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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.
Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey. I. Confirmation of an Eccentric, Cool Jupiter with an Interior Earth-sized Planet Orbiting Kepler-1514Dalba, Paul A.Kane, Stephen R.Isaacson, HowardGiacalone, StevenHoward, Andrew W.Rodriguez, Joseph E.Vanderburg, AndrewEastman, Jason D.Kraus, Adam L.Dupuy, Trent J.Weiss, Lauren M.Schwieterman, Edward W.DOI: info:10.3847/1538-3881/abd408v. 161103
Dalba, Paul A., Kane, Stephen R., Isaacson, Howard, Giacalone, Steven, Howard, Andrew W., Rodriguez, Joseph E., Vanderburg, Andrew, Eastman, Jason D., Kraus, Adam L., Dupuy, Trent J., Weiss, Lauren M., and Schwieterman, Edward W. 2021. "Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey. I. Confirmation of an Eccentric, Cool Jupiter with an Interior Earth-sized Planet Orbiting Kepler-1514." The Astronomical Journal 161:103.
ID: 159325
Type: article
Authors: Dalba, Paul A.; Kane, Stephen R.; Isaacson, Howard; Giacalone, Steven; Howard, Andrew W.; Rodriguez, Joseph E.; Vanderburg, Andrew; Eastman, Jason D.; Kraus, Adam L.; Dupuy, Trent J.; Weiss, Lauren M.; Schwieterman, Edward W.
Abstract: Despite the severe bias of the transit method of exoplanet discovery toward short orbital periods, a modest sample of transiting exoplanets with orbital periods greater than 100 days is known. Long-term radial velocity (RV) surveys are pivotal to confirming these signals and generating a set of planetary masses and densities for planets receiving moderate to low irradiation from their host stars. Here we conduct RV observations of Kepler-1514 from the Keck I telescope using the High Resolution Echelle Spectrometer. From these data, we measure the mass of the statistically validated giant (1.108 ± 0.023 RJ) exoplanet Kepler-1514 b with a 218-day orbital period as 5.28 ± 0.22 MJ. The bulk density of this cool (∼390 K) giant planet is ${4.82}_{-0.25}^{+0.26}$ g cm-3, consistent with a core supported by electron degeneracy pressure. We also infer an orbital eccentricity of ${0.401}_{-0.014}^{+0.013}$ from the RV and transit observations, which is consistent with planet-planet scattering and disk cavity migration models. The Kepler-1514 system contains an Earth-size, Kepler Object of Interest on a 10.5-day orbit that we statistically validate against false-positive scenarios, including those involving a neighboring star. The combination of the brightness (V = 11.8) of the host star and the long period, low irradiation, and high density of Kepler-1514 b places this system among a rare group of known exoplanetary systems and as one that is amenable to continued study. * Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
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.
Two Planets Straddling the Habitable Zone of the Nearby K Dwarf Gl 414ADedrick, Cayla M.Fulton, Benjamin J.Knutson, Heather A.Howard, Andrew W.Beatty, Thomas G.Cargile, Phillip A.Gaudi, B. ScottHirsch, Lea A.Kuhn, Rudolf B.Lund, Michael B.James, David J.Kosiarek, Molly R.Pepper, JoshuaPetigura, Erik A.Rodriguez, Joseph E.Stassun, Keivan G.Stevens, Daniel J.DOI: info:10.3847/1538-3881/abd0efv. 16186
Dedrick, Cayla M., Fulton, Benjamin J., Knutson, Heather A., Howard, Andrew W., Beatty, Thomas G., Cargile, Phillip A., Gaudi, B. Scott, Hirsch, Lea A., Kuhn, Rudolf B., Lund, Michael B., James, David J., Kosiarek, Molly R., Pepper, Joshua, Petigura, Erik A., Rodriguez, Joseph E., Stassun, Keivan G., and Stevens, Daniel J. 2021. "Two Planets Straddling the Habitable Zone of the Nearby K Dwarf Gl 414A." The Astronomical Journal 161:86.
ID: 159335
Type: article
Authors: Dedrick, Cayla M.; Fulton, Benjamin J.; Knutson, Heather A.; Howard, Andrew W.; Beatty, Thomas G.; Cargile, Phillip A.; Gaudi, B. Scott; Hirsch, Lea A.; Kuhn, Rudolf B.; Lund, Michael B.; James, David J.; Kosiarek, Molly R.; Pepper, Joshua; Petigura, Erik A.; Rodriguez, Joseph E.; Stassun, Keivan G.; Stevens, Daniel J.
Abstract: We present the discovery of two planets orbiting the nearby (D = 11.9 pc) K7 dwarf Gl 414A. Gl 414A b is a sub-Neptune mass planet with ${M}_{b}\sin {i}_{b}={7.60}_{-2.19}^{+2.44}$ M and a semimajor axis of 0.23 ± 0.01 au. Gl 414A c is a sub-Saturn mass planet with ${M}_{c}\sin {i}_{c}={53.83}_{-8.58}^{+9.18}$ M and a semimajor axis of 1.43 ± 0.06 au. We jointly analyzed radial velocity data from Keck/HIRES and the Automated Planet Finder at Lick Observatory, as well as photometric data from KELT, to detect the two planets and two additional signals related to the rotationally modulated activity and the long-term magnetic activity cycle of the star. The outer planet in this system may be a potential candidate for future direct-imaging missions.
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.
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.
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.
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.
Following up TESS Single Transits with Archival Photometry and Radial VelocitiesYao, XinyuPepper, JoshuaGaudi, B. ScottDalba, Paul A.Burt, Jennifer A.Wittenmyer, Robert A.Dragomir, DianaRodriguez, Joseph E.Villanueva, Steven, Jr.Stevens, Daniel J.Stassun, Keivan G.James, David J.DOI: info:10.3847/1538-3881/abdb30v. 161124
Yao, Xinyu, Pepper, Joshua, Gaudi, B. Scott, Dalba, Paul A., Burt, Jennifer A., Wittenmyer, Robert A., Dragomir, Diana, Rodriguez, Joseph E., Villanueva, Steven, Jr., Stevens, Daniel J., Stassun, Keivan G., and James, David J. 2021. "Following up TESS Single Transits with Archival Photometry and Radial Velocities." The Astronomical Journal 161:124.
ID: 159328
Type: article
Authors: Yao, Xinyu; Pepper, Joshua; Gaudi, B. Scott; Dalba, Paul A.; Burt, Jennifer A.; Wittenmyer, Robert A.; Dragomir, Diana; Rodriguez, Joseph E.; Villanueva, Steven, Jr.; Stevens, Daniel J.; Stassun, Keivan G.; James, David J.
Abstract: NASA's Transiting Exoplanet Survey Satellite (TESS) mission is expected to discover hundreds of planets via single transits first identified in their light curves. Determining the orbital period of these single-transit candidates typically requires a significant amount of follow-up work to observe a second transit or measure a radial velocity (RV) orbit. In Yao et al., we developed simulations that demonstrated the ability to use archival photometric data in combination with TESS to "precover" the orbital period for these candidates with a precision of several minutes, assuming circular orbits. In this work, we incorporate updated models for TESS single transits, allowing for eccentric orbits, along with an updated methodology to improve the reliability of the results. Additionally, we explore how RV observations can be used to follow up single-transit events, using strategies distinct from those employed when the orbital period is known. We find that the use of an estimated period based on a circular orbit to schedule reconnaissance RV observations can efficiently distinguish eclipsing binaries from planets. For candidates that pass reconnaissance RV observations, we simulate RV monitoring campaigns that enable one to obtain an approximate orbital solution. We find that this method can regularly determine the orbital periods for planets more massive than 0.5 MJ with orbital periods as long as 100 days.
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.
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.
Long-period High-amplitude Red Variables in the KELT SurveyArnold, R. AlexMcSwain, M. VirginiaPepper, JoshuaWhitelock, Patricia A.Hernitschek, NinaJames, David J.Kuhn, Rudolf B.Lund, Michael B.Rodriguez, Joseph E.Siverd, Robert J.Stassun, Keivan G.DOI: info:10.3847/1538-4365/ab6bdbv. 24744
Arnold, R. Alex, McSwain, M. Virginia, Pepper, Joshua, Whitelock, Patricia A., Hernitschek, Nina, James, David J., Kuhn, Rudolf B., Lund, Michael B., Rodriguez, Joseph E., Siverd, Robert J., and Stassun, Keivan G. 2020. "Long-period High-amplitude Red Variables in the KELT Survey." The Astrophysical Journal Supplement Series 247:44.
ID: 156294
Type: article
Authors: Arnold, R. Alex; McSwain, M. Virginia; Pepper, Joshua; Whitelock, Patricia A.; Hernitschek, Nina; James, David J.; Kuhn, Rudolf B.; Lund, Michael B.; Rodriguez, Joseph E.; Siverd, Robert J.; Stassun, Keivan G.
Abstract: We present a sample of 4132 Mira-like variables (red variables with long periods and high amplitudes) in the Kilodegree Extremely Little Telescope (KELT) survey. Of these, 376 are new Mira-like detections. We used Two Micron All Sky Survey (2MASS) colors to identify candidate asymptotic giant branch stars. We searched for photometric variability among the candidate asymptotic giant branch stars and identified stars that show periodic variability. We selected variables with high amplitudes and strong periodic behavior using a Random Forest classifier. Of the sample of 4132 Mira-like variables, we estimate that 70% are Miras and 30% are semiregular (SR) variables. We also adopt the method of using (WRP-WK_s) versus (J-{Ks) colors in distinguishing between O-rich and C-rich Miras and find it to be an improvement over 2MASS colors.
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.
TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune DesertBurt, Jennifer A.Nielsen, Louise D.Quinn, Samuel N.Mamajek, Eric E.Matthews, Elisabeth C.Zhou, GeorgeSeidel, Julia V.Huang, Chelsea X.Lopez, EricSoto, MaritzaOtegi, JonStassun, Keivan G.Kreidberg, LauraCollins, Karen A.Eastman, Jason D.Rodriguez, Joseph E.Vanderburg, AndrewHalverson, Samuel P.Teske, Johanna K.Wang, Sharon X.Butler, R. PaulBouchy, FrançoisDumusque, XavierSegransen, DamienShectman, Stephen A.Crane, Jeffrey D.Feng, FaboMontet, Benjamin T.Feinstein, Adina D.Beletski, YuriFlowers, ErinGünther, Maximilian N.Daylan, TansuCollins, Kevin I.Conti, Dennis M.Gan, TianjunJensen, Eric L. N.Kielkopf, John F.Tan, Thiam-GuanHelled, RavitDorn, CarolineHaldemann, JonasLissauer, Jack J.Ricker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.Twicken, Joseph D.Smith, Jeffrey C.Tenenbaum, PeterCartwright, ScottBarclay, ThomasPepper, JoshuaEsquerdo, GilbertFong, WilliamDOI: info:10.3847/1538-3881/abac0cv. 160153
Burt, Jennifer A., Nielsen, Louise D., Quinn, Samuel N., Mamajek, Eric E., Matthews, Elisabeth C., Zhou, George, Seidel, Julia V., Huang, Chelsea X., Lopez, Eric, Soto, Maritza, Otegi, Jon, Stassun, Keivan G., Kreidberg, Laura, Collins, Karen A., Eastman, Jason D., Rodriguez, Joseph E., Vanderburg, Andrew, Halverson, Samuel P., Teske, Johanna K., Wang, Sharon X., Butler, R. Paul, Bouchy, François, Dumusque, Xavier, Segransen, Damien, Shectman, Stephen A. et al. 2020. "TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert." The Astronomical Journal 160:153.
ID: 157601
Type: article
Authors: Burt, Jennifer A.; Nielsen, Louise D.; Quinn, Samuel N.; Mamajek, Eric E.; Matthews, Elisabeth C.; Zhou, George; Seidel, Julia V.; Huang, Chelsea X.; Lopez, Eric; Soto, Maritza; Otegi, Jon; Stassun, Keivan G.; Kreidberg, Laura; Collins, Karen A.; Eastman, Jason D.; Rodriguez, Joseph E.; Vanderburg, Andrew; Halverson, Samuel P.; Teske, Johanna K.; Wang, Sharon X.; Butler, R. Paul; Bouchy, François; Dumusque, Xavier; Segransen, Damien; Shectman, Stephen A.; Crane, Jeffrey D.; Feng, Fabo; Montet, Benjamin T.; Feinstein, Adina D.; Beletski, Yuri; Flowers, Erin; Günther, Maximilian N.; Daylan, Tansu; Collins, Kevin I.; Conti, Dennis M.; Gan, Tianjun; Jensen, Eric L. N.; Kielkopf, John F.; Tan, Thiam-Guan; Helled, Ravit; Dorn, Caroline; Haldemann, Jonas; Lissauer, Jack J.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Twicken, Joseph D.; Smith, Jeffrey C.; Tenenbaum, Peter; Cartwright, Scott; Barclay, Thomas; Pepper, Joshua; Esquerdo, Gilbert; Fong, William
Abstract: We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the Transiting Exoplanet Survey Satellite. The newly discovered planet has a radius Rp = 2.93 ± 0.20 ${R}_{\oplus }$ and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph and the High Accuracy Radial velocity Planet Searcher spectrograph confirm the existence of the planet, and we estimate its mass to be 18.47 ± 1.84 ${M}_{\oplus }$ . The planet's mean density is ${\rho }_{{\rm{p}}}$ = 4.03 ${}_{-0.78}^{+0.98}$ ${\rm{g}}\,{\mathrm{cm}}^{-3}$ , making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud-free atmosphere, and thus it is an excellent candidate for follow-up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated small planet at the edge of the hot Neptune desert that has retained its atmosphere to date.
Two Intermediate-mass Transiting Brown Dwarfs from the TESS MissionCarmichael, Theron W.Quinn, Samuel N.Mustill, Alexander J.Huang, ChelseaZhou, GeorgePersson, Carina M.Nielsen, Louise D.Collins, Karen A.Ziegler, CarlCollins, Kevin I.Rodriguez, Joseph E.Shporer, AviBrahm, RafaelMann, Andrew W.Bouchy, FrancoisFridlund, MalcolmStassun, Keivan G.Hellier, CoelSeidel, Julia V.Stalport, ManuUdry, StephanePepe, FrancescoIreland, MichaelŽerjal, MarušaBriceño, CésarLaw, NicholasJordán, AndrésEspinoza, NéstorHenning, ThomasSarkis, PaulaLatham, David W.DOI: info:10.3847/1538-3881/ab9b84v. 16053
Carmichael, Theron W., Quinn, Samuel N., Mustill, Alexander J., Huang, Chelsea, Zhou, George, Persson, Carina M., Nielsen, Louise D., Collins, Karen A., Ziegler, Carl, Collins, Kevin I., Rodriguez, Joseph E., Shporer, Avi, Brahm, Rafael, Mann, Andrew W., Bouchy, Francois, Fridlund, Malcolm, Stassun, Keivan G., Hellier, Coel, Seidel, Julia V., Stalport, Manu, Udry, Stephane, Pepe, Francesco, Ireland, Michael, Žerjal, Maruša, Briceño, César et al. 2020. "Two Intermediate-mass Transiting Brown Dwarfs from the TESS Mission." The Astronomical Journal 160:53.
ID: 157619
Type: article
Authors: Carmichael, Theron W.; Quinn, Samuel N.; Mustill, Alexander J.; Huang, Chelsea; Zhou, George; Persson, Carina M.; Nielsen, Louise D.; Collins, Karen A.; Ziegler, Carl; Collins, Kevin I.; Rodriguez, Joseph E.; Shporer, Avi; Brahm, Rafael; Mann, Andrew W.; Bouchy, Francois; Fridlund, Malcolm; Stassun, Keivan G.; Hellier, Coel; Seidel, Julia V.; Stalport, Manu; Udry, Stephane; Pepe, Francesco; Ireland, Michael; Žerjal, Maruša; Briceño, César; Law, Nicholas; Jordán, Andrés; Espinoza, Néstor; Henning, Thomas; Sarkis, Paula; Latham, David W.
Abstract: We report the discovery of two intermediate-mass transiting brown dwarfs (BDs), TOI-569b and TOI-1406b, from NASA's Transiting Exoplanet Survey Satellite mission. TOI-569b has an orbital period of P = 6.55604 ± 0.00016 days, a mass of Mb = 64.1 ± 1.9 ${M}_{{\rm{J}}}$ , and a radius of Rb = 0.75 ± 0.02 ${R}_{{\rm{J}}}$ . Its host star, TOI-569, has a mass of M = 1.21 ± 0.05 $\,{M}_{\odot }$ , a radius of R = 1.47 ± 0.03 $\,{R}_{\odot }$ , $[\mathrm{Fe}/{\rm{H}}]=+0.29\pm 0.09$ dex, and an effective temperature of Teff = 5768 ± 110 K. TOI-1406b has an orbital period of P = 10.57415 ± 0.00063 days, a mass of Mb = 46.0 ± 2.7 ${M}_{{\rm{J}}}$ , and a radius of Rb = 0.86 ± 0.03 ${R}_{{\rm{J}}}$ . The host star for this BD has a mass of M = 1.18 ± 0.09 $\,{M}_{\odot }$ , a radius of R = 1.35 ± 0.03 $\,{R}_{\odot }$ , $[\mathrm{Fe}/{\rm{H}}]=-0.08\pm 0.09$ dex, and an effective temperature of Teff = 6290 ± 100 K. Both BDs are in circular orbits around their host stars and are older than 3 Gyr based on stellar isochrone models of the stars. TOI-569 is one of two slightly evolved stars known to host a transiting BD (the other being KOI-415). TOI-1406b is one of three known transiting BDs to occupy the mass range of 40-50 ${M}_{{\rm{J}}}$ and one of two to have a circular orbit at a period near 10 days (with the first being KOI-205b). Both BDs have reliable ages from stellar isochrones, in addition to their well-constrained masses and radii, making them particularly valuable as tests for substellar isochrones in the BD mass-radius diagram.
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.
An Unusual Transmission Spectrum for the Sub-Saturn KELT-11b Suggestive of a Subsolar Water AbundanceColón, Knicole D.Kreidberg, LauraWelbanks, LuisLine, Michael R.Madhusudhan, NikkuBeatty, ThomasTamburo, PatrickStevenson, Kevin B.Mandell, AviRodriguez, Joseph E.Barclay, ThomasLopez, Eric D.Stassun, Keivan G.Angerhausen, DanielFortney, Jonathan J.James, David J.Pepper, JoshuaAhlers, John P.Plavchan, PeterAwiphan, SupachaiKotnik, CliffMcLeod, Kim K.Murawski, GabrielChotani, HeenaLeBrun, DannyMatzko, WilliamRea, DavidVidaurri, MonicaWebster, ScottWilliams, James K.Cox, Leafia SheradenTan, NicoleGilbert, Emily A.DOI: info:10.3847/1538-3881/abc1e9v. 160280
Colón, Knicole D., Kreidberg, Laura, Welbanks, Luis, Line, Michael R., Madhusudhan, Nikku, Beatty, Thomas, Tamburo, Patrick, Stevenson, Kevin B., Mandell, Avi, Rodriguez, Joseph E., Barclay, Thomas, Lopez, Eric D., Stassun, Keivan G., Angerhausen, Daniel, Fortney, Jonathan J., James, David J., Pepper, Joshua, Ahlers, John P., Plavchan, Peter, Awiphan, Supachai, Kotnik, Cliff, McLeod, Kim K., Murawski, Gabriel, Chotani, Heena, LeBrun, Danny et al. 2020. "An Unusual Transmission Spectrum for the Sub-Saturn KELT-11b Suggestive of a Subsolar Water Abundance." The Astronomical Journal 160:280.
ID: 158639
Type: article
Authors: Colón, Knicole D.; Kreidberg, Laura; Welbanks, Luis; Line, Michael R.; Madhusudhan, Nikku; Beatty, Thomas; Tamburo, Patrick; Stevenson, Kevin B.; Mandell, Avi; Rodriguez, Joseph E.; Barclay, Thomas; Lopez, Eric D.; Stassun, Keivan G.; Angerhausen, Daniel; Fortney, Jonathan J.; James, David J.; Pepper, Joshua; Ahlers, John P.; Plavchan, Peter; Awiphan, Supachai; Kotnik, Cliff; McLeod, Kim K.; Murawski, Gabriel; Chotani, Heena; LeBrun, Danny; Matzko, William; Rea, David; Vidaurri, Monica; Webster, Scott; Williams, James K.; Cox, Leafia Sheraden; Tan, Nicole; Gilbert, Emily A.
Abstract: We present an optical-to-infrared transmission spectrum of the inflated sub-Saturn KELT-11b measured with the Transiting Exoplanet Survey Satellite (TESS), the Hubble Space Telescope (HST) Wide Field Camera 3 G141 spectroscopic grism, and the Spitzer Space Telescope (Spitzer) at 3.6 µm, in addition to a Spitzer 4.5 µm secondary eclipse. The precise HST transmission spectrum notably reveals a low-amplitude water feature with an unusual shape. Based on free-retrieval analyses with varying molecular abundances, we find strong evidence for water absorption. Depending on model assumptions, we also find tentative evidence for other absorbers (HCN, TiO, and AlO). The retrieved water abundance is generally ?0.1× solar (0.001-0.7× solar over a range of model assumptions), several orders of magnitude lower than expected from planet formation models based on the solar system metallicity trend. We also consider chemical-equilibrium and self-consistent 1D radiative-convective equilibrium model fits and find that they, too, prefer low metallicities ([M/H] ? -2, consistent with the free-retrieval results). However, all of the retrievals should be interpreted with some caution because they either require additional absorbers that are far out of chemical equilibrium to explain the shape of the spectrum or are simply poor fits to the data. Finally, we find that the Spitzer secondary eclipse is indicative of full heat redistribution from KELT-11b's dayside to nightside, assuming a clear dayside. These potentially unusual results for KELT-11b's composition are suggestive of new challenges on the horizon for atmosphere and formation models in the face of increasingly precise measurements of exoplanet spectra.
The TESS-Keck Survey. I. A Warm Sub-Saturn-mass Planet and a Caution about Stray Light in TESS CamerasDalba, Paul A.Gupta, Arvind F.Rodriguez, Joseph E.Dragomir, DianaHuang, Chelsea X.Kane, Stephen R.Quinn, Samuel N.Bieryla, AllysonEsquerdo, Gilbert A.Fulton, Benjamin J.Scarsdale, NicholasBatalha, Natalie M.Beard, CoreyBehmard, AidaChontos, AshleyCrossfield, Ian J. M.Dressing, Courtney D.Giacalone, StevenHill, Michelle L.Hirsch, Lea A.Howard, Andrew W.Huber, DanielIsaacson, HowardKosiarek, MollyLubin, JackMayo, Andrew W.Mocnik, TeoAkana Murphy, Joseph M.Petigura, Erik A.Robertson, PaulRosenthal, Lee J.Roy, ArpitaRubenzahl, Ryan A.Van Zandt, JudahWeiss, Lauren M.Knudstrup, EmilAndersen, Mads F.Grundahl, FrankYao, XinyuPepper, JoshuaVillanueva, Steven, Jr.Ciardi, David R.Cloutier, RyanJacobs, Thomas LeeKristiansen, Martti H.LaCourse, Daryll M.Lendl, MonikaOsborn, Hugh P.Palle, EnricStassun, Keivan G.Stevens, Daniel J.Ricker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.Caldwell, Douglas A.Daylan, TansuFong, WilliamGoeke, Robert F.Rose, Mark E.Rowden, PamelaSchlieder, Joshua E.Smith, Jeffrey C.Vanderburg, AndrewDOI: info:10.3847/1538-3881/ab84e3v. 159241
Dalba, Paul A., Gupta, Arvind F., Rodriguez, Joseph E., Dragomir, Diana, Huang, Chelsea X., Kane, Stephen R., Quinn, Samuel N., Bieryla, Allyson, Esquerdo, Gilbert A., Fulton, Benjamin J., Scarsdale, Nicholas, Batalha, Natalie M., Beard, Corey, Behmard, Aida, Chontos, Ashley, Crossfield, Ian J. M., Dressing, Courtney D., Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kosiarek, Molly, Lubin, Jack et al. 2020. "The TESS-Keck Survey. I. A Warm Sub-Saturn-mass Planet and a Caution about Stray Light in TESS Cameras." The Astronomical Journal 159:241.
ID: 156961
Type: article
Authors: Dalba, Paul A.; Gupta, Arvind F.; Rodriguez, Joseph E.; Dragomir, Diana; Huang, Chelsea X.; Kane, Stephen R.; Quinn, Samuel N.; Bieryla, Allyson; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Scarsdale, Nicholas; Batalha, Natalie M.; Beard, Corey; Behmard, Aida; Chontos, Ashley; Crossfield, Ian J. M.; Dressing, Courtney D.; Giacalone, Steven; Hill, Michelle L.; Hirsch, Lea A.; Howard, Andrew W.; Huber, Daniel; Isaacson, Howard; Kosiarek, Molly; Lubin, Jack; Mayo, Andrew W.; Mocnik, Teo; Akana Murphy, Joseph M.; Petigura, Erik A.; Robertson, Paul; Rosenthal, Lee J.; Roy, Arpita; Rubenzahl, Ryan A.; Van Zandt, Judah; Weiss, Lauren M.; Knudstrup, Emil; Andersen, Mads F.; Grundahl, Frank; Yao, Xinyu; Pepper, Joshua; Villanueva, Steven, Jr.; Ciardi, David R.; Cloutier, Ryan; Jacobs, Thomas Lee; Kristiansen, Martti H.; LaCourse, Daryll M.; Lendl, Monika; Osborn, Hugh P.; Palle, Enric; Stassun, Keivan G.; Stevens, Daniel J.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Caldwell, Douglas A.; Daylan, Tansu; Fong, William; Goeke, Robert F.; Rose, Mark E.; Rowden, Pamela; Schlieder, Joshua E.; Smith, Jeffrey C.; Vanderburg, Andrew
Abstract: We report the detection of a Saturn-size exoplanet orbiting HD 332231 (TOI 1456) in light curves from the Transiting Exoplanet Survey Satellite (TESS). HD 332231 -- an F8 dwarf star with a V-band magnitude of 8.56 -- was observed by TESS in Sectors 14 and 15. We detect a single-transit event in the Sector 15 presearch data conditioning (PDC) light curve. We obtain spectroscopic follow-up observations of HD 332231 with the Automated Planet Finder, Keck I, and SONG telescopes. The orbital period we infer from radial velocity (RV) observations leads to the discovery of another transit in Sector 14 that was masked by PDC due to scattered light contamination. A joint analysis of the transit and RV data confirms the planetary nature of HD 332231 b, a Saturn-size ( ${0.867}_{-0.025}^{+0.027}\ {R}_{{\rm{J}}} ), sub-Saturn-mass ( $0.244\pm 0.021\ {M}_{{\rm{J}}} ) exoplanet on a 18.71 day circular orbit. The low surface gravity of HD 332231 b and the relatively low stellar flux it receives make it a compelling target for transmission spectroscopy. Also, the stellar obliquity is likely measurable via the Rossiter-McLaughlin effect, an exciting prospect given the 0.14 au orbital separation of HD 332231 b. The spectroscopic observations do not provide substantial evidence for any additional planets in the HD 332231 system, but continued RV monitoring is needed to further characterize this system. We also predict that the frequency and duration of masked data in the PDC light curves for TESS Sectors 14-16 could hide transits of some exoplanets with orbital periods between 10.5 and 17.5 days.
The First Habitable-zone Earth-sized Planet from TESS. I. Validation of the TOI-700 SystemGilbert, Emily A.Barclay, ThomasSchlieder, Joshua E.Quintana, Elisa V.Hord, Benjamin J.Kostov, Veselin B.Lopez, Eric D.Rowe, Jason F.Hoffman, KelseyWalkowicz, Lucianne M.Silverstein, Michele L.Rodriguez, Joseph E.Vanderburg, AndrewSuissa, GabrielleAirapetian, Vladimir S.Clement, Matthew S.Raymond, Sean N.Mann, Andrew W.Kruse, EthanLissauer, Jack J.Colón, Knicole D.Kopparapu, Ravi KumarKreidberg, LauraZieba, SebastianCollins, Karen A.Quinn, Samuel N.Howell, Steve B.Ziegler, CarlVrijmoet, Eliot HalleyAdams, Fred C.Arney, Giada N.Boyd, Patricia T.Brande, JonathanBurke, Christopher J.Cacciapuoti, LucaChance, QuadryChristiansen, Jessie L.Covone, GiovanniDaylan, TansuDineen, DanielleDressing, Courtney D.Essack, ZahraFauchez, Thomas J.Galgano, BriannaHowe, Alex R.Kaltenegger, LisaKane, Stephen R.Lam, ChristopherLee, Eve J.Lewis, Nikole K.Logsdon, Sarah E.Mandell, Avi M.Monsue, TeresaMullally, FergalMullally, Susan E.Paudel, Rishi R.Pidhorodetska, DariaPlavchan, PeterReyes, Naylynn TañónRinehart, Stephen A.Rojas-Ayala, BárbaraSmith, Jeffrey C.Stassun, Keivan G.Tenenbaum, PeterVega, Laura D.Villanueva, Geronimo L.Wolf, Eric T.Youngblood, AllisonRicker, George R.Vanderspek, Roland K.Latham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Bakos, Gáspár Å.Briceño, CésarCiardi, David R.Cloutier, RyanConti, Dennis M.Couperus, AndrewDi Sora, MarioEisner, Nora L.Everett, Mark E.Gan, TianjunHartman, Joel D.Henry, ToddIsopi, GiovanniJao, Wei-ChunJensen, Eric L. N.Law, NicholasMallia, FrancoMatson, Rachel A.Shappee, Benjamin J.Le Wood, MackennaeWinters, Jennifer G.DOI: info:10.3847/1538-3881/aba4b2v. 160116
Gilbert, Emily A., Barclay, Thomas, Schlieder, Joshua E., Quintana, Elisa V., Hord, Benjamin J., Kostov, Veselin B., Lopez, Eric D., Rowe, Jason F., Hoffman, Kelsey, Walkowicz, Lucianne M., Silverstein, Michele L., Rodriguez, Joseph E., Vanderburg, Andrew, Suissa, Gabrielle, Airapetian, Vladimir S., Clement, Matthew S., Raymond, Sean N., Mann, Andrew W., Kruse, Ethan, Lissauer, Jack J., Colón, Knicole D., Kopparapu, Ravi Kumar, Kreidberg, Laura, Zieba, Sebastian, Collins, Karen A. et al. 2020. "The First Habitable-zone Earth-sized Planet from TESS. I. Validation of the TOI-700 System." The Astronomical Journal 160:116.
ID: 157602
Type: article
Authors: Gilbert, Emily A.; Barclay, Thomas; Schlieder, Joshua E.; Quintana, Elisa V.; Hord, Benjamin J.; Kostov, Veselin B.; Lopez, Eric D.; Rowe, Jason F.; Hoffman, Kelsey; Walkowicz, Lucianne M.; Silverstein, Michele L.; Rodriguez, Joseph E.; Vanderburg, Andrew; Suissa, Gabrielle; Airapetian, Vladimir S.; Clement, Matthew S.; Raymond, Sean N.; Mann, Andrew W.; Kruse, Ethan; Lissauer, Jack J.; Colón, Knicole D.; Kopparapu, Ravi Kumar; Kreidberg, Laura; Zieba, Sebastian; Collins, Karen A.; Quinn, Samuel N.; Howell, Steve B.; Ziegler, Carl; Vrijmoet, Eliot Halley; Adams, Fred C.; Arney, Giada N.; Boyd, Patricia T.; Brande, Jonathan; Burke, Christopher J.; Cacciapuoti, Luca; Chance, Quadry; Christiansen, Jessie L.; Covone, Giovanni; Daylan, Tansu; Dineen, Danielle; Dressing, Courtney D.; Essack, Zahra; Fauchez, Thomas J.; Galgano, Brianna; Howe, Alex R.; Kaltenegger, Lisa; Kane, Stephen R.; Lam, Christopher; Lee, Eve J.; Lewis, Nikole K.; Logsdon, Sarah E.; Mandell, Avi M.; Monsue, Teresa; Mullally, Fergal; Mullally, Susan E.; Paudel, Rishi R.; Pidhorodetska, Daria; Plavchan, Peter; Reyes, Naylynn Tañón; Rinehart, Stephen A.; Rojas-Ayala, Bárbara; Smith, Jeffrey C.; Stassun, Keivan G.; Tenenbaum, Peter; Vega, Laura D.; Villanueva, Geronimo L.; Wolf, Eric T.; Youngblood, Allison; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Bakos, Gáspár Å.; Briceño, César; Ciardi, David R.; Cloutier, Ryan; Conti, Dennis M.; Couperus, Andrew; Di Sora, Mario; Eisner, Nora L.; Everett, Mark E.; Gan, Tianjun; Hartman, Joel D.; Henry, Todd; Isopi, Giovanni; Jao, Wei-Chun; Jensen, Eric L. N.; Law, Nicholas; Mallia, Franco; Matson, Rachel A.; Shappee, Benjamin J.; Le Wood, Mackennae; Winters, Jennifer G.
Abstract: We present the discovery and validation of a three-planet system orbiting the nearby (31.1 pc) M2 dwarf star TOI-700 (TIC 150428135). TOI-700 lies in the TESS continuous viewing zone in the Southern Ecliptic Hemisphere; observations spanning 11 sectors reveal three planets with radii ranging from 1 R to 2.6 R and orbital periods ranging from 9.98 to 37.43 days. Ground-based follow-up combined with diagnostic vetting and validation tests enables us to rule out common astrophysical false-positive scenarios and validate the system of planets. The outermost planet, TOI-700 d, has a radius of 1.19 ± 0.11 R and resides within a conservative estimate of the host star's habitable zone, where it receives a flux from its star that is approximately 86% of Earth's insolation. In contrast to some other low-mass stars that host Earth-sized planets in their habitable zones, TOI-700 exhibits low levels of stellar activity, presenting a valuable opportunity to study potentially rocky planets over a wide range of conditions affecting atmospheric escape. While atmospheric characterization of TOI-700 d with the James Webb Space Telescope (JWST) will be challenging, the larger sub-Neptune, TOI-700 c (R = 2.63 R), will be an excellent target for JWST and future space-based observatories. TESS is scheduled to once again observe the Southern Hemisphere, and it will monitor TOI-700 for an additional 11 sectors in its extended mission. These observations should allow further constraints on the known planet parameters and searches for additional planets and transit timing variations in the system.
Orbital Refinement and Stellar Properties for the HD 9446, HD 43691, and HD 179079 Planetary SystemsHill, Michelle L.Močnik, TeoKane, Stephen R.Henry, Gregory W.Pepper, JoshuaHinkel, Natalie R.Dalba, Paul A.Fulton, Benjamin J.Stassun, Keivan G.Rosenthal, Lee J.Howard, Andrew W.Howell, Steve B.Everett, Mark E.Boyajian, Tabetha S.Fischer, Debra A.Rodriguez, Joseph E.Beatty, Thomas G.James, David J.DOI: info:10.3847/1538-3881/ab7d33v. 159197
Hill, Michelle L., Močnik, Teo, Kane, Stephen R., Henry, Gregory W., Pepper, Joshua, Hinkel, Natalie R., Dalba, Paul A., Fulton, Benjamin J., Stassun, Keivan G., Rosenthal, Lee J., Howard, Andrew W., Howell, Steve B., Everett, Mark E., Boyajian, Tabetha S., Fischer, Debra A., Rodriguez, Joseph E., Beatty, Thomas G., and James, David J. 2020. "Orbital Refinement and Stellar Properties for the HD 9446, HD 43691, and HD 179079 Planetary Systems." The Astronomical Journal 159:197.
ID: 156883
Type: article
Authors: Hill, Michelle L.; Močnik, Teo; Kane, Stephen R.; Henry, Gregory W.; Pepper, Joshua; Hinkel, Natalie R.; Dalba, Paul A.; Fulton, Benjamin J.; Stassun, Keivan G.; Rosenthal, Lee J.; Howard, Andrew W.; Howell, Steve B.; Everett, Mark E.; Boyajian, Tabetha S.; Fischer, Debra A.; Rodriguez, Joseph E.; Beatty, Thomas G.; James, David J.
Abstract: The Transit Ephemeris Refinement and Monitoring Survey is a project that aims to detect transits of intermediate-long period planets by refining orbital parameters of the known radial velocity planets using additional data from ground-based telescopes, calculating a revised transit ephemeris for the planet, then monitoring the planet host star during the predicted transit window. Here we present the results from three systems that had high probabilities of transiting planets: HD 9446 b and c, HD 43691 b, and HD 179079 b. We provide new radial velocity (RV) measurements that are then used to improve the orbital solution for the known planets. We search the RV data for indications of additional planets in orbit and find that HD 9446 shows a strong linear trend of 4.8σ. Using the newly refined planet orbital solutions, which include a new best-fit solution for the orbital period of HD 9446 c, and an improved transit ephemerides, we found no evidence of transiting planets in the photometry for each system. Transits of HD 9446 b can be ruled out completely and transits HD 9446 c and HD 43691 b can be ruled out for impact parameters up to b = 0.5778 and b = 0.898, respectively, due to gaps in the photometry. A transit of HD 179079 b cannot be ruled out, however, due to the relatively small size of this planet compared to the large star and thus low signal to noise. We determine properties of the three host stars through spectroscopic analysis and find through photometric analysis that HD 9446 exhibits periodic variability.
TESS Spots a Hot Jupiter with an Inner Transiting NeptuneHuang, Chelsea X.Quinn, Samuel N.Vanderburg, AndrewBecker, JulietteRodriguez, Joseph E.Pozuelos, Francisco J.Gandolfi, DavideZhou, GeorgeMann, Andrew W.Collins, Karen A.Crossfield, IanBarkaoui, KhalidCollins, Kevin I.Fridlund, MalcolmGillon, MichaëlGonzales, Erica J.Günther, Maximilian N.Henry, Todd J.Howell, Steve B.James, Hodari-SadikiJao, Wei-ChunJehin, EmmanuëlJensen, Eric L. N.Kane, Stephen R.Lissauer, Jack J.Matthews, ElisabethMatson, Rachel A.Paredes, Leonardo A.Schlieder, Joshua E.Stassun, Keivan G.Shporer, AviSha, LizhouTan, Thiam-GuanGeorgieva, IskraMathur, SavitaPalle, EnricPersson, Carina M.Eylen, Vincent VanRicker, George R.Vanderspek, Roland K.Latham, David W.Winn, Joshua N.Seager, S.Jenkins, Jon M.Burke, Christopher J.Goeke, Robert F.Rinehart, StephenRose, Mark E.Ting, Eric B.Torres, GuillermoWong, IanDOI: info:10.3847/2041-8213/ab7302v. 892L7
Huang, Chelsea X., Quinn, Samuel N., Vanderburg, Andrew, Becker, Juliette, Rodriguez, Joseph E., Pozuelos, Francisco J., Gandolfi, Davide, Zhou, George, Mann, Andrew W., Collins, Karen A., Crossfield, Ian, Barkaoui, Khalid, Collins, Kevin I., Fridlund, Malcolm, Gillon, Michaël, Gonzales, Erica J., Günther, Maximilian N., Henry, Todd J., Howell, Steve B., James, Hodari-Sadiki, Jao, Wei-Chun, Jehin, Emmanuël, Jensen, Eric L. N., Kane, Stephen R., Lissauer, Jack J. et al. 2020. "TESS Spots a Hot Jupiter with an Inner Transiting Neptune." The Astrophysical Journal 892:L7.
ID: 156380
Type: article
Authors: Huang, Chelsea X.; Quinn, Samuel N.; Vanderburg, Andrew; Becker, Juliette; Rodriguez, Joseph E.; Pozuelos, Francisco J.; Gandolfi, Davide; Zhou, George; Mann, Andrew W.; Collins, Karen A.; Crossfield, Ian; Barkaoui, Khalid; Collins, Kevin I.; Fridlund, Malcolm; Gillon, Michaël; Gonzales, Erica J.; Günther, Maximilian N.; Henry, Todd J.; Howell, Steve B.; James, Hodari-Sadiki; Jao, Wei-Chun; Jehin, Emmanuël; Jensen, Eric L. N.; Kane, Stephen R.; Lissauer, Jack J.; Matthews, Elisabeth; Matson, Rachel A.; Paredes, Leonardo A.; Schlieder, Joshua E.; Stassun, Keivan G.; Shporer, Avi; Sha, Lizhou; Tan, Thiam-Guan; Georgieva, Iskra; Mathur, Savita; Palle, Enric; Persson, Carina M.; Eylen, Vincent Van; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, S.; Jenkins, Jon M.; Burke, Christopher J.; Goeke, Robert F.; Rinehart, Stephen; Rose, Mark E.; Ting, Eric B.; Torres, Guillermo; Wong, Ian
Abstract: Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an eleventh magnitude K-dwarf in Gaia G-band. It has two transiting planets: a Neptune-sized planet (3.65 ± 0.10 R\oplus) with a 4.1 days period, and a hot Jupiter (1.50-0.22+0.27 RJ) with an 8.4 days period. Precise radial-velocity observations show that the mass of the hot Jupiter is 0.974-0.044+0.043 MJ. For the inner Neptune, the data provide only an upper limit on the mass of 0.17 MJ (3σ). Nevertheless, we are confident that the inner planet is real, based on follow-up ground-based photometry and adaptive-optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.
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.