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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.
Early-time Light Curves of Type Ia Supernovae Observed with TESSFausnaugh, M. M.Vallely, P. J.Kochanek, C. S.Shappee, B. J.Stanek, K. Z.Tucker, M. A.Ricker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.Berta-Thompson, Zachory K.Daylan, TansuDoty, John P.Fűrész, GáborLevine, Alan M.Morris, RobertPál, AndrásSha, LizhouTing, Eric B.Wohler, BillDOI: info:10.3847/1538-4357/abcd42v. 90851
Fausnaugh, M. M., Vallely, P. J., Kochanek, C. S., Shappee, B. J., Stanek, K. Z., Tucker, M. A., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Berta-Thompson, Zachory K., Daylan, Tansu, Doty, John P., Fűrész, Gábor, Levine, Alan M., Morris, Robert, Pál, András, Sha, Lizhou, Ting, Eric B., and Wohler, Bill. 2021. "Early-time Light Curves of Type Ia Supernovae Observed with TESS." The Astrophysical Journal 908:51. https://doi.org/10.3847/1538-4357/abcd42
ID: 159622
Type: article
Authors: Fausnaugh, M. M.; Vallely, P. J.; Kochanek, C. S.; Shappee, B. J.; Stanek, K. Z.; Tucker, M. A.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Berta-Thompson, Zachory K.; Daylan, Tansu; Doty, John P.; Fűrész, Gábor; Levine, Alan M.; Morris, Robert; Pál, András; Sha, Lizhou; Ting, Eric B.; Wohler, Bill
Abstract: We present the early-time light curves of Type Ia supernovae (SNe Ia) observed in the first six sectors of Transiting Exoplanet Survey Satellite (TESS) data. Ten of these SNe were discovered by ASAS-SN, seven by ATLAS, six by ZTF, and one by Gaia. For nine of these objects with sufficient dynamic range (>3.0 mag from detection to peak), we fit power-law models and searched for signatures of companion stars. We found a diversity of early-time light-curve shapes, although most of our sources are consistent with fireball models where the flux increases as ∝t2. Three SNe displayed a flatter rise with flux ∝t. We did not find any obvious evidence for additional structures, such as multiple power-law components, in the early rising light curves. For assumptions about the SN properties and the observer viewing angle (ejecta mass of 1.4 M, expansion velocity of 104 km s-1, opacity of 0.2 cm2 g-1, and viewing angle of 45°) and a further assumption that any companion stars would be in Roche lobe overflow, it is possible to place upper limits on the radii of any companion stars. Six of the nine SNe had complete coverage of the early-time light curves, and we placed upper limits on the radii of companion stars of ≲32 R for these SNe, ≲20 R for five of the six, and ≲4 R for two of the six. The small sample size did not allow us to put limits on the occurrence rate of companion stars in the progenitors of SNe Ia. However, we expect that TESS observed enough SNe in its two-year primary mission (26 sectors) to either detect the signature of a large companion (R > 20 R) or constrain the occurrence rate of such systems, at least for the fiducial SN properties adopted here. We also show that TESS is capable of detecting emission from a 1 R companion for an SN Ia within 50 Mpc and has a reasonable chance of doing so after about six years.
Stellar Radial Velocities in the Old Open Cluster M67 (NGC 2682). II. The Spectroscopic Binary PopulationGeller, Aaron M.Mathieu, Robert D.Latham, David W.Pollack, MaxwellTorres, GuillermoLeiner, Emily M.DOI: info:10.3847/1538-3881/abdd23v. 161190
Geller, Aaron M., Mathieu, Robert D., Latham, David W., Pollack, Maxwell, Torres, Guillermo, and Leiner, Emily M. 2021. "Stellar Radial Velocities in the Old Open Cluster M67 (NGC 2682). II. The Spectroscopic Binary Population." The Astronomical Journal 161:190. https://doi.org/10.3847/1538-3881/abdd23
ID: 159321
Type: article
Authors: Geller, Aaron M.; Mathieu, Robert D.; Latham, David W.; Pollack, Maxwell; Torres, Guillermo; Leiner, Emily M.
Abstract: We present and analyze 120 spectroscopic binary and triple cluster members of the old (4 Gyr) open cluster M67 (NGC 2682). As a cornerstone of stellar astrophysics, M67 is a key cluster in the WIYN Open Cluster Study (WOCS); radial-velocity (RV) observations of M67 are ongoing and extend back over 45 yr, incorporating data from seven different telescopes, and allowing us to detect binaries with orbital periods ≲104 days. Our sample contains 1296 stars (604 cluster members) with magnitudes of 10 ≤ V ≤ 16.5 (about 1.3-0.7 M), from the giants down to ∼4 mag below the main-sequence turnoff, and extends in radius to 30' (7.4 pc at a distance of 850 pc, or ∼7 core radii). This paper focuses primarily on the main-sequence binaries, but orbital solutions are also presented for red giants, yellow giants, and sub-subgiants. Out to our period detection limit and within our magnitude and spatial domain, we find a global main-sequence incompleteness-corrected binary fraction of 34% ± 3%, which rises to 70% ± 17% in the cluster center. We derive a tidal circularization period of ${P}_{\mathrm{circ}}={11.0}_{-1.0}^{+1.1}\,\mathrm{days}$ . We also analyze the incompleteness-corrected distributions of binary orbital elements and masses. The period distribution rises toward longer periods. The eccentricity distribution, beyond Pcirc, is consistent with a uniform distribution. The mass-ratio distribution is also consistent with a uniform distribution. Overall, these M67 binaries are closely consistent with similar binaries in the galactic field, as well as with the old (7 Gyr) open cluster NGC 188. WOCS. 83.
A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of PlanetsHurt, Spencer A.Quinn, Samuel N.Latham, David W.Vanderburg, AndrewEsquerdo, Gilbert A.Calkins, Michael L.Berlind, PerryAngus, RuthLatham, Christian A.Zhou, GeorgeDOI: info:10.3847/1538-3881/abdec8v. 161157
Hurt, Spencer A., Quinn, Samuel N., Latham, David W., Vanderburg, Andrew, Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Angus, Ruth, Latham, Christian A., and Zhou, George. 2021. "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets." The Astronomical Journal 161:157. https://doi.org/10.3847/1538-3881/abdec8
ID: 159324
Type: article
Authors: Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George
Abstract: We present an analysis of 1524 spectra of Vega spanning 10 yr, in which we search for periodic radial-velocity variations. A signal with a periodicity of 0.676 day and a semi-amplitude of ∼10 m s-1 is consistent with the rotation period measured over much shorter time spans by previous spectroscopic and spectropolarimetric studies, confirming the presence of surface features on this A0 star. The activity signal appears to evolve on long timescales, which may indicate the presence of failed fossil magnetic fields on Vega. TESS data reveal Vega's photometric rotational modulation for the first time, with a total amplitude of only 10 ppm. A comparison of the spectroscopic and photometric amplitudes suggests that the surface features may be dominated by bright plages rather than dark spots. For the shortest orbital periods, transit and radial-velocity injection recovery tests exclude the presence of transiting planets larger than 2 R and most non-transiting giant planets. At long periods, we combine our radial velocities with direct imaging from the literature to produce detection limits for Vegan planets and brown dwarfs out to distances of 15 au. Finally, we detect a candidate radial-velocity signal with a period of 2.43 days and a semi-amplitude of 6 m s-1. If caused by an orbiting companion, its minimum mass would be ∼20 M; because of Vega's pole-on orientation, this would correspond to a Jovian planet if the orbit is aligned with the stellar spin. We discuss the prospects for confirmation of this candidate planet.
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.
A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)Sozzetti, A.Damasso, M.Bonomo, A. S.Alibert, Y.Sousa, S. G.Adibekyan, V.Zapatero Osorio, M. R.Gonzalez Hernandez, J. I.Barros, S. C. C.Lillo-Box, J.Stassun, K. G.Winn, J.Cristiani, S.Pepe, F.Rebolo, R.Santos, N. C.Allart, R.Barclay, T.Bouchy, F.Cabral, A.Ciardi, D.Di Marcantonio, P.D'Odorico, V.Ehrenreich, D.Fasnaugh, M.Figueira, P.Haldemann, J.Jenkins, J. M.Latham, D. W.Lavie, B.Lo Curto, G.Lovis, C.Martins, C. J. A. P.Megevand, D.Mehner, A.Micela, G.Molaro, P.Nunes, N. J.Oshagh, M.Otegi, J.Palle, E.Poretti, E.Ricker, G.Rodriguez, D.Seager, S.Suarez Mascareno, A.Twicken, J. D.Udry, S.DOI: info:10.1051/0004-6361/202040034v. 648
Sozzetti, A., Damasso, M., Bonomo, A. S., Alibert, Y., Sousa, S. G., Adibekyan, V., Zapatero Osorio, M. R., Gonzalez Hernandez, J. I., Barros, S. C. C., Lillo-Box, J., Stassun, K. G., Winn, J., Cristiani, S., Pepe, F., Rebolo, R., Santos, N. C., Allart, R., Barclay, T., Bouchy, F., Cabral, A., Ciardi, D., Di Marcantonio, P., D'Odorico, V., Ehrenreich, D., Fasnaugh, M. et al. 2021. "A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)." Astronomy & Astrophysics 648:https://doi.org/10.1051/0004-6361/202040034
ID: 159537
Type: article
Authors: Sozzetti, A.; Damasso, M.; Bonomo, A. S.; Alibert, Y.; Sousa, S. G.; Adibekyan, V.; Zapatero Osorio, M. R.; Gonzalez Hernandez, J. I.; Barros, S. C. C.; Lillo-Box, J.; Stassun, K. G.; Winn, J.; Cristiani, S.; Pepe, F.; Rebolo, R.; Santos, N. C.; Allart, R.; Barclay, T.; Bouchy, F.; Cabral, A.; Ciardi, D.; Di Marcantonio, P.; D'Odorico, V.; Ehrenreich, D.; Fasnaugh, M.; Figueira, P.; Haldemann, J.; Jenkins, J. M.; Latham, D. W.; Lavie, B.; Lo Curto, G.; Lovis, C.; Martins, C. J. A. P.; Megevand, D.; Mehner, A.; Micela, G.; Molaro, P.; Nunes, N. J.; Oshagh, M.; Otegi, J.; Palle, E.; Poretti, E.; Ricker, G.; Rodriguez, D.; Seager, S.; Suarez Mascareno, A.; Twicken, J. D.; Udry, S.
Abstract: Context. Transiting sub-Neptune-type planets, with radii approximately between 2 and 4 R-circle plus, are of particular interest as their study allows us to gain insight into the formation and evolution of a class of planets that are not found in our Solar System.Aims. We exploit the extreme radial velocity (RV) precision of the ultra-stable echelle spectrograph ESPRESSO on the VLT to unveil the physical properties of the transiting sub-Neptune TOI-130 b, uncovered by the TESS mission orbiting the nearby, bright, late F-type star HD 5278 (TOI-130) with a period of P-b = 14.3 days. Methods. We used 43 ESPRESSO high-resolution spectra and broad-band photometry information to derive accurate stellar atmospheric and physical parameters of HD 5278. We exploited the TESS light curve and spectroscopic diagnostics to gauge the impact of stellar activity on the ESPRESSO RVs. We performed separate as well as joint analyses of the TESS photometry and the ESPRESSO RVs using fully Bayesian frameworks to determine the system parameters. Results. Based on the ESPRESSO spectra, the updated stellar parameters of HD 5278 are T-eff = 6203 +/- 64 K, log g = 4.50 +/- 0.11 dex, [Fe/H] = -0.12 +/- 0.04 dex, M-star=1.126(-0.035)(+0.036) M-circle dot, and R-star=1.194(-0.016)(+0.017) R star=1.194(-0.016)(+0.017) R-circle dot. We determine HD 5278 b's mass and radius to be M-b=7.8(-1.4)(+1.5) M-circle plus and R-b = 2.45 +/- 0.05R(circle plus). The derived mean density, rho(b)=2.9(-0.5)(+0.6) g cm(-3), is consistent with the bulk composition of a sub-Neptune with a substantial (similar to 30%) water mass fraction and with a gas envelope comprising similar to 17% of the measured radius. Given the host brightness and irradiation levels, HD 5278 b is one of the best targetsorbiting G-F primaries for follow-up atmospheric characterization measurements with HST and JWST. We discover a second, non-transiting companion in the system, with a period of P-c=40.87(-0.17)(+0.18) days and a minimum mass of M-c sini(c)=18.4(-1.9)(+1.8) M-circle plus. We study emerging trends in parameters space (e.g., mass, radius, stellar insolation, and mean density) of the growing population of transiting sub-Neptunes, and provide statistical evidence for a low occurrence of close-in, 10 - 15M(circle plus) companions around G-F primaries with T-eff greater than or similar to 5500 K.
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.
Gravity-darkening Analysis of the Misaligned Hot Jupiter MASCARA-4 bAhlers, John P.Kruse, EthanColón, Knicole D.Dorval, PatrickTalens, Geert JanSnellen, IgnasAlbrecht, SimonOtten, GillesRicker, GeorgeVanderspek, RolandLatham, DavidSeager, SaraWinn, JoshuaJenkins, Jon M.Haworth, KariCartwright, ScottMorris, RobertRowden, PamTenenbaum, PeterTing, Eric B.DOI: info:10.3847/1538-4357/ab59d0v. 88863
Ahlers, John P., Kruse, Ethan, Colón, Knicole D., Dorval, Patrick, Talens, Geert Jan, Snellen, Ignas, Albrecht, Simon, Otten, Gilles, Ricker, George, Vanderspek, Roland, Latham, David, Seager, Sara, Winn, Joshua, Jenkins, Jon M., Haworth, Kari, Cartwright, Scott, Morris, Robert, Rowden, Pam, Tenenbaum, Peter, and Ting, Eric B. 2020. "Gravity-darkening Analysis of the Misaligned Hot Jupiter MASCARA-4 b." The Astrophysical Journal 888:63. https://doi.org/10.3847/1538-4357/ab59d0
ID: 155699
Type: article
Authors: Ahlers, John P.; Kruse, Ethan; Colón, Knicole D.; Dorval, Patrick; Talens, Geert Jan; Snellen, Ignas; Albrecht, Simon; Otten, Gilles; Ricker, George; Vanderspek, Roland; Latham, David; Seager, Sara; Winn, Joshua; Jenkins, Jon M.; Haworth, Kari; Cartwright, Scott; Morris, Robert; Rowden, Pam; Tenenbaum, Peter; Ting, Eric B.
Abstract: MASCARA-4 b is a hot Jupiter in a highly misaligned orbit around a rapidly rotating A3V star that was observed for 54 days by the Transiting Exoplanet Survey Satellite (TESS). We perform two analyses of MASCARA-4 b using a stellar gravity-darkened model. First, we measure MASCARA-4 b's misaligned orbital configuration by modeling its TESS photometric light curve. We take advantage of the asymmetry in MASCARA-4 b's transit due to its host star's gravity-darkened surface to measure MASCARA-4 b's true spin─orbit angle to be 104°{}-{13^\circ }+{7^\circ }. We also detect a ∼4σ secondary eclipse at 0.491 ± 0.007 orbital phase, proving that the orbit is slightly eccentric. Second, we model MASCARA-4 b's insolation including gravity darkening and find that the planet's received X-ray and ultraviolet flux varies by 4% throughout its orbit. MASCARA-4 b's short-period, polar orbit suggests that the planet likely underwent dramatic orbital evolution to end up in its present-day configuration and that it receives a varying stellar irradiance that perpetually forces the planet out of thermal equilibrium. These findings make MASCARA-4 b an excellent target for follow-up characterization to better understand the orbital evolution and present-day environment of planets around high-mass stars.
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.
HATS-71b: A Giant Planet Transiting an M3 Dwarf Star in TESS Sector 1Bakos, G. Á.Bayliss, D.Bento, J.Bhatti, W.Brahm, R.Csubry, Z.Espinoza, N.Hartman, J. D.Henning, ThJordán, A.Mancini, L.Penev, K.Rabus, M.Sarkis, P.Suc, V.de Val-Borro, M.Zhou, GeorgeButler, R. P.Crane, J.Durkan, S.Shectman, S.Kim, J.Lázár, J.Papp, I.Sári, P.Ricker, G.Vanderspek, R.Latham, David W.Seager, S.Winn, J. N.Jenkins, J.Chacon, A. D.Fűrész, G.Goeke, B.Li, J.Quinn, SamuelQuintana, E. V.Tenenbaum, P.Teske, J.Vezie, M.Yu, L.Stockdale, C.Evans, P.Relles, H. M.DOI: info:10.3847/1538-3881/ab8ad1v. 159267
Bakos, G. Á., Bayliss, D., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., Hartman, J. D., Henning, Th, Jordán, A., Mancini, L., Penev, K., Rabus, M., Sarkis, P., Suc, V., de Val-Borro, M., Zhou, George, Butler, R. P., Crane, J., Durkan, S., Shectman, S., Kim, J., Lázár, J., Papp, I., Sári, P. et al. 2020. "HATS-71b: A Giant Planet Transiting an M3 Dwarf Star in TESS Sector 1." The Astronomical Journal 159:267. https://doi.org/10.3847/1538-3881/ab8ad1
ID: 156870
Type: article
Authors: Bakos, G. Á.; Bayliss, D.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J. D.; Henning, Th; Jordán, A.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, George; Butler, R. P.; Crane, J.; Durkan, S.; Shectman, S.; Kim, J.; Lázár, J.; Papp, I.; Sári, P.; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, S.; Winn, J. N.; Jenkins, J.; Chacon, A. D.; Fűrész, G.; Goeke, B.; Li, J.; Quinn, Samuel; Quintana, E. V.; Tenenbaum, P.; Teske, J.; Vezie, M.; Yu, L.; Stockdale, C.; Evans, P.; Relles, H. M.
Abstract: We report the discovery of HATS-71b, a transiting gas giant planet on a $P=3.7955$ day orbit around a $G=15.35$ mag M3 dwarf star. HATS-71 is the coolest M dwarf star known to host a hot Jupiter. The loss of light during transits is 4.7%, more than in any other confirmed transiting planet system. The planet was identified as a candidate by the ground- based HATSouth transit survey. It was confirmed using ground-based photometry, spectroscopy, and imaging, as well as space-based photometry from the NASA Transiting Exoplanet Survey Satellite mission (TIC 234523599). Combining all of these data, and utilizing Gaia DR2, we find that the planet has a radius of $1.024\pm 0.018$ ${R}_{{\rm{J}}}$ and mass of $0.37\,\pm 0.24$ ${M}_{{\rm{J}}}$ (95% confidence upper limit of $\lt 0.80$ ${M}_{{\rm{J}}}$ ), while the star has a mass of $0.4861\pm 0.0060$ ${M}_{\odot }$ and a radius of $0.4783\pm 0.0060$ ${R}_{\odot }$ .