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A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of PlanetsHurt, Spencer A.Quinn, Samuel N.Latham, David W.Vanderburg, AndrewEsquerdo, Gilbert A.Calkins, Michael L.Berlind, PerryAngus, RuthLatham, Christian A.Zhou, GeorgeDOI: info:10.3847/1538-3881/abdec8v. 161157
Hurt, Spencer A., Quinn, Samuel N., Latham, David W., Vanderburg, Andrew, Esquerdo, Gilbert A., Calkins, Michael L., Berlind, Perry, Angus, Ruth, Latham, Christian A., and Zhou, George. 2021. "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets." The Astronomical Journal 161:157. https://doi.org/10.3847/1538-3881/abdec8
ID: 159324
Type: article
Authors: Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George
Abstract: We present an analysis of 1524 spectra of Vega spanning 10 yr, in which we search for periodic radial-velocity variations. A signal with a periodicity of 0.676 day and a semi-amplitude of ∼10 m s-1 is consistent with the rotation period measured over much shorter time spans by previous spectroscopic and spectropolarimetric studies, confirming the presence of surface features on this A0 star. The activity signal appears to evolve on long timescales, which may indicate the presence of failed fossil magnetic fields on Vega. TESS data reveal Vega's photometric rotational modulation for the first time, with a total amplitude of only 10 ppm. A comparison of the spectroscopic and photometric amplitudes suggests that the surface features may be dominated by bright plages rather than dark spots. For the shortest orbital periods, transit and radial-velocity injection recovery tests exclude the presence of transiting planets larger than 2 R⊕ and most non-transiting giant planets. At long periods, we combine our radial velocities with direct imaging from the literature to produce detection limits for Vegan planets and brown dwarfs out to distances of 15 au. Finally, we detect a candidate radial-velocity signal with a period of 2.43 days and a semi-amplitude of 6 m s-1. If caused by an orbiting companion, its minimum mass would be ∼20 M⊕; because of Vega's pole-on orientation, this would correspond to a Jovian planet if the orbit is aligned with the stellar spin. We discuss the prospects for confirmation of this candidate planet.
Type: article
Authors: Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George
Abstract: We present an analysis of 1524 spectra of Vega spanning 10 yr, in which we search for periodic radial-velocity variations. A signal with a periodicity of 0.676 day and a semi-amplitude of ∼10 m s-1 is consistent with the rotation period measured over much shorter time spans by previous spectroscopic and spectropolarimetric studies, confirming the presence of surface features on this A0 star. The activity signal appears to evolve on long timescales, which may indicate the presence of failed fossil magnetic fields on Vega. TESS data reveal Vega's photometric rotational modulation for the first time, with a total amplitude of only 10 ppm. A comparison of the spectroscopic and photometric amplitudes suggests that the surface features may be dominated by bright plages rather than dark spots. For the shortest orbital periods, transit and radial-velocity injection recovery tests exclude the presence of transiting planets larger than 2 R⊕ and most non-transiting giant planets. At long periods, we combine our radial velocities with direct imaging from the literature to produce detection limits for Vegan planets and brown dwarfs out to distances of 15 au. Finally, we detect a candidate radial-velocity signal with a period of 2.43 days and a semi-amplitude of 6 m s-1. If caused by an orbiting companion, its minimum mass would be ∼20 M⊕; because of Vega's pole-on orientation, this would correspond to a Jovian planet if the orbit is aligned with the stellar spin. We discuss the prospects for confirmation of this candidate planet.
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame ImagesRodriguez, Joseph E.Quinn, Samuel N.Zhou, GeorgeVanderburg, AndrewNielsen, Louise D.Wittenmyer, Robert A.Brahm, RafaelReed, Phillip A.Huang, Chelsea X.Vach, SydneyCiardi, David R.Oelkers, Ryan J.Stassun, Keivan G.Hellier, CoelGaudi, B. ScottEastman, Jason D.Collins, Karen A.Bieryla, AllysonChristian, SamLatham, David W.Carleo, IlariaWright, Duncan J.Matthews, ElisabethGonzales, Erica J.Ziegler, CarlDressing, Courtney D.Howell, Steve B.Tan, Thiam-GuanWittrock, JustinPlavchan, PeterMcLeod, Kim K.Baker, DavidWang, GavinRadford, Don J.Schwarz, Richard P.Esposito, MassimilianoRicker, George R.Vanderspek, Roland K.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, BrettAnderson, D. R.Barclay, ThomasBeatty, Thomas G.Berlind, PerryBouchy, FrancoisBowen, MichaelBowler, Brendan P.Brasseur, C. E.Briceño, CésarCaldwell, Douglas A.Calkins, Michael L.Cartwright, ScottChaturvedi, PriyankaChaverot, GuillaumeChimaladinne, SudhishChristiansen, Jessie L.Collins, Kevin I.Crossfield, Ian J. M.Eastridge, KevinEspinoza, NéstorEsquerdo, Gilbert A.Feliz, Dax L.Fenske, TylerFong, WilliamGan, TianjunGiacalone, StevenGill, HoldenGordon, LindseyGranados, A.Grieves, NolanGuenther, Eike W.Guerrero, NataliaHenning, ThomasHenze, Christopher E.Hesse, KatharineHobson, Melissa J.Horner, JonathanJames, David J.Jensen, Eric L. N.Jimenez, MaryJordán, AndrésKane, Stephen R.Kielkopf, JohnKim, KingsleyKuhn, Rudolf B.Latouf, NatashaLaw, Nicholas M.Levine, Alan M.Lund, Michael B.Mann, Andrew W.Mao, ShudeMatson, Rachel A.Mengel, Matthew W.Mink, JessicaNewman, PatrickO'Dwyer, TannerOkumura, JackPalle, EnricPepper, JoshuaQuintana, Elisa V.Sarkis, PaulaSavel, Arjun B.Schlieder, Joshua E.Schnaible, ChloeShporer, AviSefako, RamotholoSeidel, Julia V.Siverd, Robert J.Skinner, BrettStalport, ManuStevens, Daniel J.Stibbards, CaitlinTinney, C. G.West, R. G.Yahalomi, Daniel A.Zhang, HuiDOI: info:10.3847/1538-3881/abe38av. 161194
Rodriguez, Joseph E., Quinn, Samuel N., Zhou, George, Vanderburg, Andrew, Nielsen, Louise D., Wittenmyer, Robert A., Brahm, Rafael, Reed, Phillip A., Huang, Chelsea X., Vach, Sydney, Ciardi, David R., Oelkers, Ryan J., Stassun, Keivan G., Hellier, Coel, Gaudi, B. Scott, Eastman, Jason D., Collins, Karen A., Bieryla, Allyson, Christian, Sam, Latham, David W., Carleo, Ilaria, Wright, Duncan J., Matthews, Elisabeth, Gonzales, Erica J., Ziegler, Carl et al. 2021. "TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images." The Astronomical Journal 161:194. https://doi.org/10.3847/1538-3881/abe38a
ID: 159316
Type: article
Authors: Rodriguez, Joseph E.; Quinn, Samuel N.; Zhou, George; Vanderburg, Andrew; Nielsen, Louise D.; Wittenmyer, Robert A.; Brahm, Rafael; Reed, Phillip A.; Huang, Chelsea X.; Vach, Sydney; Ciardi, David R.; Oelkers, Ryan J.; Stassun, Keivan G.; Hellier, Coel; Gaudi, B. Scott; Eastman, Jason D.; Collins, Karen A.; Bieryla, Allyson; Christian, Sam; Latham, David W.; Carleo, Ilaria; Wright, Duncan J.; Matthews, Elisabeth; Gonzales, Erica J.; Ziegler, Carl; Dressing, Courtney D.; Howell, Steve B.; Tan, Thiam-Guan; Wittrock, Justin; Plavchan, Peter; McLeod, Kim K.; Baker, David; Wang, Gavin; Radford, Don J.; Schwarz, Richard P.; Esposito, Massimiliano; Ricker, George R.; Vanderspek, Roland K.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett; Anderson, D. R.; Barclay, Thomas; Beatty, Thomas G.; Berlind, Perry; Bouchy, Francois; Bowen, Michael; Bowler, Brendan P.; Brasseur, C. E.; Briceño, César; Caldwell, Douglas A.; Calkins, Michael L.; Cartwright, Scott; Chaturvedi, Priyanka; Chaverot, Guillaume; Chimaladinne, Sudhish; Christiansen, Jessie L.; Collins, Kevin I.; Crossfield, Ian J. M.; Eastridge, Kevin; Espinoza, Néstor; Esquerdo, Gilbert A.; Feliz, Dax L.; Fenske, Tyler; Fong, William; Gan, Tianjun; Giacalone, Steven; Gill, Holden; Gordon, Lindsey; Granados, A.; Grieves, Nolan; Guenther, Eike W.; Guerrero, Natalia; Henning, Thomas; Henze, Christopher E.; Hesse, Katharine; Hobson, Melissa J.; Horner, Jonathan; James, David J.; Jensen, Eric L. N.; Jimenez, Mary; Jordán, Andrés; Kane, Stephen R.; Kielkopf, John; Kim, Kingsley; Kuhn, Rudolf B.; Latouf, Natasha; Law, Nicholas M.; Levine, Alan M.; Lund, Michael B.; Mann, Andrew W.; Mao, Shude; Matson, Rachel A.; Mengel, Matthew W.; Mink, Jessica; Newman, Patrick; O'Dwyer, Tanner; Okumura, Jack; Palle, Enric; Pepper, Joshua; Quintana, Elisa V.; Sarkis, Paula; Savel, Arjun B.; Schlieder, Joshua E.; Schnaible, Chloe; Shporer, Avi; Sefako, Ramotholo; Seidel, Julia V.; Siverd, Robert J.; Skinner, Brett; Stalport, Manu; Stevens, Daniel J.; Stibbards, Caitlin; Tinney, C. G.; West, R. G.; Yahalomi, Daniel A.; Zhang, Hui
Abstract: We present the discovery and characterization of five hot and warm Jupiters-TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960)-based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (RP = 1.01-1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 ≤ 6460 K) and are all relatively bright (9.5 P > 1.7 RJ, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of ${6.31}_{-0.30}^{+0.28}$ MJ and a statistically significant, nonzero orbital eccentricity of e = ${0.074}_{-0.022}^{+0.021}$ . This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
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-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey SatelliteBrahm, RafaelNielsen, Louise D.Wittenmyer, Robert A.Wang, SonghuRodriguez, Joseph E.Espinoza, NéstorJones, Matías I.Jordán, AndrésHenning, ThomasHobson, MelissaKossakowski, DianaRojas, FelipeSarkis, PaulaSchlecker, MartinTrifonov, TrifonShahaf, SaharRicker, GeorgeVanderspek, RolandLatham, David W.Seager, SaraWinn, Joshua N.Jenkins, Jon M.Addison, Brett C.Bakos, Gáspár Á.Bhatti, WaqasBayliss, DanielBerlind, PerryBieryla, AllysonBouchy, FrancoisBowler, Brendan P.Briceño, CésarBrown, Timothy M.Bryant, Edward M.Caldwell, Douglas A.Charbonneau, DavidCollins, Karen A.Davis, Allen B.Esquerdo, Gilbert A.Fulton, Benjamin J.Guerrero, Natalia M.Henze, Christopher E.Hogan, AleishaHorner, JonathanHuang, Chelsea X.Irwin, JonathanKane, Stephen R.Kielkopf, JohnMann, Andrew W.Mazeh, TseviMcCormac, JamesMcCully, CurtisMengel, Matthew W.Mireles, IsmaelOkumura, JackPlavchan, PeterQuinn, Samuel N.Rabus, MarkusSaesen, SophieSchlieder, Joshua E.Segransan, DamienShiao, BernieShporer, AviSiverd, Robert J.Stassun, Keivan G.Suc, VincentTan, Thiam-GuanTorres, PascalTinney, Chris G.Udry, StephaneVanzi, LeonardoVezie, MichaelVines, Jose I.Vuckovic, MajaWright, Duncan J.Yahalomi, Daniel A.Zapata, AbnerZhang, HuiZiegler, CarlDOI: info:10.3847/1538-3881/abba3bv. 160235
Brahm, Rafael, Nielsen, Louise D., Wittenmyer, Robert A., Wang, Songhu, Rodriguez, Joseph E., Espinoza, Néstor, Jones, Matías I., Jordán, Andrés, Henning, Thomas, Hobson, Melissa, Kossakowski, Diana, Rojas, Felipe, Sarkis, Paula, Schlecker, Martin, Trifonov, Trifon, Shahaf, Sahar, Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Addison, Brett C., Bakos, Gáspár Á., Bhatti, Waqas et al. 2020. "TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite." The Astronomical Journal 160:235. https://doi.org/10.3847/1538-3881/abba3b
ID: 158644
Type: article
Authors: Brahm, Rafael; Nielsen, Louise D.; Wittenmyer, Robert A.; Wang, Songhu; Rodriguez, Joseph E.; Espinoza, Néstor; Jones, Matías I.; Jordán, Andrés; Henning, Thomas; Hobson, Melissa; Kossakowski, Diana; Rojas, Felipe; Sarkis, Paula; Schlecker, Martin; Trifonov, Trifon; Shahaf, Sahar; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett C.; Bakos, Gáspár Á.; Bhatti, Waqas; Bayliss, Daniel; Berlind, Perry; Bieryla, Allyson; Bouchy, Francois; Bowler, Brendan P.; Briceño, César; Brown, Timothy M.; Bryant, Edward M.; Caldwell, Douglas A.; Charbonneau, David; Collins, Karen A.; Davis, Allen B.; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Guerrero, Natalia M.; Henze, Christopher E.; Hogan, Aleisha; Horner, Jonathan; Huang, Chelsea X.; Irwin, Jonathan; Kane, Stephen R.; Kielkopf, John; Mann, Andrew W.; Mazeh, Tsevi; McCormac, James; McCully, Curtis; Mengel, Matthew W.; Mireles, Ismael; Okumura, Jack; Plavchan, Peter; Quinn, Samuel N.; Rabus, Markus; Saesen, Sophie; Schlieder, Joshua E.; Segransan, Damien; Shiao, Bernie; Shporer, Avi; Siverd, Robert J.; Stassun, Keivan G.; Suc, Vincent; Tan, Thiam-Guan; Torres, Pascal; Tinney, Chris G.; Udry, Stephane; Vanzi, Leonardo; Vezie, Michael; Vines, Jose I.; Vuckovic, Maja; Wright, Duncan J.; Yahalomi, Daniel A.; Zapata, Abner; Zhang, Hui; Ziegler, Carl
Abstract: We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 ${R}_{{\rm{J}}}$ and 1.07 ± 0.02 ${R}_{{\rm{J}}}$ , respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 ${M}_{{\rm{J}}}$ versus 0.95 ± 0.07 ${M}_{{\rm{J}}}$ , respectively). Both planets orbit metal-rich stars ( $[\mathrm{Fe}/{\rm{H}}]$ = $+0.26\pm 0.05$ dex and $[\mathrm{Fe}/{\rm{H}}]$ = $+0.24\pm 0.05$ for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a ${M}_{\star }$ = 1.14 ± 0.02 ${M}_{\odot }$ , ${R}_{\star }$ = 1.66 ± 0.02 ${R}_{\odot }$ G-type star ( ${T}_{\mathrm{eff}}$ = $5735\pm 72$ K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star ( ${T}_{\mathrm{eff}}$ = $6261\pm 80$ K), which has a mass of ${M}_{\star }$ = 1.28 ± 0.03 ${M}_{\odot }$ and a radius of ${R}_{\star }$ = 1.39 ± 0.02 ${R}_{\odot }$ . TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.
Type: article
Authors: Brahm, Rafael; Nielsen, Louise D.; Wittenmyer, Robert A.; Wang, Songhu; Rodriguez, Joseph E.; Espinoza, Néstor; Jones, Matías I.; Jordán, Andrés; Henning, Thomas; Hobson, Melissa; Kossakowski, Diana; Rojas, Felipe; Sarkis, Paula; Schlecker, Martin; Trifonov, Trifon; Shahaf, Sahar; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett C.; Bakos, Gáspár Á.; Bhatti, Waqas; Bayliss, Daniel; Berlind, Perry; Bieryla, Allyson; Bouchy, Francois; Bowler, Brendan P.; Briceño, César; Brown, Timothy M.; Bryant, Edward M.; Caldwell, Douglas A.; Charbonneau, David; Collins, Karen A.; Davis, Allen B.; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Guerrero, Natalia M.; Henze, Christopher E.; Hogan, Aleisha; Horner, Jonathan; Huang, Chelsea X.; Irwin, Jonathan; Kane, Stephen R.; Kielkopf, John; Mann, Andrew W.; Mazeh, Tsevi; McCormac, James; McCully, Curtis; Mengel, Matthew W.; Mireles, Ismael; Okumura, Jack; Plavchan, Peter; Quinn, Samuel N.; Rabus, Markus; Saesen, Sophie; Schlieder, Joshua E.; Segransan, Damien; Shiao, Bernie; Shporer, Avi; Siverd, Robert J.; Stassun, Keivan G.; Suc, Vincent; Tan, Thiam-Guan; Torres, Pascal; Tinney, Chris G.; Udry, Stephane; Vanzi, Leonardo; Vezie, Michael; Vines, Jose I.; Vuckovic, Maja; Wright, Duncan J.; Yahalomi, Daniel A.; Zapata, Abner; Zhang, Hui; Ziegler, Carl
Abstract: We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 ${R}_{{\rm{J}}}$ and 1.07 ± 0.02 ${R}_{{\rm{J}}}$ , respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 ${M}_{{\rm{J}}}$ versus 0.95 ± 0.07 ${M}_{{\rm{J}}}$ , respectively). Both planets orbit metal-rich stars ( $[\mathrm{Fe}/{\rm{H}}]$ = $+0.26\pm 0.05$ dex and $[\mathrm{Fe}/{\rm{H}}]$ = $+0.24\pm 0.05$ for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a ${M}_{\star }$ = 1.14 ± 0.02 ${M}_{\odot }$ , ${R}_{\star }$ = 1.66 ± 0.02 ${R}_{\odot }$ G-type star ( ${T}_{\mathrm{eff}}$ = $5735\pm 72$ K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star ( ${T}_{\mathrm{eff}}$ = $6261\pm 80$ K), which has a mass of ${M}_{\star }$ = 1.28 ± 0.03 ${M}_{\odot }$ and a radius of ${R}_{\star }$ = 1.39 ± 0.02 ${R}_{\odot }$ . TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.
TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune DesertBurt, Jennifer A.Nielsen, Louise D.Quinn, Samuel N.Mamajek, Eric E.Matthews, Elisabeth C.Zhou, GeorgeSeidel, Julia V.Huang, Chelsea X.Lopez, EricSoto, MaritzaOtegi, JonStassun, Keivan G.Kreidberg, LauraCollins, Karen A.Eastman, Jason D.Rodriguez, Joseph E.Vanderburg, AndrewHalverson, Samuel P.Teske, Johanna K.Wang, Sharon X.Butler, R. PaulBouchy, FrançoisDumusque, XavierSegransen, DamienShectman, Stephen A.Crane, Jeffrey D.Feng, FaboMontet, Benjamin T.Feinstein, Adina D.Beletski, YuriFlowers, ErinGünther, Maximilian N.Daylan, TansuCollins, Kevin I.Conti, Dennis M.Gan, TianjunJensen, Eric L. N.Kielkopf, John F.Tan, Thiam-GuanHelled, RavitDorn, CarolineHaldemann, JonasLissauer, Jack J.Ricker, George R.Vanderspek, RolandLatham, David W.Seager, S.Winn, Joshua N.Jenkins, Jon M.Twicken, Joseph D.Smith, Jeffrey C.Tenenbaum, PeterCartwright, ScottBarclay, ThomasPepper, JoshuaEsquerdo, GilbertFong, WilliamDOI: info:10.3847/1538-3881/abac0cv. 160153
Burt, Jennifer A., Nielsen, Louise D., Quinn, Samuel N., Mamajek, Eric E., Matthews, Elisabeth C., Zhou, George, Seidel, Julia V., Huang, Chelsea X., Lopez, Eric, Soto, Maritza, Otegi, Jon, Stassun, Keivan G., Kreidberg, Laura, Collins, Karen A., Eastman, Jason D., Rodriguez, Joseph E., Vanderburg, Andrew, Halverson, Samuel P., Teske, Johanna K., Wang, Sharon X., Butler, R. Paul, Bouchy, François, Dumusque, Xavier, Segransen, Damien, Shectman, Stephen A. et al. 2020. "TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert." The Astronomical Journal 160:153. https://doi.org/10.3847/1538-3881/abac0c
ID: 157601
Type: article
Authors: Burt, Jennifer A.; Nielsen, Louise D.; Quinn, Samuel N.; Mamajek, Eric E.; Matthews, Elisabeth C.; Zhou, George; Seidel, Julia V.; Huang, Chelsea X.; Lopez, Eric; Soto, Maritza; Otegi, Jon; Stassun, Keivan G.; Kreidberg, Laura; Collins, Karen A.; Eastman, Jason D.; Rodriguez, Joseph E.; Vanderburg, Andrew; Halverson, Samuel P.; Teske, Johanna K.; Wang, Sharon X.; Butler, R. Paul; Bouchy, François; Dumusque, Xavier; Segransen, Damien; Shectman, Stephen A.; Crane, Jeffrey D.; Feng, Fabo; Montet, Benjamin T.; Feinstein, Adina D.; Beletski, Yuri; Flowers, Erin; Günther, Maximilian N.; Daylan, Tansu; Collins, Kevin I.; Conti, Dennis M.; Gan, Tianjun; Jensen, Eric L. N.; Kielkopf, John F.; Tan, Thiam-Guan; Helled, Ravit; Dorn, Caroline; Haldemann, Jonas; Lissauer, Jack J.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Twicken, Joseph D.; Smith, Jeffrey C.; Tenenbaum, Peter; Cartwright, Scott; Barclay, Thomas; Pepper, Joshua; Esquerdo, Gilbert; Fong, William
Abstract: We report the detection of a transiting hot Neptune exoplanet orbiting TOI-824 (SCR J1448-5735), a nearby (d = 64 pc) K4V star, using data from the Transiting Exoplanet Survey Satellite. The newly discovered planet has a radius Rp = 2.93 ± 0.20 ${R}_{\oplus }$ and an orbital period of 1.393 days. Radial velocity measurements using the Planet Finder Spectrograph and the High Accuracy Radial velocity Planet Searcher spectrograph confirm the existence of the planet, and we estimate its mass to be 18.47 ± 1.84 ${M}_{\oplus }$ . The planet's mean density is ${\rho }_{{\rm{p}}}$ = 4.03 ${}_{-0.78}^{+0.98}$ ${\rm{g}}\,{\mathrm{cm}}^{-3}$ , making it more than twice as dense as Neptune. TOI-824 b's high equilibrium temperature makes the planet likely to have a cloud-free atmosphere, and thus it is an excellent candidate for follow-up atmospheric studies. The detectability of TOI-824 b's atmosphere from both ground and space is promising and could lead to the detailed characterization of the most irradiated small planet at the edge of the hot Neptune desert that has retained its atmosphere to date.
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.
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. https://doi.org/10.3847/1538-3881/ab9534
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.
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. 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. https://doi.org/10.3847/1538-3881/ab84e3
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.
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.
TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESSDavis, Allen B.Wang, SonghuJones, MatiasEastman, Jason D.Günther, Maximilian N.Stassun, Keivan G.Addison, Brett C.Collins, Karen A.Quinn, Samuel N.Latham, David W.Trifonov, TrifonShahaf, SaharMazeh, TseviKane, Stephen R.Narita, NorioWang, Xian-YuTan, Thiam-GuanCiardi, David R.Tokovinin, AndreiZiegler, CarlTronsgaard, RenéMillholland, SarahCruz, BryndisBerlind, PerryCalkins, Michael L.Esquerdo, Gilbert A.Collins, Kevin I.Conti, Dennis M.Murgas, FelipeEvans, PhilLewin, PabloRadford, Don J.Paredes, Leonardo A.Henry, Todd J.Hodari-Sadiki, JamesLund, Michael B.Christiansen, Jessie L.Law, Nicholas M.Mann, Andrew W.Briceño, CésarParviainen, HannuPalle, EnricWatanabe, NoriharuRicker, George R.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Krishnamurthy, AkshataBatalha, Natalie M.Burt, JenniferColón, Knicole D.Dynes, ScottCaldwell, Douglas A.Morris, RobertHenze, Christopher E.Fischer, Debra A.DOI: info:10.3847/1538-3881/aba49dv. 160229
Davis, Allen B., Wang, Songhu, Jones, Matias, Eastman, Jason D., Günther, Maximilian N., Stassun, Keivan G., Addison, Brett C., Collins, Karen A., Quinn, Samuel N., Latham, David W., Trifonov, Trifon, Shahaf, Sahar, Mazeh, Tsevi, Kane, Stephen R., Narita, Norio, Wang, Xian-Yu, Tan, Thiam-Guan, Ciardi, David R., Tokovinin, Andrei, Ziegler, Carl, Tronsgaard, René, Millholland, Sarah, Cruz, Bryndis, Berlind, Perry, Calkins, Michael L. et al. 2020. "TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS." The Astronomical Journal 160:229. https://doi.org/10.3847/1538-3881/aba49d
ID: 158650
Type: article
Authors: Davis, Allen B.; Wang, Songhu; Jones, Matias; Eastman, Jason D.; Günther, Maximilian N.; Stassun, Keivan G.; Addison, Brett C.; Collins, Karen A.; Quinn, Samuel N.; Latham, David W.; Trifonov, Trifon; Shahaf, Sahar; Mazeh, Tsevi; Kane, Stephen R.; Narita, Norio; Wang, Xian-Yu; Tan, Thiam-Guan; Ciardi, David R.; Tokovinin, Andrei; Ziegler, Carl; Tronsgaard, René; Millholland, Sarah; Cruz, Bryndis; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Collins, Kevin I.; Conti, Dennis M.; Murgas, Felipe; Evans, Phil; Lewin, Pablo; Radford, Don J.; Paredes, Leonardo A.; Henry, Todd J.; Hodari-Sadiki, James; Lund, Michael B.; Christiansen, Jessie L.; Law, Nicholas M.; Mann, Andrew W.; Briceño, César; Parviainen, Hannu; Palle, Enric; Watanabe, Noriharu; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Krishnamurthy, Akshata; Batalha, Natalie M.; Burt, Jennifer; Colón, Knicole D.; Dynes, Scott; Caldwell, Douglas A.; Morris, Robert; Henze, Christopher E.; Fischer, Debra A.
Abstract: We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of ${1.463}_{-0.096}^{+0.10}$ MJ and a radius of ${1.02}_{-0.29}^{+0.71}$ RJ. Also a classical hot Jupiter, TOI 905 b has a mass of ${0.667}_{-0.041}^{+0.042}$ MJ and radius of ${1.171}_{-0.051}^{+0.053}$ RJ. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V ˜ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of ${0.994}_{-0.049}^{+0.083}$ , making it one of only ˜20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.
Type: article
Authors: Davis, Allen B.; Wang, Songhu; Jones, Matias; Eastman, Jason D.; Günther, Maximilian N.; Stassun, Keivan G.; Addison, Brett C.; Collins, Karen A.; Quinn, Samuel N.; Latham, David W.; Trifonov, Trifon; Shahaf, Sahar; Mazeh, Tsevi; Kane, Stephen R.; Narita, Norio; Wang, Xian-Yu; Tan, Thiam-Guan; Ciardi, David R.; Tokovinin, Andrei; Ziegler, Carl; Tronsgaard, René; Millholland, Sarah; Cruz, Bryndis; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Collins, Kevin I.; Conti, Dennis M.; Murgas, Felipe; Evans, Phil; Lewin, Pablo; Radford, Don J.; Paredes, Leonardo A.; Henry, Todd J.; Hodari-Sadiki, James; Lund, Michael B.; Christiansen, Jessie L.; Law, Nicholas M.; Mann, Andrew W.; Briceño, César; Parviainen, Hannu; Palle, Enric; Watanabe, Noriharu; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Krishnamurthy, Akshata; Batalha, Natalie M.; Burt, Jennifer; Colón, Knicole D.; Dynes, Scott; Caldwell, Douglas A.; Morris, Robert; Henze, Christopher E.; Fischer, Debra A.
Abstract: We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of ${1.463}_{-0.096}^{+0.10}$ MJ and a radius of ${1.02}_{-0.29}^{+0.71}$ RJ. Also a classical hot Jupiter, TOI 905 b has a mass of ${0.667}_{-0.041}^{+0.042}$ MJ and radius of ${1.171}_{-0.051}^{+0.053}$ RJ. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V ˜ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of ${0.994}_{-0.049}^{+0.083}$ , making it one of only ˜20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.
TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major GroupMann, Andrew W.Johnson, Marshall C.Vanderburg, AndrewKraus, Adam L.Rizzuto, Aaron C.Wood, Mackenna L.Bush, Jonathan L.Rockcliffe, KeighleyNewton, Elisabeth R.Latham, David W.Mamajek, Eric E.Zhou, GeorgeQuinn, Samuel N.Thao, Pa ChiaBenatti, SerenaCosentino, RosarioDesidera, SilvanoHarutyunyan, AvetLovis, ChristopheMortier, AnneliesPepe, Francesco A.Poretti, EnnioWilson, Thomas G.Kristiansen, Martti H.Gagliano, RobertJacobs, ThomasLaCourse, Daryll M.Omohundro, MarkSchwengeler, Hans MartinTerentev, Ivan A.Kane, Stephen R.Hill, Michelle L.Rabus, MarkusEsquerdo, Gilbert A.Berlind, PerryCollins, Karen A.Murawski, GabrielSallam, Nezar HazamAitken, Michael M.Massey, BobRicker, George R.Vanderspek, RolandSeager, SaraWinn, Joshua N.Jenkins, Jon M.Barclay, ThomasCaldwell, Douglas A.Dragomir, DianaDoty, John P.Glidden, AnaTenenbaum, PeterTorres, GuillermoTwicken, Joseph D.Villanueva, Steven, Jr.DOI: info:10.3847/1538-3881/abae64v. 160179
Mann, Andrew W., Johnson, Marshall C., Vanderburg, Andrew, Kraus, Adam L., Rizzuto, Aaron C., Wood, Mackenna L., Bush, Jonathan L., Rockcliffe, Keighley, Newton, Elisabeth R., Latham, David W., Mamajek, Eric E., Zhou, George, Quinn, Samuel N., Thao, Pa Chia, Benatti, Serena, Cosentino, Rosario, Desidera, Silvano, Harutyunyan, Avet, Lovis, Christophe, Mortier, Annelies, Pepe, Francesco A., Poretti, Ennio, Wilson, Thomas G., Kristiansen, Martti H., Gagliano, Robert et al. 2020. "TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major Group." The Astronomical Journal 160:179. https://doi.org/10.3847/1538-3881/abae64
ID: 157597
Type: article
Authors: Mann, Andrew W.; Johnson, Marshall C.; Vanderburg, Andrew; Kraus, Adam L.; Rizzuto, Aaron C.; Wood, Mackenna L.; Bush, Jonathan L.; Rockcliffe, Keighley; Newton, Elisabeth R.; Latham, David W.; Mamajek, Eric E.; Zhou, George; Quinn, Samuel N.; Thao, Pa Chia; Benatti, Serena; Cosentino, Rosario; Desidera, Silvano; Harutyunyan, Avet; Lovis, Christophe; Mortier, Annelies; Pepe, Francesco A.; Poretti, Ennio; Wilson, Thomas G.; Kristiansen, Martti H.; Gagliano, Robert; Jacobs, Thomas; LaCourse, Daryll M.; Omohundro, Mark; Schwengeler, Hans Martin; Terentev, Ivan A.; Kane, Stephen R.; Hill, Michelle L.; Rabus, Markus; Esquerdo, Gilbert A.; Berlind, Perry; Collins, Karen A.; Murawski, Gabriel; Sallam, Nezar Hazam; Aitken, Michael M.; Massey, Bob; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Barclay, Thomas; Caldwell, Douglas A.; Dragomir, Diana; Doty, John P.; Glidden, Ana; Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Villanueva, Steven, Jr.
Abstract: Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (⊕ and 2.67 ± 0.12 R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using High Accuracy Radial velocity Planet Searcher for the Northern hemisphere velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V = 6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.
Type: article
Authors: Mann, Andrew W.; Johnson, Marshall C.; Vanderburg, Andrew; Kraus, Adam L.; Rizzuto, Aaron C.; Wood, Mackenna L.; Bush, Jonathan L.; Rockcliffe, Keighley; Newton, Elisabeth R.; Latham, David W.; Mamajek, Eric E.; Zhou, George; Quinn, Samuel N.; Thao, Pa Chia; Benatti, Serena; Cosentino, Rosario; Desidera, Silvano; Harutyunyan, Avet; Lovis, Christophe; Mortier, Annelies; Pepe, Francesco A.; Poretti, Ennio; Wilson, Thomas G.; Kristiansen, Martti H.; Gagliano, Robert; Jacobs, Thomas; LaCourse, Daryll M.; Omohundro, Mark; Schwengeler, Hans Martin; Terentev, Ivan A.; Kane, Stephen R.; Hill, Michelle L.; Rabus, Markus; Esquerdo, Gilbert A.; Berlind, Perry; Collins, Karen A.; Murawski, Gabriel; Sallam, Nezar Hazam; Aitken, Michael M.; Massey, Bob; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Barclay, Thomas; Caldwell, Douglas A.; Dragomir, Diana; Doty, John P.; Glidden, Ana; Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Villanueva, Steven, Jr.
Abstract: Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (⊕ and 2.67 ± 0.12 R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using High Accuracy Radial velocity Planet Searcher for the Northern hemisphere velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V = 6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.
An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELTStevens, Daniel J.Zhou, GeorgeJohnson, Marshall C.Rizzuto, Aaron C.Rodriguez, Joseph E.Bieryla, AllysonCollins, Karen A.Villanueva, Steven, Jr.Wright, Jason T.Gaudi, B. ScottLatham, David W.Beatty, Thomas G.Lund, Michael B.Siverd, Robert J.Kraus, Adam L.Wachiraphan, PatcharapolBerlind, PerryCalkins, Michael L.Esquerdo, Gilbert A.Kielkopf, John F.Kuhn, Rudolf B.Manner, MarkPepper, JoshuaStassun, Keivan G.DOI: info:10.1093/mnras/staa3142v. 4993775–3791
Stevens, Daniel J., Zhou, George, Johnson, Marshall C., Rizzuto, Aaron C., Rodriguez, Joseph E., Bieryla, Allyson, Collins, Karen A., Villanueva, Steven, Jr., Wright, Jason T., Gaudi, B. Scott, Latham, David W., Beatty, Thomas G., Lund, Michael B., Siverd, Robert J., Kraus, Adam L., Wachiraphan, Patcharapol, Berlind, Perry, Calkins, Michael L., Esquerdo, Gilbert A., Kielkopf, John F., Kuhn, Rudolf B., Manner, Mark, Pepper, Joshua, and Stassun, Keivan G. 2020. "An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT." Monthly Notices of the Royal Astronomical Society 499:3775– 3791. https://doi.org/10.1093/mnras/staa3142
ID: 158638
Type: article
Authors: Stevens, Daniel J.; Zhou, George; Johnson, Marshall C.; Rizzuto, Aaron C.; Rodriguez, Joseph E.; Bieryla, Allyson; Collins, Karen A.; Villanueva, Steven, Jr.; Wright, Jason T.; Gaudi, B. Scott; Latham, David W.; Beatty, Thomas G.; Lund, Michael B.; Siverd, Robert J.; Kraus, Adam L.; Wachiraphan, Patcharapol; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Kielkopf, John F.; Kuhn, Rudolf B.; Manner, Mark; Pepper, Joshua; Stassun, Keivan G.
Abstract: We present the discovery of KELT J072709 + 072007 (HD 58730), a very low mass ratio (q = M2/M1 ? 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective ( $M_2 = 0.22 \pm 0.02\ \, \mathrm{M}_{\odot })$ M star transiting a late-B primary ( $M_1 = 3.34^{+0.07}_{-0.09}\ \, \mathrm{M}_{\odot }\,\mathrm{ and}\,\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$ ). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star's radius is inflated by $26 \pm 8{{\ \rm per\ cent}}$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star's properties in such a binary might differ from the properties it would have in isolation.
Type: article
Authors: Stevens, Daniel J.; Zhou, George; Johnson, Marshall C.; Rizzuto, Aaron C.; Rodriguez, Joseph E.; Bieryla, Allyson; Collins, Karen A.; Villanueva, Steven, Jr.; Wright, Jason T.; Gaudi, B. Scott; Latham, David W.; Beatty, Thomas G.; Lund, Michael B.; Siverd, Robert J.; Kraus, Adam L.; Wachiraphan, Patcharapol; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Kielkopf, John F.; Kuhn, Rudolf B.; Manner, Mark; Pepper, Joshua; Stassun, Keivan G.
Abstract: We present the discovery of KELT J072709 + 072007 (HD 58730), a very low mass ratio (q = M2/M1 ? 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective ( $M_2 = 0.22 \pm 0.02\ \, \mathrm{M}_{\odot })$ M star transiting a late-B primary ( $M_1 = 3.34^{+0.07}_{-0.09}\ \, \mathrm{M}_{\odot }\,\mathrm{ and}\,\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$ ). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star's radius is inflated by $26 \pm 8{{\ \rm per\ cent}}$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star's properties in such a binary might differ from the properties it would have in isolation.
TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS MissionŠubjak, JánSharma, RishikeshCarmichael, Theron W.Johnson, Marshall C.Gonzales, Erica J.Matthews, ElisabethBoffin, Henri M. J.Brahm, RafaelChaturvedi, PriyankaChakraborty, AbhijitCiardi, David R.Collins, Karen A.Esposito, MassimilianoFridlund, MalcolmGan, TianjunGandolfi, DavideGarcía, Rafael A.Guenther, EikeHatzes, ArtieLatham, David W.Mathis, StéphaneMathur, SavitaPersson, Carina M.Relles, Howard M.Schlieder, Joshua E.Barclay, ThomasDressing, Courtney D.Crossfield, IanHoward, Andrew W.Rodler, FlorianZhou, GeorgeQuinn, Samuel N.Esquerdo, Gilbert A.Calkins, Michael L.Berlind, PerryStassun, Keivan G.Blažek, MartinSkarka, MarekŠpoková, MagdalenaŽák, JiříAlbrecht, SimonSobrino, Roi AlonsoBeck, PaulCabrera, JuanCarleo, IlariaCochran, William D.Csizmadia, SzilardDai, FeiDeeg, Hans J.de Leon, Jerome P.Eigmüller, PhilippEndl, MichaelErikson, AndersFukui, AkihikoGeorgieva, IskraGonzález-Cuesta, LucíaGrziwa, SaschaHidalgo, DiegoHirano, TeruyukiHjorth, MariaKnudstrup, EmilKorth, JudithLam, Kristine W. F.Livingston, John H.Lund, Mikkel N.Luque, RafaelRodríguez, Pilar MontanesMurgas, FelipeNarita, NorioNespral, DavidNiraula, PrajwalNowak, GrzegorzPallé, EnricPätzold, MartinPrieto-Arranz, JorgeRauer, HeikeRedfield, SethRibas, IgnasiSmith, Alexis M. S.Eylen, Vincent VanKabáth, PetrDOI: info:10.3847/1538-3881/ab7245v. 159151
Šubjak, Ján, Sharma, Rishikesh, Carmichael, Theron W., Johnson, Marshall C., Gonzales, Erica J., Matthews, Elisabeth, Boffin, Henri M. J., Brahm, Rafael, Chaturvedi, Priyanka, Chakraborty, Abhijit, Ciardi, David R., Collins, Karen A., Esposito, Massimiliano, Fridlund, Malcolm, Gan, Tianjun, Gandolfi, Davide, García, Rafael A., Guenther, Eike, Hatzes, Artie, Latham, David W., Mathis, Stéphane, Mathur, Savita, Persson, Carina M., Relles, Howard M., Schlieder, Joshua E. et al. 2020. "TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission." The Astronomical Journal 159:151. https://doi.org/10.3847/1538-3881/ab7245
ID: 157123
Type: article
Authors: Šubjak, Ján; Sharma, Rishikesh; Carmichael, Theron W.; Johnson, Marshall C.; Gonzales, Erica J.; Matthews, Elisabeth; Boffin, Henri M. J.; Brahm, Rafael; Chaturvedi, Priyanka; Chakraborty, Abhijit; Ciardi, David R.; Collins, Karen A.; Esposito, Massimiliano; Fridlund, Malcolm; Gan, Tianjun; Gandolfi, Davide; García, Rafael A.; Guenther, Eike; Hatzes, Artie; Latham, David W.; Mathis, Stéphane; Mathur, Savita; Persson, Carina M.; Relles, Howard M.; Schlieder, Joshua E.; Barclay, Thomas; Dressing, Courtney D.; Crossfield, Ian; Howard, Andrew W.; Rodler, Florian; Zhou, George; Quinn, Samuel N.; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Stassun, Keivan G.; Blažek, Martin; Skarka, Marek; Špoková, Magdalena; Žák, Jiří; Albrecht, Simon; Sobrino, Roi Alonso; Beck, Paul; Cabrera, Juan; Carleo, Ilaria; Cochran, William D.; Csizmadia, Szilard; Dai, Fei; Deeg, Hans J.; de Leon, Jerome P.; Eigmüller, Philipp; Endl, Michael; Erikson, Anders; Fukui, Akihiko; Georgieva, Iskra; González-Cuesta, Lucía; Grziwa, Sascha; Hidalgo, Diego; Hirano, Teruyuki; Hjorth, Maria; Knudstrup, Emil; Korth, Judith; Lam, Kristine W. F.; Livingston, John H.; Lund, Mikkel N.; Luque, Rafael; Rodríguez, Pilar Montanes; Murgas, Felipe; Narita, Norio; Nespral, David; Niraula, Prajwal; Nowak, Grzegorz; Pallé, Enric; Pätzold, Martin; Prieto-Arranz, Jorge; Rauer, Heike; Redfield, Seth; Ribas, Ignasi; Smith, Alexis M. S.; Eylen, Vincent Van; Kabáth, Petr
Abstract: We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P = 3.6772 ± 0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD's radius ( ${R}_{b}={1.34}_{-0.15}^{+0.26}{R}_{{\rm{J}}} ). We obtained high- resolution spectroscopic observations with the FIES, Ondřejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be Mb = 53.7 ± 1.2 ${M}_{{\rm{J}}} . The host star has a mass of M⋆ = 1.80 ± 0.06 M☉, a radius of R⋆ = 1.70 ± 0.05R☉, an effective temperature of Teff = 7650 ± 160 K, and a relatively high metallicity of 0.61 ± 0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main-sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert ( $35\mbox{--}55{M}_{{\rm{J}}}\sin i ) is reforesting.
Type: article
Authors: Šubjak, Ján; Sharma, Rishikesh; Carmichael, Theron W.; Johnson, Marshall C.; Gonzales, Erica J.; Matthews, Elisabeth; Boffin, Henri M. J.; Brahm, Rafael; Chaturvedi, Priyanka; Chakraborty, Abhijit; Ciardi, David R.; Collins, Karen A.; Esposito, Massimiliano; Fridlund, Malcolm; Gan, Tianjun; Gandolfi, Davide; García, Rafael A.; Guenther, Eike; Hatzes, Artie; Latham, David W.; Mathis, Stéphane; Mathur, Savita; Persson, Carina M.; Relles, Howard M.; Schlieder, Joshua E.; Barclay, Thomas; Dressing, Courtney D.; Crossfield, Ian; Howard, Andrew W.; Rodler, Florian; Zhou, George; Quinn, Samuel N.; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Stassun, Keivan G.; Blažek, Martin; Skarka, Marek; Špoková, Magdalena; Žák, Jiří; Albrecht, Simon; Sobrino, Roi Alonso; Beck, Paul; Cabrera, Juan; Carleo, Ilaria; Cochran, William D.; Csizmadia, Szilard; Dai, Fei; Deeg, Hans J.; de Leon, Jerome P.; Eigmüller, Philipp; Endl, Michael; Erikson, Anders; Fukui, Akihiko; Georgieva, Iskra; González-Cuesta, Lucía; Grziwa, Sascha; Hidalgo, Diego; Hirano, Teruyuki; Hjorth, Maria; Knudstrup, Emil; Korth, Judith; Lam, Kristine W. F.; Livingston, John H.; Lund, Mikkel N.; Luque, Rafael; Rodríguez, Pilar Montanes; Murgas, Felipe; Narita, Norio; Nespral, David; Niraula, Prajwal; Nowak, Grzegorz; Pallé, Enric; Pätzold, Martin; Prieto-Arranz, Jorge; Rauer, Heike; Redfield, Seth; Ribas, Ignasi; Smith, Alexis M. S.; Eylen, Vincent Van; Kabáth, Petr
Abstract: We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P = 3.6772 ± 0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD's radius ( ${R}_{b}={1.34}_{-0.15}^{+0.26}{R}_{{\rm{J}}} ). We obtained high- resolution spectroscopic observations with the FIES, Ondřejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be Mb = 53.7 ± 1.2 ${M}_{{\rm{J}}} . The host star has a mass of M⋆ = 1.80 ± 0.06 M☉, a radius of R⋆ = 1.70 ± 0.05R☉, an effective temperature of Teff = 7650 ± 160 K, and a relatively high metallicity of 0.61 ± 0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main-sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert ( $35\mbox{--}55{M}_{{\rm{J}}}\sin i ) is reforesting.
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. https://doi.org/10.3847/1538-3881/ab8d31
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.
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.
Qatar Exoplanet Survey: Qatar-7b—A Very Hot Jupiter Orbiting a Metal-rich F-StarAlsubai, KhalidTsvetanov, Zlatan I.Latham, David W.Bieryla, AllysonPyrzas, StylianosMislis, DimitrisEsquerdo, Gilbert A.Esamdin, AliLiu, JinzhongMa, LuBretton, MarcPallé, EnricMurgas, FelipeVilchez, Nicolas P. E.Morton, Timothy D.Parviainien, HannuMontañes-Rodriguez, PilarNarita, NorioFukui, AkihikoKusakabe, NobuhikoTamura, MotohideDOI: info:10.3847/1538-3881/aaf80av. 15774
Alsubai, Khalid, Tsvetanov, Zlatan I., Latham, David W., Bieryla, Allyson, Pyrzas, Stylianos, Mislis, Dimitris, Esquerdo, Gilbert A., Esamdin, Ali, Liu, Jinzhong, Ma, Lu, Bretton, Marc, Pallé, Enric, Murgas, Felipe, Vilchez, Nicolas P. E., Morton, Timothy D., Parviainien, Hannu, Montañes-Rodriguez, Pilar, Narita, Norio, Fukui, Akihiko, Kusakabe, Nobuhiko, and Tamura, Motohide. 2019. "Qatar Exoplanet Survey: Qatar-7b—A Very Hot Jupiter Orbiting a Metal-rich F-Star." The Astronomical Journal 157:74. https://doi.org/10.3847/1538-3881/aaf80a
ID: 150484
Type: article
Authors: Alsubai, Khalid; Tsvetanov, Zlatan I.; Latham, David W.; Bieryla, Allyson; Pyrzas, Stylianos; Mislis, Dimitris; Esquerdo, Gilbert A.; Esamdin, Ali; Liu, Jinzhong; Ma, Lu; Bretton, Marc; Pallé, Enric; Murgas, Felipe; Vilchez, Nicolas P. E.; Morton, Timothy D.; Parviainien, Hannu; Montañes-Rodriguez, Pilar; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Tamura, Motohide
Abstract: We present the discovery of Qatar-7b—a very hot and inflated giant gas planet orbiting close to its parent star. The host star is a relatively massive main-sequence F-star with mass and radius {M}\star =1.41+/- 0.03 {M}ȯ and {R}\star =1.56+/- 0.02 {R}ȯ , respectively, at a distance d = 726 ± 26 pc, and an estimated age ∼1 Gyr. With its orbital period of P = 2.032 days, the planet is located less than five stellar radii from its host star and is heated to a high temperature T eq ≈ 2100 K. From a global solution to the available photometric and radial velocity observations, we calculate the mass and radius of the planet to be {M}{{P}} = 1.88 ± 0.25 {M}{{J}} and {R}{{P}} = 1.70 ± 0.03 {R}{{J}}, respectively. The planet radius and equilibrium temperature put Qatar-7b in the top 6% of the hottest and largest known exoplanets. With its large radius and high temperature, Qatar-7b is a valuable addition to the short list of targets that offer the best opportunity for studying their atmospheres through transmission spectroscopy.
Type: article
Authors: Alsubai, Khalid; Tsvetanov, Zlatan I.; Latham, David W.; Bieryla, Allyson; Pyrzas, Stylianos; Mislis, Dimitris; Esquerdo, Gilbert A.; Esamdin, Ali; Liu, Jinzhong; Ma, Lu; Bretton, Marc; Pallé, Enric; Murgas, Felipe; Vilchez, Nicolas P. E.; Morton, Timothy D.; Parviainien, Hannu; Montañes-Rodriguez, Pilar; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Tamura, Motohide
Abstract: We present the discovery of Qatar-7b—a very hot and inflated giant gas planet orbiting close to its parent star. The host star is a relatively massive main-sequence F-star with mass and radius {M}\star =1.41+/- 0.03 {M}ȯ and {R}\star =1.56+/- 0.02 {R}ȯ , respectively, at a distance d = 726 ± 26 pc, and an estimated age ∼1 Gyr. With its orbital period of P = 2.032 days, the planet is located less than five stellar radii from its host star and is heated to a high temperature T eq ≈ 2100 K. From a global solution to the available photometric and radial velocity observations, we calculate the mass and radius of the planet to be {M}{{P}} = 1.88 ± 0.25 {M}{{J}} and {R}{{P}} = 1.70 ± 0.03 {R}{{J}}, respectively. The planet radius and equilibrium temperature put Qatar-7b in the top 6% of the hottest and largest known exoplanets. With its large radius and high temperature, Qatar-7b is a valuable addition to the short list of targets that offer the best opportunity for studying their atmospheres through transmission spectroscopy.
Qatar Exoplanet Survey: Qatar-8b, 9b, and 10b—A Hot Saturn and Two Hot JupitersAlsubai, KhalidTsvetanov, Zlatan I.Pyrzas, StylianosLatham, David W.Bieryla, AllysonEastman, JasonMislis, DimitrisEsquerdo, Gilbert A.Southworth, JohnMancini, LuigiEsamdin, AliLiu, JinzhongMa, LuBretton, MarcPallé, EnricMurgas, FelipeVilchez, Nicolas P. E.Parviainien, HannuMontañes-Rodriguez, PilarNarita, NorioFukui, AkihikoKusakabe, NobuhikoTamura, MotohideBarkaoui, KhalidPozuelos, FranciscoGillon, MichaelJehin, EmmanuelBenkhaldoun, ZouhairDaassou, AhmedDOI: info:10.3847/1538-3881/ab19bcv. 157224
Alsubai, Khalid, Tsvetanov, Zlatan I., Pyrzas, Stylianos, Latham, David W., Bieryla, Allyson, Eastman, Jason, Mislis, Dimitris, Esquerdo, Gilbert A., Southworth, John, Mancini, Luigi, Esamdin, Ali, Liu, Jinzhong, Ma, Lu, Bretton, Marc, Pallé, Enric, Murgas, Felipe, Vilchez, Nicolas P. E., Parviainien, Hannu, Montañes-Rodriguez, Pilar, Narita, Norio, Fukui, Akihiko, Kusakabe, Nobuhiko, Tamura, Motohide, Barkaoui, Khalid, Pozuelos, Francisco et al. 2019. "Qatar Exoplanet Survey: Qatar-8b, 9b, and 10b—A Hot Saturn and Two Hot Jupiters." The Astronomical Journal 157:224. https://doi.org/10.3847/1538-3881/ab19bc
ID: 152879
Type: article
Authors: Alsubai, Khalid; Tsvetanov, Zlatan I.; Pyrzas, Stylianos; Latham, David W.; Bieryla, Allyson; Eastman, Jason; Mislis, Dimitris; Esquerdo, Gilbert A.; Southworth, John; Mancini, Luigi; Esamdin, Ali; Liu, Jinzhong; Ma, Lu; Bretton, Marc; Pallé, Enric; Murgas, Felipe; Vilchez, Nicolas P. E.; Parviainien, Hannu; Montañes-Rodriguez, Pilar; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Tamura, Motohide; Barkaoui, Khalid; Pozuelos, Francisco; Gillon, Michael; Jehin, Emmanuel; Benkhaldoun, Zouhair; Daassou, Ahmed
Abstract: In this paper we present three new extrasolar planets from the Qatar Exoplanet Survey. Qatar-8b is a hot Saturn, with M P = 0.37 M J and R P = 1.3 R J, orbiting a solar-like star every P orb = 3.7 days. Qatar-9b is a hot Jupiter with a mass of M P = 1.2 M J and a radius of R P = 1 R J, in an orbit of P orb = 1.5 days around a low mass, M ⋆ = 0.7 M ⊙, mid-K main-sequence star. Finally, Qatar-10b is a hot, T eq ∼ 2000 K, sub-Jupiter mass planet, M P = 0.7 M J, with a radius of R P = 1.54 R J and an orbital period of P orb = 1.6 days, placing it on the edge of the sub-Jupiter desert.
Type: article
Authors: Alsubai, Khalid; Tsvetanov, Zlatan I.; Pyrzas, Stylianos; Latham, David W.; Bieryla, Allyson; Eastman, Jason; Mislis, Dimitris; Esquerdo, Gilbert A.; Southworth, John; Mancini, Luigi; Esamdin, Ali; Liu, Jinzhong; Ma, Lu; Bretton, Marc; Pallé, Enric; Murgas, Felipe; Vilchez, Nicolas P. E.; Parviainien, Hannu; Montañes-Rodriguez, Pilar; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Tamura, Motohide; Barkaoui, Khalid; Pozuelos, Francisco; Gillon, Michael; Jehin, Emmanuel; Benkhaldoun, Zouhair; Daassou, Ahmed
Abstract: In this paper we present three new extrasolar planets from the Qatar Exoplanet Survey. Qatar-8b is a hot Saturn, with M P = 0.37 M J and R P = 1.3 R J, orbiting a solar-like star every P orb = 3.7 days. Qatar-9b is a hot Jupiter with a mass of M P = 1.2 M J and a radius of R P = 1 R J, in an orbit of P orb = 1.5 days around a low mass, M ⋆ = 0.7 M ⊙, mid-K main-sequence star. Finally, Qatar-10b is a hot, T eq ∼ 2000 K, sub-Jupiter mass planet, M P = 0.7 M J, with a radius of R P = 1.54 R J and an orbital period of P orb = 1.6 days, placing it on the edge of the sub-Jupiter desert.
Identifying Exoplanets with Deep Learning. II. Two New Super-Earths Uncovered by a Neural Network in K2 DataDattilo, AnneVanderburg, AndrewShallue, Christopher J.Mayo, Andrew W.Berlind, PerryBieryla, AllysonCalkins, Michael L.Esquerdo, Gilbert A.Everett, Mark E.Howell, Steve B.Latham, David W.Scott, Nicholas J.Yu, LiangDOI: info:10.3847/1538-3881/ab0e12v. 157169
Dattilo, Anne, Vanderburg, Andrew, Shallue, Christopher J., Mayo, Andrew W., Berlind, Perry, Bieryla, Allyson, Calkins, Michael L., Esquerdo, Gilbert A., Everett, Mark E., Howell, Steve B., Latham, David W., Scott, Nicholas J., and Yu, Liang. 2019. "Identifying Exoplanets with Deep Learning. II. Two New Super-Earths Uncovered by a Neural Network in K2 Data." The Astronomical Journal 157:169. https://doi.org/10.3847/1538-3881/ab0e12
ID: 151839
Type: article
Authors: Dattilo, Anne; Vanderburg, Andrew; Shallue, Christopher J.; Mayo, Andrew W.; Berlind, Perry; Bieryla, Allyson; Calkins, Michael L.; Esquerdo, Gilbert A.; Everett, Mark E.; Howell, Steve B.; Latham, David W.; Scott, Nicholas J.; Yu, Liang
Abstract: For years, scientists have used data from NASA’s Kepler Space Telescope to look for and discover thousands of transiting exoplanets. In its extended K2 mission, Kepler observed stars in various regions of the sky all across the ecliptic plane, and therefore in different galactic environments. Astronomers want to learn how the populations of exoplanets are different in these different environments. However, this requires an automatic and unbiased way to identify exoplanets in these regions and rule out false-positive signals that mimic transiting planet signals. We present a method for classifying these exoplanet signals using deep learning, a class of machine learning algorithms that have become popular in fields ranging from medical science to linguistics. We modified a neural network previously used to identify exoplanets in the Kepler field to be able to identify exoplanets in different K2 campaigns that exist in a range of galactic environments. We train a convolutional neural network, called AstroNet- K2, to predict whether a given possible exoplanet signal is really caused by an exoplanet or a false positive. AstroNet- K2 is highly successful at classifying exoplanets and false positives, with accuracy of 98% on our test set. It is especially efficient at identifying and culling false positives, but for now, it still needs human supervision to create a complete and reliable planet candidate sample. We use AstroNet- K2 to identify and validate two previously unknown exoplanets. Our method is a step toward automatically identifying new exoplanets in K2 data and learning how exoplanet populations depend on their galactic birthplace.
Type: article
Authors: Dattilo, Anne; Vanderburg, Andrew; Shallue, Christopher J.; Mayo, Andrew W.; Berlind, Perry; Bieryla, Allyson; Calkins, Michael L.; Esquerdo, Gilbert A.; Everett, Mark E.; Howell, Steve B.; Latham, David W.; Scott, Nicholas J.; Yu, Liang
Abstract: For years, scientists have used data from NASA’s Kepler Space Telescope to look for and discover thousands of transiting exoplanets. In its extended K2 mission, Kepler observed stars in various regions of the sky all across the ecliptic plane, and therefore in different galactic environments. Astronomers want to learn how the populations of exoplanets are different in these different environments. However, this requires an automatic and unbiased way to identify exoplanets in these regions and rule out false-positive signals that mimic transiting planet signals. We present a method for classifying these exoplanet signals using deep learning, a class of machine learning algorithms that have become popular in fields ranging from medical science to linguistics. We modified a neural network previously used to identify exoplanets in the Kepler field to be able to identify exoplanets in different K2 campaigns that exist in a range of galactic environments. We train a convolutional neural network, called AstroNet- K2, to predict whether a given possible exoplanet signal is really caused by an exoplanet or a false positive. AstroNet- K2 is highly successful at classifying exoplanets and false positives, with accuracy of 98% on our test set. It is especially efficient at identifying and culling false positives, but for now, it still needs human supervision to create a complete and reliable planet candidate sample. We use AstroNet- K2 to identify and validate two previously unknown exoplanets. Our method is a step toward automatically identifying new exoplanets in K2 data and learning how exoplanet populations depend on their galactic birthplace.
TOI-216b and TOI-216 c: Two Warm, Large Exoplanets in or Slightly Wide of the 2:1 Orbital ResonanceDawson, Rebekah I.Huang, Chelsea X.Lissauer, Jack J.Collins, Karen A.Sha, LizhouArmstrong, JamesConti, Dennis M.Collins, Kevin I.Evans, PhilGan, TianjunHorne, KeithIreland, MichaelMurgas, FelipeMyers, GordonRelles, Howard M.Sefako, RamotholoShporer, AviStockdale, ChrisŽerjal, MarušaZhou, GeorgeRicker, G.Vanderspek, R.Latham, David W.Seager, S.Winn, J.Jenkins, Jon M.Bouma, L. G.Caldwell, Douglas A.Daylan, TansuDoty, John P.Dynes, ScottEsquerdo, Gilbert A.Rose, MarkSmith, Jeffrey C.Yu, LiangDOI: info:10.3847/1538-3881/ab24bav. 15865
Dawson, Rebekah I., Huang, Chelsea X., Lissauer, Jack J., Collins, Karen A., Sha, Lizhou, Armstrong, James, Conti, Dennis M., Collins, Kevin I., Evans, Phil, Gan, Tianjun, Horne, Keith, Ireland, Michael, Murgas, Felipe, Myers, Gordon, Relles, Howard M., Sefako, Ramotholo, Shporer, Avi, Stockdale, Chris, Žerjal, Maruša, Zhou, George, Ricker, G., Vanderspek, R., Latham, David W., Seager, S., Winn, J. et al. 2019. "TOI-216b and TOI-216 c: Two Warm, Large Exoplanets in or Slightly Wide of the 2:1 Orbital Resonance." The Astronomical Journal 158:65. https://doi.org/10.3847/1538-3881/ab24ba
ID: 154240
Type: article
Authors: Dawson, Rebekah I.; Huang, Chelsea X.; Lissauer, Jack J.; Collins, Karen A.; Sha, Lizhou; Armstrong, James; Conti, Dennis M.; Collins, Kevin I.; Evans, Phil; Gan, Tianjun; Horne, Keith; Ireland, Michael; Murgas, Felipe; Myers, Gordon; Relles, Howard M.; Sefako, Ramotholo; Shporer, Avi; Stockdale, Chris; Žerjal, Maruša; Zhou, George; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, S.; Winn, J.; Jenkins, Jon M.; Bouma, L. G.; Caldwell, Douglas A.; Daylan, Tansu; Doty, John P.; Dynes, Scott; Esquerdo, Gilbert A.; Rose, Mark; Smith, Jeffrey C.; Yu, Liang
Abstract: Warm, large exoplanets with 10-100 day orbital periods pose a major challenge to our understanding of how planetary systems form and evolve. Although high eccentricity tidal migration has been invoked to explain their proximity to their host stars, a handful reside in or near orbital resonance with nearby planets, suggesting a gentler history of in situ formation or disk migration. Here we confirm and characterize a pair of warm, large exoplanets discovered by the TESS Mission orbiting K-dwarf TOI-216. Our analysis includes additional transits and transit exclusion windows observed via ground-based follow-up. We find two families of solutions, one corresponding to a sub-Saturn-mass planet accompanied by a Neptune-mass planet and the other to a Jupiter in resonance with a sub-Saturn-mass planet. We prefer the second solution based on the orbital period ratio, the planet radii, the lower free eccentricities, and libration of the 2:1 resonant argument, but cannot rule out the first. The free eccentricities and mutual inclination are compatible with stirring by other, undetected planets in the system, particularly for the second solution. We discuss prospects for better constraints on the planets' properties and orbits through follow-up, including transits observed from the ground.
Type: article
Authors: Dawson, Rebekah I.; Huang, Chelsea X.; Lissauer, Jack J.; Collins, Karen A.; Sha, Lizhou; Armstrong, James; Conti, Dennis M.; Collins, Kevin I.; Evans, Phil; Gan, Tianjun; Horne, Keith; Ireland, Michael; Murgas, Felipe; Myers, Gordon; Relles, Howard M.; Sefako, Ramotholo; Shporer, Avi; Stockdale, Chris; Žerjal, Maruša; Zhou, George; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, S.; Winn, J.; Jenkins, Jon M.; Bouma, L. G.; Caldwell, Douglas A.; Daylan, Tansu; Doty, John P.; Dynes, Scott; Esquerdo, Gilbert A.; Rose, Mark; Smith, Jeffrey C.; Yu, Liang
Abstract: Warm, large exoplanets with 10-100 day orbital periods pose a major challenge to our understanding of how planetary systems form and evolve. Although high eccentricity tidal migration has been invoked to explain their proximity to their host stars, a handful reside in or near orbital resonance with nearby planets, suggesting a gentler history of in situ formation or disk migration. Here we confirm and characterize a pair of warm, large exoplanets discovered by the TESS Mission orbiting K-dwarf TOI-216. Our analysis includes additional transits and transit exclusion windows observed via ground-based follow-up. We find two families of solutions, one corresponding to a sub-Saturn-mass planet accompanied by a Neptune-mass planet and the other to a Jupiter in resonance with a sub-Saturn-mass planet. We prefer the second solution based on the orbital period ratio, the planet radii, the lower free eccentricities, and libration of the 2:1 resonant argument, but cannot rule out the first. The free eccentricities and mutual inclination are compatible with stirring by other, undetected planets in the system, particularly for the second solution. We discuss prospects for better constraints on the planets' properties and orbits through follow-up, including transits observed from the ground.
KELT-22Ab: A Massive, Short-Period Hot Jupiter Transiting a Near-solar TwinLabadie-Bartz, JonathanRodriguez, Joseph E.Stassun, Keivan G.Ciardi, David R.Penev, KaloyanJohnson, Marshall C.Gaudi, B. ScottColón, Knicole D.Bieryla, AllysonLatham, David W.Pepper, JoshuaCollins, Karen A.Evans, PhilRelles, HowardSiverd, Robert J.Bento, JoaoYao, XinyuStockdale, ChrisTan, Thiam-GuanZhou, GeorgeEastman, Jason D.Albrow, Michael D.Bayliss, DanielBeatty, Thomas G.Berlind, PerryBozza, ValerioCalkins, Michael L.Cohen, David H.Curtis, Ivan A.Esquerdo, Gilbert A.Feliz, DaxFulton, Benjamin J.Gregorio, JoaoJames, DavidJensen, Eric L. N.Johnson, John AsherJohnson, Samson A.Joner, Michael D.Kasper, DavidKielkopf, John F.Kuhn, Rudolf B.Lund, Michael B.Malpas, AmberManner, MarkMcCrady, NateMcLeod, Kim K.Oberst, Thomas E.Penny, Matthew T.Reed, Phillip A.Sliski, David H.Stephens, Denise C.Stevens, Daniel J.Villanueva, Steven, Jr.Wittenmyer, Robert A.Wright, J. T.Zambelli, RobertoDOI: info:10.3847/1538-4365/aaee7ev. 24013
Labadie-Bartz, Jonathan, Rodriguez, Joseph E., Stassun, Keivan G., Ciardi, David R., Penev, Kaloyan, Johnson, Marshall C., Gaudi, B. Scott, Colón, Knicole D., Bieryla, Allyson, Latham, David W., Pepper, Joshua, Collins, Karen A., Evans, Phil, Relles, Howard, Siverd, Robert J., Bento, Joao, Yao, Xinyu, Stockdale, Chris, Tan, Thiam-Guan, Zhou, George, Eastman, Jason D., Albrow, Michael D., Bayliss, Daniel, Beatty, Thomas G., Berlind, Perry et al. 2019. "KELT-22Ab: A Massive, Short-Period Hot Jupiter Transiting a Near-solar Twin." The Astrophysical Journal Supplement Series 240:13. https://doi.org/10.3847/1538-4365/aaee7e
ID: 150442
Type: article
Authors: Labadie-Bartz, Jonathan; Rodriguez, Joseph E.; Stassun, Keivan G.; Ciardi, David R.; Penev, Kaloyan; Johnson, Marshall C.; Gaudi, B. Scott; Colón, Knicole D.; Bieryla, Allyson; Latham, David W.; Pepper, Joshua; Collins, Karen A.; Evans, Phil; Relles, Howard; Siverd, Robert J.; Bento, Joao; Yao, Xinyu; Stockdale, Chris; Tan, Thiam-Guan; Zhou, George; Eastman, Jason D.; Albrow, Michael D.; Bayliss, Daniel; Beatty, Thomas G.; Berlind, Perry; Bozza, Valerio; Calkins, Michael L.; Cohen, David H.; Curtis, Ivan A.; Esquerdo, Gilbert A.; Feliz, Dax; Fulton, Benjamin J.; Gregorio, Joao; James, David; Jensen, Eric L. N.; Johnson, John Asher; Johnson, Samson A.; Joner, Michael D.; Kasper, David; Kielkopf, John F.; Kuhn, Rudolf B.; Lund, Michael B.; Malpas, Amber; Manner, Mark; McCrady, Nate; McLeod, Kim K.; Oberst, Thomas E.; Penny, Matthew T.; Reed, Phillip A.; Sliski, David H.; Stephens, Denise C.; Stevens, Daniel J.; Villanueva, Steven, Jr.; Wittenmyer, Robert A.; Wright, J. T.; Zambelli, Roberto
Abstract: We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright (V ∼ 11.1) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of P =1.3866529+/- 0.0000027 days, a radius of {R}P={1.285}-0.071+0.12 {R}J, and a relatively large mass of {M}P={3.47}-0.14+0.15 {M}J. The star has {R}\star ={1.099}-0.046+0.079 {R}ȯ , {M}\star ={1.092}-0.041+0.045 {M}ȯ , {T}eff} ={5767}-49+50 K, {log}{g}\star ={4.393}-0.060+0.039 (cgs), and [m/H] = +{0.259}-0.083+0.085; thus other than its slightly super-solar metallicity, it appears to be a near-solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin-disk stars. Nevertheless, the star is rotating rapidly for its estimated age, and shows evidence of chromospheric activity. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6″ (∼1400 au). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A, suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semimajor axis of a/{R}\star =4.97), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semimajor axis is decreasing rapidly, and KELT-22Ab is predicted to spiral into the star within the next Gyr.
Type: article
Authors: Labadie-Bartz, Jonathan; Rodriguez, Joseph E.; Stassun, Keivan G.; Ciardi, David R.; Penev, Kaloyan; Johnson, Marshall C.; Gaudi, B. Scott; Colón, Knicole D.; Bieryla, Allyson; Latham, David W.; Pepper, Joshua; Collins, Karen A.; Evans, Phil; Relles, Howard; Siverd, Robert J.; Bento, Joao; Yao, Xinyu; Stockdale, Chris; Tan, Thiam-Guan; Zhou, George; Eastman, Jason D.; Albrow, Michael D.; Bayliss, Daniel; Beatty, Thomas G.; Berlind, Perry; Bozza, Valerio; Calkins, Michael L.; Cohen, David H.; Curtis, Ivan A.; Esquerdo, Gilbert A.; Feliz, Dax; Fulton, Benjamin J.; Gregorio, Joao; James, David; Jensen, Eric L. N.; Johnson, John Asher; Johnson, Samson A.; Joner, Michael D.; Kasper, David; Kielkopf, John F.; Kuhn, Rudolf B.; Lund, Michael B.; Malpas, Amber; Manner, Mark; McCrady, Nate; McLeod, Kim K.; Oberst, Thomas E.; Penny, Matthew T.; Reed, Phillip A.; Sliski, David H.; Stephens, Denise C.; Stevens, Daniel J.; Villanueva, Steven, Jr.; Wittenmyer, Robert A.; Wright, J. T.; Zambelli, Roberto
Abstract: We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright (V ∼ 11.1) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of P =1.3866529+/- 0.0000027 days, a radius of {R}P={1.285}-0.071+0.12 {R}J, and a relatively large mass of {M}P={3.47}-0.14+0.15 {M}J. The star has {R}\star ={1.099}-0.046+0.079 {R}ȯ , {M}\star ={1.092}-0.041+0.045 {M}ȯ , {T}eff} ={5767}-49+50 K, {log}{g}\star ={4.393}-0.060+0.039 (cgs), and [m/H] = +{0.259}-0.083+0.085; thus other than its slightly super-solar metallicity, it appears to be a near-solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin-disk stars. Nevertheless, the star is rotating rapidly for its estimated age, and shows evidence of chromospheric activity. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6″ (∼1400 au). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A, suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semimajor axis of a/{R}\star =4.97), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semimajor axis is decreasing rapidly, and KELT-22Ab is predicted to spiral into the star within the next Gyr.
A Second Terrestrial Planet Orbiting the Nearby M Dwarf LHS 1140Ment, KristoDittmann, Jason A.Astudillo-Defru, NicolaCharbonneau, DavidIrwin, JonathanBonfils, XavierMurgas, FelipeAlmenara, Jose-ManuelForveille, ThierryAgol, EricBallard, SarahBerta-Thompson, Zachory K.Bouchy, FrançoisCloutier, RyanDelfosse, XavierDoyon, RenéDressing, Courtney D.Esquerdo, Gilbert A.Haywood, Raphaëlle D.Kipping, David M.Latham, David W.Lovis, ChristopheNewton, Elisabeth R.Pepe, FrancescoRodriguez, Joseph E.Santos, Nuno C.Tan, Thiam-GuanUdry, StephaneWinters, Jennifer G.Wünsche, AnaëlDOI: info:10.3847/1538-3881/aaf1b1v. 15732
Ment, Kristo, Dittmann, Jason A., Astudillo-Defru, Nicola, Charbonneau, David, Irwin, Jonathan, Bonfils, Xavier, Murgas, Felipe, Almenara, Jose-Manuel, Forveille, Thierry, Agol, Eric, Ballard, Sarah, Berta-Thompson, Zachory K., Bouchy, François, Cloutier, Ryan, Delfosse, Xavier, Doyon, René, Dressing, Courtney D., Esquerdo, Gilbert A., Haywood, Raphaëlle D., Kipping, David M., Latham, David W., Lovis, Christophe, Newton, Elisabeth R., Pepe, Francesco, Rodriguez, Joseph E. et al. 2019. "A Second Terrestrial Planet Orbiting the Nearby M Dwarf LHS 1140." The Astronomical Journal 157:32. https://doi.org/10.3847/1538-3881/aaf1b1
ID: 150413
Type: article
Authors: Ment, Kristo; Dittmann, Jason A.; Astudillo-Defru, Nicola; Charbonneau, David; Irwin, Jonathan; Bonfils, Xavier; Murgas, Felipe; Almenara, Jose-Manuel; Forveille, Thierry; Agol, Eric; Ballard, Sarah; Berta-Thompson, Zachory K.; Bouchy, François; Cloutier, Ryan; Delfosse, Xavier; Doyon, René; Dressing, Courtney D.; Esquerdo, Gilbert A.; Haywood, Raphaëlle D.; Kipping, David M.; Latham, David W.; Lovis, Christophe; Newton, Elisabeth R.; Pepe, Francesco; Rodriguez, Joseph E.; Santos, Nuno C.; Tan, Thiam-Guan; Udry, Stephane; Winters, Jennifer G.; Wünsche, Anaël
Abstract: LHS 1140 is a nearby mid-M dwarf known to host a temperate rocky super-Earth (LHS 1140 b) on a 24.737-day orbit. Based on photometric observations by MEarth and Spitzer as well as Doppler spectroscopy from the High Accuracy Radial velocity Planet Searcher, we report the discovery of an additional transiting rocky companion (LHS 1140 c) with a mass of 1.81 ± 0.39 M ⊕ and a radius of 1.282 ± 0.024 R ⊕ on a tighter, 3.77795-day orbit. We also obtain more precise estimates for the mass and radius of LHS 1140 b, which are 6.98 ± 0.89 M ⊕ and 1.727 ± 0.032 R ⊕. The mean densities of planets b and c are 7.5 ± 1.0 g cm‑3 and 4.7 ± 1.1 g cm‑3, respectively, both consistent with the Earth’s ratio of iron to magnesium silicate. The orbital eccentricities of LHS 1140 b and c are consistent with circular orbits and constrained to be below 0.06 and 0.31, respectively, with 90% confidence. Because the orbits of the two planets are coplanar and because we know from previous analyses of Kepler data that compact systems of small planets orbiting M dwarfs are commonplace, a search for more transiting planets in the LHS 1140 system could be fruitful. LHS 1140 c is one of the few known nearby terrestrial planets whose atmosphere could be studied with the upcoming James Webb Space Telescope.
Type: article
Authors: Ment, Kristo; Dittmann, Jason A.; Astudillo-Defru, Nicola; Charbonneau, David; Irwin, Jonathan; Bonfils, Xavier; Murgas, Felipe; Almenara, Jose-Manuel; Forveille, Thierry; Agol, Eric; Ballard, Sarah; Berta-Thompson, Zachory K.; Bouchy, François; Cloutier, Ryan; Delfosse, Xavier; Doyon, René; Dressing, Courtney D.; Esquerdo, Gilbert A.; Haywood, Raphaëlle D.; Kipping, David M.; Latham, David W.; Lovis, Christophe; Newton, Elisabeth R.; Pepe, Francesco; Rodriguez, Joseph E.; Santos, Nuno C.; Tan, Thiam-Guan; Udry, Stephane; Winters, Jennifer G.; Wünsche, Anaël
Abstract: LHS 1140 is a nearby mid-M dwarf known to host a temperate rocky super-Earth (LHS 1140 b) on a 24.737-day orbit. Based on photometric observations by MEarth and Spitzer as well as Doppler spectroscopy from the High Accuracy Radial velocity Planet Searcher, we report the discovery of an additional transiting rocky companion (LHS 1140 c) with a mass of 1.81 ± 0.39 M ⊕ and a radius of 1.282 ± 0.024 R ⊕ on a tighter, 3.77795-day orbit. We also obtain more precise estimates for the mass and radius of LHS 1140 b, which are 6.98 ± 0.89 M ⊕ and 1.727 ± 0.032 R ⊕. The mean densities of planets b and c are 7.5 ± 1.0 g cm‑3 and 4.7 ± 1.1 g cm‑3, respectively, both consistent with the Earth’s ratio of iron to magnesium silicate. The orbital eccentricities of LHS 1140 b and c are consistent with circular orbits and constrained to be below 0.06 and 0.31, respectively, with 90% confidence. Because the orbits of the two planets are coplanar and because we know from previous analyses of Kepler data that compact systems of small planets orbiting M dwarfs are commonplace, a search for more transiting planets in the LHS 1140 system could be fruitful. LHS 1140 c is one of the few known nearby terrestrial planets whose atmosphere could be studied with the upcoming James Webb Space Telescope.
The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodicOsborn, H. P.Kenworthy, M.Rodriguez, J. E.de Mooij, E. J. W.Kennedy, G. M.Relles, H.Gomez, E.Hippke, M.Banfi, M.Barbieri, L.Becker, I. S.Benni, P.Berlind, P.Bieryla, A.Bonnoli, G.Boussier, H.Brincat, S. M.Briol, J.Burleigh, M. R.Butterley, T.Calkins, M. L.Chote, P.Ciceri, S.Deldem, M.Dhillon, V. S.Dose, E.Dubois, F.Dvorak, S.Esquerdo, G. A.Evans, D. F.Ferratfiat, S.Fossey, S. J.Günther, M. N.Hall, J.Hambsch, F. -JHerrero, E.Hills, K.James, R.Jayawardhana, R.Kafka, S.Killestein, T. L.Kotnik, C.Latham, D. W.Lemay, D.Lewin, P.Littlefair, S.Lopresti, C.Mallonn, M.Mancini, L.Marchini, A.McCormac, J. J.Murawski, G.Myers, G.Papini, R.Popov, V.Quadri, U.Quinn, S. N.Raynard, L.Rizzuti, L.Robertson, J.Salvaggio, F.Scholz, A.Sfair, R.Smith, A. M. S.Southworth, J.Tan, T. G.Vanaverbeke, S.Waagen, E. O.Watson, C. A.West, R. G.Winter, O. C.Wheatley, P. J.Wilson, R. W.Zhou, GeorgeDOI: info:10.1093/mnras/stz283v. 4851614–1625
Osborn, H. P., Kenworthy, M., Rodriguez, J. E., de Mooij, E. J. W., Kennedy, G. M., Relles, H., Gomez, E., Hippke, M., Banfi, M., Barbieri, L., Becker, I. S., Benni, P., Berlind, P., Bieryla, A., Bonnoli, G., Boussier, H., Brincat, S. M., Briol, J., Burleigh, M. R., Butterley, T., Calkins, M. L., Chote, P., Ciceri, S., Deldem, M., Dhillon, V. S. et al. 2019. "The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic." Monthly Notices of the Royal Astronomical Society 485:1614– 1625. https://doi.org/10.1093/mnras/stz283
ID: 151860
Type: article
Authors: Osborn, H. P.; Kenworthy, M.; Rodriguez, J. E.; de Mooij, E. J. W.; Kennedy, G. M.; Relles, H.; Gomez, E.; Hippke, M.; Banfi, M.; Barbieri, L.; Becker, I. S.; Benni, P.; Berlind, P.; Bieryla, A.; Bonnoli, G.; Boussier, H.; Brincat, S. M.; Briol, J.; Burleigh, M. R.; Butterley, T.; Calkins, M. L.; Chote, P.; Ciceri, S.; Deldem, M.; Dhillon, V. S.; Dose, E.; Dubois, F.; Dvorak, S.; Esquerdo, G. A.; Evans, D. F.; Ferratfiat, S.; Fossey, S. J.; Günther, M. N.; Hall, J.; Hambsch, F. -J; Herrero, E.; Hills, K.; James, R.; Jayawardhana, R.; Kafka, S.; Killestein, T. L.; Kotnik, C.; Latham, D. W.; Lemay, D.; Lewin, P.; Littlefair, S.; Lopresti, C.; Mallonn, M.; Mancini, L.; Marchini, A.; McCormac, J. J.; Murawski, G.; Myers, G.; Papini, R.; Popov, V.; Quadri, U.; Quinn, S. N.; Raynard, L.; Rizzuti, L.; Robertson, J.; Salvaggio, F.; Scholz, A.; Sfair, R.; Smith, A. M. S.; Southworth, J.; Tan, T. G.; Vanaverbeke, S.; Waagen, E. O.; Watson, C. A.; West, R. G.; Winter, O. C.; Wheatley, P. J.; Wilson, R. W.; Zhou, George
Abstract: PDS 110 is a young disc-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper, we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in 2017 September. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for radial velocity (RV) oscillations caused by any hypothetical companion and can rule out close binaries to 0.1Ms. A search of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 yr, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and of shorter duration than those of UX Ori variables, but may have a similar mechanism.
Type: article
Authors: Osborn, H. P.; Kenworthy, M.; Rodriguez, J. E.; de Mooij, E. J. W.; Kennedy, G. M.; Relles, H.; Gomez, E.; Hippke, M.; Banfi, M.; Barbieri, L.; Becker, I. S.; Benni, P.; Berlind, P.; Bieryla, A.; Bonnoli, G.; Boussier, H.; Brincat, S. M.; Briol, J.; Burleigh, M. R.; Butterley, T.; Calkins, M. L.; Chote, P.; Ciceri, S.; Deldem, M.; Dhillon, V. S.; Dose, E.; Dubois, F.; Dvorak, S.; Esquerdo, G. A.; Evans, D. F.; Ferratfiat, S.; Fossey, S. J.; Günther, M. N.; Hall, J.; Hambsch, F. -J; Herrero, E.; Hills, K.; James, R.; Jayawardhana, R.; Kafka, S.; Killestein, T. L.; Kotnik, C.; Latham, D. W.; Lemay, D.; Lewin, P.; Littlefair, S.; Lopresti, C.; Mallonn, M.; Mancini, L.; Marchini, A.; McCormac, J. J.; Murawski, G.; Myers, G.; Papini, R.; Popov, V.; Quadri, U.; Quinn, S. N.; Raynard, L.; Rizzuti, L.; Robertson, J.; Salvaggio, F.; Scholz, A.; Sfair, R.; Smith, A. M. S.; Southworth, J.; Tan, T. G.; Vanaverbeke, S.; Waagen, E. O.; Watson, C. A.; West, R. G.; Winter, O. C.; Wheatley, P. J.; Wilson, R. W.; Zhou, George
Abstract: PDS 110 is a young disc-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper, we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in 2017 September. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for radial velocity (RV) oscillations caused by any hypothetical companion and can rule out close binaries to 0.1Ms. A search of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 yr, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and of shorter duration than those of UX Ori variables, but may have a similar mechanism.
The Kepler Smear Campaign: Light Curves for 102 Very Bright StarsPope, Benjamin J. S.Davies, Guy R.Hawkins, KeithWhite, Timothy R.Stokholm, AmalieBieryla, AllysonLatham, David W.Lucey, MadelineAerts, ConnyAigrain, SuzanneAntoci, VictoriaBedding, Timothy R.Bowman, Dominic M.Caldwell, Douglas A.Chontos, AshleyEsquerdo, Gilbert A.Huber, DanielJofré, PaulaMurphy, Simon J.van Reeth, TimothySilva Aguirre, VictorYu, JieDOI: info:10.3847/1538-4365/ab2c04v. 24418
Pope, Benjamin J. S., Davies, Guy R., Hawkins, Keith, White, Timothy R., Stokholm, Amalie, Bieryla, Allyson, Latham, David W., Lucey, Madeline, Aerts, Conny, Aigrain, Suzanne, Antoci, Victoria, Bedding, Timothy R., Bowman, Dominic M., Caldwell, Douglas A., Chontos, Ashley, Esquerdo, Gilbert A., Huber, Daniel, Jofré, Paula, Murphy, Simon J., van Reeth, Timothy, Silva Aguirre, Victor, and Yu, Jie. 2019. "The Kepler Smear Campaign: Light Curves for 102 Very Bright Stars." The Astrophysical Journal Supplement Series 244:18. https://doi.org/10.3847/1538-4365/ab2c04
ID: 154448
Type: article
Authors: Pope, Benjamin J. S.; Davies, Guy R.; Hawkins, Keith; White, Timothy R.; Stokholm, Amalie; Bieryla, Allyson; Latham, David W.; Lucey, Madeline; Aerts, Conny; Aigrain, Suzanne; Antoci, Victoria; Bedding, Timothy R.; Bowman, Dominic M.; Caldwell, Douglas A.; Chontos, Ashley; Esquerdo, Gilbert A.; Huber, Daniel; Jofré, Paula; Murphy, Simon J.; van Reeth, Timothy; Silva Aguirre, Victor; Yu, Jie
Abstract: We present the first data release of the Kepler Smear Campaign, using collateral "smear" data obtained in the Kepler four-year mission to reconstruct light curves of 102 stars too bright to have been otherwise targeted. We describe the pipeline developed to extract and calibrate these light curves and show that we attain photometric precision comparable to stars analyzed by the standard pipeline in the nominal Kepler mission. In this paper, aside from publishing the light curves of these stars, we focus on 66 red giants for which we detect solar-like oscillations, characterizing 33 of these in detail with spectroscopic chemical abundances and asteroseismic masses as benchmark stars. We also classify the whole sample, finding nearly all to be variable, with classical pulsations and binary effects. All source code, light curves, Tillinghast Reflector Échelle Spectrograph spectra, and asteroseismic and stellar parameters are publicly available as a Kepler legacy sample.
Type: article
Authors: Pope, Benjamin J. S.; Davies, Guy R.; Hawkins, Keith; White, Timothy R.; Stokholm, Amalie; Bieryla, Allyson; Latham, David W.; Lucey, Madeline; Aerts, Conny; Aigrain, Suzanne; Antoci, Victoria; Bedding, Timothy R.; Bowman, Dominic M.; Caldwell, Douglas A.; Chontos, Ashley; Esquerdo, Gilbert A.; Huber, Daniel; Jofré, Paula; Murphy, Simon J.; van Reeth, Timothy; Silva Aguirre, Victor; Yu, Jie
Abstract: We present the first data release of the Kepler Smear Campaign, using collateral "smear" data obtained in the Kepler four-year mission to reconstruct light curves of 102 stars too bright to have been otherwise targeted. We describe the pipeline developed to extract and calibrate these light curves and show that we attain photometric precision comparable to stars analyzed by the standard pipeline in the nominal Kepler mission. In this paper, aside from publishing the light curves of these stars, we focus on 66 red giants for which we detect solar-like oscillations, characterizing 33 of these in detail with spectroscopic chemical abundances and asteroseismic masses as benchmark stars. We also classify the whole sample, finding nearly all to be variable, with classical pulsations and binary effects. All source code, light curves, Tillinghast Reflector Échelle Spectrograph spectra, and asteroseismic and stellar parameters are publicly available as a Kepler legacy sample.
A Hot Saturn Near (but Unassociated with) the Open Cluster NGC 1817Rampalli, RaynaVanderburg, AndrewBieryla, AllysonLatham, David W.Quinn, Samuel N.Baranec, ChristophBerlind, PerryCalkins, Michael L.Cochran, William D.Duev, Dmitry A.Endl, MichaelEsquerdo, Gilbert A.Jensen-Clem, RebeccaLaw, Nicholas M.Mayo, Andrew W.Riddle, ReedSalama, MaïssaDOI: info:10.3847/1538-3881/ab27c2v. 15862
Rampalli, Rayna, Vanderburg, Andrew, Bieryla, Allyson, Latham, David W., Quinn, Samuel N., Baranec, Christoph, Berlind, Perry, Calkins, Michael L., Cochran, William D., Duev, Dmitry A., Endl, Michael, Esquerdo, Gilbert A., Jensen-Clem, Rebecca, Law, Nicholas M., Mayo, Andrew W., Riddle, Reed, and Salama, Maïssa. 2019. "A Hot Saturn Near (but Unassociated with) the Open Cluster NGC 1817." The Astronomical Journal 158:62. https://doi.org/10.3847/1538-3881/ab27c2
ID: 154287
Type: article
Authors: Rampalli, Rayna; Vanderburg, Andrew; Bieryla, Allyson; Latham, David W.; Quinn, Samuel N.; Baranec, Christoph; Berlind, Perry; Calkins, Michael L.; Cochran, William D.; Duev, Dmitry A.; Endl, Michael; Esquerdo, Gilbert A.; Jensen-Clem, Rebecca; Law, Nicholas M.; Mayo, Andrew W.; Riddle, Reed; Salama, Maïssa
Abstract: We report on the discovery of a hot Saturn-sized planet (9.916 ± 0.985 R ⊕) around a late F-star, K2-308, observed in Campaign 13 of the K2 mission. We began studying this planet candidate because prior to the release of Gaia DR2, the host star was thought to have been a member (≥slant 90 % membership probability) of the ≈ 1 {Gyr} open cluster NGC 1817 based on its kinematics and photometric distance. We identify the host star (among three stars within the K2 photometric aperture) using seeing-limited photometry and rule out false-positive scenarios using adaptive optics imaging and radial velocity observations. We statistically validate K2-308b by calculating a false-positive probability rate of 0.01 % . However, we also show using new kinematic measurements provided by Gaia DR2 and our measured radial velocity of the system that K2-308 is unassociated with the cluster NGC 1817. Therefore, the long running search for a giant transiting planet in an open cluster remains fruitless. Finally, we note that our use of seeing-limited photometry is a good demonstration of similar techniques that are already being used to follow up Transiting Exoplanet Survey Satellite (TESS) planet candidates, especially in crowded regions.
Type: article
Authors: Rampalli, Rayna; Vanderburg, Andrew; Bieryla, Allyson; Latham, David W.; Quinn, Samuel N.; Baranec, Christoph; Berlind, Perry; Calkins, Michael L.; Cochran, William D.; Duev, Dmitry A.; Endl, Michael; Esquerdo, Gilbert A.; Jensen-Clem, Rebecca; Law, Nicholas M.; Mayo, Andrew W.; Riddle, Reed; Salama, Maïssa
Abstract: We report on the discovery of a hot Saturn-sized planet (9.916 ± 0.985 R ⊕) around a late F-star, K2-308, observed in Campaign 13 of the K2 mission. We began studying this planet candidate because prior to the release of Gaia DR2, the host star was thought to have been a member (≥slant 90 % membership probability) of the ≈ 1 {Gyr} open cluster NGC 1817 based on its kinematics and photometric distance. We identify the host star (among three stars within the K2 photometric aperture) using seeing-limited photometry and rule out false-positive scenarios using adaptive optics imaging and radial velocity observations. We statistically validate K2-308b by calculating a false-positive probability rate of 0.01 % . However, we also show using new kinematic measurements provided by Gaia DR2 and our measured radial velocity of the system that K2-308 is unassociated with the cluster NGC 1817. Therefore, the long running search for a giant transiting planet in an open cluster remains fruitless. Finally, we note that our use of seeing-limited photometry is a good demonstration of similar techniques that are already being used to follow up Transiting Exoplanet Survey Satellite (TESS) planet candidates, especially in crowded regions.