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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.
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.
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 Observations of the WASP-121 b Phase CurveDaylan, TansuGünther, Maximilian N.Mikal-Evans, ThomasSing, David K.Wong, IanShporer, AviNiraula, Prajwalde Wit, JulienKoll, Daniel D. B.Parmentier, VivienFetherolf, TaraKane, Stephen R.Ricker, George R.Vanderspek, RolandSeager, S.Winn, Joshua N.Jenkins, Jon M.Caldwell, Douglas A.Charbonneau, DavidHenze, Christopher E.Paegert, MartinRinehart, StephenRose, MarkSha, LizhouQuintana, ElisaVillasenor, Jesus NoelDOI: info:10.3847/1538-3881/abd8d2v. 161131
Daylan, Tansu, Günther, Maximilian N., Mikal-Evans, Thomas, Sing, David K., Wong, Ian, Shporer, Avi, Niraula, Prajwal, de Wit, Julien, Koll, Daniel D. B., Parmentier, Vivien, Fetherolf, Tara, Kane, Stephen R., Ricker, George R., Vanderspek, Roland, Seager, S., Winn, Joshua N., Jenkins, Jon M., Caldwell, Douglas A., Charbonneau, David, Henze, Christopher E., Paegert, Martin, Rinehart, Stephen, Rose, Mark, Sha, Lizhou, Quintana, Elisa et al. 2021. "TESS Observations of the WASP-121 b Phase Curve." The Astronomical Journal 161:131.
ID: 159326
Type: article
Authors: Daylan, Tansu; Günther, Maximilian N.; Mikal-Evans, Thomas; Sing, David K.; Wong, Ian; Shporer, Avi; Niraula, Prajwal; de Wit, Julien; Koll, Daniel D. B.; Parmentier, Vivien; Fetherolf, Tara; Kane, Stephen R.; Ricker, George R.; Vanderspek, Roland; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Caldwell, Douglas A.; Charbonneau, David; Henze, Christopher E.; Paegert, Martin; Rinehart, Stephen; Rose, Mark; Sha, Lizhou; Quintana, Elisa; Villasenor, Jesus Noel
Abstract: We study the red-optical photometry of the ultrahot Jupiter WASP-121 b as observed by the Transiting Exoplanet Survey Satellite (TESS) and model its atmosphere through a radiative transfer simulation. Given its short orbital period of ∼1.275 days, inflated state, and bright host star, WASP-121 b is exceptionally favorable for detailed atmospheric characterization. Toward this purpose, we use allesfitter to characterize its full red-optical phase curve, including the planetary phase modulation and secondary eclipse. We measure the day- and nightside brightness temperatures in the TESS passband as ${3012}_{-42}^{+40}$ and ${2022}_{-602}^{+254}$ K, respectively, and do not find a statistically significant phase shift between the brightest and substellar points. This is consistent with inefficient heat recirculation on the planet. We then perform an atmospheric retrieval analysis to infer the dayside atmospheric properties of WASP-121 b, such as its bulk composition, albedo, and heat recirculation. We confirm the temperature inversion in the atmosphere and suggest H-, TiO, and VO as potential causes of the inversion, absorbing heat at optical wavelengths at low pressures. Future Hubble Space Telescope and James Webb Space Telescope observations of WASP-121 b will benefit from its first full phase curve measured by TESS.
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.
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 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. 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.
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 ( or via 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.
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.
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.
A Pair of TESS Planets Spanning the Radius Valley around the Nearby Mid-M Dwarf LTT 3780Cloutier, RyanEastman, Jason D.Rodriguez, Joseph E.Astudillo-Defru, NicolaBonfils, XavierMortier, AnneliesWatson, Christopher A.Stalport, ManuPinamonti, MatteoLienhard, FlorianHarutyunyan, AvetDamasso, MarioLatham, David W.Collins, Karen A.Massey, RobertIrwin, JonathanWinters, Jennifer G.Charbonneau, DavidZiegler, CarlMatthews, ElisabethCrossfield, Ian J. M.Kreidberg, LauraQuinn, Samuel N.Ricker, GeorgeVanderspek, RolandSeager, SaraWinn, JoshuaJenkins, Jon M.Vezie, MichaelUdry, StéphaneTwicken, Joseph D.Tenenbaum, PeterSozzetti, AlessandroSégransan, DamienSchlieder, Joshua E.Sasselov, DimitarSantos, Nuno C.Rice, KenRackham, Benjamin V.Poretti, EnnioPiotto, GiampaoloPhillips, DavidPepe, FrancescoMolinari, EmilioMignon, LucileMicela, GiuseppinaMelo, Claudiode Medeiros, José R.Mayor, MichelMatson, Rachel A.Martinez Fiorenzano, Aldo F.Mann, Andrew W.Magazzú, AntonioLovis, ChristopheLópez-Morales, MercedesLopez, EricLissauer, Jack J.Lépine, SébastienLaw, NicholasKielkopf, John F.Johnson, John A.Jensen, Eric L. N.Howell, Steve B.Gonzales, EricaGhedina, AdrianoForveille, ThierryFigueira, PedroDumusque, XavierDressing, Courtney D.Doyon, RenéDíaz, Rodrigo F.Fabrizio, Luca DiDelfosse, XavierCosentino, RosarioConti, Dennis M.Collins, Kevin I.Cameron, Andrew CollierCiardi, DavidCaldwell, Douglas A.Burke, ChristopherBuchhave, LarsBriceño, CésarBoyd, PatriciaBouchy, FrançoisBeichman, CharlesArtigau, ÉtienneAlmenara, Jose M.DOI: info:10.3847/1538-3881/ab91c2v. 160No. 13
Cloutier, Ryan, Eastman, Jason D., Rodriguez, Joseph E., Astudillo-Defru, Nicola, Bonfils, Xavier, Mortier, Annelies, Watson, Christopher A., Stalport, Manu, Pinamonti, Matteo, Lienhard, Florian, Harutyunyan, Avet, Damasso, Mario, Latham, David W., Collins, Karen A., Massey, Robert, Irwin, Jonathan, Winters, Jennifer G., Charbonneau, David, Ziegler, Carl, Matthews, Elisabeth, Crossfield, Ian J. M., Kreidberg, Laura, Quinn, Samuel N., Ricker, George, Vanderspek, Roland et al. 2020. "A Pair of TESS Planets Spanning the Radius Valley around the Nearby Mid-M Dwarf LTT 3780." The Astronomical Journal 160 (1):3.
ID: 157584
Type: article
Authors: Cloutier, Ryan; Eastman, Jason D.; Rodriguez, Joseph E.; Astudillo-Defru, Nicola; Bonfils, Xavier; Mortier, Annelies; Watson, Christopher A.; Stalport, Manu; Pinamonti, Matteo; Lienhard, Florian; Harutyunyan, Avet; Damasso, Mario; Latham, David W.; Collins, Karen A.; Massey, Robert; Irwin, Jonathan; Winters, Jennifer G.; Charbonneau, David; Ziegler, Carl; Matthews, Elisabeth; Crossfield, Ian J. M.; Kreidberg, Laura; Quinn, Samuel N.; Ricker, George; Vanderspek, Roland; Seager, Sara; Winn, Joshua; Jenkins, Jon M.; Vezie, Michael; Udry, Stéphane; Twicken, Joseph D.; Tenenbaum, Peter; Sozzetti, Alessandro; Ségransan, Damien; Schlieder, Joshua E.; Sasselov, Dimitar; Santos, Nuno C.; Rice, Ken; Rackham, Benjamin V.; Poretti, Ennio; Piotto, Giampaolo; Phillips, David; Pepe, Francesco; Molinari, Emilio; Mignon, Lucile; Micela, Giuseppina; Melo, Claudio; de Medeiros, José R.; Mayor, Michel; Matson, Rachel A.; Martinez Fiorenzano, Aldo F.; Mann, Andrew W.; Magazzú, Antonio; Lovis, Christophe; López-Morales, Mercedes; Lopez, Eric; Lissauer, Jack J.; Lépine, Sébastien; Law, Nicholas; Kielkopf, John F.; Johnson, John A.; Jensen, Eric L. N.; Howell, Steve B.; Gonzales, Erica; Ghedina, Adriano; Forveille, Thierry; Figueira, Pedro; Dumusque, Xavier; Dressing, Courtney D.; Doyon, René; Díaz, Rodrigo F.; Fabrizio, Luca Di; Delfosse, Xavier; Cosentino, Rosario; Conti, Dennis M.; Collins, Kevin I.; Cameron, Andrew Collier; Ciardi, David; Caldwell, Douglas A.; Burke, Christopher; Buchhave, Lars; Briceño, César; Boyd, Patricia; Bouchy, François; Beichman, Charles; Artigau, Étienne; Almenara, Jose M.
Abstract: We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, V = 13.07, Ks = 8.204, Rs = 0.374 R, Ms = 0.401 M, d = 22 pc). The two planet candidates are identified in a single Transiting Exoplanet Survey Satellite sector and validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of Pb = 0.77, Pc = 12.25 days and sizes rp,b = 1.33 ± 0.07, rp,c = 2.30 ± 0.16 R, the two planets span the radius valley in period-radius space around low-mass stars, thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial velocity measurements from the High Accuracy Radial velocity Planet Searcher (HARPS) and HARPS-N, we measure planet masses of ${m}_{p,b}={2.62}_{-0.46}^{+0.48}$ and ${m}_{p,c}={8.6}_{-1.3}^{+1.6}$ M, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and core-powered mass-loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley.
TOI-1235 b: A Keystone Super-Earth for Testing Radius Valley Emergence Models around Early M DwarfsCloutier, RyanRodriguez, Joseph E.Irwin, JonathanCharbonneau, DavidStassun, Keivan G.Mortier, AnneliesLatham, David W.Isaacson, HowardHoward, Andrew W.Udry, StéphaneWilson, Thomas G.Watson, Christopher A.Pinamonti, MatteoLienhard, FlorianGiacobbe, PaoloGuerra, PereCollins, Karen A.Beiryla, AllysonEsquerdo, Gilbert A.Matthews, ElisabethMatson, Rachel A.Howell, Steve B.Furlan, EliseCrossfield, Ian J. M.Winters, Jennifer G.Nava, ChantanelleMent, KristoLopez, Eric D.Ricker, GeorgeVanderspek, RolandSeager, SaraJenkins, Jon M.Ting, Eric B.Tenenbaum, PeterSozzetti, AlessandroSha, LizhouSégransan, DamienSchlieder, Joshua E.Sasselov, DimitarRoy, ArpitaRobertson, PaulRice, KenPoretti, EnnioPiotto, GiampaoloPhillips, DavidPepper, JoshuaPepe, FrancescoMolinari, EmilioMocnik, TeoMicela, GiuseppinaMayor, MichelMartinez Fiorenzano, Aldo F.Mallia, FrancoLubin, JackLovis, ChristopheLópez-Morales, MercedesKosiarek, Molly R.Kielkopf, John F.Kane, Stephen R.Jensen, Eric L. N.Isopi, GiovanniHuber, DanielHill, Michelle L.Harutyunyan, AvetGonzales, EricaGiacalone, StevenGhedina, AdrianoErcolino, AndreaDumusque, XavierDressing, Courtney D.Damasso, MarioDalba, Paul A.Cosentino, RosarioConti, Dennis M.Colón, Knicole D.Collins, Kevin I.Cameron, Andrew CollierCiardi, DavidChristiansen, JessieChontos, AshleyCecconi, MassimoCaldwell, Douglas A.Burke, ChristopherBuchhave, LarsBeichman, CharlesBehmard, AidaBeard, CoreyAkana Murphy, Joseph M.DOI: info:10.3847/1538-3881/ab9534v. 160No. 122
Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G. et al. 2020. "TOI-1235 b: A Keystone Super-Earth for Testing Radius Valley Emergence Models around Early M Dwarfs." The Astronomical Journal 160 (1):22.
ID: 157585
Type: article
Authors: Cloutier, Ryan; Rodriguez, Joseph E.; Irwin, Jonathan; Charbonneau, David; Stassun, Keivan G.; Mortier, Annelies; Latham, David W.; Isaacson, Howard; Howard, Andrew W.; Udry, Stéphane; Wilson, Thomas G.; Watson, Christopher A.; Pinamonti, Matteo; Lienhard, Florian; Giacobbe, Paolo; Guerra, Pere; Collins, Karen A.; Beiryla, Allyson; Esquerdo, Gilbert A.; Matthews, Elisabeth; Matson, Rachel A.; Howell, Steve B.; Furlan, Elise; Crossfield, Ian J. M.; Winters, Jennifer G.; Nava, Chantanelle; Ment, Kristo; Lopez, Eric D.; Ricker, George; Vanderspek, Roland; Seager, Sara; Jenkins, Jon M.; Ting, Eric B.; Tenenbaum, Peter; Sozzetti, Alessandro; Sha, Lizhou; Ségransan, Damien; Schlieder, Joshua E.; Sasselov, Dimitar; Roy, Arpita; Robertson, Paul; Rice, Ken; Poretti, Ennio; Piotto, Giampaolo; Phillips, David; Pepper, Joshua; Pepe, Francesco; Molinari, Emilio; Mocnik, Teo; Micela, Giuseppina; Mayor, Michel; Martinez Fiorenzano, Aldo F.; Mallia, Franco; Lubin, Jack; Lovis, Christophe; López-Morales, Mercedes; Kosiarek, Molly R.; Kielkopf, John F.; Kane, Stephen R.; Jensen, Eric L. N.; Isopi, Giovanni; Huber, Daniel; Hill, Michelle L.; Harutyunyan, Avet; Gonzales, Erica; Giacalone, Steven; Ghedina, Adriano; Ercolino, Andrea; Dumusque, Xavier; Dressing, Courtney D.; Damasso, Mario; Dalba, Paul A.; Cosentino, Rosario; Conti, Dennis M.; Colón, Knicole D.; Collins, Kevin I.; Cameron, Andrew Collier; Ciardi, David; Christiansen, Jessie; Chontos, Ashley; Cecconi, Massimo; Caldwell, Douglas A.; Burke, Christopher; Buchhave, Lars; Beichman, Charles; Behmard, Aida; Beard, Corey; Akana Murphy, Joseph M.
Abstract: Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period-radius space. Here we present the confirmation of TOI-1235 b (P = 3.44 days, ${r}_{{\rm{p}}}={1.738}_{-0.076}^{+0.087}$ ${R}_{\oplus }$ ), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (Rs = 0.630 ± 0.015 ${R}_{\odot }$ , Ms = 0.640 ± 0.016 ${M}_{\odot }$ ). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of ${6.91}_{-0.85}^{+0.75}$ ${M}_{\oplus }$ , which implies an iron core mass fraction of ${20}_{-12}^{+15}$ % in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be <0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin ( $P={21.8}_{-0.8}^{+0.9}$ days, ${m}_{{\rm{p}}}\sin i={13.0}_{-5.3}^{+3.8}$ ${M}_{\oplus }$ ) that cannot be firmly ruled out by our data.
The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 cDai, FeiRoy, ArpitaFulton, BenjaminRobertson, PaulHirsch, LeaIsaacson, HowardAlbrecht, SimonMann, Andrew W.Kristiansen, Martti H.Batalha, Natalie M.Beard, CoreyBehmard, AidaChontos, AshleyCrossfield, Ian J. M.Dalba, Paul A.Dressing, CourtneyGiacalone, StevenHill, MichelleHoward, Andrew W.Huber, DanielKane, Stephen R.Kosiarek, MollyLubin, JackMayo, AndrewMocnik, TeoAkana Murphy, Joseph M.Petigura, Erik A.Rosenthal, LeeRubenzahl, Ryan A.Scarsdale, NicholasWeiss, Lauren M.Van Zandt, JudahRicker, George R.Vanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Caldwell, Douglas A.Charbonneau, DavidDaylan, TansuGünther, Maximilian N.Morgan, EdwardQuinn, Samuel N.Rose, Mark E.Smith, Jeffrey C.DOI: info:10.3847/1538-3881/abb3bdv. 160193
Dai, Fei, Roy, Arpita, Fulton, Benjamin, Robertson, Paul, Hirsch, Lea, Isaacson, Howard, Albrecht, Simon, Mann, Andrew W., Kristiansen, Martti H., Batalha, Natalie M., Beard, Corey, Behmard, Aida, Chontos, Ashley, Crossfield, Ian J. M., Dalba, Paul A., Dressing, Courtney, Giacalone, Steven, Hill, Michelle, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Kosiarek, Molly, Lubin, Jack, Mayo, Andrew, Mocnik, Teo et al. 2020. "The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 c." The Astronomical Journal 160:193.
ID: 157582
Type: article
Authors: Dai, Fei; Roy, Arpita; Fulton, Benjamin; Robertson, Paul; Hirsch, Lea; Isaacson, Howard; Albrecht, Simon; Mann, Andrew W.; Kristiansen, Martti H.; Batalha, Natalie M.; Beard, Corey; Behmard, Aida; Chontos, Ashley; Crossfield, Ian J. M.; Dalba, Paul A.; Dressing, Courtney; Giacalone, Steven; Hill, Michelle; Howard, Andrew W.; Huber, Daniel; Kane, Stephen R.; Kosiarek, Molly; Lubin, Jack; Mayo, Andrew; Mocnik, Teo; Akana Murphy, Joseph M.; Petigura, Erik A.; Rosenthal, Lee; Rubenzahl, Ryan A.; Scarsdale, Nicholas; Weiss, Lauren M.; Van Zandt, Judah; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Caldwell, Douglas A.; Charbonneau, David; Daylan, Tansu; Günther, Maximilian N.; Morgan, Edward; Quinn, Samuel N.; Rose, Mark E.; Smith, Jeffrey C.
Abstract: We report the measurement of a spectroscopic transit of TOI-1726c, one of two planets transiting a G-type star with V = 6.9 in the Ursa Major Moving Group (∼400 Myr). With a precise age constraint from cluster membership, TOI-1726 provides a great opportunity to test various obliquity excitation scenarios that operate on different timescales. By modeling the Rossiter-McLaughlin (RM) effect, we derived a sky-projected obliquity of $-{1}_{-32}^{{+35}^\circ} $ . This result rules out a polar/retrograde orbit and is consistent with an aligned orbit for planet c. Considering the previously reported, similarly prograde RM measurement of planet b and the transiting nature of both planets, TOI-1726 tentatively conforms to the overall picture that compact multitransiting planetary systems tend to have coplanar, likely aligned orbits. TOI-1726 is also a great atmospheric target for understanding differential atmospheric loss of sub-Neptune planets (planet b 2.2 R and c 2.7 R both likely underwent photoevaporation). The coplanar geometry points to a dynamically cold history of the system that simplifies any future modeling of atmospheric escape.
The K2 and TESS Synergy. I. Updated Ephemerides and Parameters for K2-114, K2-167, K2-237, and K2-261Ikwut-Ukwa, MmaRodriguez, Joseph E.Bieryla, AllysonVanderburg, AndrewMocnik, TeoKane, Stephen R.Quinn, Samuel N.Colón, Knicole D.Zhou, GeorgeEastman, Jason D.Huang, Chelsea X.Latham, David W.Dotson, JessieJenkins, Jon M.Ricker, George R.Seager, SaraVanderspek, Roland K.Winn, Joshua N.Barclay, ThomasBarentsen, GeertBerta-Thompson, ZachoryCharbonneau, DavidDragomir, DianaDaylan, TansuGünther, Maximilian N.Hedges, ChristinaHenze, Christopher E.McDermott, ScottSchlieder, Joshua E.Quintana, Elisa V.Smith, Jeffrey C.Twicken, Joseph D.Yahalomi, Daniel A.DOI: info:10.3847/1538-3881/aba964v. 160209
Ikwut-Ukwa, Mma, Rodriguez, Joseph E., Bieryla, Allyson, Vanderburg, Andrew, Mocnik, Teo, Kane, Stephen R., Quinn, Samuel N., Colón, Knicole D., Zhou, George, Eastman, Jason D., Huang, Chelsea X., Latham, David W., Dotson, Jessie, Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland K., Winn, Joshua N., Barclay, Thomas, Barentsen, Geert, Berta-Thompson, Zachory, Charbonneau, David, Dragomir, Diana, Daylan, Tansu, Günther, Maximilian N. et al. 2020. "The K2 and TESS Synergy. I. Updated Ephemerides and Parameters for K2-114, K2-167, K2-237, and K2-261." The Astronomical Journal 160:209.
ID: 158655
Type: article
Authors: Ikwut-Ukwa, Mma; Rodriguez, Joseph E.; Bieryla, Allyson; Vanderburg, Andrew; Mocnik, Teo; Kane, Stephen R.; Quinn, Samuel N.; Colón, Knicole D.; Zhou, George; Eastman, Jason D.; Huang, Chelsea X.; Latham, David W.; Dotson, Jessie; Jenkins, Jon M.; Ricker, George R.; Seager, Sara; Vanderspek, Roland K.; Winn, Joshua N.; Barclay, Thomas; Barentsen, Geert; Berta-Thompson, Zachory; Charbonneau, David; Dragomir, Diana; Daylan, Tansu; Günther, Maximilian N.; Hedges, Christina; Henze, Christopher E.; McDermott, Scott; Schlieder, Joshua E.; Quintana, Elisa V.; Smith, Jeffrey C.; Twicken, Joseph D.; Yahalomi, Daniel A.
Abstract: Although the Transiting Exoplanet Survey Satellite (TESS) primary mission observed the northern and southern ecliptic hemispheres, generally avoiding the ecliptic, and the Kepler space telescope during the K2 mission could only observe near the ecliptic, many of the K2 fields extend far enough from the ecliptic plane that sections overlap with TESS fields. Using photometric observations from both K2 and TESS, combined with archival spectroscopic observations, we globally modeled four known planetary systems discovered by K2 that were observed in the first year of the primary TESS mission. Specifically, we provide updated ephemerides and system parameters for K2-114 b, K2-167 b, K2-237 b, and K2-261 b. These were some of the first K2 planets to be observed by TESS in the first year and include three Jovian sized planets and a sub-Neptune with orbital periods less than 12 days. In each case, the updated ephemeris significantly reduces the uncertainty in prediction of future times of transit, which is valuable for planning observations with the James Webb Space Telescope and other future facilities. The TESS extended mission is expected to observe about half of the K2 fields, providing the opportunity to perform this type of analysis on a larger number of systems.
The Young Planetary System K2-25: Constraints on Companions and StarspotsKain, Isabel J.Newton, Elisabeth R.Dittmann, Jason A.Irwin, Jonathan M.Mann, Andrew W.Thao, Pa ChiaCharbonneau, DavidWinters, Jennifer G.DOI: info:10.3847/1538-3881/ab655bv. 15983
Kain, Isabel J., Newton, Elisabeth R., Dittmann, Jason A., Irwin, Jonathan M., Mann, Andrew W., Thao, Pa Chia, Charbonneau, David, and Winters, Jennifer G. 2020. "The Young Planetary System K2-25: Constraints on Companions and Starspots." The Astronomical Journal 159:83.
ID: 156364
Type: article
Authors: Kain, Isabel J.; Newton, Elisabeth R.; Dittmann, Jason A.; Irwin, Jonathan M.; Mann, Andrew W.; Thao, Pa Chia; Charbonneau, David; Winters, Jennifer G.
Abstract: The abundance of planets with orbital periods of a few to tens of days suggests that exoplanets experience complex dynamical histories. Planets in young stellar clusters or associations have well-constrained ages and therefore provide an opportunity to explore the dynamical evolution of exoplanets. K2-25b is a Neptune-sized planet in an eccentric, 3.48 day orbit around an M4.5 dwarf star in the Hyades cluster (650 Myr). In order to investigate its non-zero eccentricity and tight orbit, we analyze transit timing variations (TTVs) which could reveal clues to the migration processes that may have acted on the planet. We obtain 12 nonconsecutive transits using the MEarth observatories and long-term photometric monitoring, which we combine with 10 transits from the Spitzer Space Telescope and 20 transits from K2. Tables of MEarth photometry accompany this work. We fit each transit lightcurve independently. We first investigate whether inhomogeneities on the stellar surface (such as spots or plages) are differentially affecting our transit observations. The measured transit depth does not vary significantly between transits, though we see some deviations from the fiducial transit model. We then looked for TTVs as evidence of a nontransiting perturber in the system. We find no evidence for >1 M mass companions within a 2:1 period ratio, or for >5 M mass planets within a 7:2 period ratio.
Erratum: An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star (2019, AJ, 158, 165)Mayo, Andrew W.Rajpaul, Vinesh M.Buchhave, Lars A.Dressing, Courtney D.Mortier, AnneliesZeng, LiFortenbach, Charles D.Aigrain, SuzanneBonomo, Aldo S.Collier Cameron, AndrewCharbonneau, DavidCoffinet, AdrienCosentino, RosarioDamasso, MarioDumusque, XavierMartinez Fiorenzano, A. F.Haywood, Raphaëlle D.Latham, David W.López-Morales, MercedesMalavolta, LucaMicela, GiusiMolinari, EmilioPearce, LoganPepe, FrancescoPhillips, DavidPiotto, GiampaoloPoretti, EnnioRice, KenSozzetti, AlessandroUdry, StephaneDOI: info:10.3847/1538-3881/ab5e5ev. 15934
Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Collier Cameron, Andrew, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Martinez Fiorenzano, A. F., Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David et al. 2020. "Erratum: "An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star" (2019, AJ, 158, 165)." The Astronomical Journal 159:34.
ID: 155703
Type: article
Authors: Mayo, Andrew W.; Rajpaul, Vinesh M.; Buchhave, Lars A.; Dressing, Courtney D.; Mortier, Annelies; Zeng, Li; Fortenbach, Charles D.; Aigrain, Suzanne; Bonomo, Aldo S.; Collier Cameron, Andrew; Charbonneau, David; Coffinet, Adrien; Cosentino, Rosario; Damasso, Mario; Dumusque, Xavier; Martinez Fiorenzano, A. F.; Haywood, Raphaëlle D.; Latham, David W.; López-Morales, Mercedes; Malavolta, Luca; Micela, Giusi; Molinari, Emilio; Pearce, Logan; Pepe, Francesco; Phillips, David; Piotto, Giampaolo; Poretti, Ennio; Rice, Ken; Sozzetti, Alessandro; Udry, Stephane
Flare Rates, Rotation Periods, and Spectroscopic Activity Indicators of a Volume-complete Sample of Mid- to Late-M Dwarfs within 15 pcMedina, Amber A.Winters, Jennifer G.Irwin, Jonathan M.Charbonneau, DavidDOI: info:10.3847/1538-4357/abc686v. 905107
Medina, Amber A., Winters, Jennifer G., Irwin, Jonathan M., and Charbonneau, David. 2020. "Flare Rates, Rotation Periods, and Spectroscopic Activity Indicators of a Volume-complete Sample of Mid- to Late-M Dwarfs within 15 pc." The Astrophysical Journal 905:107.
ID: 158738
Type: article
Authors: Medina, Amber A.; Winters, Jennifer G.; Irwin, Jonathan M.; Charbonneau, David
Abstract: We present a study of flare rates, rotation periods, and spectroscopic activity indicators of 125 single stars within 15 parsecs and with masses between 0.1 and 0.3 M? observed during the first year of the TESS mission, with the goal of elucidating the relationship between these various magnetically connected phenomena. We gathered multiepoch high-resolution spectra of each target, and we measured equivalent widths of the activity indicators helium I D3, Ha, and the calcium infrared triplet line at 8542.09 Å. We present 18 new rotation periods from MEarth photometry and 19 new rotation periods from TESS photometry. We present a catalog of 1392 flares. After correcting for sensitivity, we find the slope of the flare frequency distribution for all stars to have a standard value of a = 1.98 ± 0.02. We determine R31.5, the rate of flares per day with energies above E = 3.16 × 1031 ergs in the TESS bandpass. We find that below a critical value of Ha EW = -0.71 Å, log R31.5 increases linearly with increasing Ha emission; above this value, log R31.5 declines rapidly. The stars divide into two groups: 26% have Ha in emission, high flare rates with typical values of log R31.5 = -1.30 ± 0.08, and have Rossby numbers = -1.30 ± 0.08, and have Rossby numbers 31.5 < -3.86, with the majority of these stars not showing a single flare during the TESS observations.
K2-111: an old system with two planets in near-resonanceMortier, A.Zapatero Osorio, M. R.Malavolta, L.Alibert, Y.Rice, K.Lillo-Box, J.Vanderburg, A.Oshagh, M.Buchhave, L.Adibekyan, V.Delgado Mena, E.Lopez-Morales, MercedesCharbonneau, DavidSousa, S. G.Lovis, C.Affer, L.Allende Prieto, C.Barros, S. C. C.Benatti, S.Bonomo, A. S.Boschin, W.Bouchy, F.Cabral, A.Collier Cameron, A.Cosentino, R.Cristiani, S.Demangeon, O. D. S.Di Marcantonio, P.D'Odorico, V.Dumusque, X.Ehrenreich, D.Figueira, P.Fiorenzano, A.Ghedina, A.González Hernández, J. I.Haldemann, J.Harutyunyan, A.Haywood, Raphaëlle D.Latham, David W.Lavie, B.Lo Curto, G.Maldonado, J.Manescau, A.Martins, C. J. A. P.Mayor, M.Mégevand, D.Mehner, A.Micela, G.Molaro, P.Molinari, E.Nunes, N. J.Pepe, F. A.Palle, E.Phillips, DavidPiotto, G.Pinamonti, M.Poretti, E.Riva, M.Rebolo, R.Santos, N. C.Sasselov, DimitarSozzetti, A.Suárez Mascareño, A.Udry, S.West, R. G.Watson, C. A.Wilson, T. G.DOI: info:10.1093/mnras/staa3144v. 4995004–5021
Mortier, A., Zapatero Osorio, M. R., Malavolta, L., Alibert, Y., Rice, K., Lillo-Box, J., Vanderburg, A., Oshagh, M., Buchhave, L., Adibekyan, V., Delgado Mena, E., Lopez-Morales, Mercedes, Charbonneau, David, Sousa, S. G., Lovis, C., Affer, L., Allende Prieto, C., Barros, S. C. C., Benatti, S., Bonomo, A. S., Boschin, W., Bouchy, F., Cabral, A., Collier Cameron, A., Cosentino, R. et al. 2020. "K2-111: an old system with two planets in near-resonance." Monthly Notices of the Royal Astronomical Society 499:5004– 5021.
ID: 158737
Type: article
Authors: Mortier, A.; Zapatero Osorio, M. R.; Malavolta, L.; Alibert, Y.; Rice, K.; Lillo-Box, J.; Vanderburg, A.; Oshagh, M.; Buchhave, L.; Adibekyan, V.; Delgado Mena, E.; Lopez-Morales, Mercedes; Charbonneau, David; Sousa, S. G.; Lovis, C.; Affer, L.; Allende Prieto, C.; Barros, S. C. C.; Benatti, S.; Bonomo, A. S.; Boschin, W.; Bouchy, F.; Cabral, A.; Collier Cameron, A.; Cosentino, R.; Cristiani, S.; Demangeon, O. D. S.; Di Marcantonio, P.; D'Odorico, V.; Dumusque, X.; Ehrenreich, D.; Figueira, P.; Fiorenzano, A.; Ghedina, A.; González Hernández, J. I.; Haldemann, J.; Harutyunyan, A.; Haywood, Raphaëlle D.; Latham, David W.; Lavie, B.; Lo Curto, G.; Maldonado, J.; Manescau, A.; Martins, C. J. A. P.; Mayor, M.; Mégevand, D.; Mehner, A.; Micela, G.; Molaro, P.; Molinari, E.; Nunes, N. J.; Pepe, F. A.; Palle, E.; Phillips, David; Piotto, G.; Pinamonti, M.; Poretti, E.; Riva, M.; Rebolo, R.; Santos, N. C.; Sasselov, Dimitar; Sozzetti, A.; Suárez Mascareño, A.; Udry, S.; West, R. G.; Watson, C. A.; Wilson, T. G.
Abstract: This paper reports on the detailed characterization of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry, as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved (log g = 4.17), iron-poor ([Fe/H] = -0.46), but alpha-enhanced ([a/Fe]=0.27), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT, shows that the transiting planet, K2-111 b, orbits with a period Pb = 5.3518 ± 0.0004 d and has a planet radius of $1.82^{+0.11}_{-0.09}$ R? and a mass of $5.29^{+0.76}_{-0.77}$ M?, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111 b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111 c, with an orbital period of 15.6785 ± 0.0064 d, orbiting in near-3:1 mean motion resonance with the transiting planet, and a minimum planet mass of 11.3 ± 1.1 M?. Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters.
MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarfParviainen, H.Palle, E.Zapatero-Osorio, M. R.Montanes Rodriguez, P.Murgas, F.Narita, N.Hidalgo Soto, D.Béjar, V. J. S.Korth, J.Monelli, M.Casasayas Barris, N.Crouzet, Leon, J. P.Fukui, A.Hernandez, A.Klagyivik, P.Kusakabe, N.Luque, R.Mori, M.Nishiumi, T.Prieto-Arranz, J.Tamura, M.Watanabe, N.Burke, C.Charbonneau, DavidCollins, Karen A.Collins, K. I.Conti, D.Garcia Soto, A.Jenkins, J. S.Jenkins, J. M.Levine, A.Li, J.Rinehart, S.Seager, S.Tenenbaum, P.Ting, E. B.Vanderspek, R.Vezie, M.Winn, J. N.DOI: info:10.1051/0004-6361/201935958v. 633A28
Parviainen, H., Palle, E., Zapatero-Osorio, M. R., Montanes Rodriguez, P., Murgas, F., Narita, N., Hidalgo Soto, D., Béjar, V. J. S., Korth, J., Monelli, M., Casasayas Barris, N., Crouzet, N., de Leon, J. P., Fukui, A., Hernandez, A., Klagyivik, P., Kusakabe, N., Luque, R., Mori, M., Nishiumi, T., Prieto-Arranz, J., Tamura, M., Watanabe, N., Burke, C., Charbonneau, David et al. 2020. "MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf." Astronomy and Astrophysics 633:A28.
ID: 155682
Type: article
Authors: Parviainen, H.; Palle, E.; Zapatero-Osorio, M. R.; Montanes Rodriguez, P.; Murgas, F.; Narita, N.; Hidalgo Soto, D.; Béjar, V. J. S.; Korth, J.; Monelli, M.; Casasayas Barris, N.; Crouzet, N.; de Leon, J. P.; Fukui, A.; Hernandez, A.; Klagyivik, P.; Kusakabe, N.; Luque, R.; Mori, M.; Nishiumi, T.; Prieto-Arranz, J.; Tamura, M.; Watanabe, N.; Burke, C.; Charbonneau, David; Collins, Karen A.; Collins, K. I.; Conti, D.; Garcia Soto, A.; Jenkins, J. S.; Jenkins, J. M.; Levine, A.; Li, J.; Rinehart, S.; Seager, S.; Tenenbaum, P.; Ting, E. B.; Vanderspek, R.; Vezie, M.; Winn, J. N.
Abstract: Context. We report the discovery of TOI 263.01 (TIC 120916706), a transiting substellar object (R = 0.87 RJup) orbiting a faint M3.5 V dwarf (V = 18.97) on a 0.56 d orbit. Aims: We setout to determine the nature of the Transiting Exoplanet Survey Satellite (TESS) planet candidate TOI 263.01 using ground-based multicolour transit photometry. The host star is faint, which makes radial-velocity confirmation challenging, but the large transit depth makes the candidate suitable for validation through multicolour photometry. Methods: Our analysis combines three transits observed simultaneously in r', i', and zs bands usingthe MuSCAT2 multicolour imager, three LCOGT-observed transit light curves in g', r', and i' bands, a TESS light curve from Sector 3, and a low-resolution spectrum for stellar characterisation observed with the ALFOSC spectrograph. We modelled the light curves with PYTRANSIT using a transit model that includes a physics-based light contamination component, allowing us to estimate the contamination from unresolved sources from the multicolour photometry. Using this information we were able to derive the true planet-star radius ratio marginalised over the contamination allowed by the photometry.Combining this with the stellar radius, we were able to make a reliable estimate of the absolute radius of the object. Results: The ground-based photometry strongly excludes contamination from unresolved sources with a significant colour difference to TOI 263. Furthermore, contamination from sources of the same stellar type as the host is constrained to levels where the true radius ratio posterior has a median of 0.217 and a 99 percentile of0.286. The median and maximum radius ratios correspond to absolute planet radii of 0.87 and 1.41 RJup, respectively,which confirms the substellar nature of the planet candidate. The object is either a giant planetor a brown dwarf (BD) located deep inside the so-called "brown dwarf desert". Both possibilities offer a challenge to current planet/BD formation models and make TOI 263.01 an object that merits in-depth follow-up studies.
The First Habitable-zone Earth-sized Planet from TESS. II. Spitzer Confirms TOI-700 dRodriguez, Joseph E.Vanderburg, AndrewZieba, SebastianKreidberg, LauraMorley, Caroline V.Eastman, Jason D.Kane, Stephen R.Spencer, AltonQuinn, Samuel N.Cloutier, RyanHuang, Chelsea X.Collins, Karen A.Mann, Andrew W.Gilbert, EmilySchlieder, Joshua E.Quintana, Elisa V.Barclay, ThomasSuissa, GabrielleKopparapu, Ravi KumarDressing, Courtney D.Ricker, George R.Vanderspek, Roland K.Latham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Berta-Thompson, ZachoryBoyd, Patricia T.Charbonneau, DavidCaldwell, Douglas A.Chiang, EugeneChristiansen, Jessie L.Ciardi, David R.Colón, Knicole D.Doty, JohnGan, TianjunGuerrero, NataliaGünther, Maximilian N.Lee, Eve J.Levine, Alan M.Lopez, EricMuirhead, Philip S.Newton, ElisabethRose, Mark E.Twicken, Joseph D.Villaseñor, Jesus NoelDOI: info:10.3847/1538-3881/aba4b3v. 160117
Rodriguez, Joseph E., Vanderburg, Andrew, Zieba, Sebastian, Kreidberg, Laura, Morley, Caroline V., Eastman, Jason D., Kane, Stephen R., Spencer, Alton, Quinn, Samuel N., Cloutier, Ryan, Huang, Chelsea X., Collins, Karen A., Mann, Andrew W., Gilbert, Emily, Schlieder, Joshua E., Quintana, Elisa V., Barclay, Thomas, Suissa, Gabrielle, Kopparapu, Ravi Kumar, Dressing, Courtney D., Ricker, George R., Vanderspek, Roland K., Latham, David W., Seager, Sara, Winn, Joshua N. et al. 2020. "The First Habitable-zone Earth-sized Planet from TESS. II. Spitzer Confirms TOI-700 d." The Astronomical Journal 160:117.
ID: 157583
Type: article
Authors: Rodriguez, Joseph E.; Vanderburg, Andrew; Zieba, Sebastian; Kreidberg, Laura; Morley, Caroline V.; Eastman, Jason D.; Kane, Stephen R.; Spencer, Alton; Quinn, Samuel N.; Cloutier, Ryan; Huang, Chelsea X.; Collins, Karen A.; Mann, Andrew W.; Gilbert, Emily; Schlieder, Joshua E.; Quintana, Elisa V.; Barclay, Thomas; Suissa, Gabrielle; Kopparapu, Ravi Kumar; Dressing, Courtney D.; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Berta-Thompson, Zachory; Boyd, Patricia T.; Charbonneau, David; Caldwell, Douglas A.; Chiang, Eugene; Christiansen, Jessie L.; Ciardi, David R.; Colón, Knicole D.; Doty, John; Gan, Tianjun; Guerrero, Natalia; Günther, Maximilian N.; Lee, Eve J.; Levine, Alan M.; Lopez, Eric; Muirhead, Philip S.; Newton, Elisabeth; Rose, Mark E.; Twicken, Joseph D.; Villaseñor, Jesus Noel
Abstract: We present Spitzer 4.5 μm observations of the transit of TOI-700 d, a habitable-zone Earth-sized planet in a multiplanet system transiting a nearby M-dwarf star (TIC 150428135, 2MASS J06282325-6534456). TOI-700 d has a radius of ${1.144}_{-0.061}^{+0.062}{R}_{\oplus }$ and orbits within its host star's conservative habitable zone with a period of 37.42 days (Teq ∼ 269 K). TOI-700 also hosts two small inner planets (Rb = ${1.037}_{-0.064}^{+0.065}{R}_{\oplus }$ and Rc = ${2.65}_{-0.15}^{+0.16}{R}_{\oplus }$ ) with periods of 9.98 and 16.05 days, respectively. Our Spitzer observations confirm the Transiting Exoplanet Survey Satellite (TESS) detection of TOI-700 d and remove any remaining doubt that it is a genuine planet. We analyze the Spitzer light curve combined with the 11 sectors of TESS observations and a transit of TOI-700 c from the LCOGT network to determine the full system parameters. Although studying the atmosphere of TOI-700 d is not likely feasible with upcoming facilities, it may be possible to measure the mass of TOI-700 d using state-of-the-art radial velocity (RV) instruments (expected RV semiamplitude of ∼70 cm s-1).
GJ 1252 b: A 1.2 R⊕ Planet Transiting an M3 Dwarf at 20.4 pcShporer, AviCollins, Karen A.Astudillo-Defru, NicolaIrwin, JonathanBonfils, XavierCollins, Kevin I.Matthews, ElisabethWinters, Jennifer G.Anderson, David R.Armstrong, James D.Charbonneau, DavidCloutier, RyanDaylan, TansuGan, TianjunGünther, Maximilian N.Hellier, CoelHorne, KeithHuang, Chelsea X.Jensen, Eric L. N.Kielkopf, JohnPalle, EnricSefako, RamotholoStassun, Keivan G.Tan, Thiam-GuanVanderburg, AndrewRicker, George R.Latham, David W.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Colon, KnicoleDressing, Courtney D.Léepine, SébastienMuirhead, Philip S.Rose, Mark E.Twicken, Joseph D.Villasenor, Jesus NoelDOI: info:10.3847/2041-8213/ab7020v. 890L7
Shporer, Avi, Collins, Karen A., Astudillo-Defru, Nicola, Irwin, Jonathan, Bonfils, Xavier, Collins, Kevin I., Matthews, Elisabeth, Winters, Jennifer G., Anderson, David R., Armstrong, James D., Charbonneau, David, Cloutier, Ryan, Daylan, Tansu, Gan, Tianjun, Günther, Maximilian N., Hellier, Coel, Horne, Keith, Huang, Chelsea X., Jensen, Eric L. N., Kielkopf, John, Palle, Enric, Sefako, Ramotholo, Stassun, Keivan G., Tan, Thiam-Guan, Vanderburg, Andrew et al. 2020. "GJ 1252 b: A 1.2 R Planet Transiting an M3 Dwarf at 20.4 pc." The Astrophysical Journal 890:L7.
ID: 156226
Type: article
Authors: Shporer, Avi; Collins, Karen A.; Astudillo-Defru, Nicola; Irwin, Jonathan; Bonfils, Xavier; Collins, Kevin I.; Matthews, Elisabeth; Winters, Jennifer G.; Anderson, David R.; Armstrong, James D.; Charbonneau, David; Cloutier, Ryan; Daylan, Tansu; Gan, Tianjun; Günther, Maximilian N.; Hellier, Coel; Horne, Keith; Huang, Chelsea X.; Jensen, Eric L. N.; Kielkopf, John; Palle, Enric; Sefako, Ramotholo; Stassun, Keivan G.; Tan, Thiam-Guan; Vanderburg, Andrew; Ricker, George R.; Latham, David W.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Colon, Knicole; Dressing, Courtney D.; Léepine, Sébastien; Muirhead, Philip S.; Rose, Mark E.; Twicken, Joseph D.; Villasenor, Jesus Noel
Abstract: We report the discovery of GJ 1252 b, a planet with a radius of 1.193 ± 0.074 ${R}_{\oplus }$ and an orbital period of 0.52 days around an M3-type star (0.381 ± 0.019 ${M}_{\odot }$ , 0.391 ± 0.020 ${R}_{\odot }$ ) located 20.385 ± 0.019 pc away. We use Transiting Exoplanet Survey Satellite (TESS) data, ground-based photometry and spectroscopy, Gaia astrometry, and high angular resolution imaging to show that the transit signal seen in the TESS data must originate from a transiting planet. We do so by ruling out all false-positive scenarios that attempt to explain the transit signal as originating from an eclipsing stellar binary. Precise Doppler monitoring also leads to a tentative mass measurement of 2.09 ± 0.56 M. The host star proximity, brightness (V = 12.19 mag, K = 7.92 mag), low stellar activity, and the system's short orbital period make this planet an attractive target for detailed characterization, including precise mass measurement, looking for other objects in the system, and planet atmosphere characterization.
Zodiacal Exoplanets in Time (ZEIT). IX. A Flat Transmission Spectrum and a Highly Eccentric Orbit for the Young Neptune K2-25b as Revealed by SpitzerThao, Pa ChiaMann, Andrew W.Johnson, Marshall C.Newton, Elisabeth R.Guo, XueyingKain, Isabel J.Rizzuto, Aaron C.Charbonneau, DavidDalba, Paul A.Gaidos, EricIrwin, Jonathan M.Kraus, Adam L.DOI: info:10.3847/1538-3881/ab579bv. 15932
Thao, Pa Chia, Mann, Andrew W., Johnson, Marshall C., Newton, Elisabeth R., Guo, Xueying, Kain, Isabel J., Rizzuto, Aaron C., Charbonneau, David, Dalba, Paul A., Gaidos, Eric, Irwin, Jonathan M., and Kraus, Adam L. 2020. "Zodiacal Exoplanets in Time (ZEIT). IX. A Flat Transmission Spectrum and a Highly Eccentric Orbit for the Young Neptune K2-25b as Revealed by Spitzer." The Astronomical Journal 159:32.
ID: 155696
Type: article
Authors: Thao, Pa Chia; Mann, Andrew W.; Johnson, Marshall C.; Newton, Elisabeth R.; Guo, Xueying; Kain, Isabel J.; Rizzuto, Aaron C.; Charbonneau, David; Dalba, Paul A.; Gaidos, Eric; Irwin, Jonathan M.; Kraus, Adam L.
Abstract: Transiting planets in nearby young clusters offer the opportunity to study the atmospheres and dynamics of planets during their formative years. To this end, we focused on K2-25b-a close-in (P = 3.48 days), Neptune-sized exoplanet orbiting a M4.5 dwarf in the 650 Myr Hyades cluster. We combined photometric observations of K2-25 covering a total of 44 transits and spanning >2 yr, drawn from a mix of space-based telescopes (Spitzer Space Telescope and K2) and ground-based facilities (Las Cumbres Observatory Global Telescope network and MEarth). The transit photometry spanned 0.6─4.5 μm, which enabled our study of K2-25b's transmission spectrum. We combined and fit each data set at a common wavelength within a Markov Chain Monte Carlo framework, yielding consistent planet parameters. The resulting transit depths ruled out a solar-composition atmosphere for K2-25b for the range of expected planetary masses and equilibrium temperature at a >4σ confidence level, and are consistent with a flat transmission spectrum. Mass constraints and transit observations at a finer grid of wavelengths (e.g., from the Hubble Space Telescope) are needed to make more definitive statements about the presence of clouds or an atmosphere of high mean molecular weight. Our precise measurements of K2-25b's transit duration also enabled new constraints on the eccentricity of K2-25's orbit. We find K2-25b's orbit to be eccentric (e > 0.20) for all reasonable stellar densities and independent of the observation wavelength or instrument. The high eccentricity is suggestive of a complex dynamical history and motivates future searches for additional planets or stellar companions.
The spectral impact of magnetic activity on disc-integrated HARPS-N solar observations: exploring new activity indicatorsThompson, A. P. G.Watson, C. A.Haywood, Raphaëlle D.Costes, J. Mooij, E.Collier Cameron, A.Dumusque, X.Phillips, David F.Saar, Steven H.Mortier, A.Milbourne, T. W.Aigrain, S.Cegla, H. M.Charbonneau, DavidCosentino, R.Ghedina, A.Latham, David W.López-Morales, M.Micela, G.Molinari, E.Poretti, E.Sozzetti, A.Thompson, S.Walsworth, Ronald L.DOI: info:10.1093/mnras/staa1010v. 4944279–4290
Thompson, A. P. G., Watson, C. A., Haywood, Raphaëlle D., Costes, J. C., de Mooij, E., Collier Cameron, A., Dumusque, X., Phillips, David F., Saar, Steven H., Mortier, A., Milbourne, T. W., Aigrain, S., Cegla, H. M., Charbonneau, David, Cosentino, R., Ghedina, A., Latham, David W., López-Morales, M., Micela, G., Molinari, E., Poretti, E., Sozzetti, A., Thompson, S., and Walsworth, Ronald L. 2020. "The spectral impact of magnetic activity on disc-integrated HARPS-N solar observations: exploring new activity indicators." Monthly Notices of the Royal Astronomical Society 494:4279– 4290.
ID: 157129
Type: article
Authors: Thompson, A. P. G.; Watson, C. A.; Haywood, Raphaëlle D.; Costes, J. C.; de Mooij, E.; Collier Cameron, A.; Dumusque, X.; Phillips, David F.; Saar, Steven H.; Mortier, A.; Milbourne, T. W.; Aigrain, S.; Cegla, H. M.; Charbonneau, David; Cosentino, R.; Ghedina, A.; Latham, David W.; López-Morales, M.; Micela, G.; Molinari, E.; Poretti, E.; Sozzetti, A.; Thompson, S.; Walsworth, Ronald L.
Abstract: Stellar activity is the major roadblock on the path to finding true Earth-analogue planets with the Doppler technique. Thus, identifying new indicators that better trace magnetic activity (I.e. faculae and spots) is crucial to aid in disentangling these signals from that of a planet's Doppler wobble. In this work, we investigate activity related features as seen in disc-integrated spectra from the HARPS-N solar telescope. We divide high-activity spectral echelle orders by low-activity master templates (as defined using both $\log {R^{\prime }_{HK}}$ and images from the Solar Dynamics Observatory, SDO), creating 'relative spectra'. With resolved images of the surface of the Sun (via SDO), the faculae and spot filling factors can be calculated, giving a measure of activity independent of, and in addition to, $\log {R^{\prime }_{HK}}$ . We find pseudo-emission (and pseudo-absorption) features in the relative spectra that are similar to those reported in our previous work on α Cen B. In α Cen B, the features are shown to correlate better to changes in faculae filling factor than spot filling factor. In this work, we more confidently identify changes in faculae coverage of the visible hemisphere of the Sun as the source of features produced in the relative spectra. Finally, we produce trailed spectra to observe the radial velocity component of the features, which show that the features move in a redward direction as one would expect when tracking active regions rotating on the surface of a star.
Spectroscopic Orbits of 11 Nearby, Mid-to-late M-dwarf BinariesWinters, Jennifer G.Irwin, Jonathan M.Charbonneau, DavidLatham, David W.Medina, Amber M.Mink, JessicaEsquerdo, Gilbert A.Berlind, PerryCalkins, Michael L.Berta-Thompson, Zachory K.DOI: info:10.3847/1538-3881/ab8d31v. 159290
Winters, Jennifer G., Irwin, Jonathan M., Charbonneau, David, Latham, David W., Medina, Amber M., Mink, Jessica, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., and Berta-Thompson, Zachory K. 2020. "Spectroscopic Orbits of 11 Nearby, Mid-to-late M-dwarf Binaries." The Astronomical Journal 159:290.
ID: 156878
Type: article
Authors: Winters, Jennifer G.; Irwin, Jonathan M.; Charbonneau, David; Latham, David W.; Medina, Amber M.; Mink, Jessica; Esquerdo, Gilbert A.; Berlind, Perry; Calkins, Michael L.; Berta-Thompson, Zachory K.
Abstract: We present the spectroscopic orbits of 11 nearby, mid-to-late M dwarf binary systems in a variety of configurations: 2 single-lined binaries (SB1s), 7 double-lined binaries (SB2s), 1 double-lined triple (ST2), and 1 triple-lined triple (ST3). Eight of these orbits are the first published for these systems, while five are newly identified multiples. We obtained multi-epoch, high-resolution spectra with the TRES instrument on the 1.5 m Tillinghast Reflector at the Fred Lawrence Whipple Observatory located on Mt. Hopkins in AZ. Using the TiO molecular bands at 7065-7165 Å, we calculated radial velocities for these systems, from which we derived their orbits. We find LHS 1817 to have in a 7 hr period a companion that is likely a white dwarf, due to the ellipsoidal modulation we see in our MEarth-North light-curve data. We find G 123-45 and LTT 11586 to host companions with minimum masses of 41 MJup and 44 MJup with orbital periods of 35 and 15 days, respectively. We find 2MA 0930+0227 to have a rapidly rotating stellar companion in a 917 day orbital period. GJ 268, GJ 1029, LP 734-34, GJ 1182, G 258-17, and LTT 7077are SB2s with stellar companions with orbital periods of 10, 96, 34, 154, 5, and 84 days; LP 655-43 is an ST3 with one companion in an 18 day orbital period and an outer component in a longer undetermined period. In addition, we present radial velocities for both components of L 870-44AB and for the outer components of LTT 11586 and LP 655-43.