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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.
TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to InflationSha, LizhouHuang, Chelsea X.Shporer, AviRodriguez, Joseph E.Vanderburg, AndrewBrahm, RafaelHagelberg, JanisMatthews, Elisabeth C.Ziegler, CarlLivingston, John H.Stassun, Keivan G.Wright, Duncan J.Crane, Jeffrey D.Espinoza, NéstorBouchy, FrançoisBakos, Gáspár Á.Collins, Karen A.Zhou, GeorgeBieryla, AllysonHartman, Joel D.Wittenmyer, Robert A.Nielsen, Louise D.Plavchan, PeterBayliss, DanielSarkis, PaulaTan, Thiam-GuanCloutier, RyanMancini, LuigiJordán, AndrésWang, SharonHenning, ThomasNarita, NorioPenev, KaloyanTeske, Johanna K.Kane, Stephen R.Mann, Andrew W.Addison, Brett C.Tamura, MotohideHorner, JonathanBarbieri, MauroBurt, Jennifer A.Díaz, Matías R.Crossfield, Ian J. M.Dragomir, DianaDrass, HolgerFeinstein, Adina D.Zhang, HuiHart, RhodesKielkopf, John F.Jensen, Eric L. N.Montet, Benjamin T.Ottoni, GaëlSchwarz, Richard P.Rojas, FelipeNespral, DavidTorres, PascalMengel, Matthew W.Udry, StéphaneZapata, AbnerSnoddy, ErinOkumura, JackRicker, George R.Vanderspek, Roland K.Latham, David W.Winn, Joshua N.Seager, SaraJenkins, Jon M.Colón, Knicole D.Henze, Christopher E.Krishnamurthy, AkshataTing, Eric B.Vezie, MichaelVillanueva, StevenDOI: info:10.3847/1538-3881/abd187v. 16182
Sha, Lizhou, Huang, Chelsea X., Shporer, Avi, Rodriguez, Joseph E., Vanderburg, Andrew, Brahm, Rafael, Hagelberg, Janis, Matthews, Elisabeth C., Ziegler, Carl, Livingston, John H., Stassun, Keivan G., Wright, Duncan J., Crane, Jeffrey D., Espinoza, Néstor, Bouchy, François, Bakos, Gáspár Á., Collins, Karen A., Zhou, George, Bieryla, Allyson, Hartman, Joel D., Wittenmyer, Robert A., Nielsen, Louise D., Plavchan, Peter, Bayliss, Daniel, Sarkis, Paula et al. 2021. "TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to Inflation." The Astronomical Journal 161:82. https://doi.org/10.3847/1538-3881/abd187
ID: 159334
Type: article
Authors: Sha, Lizhou; Huang, Chelsea X.; Shporer, Avi; Rodriguez, Joseph E.; Vanderburg, Andrew; Brahm, Rafael; Hagelberg, Janis; Matthews, Elisabeth C.; Ziegler, Carl; Livingston, John H.; Stassun, Keivan G.; Wright, Duncan J.; Crane, Jeffrey D.; Espinoza, Néstor; Bouchy, François; Bakos, Gáspár Á.; Collins, Karen A.; Zhou, George; Bieryla, Allyson; Hartman, Joel D.; Wittenmyer, Robert A.; Nielsen, Louise D.; Plavchan, Peter; Bayliss, Daniel; Sarkis, Paula; Tan, Thiam-Guan; Cloutier, Ryan; Mancini, Luigi; Jordán, Andrés; Wang, Sharon; Henning, Thomas; Narita, Norio; Penev, Kaloyan; Teske, Johanna K.; Kane, Stephen R.; Mann, Andrew W.; Addison, Brett C.; Tamura, Motohide; Horner, Jonathan; Barbieri, Mauro; Burt, Jennifer A.; Díaz, Matías R.; Crossfield, Ian J. M.; Dragomir, Diana; Drass, Holger; Feinstein, Adina D.; Zhang, Hui; Hart, Rhodes; Kielkopf, John F.; Jensen, Eric L. N.; Montet, Benjamin T.; Ottoni, Gaël; Schwarz, Richard P.; Rojas, Felipe; Nespral, David; Torres, Pascal; Mengel, Matthew W.; Udry, Stéphane; Zapata, Abner; Snoddy, Erin; Okumura, Jack; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, Sara; Jenkins, Jon M.; Colón, Knicole D.; Henze, Christopher E.; Krishnamurthy, Akshata; Ting, Eric B.; Vezie, Michael; Villanueva, Steven
Abstract: We report the discovery of two short-period Saturn-mass planets, one transiting the G subgiant TOI-954 (TIC 44792534, V = 10.343, T = 9.78) observed in TESS sectors 4 and 5 and one transiting the G dwarf K2-329 (EPIC 246193072, V = 12.70, K = 10.67) observed in K2 campaigns 12 and 19. We confirm and characterize these two planets with a variety of ground-based archival and follow-up observations, including photometry, reconnaissance spectroscopy, precise radial velocity, and high-resolution imaging. Combining all available data, we find that TOI-954 b has a radius of ${0.852}_{-0.062}^{+0.053}\,{R}_{{\rm{J}}}$ and a mass of ${0.174}_{-0.017}^{+0.018}$ MJ and is in a 3.68 day orbit, while K2-329 b has a radius of ${0.774}_{-0.024}^{+0.026}\,{R}_{{\rm{J}}}$ and a mass of ${0.260}_{-0.022}^{+0.020}$ MJ and is in a 12.46 day orbit. As TOI-954 b is 30 times more irradiated than K2-329 b but more or less the same size, these two planets provide an opportunity to test whether irradiation leads to inflation of Saturn-mass planets and contribute to future comparative studies that explore Saturn-mass planets at contrasting points in their lifetimes.
Measured Lightcurves and Rotational Periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105Abrams, Natasha S.Bieryla, AllysonGomez, SebastianHuang, JaneLewis, John ArbanGarrison, Lehman H.Carmichael, Theronv. 473–4
Abrams, Natasha S., Bieryla, Allyson, Gomez, Sebastian, Huang, Jane, Lewis, John Arban, Garrison, Lehman H., and Carmichael, Theron. 2020. "Measured Lightcurves and Rotational Periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105." Minor Planet Bulletin 47:3– 4.
ID: 158251
Type: article
Authors: Abrams, Natasha S.; Bieryla, Allyson; Gomez, Sebastian; Huang, Jane; Lewis, John Arban; Garrison, Lehman H.; Carmichael, Theron
Abstract: We determined the rotational periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105 with the Harvard Clay Telescope and KeplerCam at the Fred L. Whipple Observatory. We found the rotational periods to be 2.3580 ± 0.0015 h, 17.059 ± 0.017 h, and 1.813 ± 0.00003 h, respectively. Our measurement of 3122 Florence's period agrees with Warner (2016), who reported 2.3580 ± 0.0002 h.
Measured Lightcurves and Rotational Periods of (16579) 1992 GO (25660) 2000 AO88, And (37652) 1994 JS1Abrams, Natasha S.Gomez, SebastianBieryla, Allysonv. 47168–169
Abrams, Natasha S., Gomez, Sebastian, and Bieryla, Allyson. 2020. "Measured Lightcurves and Rotational Periods of (16579) 1992 GO (25660) 2000 AO88, And (37652) 1994 JS1." Minor Planet Bulletin 47:168– 169.
ID: 158252
Type: article
Authors: Abrams, Natasha S.; Gomez, Sebastian; Bieryla, Allyson
Abstract: We determined the rotational periods of (16579) 1992 GO, (25660) 2000 AO88 and (37652) 1994 JS1, with the 1.2 m telescope at the Fred L. Whipple Observatory. We found the rotational periods to be 10.9887 ± 0.0004 h, 2.63705 ± 0.00004 h, and 17.4433 ± 0.0007 h, respectively. The former two were previously undetermined periods. The period that we determined for 1994 JS1 agrees well with the previously measured periods of 17.4501 ± 0.0014 (Noschese et al., 2019) and 17.459 ± 0.002 h (Marchini et al., 2019).
HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc AwayBadenas-Agusti, MarionaGünther, Maximilian N.Daylan, TansuMikal-Evans, ThomasVanderburg, AndrewHuang, Chelsea X.Matthews, ElisabethRackham, Benjamin V.Bieryla, AllysonStassun, Keivan G.Kane, Stephen R.Shporer, AviFulton, Benjamin J.Hill, Michelle L.Nowak, GrzegorzRibas, IgnasiPallé, EnricJenkins, Jon M.Latham, David W.Seager, SaraRicker, George R.Vanderspek, Roland K.Winn, Joshua N.Abril-Pla, OriolCollins, Karen A.Serra, Pere GuerraNiraula, PrajwalRustamkulov, ZafarBarclay, ThomasCrossfield, Ian J. M.Howell, Steve B.Ciardi, David R.Gonzales, Erica J.Schlieder, Joshua E.Caldwell, Douglas A.Fausnaugh, MichaelMcDermott, ScottPaegert, MartinPepper, JoshuaRose, Mark E.Twicken, Joseph D.DOI: info:10.3847/1538-3881/aba0b5v. 160113
Badenas-Agusti, Mariona, Günther, Maximilian N., Daylan, Tansu, Mikal-Evans, Thomas, Vanderburg, Andrew, Huang, Chelsea X., Matthews, Elisabeth, Rackham, Benjamin V., Bieryla, Allyson, Stassun, Keivan G., Kane, Stephen R., Shporer, Avi, Fulton, Benjamin J., Hill, Michelle L., Nowak, Grzegorz, Ribas, Ignasi, Pallé, Enric, Jenkins, Jon M., Latham, David W., Seager, Sara, Ricker, George R., Vanderspek, Roland K., Winn, Joshua N., Abril-Pla, Oriol, Collins, Karen A. et al. 2020. "HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc Away." The Astronomical Journal 160:113. https://doi.org/10.3847/1538-3881/aba0b5
ID: 158027
Type: article
Authors: Badenas-Agusti, Mariona; Günther, Maximilian N.; Daylan, Tansu; Mikal-Evans, Thomas; Vanderburg, Andrew; Huang, Chelsea X.; Matthews, Elisabeth; Rackham, Benjamin V.; Bieryla, Allyson; Stassun, Keivan G.; Kane, Stephen R.; Shporer, Avi; Fulton, Benjamin J.; Hill, Michelle L.; Nowak, Grzegorz; Ribas, Ignasi; Pallé, Enric; Jenkins, Jon M.; Latham, David W.; Seager, Sara; Ricker, George R.; Vanderspek, Roland K.; Winn, Joshua N.; Abril-Pla, Oriol; Collins, Karen A.; Serra, Pere Guerra; Niraula, Prajwal; Rustamkulov, Zafar; Barclay, Thomas; Crossfield, Ian J. M.; Howell, Steve B.; Ciardi, David R.; Gonzales, Erica J.; Schlieder, Joshua E.; Caldwell, Douglas A.; Fausnaugh, Michael; McDermott, Scott; Paegert, Martin; Pepper, Joshua; Rose, Mark E.; Twicken, Joseph D.
Abstract: We present the discovery of three sub-Neptune-sized planets transiting the nearby and bright Sun-like star HD 191939 (TIC 269701147, TOI 1339), a Ks = 7.18 mag G8 V dwarf at a distance of only 54 pc. We validate the planetary nature of the transit signals by combining 5 months of data from the Transiting Exoplanet Survey Satellite with follow-up ground-based photometry, archival optical images, radial velocities, and high angular resolution observations. The three sub-Neptunes have similar radii ( ${R}_{{\rm{b}}}={3.42}_{-0.11}^{+0.11}$ , ${R}_{{\rm{c}}}={3.23}_{-0.11}^{+0.11}$ , and ${R}_{{\rm{d}}}={3.16}_{-0.11}^{+0.11}\,{R}_{\oplus }$ ), and their orbits are consistent with a stable, circular, and coplanar architecture near mean-motion resonances of 1:3 and 3:4 (Pb = 8.88, Pc = 28.58, and Pd = 38.35 days). The HD 191939 system is an excellent candidate for precise mass determinations of the planets with high-resolution spectroscopy due to the host star's brightness and low chromospheric activity. Moreover, the system's compact and near-resonant nature can provide an independent way to measure planetary masses via transit timing variations while also enabling dynamical and evolutionary studies. Finally, as a promising target for multiwavelength transmission spectroscopy of all three planets' atmospheres, HD 191939 can offer valuable insight into multiple sub-Neptunes born from a protoplanetary disk that may have resembled that of the early Sun.
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.
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.
A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266Demory, B. -OPozuelos, F. J.Gómez Maqueo Chew, Y.Sabin, L.Petrucci, R.Schroffenegger, U.Grimm, S. L.Sestovic, M.Gillon, M.McCormac, J.Barkaoui, K.Benz, W.Bieryla, AllysonBouchy, F.Burdanov, A.Collins, Karen A.de Wit, J.Dressing, C. D.Garcia, L. J.Giacalone, S.Guerra, P.Haldemann, J.Heng, K.Jehin, E.Jofré, E.Kane, S. R.Lillo-Box, J.Maigné, V.Mordasini, C.Morris, B. M.Niraula, P.Queloz, D.Rackham, B. V.Savel, A. B.Soubkiou, A.Srdoc, G.Stassun, K. G.Triaud, A. H. M. J.Zambelli, R.Ricker, G.Latham, David W.Seager, S.Winn, J. N.Jenkins, J. M.Calvario-Velásquez, T.Franco Herrera, J. A.Colorado, E.Cadena Zepeda, E. O.Figueroa, L.Watson, A. M.Lugo-Ibarra, E. E.Carigi, L.Guisa, G.Herrera, J.Sierra Díaz, G.Suárez, J. C.Barrado, D.Batalha, N. M.Benkhaldoun, Z.Chontos, A.Dai, F.Essack, Z.Ghachoui, M.Huang, C. X.Huber, D.Isaacson, H.Lissauer, J. J.Morales-Calderón, M.Robertson, P.Roy, A.Twicken, J. D.Vanderburg, A.Weiss, L. M.DOI: info:10.1051/0004-6361/202038616v. 642A49
Demory, B. -O, Pozuelos, F. J., Gómez Maqueo Chew, Y., Sabin, L., Petrucci, R., Schroffenegger, U., Grimm, S. L., Sestovic, M., Gillon, M., McCormac, J., Barkaoui, K., Benz, W., Bieryla, Allyson, Bouchy, F., Burdanov, A., Collins, Karen A., de Wit, J., Dressing, C. D., Garcia, L. J., Giacalone, S., Guerra, P., Haldemann, J., Heng, K., Jehin, E., Jofré, E. et al. 2020. "A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266." Astronomy and Astrophysics 642:A49. https://doi.org/10.1051/0004-6361/202038616
ID: 157579
Type: article
Authors: Demory, B. -O; Pozuelos, F. J.; Gómez Maqueo Chew, Y.; Sabin, L.; Petrucci, R.; Schroffenegger, U.; Grimm, S. L.; Sestovic, M.; Gillon, M.; McCormac, J.; Barkaoui, K.; Benz, W.; Bieryla, Allyson; Bouchy, F.; Burdanov, A.; Collins, Karen A.; de Wit, J.; Dressing, C. D.; Garcia, L. J.; Giacalone, S.; Guerra, P.; Haldemann, J.; Heng, K.; Jehin, E.; Jofré, E.; Kane, S. R.; Lillo-Box, J.; Maigné, V.; Mordasini, C.; Morris, B. M.; Niraula, P.; Queloz, D.; Rackham, B. V.; Savel, A. B.; Soubkiou, A.; Srdoc, G.; Stassun, K. G.; Triaud, A. H. M. J.; Zambelli, R.; Ricker, G.; Latham, David W.; Seager, S.; Winn, J. N.; Jenkins, J. M.; Calvario-Velásquez, T.; Franco Herrera, J. A.; Colorado, E.; Cadena Zepeda, E. O.; Figueroa, L.; Watson, A. M.; Lugo-Ibarra, E. E.; Carigi, L.; Guisa, G.; Herrera, J.; Sierra Díaz, G.; Suárez, J. C.; Barrado, D.; Batalha, N. M.; Benkhaldoun, Z.; Chontos, A.; Dai, F.; Essack, Z.; Ghachoui, M.; Huang, C. X.; Huber, D.; Isaacson, H.; Lissauer, J. J.; Morales-Calderón, M.; Robertson, P.; Roy, A.; Twicken, J. D.; Vanderburg, A.; Weiss, L. M.
Abstract: We report the discovery and characterisation of a super-Earth and a sub-Neptune transiting the bright (K = 8.8), quiet, and nearby (37 pc) M3V dwarf TOI-1266. We validate the planetary nature of TOI-1266 b and c using four sectors of TESS photometry and data from the newly-commissioned 1-m SAINT-EX telescope located in San Pedro Mártir (México). We also include additional ground-based follow-up photometry as well as high-resolution spectroscopy and high-angular imaging observations. The inner, larger planet has a radius of R = 2.37-0.12+0.16 R and an orbital period of 10.9 days. The outer, smaller planet has a radius of R = 1.56-0.13+0.15 R on an 18.8-day orbit. The data are found to be consistent with circular, co-planar and stable orbits that are weakly influenced by the 2:1 mean motion resonance. Our TTV analysis of the combined dataset enables model-independent constraints on the masses and eccentricities of the planets. We find planetary masses of Mp = 13.5-9.0+11.0 M ( ( at 2-σ) for TOI-1266 b and 2.2-1.5+2.0 M ( ( at 2-σ) for TOI-1266 c. We find small but non-zero orbital eccentricities of 0.09-0.05+0.06 (<0.21 at 2-σ) for TOI-1266 b and 0.04 ± 0.03 (< 0.10 at 2-σ) for TOI-1266 c. The equilibrium temperatures of both planets are of 413 ± 20 and 344 ± 16 K, respectively, assuming a null Bond albedo and uniform heat redistribution from the day-side to the night-side hemisphere. The host brightness and negligible activity combined with the planetary system architecture and favourable planet-to-star radii ratios makes TOI-1266 an exquisite system for a detailed characterisation.
The K2 and TESS Synergy. I. Updated Ephemerides and Parameters for K2-114, K2-167, K2-237, and K2-261Ikwut-Ukwa, MmaRodriguez, Joseph E.Bieryla, AllysonVanderburg, AndrewMocnik, TeoKane, Stephen R.Quinn, Samuel N.Colón, Knicole D.Zhou, GeorgeEastman, Jason D.Huang, Chelsea X.Latham, David W.Dotson, JessieJenkins, Jon M.Ricker, George R.Seager, SaraVanderspek, Roland K.Winn, Joshua N.Barclay, ThomasBarentsen, GeertBerta-Thompson, ZachoryCharbonneau, DavidDragomir, DianaDaylan, TansuGünther, Maximilian N.Hedges, ChristinaHenze, Christopher E.McDermott, ScottSchlieder, Joshua E.Quintana, Elisa V.Smith, Jeffrey C.Twicken, Joseph D.Yahalomi, Daniel A.DOI: info:10.3847/1538-3881/aba964v. 160209
Ikwut-Ukwa, Mma, Rodriguez, Joseph E., Bieryla, Allyson, Vanderburg, Andrew, Mocnik, Teo, Kane, Stephen R., Quinn, Samuel N., Colón, Knicole D., Zhou, George, Eastman, Jason D., Huang, Chelsea X., Latham, David W., Dotson, Jessie, Jenkins, Jon M., Ricker, George R., Seager, Sara, Vanderspek, Roland K., Winn, Joshua N., Barclay, Thomas, Barentsen, Geert, Berta-Thompson, Zachory, Charbonneau, David, Dragomir, Diana, Daylan, Tansu, Günther, Maximilian N. et al. 2020. "The K2 and TESS Synergy. I. Updated Ephemerides and Parameters for K2-114, K2-167, K2-237, and K2-261." The Astronomical Journal 160:209. https://doi.org/10.3847/1538-3881/aba964
ID: 158655
Type: article
Authors: Ikwut-Ukwa, Mma; Rodriguez, Joseph E.; Bieryla, Allyson; Vanderburg, Andrew; Mocnik, Teo; Kane, Stephen R.; Quinn, Samuel N.; Colón, Knicole D.; Zhou, George; Eastman, Jason D.; Huang, Chelsea X.; Latham, David W.; Dotson, Jessie; Jenkins, Jon M.; Ricker, George R.; Seager, Sara; Vanderspek, Roland K.; Winn, Joshua N.; Barclay, Thomas; Barentsen, Geert; Berta-Thompson, Zachory; Charbonneau, David; Dragomir, Diana; Daylan, Tansu; Günther, Maximilian N.; Hedges, Christina; Henze, Christopher E.; McDermott, Scott; Schlieder, Joshua E.; Quintana, Elisa V.; Smith, Jeffrey C.; Twicken, Joseph D.; Yahalomi, Daniel A.
Abstract: Although the Transiting Exoplanet Survey Satellite (TESS) primary mission observed the northern and southern ecliptic hemispheres, generally avoiding the ecliptic, and the Kepler space telescope during the K2 mission could only observe near the ecliptic, many of the K2 fields extend far enough from the ecliptic plane that sections overlap with TESS fields. Using photometric observations from both K2 and TESS, combined with archival spectroscopic observations, we globally modeled four known planetary systems discovered by K2 that were observed in the first year of the primary TESS mission. Specifically, we provide updated ephemerides and system parameters for K2-114 b, K2-167 b, K2-237 b, and K2-261 b. These were some of the first K2 planets to be observed by TESS in the first year and include three Jovian sized planets and a sub-Neptune with orbital periods less than 12 days. In each case, the updated ephemeris significantly reduces the uncertainty in prediction of future times of transit, which is valuable for planning observations with the James Webb Space Telescope and other future facilities. The TESS extended mission is expected to observe about half of the K2 fields, providing the opportunity to perform this type of analysis on a larger number of systems.
An ultrahot Neptune in the Neptune desertJenkins, James S.Díaz, Matías R.Kurtovic, Nicolás T.Espinoza, NéstorVines, Jose I.Rojas, Pablo A. PeñaBrahm, RafaelTorres, PascalCortés-Zuleta, PíaSoto, Maritza G.Lopez, Eric D.King, George W.Wheatley, Peter J.Winn, Joshua N.Ciardi, David R.Ricker, GeorgeVanderspek, RolandLatham, David W.Seager, SaraJenkins, Jon M.Beichman, Charles A.Bieryla, AllysonBurke, Christopher J.Christiansen, Jessie L.Henze, Christopher E.Klaus, Todd C.McCauliff, SeanMori, MayukoNarita, NorioNishiumi, TakuTamura, Motohidede Leon, Jerome PitogoQuinn, Samuel N.Villaseñor, Jesus NoelVezie, MichaelLissauer, Jack J.Collins, Karen A.Collins, Kevin I.Isopi, GiovanniMallia, FrancoErcolino, AndreaPetrovich, CristobalJordán, AndrésActon, Jack S.Armstrong, David J.Bayliss, DanielBouchy, FrançoisBelardi, ClaudiaBryant, Edward M.Burleigh, Matthew R.Cabrera, JuanCasewell, Sarah L.Chaushev, AlexanderCooke, Benjamin F.Eigmüller, PhilippErikson, AndersFoxell, EmmaGänsicke, Boris T.Gill, SamuelGillen, EdwardGünther, Maximilian N.Goad, Michael R.Hooton, Matthew J.Jackman, James A. G.Louden, TomMcCormac, JamesMoyano, MaximilianoNielsen, Louise D.Pollacco, DonQueloz, DidierRauer, HeikeRaynard, LiamSmith, Alexis M. S.Tilbrook, Rosanna H.Titz-Weider, RuthTurner, OliverUdry, StéphaneWalker, Simon R.Watson, Christopher A.West, Richard G.Palle, EnricZiegler, CarlLaw, NicholasMann, Andrew W.DOI: info:10.1038/s41550-020-1142-zv. 41148–1157
Jenkins, James S., Díaz, Matías R., Kurtovic, Nicolás T., Espinoza, Néstor, Vines, Jose I., Rojas, Pablo A. Peña, Brahm, Rafael, Torres, Pascal, Cortés-Zuleta, Pía, Soto, Maritza G., Lopez, Eric D., King, George W., Wheatley, Peter J., Winn, Joshua N., Ciardi, David R., Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Jenkins, Jon M., Beichman, Charles A., Bieryla, Allyson, Burke, Christopher J., Christiansen, Jessie L., Henze, Christopher E. et al. 2020. "An ultrahot Neptune in the Neptune desert." Nature Astronomy 4:1148– 1157. https://doi.org/10.1038/s41550-020-1142-z
ID: 158870
Type: article
Authors: Jenkins, James S.; Díaz, Matías R.; Kurtovic, Nicolás T.; Espinoza, Néstor; Vines, Jose I.; Rojas, Pablo A. Peña; Brahm, Rafael; Torres, Pascal; Cortés-Zuleta, Pía; Soto, Maritza G.; Lopez, Eric D.; King, George W.; Wheatley, Peter J.; Winn, Joshua N.; Ciardi, David R.; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Jenkins, Jon M.; Beichman, Charles A.; Bieryla, Allyson; Burke, Christopher J.; Christiansen, Jessie L.; Henze, Christopher E.; Klaus, Todd C.; McCauliff, Sean; Mori, Mayuko; Narita, Norio; Nishiumi, Taku; Tamura, Motohide; de Leon, Jerome Pitogo; Quinn, Samuel N.; Villaseñor, Jesus Noel; Vezie, Michael; Lissauer, Jack J.; Collins, Karen A.; Collins, Kevin I.; Isopi, Giovanni; Mallia, Franco; Ercolino, Andrea; Petrovich, Cristobal; Jordán, Andrés; Acton, Jack S.; Armstrong, David J.; Bayliss, Daniel; Bouchy, François; Belardi, Claudia; Bryant, Edward M.; Burleigh, Matthew R.; Cabrera, Juan; Casewell, Sarah L.; Chaushev, Alexander; Cooke, Benjamin F.; Eigmüller, Philipp; Erikson, Anders; Foxell, Emma; Gänsicke, Boris T.; Gill, Samuel; Gillen, Edward; Günther, Maximilian N.; Goad, Michael R.; Hooton, Matthew J.; Jackman, James A. G.; Louden, Tom; McCormac, James; Moyano, Maximiliano; Nielsen, Louise D.; Pollacco, Don; Queloz, Didier; Rauer, Heike; Raynard, Liam; Smith, Alexis M. S.; Tilbrook, Rosanna H.; Titz-Weider, Ruth; Turner, Oliver; Udry, Stéphane; Walker, Simon R.; Watson, Christopher A.; West, Richard G.; Palle, Enric; Ziegler, Carl; Law, Nicholas; Mann, Andrew W.
Abstract: About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R?), or apparently rocky planets smaller than 2 R?. Such lack of planets of intermediate size (the `hot Neptune desert') has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R? and a mass of 29 M?, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0-2.9+2.7?% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this `ultrahot Neptune' managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag = 9.8).
An extremely energetic supernova from a very massive star in a dense mediumNicholl, MattBlanchard, Peter K.Berger, EdoChornock, RyanMargutti, RaffaellaGomez, SebastianLunnan, RagnhildMiller, Adam A.Fong, Wen-faiTerreran, GiacomoVigna-Gómez, AlejandroBhirombhakdi, KornpobBieryla, AllysonChallis, PeteLaher, Russ R.Masci, Frank J.Paterson, KerryDOI: info:10.1038/s41550-020-1066-7v. 4893–899
Nicholl, Matt, Blanchard, Peter K., Berger, Edo, Chornock, Ryan, Margutti, Raffaella, Gomez, Sebastian, Lunnan, Ragnhild, Miller, Adam A., Fong, Wen-fai, Terreran, Giacomo, Vigna-Gómez, Alejandro, Bhirombhakdi, Kornpob, Bieryla, Allyson, Challis, Pete, Laher, Russ R., Masci, Frank J., and Paterson, Kerry. 2020. "An extremely energetic supernova from a very massive star in a dense medium." Nature Astronomy 4:893– 899. https://doi.org/10.1038/s41550-020-1066-7
ID: 158742
Type: article
Authors: Nicholl, Matt; Blanchard, Peter K.; Berger, Edo; Chornock, Ryan; Margutti, Raffaella; Gomez, Sebastian; Lunnan, Ragnhild; Miller, Adam A.; Fong, Wen-fai; Terreran, Giacomo; Vigna-Gómez, Alejandro; Bhirombhakdi, Kornpob; Bieryla, Allyson; Challis, Pete; Laher, Russ R.; Masci, Frank J.; Paterson, Kerry
Abstract: The interaction of a supernova with a circumstellar medium (CSM) can dramatically increase the emitted luminosity by converting kinetic energy to thermal energy. In `superluminous' supernovae of type IIn-named for narrow hydrogen lines1 in their spectra-the integrated emission can reach2-6 ~1051 erg, attainable by thermalizing most of the kinetic energy of a conventional supernova. A few transients in the centres of active galaxies have shown similar spectra and even larger energies7,8, but are difficult to distinguish from accretion onto the supermassive black hole. Here we present a new event, SN2016aps, offset from the centre of a low-mass galaxy, that radiated ?5 × 1051 erg, necessitating a hyper-energetic supernova explosion. We find a total (supernova ejecta + CSM) mass likely exceeding 50-100 M?, with energy ?1052 erg, consistent with some models of pair-instability supernovae or pulsational pair-instability supernovae-theoretically predicted thermonuclear explosions from helium cores >50 M?. Independent of the explosion mechanism, this event demonstrates the existence of extremely energetic stellar explosions, detectable at very high redshifts, and provides insight into dense CSM formation in the most massive stars.
KELT-25 b and KELT-26 b: A Hot Jupiter and a Substellar Companion Transiting Young A Stars Observed by TESSRodríguez Martínez, RomyGaudi, B. ScottRodriguez, Joseph E.Zhou, GeorgeLabadie-Bartz, JonathanQuinn, Samuel N.Penev, KaloyanTan, Thiam-GuanLatham, David W.Paredes, Leonardo A.Kielkopf, John F.Addison, BrettWright, Duncan J.Teske, JohannaHowell, Steve B.Ciardi, DavidZiegler, CarlStassun, Keivan G.Johnson, Marshall C.Eastman, Jason D.Siverd, Robert J.Beatty, Thomas G.Bouma, LukeBedding, TimothyPepper, JoshuaWinn, JoshuaLund, Michael B.Villanueva, Steven, Jr.Stevens, Daniel J.Jensen, Eric L. N.Kilby, ColemanCrane, Jeffrey D.Tokovinin, AndreiEverett, Mark E.Tinney, C. G.Fausnaugh, MichaelCohen, David H.Bayliss, DanielBieryla, AllysonCargile, Phillip A.Collins, Karen A.Conti, Dennis M.Colón, Knicole D.Curtis, Ivan A.DePoy, D. L.Evans, PhilFeliz, Dax L.Gregorio, JoaoRothenberg, JasonJames, David J.Joner, Michael D.Kuhn, Rudolf B.Manner, MarkKhakpash, SomayehMarshall, Jennifer L.McLeod, Kim K.Penny, Matthew T.Reed, Phillip A.Relles, Howard M.Stephens, Denise C.Stockdale, ChrisTrueblood, MarkTrueblood, PatYao, XinyuZambelli, RobertoVanderspek, RolandSeager, SaraJenkins, Jon M.Henry, Todd J.James, Hodari-SadikiJao, Wei-ChunWang, Sharon XuesongButler, PaulThompson, IanShectman, StephenWittenmyer, RobertBowler, Brendan P.Horner, JonathanKane, Stephen R.Mengel, Matthew W.Morton, Timothy D.Okumura, JackPlavchan, PeterZhang, HuiScott, Nicholas J.Matson, Rachel A.Mann, Andrew W.Dragomir, DianaGünther, MaxTing, Eric B.Glidden, AnaQuintana, Elisa V.DOI: info:10.3847/1538-3881/ab9f2dv. 160111
Rodríguez Martínez, Romy, Gaudi, B. Scott, Rodriguez, Joseph E., Zhou, George, Labadie-Bartz, Jonathan, Quinn, Samuel N., Penev, Kaloyan, Tan, Thiam-Guan, Latham, David W., Paredes, Leonardo A., Kielkopf, John F., Addison, Brett, Wright, Duncan J., Teske, Johanna, Howell, Steve B., Ciardi, David, Ziegler, Carl, Stassun, Keivan G., Johnson, Marshall C., Eastman, Jason D., Siverd, Robert J., Beatty, Thomas G., Bouma, Luke, Bedding, Timothy, Pepper, Joshua et al. 2020. "KELT-25 b and KELT-26 b: A Hot Jupiter and a Substellar Companion Transiting Young A Stars Observed by TESS." The Astronomical Journal 160:111. https://doi.org/10.3847/1538-3881/ab9f2d
ID: 157580
Type: article
Authors: Rodríguez Martínez, Romy; Gaudi, B. Scott; Rodriguez, Joseph E.; Zhou, George; Labadie-Bartz, Jonathan; Quinn, Samuel N.; Penev, Kaloyan; Tan, Thiam-Guan; Latham, David W.; Paredes, Leonardo A.; Kielkopf, John F.; Addison, Brett; Wright, Duncan J.; Teske, Johanna; Howell, Steve B.; Ciardi, David; Ziegler, Carl; Stassun, Keivan G.; Johnson, Marshall C.; Eastman, Jason D.; Siverd, Robert J.; Beatty, Thomas G.; Bouma, Luke; Bedding, Timothy; Pepper, Joshua; Winn, Joshua; Lund, Michael B.; Villanueva, Steven, Jr.; Stevens, Daniel J.; Jensen, Eric L. N.; Kilby, Coleman; Crane, Jeffrey D.; Tokovinin, Andrei; Everett, Mark E.; Tinney, C. G.; Fausnaugh, Michael; Cohen, David H.; Bayliss, Daniel; Bieryla, Allyson; Cargile, Phillip A.; Collins, Karen A.; Conti, Dennis M.; Colón, Knicole D.; Curtis, Ivan A.; DePoy, D. L.; Evans, Phil; Feliz, Dax L.; Gregorio, Joao; Rothenberg, Jason; James, David J.; Joner, Michael D.; Kuhn, Rudolf B.; Manner, Mark; Khakpash, Somayeh; Marshall, Jennifer L.; McLeod, Kim K.; Penny, Matthew T.; Reed, Phillip A.; Relles, Howard M.; Stephens, Denise C.; Stockdale, Chris; Trueblood, Mark; Trueblood, Pat; Yao, Xinyu; Zambelli, Roberto; Vanderspek, Roland; Seager, Sara; Jenkins, Jon M.; Henry, Todd J.; James, Hodari-Sadiki; Jao, Wei-Chun; Wang, Sharon Xuesong; Butler, Paul; Thompson, Ian; Shectman, Stephen; Wittenmyer, Robert; Bowler, Brendan P.; Horner, Jonathan; Kane, Stephen R.; Mengel, Matthew W.; Morton, Timothy D.; Okumura, Jack; Plavchan, Peter; Zhang, Hui; Scott, Nicholas J.; Matson, Rachel A.; Mann, Andrew W.; Dragomir, Diana; Günther, Max; Ting, Eric B.; Glidden, Ana; Quintana, Elisa V.
Abstract: We present the discoveries of KELT-25 b (TIC 65412605, TOI-626.01) and KELT-26 b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A stars. The transit signals were initially detected by the KELT survey and subsequently confirmed by Transiting Exoplanet Survey Satellite (TESS) photometry. KELT-25 b is on a 4.40 day orbit around the V = 9.66 star CD-24 5016 ( ${T}_{\mathrm{eff}}={8280}_{-180}^{+440}$ K, M = ${2.18}_{-0.11}^{+0.12}$ M), while KELT-26 b is on a 3.34 day orbit around the V = 9.95 star HD 134004 ( ${T}_{\mathrm{eff}}$ = ${8640}_{-240}^{+500}$ K, M = ${1.93}_{-0.16}^{+0.14}$ M), which is likely an Am star. We have confirmed the substellar nature of both companions through detailed characterization of each system using ground-based and TESS photometry, radial velocity measurements, Doppler tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of RP = ${1.64}_{-0.043}^{+0.039}$ RJ and a 3σ upper limit on the companion's mass of ∼64 MJ. For KELT-26 b, we infer a planetary mass and radius of MP = ${1.41}_{-0.51}^{+0.43}$ ${M}_{{\rm{J}}}$ and RP = ${1.94}_{-0.058}^{+0.060}$ RJ. From Doppler tomographic observations, we find KELT-26 b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the TESS data. KELT-25 b appears to be in a well-aligned, prograde orbit, and the system is likely a member of the cluster Theia 449. * This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
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.
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.
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.
The Curious Case of KOI 4: Confirming Kepler’s First Exoplanet DetectionChontos, AshleyHuber, DanielLatham, David W.Bieryla, AllysonVan Eylen, VincentBedding, Timothy R.Berger, TravisBuchhave, Lars A.Campante, Tiago L.Chaplin, William J.Colman, Isabel L.Coughlin, Jeff L.Davies, GuyHirano, TeruyukiHoward, Andrew W.Isaacson, HowardDOI: info:10.3847/1538-3881/ab0e8ev. 157192
Chontos, Ashley, Huber, Daniel, Latham, David W., Bieryla, Allyson, Van Eylen, Vincent, Bedding, Timothy R., Berger, Travis, Buchhave, Lars A., Campante, Tiago L., Chaplin, William J., Colman, Isabel L., Coughlin, Jeff L., Davies, Guy, Hirano, Teruyuki, Howard, Andrew W., and Isaacson, Howard. 2019. "The Curious Case of KOI 4: Confirming Kepler’s First Exoplanet Detection." The Astronomical Journal 157:192. https://doi.org/10.3847/1538-3881/ab0e8e
ID: 151837
Type: article
Authors: Chontos, Ashley; Huber, Daniel; Latham, David W.; Bieryla, Allyson; Van Eylen, Vincent; Bedding, Timothy R.; Berger, Travis; Buchhave, Lars A.; Campante, Tiago L.; Chaplin, William J.; Colman, Isabel L.; Coughlin, Jeff L.; Davies, Guy; Hirano, Teruyuki; Howard, Andrew W.; Isaacson, Howard
Abstract: The discovery of thousands of planetary systems by Kepler has demonstrated that planets are ubiquitous. However, a major challenge has been the confirmation of Kepler planet candidates, many of which still await confirmation. One of the most enigmatic examples is KOI 4.01, Kepler’s first discovered planet candidate detection (as KOI 1.01, 2.01, and 3.01 were known prior to launch). Here we present the confirmation and characterization of KOI 4.01 (now Kepler-1658), using a combination of asteroseismology and radial velocities. Kepler-1658 is a massive, evolved subgiant (M = 1.45 ± 0.06 M , R = 2.89 ± 0.12 R ) hosting a massive ({M}{{p}} = 5.88 ± 0.47 {M}{{J}}, {R}{{p}} = 1.07 ± 0.05 {R}{{J}}) hot Jupiter that orbits every 3.85 days. Kepler-1658 joins a small population of evolved hosts with short-period (≤100 days) planets and is now the closest known planet in terms of orbital period to an evolved star. Because of its uniqueness and short orbital period, Kepler-1658 is a new benchmark system for testing tidal dissipation and hot Jupiter formation theories. Using all four years of the Kepler data, we constrain the orbital decay rate to be \dot{P} ≤ ‑0.42 s yr‑1, corresponding to a strong observational limit of {Q}\star {\prime } ≥ 4.826 × {10}3 for the tidal quality factor in evolved stars. With an effective temperature of {T}eff} ∼ 6200 K, Kepler-1658 sits close to the spin–orbit misalignment boundary at ∼6250 K, making it a prime target for follow-up observations to better constrain its obliquity and to provide insight into theories for hot Jupiter formation and migration.
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.
A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESSHuber, DanielChaplin, William J.Chontos, AshleyKjeldsen, HansChristensen-Dalsgaard, JørgenBedding, Timothy R.Ball, WarrickBrahm, RafaelEspinoza, NestorHenning, ThomasJordán, AndrésSarkis, PaulaKnudstrup, EmilAlbrecht, SimonGrundahl, FrankFredslund Andersen, MadsPallé, Pere L.Crossfield, IanFulton, BenjaminHoward, Andrew W.Isaacson, Howard T.Weiss, Lauren M.Handberg, RasmusLund, Mikkel N.Serenelli, Aldo M.Rørsted Mosumgaard, JakobStokholm, AmalieBieryla, AllysonBuchhave, Lars A.Latham, David W.Quinn, Samuel N.Gaidos, EricHirano, TeruyukiRicker, George R.Vanderspek, Roland K.Seager, SaraJenkins, Jon M.Winn, Joshua N.Antia, H. M.Appourchaux, ThierryBasu, SarbaniBell, Keaton J.Benomar, OthmanBonanno, AlfioBuzasi, Derek L.Campante, Tiago L.Çelik Orhan, Z.Corsaro, EnricoCunha, Margarida S.Davies, Guy R.Deheuvels, SebastienGrunblatt, Samuel K.Hasanzadeh, AmirDi Mauro, Maria PiaGarcía, Rafael A.Gaulme, PatrickGirardi, LéoGuzik, Joyce A.Hon, MarcJiang, ChenKallinger, ThomasKawaler, Steven D.Kuszlewicz, James S.Lebreton, YvelineLi, TandaLucas, MilesLundkvist, Mia S.Mann, Andrew W.Mathis, StéphaneMathur, SavitaMazumdar, AnweshMetcalfe, Travis S.Miglio, AndreaMonteiro, Mário J. P. F. G.Mosser, BenoitNoll, AnthonyNsamba, BenardOng, Jia Mian JoelÖrtel, S.Pereira, FilipeRanadive, PriteshRégulo, ClaraRodrigues, Thaíse S.Roxburgh, Ian W.Silva Aguirre, VictorSmalley, BarrySchofield, MathewSousa, Sérgio G.Stassun, Keivan G.Stello, DennisTayar, JamieWhite, Timothy R.Verma, KuldeepVrard, MathieuYıldız, M.Baker, DavidBazot, MichaëlBeichmann, CharlesBergmann, ChristophBugnet, LisaCale, BrysonCarlino, RobertoCartwright, Scott M.Christiansen, Jessie L.Ciardi, David R.Creevey, OrlaghDittmann, Jason A.Do Nascimento, Jose-Dias, Jr.Van Eylen, VincentFürész, GaborGagné, JonathanGao, PeterGazeas, KosmasGiddens, FrankHall, Oliver J.Hekker, SaskiaIreland, Michael J.Latouf, NatashaLeBrun, DannyLevine, Alan M.Matzko, WilliamNatinsky, EvaPage, EmmaPlavchan, PeterMansouri-Samani, MasoudMcCauliff, SeanMullally, Susan E.Orenstein, BrendanGarcia Soto, AylinPaegert, Martinvan Saders, Jennifer L.Schnaible, ChloeSoderblom, David R.Szabó, RóbertTanner, AngelleTinney, C. G.Teske, JohannaThomas, AlexandraTrampedach, RegnerWright, DuncanYuan, Thomas T.Zohrabi, FarzanehDOI: info:10.3847/1538-3881/ab1488v. 157245
Huber, Daniel, Chaplin, William J., Chontos, Ashley, Kjeldsen, Hans, Christensen-Dalsgaard, Jørgen, Bedding, Timothy R., Ball, Warrick, Brahm, Rafael, Espinoza, Nestor, Henning, Thomas, Jordán, Andrés, Sarkis, Paula, Knudstrup, Emil, Albrecht, Simon, Grundahl, Frank, Fredslund Andersen, Mads, Pallé, Pere L., Crossfield, Ian, Fulton, Benjamin, Howard, Andrew W., Isaacson, Howard T., Weiss, Lauren M., Handberg, Rasmus, Lund, Mikkel N., Serenelli, Aldo M. et al. 2019. "A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS." The Astronomical Journal 157:245. https://doi.org/10.3847/1538-3881/ab1488
ID: 152885
Type: article
Authors: Huber, Daniel; Chaplin, William J.; Chontos, Ashley; Kjeldsen, Hans; Christensen-Dalsgaard, Jørgen; Bedding, Timothy R.; Ball, Warrick; Brahm, Rafael; Espinoza, Nestor; Henning, Thomas; Jordán, Andrés; Sarkis, Paula; Knudstrup, Emil; Albrecht, Simon; Grundahl, Frank; Fredslund Andersen, Mads; Pallé, Pere L.; Crossfield, Ian; Fulton, Benjamin; Howard, Andrew W.; Isaacson, Howard T.; Weiss, Lauren M.; Handberg, Rasmus; Lund, Mikkel N.; Serenelli, Aldo M.; Rørsted Mosumgaard, Jakob; Stokholm, Amalie; Bieryla, Allyson; Buchhave, Lars A.; Latham, David W.; Quinn, Samuel N.; Gaidos, Eric; Hirano, Teruyuki; Ricker, George R.; Vanderspek, Roland K.; Seager, Sara; Jenkins, Jon M.; Winn, Joshua N.; Antia, H. M.; Appourchaux, Thierry; Basu, Sarbani; Bell, Keaton J.; Benomar, Othman; Bonanno, Alfio; Buzasi, Derek L.; Campante, Tiago L.; Çelik Orhan, Z.; Corsaro, Enrico; Cunha, Margarida S.; Davies, Guy R.; Deheuvels, Sebastien; Grunblatt, Samuel K.; Hasanzadeh, Amir; Di Mauro, Maria Pia; García, Rafael A.; Gaulme, Patrick; Girardi, Léo; Guzik, Joyce A.; Hon, Marc; Jiang, Chen; Kallinger, Thomas; Kawaler, Steven D.; Kuszlewicz, James S.; Lebreton, Yveline; Li, Tanda; Lucas, Miles; Lundkvist, Mia S.; Mann, Andrew W.; Mathis, Stéphane; Mathur, Savita; Mazumdar, Anwesh; Metcalfe, Travis S.; Miglio, Andrea; Monteiro, Mário J. P. F. G.; Mosser, Benoit; Noll, Anthony; Nsamba, Benard; Ong, Jia Mian Joel; Örtel, S.; Pereira, Filipe; Ranadive, Pritesh; Régulo, Clara; Rodrigues, Thaíse S.; Roxburgh, Ian W.; Silva Aguirre, Victor; Smalley, Barry; Schofield, Mathew; Sousa, Sérgio G.; Stassun, Keivan G.; Stello, Dennis; Tayar, Jamie; White, Timothy R.; Verma, Kuldeep; Vrard, Mathieu; Yıldız, M.; Baker, David; Bazot, Michaël; Beichmann, Charles; Bergmann, Christoph; Bugnet, Lisa; Cale, Bryson; Carlino, Roberto; Cartwright, Scott M.; Christiansen, Jessie L.; Ciardi, David R.; Creevey, Orlagh; Dittmann, Jason A.; Do Nascimento, Jose-Dias, Jr.; Van Eylen, Vincent; Fürész, Gabor; Gagné, Jonathan; Gao, Peter; Gazeas, Kosmas; Giddens, Frank; Hall, Oliver J.; Hekker, Saskia; Ireland, Michael J.; Latouf, Natasha; LeBrun, Danny; Levine, Alan M.; Matzko, William; Natinsky, Eva; Page, Emma; Plavchan, Peter; Mansouri-Samani, Masoud; McCauliff, Sean; Mullally, Susan E.; Orenstein, Brendan; Garcia Soto, Aylin; Paegert, Martin; van Saders, Jennifer L.; Schnaible, Chloe; Soderblom, David R.; Szabó, Róbert; Tanner, Angelle; Tinney, C. G.; Teske, Johanna; Thomas, Alexandra; Trampedach, Regner; Wright, Duncan; Yuan, Thomas T.; Zohrabi, Farzaneh
Abstract: We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R = 2.943 ± 0.064 R ), mass (M = 1.212 ± 0.074 M ), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a “hot Saturn” (R p = 9.17 ± 0.33 R ) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F , and moderate mass (M p = 60.5 ± 5.7 M ) and density (ρ p = 0.431 ± 0.062 g cm‑3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R ) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology.
KELT-23Ab: A Hot Jupiter Transiting a Near-solar Twin Close to the TESS and JWST Continuous Viewing ZonesJohns, DanielReed, Phillip A.Rodriguez, Joseph E.Pepper, JoshuaStassun, Keivan G.Penev, KaloyanGaudi, B. ScottLabadie-Bartz, JonathanFulton, Benjamin J.Quinn, Samuel N.Eastman, Jason D.Ciardi, David R.Hirsch, LeaStevens, Daniel J.Stevens, Catherine P.Oberst, Thomas E.Cohen, David H.Jensen, Eric L. N.Benni, PaulVillanueva, Steven, Jr.Murawski, GabrielBieryla, AllysonLatham, David W.Vanaverbeke, SiegfriedDubois, FrankyRau, SteveLogie, LudwigRauenzahn, Ryan F.Wittenmyer, Robert A.Zambelli, RobertoBayliss, DanielBeatty, Thomas G.Collins, Karen A.Colón, Knicole D.Curtis, Ivan A.Evans, PhilGregorio, JoaoJames, DavidDePoy, D. L.Johnson, Marshall C.Joner, Michael D.Kasper, David H.Khakpash, SomayehKielkopf, John F.Kuhn, Rudolf B.Lund, Michael B.Manner, MarkMarshall, Jennifer L.McLeod, Kim K.Penny, Matthew T.Relles, HowardSiverd, Robert J.Stephens, Denise C.Stockdale, ChrisTan, Thiam-GuanTrueblood, MarkTrueblood, PatYao, XinyuDOI: info:10.3847/1538-3881/ab24c7v. 15878
Johns, Daniel, Reed, Phillip A., Rodriguez, Joseph E., Pepper, Joshua, Stassun, Keivan G., Penev, Kaloyan, Gaudi, B. Scott, Labadie-Bartz, Jonathan, Fulton, Benjamin J., Quinn, Samuel N., Eastman, Jason D., Ciardi, David R., Hirsch, Lea, Stevens, Daniel J., Stevens, Catherine P., Oberst, Thomas E., Cohen, David H., Jensen, Eric L. N., Benni, Paul, Villanueva, Steven, Jr., Murawski, Gabriel, Bieryla, Allyson, Latham, David W., Vanaverbeke, Siegfried, Dubois, Franky et al. 2019. "KELT-23Ab: A Hot Jupiter Transiting a Near-solar Twin Close to the TESS and JWST Continuous Viewing Zones." The Astronomical Journal 158:78. https://doi.org/10.3847/1538-3881/ab24c7
ID: 154278
Type: article
Authors: Johns, Daniel; Reed, Phillip A.; Rodriguez, Joseph E.; Pepper, Joshua; Stassun, Keivan G.; Penev, Kaloyan; Gaudi, B. Scott; Labadie-Bartz, Jonathan; Fulton, Benjamin J.; Quinn, Samuel N.; Eastman, Jason D.; Ciardi, David R.; Hirsch, Lea; Stevens, Daniel J.; Stevens, Catherine P.; Oberst, Thomas E.; Cohen, David H.; Jensen, Eric L. N.; Benni, Paul; Villanueva, Steven, Jr.; Murawski, Gabriel; Bieryla, Allyson; Latham, David W.; Vanaverbeke, Siegfried; Dubois, Franky; Rau, Steve; Logie, Ludwig; Rauenzahn, Ryan F.; Wittenmyer, Robert A.; Zambelli, Roberto; Bayliss, Daniel; Beatty, Thomas G.; Collins, Karen A.; Colón, Knicole D.; Curtis, Ivan A.; Evans, Phil; Gregorio, Joao; James, David; DePoy, D. L.; Johnson, Marshall C.; Joner, Michael D.; Kasper, David H.; Khakpash, Somayeh; Kielkopf, John F.; Kuhn, Rudolf B.; Lund, Michael B.; Manner, Mark; Marshall, Jennifer L.; McLeod, Kim K.; Penny, Matthew T.; Relles, Howard; Siverd, Robert J.; Stephens, Denise C.; Stockdale, Chris; Tan, Thiam-Guan; Trueblood, Mark; Trueblood, Pat; Yao, Xinyu
Abstract: We announce the discovery of KELT-23Ab, a hot Jupiter transiting the relatively bright (V = 10.3) star BD+66 911 (TYC 4187-996-1), and characterize the system using follow-up photometry and spectroscopy. A global fit to the system yields host-star properties of {T}eff} =5900+/- 49 K, {M}* ={0.945}-0.054+0.060 {M}, {R}* =0.995+/- 0.015 {R}, {L}* ={1.082}-0.048+0.051 {L}, {log}{g}\star ={4.418}-0.025+0.026 (cgs), and ≤ft[{Fe}/{{H}}\right]=-0.105+/- 0.077. KELT-23Ab is a hot Jupiter with a mass of {M}P={0.938}-0.042+0.045 {M}{{J}}, radius of {R}P=1.322+/- 0.025 {R}{{J}}, and density of {ρ }P={0.504}-0.035+0.038 g cm-3. Intense insolation flux from the star has likely caused KELT-23Ab to become inflated. The time of inferior conjunction is {T}0=2458149.40776+/- 0.00091 {BJD}}TDB} and the orbital period is P={2.255353}-0.000030+0.000031 days. There is strong evidence that KELT-23A is a member of a long-period binary star system with a less luminous companion, and due to tidal interactions, the planet is likely to spiral into its host within roughly a gigayear. This system has one of the highest positive ecliptic latitudes of all transiting planet hosts known to date, placing it near the Transiting Planet Survey Satellite and James Webb Space Telescope continuous viewing zones. Thus we expect it to be an excellent candidate for long-term monitoring and follow up with these facilities.
KOI-3890: a high-mass-ratio asteroseismic red giant+M-dwarf eclipsing binary undergoing heartbeat tidal interactionsKuszlewicz, James S.North, Thomas S. H.Chaplin, William J.Bieryla, AllysonLatham, David W.Miglio, AndreaBell, Keaton J.Davies, Guy R.Hekker, SaskiaCampante, Tiago L.Deheuvels, SebastienLund, Mikkel N.DOI: info:10.1093/mnras/stz1185v. 48714–23
Kuszlewicz, James S., North, Thomas S. H., Chaplin, William J., Bieryla, Allyson, Latham, David W., Miglio, Andrea, Bell, Keaton J., Davies, Guy R., Hekker, Saskia, Campante, Tiago L., Deheuvels, Sebastien, and Lund, Mikkel N. 2019. "KOI-3890: a high-mass-ratio asteroseismic red giant+M-dwarf eclipsing binary undergoing heartbeat tidal interactions." Monthly Notices of the Royal Astronomical Society 487:14– 23. https://doi.org/10.1093/mnras/stz1185
ID: 154148
Type: article
Authors: Kuszlewicz, James S.; North, Thomas S. H.; Chaplin, William J.; Bieryla, Allyson; Latham, David W.; Miglio, Andrea; Bell, Keaton J.; Davies, Guy R.; Hekker, Saskia; Campante, Tiago L.; Deheuvels, Sebastien; Lund, Mikkel N.
Abstract: KOI-3890 is a highly eccentric, 153-d period eclipsing, single-lined spectroscopic binary system containing a red giant star showing solar- like oscillations alongside tidal interactions. The combination of transit photometry, radial velocity observations, and asteroseismology has enabled the detailed characterization of both the red giant primary and the M-dwarf companion, along with the tidal interaction and the geometry of the system. The stellar parameters of the red giant primary are determined through the use of asteroseismology and grid-based modelling to give a mass and radius of M_{\star }=1.04± 0.06 M_{☉} and R_{\star }=5.8± 0.2 R_{☉}, respectively. When combined with transit photometry, the M-dwarf companion is found to have a mass and radius of Mc=0.23± 0.01 M_{☉} and Rc=0.256± 0.007 R_{☉}. Moreover, through asteroseismology we constrain the age of the system through the red giant primary to be 9.1^{+2.4}_{-1.7} Gyr. This provides a constraint on the age of the M-dwarf secondary, which is difficult to do for other M-dwarf binary systems. In addition, the asteroseismic analysis yields an estimate of the inclination angle of the rotation axis of the red giant star of i=87.6^{+2.4}_{-1.2} degrees. The obliquity of the system - the angle between the stellar rotation axis and the angle normal to the orbital plane - is also derived to give ψ =4.2^{+2.1}_{-4.2} degrees, showing that the system is consistent with alignment. We observe no radius inflation in the M-dwarf companion when compared to current low-mass stellar models.