonov, T.Vines, J. I.Vuckovic, M.Ziegler, C.Law, N.Mann, A. W.Ricker, G. R.Vanderspek, R.Seager, S.Jenkins, J. M.Burke, C. J.Dragomir, D.Levine, A. M.Quintana, E. V.Rodriguez, J. E.Smith, J. C.Wohler, B.DOI: info:10.3847/1538-3881/abb9abv. 160239
Bouma, L. G., Hartman, J. D., Brahm, R., Evans, P., Collins, Karen A., Zhou, George, Sarkis, P., Quinn, Samuel N., de Leon, J., Livingston, J., Bergmann, C., Stassun, K. G., Bhatti, W., Winn, J. N., Bakos, G. Á., Abe, L., Crouzet, N., Dransfield, G., Guillot, T., Marie-Sainte, W., Mékarnia, D., Triaud, A. H. M. J., Tinney, C. G., Henning, T., Espinoza, N. et al. 2020. "Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602." The Astronomical Journal 160:239. https://doi.org/10.3847/1538-3881/abb9ab
ID: 158651
Type: article
Authors: Bouma, L. G.; Hartman, J. D.; Brahm, R.; Evans, P.; Collins, Karen A.; Zhou, George; Sarkis, P.; Quinn, Samuel N.; de Leon, J.; Livingston, J.; Bergmann, C.; Stassun, K. G.; Bhatti, W.; Winn, J. N.; Bakos, G. Á.; Abe, L.; Crouzet, N.; Dransfield, G.; Guillot, T.; Marie-Sainte, W.; Mékarnia, D.; Triaud, A. H. M. J.; Tinney, C. G.; Henning, T.; Espinoza, N.; Jordán, A.; Barbieri, M.; Nandakumar, S.; Trifonov, T.; Vines, J. I.; Vuckovic, M.; Ziegler, C.; Law, N.; Mann, A. W.; Ricker, G. R.; Vanderspek, R.; Seager, S.; Jenkins, J. M.; Burke, C. J.; Dragomir, D.; Levine, A. M.; Quintana, E. V.; Rodriguez, J. E.; Smith, J. C.; Wohler, B.
Abstract: We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA Transiting Exoplanet Survey Satellite mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a T = 9.9 mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore ${35}_{-5}^{+11}$ million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of $8.3\,\mathrm{days}$ and is slightly smaller than Jupiter ( ${R}_{{\rm{p}}}={0.77}_{-0.07}^{+0.09}\,{R}_{\mathrm{Jup}}$ ). From radial velocity monitoring, we limit ${M}_{{\rm{p}}}\sin i$ to less than 1.20 MJup (3s). The transits either graze or nearly graze the stellar limb. Grazing transits are a cause for concern, as they are often indicative of astrophysical false-positive scenarios. Our follow-up data show that such scenarios are unlikely. Our combined multicolor photometry, high-resolution imaging, and radial velocities rule out hierarchical eclipsing binary scenarios. Background eclipsing binary scenarios, though limited by speckle imaging, remain a 0.2% possibility. TOI 837b is therefore a validated adolescent exoplanet. The planetary nature of the system can be confirmed or refuted through observations of the stellar obliquity and the planetary mass. Such observations may also improve our understanding of how the physical and orbital properties of exoplanets change in time.
PTFO 8-8695: Two Stars, Two Signals, No PlanetBouma, L. G.Winn, J. N.Ricker, G. R.Vanderspek, R.Latham, David W.Seager, S.Jenkins, J. M.Barclay, T.Collins, Karen A.Doty, J. P.Louie, D. R.Quinn, Samuel N.Rose, M. E.Smith, J. C.Villaseñor, J.Wohler, B.DOI: info:10.3847/1538-3881/ab9e73v. 16086
Bouma, L. G., Winn, J. N., Ricker, G. R., Vanderspek, R., Latham, David W., Seager, S., Jenkins, J. M., Barclay, T., Collins, Karen A., Doty, J. P., Louie, D. R., Quinn, Samuel N., Rose, M. E., Smith, J. C., Villaseñor, J., and Wohler, B. 2020. "PTFO 8-8695: Two Stars, Two Signals, No Planet." The Astronomical Journal 160:86. https://doi.org/10.3847/1538-3881/ab9e73
ID: 157771
Type: article
Authors: Bouma, L. G.; Winn, J. N.; Ricker, G. R.; Vanderspek, R.; Latham, David W.; Seager, S.; Jenkins, J. M.; Barclay, T.; Collins, Karen A.; Doty, J. P.; Louie, D. R.; Quinn, Samuel N.; Rose, M. E.; Smith, J. C.; Villaseñor, J.; Wohler, B.
Abstract: PTFO 8-8695 (CVSO 30) is a star in the 7-10 million year old Orion OB1a cluster that shows brightness dips that resemble planetary transits. Although strong evidence against the planet hypothesis has been presented, the possibility remains debated in the literature. To obtain further clues, we inspected data from the NASA Transiting Exoplanet Survey Satellite (TESS) and the ESA Gaia mission. The Gaia data suggest that PTFO 8-8695 is a binary: the photometric data show it to be overluminous with respect to members of its kinematic group, and the astrometric data are inconsistent with a single star. The TESS light curve shows two different photometric periods. The variability is dominated by a sinusoidal signal with a period of 11.98 hr, presumably caused by stellar rotation. Also present is a 10.76 hr signal consisting of a not-quite sinusoid interrupted by hour-long dips, the type of signal previously interpreted as planetary transits. The phase of the dips is nearly 180° away from the phase of the originally reported dips. As noted previously, this makes them difficult to explain as planetary transits. Instead, we believe that PTFO 8-8695 is a pair of young and rapidly rotating M dwarfs, one of which shows the same "transient-dipper" behavior that has been seen in at least five other cases. The origin of these transient dips is still unknown but likely involves circumstellar material.
TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey SatelliteBrahm, RafaelNielsen, Louise D.Wittenmyer, Robert A.Wang, SonghuRodriguez, Joseph E.Espinoza, NéstorJones, Matías I.Jordán, AndrésHenning, ThomasHobson, MelissaKossakowski, DianaRojas, FelipeSarkis, PaulaSchlecker, MartinTrifonov, TrifonShahaf, SaharRicker, GeorgeVanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, Brett C.Bakos, Gáspár Á.Bhatti, WaqasBayliss, DanielBerlind, PerryBieryla, AllysonBouchy, FrancoisBowler, Brendan P.Briceño, CésarBrown, Timothy M.Bryant, Edward M.Caldwell, Douglas A.Charbonneau, DavidCollins, Karen A.Davis, Allen B.Esquerdo, Gilbert A.Fulton, Benjamin J.Guerrero, Natalia M.Henze, Christopher E.Hogan, AleishaHorner, JonathanHuang, Chelsea X.Irwin, JonathanKane, Stephen R.Kielkopf, JohnMann, Andrew W.Mazeh, TseviMcCormac, JamesMcCully, CurtisMengel, Matthew W.Mireles, IsmaelOkumura, JackPlavchan, PeterQuinn, Samuel N.Rabus, MarkusSaesen, SophieSchlieder, Joshua E.Segransan, DamienShiao, BernieShporer, AviSiverd, Robert J.Stassun, Keivan G.Suc, VincentTan, Thiam-GuanTorres, PascalTinney, Chris G.Udry, StephaneVanzi, LeonardoVezie, MichaelVines, Jose I.Vuckovic, MajaWright, Duncan J.Yahalomi, Daniel A.Zapata, AbnerZhang, HuiZiegler, CarlDOI: info:10.3847/1538-3881/abba3bv. 160235
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 et al. 2020. "TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite." The Astronomical Journal 160:235. https://doi.org/10.3847/1538-3881/abba3b
ID: 158644
Type: article
Authors: 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; Ziegler, Carl
Abstract: We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite 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 ± 0.01 ${R}_{{\rm{J}}}$ and 1.07 ± 0.02 ${R}_{{\rm{J}}}$ , respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 ${M}_{{\rm{J}}}$ versus 0.95 ± 0.07 ${M}_{{\rm{J}}}$ , respectively). Both planets orbit metal-rich stars ( $[\mathrm{Fe}/{\rm{H}}]$ = $+0.26\pm 0.05$ dex and $[\mathrm{Fe}/{\rm{H}}]$ = $+0.24\pm 0.05$ for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a ${M}_{\star }$ = 1.14 ± 0.02 ${M}_{\odot }$ , ${R}_{\star }$ = 1.66 ± 0.02 ${R}_{\odot }$ G-type star ( ${T}_{\mathrm{eff}}$ = $5735\pm 72$ 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 ( ${T}_{\mathrm{eff}}$ = $6261\pm 80$ K), which has a mass of ${M}_{\star }$ = 1.28 ± 0.03 ${M}_{\odot }$ and a radius of ${R}_{\star }$ = 1.39 ± 0.02 ${R}_{\odot }$ . 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.
TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune DesertBurt, Jennifer A.Nielsen, Louise D.Quinn, Samuel N.Mamajek, Eric E.Matthews, Elisabeth C.Zhou, GeorgeSeidel, Julia V.Huang, Chelsea X.Lopez, EricSoto, MaritzaOtegi, JonStassun, Keivan G.Kreidberg, LauraCollins, Karen A.Eastman, Jason D.Rodriguez, Joseph E.Vanderburg, AndrewHalverson, Samuel P.Teske, Johanna K.Wang, Sharon X.Butler, R. PaulBouchy, FrançoisDumusque, XavierSegransen, DamienShectman, Stephen A.Crane, Jeffrey D.Feng, FaboMontet, Benjamin T.Feinstein, Adina D.Beletski, YuriFlowers, ErinGünther, Maximilian N.Daylan, TansuCollins, Kevin I.Conti, Dennis M.Gan, TianjunJensen, Eric L. N.Kielkopf, John F.Tan, Thiam-GuanHelled, RavitDorn, CarolineHaldemann, JonasLissauer, Jack J.Ricker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.Twicken, Joseph D.Smith, Jeffrey C.Tenenbaum, PeterCartwright, ScottBarclay, ThomasPepper, JoshuaEsquerdo, GilbertFong, WilliamDOI: info:10.3847/1538-3881/abac0cv. 160153
Burt, Jennifer A., Nielsen, Louise D., Quinn, Samuel N., Mamajek, Eric E., Matthews, Elisabeth C., Zhou, George, Seidel, Julia V., Huang, Chelsea X., Lopez, Eric, Soto, Maritza, Otegi, Jon, Stassun, Keivan G., Kreidberg, Laura, Collins, Karen A., Eastman, Jason D., Rodriguez, Joseph E., Vanderburg, Andrew, Halverson, Samuel P., Teske, Johanna K., Wang, Sharon X., Butler, R. Paul, Bouchy, François, Dumusque, Xavier, Segransen, Damien, Shectman, Stephen A. et al. 2020. "TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert." The Astronomical Journal 160:153. https://doi.org/10.3847/1538-3881/abac0c
ID: 157601
Type: article
Authors: Burt, Jennifer A.; Nielsen, Louise D.; Quinn, Samuel N.; Mamajek, Eric E.; Matthews, Elisabeth C.; Zhou, George; Seidel, Julia V.; Huang, Chelsea X.; Lopez, Eric; Soto, Maritza; Otegi, Jon; Stassun, Keivan G.; Kreidberg, Laura; Collins, Karen A.; Eastman, Jason D.; Rodriguez, Joseph E.; Vanderburg, Andrew; Halverson, Samuel P.; Teske, Johanna K.; Wang, Sharon X.; Butler, R. Paul; Bouchy, François; Dumusque, Xavier; Segransen, Damien; Shectman, Stephen A.; Crane, Jeffrey D.; Feng, Fabo; Montet, Benjamin T.; Feinstein, Adina D.; Beletski, Yuri; Flowers, Erin; Günther, Maximilian N.; Daylan, Tansu; Collins, Kevin I.; Conti, Dennis M.; Gan, Tianjun; Jensen, Eric L. N.; Kielkopf, John F.; Tan, Thiam-Guan; Helled, Ravit; Dorn, Caroline; Haldemann, Jonas; Lissauer, Jack J.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Twicken, Joseph D.; Smith, Jeffrey C.; Tenenbaum, Peter; Cartwright, Scott; Barclay, Thomas; Pepper, Joshua; Esquerdo, Gilbert; Fong, William
Abstract: We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the Transiting Exoplanet Survey Satellite. The newly discovered planet has a radius Rp = 2.93 ± 0.20 ${R}_{\oplus }$ and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph and the High Accuracy Radial velocity Planet Searcher spectrograph confirm the existence of the planet, and we estimate its mass to be 18.47 ± 1.84 ${M}_{\oplus }$ . The planet's mean density is ${\rho }_{{\rm{p}}}$ = 4.03 ${}_{-0.78}^{+0.98}$ ${\rm{g}}\,{\mathrm{cm}}^{-3}$ , making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud-free atmosphere, and thus it is an excellent candidate for follow-up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated small planet at the edge of the hot Neptune desert that has retained its atmosphere to date.